Author name code: foing
ADS astronomy entries on 2022-09-14
author:"Foing, Bernard H."
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Title: Astronaut analogue habitats as testing grounds for research
in stress and confinement conditions for future space missions
Authors: Miranda, Silvana; Foing, Bernard H.; Baatout, Sarah;
Kołodziejczyk, Agata; Baselet, Bjorn; Vermessen, Randy; Radstake,
Eline; Callant, Jonas; van Eysendeyk, Ot; van Linden Tol, Aoife;
Raimbault, Manuela
Bibcode: 2022cosp...44.2882M
Altcode:
The high pressure nature of a deep space mission and the confinement to
which the astronauts are subjected to has been known to increase their
stress levels. As we move to a new space era, with the implementation
of longer and more complex deep space missions characterized by
additional and new stress factors, such as distance from earth and
delay in communications, more research is required to understand
the physiological changes that result from such heightened stressful
environment. Analogue habitats are ground based facilities that are
developed to mimic the isolation and confinement to which a crew of
astronauts is exposed to. EuroMoonMarsPOLand (EMMPOL) analogue missions
arise from a collaboration between Analogue Astronaut Training Center
(AATC) and EuroMoonMars LUNEX/EMMESI EuroMoonMars Earth Space Innovation
and are specially developed for this purpose. During an isolation
period of 1 week, researchers can perform small research experiments
in a student-based atmosphere. At current, several biomarkers are being
proposed as potential monitoring targets to indicate the stress levels
of crew members during missions. Within this context, cortisol levels
in response to prolonged stress exposure have been shown to correlate
with increased DNA damage and to interfere with cell-cycle regulation
and DNA repair. To this aim, saliva is a body fluid that provides a
good correlation with serum values, can be collected in an non-invasive
manner and has the potential to serve as a tool for health monitoring of
astronauts during deep space missions. The aim of our pilot study was
to assess salivary cortisol levels and DNA damage in a crew of EMMPOL
analogue astronauts. We hypothesized that (1) salivary stress hormone
levels would be elevated during a prolonged stay in the habitat and that
(2) these elevated stress hormone levels are correlated to an increased
level of oxidative DNA damage markers found in saliva. For this purpose,
a crew of six analogue astronauts in total were isolated inside the
EMMPOL simulated moon habitat for the duration of one week. During
this period, saliva samples were collected immediately after waking,
followed by a one day sampling campaign on mission day one, day three
and the final mission day. Crew members were not allowed to brush their
teeth, exercise or eat 30 minutes prior to saliva sampling. DNA damage
was assessed by the marker 8-hydroxy-2'-deoxyguanosine (8-OHdG), a
byproduct of DNA damage repair. Both salivary cortisol and 8-OHdG levels
were measured via enzyme-linked immunosorbent assay (ELISA). Salivary
cortisol concentrations showed the expected daily circadian rhythm,
with a peak immediately after waking followed by a steady decrease. Of
interest, the total salivary cortisol concentration showed an increasing
trend during the duration of the mission with the highest measures
observed during the last day of the simulation. This increase in
salivary cortisol concentrations was correlated by an overall increase
in the total salivary 8-OHdG levels. Cortisol concentration in saliva
is a promising biomarker for stress monitoring during space simulation
missions and are potentially linked to an increase in oxidative DNA
damage. More data and longer mission durations are needed to better
understand the effects of isolation on the circadian cortisol rhythm,
its link to oxidative DNA damage and to uncover the full potential
of saliva as a monitoring tool for astronauts' health during space
missions. Acknowledgements: This work was funded by ESA/BELSPO/Prodex
IMPULSE-2 contract (PEA 4000109861). SM and ER are supported by
a doctoral SCK CEN/UGhent grant. JC and OVE are supported by the
Catholic University of Leuven. The mission was made possible with
the organization of LUNEX/EMMESI EuroMoonMars Earth Space Innovation
and AATC.
Title: Highlights from ILEWG LUNEX EuroMoonMars Earth Space
Innovation, ArtMoonMars, Space Renaissance & EuroSpaceHub
Authors: Foing, Bernard H.
Bibcode: 2022cosp...44..292F
Altcode:
EuroMoonMars is an ILEWG/LUNEX programme in collaboration with
space agencies, academia, universities and research institutions
and industries. The programme includes research activities for
data analysis, instruments tests and development, field tests in
MoonMars analogue, pilot projects, training and hands-on workshops,
and outreach activities. Extreme environments on Earth often provide
similar terrain conditions to sites on the Moon and Mars. In order
to maximize scientific return it becomes more important to rehearse
mission operations in the field and through simulations. EuroMoonMars
field campaigns have then been organised in specific locations
of technical, scientific and exploration interest. Field tests
have been conduct ed in ESTEC, EAC, at Utah MDRS station , Eifel,
Rio Tinto, Iceland, La Reunion, LunAres AATC bases in Poland, and
at Hawaii. Latest campaigns have been conducted jointly between
EuroMoonMars -International Moon Base Alliance -HI-SEAS (EMMIHS)
at Mauna Loa Hawaii since 2018. Samples of different lava flows from
Mauna Loa have been compared to measurements of the Mars Exploration
Rovers (MER) in order to provide more insight in the similarities of the
effects of hydrous alteration on volcanic rocks on Mars. In lava tubes
accessible from HI-SEAS, Hawaii, there are several minerals present
that appear to form from the surrounding basaltic rock by hydrological
and microbial processes. The purpose of this study is to research the
secondary mineralization in lava tubes to understand the characteristics
and formation processes of the mineral precipitates as analogue for
the presence of secondary minerals in lava tubes on other terrestrial
bodies in the solar system. We supported telerobotic campaigns at Etna
in 2017 (DLR/ROBEX), and one in June 2022 (ARCHES collaboration) and
organized EMM-Etna in July 2021. We performed in 2019-2020 scouting
analogue campaigns in Iceland. The EuroMoonMars CHILL-ICE mission in
July-August 2021, was set in the Surtshellir-Stefanshellir cave system
in the Hallmundarhraun lava flow located in Western Iceland. We tested
instruments and equipment (rovers, drones) in a lunar_x0002_analogue
field terrain. 2x3 astronauts in EVA deployed ECHO emergency
shelter in a lavatube where they stayed for 2x3 days. In Chile,
the Atacama Desert and the neighboring Arid Central Andes (Puna)
represent a geograph_x0002_ical site whose particular environmental
conditions make it a potential Mars analogue. A scout Chile MoonMars
campaign was organized in February 2021, and a large Atacama Ojos del
Salado campaign was conducted 21 Feb-6 March 2022. The ArtMoonMars
programme of cultural and artistic activities was started in 2010 by
ILEWG/LUNEX Lunar Explorers Group in collaboration with ESA ESTEC and
number of partner institutions, with more than 45 events (workshops,
space artscience classes, public events, sessions at international
conferences) and exhibitions. What payload for an Artscience Museum
on the Moon ? After SMART-1 missions and lunar lander studies, Bernard
Foing was working on lander payload for Google Lunar X prize project and
built a prototype ExoGeoLab lander in 2009. He looked at possibility
to host cultural or artscience payload on such landers. More than 50
ArtMoonMars events between space science, technology and art communities
were organized since MoonLife Academy in 2010. The MoonGallery idea
and concept was developed by Bernard Foing from 2010 (inspired by FOTON
Biopan in 2005 and EXPOSE ISS in 2008), to send an expanded gallery of
artscience artefacts to the Moon on possible landers. The price for
such commercial landers is about 1 Meu/ kg therefore he targeted the
smallest weight possible, and he proposed a grid gallery 10x10 cm x 1
cm that could be attached to a 10 cm cubesat, or to a lander. He called
this concept MoonGallery, as an international collaborative artwork and
a gallery of ideas worth sending to the Moon. Moon Gallery aims to set
up the first permanent museum on the Moon. Moon Gallery will launch
100 artefacts to the Moon within the compact format of 10 x 10 x 1cm
plate on a lunar lander exterior panelling as early as 2022 . What are
the ideas we want to promote into the future? What are the ideas we
want to leave behind? A MoonGallery project team was formed in 2018
to issue a call for the community of artists. For these activities,
ILEWG established ArtMoonMars grants to MoonGallery curators, and to
some artists or temporary team members. The MoonGallery team since
2018 together created more than 30 events, workshops, exhibitions
where ArtMoonMars and MoonGallery activies were presented and where
artscientists were participating.' MoonGallery Test ISS is one of the
ongoing projects of MGF. A contract was signed with NanoRacks provider
company to launch MG-ISS operate it, and return it to Earth. A new
effort with external partners building on previous ArtMoonMars and
EuroMoonMars pro_x0002_grammes led to the definition of a new MoonMars
initiative with broader objectives to develop opportu_x0002_nities
and funding, to various groups including space artists. ArtMoonMars
also collaborates with Space Renaissance Art chapter.
Title: Celebrating the First International Moon Day
Authors: Danos, George A.; Foing, Bernard H.; Murrow, David
Bibcode: 2022cosp...44..293D
Altcode:
The UN GA has declared the 20th of July as the International
Moon Day. This will be celebrated for the first time at COSPAR
2022. Representatives from the Moon Village Association, the Cyprus
Space Research Organization, Lockheed Martin, and International Lunar
Exploration Working Group will present the importance of this day.
Title: ALOHA - the new Analog Lunar Outpost Habitats for Astronautics,
a precursor for the future analog Moon Village
Authors: Bustamante, Ignacio; Foing, Bernard H.
Bibcode: 2022cosp...44..302B
Altcode:
We present the Analog Lunar Outpost Habitats & Astronautics
(ALOHA) project, an analog precursor for the future Moon Village. The
objective of the project is to create the prototype of a new generation
of versatile, affordable, and science agnostic analog habitats. The
project will include the definition and integration of laboratories
and experiments in the fields of astrophysics, photonics, robotics
and astrobiology, to be used on field campaigns during the project,
which will serve as a conduit for organizations to kickoff their
own initiatives. The final goal of ALOHA is to create a European hub
for astronautic training, to be used by industry, public and private
institutions, in and out of the space sector, for the qualification
of personnel in activities related to astronautics. These objectives
will be achieved by (1) the procurement of two analog habitats,
one stationary, and one mobile, (2) the design and implementation of
laboratories, robotic infrastructures, and experiments specific for
analog astronautic training, and (3) the execution of a number of field
campaigns in different sites of Europe to test and demonstrate the full
potential of the project. The project will have an expected duration of
3 years, scheduled so its results and conclusions will be applicable
for the upcoming Artemis mission, and will include a legacy program
to extend its lifetime and impact. This project is being coordinated
by the Lunar Explorers Society/ILEWG, along with European Universities
and industry experts.
Title: EMMPOL 10 & 11 Space Analog Simulation Campaigns: studies
on physiology, space technologies and life support
Authors: Dobney, William; Foing, Bernard H.; Baatout, Sarah;
Kołodziejczyk, Agata; Harasymczuk, Matt; Pavanello, . Sofia, ,
PROF.; Tabury, Kevin; Baselet, Bjorn; Frering, Philippe; Bustamante,
Ignacio; Palma, Flavia; Claeys, Kato; Mutte, Saikumar; Gautam, Kiran;
Byrne, Luke; Solbiati, Sarah; Renaghan, Jack; Reymen, Brent; Perrier,
Iona-Roxana; Avila-Rauch, Celia; Vadakken Gigimon, Anet
Bibcode: 2022cosp...44.2881D
Altcode:
Since 2020, it has been possible to participate in space analog missions
in Poland. Thanks to the Analog Astronaut Training Center (AATC), a
series of EuroMoonMars POLand (EMMPOL) habitat isolation missions are
taking place. The aim of these campaigns is to investigate the effects
of isolation on the crew as well as to conduct unique scientific
experiments to advance space science. These missions also serve as
training simulations to prepare future astronauts for the rigours
of space exploration. The EMMPOL 10-11 missions will take place in
April 2022. The crew will be supported by mission control. Both these
seven-day isolation periods will give the crew the opportunity to
broaden their scientific skills and knowledge as they perform their
individual and collective experiments. Communal activities, such as
eating, physical training and rests, will aid the crew to work as a
collective. The EMMPOL 10-11 campaigns have crews of five to six analog
astronauts, with each crew member being assigned a role based on their
expertise and background. Crew composition for EMMPOL 10/11 is the
following: commander (I. Bustamante/P. Frering), vice-commander/Capcom
(W. Dobney/K. Gautam), medical officer / biomedical engineer
(F. Palma, S. Solbiati), engineer (S. Mutte/ L. Bryne/J. Renaghan),
public relations officer (K. Claeys/A. Gigimon). During these isolation
periods, a series of important scientific experiments will take place
to investigate different aspects of space travel. These experiments
include comprehensive physiological studies related to nutrition,
sleep, blood, cognitive skills, mental health, memory, and the
effects of cryotherapy. Furthermore, the impact of virtual reality on
stress levels, metabolism and other physiological parameters including
breathing and heart activity will be monitored. Simultaneously, studies
focusing on living quarter usage and proxemics will take place. The
use of remote-controlled telescopes from inside this isolated, confined
and artificial environment representative of a space habitat, will be
evaluated. Lastly, space life support systems (plants, rotifers and
bacteria) and crystal structure growth, in specifically designed 3D
printed modules, will be subjected to simulated microgravity using
a Random Positioning Machine (RPM) along with cryogenic treatments
to study the effects of microgravity and temperature dependant
behaviour. To further aid the mission, a dedicated imaging system will
be developed and mounted on the RPM. The results obtained during EMMPOL
10 & 11 will further broaden our scientific understanding and the
effects of isolation in a space analog habitat. Such missions will be
discussed in detail in this presentation. Acknowledgements: Student
grants and support provided by KU Leuven, SCK CEN and EMMESI. This work
was funded by ESA/BELSPO/Prodex IMPULSE-2 contract (PEA 4000109861). The
mission was made possible with the organization of EuroMoonMars and
AATC Poland.
Title: The EDIBLES survey. V. Line profile variations in the λλ5797,
6379, and 6614 diffuse interstellar bands as a tool to constrain
carrier sizes
Authors: MacIsaac, Heather; Cami, Jan; Cox, Nick L. J.; Farhang, Amin;
Smoker, Jonathan; Elyajouri, Meriem; Lallement, Rosine; Sarre, Peter
J.; Cordiner, Martin A.; Fan, Haoyu; Kulik, Klay; Linnartz, Harold;
Foing, Bernard H.; van Loon, Jacco Th.; Mulas, Giacomo; Smith, Keith T.
Bibcode: 2022A&A...662A..24M
Altcode: 2022arXiv220301803M
Context. Several diffuse interstellar bands (DIBs) have profiles
with resolved sub-peaks that resemble rotational bands of large
molecules. Analysis of these profiles can constrain the sizes and
geometries of the DIB carriers, especially if the profiles exhibit
clear variations along lines of sight probing different physical
conditions.
Aims: Using the extensive data set from the ESO
Diffuse Interstellar Bands Large Exploration Survey we searched
for systematic variations in the peak-to-peak separation of these
sub-peaks for three well-known DIBs in lines of sight with a single
dominant interstellar cloud.
Methods: We used the spectra of
twelve single-cloud sight lines to examine the λλ5797, 6379, and
6614 DIB profiles. We measured the peak-to-peak separation in the band
profile substructures for these DIBs. We adopted the rotational contour
formalism for linear or spherical top molecules to infer the rotational
constant for each DIB carrier and the rotational excitation temperature
in the sight lines. We compared these to experimentally or theoretically
obtained rotational constants for linear and spherical molecules to
estimate the DIB carrier sizes.
Results: All three DIBs have peak
separations that vary systematically between lines of sight, indicating
correlated changes in the rotational excitation temperatures. The
rotational constant B of the λ6614 DIB was determined independently
of the rotational excitation temperature; we derived B6614
= (22.2 ± 8.9) x 10−3 cm−1, consistent
with previous estimates. Assuming a similar rotational temperature
for the λ6614 DIB carrier and assuming a linear carrier, we found
B5797linear = (5.1 ± 2.0) × 10−3
cm−1 and B6379linear = (2.3
± 0.9) × 10−3 cm−1. If the carriers of
those DIBs are spherical species, on the other hand, their rotational
constants are half that value, B5797spherical
= (2.6 ± 1.0) × 10−3 cm−1 and
B6379spherical = (1.1 ± 0.4) × 10−3
cm−1.
Conclusions: Systematic variations in the DIB
profiles provide the means to constrain the molecular properties. We
estimate molecule sizes that range from 7-9 carbon atoms (λ6614
carrier, linear) to 77-114 carbon atoms (λ6379, spherical).
Title: Space Habitat Astronautics: Multicolour Lighting Psychology
in a 7-Day Simulated Habitat
Authors: Jiang, Ao; Schlacht, Irene Lia; Yao, Xiang; Foing, Bernard;
Fang, Zhixiong; Westland, Stephen; Hemingray, Caroline; Yao, Wenhao
Bibcode: 2022SpScT202282706J
Altcode:
During space missions, astronauts live in a confined technological
environment, completely isolated and deprived of the variety and
variation found in the environment on Earth. This circumstance
has a strong impact on the psycho-physiological states of the
crew. Particularly in light of the plans for long-duration missions,
new research needs to be carried out. The goal of this study, conducted
at Xiangtan Central Hospital in China, was to test whether multicolour
lighting can improve people's psychological state in an isolated and
confined environment over a period of seven days. Twenty participants
(10 male and 10 female) were randomly divided into two groups: one group
that was exposed to multicolour lighting and a control group, which
was exposed to a static, monotonous white interior. The participants'
psychological state was recorded on the first day, the fourth day,
and the seventh day. The results of the control group showed that
the participants' negative emotions and anxiety continued to increase
over time, whereas the group randomly exposed to multicolour lighting
that changed every three hours did not show any significant increase
in negative emotions and anxiety. Moreover, the random change
of light colour in the isolated environment appeared to help the
participants increase their sense of surprise, thereby counteracting
monotony. Finally, during this experiment, it was observed that when
people who are accustomed to being connected to social networks were
deprived of this, they experienced insomnia and unaccustomed reactions,
in particular on the first days of deprivation. This article contributes
to future space exploration and to social and psychological support
of life in isolated and confined environments.
Title: Exploring the Benefits of Analog Astronautical Simulations
in ICEE (Isolated, Confined Extreme Environments) as Preparation
for Geological Artemis EVAs (Extra-Vehicular Activities)
Authors: Pouwels, C. R.; Poli, E. C.; Musilova, M.; Nunes, A. P. C. P.;
Toop-Rose, J.; Heemskerk, M. V.; Foing, B. H.
Bibcode: 2022LPICo2678.2198P
Altcode:
An international and interdisciplinary overview of some of the benefits
of ICEE Analog Astronaut missions for future extraterrestrial human
geo-exploration.
Title: Families and clusters of diffuse interstellar bands: a
data-driven correlation analysis
Authors: Fan, Haoyu; Schwartz, Madison; Farhang, Amin; Cox, Nick L. J.;
Ehrenfreund, Pascale; Monreal-Ibero, Ana; Foing, Bernard H.; Salama,
Farid; Kulik, Klay; MacIsaac, Heather; van Loon, Jacco Th; Cami, Jan
Bibcode: 2022MNRAS.510.3546F
Altcode: 2021MNRAS.tmp.3337F; 2021arXiv211204541F
More than 500 diffuse interstellar bands (DIBs) have been observed in
astronomical spectra, and their signatures and correlations in different
environments have been studied over the past decades to reveal clues
about the nature of the carriers. We compare the equivalent widths
of the DIBs, normalized to the amount of reddening, EB-V,
to search for anticorrelated DIB pairs using a data sample containing
54 DIBs measured in 25 sightlines. This data sample covers most of
the strong and commonly detected DIBs in the optical region, and the
sightlines probe a variety of interstellar medium conditions. We find
that 12.9 per cent of the DIB pairs are anticorrelated, and the lowest
Pearson correlation coefficient is rnorm ~ -0.7. We revisit
correlation-based DIB families and are able to reproduce the assignments
of such families for the well-studied DIBs by applying hierarchical
agglomerative and k-means clustering algorithms. We visualize the
dissimilarities between DIBs, represented by 1 - rnorm,
using multidimensional scaling (MDS). With this representation, we find
that the DIBs form a rather continuous sequence, which implies that
some properties of the DIB carriers are changing gradually following
this sequence. We also find that at that least two factors are needed
to properly explain the dissimilarities between DIBs. While the first
factor may be interpreted as related to the ionization properties
of the DIB carriers, a physical interpretation of the second factor
is less clear and may be related to how DIB carriers interact with
surrounding interstellar material.
Title: Multidisciplinary High Altitude Expedition in the Puna de
Atacama: Geo and Environmental Sciences as a First Step to Define
the Potential of the Ojos del Salado Region as a Terrestrial Analogue
Authors: Tavernier, A.; Garcia, A.; Ulloa, C.; Allard, C.; Astudillo,
P.; Behn, C.; Beniest, A.; Bonnail, E.; Borella, E.; Bosco, G.;
Bustamante, I.; Caviedes, C.; Crotti, S.; Echeverria, C.; Ehreiser, A.;
Giacon, T.; Heemskerk, M.; Ibarra, C.; Indriðadóttir, B.; Marquardt,
A.; McGrath, K.; Mrakic-Sposta, S.; Narici, M.; Pavanello, S.; Pinto,
G. A.; Schlarmann, L.; Strahsburger, E.; Sztajnkrycer, N.; Valenzuela,
M.; Vieira, R. K.; Foing, B.
Bibcode: 2022LPICo2678.2611T
Altcode:
This study presents the context of the organization of multidisciplinary
scientific expeditions in the Puna de Atacama, near the Ojos del
Salado volcano.
Title: An Endorsement to Utilize TerrestrialAanalogs as Support for
the Upcoming Artemis Missions
Authors: Pouwels, C.; Nunes, A. P. C. P.; Musilova, M.; Toop-Rose,
J.; Poli, E. C.; Foing, B.
Bibcode: 2022LPICo2678.1902P
Altcode:
An endorsement to utilize terrestrial analogs as support and pathway
for the upcoming human exploration missions such as Orion module
and Gateway.
Title: EuroMoonMars Earth Space Innovation Highlights
Authors: Foing, B. H.; Tavernier, A.; Crotti, S.; Pascual, J.;
Bustamante, I.; Kolodziejczyk, A.; Perrier, I. R.; Autino, A.;
Schlarmann, L.; Pouwels, C.; Heemskerk, M. V.; Pavanello, S.; Rogers,
H.; Musilova, M.; Ehreiser, A.; Stoker, C.; McGrath, K.; Baatout, S.;
Reymen, B.; Wedler, A.; Mura, J.; Kerber, S.; Mulder, S.; Feenstra,
M.; Eckelkamp, N.; Weert, A.; Castro, A.; Reilly, H.; Moyan, C.;
Brady, G.; Das Rajkakati, P.; Heemskerk, R.; Sirikan, N.; Boross,
H.; Landolina, R.; Spilkin, A.; EuroMoonMars Team
Bibcode: 2022LPICo2678.2042F
Altcode:
EMMESI EuroMoonMars Earth Space Innovation highlights at Utah MDRS,
HI-SEAS, Etna, Iceland, Chile Atacama for planetary science, technology,
and astronautics.
Title: Mars: new insights and unresolved questions - Corrigendum
Authors: Changela, Hitesh G.; Chatzitheodoridis, Elias; Antunes, Andre;
Beaty, David; Bouw, Kristian; Bridges, John C.; Capova, Klara Anna;
Cockell, Charles S.; Conley, Catharine A.; Dadachova, Ekaterina;
Dallas, Tiffany D.; de Mey, Stefaan; Dong, Chuanfei; Ellery, Alex;
Ferus, Martin; Foing, Bernard; Fu, Xiaohui; Fujita, Kazuhisa; Lin,
Yangting; Jheeta, Sohan; Hicks, Leon J.; Hu, Sen; Kereszturi, Akos;
Krassakis, Alexandros; Liu, Yang; Oberst, Juergen; Michalski, Joe;
Ranjith, P. M.; Rinaldi, Teresa; Rothery, David; Stavrakakis, Hector
A.; Selbmann, Laura; Sinha, Rishitosh K.; Wang, Alian; Williford, Ken;
Vaci, Zoltan; Vago, Jorge L.; Waltemathe, Michael; Hallsworth, John E.
Bibcode: 2022IJAsB..21...46C
Altcode:
No abstract at ADS
Title: C60+ diffuse interstellar band
correlations and environmental variations
Authors: Schlarmann, Leander; Foing, Bernard; Cami, Jan; Fan, Haoyu
Bibcode: 2021A&A...656L..17S
Altcode: 2021arXiv211203593S
Context. The diffuse interstellar bands (DIBs) are absorption
features seen in the spectra of astronomical objects that arise
in the interstellar medium. Today, more than 500 DIBs have been
observed, mostly in the optical and near-infrared wavelengths. The
origin of the DIBs is unclear; only ionised buckminsterfullerene,
C60+, has been identified as a viable candidate
for two strong and three weaker DIBs.
Aims: We investigate
the correlations between the strengths of the two strongest
C60+ DIBs as well as their environmental
behaviour.
Methods: We analysed measurements of the strengths
of the two C60+ DIBs at 9577 and 9633 Å for
26 lines of sight. We used two different methods, including Monte
Carlo simulations, to study their correlations and the influence of
measurement errors on the correlation coefficients. We examined how the
strength of the C60+ DIBs changes as a result of
different environmental conditions, as measured by the concentration
of H/H2 and the strength of the ambient UV radiation.
Results: In contrast to results recently reported by Galazutdinov
et al. (2021, AJ, 161, 127), we find a high correlation between the
strengths of the C60+ DIBs. We also discovered
that the behaviour of the correlated C60+
bands is quite distinct from other DIBs at 5780, 5797, and 6203 Å in
different environments.
Title: Mars: new insights and unresolved questions
Authors: Changela, Hitesh G.; Chatzitheodoridis, Elias; Antunes, Andre;
Beaty, David; Bouw, Kristian; Bridges, John C.; Capova, Klara Anna;
Cockell, Charles S.; Conley, Catharine A.; Dadachova, Ekaterina;
Dallas, Tiffany D.; de Mey, Stefaan; Dong, Chuanfei; Ellery, Alex;
Ferus, Martin; Foing, Bernard; Fu, Xiaohui; Fujita, Kazuhisa; Lin,
Yangtin; Jheeta, Sohan; Hicks, Leon J.; Hu, Sen; Kereszturi, Akos;
Krassakis, Alexandros; Liu, Yang; Oberst, Juergen; Michalski, Joe;
Ranjith, P. M.; Rinaldi, Teresa; Rothery, David; Stavrakakis, Hector
A.; Selbmann, Laura; Sinha, Rishitosh K.; Wang, Alian; Williford, Ken;
Vaci, Zoltan; Vago, Jorge L.; Waltemathe, Michael; Hallsworth, John E.
Bibcode: 2021IJAsB..20..394C
Altcode: 2021arXiv211200596C
Mars exploration motivates the search for extraterrestrial life, the
development of space technologies, and the design of human missions and
habitations. Here we seek new insights and pose unresolved questions
relating to the natural history of Mars, habitability, robotic and
human exploration, planetary protection, and the impacts on human
society. Key observations and findings include:(1)high escape rates of
early Mars' atmosphere, including loss of water, impact present-day
habitability;(2)putative fossils on Mars will likely be ambiguous
biomarkers for life;(3)microbial contamination resulting from human
habitation is unavoidable;(4)based on Mars' current planetary protection
category, robotic payload(s) should characterize the local martian
environment for any life-forms prior to human habitation. Some
of the outstanding questions are:(1)which interpretation of the
hemispheric dichotomy of the planet is correct;(2)to what degree
did deep-penetrating faults transport subsurface liquids to Mars'
surface;(3)in what abundance are carbonates formed by atmospheric
processes;(4)what properties of martian meteorites could be used
to constrain their source locations;(5)the origin(s) of organic
macromolecules;(6)was/is Mars inhabited;(7)how can missions designed
to uncover microbial activity in the subsurface eliminate potential
false positives caused by microbial contaminants from Earth;(8)how
can we ensure that humans and microbes form a stable and benign
biosphere;(9)should humans relate to putative extraterrestrial life from
a biocentric viewpoint (preservation of all biology), or anthropocentric
viewpoint of expanding habitation of space? Studies of Mars' evolution
can shed light on the habitability of extrasolar planets. In addition,
Mars exploration can drive future policy developments and confirm (or
put into question) the feasibility and/or extent of human habitability
of space.
Title: Automatically detecting anomalous exoplanet transits
Authors: Hönes, Christoph J.; Miller, Benjamin Kurt; Heras, Ana M.;
Foing, Bernard H.
Bibcode: 2021arXiv211108679H
Altcode:
Raw light curve data from exoplanet transits is too complex to naively
apply traditional outlier detection methods. We propose an architecture
which estimates a latent representation of both the main transit and
residual deviations with a pair of variational autoencoders. We show,
using two fabricated datasets, that our latent representations of
anomalous transit residuals are significantly more amenable to outlier
detection than raw data or the latent representation of a traditional
variational autoencoder. We then apply our method to real exoplanet
transit data. Our study is the first which automatically identifies
anomalous exoplanet transit light curves. We additionally release
three first-of-their-kind datasets to enable further research.
Title: To other planets with upgraded millennial kombucha in rhythms
of sustainability and health support
Authors: Kozyrovska, Natalia; Reva, Oleg; Podolich, Olga; Kukharenko,
Olga; Orlovska, Iryna; Terzova, Vitalia; Zubova, Ganna; Trovatti
Uetanabaro, Ana Paula; Góes-Neto, Aristóteles; Azevedo, Vasco;
Barh, Debmalya; Verseux, Cyprien; Billi, Daniela; Kołodziejczyk,
Agata Maria; Foing, Bernard; Demets, René; de Vera, Jean-Pierre
Bibcode: 2021FrASS...8..182K
Altcode:
Humankind has entered a new era of space exploration: settlements on
other planetary bodies are foreseen in the near future. Advanced
technologies are being developed to support the adaptation to
extraterrestrial environments and, with a view on the longer term, to
support the viability of an independent economy. Biological processes
will likely play a key role and lead to the production of life-support
consumables, and other commodities, in a way that is cheaper and more
sustainable than exclusively abiotic processes. Microbial communities
could be used to sustain the crews' health as well as for the production
of consumables, for waste recycling, and for biomining. They can
self-renew with little resources from Earth, be highly productive
on a per-volume basis, and be highly versatile—all of which
will be critical in planetary outposts. Well-defined, semi-open,
and stress-resistant microecosystems are particularly promising. An
instance of it is kombucha, known worldwide as a microbial association
that produces an eponymous, widespread soft drink that could be valuable
for sustaining crews' health or as a synbiotic (i.e., probiotic and
prebiotic) after a rational assemblage of defined probiotic bacteria
and yeasts with endemic or engineered cellulose producers. Bacterial
cellulose products offer a wide spectrum of possible functions, from
leather-like to innovative smart materials during long-term missions and
future activities in extraterrestrial settlements. Cellulose production
by kombucha is zero-waste and could be linked to bioregenerative life
support system (BLSS) loops. Another advantage of kombucha lies in its
ability to mobilize inorganic ions from rocks, which may help feed BLSS
from local resources. Besides outlining those applications and others,
we discuss needs for knowledge and other obstacles, among which is
the biosafety of microbial producers.
Title: Rover testing for lunar science and innovation
Authors: Mohan, Chirayu; Foing, Bernard; Charasse, Mael-Alois
Bibcode: 2021EPSC...15..850M
Altcode:
REMMI, Rover for EuroMoonMars Investigations has been built at
EMMIHS campaign in HI-SEAS Hawaii in 2019 and teleoperated locally
and from The Netherlands. For EuroMoonMars 2021 projects, a number of
scientific experiments were carried out with the REMMI rover. These
experiments were based primarily on teleoperation of the REMMI rover
and its mobility system. The rover's mobility system is based on a
continuous track system. It was discovered through experimentation
that these tracks are suitable for a number of environments but
unsuitable for others. When testing was done in the Analog Astronaut
Training Center in Poland, the rover showed that it had difficulty
getting a grip on metal surfaces. However, through testing in other
outdoor facilities, it was observed that the rover had greater grip
on sandy surfaces, grass surfaces and rocks. There was, however,
a number of issues with these surfaces. On grass and rock surfaces,
small debris would often interfere with the gears of the rover and
would prevent movement. The solution to this would be to have a
covering to shield the mobility system from both smaller debris and
in future, lunar regolith. The rover also had issues with large slopes
and inclines. Overall, it was discovered that the REMMI rover was more
of a support rover than an exploration rover.The REMMI rover also has
a camera on it to allow for remote operation. This camera unlocks a
number of future possibilities. Firstly, it will allow the rover to
take pictures of samples and areas which the astronaut may want to
collect or explore. This is a great feature for the astronaut as they
will not have to waste oxygen and resources during an EVA searching
for samples. The REMMI rover's camera also unlocks the possibility
to use artificial intelligence to recognise different features of the
environment. Similar to self-driving cars, it would theoretically be
possible to allow the rover to recognise features of the landscape
which would show dangerous terrain for the rover or perhaps a new
area to discover. The possibilities will be further tested in July
2021 on Mt Etna, Italy. Acknowledgements: The authors would like to
thank the Analog Astronaut Training Center and Dr. Kołodziejczyk
for allowing the REMMI rover to be tested in their facilities and
for their support throughout. The authors would also like to thank
ILEWG EuroMoonMars for providing the REMMI rover for testing.Figure 1:
REMMI rover showing continuous track system and manoeuvrable camera.
Title: Instruments Operations, Science and Innovation in Expedition
Support: EuroMoonMars-Etna campaign 2021
Authors: Reilly, Hannah; Foing, Bernard; Brady, Gary; Mohan, Chirayu;
McGrath, Kevin; Lakomiec, Patrycja; Ehreiser, Anouk; De Palma, Gaia;
Schlarmann, Leander; Wedler, Armin; Schmitz, Nicole; Pagano, Isabella
Bibcode: 2021EPSC...15..848R
Altcode:
An expedition EMM-Etna to simulate the Lunar and Martian volcanic
and soil environment will be carried out at Mount.Etna's Cratere del
Laghetto in Sicily, near Catania Italy by the EuroMoonMars TUDublin
and LEAPS ExoMars groups. This scouting campaign intends to train in
using instruments to be used on MoonMars landers and rovers, with a
perspective of ARCHES DLR telerobotics campaign to be conducted in June
2022, and in preparation for ExoMars rover instruments (PANCAM, CLUPI
and spectrometers) science and operations. Figure 1: Lunar Lander and
REMMI Rover for Sample AnalysisThe aim of this EMM-Etna expedition is to
investigate and analyse the terrain with the use of different scientific
instruments. The topography of the landscape will be photographed
using a 360° panoramic camera and drone; it will be processed, and
a 3D model developed. The terrain will also be investigated using
the REMMI Rover, the abilities of the rover to operate and transport
equipment will be monitored. This will further develop the knowledge
available of the terrain and help future expeditions to identify
different landmarks. The use of a Radio Jove Antenna will permit the
team to monitor transmissions from both the Sun and Jupiter. This will
allow different cosmic events or changes in the celestial objects to
be studied and explored. On site a selection of different samples will
also be collected and examined using the REMMI Rover. An Ocean Optics
UV-Vis-NIR spectrometer will a be operated in order to evaluate the
existence of biological compounds and substances within these samples
and in the area itself. It is key to understand the molecular makeup
of one's surroundings when in an unknown environment. By analysing
samples collected, spectroscopy can be used to identify and determine
a diagnostic for each substance. This process will be monitored by a
Logitech camera to ensure it is carried put correctly. A selection of
photographs will be captured of each sample using a portable optical
microscope. This will allow an in-depth analysis of the microscopic
structure of each collected sample. The use of all of the instruments
mentioned above is key in the investigation and research into the Moon
and Martian-like volcanic environment that is Mount Etna.We would also
like to thank Prof I. Pagano's team from the University of Catania and
Dr A.Wedler's team from DLR Deutsches Zentrum für Luft- und Raumfahrt
for their support in organising this expedition.
Title: Characterization of the Potential of the Puna de Atacama region
in terms of Planetary Analogs : Preliminary results for the Salar
de Maricunga, Tres Cruces, Laguna Verde and Ojos del Salado Areas
Authors: Tavernier, Adrien; Garcia, Ayon; Ulloa, Christopher; Oses,
Romulo; Bonnail, Estefania; McGrath, Kevin; Mohan, Chirayu; Reilly,
Hannah; Brady, Gary; Foing, Bernard
Bibcode: 2021EPSC...15..452T
Altcode:
The Atacama Desert and the Puna (an ecoregion of the Central Andes that
mainly straddles three South American countries, Argentina, Bolivia
and Chile, with altitudes ranging from 3500 to 4800 meters above sea
level [masl] see. Figure 1) have extreme terrestrial environmental
characteristics that make these two geographic locations potential
analogs of the conditions that Mars may have experienced during its
geological history [1,2].Figure 1 : Geographical landmark / Bottom left,
Zoom in on the campaign area with sampling points present (Copyright
: Google Earth)The University of Atacama (UDA) located in Copiapo
(27º37S / 70º33W) in Chile, aims to conduct multidisciplinary
studies to better characterize the extreme environment of the Puna
de Atacama. This project is based, in particular, on the forthcoming
implementation of a high-altitude laboratory located at 3800 masl in
the vicinity of the Salar de Maricunga (26º92S / 69º08W) [3]. The
construction of this high-altitude laboratory should enable the
scientific exploration of the region to be strengthened. Moreover,
in order to benefit from expertise in the field of planetary analogs,
the UDA has approached the EuroMoonMars program [4], which has more
than ten years of experience in organizing analog field campaigns. This
partnership in the making has taken shape with the setting-up of a first
joint expedition at the end of February/beginning of March 2021. This
expedition was organized by the Cryosphere and Water laboratory of
the UDA (LICA) and has also been supported remotely by members of
the EuroMoonMars program. During this high-altitude 10-days campaign
(between 3800 and 6500 masl) the geographical extend included the
Salar de Maricunga (26º92S / 69º08W), the Tres Cruces (27º07S /
68º79W), the Laguna Verde (28º88S / 68º47W) and finally the Ojos del
Salado areas (27º11S / 68º54W) (see. Figure 1), whose potential as
a Martian analog has been highlighted in recent publications [5]. To
the initial objectives related to environmental sciences, scientific,
technical, logistical and medical protocols specific to planetary
science and space exploration were added, as the first steps towards
for the organization of more complex campaigns involving EuroMoonMars
people in the field. According to the multidisciplinary perspective of
characterizing the environment of the Puna de Atacama and in addition
to geophysical work, soil, water and biological material sampling was
carried out along an altitudinal gradient (see. Figure 1). This study
aims to review the preliminary results of these samples, notably via
the geochemical analysis of the soils (carried out using Inductively
Couple Plasma spectrometry (ICP) and X-fluorescence spectroscopy)
contextualized in the perspective of considering the Puna de Atacama
as a Martian analog. Acknowledgments: The authors would like to thank
the people involved in the success of this project, which aims to both
promote and protect the incredible natural heritage of the Puna de
Atacama region. References: [1] Navarro-González, R. et al. (2003)
Science, 302(5647), 1018-1021. [2] Schmidt, S. K. et al. Antonie
van Leeuwenhoek, 111(8), 1389-1401. [3] Tavernier, A. et al. (2021)
52nd LPSC conference 15-19 March, 2021. LPI Contribution No. 2548,
id.2253.[4] Foing, B. et al. (2020) p. EPSC2020-14. [5] Kereszturi,
Á. et al. (2020) Astrobiology, 20(6),677-683.
Title: Construction of the Inflatable Habitat ECHO for Inside a
Lunar-analogue Lava-tube
Authors: Pouwels, Charlotte; Fairburn, Sue; van Rikxoort, Bailee;
Alary, Marie-Pierre; Heemskerk, Marc; Kerber, Sabrina; Foing, Bernard
Bibcode: 2021EPSC...15..835P
Altcode:
; In the summer of 2021, the analogue astronaut mission "CHILL-ICE"
shall be carried out inside the Stefanshellir cave system. This short
term 2-night mission has the objective to put up an inflatable habitat
inside a Lunar-analogue Lava tube within 8 hours. This 8h requirement
simulates the lifespan of the oxygen tank that astronauts would have,
during an emergency Extra Vehicular Activity (EVA).Requirements; For the
CHILL-ICE mission, a habitat prototype has been developed by the Wilson
School of Design, Kwantlen Polytechnic University Canada. The habitat,
named acronymically ECHO (Extreme Cave Habitat One) needed to fulfil
the following mission requirements:8H put up/ Take down Essential for
the astronauts to stay alive. Portable for 2 persons to carry inside
the selected lava tube 38° slope / 11 m and max. weight 50 kg Free
standing Fidelity for an analogous mission and no reliance on ground
conditions. Habitable for 3 persons [2] Min. 8 m3 but preferred >21
m3 Re-deployable Needs to be used for recurring phases of analogue
missions. Airlock Fidelity in simulating the ingress/egress process
and the design of the structure. Water-resistant Interior needs to
stay dry. The caves on Earth can be subject to high humidity and cave
rain. Dimensional restrictions due to cave location. 7.5 x 4.6 x 4.15
m (Figure 1: Habitat material properties hierarchy.)For this analogue
mission and the construction of this habitat, the influence of gravity
and space vacuum has been neglected. For the design of the habitat,
all spaces shall require multiple functions to provide enough space
for a sleeping, bathroom, working and experiment station. Furthermore,
as the Stefanshellir cave system consist of a rocky basaltic terrain,
the floor of the habitat needs to be able to withstand possible
ruptures. The material priority hierarchy can be found in figure 1.All
materials selected for the habitat have been subjected, prior of usage,
to testing to comply with the material hierarchy as mentioned in figure
1.ECHO Habitat; The final result of the habitat can be seen in figure 2
and figure 3. The technical overview of the habitat features is given
in table 1.(Figure 2: The habitat ECHO (Extreme Cave Habitat One)
in a deployed state with airlock.)(Figure 3: Interior design of the
ECHO habitat with Airlock door provided and mylar pillows for thermal
insulation.) Habitat features Mass 30 kg Capacity 40 m3 Dimension 4.0 x
3.5 x 2.1 m Dim. Airlock 1.1 x 3.5 m Max. persons 3 Fly material Nylon
Shell material Tyvek (spun-bound polyethylene) Floor - Cordura nylon
- Mylar - Open Cell Polyurethane foam Free standing Yes Portal for
cabling Yes (Table 1: Overview of habitat features.)The selected form
of the habitat is a 'barrel vault' or 'Quonset' archetype. This shape
aligns with the available space left in the selected spot inside the
terrestrial lava tube. The structure of the habitat consists of four
air members and two poles. This combination results in a redundancy in
the event of air member failure and/or leakage. The skin is constructed
of Tyvek (spun-bound polyethylene) building membrane material. This
material is chosen upon its lightweight and economical benefits.In
addition, to protect ECHO and the analogue astronauts against any
lightweight falling debris from the cave an external lightweight fly
has been added to the shell. The floor is constructed of 3 layers
and is removable. These layers will provide thermal insultation, some
protection from the uneven/basalt cave floor and a durable surface for
the range of activities.As mentioned in table 1, the habitat offers
accommodation for 3 crew members comfortably. Inside the airlock,
1 crew member can get changed in their EVA suits, provided by the
Astroland Interplanetary Agency. When not in use, the EVA suits can be
stored in the airlock. The airlock room has a multifunction as it is
also the private bathroom area.Lastly, there is a set of mylar pillows
(see figure 2) that serve as thermal insulation and are reflective of
light sources. These pillows are to be filled with air, secured and
placed against the walls, as needed, to achieve and retain thermal
comfort. To hold the pillows in place, a set of diagonally placed
elastics are used. In addition, these elastics can also hold deployed
sleeping mattresses during the day. For storing lightweight items, a
set of pockets that run lengthwise in the main volume of the habitat are
made.Acknowledgements;First, we would like to thank the FULLAIR and ECHO
teams from Wilson School of Design (S. Fairburn, S. Phillips, L. Norris,
B. van Rikxoort, M. Alary, K. Langer, J. Legoff, A. Nelmes, D. Seriani,
A. Sullivan, G. Wong, C. Michel, W. Tsz Long Lo) for their amazing
work in research and developing this habitat for the CHILL-ICE mission,
during this difficult COVID period. They have been the key factor for
the success of this mission and therefore this research.In addition,
we would like to thank the whole CHILL-ICE team for their remote
support during the development of this habitat.Lastly, we acknowledge
the ILEWG EuroMoonMars manager B. Foing for making this research
possible.References;[1] M.V. Heemskerk et al., EGU2020-901-1, (2020)[2]
NASA STD-3000-90 8.6.2.1[3] 2021LPI....52.2762H2021/03CHILL-ICE
(Construction of a Habitat Inside a Lunar-Analogue Lava Tube): Building
and Testing of a Deployable Habitat in Icelandic Lava Tubes for Space
Exploration PurposesHeemskerk, M. V.; Pouwels, C. R.; Heemskerk, R. S.;
Kerber, S.; Foing, B. H.[4] 2021LPI....52.2502F2021/03Life and Research
at SouthPole Moonbase: EuroMoonMars Campaigns Results 2019-2020Foing,
B. H.; Rogers, H.; Musilova, M.; Weert, A.; Mulder, S.; Kerber, S.;
Castro, A.; Pouwels, C.; Das Rajkakati, P.; Heemskerk, M.; et al
Title: Science and innovation from the Moon: Radio antenna precursor
observations
Authors: Brady, Gary; Foing, Bernard
Bibcode: 2021EPSC...15..852B
Altcode:
In coordination with ILEWG EuroMoonMars, a number of radio antenna
tests have been carried out and analysed for solar observations. The
instrument used for this data collection is the radio Jove, connected
to a single dipole antenna at a set height. Data is recorded using
a software program known as Radio-SkyPipe and the audio from the
observations is analysed in person by the operator and recorded using
livestreaming platforms for later analysis. Noise is a major factor
while trying to operate this device, as such, a quiet location and fine
tuning is essential for isolating the favoured frequency range. Solar
activity plays a major role in the success of the device. While carrying
out solar observations, the sought after transmissions are from solar
bursts and flares. These transmissions can be very difficult to capture
as a result of low solar activity, up-time of the device and external
noise. The device has been tested in a number of locations in Leiden,
Netherlands and will be later tested on on lunar volcanic ash analogue
in Cratere di Laghetto, in Mount Etna, Catania, Sicily. As a result
of observations to date, a solar burst has been isolated for later
analysis. In the near future, the device will be used for Jupiter
observations. This data will be analysed and compared to data which has
been obtained through solar observations in order to see the changes
between the two transmissions. We shall learn from this EMM-Etna field
tests to prepare the analysis of DLR-ESA ARCHES Etna 2022 tele-robotic
campaign that will deploy with rovers an array of 4 radio VLF antennas,
among a number of rover science and technical tasks. Acknowledgements:
we thank Chirayu Mohan, Kevin McGrath and Hannah Reilly for their help
setting up the device. As well as Fabian Mulder for his hospitality in
Leiden Innovation CenterPLNT & "The Field" and the EuroMoonMars
ExoMars team along with the ARCHES Etna team for providing support
in Sicily. Fig. Single dipole set-up for solar, jovian and cosmic
observations
Title: Overview of the Photo Voltaic Energy System (PVES) for the
CHILL-ICE mission
Authors: Pouwels, Charlotte; Elstgeest, Jaap; Heemskerk, Marc;
Foing, Bernard
Bibcode: 2021EPSC...15..836P
Altcode:
In the summer of 2021, the analogue astronaut mission "CHILL-ICE" shall
be carried out inside the Stefanshellir cave system. This short term
2-night emergency mission has the objective to put up an inflatable
habitat inside a Lunar-analogue Lava tube, while wearing simulated
space suits. For all extra-terrestrial missions, power is mandatory
for survival of the crew. Therefore, this is likewise introduced in the
CHILL-ICE analogue mission. A lot of devices such as; the short and long
communication system, lighting, cooking area, equipment, Lunar Zebro
rover and research projects all depend on this power system. System
requirements; For the CHILL-ICE mission, a solar power system for remote
areas has been developed by our partner Blinkinglights. The system
with acronym PVES (Photo Voltaic Energy System) needed to fulfil the
following mission requirements:8H put up/ Take down Essential for the
astronauts to stay alive. Portable for 2 persons to carry around the
selected lava tube Free standing Fidelity for an analogous mission and
no reliance on ground conditions. Peak power (Wp) of 2200W Re-deployable
Needs to be used for recurring phases of analogue missions. Easy to
handle while wearing simulated space suits. Fidelity in simulating the
usage of a power system in an emergency situation in a extra-terrestrial
environment. Weather resistant Interior needs to stay dry. The caves
on Earth can be subject to high humidity and cave rain. For this
analogue mission and the usage of PVES, the influence of gravity
and space vacuum has been neglected. In addition, PVES shall have an
automatous function to shut down when a spike in current is measured
above a certain threshold, preventing possible fires and/or harmful
situations.Furthermore, as the Stefanshellir cave system consist of a
rocky basaltic terrain, the cable going from PVES to the habitat, needs
to be able to withstand possible ruptures. PVES; The PVES (Photo Voltaic
Energy System) is designed to provide an electrical power supply for
use in a remote location where no grid-power is available. It has to be
portable and should be able to be set up with two persons in a limited
timeframe. Because of the rough terrain in Iceland care was taken,
to design a ruggedized system that should be able to withstand impact
with sharp rocks and outdoor weather conditions (complying roughly with
IP54 specifications).The system is built from different components that
can each be carried into the lava cave area by foot. These components
can then be connected together using interconnect cables with locking
connectors. Different types of connectors have been chosen to discern
between different types of electrical connections, as to prevent
accidental misconnections and reduce the risk of electrical shock to
the operator.There are four main components to the PVES (fig. 1): PV
panels (2x), SolarBox MPPT solar charge controller, PowerBox Lithium
battery + power inverter and an additional ChargerBox that can be used
to charge the battery from a regular power socket or a generator when
solar energy is insufficient. (Figure 1: Overview of the PVES and its
subsystems.)There are three different voltages present in this system:
PV output voltage (~ 30 VDC), DC battery voltage (12 VDC) and AC voltage
(230 VAC). The 12 V connections to the PowerBox are fused to protect
the wiring and connectors from overheating in case of a short or
overcurrent situation. The AC output power is automatically protected
by the inverter in the PowerBox. When excessive power is drawn (and
the inverter heats up too much) it will shut down automatically. It
will have to be reset manually after this. It is important that all
devices that will be connected to the AC output of the PowerBox are
doubly insulated (IEC 61140 Class II, indicated by the symbol ⧈ (a
square inside a square)), as there is no proper safety earthing provided
by the PVES. The system will operate in what's called an unearthed
IT AC system. Currently no provision is made to monitor insulation
resistance in accordance with IEC 61557-8 because of the short timeframe
of preparations for the CHILL-ICE mission.Care is taken to choose a
cable type that is suited for use in these rough environments. The
cable type used throughout the PVES is H07BQ-F polyurethane sheathed
cable with an orange jacket for visibility. This cable is designed to
withstand abrasion and specifically use around sharp objects. It is UV
and moisture resistant. The technical specifications of the PVES are
given in table 1 below. (Table 1: PVES technical specifications.) PVES
technical specifications Peak power (Wp) 3000 W Continues Power (Wc)
1200 W Dimension Standard Euroboxes Output 230 V Type solar cells
60 cell Poly-crystalline Battery type Lithium (LiFePo4) 2kWh stored
Expected solar yield 1 kWh/day [4] Acknowledgements;First, we would like
to thank Jaap Elstgeest from Blinkinglights for his amazing work in
researching and developing the PVES system for the CHILL-ICE mission,
during this difficult COVID period. He has been the key factor for the
success of the power system and therefore contributed significantly to
this mission.In addition, we would like to thank the whole CHILL-ICE
team for their remote support during the development of PVES.Lastly,
we acknowledge the ILEWG EuroMoonMars manager B. Foing for making this
research possible. References;[1] M.V. Heemskerk et al., EGU2020-901-1,
(2020)[2] 2021LPI....52.2762H2021/03 CHILL-ICE (Construction of a
Habitat Inside a Lunar-Analogue Lava Tube): Building and Testing of
a Deployable Habitat in Icelandic Lava Tubes for Space Exploration
Purposes Heemskerk, M. V.; Pouwels, C. R.; Heemskerk, R. S.; Kerber,
S.; Foing, B. H.[3] 2021LPI....52.2502F2021/03 Life and Research at
SouthPole Moonbase: EuroMoonMars Campaigns Results 2019-2020 Foing,
B. H.; Rogers, H.; Musilova, M.; Weert, A.; Mulder, S.; Kerber, S.;
Castro, A.; Pouwels, C.; Das Rajkakati, P.; Heemskerk, M.; et al[4]
Calculated with https://www.victronenergy.com/mppt-calculator
Title: EuroMoonMars Highlights from Terrestrial Analogues
Authors: Foing, B. H.; Stoker, C.; Rogers, H.; Musilova, M.; Weert,
A.; Mulder, S.; Kerber, S.; Castro, A.; Pouwels, C.; Das Rajkakati, P.;
Heemskerk, M.; Heemskerk, R.; Sirikan, N.; Boross, H.; Kolodziejczyk,
A.; Perrier, I. R.; Laffont, M.; Landolina, R.; Spilkin, A.; Tavernier,
A.; McGrath, K.; Reilly, H.; Mohan, C.; Brady, G.; Wedler, A.
Bibcode: 2021LPICo2595.8111F
Altcode:
We report scitech highlights from ILEWG EuroMoonMars field analogue
campaigns conducted since 2009 in ESTEC, EAC astronaut center, Utah
MDRS station, Eifel area, Rio Tinto, Iceland, La Reunion, EMMPOL Poland,
Atacama and IMA HI-SEAS Hawaii.
Title: Environmental Characterization and Development of Planetary
Science in the Puna de Atacama
Authors: Tavernier, A.; Garcia, A.; Ulloa, C.; Oses, R.; Bonnail,
E.; Santibañez, T.; McGrath, K.; Mohan, C.; Reilly, H.; Brady, G.;
Foing, B.
Bibcode: 2021LPICo2595.8124T
Altcode:
The University of Atacama and the EuroMoonMars program have started
in 2021 a joint project to characterize the environment of the Puna
de Atacama region, with the aim of developing an analog component.
Title: Hydrous Alteration of Lava Flows on Mauna Loa (Hawaii)
Compared to Martian Volcanic Soils
Authors: Weert, A. M. P.; Foing, B. H.; Mulder, S. J.
Bibcode: 2021LPICo2595.8058W
Altcode:
Comparisons between Hawaiian rocks and martian datasets show that
alteration products likely formed in a similar environment. The
comparison suggests an arid to semi-arid environment with cold to
moderate temperatures was present on an early Mars.
Title: Life & Research at Moonbase: ILEWG EuroMoonMars campaigns
results 2018-2020
Authors: Foing, Bernard; Rogers, Henk; Musilova, Michaela; Kerber,
Sabrina; Pouwels, Charlotte; Heemskerk, Marc; Sirikan, Nityaporn;
Kolodziejczyk, Agata; Perrier, Iona-Roxana; Spilkin, Amanda; Vermeulen,
Nancy; Villa-Massone, Julien; Schlacht, Irene; Waltemathe, Michael;
Hemminger, Elke; Tavernier, Adrien; The Emmihs Euromoonmars-Intl
Moonbase Alliance, Hiseas Team; The Emmpol Euromoonmars Poland Team
Bibcode: 2021EGUGA..2315626F
Altcode:
We give an update on ILEWG EuroMoonMars Results, with emphasis
on activities and field campaigns that took place in 2019-2020
including lunar astronautics events during 2020 pandemics. We
present life and research at Moonbase from EuroMoonMars campaigns
EMMIHS HISEAs, EMMPOL Poland that simulated science and operations
at future Moonbases. EuroMoonMars is an ILEWG programme following up
ICEUM declarations as a collaboration between ILEWG, space agencies,
academia, universities and research institutions and industries .EMMIHS
campaigns (EuroMoonMars-IMA International Moonbase Alliance- HiSEAS):
EuroMoonMars 2018-20 supported field campaigns at IMA HI-SEAS base on
Mauna Loa volcano in Hawaii. The International Moonbase Alliance (IMA),
an organization dedicated to building sustainable settlements on the
Moon, has been organising regular simulated missions to the Moon or
Mars at HI-SEAS. In 2019, the EuroMoonMars campaigns were launched at
HI-SEAS, bringing together researchers from the European Space Agency,
VU Amsterdam, ILEWG and IMA. Six scientists, engineers, explorers,
journalists spent two weeks at the HI-SEAS station performing research
relevant to both the Moon and Mars there. Research and technological
experiments conducted at HI-SEAS will be used to help build a
Moonbase .EuroMoonMars during 2020 Pandemics We had to replan and
adapt EuroMoonMars workshops and fields events. A number of hybrid
and virtual events could be organized following safety distancing
instructions. We conducted 35 weekly plenary EMM teleconferences
(Fridays 17h CET) and many EMM splinter groups meetings.2020/06
EMM Iceland CHILL-ICE Scouting. A small team explored locations and
collaborations for installing a deployable research habitat in lavatube
for May 2021. 2020/10 EMMPOL EuroMoonMars Poland. We were able to
organise in controlled safety conditions 2 one-week Moonbase isolation
simulations, in order to conduct a number of research investigations,
human factors studies, with 5 crew supported by a remote support
team.*Acknowledgements: We thank ILEWG EuroMoonMars field campaigns
crew 2016-2020 (including the EMMIHS crew and remote support team from
EMMIHS 1-4 and EMMPOL1 &2 .
Title: Geological context of recent Lunar landing sites using
Multispectral analysis.
Authors: Mcilquham, Jourdain; Borst, Anouk M.; Allender, Elyse J.;
Foing, Bernard
Bibcode: 2021EGUGA..2316055M
Altcode:
Geological context of recent lunar landing sites using multispectral
analysis. (Mcilquham J, Borst A, Allender E and Foing B)The Moon
Mineralogy Mapper (M3) was a guest instrument aboard the Chandrayaan-1
mission. The instrument collected spectral data, ranging from 430
nm to 3000 nm at an average resolution of 140 m/pixel. This research
utilises M3 spectral data to visualise and understand the geology of
lunar landing sites visited by Chang"e 4 and 5. The aims of this study
are aligned to lunar exploration goals produced by the National Research
Council. We use Python scripts to undertake data analysis, creating site
maps using continuum removal methods and assigning RGB image channels to
highlight absorption features of interest. The Chang"e 4 landing site
is located on the lunar far side within the Von Karman crater, located
in the large South Pole Aitken impact basin. At Von Karman lunar mantle
or lower crustal material may be exposed in the central peak. This could
provide valuable insights into lunar geological history. We create maps
to visualise the location of pyroxene end-members and olivine-rich rocks
of the Von Karman crater, adding data to understand the composition
of the deeper lunar lithologies. Orbital data presented in this study
can be compared with ground-truth data gathered from the Yutu 2 rover
to confirm the minerals present. More recently the Chang"e 5 mission
provided a further landing site for study. Using the same methods
as presented above we will compare its spectral composition to the
Chang"e 4 landing site. Our maps can help to understand the key factors
used to determine a suitable landing site and potentially a suitable
location for a lunar base. By comparing Chang"e landing sites this
study provides a unique insight into the craters in which they landed,
allowing direct comparisons to be drawn. Preliminary findings identify
non-mare units within the Von Karman crater as well as various Ca-rich
and Ca-poor pyroxene-bearing lithologies.
Title: Monitoring Temporal Developments from Remote Sensing Data
using AI Fine-Grained Segmentation
Authors: Zamarialai, Samir; Perenboom, Thijs; Kruijver, Amanda; Shi,
Zenglin; Foing, Bernard
Bibcode: 2021EGUGA..2315917Z
Altcode:
Remote sensing (RS) imagery, generated by e.g. cameras on satellites,
airplanes and drones, has been used for a variety of applications
such as environmental monitoring, detection of craters, monitoring
temporal changes on planetary surfaces.In recent years, researchers
started applying Computer Vision [TP1] methods on RS data. This led to
a steady development of remote sensing classification, providing good
results on classification and segmentation tasks on RS data. However,
there are still problems with current approaches. Firstly, the main
focus is on high-resolution RS imagery. Apart from the fact that these
data are not accessible to everyone, the models fail to generalize on
lower resolution data. Secondly, the models fail to generalize on more
fine-grained classes. For example, models tend to generalize very well
on detecting buildings in general, however they fail to distinguish
if a building belongs to a fine-grained subclass like residential or
commercial buildings. Fine-grained classes often appear very similar
to each other, therefore, models have problems to distinguish between
them. This problem occurs both in high-resolution and low-resolution
RS imagery, however the drop in accuracy is much more significant when
using lower resolution data.For these reasons, we propose a Multi-Task
Convolutional Neural Network (CNN) with three objective functions for
segmentation of RS imagery. This model should be able to generalize on
different resolutions and receive better accuracy than state-of the-art
approaches, especially on fine-grained classes.The model consists of
two main components. The first component is a CNN that transforms the
input image to a segmentation map. This module is optimized with a
pixel-wise Cross-Entropy loss function between the segmentation map of
the model and the ground truth annotations. If the input image is of
lower resolution, this segmentation map will miss out on the complete
structure of input images. The second component is another CNN to build
a high-resolution image from the low-resolution input image in order to
reconstruct fine-grained structure information. This module essentially
guides the model to learn more fine-grained feature representations. The
transformed image from this module will have much more details like
sharper edges and better color. The second CNN module is optimized with
a Mean-Squared-Error loss function between the original high-resolution
image and the transformed image. Finally, the two images created by
the model are then evaluated by a third objective function that aims to
learn the distance of similarity between the segmented input image and
the super-high resolution segmentation. The final objective function
consists of a sum of the three objectives mentioned above. After the
model is finished with training, the second module should be detached,
meaning high-resolution imagery is only needed during the training
phase.At the moment we are implementing the model. Afterwards, we will
benchmark the model against current state of the art approaches. The
status will be presented at EGU 2021.
Title: Simulating lava tube exploration research during analog lunar
and Martian missions at HI-SEAS in Hawaii
Authors: Musilova, Michaela; Foing, Bernard; Rogers, Henk
Bibcode: 2021EGUGA..2314600M
Altcode:
Lava tube exploration has become an important part of discussions
relating to the search for life on Mars by both humans and
robots. On Mars, lava tubes may contain biosignatures and existing
lifeforms. Alternatively, on the Moon, lava tubes may serve as sheltered
environments for the construction of human settlements. Nevertheless,
lava tubes can also be difficult environments for robotic operations
and they can pose a safety hazard to humans as well. It will thus
be extremely important to prepare for lava tube exploration by
humans and robots in analog environments on Earth. The Hawaii Space
Exploration Analog and Simulation (HI-SEAS) habitat is a lunar and
Martian analog research station located on the volcano Mauna Loa in
Hawaii. The International MoonBase Alliance (IMA) organises missions
at HI-SEAS, during which crews of six analog astronauts perform
research and technology testing relevant to the exploration of the
Moon and Mars. The missions that take place at HI-SEAS can be of varied
duration, from several days to several months, depending on the needs
of the researchers. They are open to space agencies, organizations
and companies worldwide to take part in, provided their research and
technology testing will help contribute to the exploration of the
Moon and Mars. Since the HI-SEAS habitat is located on lava flows,
its surroundings provide valuable access to performing high-fidelity
planetary science fieldwork with very little plant or animal life
present, and a wide variety of volcanic features to explore, such as
lava tubes, channels, and tumuli. This terrain is also ideal for rover
and in situ resource utilization (ISRU) testing because of its great
similarity to the basaltic terrains on the Moon and Mars. HI-SEAS crews
have performed a number of biochemical and geophysical research projects
in the lava tubes accessible to them near the habitat. They explored and
collected research samples while wearing Extra-vehicular Activity (EVA)
analog spacesuits and following strict EVA protocols. These activities
are very challenging for the crew, due to the bulky gloves and EVA
equipment they have to wear, while performing precise biochemical
research that is sensitive to contamination. The crews also have
to take into consideration their safety, their limited life support
systems during EVAs and a number of other factors relevant to space
exploration missions. Further studies will be needed to assess how
best to combine scientific goals with human exploration goals during
future human missions, which may use lava tubes as a resource as well
as a key site for scientific research.
Title: Machine Learning applied to Lunar Data to Characterize
Potential Sites for Future Science, Mobile Exploration, Utilization,
lunar Bases and Moon Villages.
Authors: den Heijer, Daniël; Foing, Bernard
Bibcode: 2021EGUGA..2316141D
Altcode:
The lunar south pole is of particular interest to researchers because
of its unique geographical features. It contains craters where the
near-constant sunlight does not reach the interior. These craters
are of enormous importance in the process of human exploration of the
moon.This research aims to develop an identification algorithm applied
to LROC data to characterize and identify potential regions of interest
on the lunar south pole. Such areas of interest include (surroundings
of) lava tubes, skylights, crater detection for age estimation, and
planning traverses for the Artemis successive missions.Identifying
these regions will be done using machine learning techniques such as a
deep convolutional neural network that will be trained on labeled data
and are then used to identify and characterize new regions of interest.
Title: Shape Characterization and Temporal Analysis of Exoplanet
Transits with Deep Learning
Authors: Hönes, C. J.; Heras, A. M.; Foing, B.; Rusticus, Y.; Foing,
V.; Terpstra, J. M.
Bibcode: 2021LPI....52.2071H
Altcode:
We apply Deep Learning methods to TESS light curve data to analyze the
shape of exoplanet transits. This can be used to classify different
exoplanet types or to discover new phenomena. We plan to also track
variations in the transit shape over time.
Title: Monitoring Temporal Developments from Remote Sensing Data
Using Fine-Grained Segmentation
Authors: Zamarialai, S.; Shi, Z.; Foing, B.; Perenboom, M. J. L.;
Kruijver, A.
Bibcode: 2021LPI....52.2279Z
Altcode:
Multi-Task Convolutional Neural Network (CNN) with three objective
functions for fine-grained segmentation of RS imagery into classes
which generalizes on different resolutions RS imagery.
Title: Euro-Moon-Mars Astronautics Training Academy
Authors: Vermeulen, N. M. J.; Villa-Massone, J.; Waltemathe, M.;
Hemminger, E.; Kolodziejczyk, A.; Heemskerk, M.; Kerber, S.; Foing, B.
Bibcode: 2021LPI....52.2341V
Altcode:
At the EuroMoonMars Astronautics Training Academy we train researchers
and young professionals in order to prepare them for a possible role in
the space industry. Therefore, we developed a unique training programme
based on international experience.
Title: CHILL-ICE (Construction of a Habitat Inside a Lunar-Analogue
Lava Tube): Building and Testing of a Deployable Habitat in Icelandic
Lava Tubes for Space Exploration Purposes
Authors: Heemskerk, M. V.; Pouwels, C. R.; Heemskerk, R. S.; Kerber,
S.; Foing, B. H.
Bibcode: 2021LPI....52.2762H
Altcode:
CHILL-ICE (Construction of a Habitat Inside a Lunar-Analogue Lava tube
— Iceland Campaign of EuroMoonMars) is setting up the prototype
habitat for human lunar subsurface settlement inside a lava tube
on Iceland.
Title: Cultural and Educational Aspects of Space Exploration
Authors: Waltemathe, M.; Hemminger, E.; Foing, B.
Bibcode: 2021LPI....52.2441W
Altcode:
Space-exploration relies on complex connections between different
cultures of academia, like science and humanities. An interdisciplinary
teaching program makes students stakeholders in the societal and
academic discourses on science and technology.
Title: Characterizing Exoplanet Transits and Stellar Activity in
Kepler Lightcurves with Scalable Gaussian Processes
Authors: Foing, V.; Heras, A. M.; Foing, B.
Bibcode: 2021LPI....52.1552F
Altcode:
We apply scalable Gaussian Process (GP) models to characterize exoplanet
transits and stellar activity in Kepler lightcurves. Our aim is to
retrieve accurate transit and rotation parameters, such as planet
radii and stellar rotation periods.
Title: ArtMoonMars Cultural and Artistic Activities
Authors: Foing, B. H.; Glukhova, E.; Sitnikova, A.; Mulder, F.; Ten
Helden, C.; Kuiper, M.; Vles, R.; Moon Gallery Artists; Preusterink,
J.; Kruijver, A.; Waltemathe, M.; Hemminger, E.; Perrier, I. R.;
Galluzzo, G.; Burger, T.; Prokofieva, M.; Sokolsky, D.; Sykutera, M.;
van der Linden, A.; Ben Hayoun, N.; Pell, S. J.; Hall, N.; Malina, R.;
van Gammeren, S.; Russo, P.; Almeida, P.; MoonWalk Team; Kerber, S.;
Das Rajkakati, P.; Rogers, H.; Musilova, M.; Heemskerk, M.; Ben Orin,
O.; Robberstad, J.; Global Science Opera; Verschoor, N.; Hoppe, I.;
van Winden, O.; Todays Art Festival; van den Heide, E.; Domnitch,
E.; Gelfand, D.; de Wilde, F.; Aloserij, S.; Burke, J.; Peutz, T.;
Framis, A.; MoonLife Academy; van Gronendaal, J.; Ono, A.; Schlacht, I.
Bibcode: 2021LPI....52.2595F
Altcode:
ILEWG ArtMoonMars programme of cultural and artistic activities was
started by ILEWG with ESA ESTEC and partners including IAF ITACCUS,
Global Science Opera, Todays Art, KABK, WDKA, with workshops,
residencies, projects, and MoonGallery.eu for launch.
Title: Exokite, Design of an Aerial Decision-Support Platform in a
Martian Inhabited Space Exploration Context
Authors: Tavernier, A.; Demarzo, M.; Pinto, G.; Ulloa, C.; Garcia,
A.; Foing, B. H.
Bibcode: 2021LPI....52.2278T
Altcode:
The ExoKite project aims to federate young professionals around a
multidisciplinary technical project oriented towards the design of
an aerial decision-support platform for the simulation of scientific
field campaigns in a martian analogue context.
Title: TESS Data and Ground-based Observations
Authors: Terpstra, J. M.; Foing, B. H.; Heras, A. M.; Foing, V.;
Rusticus, Y. J.; Hönes, C.; Schuring, I.
Bibcode: 2021LPI....52.2476T
Altcode:
Comparing data from space-based observatories such as TESS with data
from ground-based telescopes can lead to new conclusions. We perform
a case study on WASP-140 and AU Mic.
Title: Towards Deep Learning for Transiting Exoplanet Search Using
Simulated TESS Data
Authors: Rusticus, Y. J.; Foing, B. H.; Heras, A. M.; Foing, V.;
Hönes, C. J.; Terpstra, J. M.
Bibcode: 2021LPI....52.2080R
Altcode:
We discuss the necessity of Deep Learning methods for transit detection,
and present early results of the ongoing research to develop such
methods using simulated TESS-like light curves.
Title: Life and Research at SouthPole Moonbase: EuroMoonMars Campaigns
Results 2019-2020
Authors: Foing, B. H.; Rogers, H.; Musilova, M.; Weert, A.; Mulder, S.;
Kerber, S.; Castro, A.; Pouwels, C.; Das Rajkakati, P.; Heemskerk, M.;
Heemskerk, R.; Sirikan, N.; Boross, H.; Kolodziejczyk, A.; Perrier,
I. R.; Landolina, R.; Spilkin, A.; Preusterink, J.; Vermeulen, N.;
Villa-Massone, J.; Schlacht, I.; Glukhova, E.; Sitnikova, A.; Kuiper,
M.; Waltemathe, M.; Hemminger, E.
Bibcode: 2021LPI....52.2502F
Altcode:
We present life and research on the SouthPole Moonbase, as experienced
from EuroMoonMars campaigns EMMIHS HISEAs, EMMPOL Poland that simulated
expected science and operations at the base. We give an update on
ILEWG EuroMoonMars Results in 2019-2020.
Title: EuroMoonMars Atacama (ChileMoonMars): Prospect for the
Installation of an Analogue Martian Base in the Arid Central Andes
(Puna) and Development of Planetary Sciences in the Atacama Region
(Chile)
Authors: Tavernier, A.; Garcia, A.; Pinto, G.; Ulloa, C.; Santibañez,
T.; Nascimento, D. C.; Oses, R.; Foing, B. H.
Bibcode: 2021LPI....52.2253T
Altcode:
This abstract presents the first stages of prospective and inventory
aimed at mapping the Puna de Atacama region's potential in terms
of planetary analogues, this through an extension, in Chile, of the
EuroMoonMars programme.
Title: Preparing Future Engineers and Astronauts for Moon Exploration:
EMMPOL EuroMoonMars Poland 2020 Campaign
Authors: Perrier, I. R.; Foing, B. H.; Kołodziejczyk, A.; Komenda,
K.; Clain, M.; Forgues--Mayet, E.; Podolsky, T.; Bardin-Codine, J.;
Castaing, H.; Gouault, Q.; Spilkin, A.; Landolina, R.
Bibcode: 2021LPI....52.2562P
Altcode:
Analog missions allow us today a better understanding of the future
space exploration. During the October 2020 Moon analog EMMPOL missions,
we trained and prepared as future engineers and astronauts respecting
a strict schedule.
Title: International Moonbase Alliance campaigns at HI-SEAS -
Preparing for Future Moon & Mars Human Exploration
Authors: Musilova, Michaela; Foing, Bernard H.; Rogers, Henk
Bibcode: 2021cosp...43E.156M
Altcode:
The International MoonBase Alliance (IMA), has been organizing
regular simulated missions to the Moon and Mars at the Hawaii Space
Exploration Analog and Simulation (HI-SEAS) habitat since 2018. HI-SEAS
is a lunar and Martian analog research station located on the active
volcano Mauna Loa in Hawaii. The missions that take place at HI-SEAS
are open to space agencies, organizations and companies worldwide to
take part in, provided their research and technology testing will
help contribute to the exploration of the Moon and Mars. The crews
are supported by a Mission Control Center based on the Big Island
of Hawaii as well. A series of EuroMoonMars IMA HI-SEAS (EMMIHS)
missions have been taking place at HI-SEAS since 2019. These missions
bring together researchers from the European Space Agency (ESA),
IMA, the International Lunar Exploration Working Group (ILEWG),
European Space Research and Technology Centre (ESTEC), VU Amsterdam
and many other international organizations. Crews on these missions
perform geological, astrobiological and architectural research;
technological tests using drones, 3Dprinters and rovers; as well as
performing outreach and educational projects. The EMMIHS missions
typically last for two weeks each. During this time, the crew is
isolated within the HI-SEAS habitat, which they cannot leave without
performing EVAs (Extra-Vehicular Activities) in analog space-suits and
with the permission of Mission Control. Further support for the crew
is provided by a remote support team based at the EuroMoonMars center
at ESA/ESTEC in Noordwijk, the Netherlands. The EMMIHS campaigns aim
to increase the awareness about the research and technology testing
that can be performed in analogue environments, in order to help
humans become multiplanetary species. Furthermore, the research and
technological experiments conducted at HI-SEAS are going to be used to
help build a Moon base in Hawaii, and ultimately to create an actual
Moon base on the Moon, as part of IMA's major goals. Such technology
testing will include closed-loop systems, in situ resource utilisation,
construction of agricultural systems and other sustainable processes
at HI-SEAS. Future missions at HI-SEAS include more EMMIHS campaigns,
collaborative missions with ESA, NASA, University of Hawaii and with
companies, such as SIFT and Ketone Technologies.
Title: German Aerospace Center's advanced robotic technology for
future lunar scientific missions
Authors: Wedler, Armin; Schuster, Martin J.; Müller, Marcus G.;
Vodermayer, Bernhard; Meyer, Lukas; Giubilato, Riccardo; Vayugundla,
Mallikarjuna; Smisek, Michal; Dömel, Andreas; Steidle, Florian;
Lehner, Peter; Schröder, Susanne; Staudinger, Emanuel; Foing, Bernard;
Reill, Josef
Bibcode: 2021RSPTA.37990574W
Altcode:
The Earth's moon is currently an object of interest of many space
agencies for unmanned robotic missions within this decade. Besides
future prospects for building lunar gateways as support to human
space flight, the Moon is an attractive location for scientific
purposes. Not only will its study give insight on the foundations of
the Solar System but also its location, uncontaminated by the Earth's
ionosphere, represents a vantage point for the observation of the Sun
and planetary bodies outside the Solar System. Lunar exploration has
been traditionally conducted by means of single-agent robotic assets,
which is a limiting factor for the return of scientific missions. The
German Aerospace Center (DLR) is developing fundamental technologies
towards increased autonomy of robotic explorers to fulfil more complex
mission tasks through cooperation. This paper presents an overview of
past, present and future activities of DLR towards highly autonomous
systems for scientific missions targeting the Moon and other planetary
bodies. The heritage from the Mobile Asteroid Scout (MASCOT), developed
jointly by DLR and CNES and deployed on asteroid Ryugu on 3 October
2018 from JAXA's Hayabusa2 spacecraft, inspired the development
of novel core technologies towards higher efficiency in planetary
exploration. Together with the lessons learnt from the ROBEX project
(2012-2017), where a mobile robot autonomously deployed seismic sensors
at a Moon analogue site, this experience is shaping the future steps
towards more complex space missions. They include the development of
a mobile rover for JAXA's Martian Moons eXploration (MMX) in 2024 as
well as demonstrations of novel multi-robot technologies at a Moon
analogue site on the volcano Mt Etna in the ARCHES project. Within
ARCHES, a demonstration mission is planned from the 14 June to 10
July 2021,1 during which heterogeneous teams of robots will
autonomously conduct geological and mineralogical analysis experiments
and deploy an array of low-frequency antennas to measure Jovian and
solar bursts. This article is part of a discussion meeting issue
`Astronomy from the Moon: the next decades'.
Title: Moon Gallery: the Search for the best Visions to Start Shaping
Moon Culture
Authors: Glukhova, Elizaveta; Foing, Bernard H.; Sitnikova, Anna;
Ageli, Jamal; Das Rajkakati, Priyanka; Kuiper, Mary
Bibcode: 2021cosp...43E2184G
Altcode:
Introduction: Moon Gallery [1] is an international collaborative artwork
and a gallery of ideas worth sending to the Moon. Moon Gallery intends
to launch 100 artefacts to the Moon within the compact format of 10
x 10 x 1cm plate on a lunar lander as early as 2022. In this Petri
dish like gallery we are developing culture for future interplanetary
society. What are the ideas we want to promote into the future? What
are the ideas we want to leave behind? Moon Gallery as a pilot platform
within the framework of the Moon Village, ITACCUS & ILEWG aims to
instigate inspiration for the global space exploration and demonstrate
how the challenges along this journey drive innovative design thinking
and interdisciplinary collaborations. Art Moon Mars collective leads
this project, coordinates events and develops content through a series
of open calls. * We invite art projects and artefacts, inspired by
the Moon and human exploration. One of the biggest challenges of space
exploration is a disparity between big ideas and resources for their
realization. We ask our participants to think big but small. Each idea
has to fit within just 1 cubic cm. To answer this challenge we strongly
encourage interdisciplinary cooperation: bridging engineering, science
and art together. * The presentation at COSPAR will cover overall
Moon Gallery concept, open call and overview of submitted projects,
description of the milestones reached, results from the exhibitions
and workshops, and the next steps towards the implementation of the
actual gallery on the Moon. Mission Statement: We hope to bring the
best of humanity to the Moon, and to bring the benefits of the Moon
to all people on Earth through a sustainable exploration process. Our
initiatives connect Art, Moon, Mars and beyond. This includes the
organisation of meetings, workshops, art science space classes and
projects at various universities, sessions at international conferences,
art exhibitions, musical and visual performances, and art science
space platform - Moon gallery. * Miniature artworks - payloads will
serve as seeds of new culture, designed to inhabit and make the Moon a
more habitable place. Each piece is a part of a collaborative artwork
and an evolving shared vision of Moon Gallery: * What would be our
new values and ideals, aesthetics in space based on lessons learnt
on Earth? How for example sculpture would work in 1/6th gravity? And
how our bodies and perception of beauty will change (while our bodies
adapt to new conditions)? How would we perceive colours without the
atmosphere? Which new art forms will sprout? Relevance/significance:
-promoting cooperation: bridging innovation, science and art, crossover
with space research, developing a space art experiment; - stimulating
research: collective reflection on artistic heritage, analysis -
how to design for space (1/6th gravity, extreme environment); -
promoting artistic quality: offering artists follow up opportunities
involving space science expertise; - reinforcing international
position of artistic practice: "International cooperation towards a
world strategy for the exploration and utilization of the Moon - our
natural satellite" (International Lunar Workshop, Beatenberg (CH),
June 1994). Exemplary commissioning: follow professional process -
idea - concept - feasibility - pilot project - Earth prototype -
Moon Gallery commission for space. Acknowledgements: We acknowledge
Alexander Zaklynsky contribution to the project research, development
and production in 2018. We acknowledge Moon Gallery artists for support
in Moon Gallery events. References: [1] http://www.moongallery.eu
Title: Human habitats: prospects for infrastructure supporting
astronomy from the Moon
Authors: Heinicke, C.; Foing, B.
Bibcode: 2021RSPTA.37990568H
Altcode:
There is strong interest in lunar exploration from governmental space
agencies, private companies and the public. NASA is about to send
humans to the lunar surface again within the next few years, and ESA has
proposed the concept of the Moon Village, with the goal of a sustainable
human presence and activity on the lunar surface. Although construction
of the infrastructure for this permanent human settlement is envisaged
for the end of this decade by many, there is no definite mission plan
yet. While this may be unsatisfactory for the impatient, this fact
actually carries great potential: this is the optimal time to develop
a forward-looking science input and influence mission planning. Based
on data from recent missions (SMART-1, Kaguya, Chang'E, Chandrayaan-1
and LRO) as well as simulation campaigns (e.g. ILEWG EuroMoonMars),
we provide initial input on how astronomy could be incorporated into
a future Moon Village, and how the presence of humans (and robots)
on the Moon could help deploy and maintain astronomical hardware. This article is part of a discussion meeting issue `Astronomy from
the Moon: the next decades'.
Title: Results from the EMMIHS-1 campaign (EuroMoonMars - IMA -
HI-SEAS)
Authors: Weert, Annelotte; Foing, Bernard H.; Mulder, Sebastian;
Musilova, Michaela
Bibcode: 2021cosp...43E.157W
Altcode:
Future human space exploration of the Moon and Mars could lead to the
study of processes on the surface and subsurface of these planetary
bodies in more detail. Nowadays, analogue space missions on Earth
are used to prepare humanity for the challenges that will need to be
overcome in order to settle on the Moon or Mars. The Hawaii - Space
Exploration Analog and Simulation (HI-SEAS) habitat, is one of the
places where these types of missions are performed. The habitat is
located on the volcano Mauna Loa (Hawaii). Currently, operations of
simulated missions at HI-SEAS are coordinated by the International
MoonBase Alliance (IMA), an organization dedicated to building a
Moon base prototype in Hawaii and ultimately a real settlement on the
Moon. During the EMMIHS-1 campaign, a two week analog mission to the
Moon was performed from the 20th of February till the 6th of March
2019. EMMIHS-1 was the first of a series of analogue Moon missions
at the HI-SEAS habitat, as part of the EuroMoonMars program. Results
of the simulated missions contribute to the understanding of how to
properly build a Moon base on the lunar surface in the near future
and what research still needs to be performed in order for humans
to return to the Moon. Part of the lunar simulation was focused
on how to do geological fieldwork despite the limitations of the
analog spacesuits. This included the field research of secondary
mineralization inside lava tubes and the hydrous alteration of lava
flows. The research was conducted wearing analog spacesuits during
extra vehicular activities (EVAs) with basic geological equipment and
a drone. Infrared spectroscopy was applied on all collected samples,
as an easy and quick tool for mineral identification. Furthermore,
lab-measurements will deliver a better characterization of the
mineralogical and elemental content of the samples. Another type of
geological research that was performed during the mission was the
study of the alteration of the lava flows on Mauna Loa, which can
be used as an analogue for the hydrous alteration of basaltic rocks
on Mars. Its goal was to help understand the surface processes on
the red planet. Furthermore, the samples collected from within the
lava tubes can help determine the impact of biogeological activity
on secondary mineralization within those environments. As lava tubes
mimic subsurface conditions of other planetary bodies, the results can
be used to help find microbial extraterrestrial life on other planets.
Title: ILEWG report to COSPAR PEX Planetary Exploration Panel
Authors: Foing, Bernard H.
Bibcode: 2021cosp...43E2228F
Altcode:
The International Lunar Exploration Working Group (ILEWG) is a public
forum sponsored by the world's space agencies and stakeholders to
support "international cooperation towards a world strategy for the
exploration and utilization of the Moon - our natural satellite"
(International Lunar Workshop, Beatenberg (CH), June 1994). The Forum
is intended to serve three relevant groups:
Title: Horizon 2061: MoonVillage Perspectives for Science, Missions,
Technologies, Infrastructures and Society
Authors: Foing, Bernard H.
Bibcode: 2021cosp...43E.246F
Altcode:
We discuss MoonVillage Perspectives at Horizon 2061 addressing Science,
Missions, Technologies, Infrastructures and Society. ESA, ILEWG and
partners have been elaborating the concept of a Moon Village with
the goal of a sustainable human presence and activity on the lunar
surface as an ensemble where multiple users can carry out multiple
activities, This enterprise can federate all interested Nations
and partners. The Moon represents a prime choice for political,
programmatic, technical, scientific, operational, economical and
inspirational reasons. Why the Moon Village? The Moon Village has
the ambition to serve a number of objectives (including planetary
science, life sciences, astronomy, fundamental research, resources
utilization, human spaceflight, economic development, etc. ) to the
community and should be the catalyst of new alliances between public
and private entities including non-space industries. Additionally
the Moon Village should provide a strong inspirational, capacity
building, workforce development and education tool for the younger
generations. Previous and ongoing projects are relevant to Moon
Village. Future space exploration is building on the International
Space Station, and on the current and upcoming automatic and planetary
robotic missions. COSPAR and its ILEWG International Lunar Exploration
Working Group (created 25 years ago) have been supporting opportunities
of collaboration between lunar missions and exchange on future projects
[4-8]. A flotilla of lunar orbiters has been deployed for science
and reconnaissance in the last international lunar decade (SMART-1,
Kaguya, Chang'E1&2, Chandrayaan-1, LCROSS, LRO, GRAIL, LADEE). De
facto, collaborative opportunities and elements of a Robotic Village
on the Moon exist, as China landed in 2013 the Chang'E3 and its Yutu
rover, and ChangÉ 4 on the FarSide in 2019. Other landers are planned
(Chang'E 5, Chandrayaan-3, SLIM, Luna 25-27, CLPS, etc..). Programmes
towards humans in lunar orbit, on the lunar surface and sustainable
Moonbases are also advancing (Artemis, China, Commercial) . We discuss
also the MoonVillage in the frame of "Planetary Exploration, Horizon
2061" long-term foresight exercise initially proposed by the Air and
Space Academy and led by scientists, engineers and technology experts
heavily involved in planetary sciences and in the space exploration
of the Solar System. This exercise involved three successive steps
designed to progressively build what we called the four "pillars" of
Planetary Exploration: 1. our major scientific questions on planetary
systems; 2. the different types of space missions that we need to fly
to address these questions; 3. the key technologies we need to master
to make these missions flyable; 4. the ground-based and space-based
infrastructures needed in support to these missions. Bernard Foing
(1,2), Michel Blanc (3) , MoonVillage & ILEWG Task Groups &
Horizon 2061 Team, (1) ESA ESTEC, Noordwijk, The Netherlands; (2)
ILEWG International Lunar Exploration Working Group, (3) IRAP Toulouse
Title: ILEWG report to COSPAR: Science, Technology, human aspects,
roadmaps, socio-economics, young lunar explorers, MoonVillage,
MoonMars synergies, EuroMoonMars, ArtMoonMars
Authors: Foing, Bernard H.
Bibcode: 2021cosp...43E.159F
Altcode:
ILEWG has been organising since 1994 ICEUM International Conferences on
Exploration & Utilisation of the Moon with published proceedings,
and where community declarations have been prepared and endorsed by
community participants. ILEWG has co-organised and co-sponsored lunar
sessions at EGU, COSPAR, EPSC. ILEWG task groups include science,
technology, human aspects, socio-economics, young explorers and
outreach, programmatics, roadmaps and synergies with Mars exploration,
MoonBase, MoonVillage, EuroMoonMars, ArtMoonMars, Young Lunar Explorers,
ILEWG Young Professional Grantees. ILEWG has also sponsored a number of
activities, workshops, tasks groups and publications in collaborations
with other organisations: COSPAR, space agencies, IAA, IAF, EGU Besides
the discussion forums, users can also obtain information on how to
participate, as well as details on the latest news and events regarding
lunar exploration, forthcoming meetings, relevant reports and documents
of importance for the work of the ILEWG, summary descriptions of recent
and future lunar exploration projects (such as SMART-1, Chang'E1-5
, Selene Kaguya, Chandrayaan-1-2, LRO, LCROSS), GRAIL, ARTEMIS,
international lunar exploration projects) funded by various space
agencies, and basic data on the Moon itself. Activities of the related
space agencies and organizations can also be found. The ILEWG Forum
also hosts the Lunar Explorer's Society. http://www.lunarexplorers.net/
The International Lunar Exploration Working Group (ILEWG) is a public
forum sponsored by the world's space agencies to support "international
cooperation towards a world strategy for the exploration and utilization
of the Moon - our natural satellite" (International Lunar Workshop,
Beatenberg (CH), June 1994). The Forum is intended to serve three
relevant groups: Actual members of the ILEWG, i.e. delegates and
representatives of the participating Space Agencies and organizations -
allowing them to discuss and possibly harmonize their draft concepts and
plans in the spirit of the Beatenberg Declaration (see below). Team
members of the relevant space projects - allowing them to coordinate
their internal work according to the guidelines provided by the ILEWG
Charter (see below). Members of the general public and of the Lunar
Explorer's Society who are interested and wish to be informed on the
progress of the Moon projects and possibly contribute their own ideas.
Title: Planetary exploration, Horizon 2061- report on Pillar 4:
Infrastructures and services for planetary exploration
Authors: Foing, Bernard H.
Bibcode: 2021cosp...43E.261F
Altcode:
"Planetary Exploration, Horizon 2061" is a long-term foresight exercise
initially proposed by the Air and Space Academy and led by scientists,
engineers and technology experts heavily involved in planetary sciences
and in the space exploration of the Solar System. This exercise
involved three successive steps designed to progressively build what
we called the four "pillars" of Planetary Exploration: 1. our major
scientific questions on planetary systems; 2. the different types of
space missions that we need to fly to address these questions; 3. the
key technologies we need to master to make these missions flyable;
4. the ground-based and space-based infrastructures needed in support to
these missions. This talk will report to the COSPAR scientific assembly
delegates the main results concerning the fourth pillar, which deals
with the infrastructures and services that will be needed to fly by 2061
the set of representative planetary exploration missions identified as
components of Pillar 2. It will briefly review the following themes
of infrastructures and services for the future: A- Solar system
space weather B- Communications and navigation infrastructures C-
Overall Ground/Space infrastructures for sample collection and return,
sample analysis, contamination control, sample curation and analysis,
planetary and Earth protection. D- Future data systems: from data
collection to the scientific end-user and to the public. E- Earth-Moon
system gateways: infrastructures for access to Moon surface and to
farther destinations. F- Future Moon and Mars research outposts
Title: ILEWG EuroMoonMars Highlights 2018-2020
Authors: Foing, Bernard
Bibcode: 2020EPSC...14...14F
Altcode:
The EuroMoonMars Programme started in 2009 by ILEWG, ESA ESTEC, NASA,
VU Amsterdam and supported by various space agencies, universities and
academic or industrial partners has to bring together : space science
and astronomy, Earth and planetary sciences and biology, technology,
field work campaigns in extreme environments, resource utilisation
and economy, human factors, international cooperation. Space and
society, bridging to Arts and social sciences through the ArtMoonMars
initiative.We shall describe how EuroMoonMars can contribute to
European astronomy and space science: public and political engagement
education in areas of education, research, innovation, culture, youth
and sport policies, and industry, digital single market, space and
safety, policies .The International Lunar Exploration Working Group
(ILEWG) is a public forum sponsored by the world's space agencies
to support "international cooperation towards a world strategy for
the exploration and utilization of the Moon - our natural satellite"
(International Lunar Workshop, Beatenberg (CH), June 1994). ILEWG was
founded by several space agencies: ASA, ASI, BNSC, CNES, DARA, ESA,
ISAS, NASA, NASDA, RSA. ILEWG has been organising since 1994 the ICEUM
International Conferences on Exploration & Utilisation of the Moon
with published proceedings, and where community declarations have been
prepared and endorsed by community participants. ILEWG has co-organised
and co-sponsored lunar sessions at EGU, COSPAR, EPSC. Declarations
from ICEUM conferences cover all aspects of science, technology,
cooperation, industry, society and inspiration. ICEUM13 took place
together with COSPAR in Pasadena in 2018, and ICEUM14 with EPSC-DPS
in Geneva in 2019. Next ICEUM15 is to take place with COSPAR B/PEX
symposia (co-chairs: C. Pieters, B. Foing, G. Schmidt, C. Heinicke),
in Sydney in January 2021.ILEWG founded in 2009 the EuroMoonMars
initiative, which comprises field campaigns in Moon-Mars analogue
environments.The EuroMoonMars field campaigns have been organised
in specific locations of technical, scientific and exploration
interest. The campaigns started with EuroGeoMars2009 (Utah MDRS,
24 Jan-1 Mar 2009) with ILEWG, ESA ESTEC, NASA Ames, VU Amsterdam
and GWU and continued yearly at MDRS and other extreme field sites
on Earth.The EuroMoonMars campaigns consist of research activities
for data analysis, instruments tests and development, field tests in
Moon-Mars analogues, pilot projects, training and hands-on workshops
and outreach activities.In 2019 ILEWG contributed to IgLuna first ESA
Lab inter-University demonstrator project, hosted by the Swiss Space
Centre (SSC) with the vision to create an analogue habitat inside lunar
ice caps. The campaigns were held from 17-30 June 2019 and involved 18
student teams from 9 countries across Europe. The students developed
modular demonstrators and tested them during a field test conducted
inside the moon-like extreme environment of the Glacier Palace inside
the Zermatt Matterhorn glacier.Currently, ILEWG is collaborating
with the International Moonbase Alliance (IMA)] and the Hawaii Space
Exploration Analog and Simulation (HI-SEAS) on a series of EuroMoonMars,
IMA and HI-SEAS (EMMIHS) campaigns, at the HI-SEAS analogue facilities
in Hawaii.ArtMoonMars, Moon Village & ITACCUS (IAF ITACCUS Committee
on Socio Cultural Utilisation of Space) activities were performed,
with emphasis on events and workshops. The Moon Village is an open
concept proposed with the goal of a sustainable human and robotic
presence on the lunar surface as an ensemble where multiple users can
carry out multiple activities. We want to involve everybody including
Socio cultural and Artistic aspects. Why ArtMoonMars? Artists can
convey multiple messages of the community including planetary
science, life sciences, astronomy, fundamental research,
resources utilisation, human spaceflight, peaceful cooperation,
economical development, inspiration, training & capacity
building.Referenceshttps://en.wikipedia.org/wiki/International_Lunar_Exploration_Working_Group
Title: Towards a rules-based order for the emergence of a space
resources-based economy leading to a lunar renaissance
Authors: Beldavs, Vidvuds; Foing, Bernard; Crisafulli, Jim; O'Brien,
Dennis
Bibcode: 2020EPSC...14.1107B
Altcode:
The International Lunar Decade (ILD) is proposed as a framework for
international cooperation in lunar exploration and development from
2021-2030. ILD is inspired by the International Geophysical Year (IGY -
1957-8) when 66 countries and tens of thousands of scientists cooperated
to understand planet Earth as a whole. Satellites were launched by the
USSR. and the U.S. marking the dawn of the space age. Discovery of the
Van Allen belts and knowledge and capabilities across many fields gained
thru IGY led to the technologies that undergird the modern economy
that depend on satellites for global communications, positioning
and navigation, and Earth observation. IGY fostered international
cooperation that has enabled global challenges like climate change
to be understood and strategies framed to enable global action to
mitigate climate change and other emerging global threats.As with IGY
the ILD global initiative will be coordinated by a small secretariat
established by the UN. Countries, international organizations such
as COSPAR, NGOs, universities, cities and regions, and private firms
will propose and manage projects with knowledge coordination thru the
ILD secretariat and knowledge sharing thru numerous mechanisms many
with a legacy to IGY.In the coming decades the ILD as a framework for
development of a rules-based order can have an impact comparable to
the future creating transformational impact of IGY. A rules-based order
is necessary for sustainable development. A rules-based order enables
effective conflict resolution. Poor conflict resolution leads to the
development of weapons, fielding of militaries, hostilities and war -
the most wasteful, costly and destructive human activity.ILD is intended
to open opportunities for small and developing countries to take
part in creating the space-resources economy building upon the lunar
exploration activities initiated by the U.S. and larger spacefaring
powers including Russia, China, ESA, India, Japan, and others that
are already actively involved in lunar exploration. A rules-based
order enables shared infrastructures and international financing
mechanism that enable infrastructure financing and the cooperation
that enables knowledge sharing and that can accelerate adoption of
innovations. The ILD enables the rules-based order in outer space that
opens the possibility for sustainable development for centuries to come
while strengthening the international cooperation necessary to avert
global catastrophe in the decade ahead. ILD provides a framework to
enable a rules-based order necessary for success in meeting UN Space
2030 goals.The specific goal of ILD is to achieve sustainable presence
on the Moon by 2030. The ILD framework will enable the development of
policies for use of lunar resources as well as to govern operations
on the Moon by multiple parties. The ILD offers the opportunity to
advance a rules-based order to govern humankind"s expansion into
the Solar System to fulfill the intent of space treaties that have
been negotiated thus far thru the United Nations whose aspiration is
summarized in Article I of the Outer Space Treaty:The exploration and
use of outer space, including the moon and other celestial bodies, shall
be carried out for the benefit and in the interests of all countries,
irrespective of their degree of economic or scientific development, and
shall be the province of all mankind.The ILD is fully consistent with
and welcomes all other lunar exploration and development initiatives
including the Moon Village, the U.S. Artemis project, China's Chang'e
Project, and other initiatives. The ILD provides a framework for
cooperation that can boost and broaden all lunar exploration and
development initiatives that do not have a military orientation.
Title: International MoonBase Alliance missions at HISEAS
Authors: Musilova, Michaela; Rogers, Henk; Foing, Bernard
Bibcode: 2020EPSC...14.1035M
Altcode:
IntroductionThe Hawaii Space Exploration Analog and Simulation
(HI-SEAS) habitat is a lunar and Martian analog research station
located on the active volcano Mauna Loa in Hawaii [1]. Missions that
take place at HI-SEAS are open to space agencies, organizations and
companies worldwide to take part in, provided their research and
technology testing will help contribute to the exploration of the
Moon and Mars [Figure 1]. The International MoonBase Alliance (IMA)
has been organizing regular simulated missions to the Moon and Mars at
the HI-SEAS habitat since 2018. A series of EuroMoonMars IMA HI-SEAS
(EMMIHS) missions have been taking place at HI-SEAS since 2019. These
missions bring together researchers from the European Space Agency
(ESA), IMA, the International Lunar Exploration Working Group (ILEWG),
European Space Research and Technology Centre (ESTEC), VU Amsterdam
and many other international organizations [2,3]. The EMMIHS missions
typically last for two weeks each. During this time, the crew is
isolated within the HI-SEAS habitat, which they cannot leave without
performing EVAs (Extra-Vehicular Activities) in analog spacesuits
and with the permission of Mission Control, also based in Hawaii
[3,4,5]. A remote support team at ESTEC, the Netherlands, provides
further support for the crew. Figure 1: Analog astronauts entering a
lava tube entrance close to HI-SEAS. Research ProjectsThe surroundings
of the HI-SEAS habitat are covered in lava and they contain very
interesting geological features from a planetary science perspective,
such as lava tubes. Crews and researchers have been collaborating with
scientists at NASA Goddard, for instance, on performing biochemical
and geophysical studies on some of the lava tubes. Research at HI-SEAS
is thus focused on collecting geological and geochemical samples with
implications for astrobiology, past lunar and Martian geology, and for
habitability research purposes. The crews also perform architectural
research inside the habitat and inside lava tubes, with implications
on human psychology during long duration space missions. Furthermore,
the effects of radiation on humans and the potential of growing
food using local regolith is also studied at HI-SEAS.Technology
Field-TestingFrom a technological point of view, the crews at HI-SEAS
also test various equipment that is likely to be of great importance
to humans living on the Moon and Mars. These include different types
of rovers, drones and 3D printers. All of these technologies have
proven to be very useful and needed by the crews. Future campaigns
will be further developing tests on these devices and they will be
integrating them even more into the mission operations.Outreach &
Educational WorkMissions at HI-SEAS also aim to increase the awareness
about the research and technology testing that can be performed in
analogue environments, in order to help humans become a multiplanetary
species. Mission crews thus perform outreach and educational activities
as well. Their goal is to reach out to and inspire as many young
people as possible to be interested in STEM subjects. Some of these
projects involve installing art projects at HI-SEAS, creating videos
for school children and performing research experiments designed by
students from all around the world [Figure 2].Figure 2: IMA mission
crewmembers performing outreach activities. Future PlansThe research
and technological experiments conducted at HI-SEAS are going to be
used to help build a high fidelity Moon base simulator in Hawaii, and
ultimately to establish an actual base on the Moon, as part of IMA"s
major goals. Such technology testing will include closed-loop systems,
in situ resource utilization, construction of agricultural systems
and other sustainable processes at HI-SEAS. Furthermore, future
missions at HI-SEAS include more EMMIHS campaigns, collaborative
missions with ESA, NASA, University of Hawaii and with companies,
such as SIFT and Ketone Technologies.AcknowledgementsWe would
like to thank the crews EMMIHS-I through to EMMIHS IV (S. Mulder,
A. Weert, M. Musilova, N. Sirikan, J. Burstein, B. Pothier, S. Kerber,
A. Wanske, J. D"Angelo, A. P. Castro de Paula Nunes & C.R. Pouwels,
et al.) and the HI-SEAS Mission Control support staff (Andrew Cox, Paul
Ponthieux et al.). We would also like to thank the ILEWG EuroMoonMars
remote support team (B. Foing, J. Ageli, J. Preusterink, A. Beniest,
A. Sitnikova, M. Heemskerk, et al.).References[1] https://hi-seas.org[2]
Musilova M, Rogers H, Foing B, Sirikan N. et al. (2019), EMM IMA
HI-SEAS campaign February 2019, EPSC-DPS2019-1152[3] Sirikan, N.,
Foing, B., Musilova, M., et al. (2019). EuroMoonMars IMA HI-SEAS
2019 Campaign: An Engineering Perspective on a Moon Base, IAC, 21-25
October 2019. Washington DC, USA.[4] Musilova, Michaela, Henk Rogers,
and Bernard Foing. "Analogue research performed at the HI-SEAS research
station in Hawaii." Geophysical Research Abstracts. Vol. 21. 2019. [5]
https://moonbasealliance.com
Title: The Second EuroMoonMars IMA at HI-SEA Field Campaign: An
Overview of The EMMIHS-II Analog Mission to the Moon
Authors: Musilova, Michaela; Nunes, Ana; Kerber, Sabrina; Pouwels,
Charlotte; Wanske, Ariane; D'Angelo, Joseph; Foing, Bernard; Rogers,
Henk
Bibcode: 2020EPSC...14.1020M
Altcode:
Introduction: Simulated missions to the Moon and Mars have been taking
place at the analog research station HI-SEAS (Hawaii - Space Exploration
Analog and Simulation) since 2013. The so-called Martian and lunar
habitat, HI-SEAS, is located in Hawaii and its research projects are run
by the International Moonbase Alliance (IMA) [1]. Numerous aspects of
space missions are simulated in order to make them be as realistic as
possible, including time delays in communication, emergency procedures
and performing relevant research.In 2019, the EuroMoonMars campaign was
launched at HI-SEAS, bringing together researchers from the European
Space Agency (ESA), IMA, the International Lunar Exploration Working
Group (ILEWG), VU Amsterdam and many other international organizations
[2,3]. The campaign aims to increase awareness about the research
and technology testing that can be performed in analog environments,
in order to help humans become multi-planetary species. Furthermore,
the research and technological experiments conducted at HI-SEAS are
going to be used to help build a Moon base in Hawaii, and ultimately
to create an actual Moonbase on the Moon, as part of IMA"s primary
goals [3,4,5]. The EMMIHS II mission research: EMMIHS-II was the second
campaign organized by the EuroMoonMars group, taking place from December
8th-22nd, 2019. When the crew left the HI-SEAS habitat, they wore
analog space-suits and went through full extravehicular activity (EVA)
protocols to perform their research in the simulated lunar terrain. The
crew was supported by a Mission Control Center (MCC) based in Hawaii and
a Remote Support team based at EuroMoonMars ESA/ESTEC in the Netherlands
[2,3,4,5]. The main research themes of the EMMIHS-II campaign were
as follows:Engineering research: Crew engineers are responsible for
numerous tasks to ensure nominal operations and the maintenance of
the EVA and habitat equipment. They prepare a daily Engineering
Report for the MCC, which includes the status of the equipment,
recommendations for improvements and any requests for support. They are
also responsible for supporting other crew members" research projects
if needed. At least two crewmembers should serve as crew engineers with
strong analytical, troubleshooting and hands-on technical skills.Lava
tubes as habitats: Detailed investigations were performed of the lava
tubes in the vicinity of the HI-SEAS habitat [Figure 1]. They were
subsequently compared to lava tubes on the Moon, with the intension
of creating an environmental guideline for the architectural lunar
habitat development in lava tubes.Figure 1. EMMIHS-II crew exploring
lava tubes with drone in-field recognition.Nutrition for astronauts:
Dietary needs and the health of each crew member was monitored and the
crew followed a pre-prepared personal menu based on their intolerances
and daily activities. Various digestive problems were identified. In
order to avoid this on future missions, the dietary intake of vegetable
fiber for each individual could be estimated before the mission start
in order to adapt the fruit and vegetable rations individually. It
was found that freeze-dried food did not contribute to the emotional
well-being of the astronauts.Growing fresh food using analog lunar soil:
The fast-growing garden cress was sown in analog lunar soil collected by
the HI-SEAS habitat. Coarse soil mixed with a small amount of compost is
sufficient for germination and plant growth in the first stage of plant
development. In the future, such crops could be grown more extensively
in greenhouses on Mars or the Moon as sources of nutrients and oxygen
for the crew, as well as to reduce compost and fertilizer payloads.3D
additive manufacturing: Dual extrusion 3D printing technologies were
used to assess how additive manufacturing can improve livability in a
space habitat. For instance, personal items for the analog astronauts"
leisure time activities and engineering tools were printed. Their
effects on the crew were evaluated in a comparative survey.Privacy
and color during space missions: Comparative daily surveys were
undertaken by the crew to evaluate the effects of different types of
privacy and color deprivation situations. The findings will serve as
a basis for future architectural design concepts in extra-terrestrial
habitats.Emergency medical simulation: A casualty evacuation (CASEVAC)
exercise was performed to execute a mock injury while 1) maintaining
simulation conditions as if on an EVA, or 2) "breaking simulation" to
allow the crew to train for a real world situation. The in-simulation
injury scenario was executed in the spirit of a robust approach to
understanding the unexpected problems which may arise during space
exploration [Figure 2]. Figure 2. EMMIHS-II crewmembers are performing
a CASEVAC (Casualty Evacuation) drill during an EVA.Outreach: Outreach
and educational activities were performed in order to reach out to
and inspire as many young people as possible to be interested in STEM
subjects. Some of these projects involved installing a Moon gallery
at the HI-SEAS habitat, creating videos for school children during the
missions, and performing research experiments designed by students all
around the world. Future plans: Future missions at HI-SEAS include more
EuroMoonMars IMA HI-SEAS (EMMIHS) missions, collaborative missions with
ESA, NASA, universities worldwide and with companies. These missions
will continue to contribute to the development of technologies
to lay a foundation for creating a sustainable settlement on the
Moon. Acknowledgments: First, we would like to thank the EMMIHS II crew
(M. Musilova, S Kerber, A Wanske, J D"Angelo, A P Castro de Paula Nunes,
C R Pouwels), the Mission Control from HI-SEAS (Andrew Cox et al.),
ILEWG"s EuroMoonMars Manager B. Foing, and the Remote Control team
(A. Jageli, J. Preusterink, A. Beniest, A. Sitnikova, et al.). We
would also like to thank our sponsors and their generous support: Ruag
Space, Capable BV, Kurtz Ersa, dB Matik AG, Tridonic GmbH CoKG, and
the Brazilian Space Agency (AEB)References:[1] https://hi-seas.org[2]
Musilova M, Rogers H, Foing B, Sirikan N. et al. (2019), EMM IMA
HI-SEAS campaign February 2019, EPSC-DPS2019-1152[3] Sirikan, N.,
Foing, B., Musilova, M., et al. (2019). EuroMoonMars IMA HI-SEAS
2019 Campaign: An Engineering Perspective on a Moon Base, IAC, 21-25
October 2019. Washington DC, USA.[4] Musilova, Michaela, Henk Rogers,
and Bernard Foing. "Analogue research performed at the HI-SEAS research
station in Hawaii." Geophysical Research Abstracts. Vol. 21. 2019. [5]
https://moonbasealliance.com/
Title: CHILL-ICE: Construction of a Habitat Inside a Lunar-analogue
Lava-tube: Iceland Campaign of EuroMoonMars
Authors: Heemskerk, Marc; Pouwels, Charlotte; Kerber, Sabrina; Downes,
Eibhlin; Heemskerk, Robert; Foing, Bernard
Bibcode: 2020EPSC...14..901H
Altcode:
In May 2021, a group of students and young professionals from
EuroMoonMars will construct a lunar-analogue habitat inside a lava tube
in Iceland, known as CHILL-ICE.As a preparation for semi-permanent
humanned missions to the lunar surface, analogue field tests on
Earth will greatly improve the chance of a mission success. Looking
at prospective habitat locations in or on the lunar surface, lava
tubes may present an excellent opportunity in terms of safety
and efficiency. These locally occurring features provide a rigid
structure with a solid ground, and therefore offer protection from
radiation, temperature variations, regolith, and micrometeorite impacts
[1]. Furthermore, the unaltered rocks and minerals inside lunar lava
tube systems will grant a unique insight into the origin of the Moon,
and with that, the Earth [2].Lava TubesLava tubes on Earth are most
commonly found in areas with deep-mantle volcanic activity, such as
"hot spots": places where mantle plumes arrive at the surface (Hawaii,
Iceland, Canary Islands). Geochemically speaking, the basaltic rocks
present at these locations on Earth are quite comparable to their lunar
counterparts in major element compositions. As most of the larger lava
tubes on Earth are located on oceanic islands, they are highly suited to
explore the psychological factors of being remotely distanced from the
rest of the Earth. Colder regions, such as on Iceland or at the high
peaks of Mauna Loa on Hawaii, are preferred for analogue habitats due
to less biochemical weathering of the environment. The high latitude
of Iceland further aids the lunar-day simulation aspect of an analogue
habitat, as there can be over 20 hours of sunlight in the summer, and
only 4 hours of sunlight in the winter. The EuroMoonMars and future
EXTAR teams are therefore planning to set up a lunar-analogue habitat
inside a lava tube on Iceland. Earlier campaignsIn September 2018,
a reconnaissance campaign was organized to scout multiple lava fields
across Iceland for their suitability to host a lunar analog habitat
[3]. The most promising site found was the Surtshellir-Stefanshellir
cave system in the Hallmundarhraun lava flow in the Western part of
Iceland, see Figure 1. At the easternmost part of the Stefanshellir
lava tube, there is a large open gallery with a relatively flat surface
within the tube. This would be an optimal location for the construction
of a lava tube habitat.Figure 1: Location of the Stefanshellir cave
system. Top left image shows the location in Iceland, top right shows
the Hallmundarhraun lava field (in light yellow). Bottom right shows
an overlay of the Stefanshellir cave system as drawn by J.R. Reich
jr., in 1975, over aerial footage. Upcoming scout missionThis year a
follow-up scout mission to the lava tube systems of Hallmundarhraun
is planned for the 28th of June until the 4th of July 2020. The main
goal is to investigate the lava tube and its direct surroundings into a
much greater detail. Inside Stefanshellir, the aim is to make at least
two 180-degree 3D movies for a virtual walkthrough tour, take precise
measurements of the dimensions of the gallery, and 360 degrees pictures
for a model. On the surface, the focus lies on making aerial maps to
scout for visible signs of the subsurface lava tubes [4] and setting up
communications and solar observational antennae.Besides investigations
regarding the lunar analog mission, geological fieldwork to the lava
field will be performed to create a clearer reconstruction between
Stefanshellir and other lava tubes within Hallmundarhraun. Directly
located to the east of Stefanshellir, lies Surtshellir, a maze-like
cave that is unlikely to have formed in one event. Another lava tube
is located directly to the west, called Hulduhellir, or "secret cave"
[5], as it has no openings to the surface and is known only through
ground penetrating radar and magnetometric studies. There are in total
another seven lava tubes in the lava flow confirmed and discovered thus
far, but it is likely that there are other, still pristine and unopened
lava tubes yet to be found. Simulation missionThe final lunar analog
habitat will be constructed end of May 2021. Besides earlier campaign
objectives, the simulation mission will focus on the feasibility of
setting up a lunar tube habitat in-sim. This means that the habitat
should be deployable by four astronauts in a tight and possibly dark
environment within ten hours. Other instruments will be deployed out
of simulation, this would compare to the deployment of instruments
via robotic missions in earlier stages of lunar habitation. Figure 2
provides a rough overview sketch of some crucial instruments used in
the simulation mission.Figure 2: Rough sketch of the planned base for
the CHILL-ICE campaign in May 2021. The subsurface habitat"s shape
is still to be determined and will not (yet) include any large life
support systems, such as greenhouses or water replenishment systems. On
the surface, several instruments will be deployed out-of-simulation;
comparable to robotic deployment in lunar missions. Even with a
lightweight, partially inflatable, habitat, this is expected to take
up the largest part of the first mission. From the ten days set out for
the campaign, only two and a half day will be spent in simulation; the
rest of time will be to conduct further research to the terrain and its
origin, other ISRU objectives, drone mapping, communication protocols,
solar observations, (aerial) gravimetric, LIDAR, and magnetometric
studies, and of course training in setting up the habitat locally in
an efficient and safe manner.We would like to thank Space Iceland,
4th Planet Logistics, Prof. Bernard Foing, EuroMoonMars, and ILEWG
for their great support during our campaign.[1] M.V. Heemskerk et al.,
LPSC50, #1693, (2019)[2] C.L. York et al., LPI Joint Workshop on New
Technologies for Lunar Resource Assessment, (1992)[3] M.V. Heemskerk et
al., EGU2019-17503-1, (2019)[4] P. Lee et al., LPSC50, #3118, (2019)[5]
C. Wood et al., Expedition Report Hallmundarhraun 2003 Iceland, (2004)
Title: Moon Gallery Garden: Moon Gallery update 2020
Authors: Glukhova, Elizaveta; Sitnikova, Anna; Foing, Bernard; Ageli,
Jamal; Kuiper, Mary
Bibcode: 2020EPSC...14..703G
Altcode:
Moon Gallery GardenWe will give a report on Moon Gallery Garden
exhibition 6 June to 12 July, 2020, Amsterdam and give an update on
recent Moon Gallery activities and steps towards the implementation
of establishing the first gallery of art, artefacts and science
on the Moon. A lunar lander with rovers and telescopes settled at
Zone2Source in the Glass House, Amsterdam along with a selection of
artworks and prototypes designed to be sent to the Moon by the end
of the year 2022. The exhibition also included astronaut performances
while wearing spacesuits to ensure safety and avoid contamination.About
Moon Gallery:Moon Gallery aims to set up the first permanent gallery
on the Moon. Moon Gallery intends to launch 100 artefacts to the Moon
within the compact format of 10 x 10 x 1cm plate on a lunar lander
exterior panelling as early as 2022. In this Petri-dish-like gallery,
we are developing a culture for future interplanetary society. What
are the ideas we want to promote into the future? What are the ideas
we want to leave behind? Moon Gallery as a pilot platform within the
framework of the Moon Village, ITACCUS & ILEWG aims to instigate
inspiration for the global space exploration and demonstrate how
the challenges along this journey drive innovative design thinking
and interdisciplinary collaborations. ILEWG Art Moon Mars collective
leads this project, coordinates events and develops content through
a series of open calls. Relevance/Significance: Size is one of the
biggest challenges of space exploration and the disparity between big
ideas and resources for their realisation often stands in the way of
many experiments. We ask our participants to think big but small -
each idea has to fit within just 1 cubic cm. Creativity is defined
as the production of ideas or solutions that are novel and useful
(Amabile,1988, 1996). Constraints can give creativity a purpose, a
perspective, a starting point. Constraints make us feel challenged
and in particular, this statement is accurate for the subject of
space. The most challenging and full of constraints environment -
Moon - should bring us to the most creative culture and society we
believe. At the moment the human presence beyond the Earth is only a
matter of survival, but how to make the first step towards making it
habitable? We suggest bringing this collection of ideas as the seeds of
a new culture. We believe that culture makes a distinction between mere
survival and life. Moon Gallery is a symbolic gesture that has a real
influence - a way to reboot culture, rethink our values for better
living on Earth planet.Moon Gallery is a Manifestation. Neither a
place nor an object. Paradoxically a tiny gallery too small for Earth
is designed to last on the Moon as a monumental heritage site for
thousands of years. Building an everlasting monument, say a pyramid on
Earth took a joint effort of a great nation, launching a rocket takes
a multinational effort.Mission Statement: We hope to bring the best of
humanity to the Moon and to bring the benefits of the Moon to all people
on Earth through a sustainable exploration process. Our initiatives
connect Art, Moon, Mars and beyond. This includes the organisation of
meetings, workshops, art-science-space classes and projects at various
universities, sessions at international conferences, art exhibitions,
musical and visual performances, and art-science-space platform - Moon
Gallery Foundation.Moon Gallery Objectives: - promoting cooperation:
bridging innovation, science and art, crossover with space research,
developing a space art experiment;- stimulating research: a collective
reflection on artistic heritage, analysis - how to design for space
(1/6th gravity, extreme environment);- promoting artistic quality:
offering artists follow up opportunities involving space science
expertise;- reinforcing international position of artistic practice:
"International cooperation towards a world strategy for the exploration
and utilization of the Moon - our natural satellite" (International
Lunar Workshop, Beatenberg (CH), June 1994).Acknowledgements: We
acknowledge Hans Broymans and Alice Smits (Zone2Source) for the support
of the Moon Gallery Garden in 2020; Moon Gallery Garden Participating
artists: Eva Petric, Aneta Zeleznikova, Lakshmi Mohanbabu, Jamal Ageli,
Ronald Vles, Ilaria Cinelli, Isabella Douzoglou, Eduardo Kac, Mai Wada,
Andy Gracie, Oded Ben-Horin, Priyanka Das Rajkakati, Hady Milani,
Sophie Hooghiemstra, Max Baraitser Smith, Sofia Chin, Zuza Banasinska,
Renato Japi, Tobias Schalm & Alban Muret, Minna Philips, Maria
Polushkina, Johan Recen Larsson, Hans Brooymans, Mary Kuiper, Alexandra
Arshanskaya, Badriah Hamelink, Thomas Heidtmann, Anastasia Izotova,
Jorick De Quaasteniet, Arina Livadari, Daria Kozhina, Daria Akhrameika,
Maria Beaumaster & Sarah Bovelett, Studio Samira Boon, Dana Lamonda,
Mark IJzerman, Martin Sjardijn, Guy Livingston, Alexandra Ljadova, Lisa
Van Casand, Studio Furthermore, Gabriele Lorusso, Emmanuele Villani. We
thank Cesare Barbieri for hosting Moon Gallery lecture at Rotary Club,
Università di Padova; EuroMoonMars analog astronauts and colleagues who
deployed and tested the gallery prototype at various analogue campaigns:
EMMIHS Hawaii, Igluna Zermatt and EMM Iceland. We thank ILEWG and IAF
ITACCUS for endorsing the project. We acknowledge Alexander Zaklynsky
contribution to the project in 2018.
Title: EMMIHS-2 Analog Moonbase Viewpoint And Results - An Engineering
Outlook at the Second Euro-MoonMars IMA HI-SEAS 2019 Campaign
Authors: Castro Nunes, Ana; Musilova, Micaella; Kerber, Sabrina;
Pouwels, Charlotte; Wanske, Ariane; D'Angelo, Josep; Foing, Bernard;
Rogers, Henk
Bibcode: 2020EPSC...14.1110C
Altcode:
Introduction: The EuroMoonMars IMA HI-SEAS 2019 campaigns (EMMIHS) are
field research campaigns, an initiative directed by the International
Lunar Exploration Working Group (ILEWG) of the European Space Agency
(ESA) in collaboration with the International MoonBase Alliance
(IMA). The purpose of these campaigns is to conduct scientific
experiments and test technological instruments relevant to space
exploration and extraterrestrial habitation. The team for the second
edition of this campaign consisted of six crewmembers, based at the
Hawaii Space Exploration Analog and Simulation (HI-SEAS) [1] habitat
with support from the Mission Control Centre (MCC), based at the Blue
Planet Research Lab in Hawaii, and remote support based at EuroMoonMars
ESA/ESTEC in Noordwijk, the Netherlands.In 2019, the EuroMoonMars
campaign was launched at HI-SEAS, bringing together researchers from the
European Space Agency (ESA), IMA, the International Lunar Exploration
Working Group (ILEWG), European Space Research and Technology Centre
(ESTEC), VU Amsterdam and many other international organizations
[2,3]. These campaigns aim to increase awareness about the research
and technology testing that can be performed in analog environments
in order to help humans become multi-planetary species.Furthermore,
the research and technological experiments conducted at HI-SEAS are
going to be used to help build a Moon base in Hawai"i, and ultimately
to create an actual Moonbase on the Moon, as part of IMA"s primary
goals [6].This paper will deliver details of the research projects
conducted and an overview of the crew engineer"s routine. The paper
will also present the challenges and outcomes of the mission and its
activities from an engineering perspective. Fig. 1 HI-SEAS habitat
view. The picture was taken during an EVA using a drone. The Role of
The Crew Engineer: It was established, based on the feedback from
previous analog missions, that at least one crewmember serving as
an engineer with strong analytical, troubleshooting, and hands-on
technical skills is vital for the mission"s success. The engineer"s
tasks include successfully performing technological research using
a drone; the assembly of a small rover to be operated remotely by
remote control; HI-SEAS habitat operations and maintenance; network
communication systems and data exchange between the "Moon" and
"Earth."The crew engineer (CE) is responsible for ensuring nominal
operations and the maintenance of the EVA (extra-vehicular activity
- any activity performed outside the habitat while wearing analog
spacesuits) equipment like EVA spacesuits, life support systems, the
communication network, and devices). The engineer is also responsible
for the habitat equipment (power systems, solar panels, inverters,
batteries, generators, weather stations, surveillance systems, heating
systems, and network communication systems).The CE is also in charge
of checking the status of the EVA equipment before and after each EVA,
as well as gathering feedback from the EVA team. A daily Engineering
Report is prepared and provided to the MCC with a summary of engineering
specific activities, the status of the equipment, recommendations
for improvements, and any requests for further support from the MCC
Engineering Support Team. The CE is also in charge of supporting
other crew members" research projects if needed. Fig. 2 HI-SEAS
control panel. Fig. 3- EVA Equipment and maintenance With various
responsibilities, the CE is vital to ensuring the mission"s safety
and projects to be performed with success. Crew Engineers should be
prepared not only to operate and maintain the habitat but also to deal
with any challenges that might arise from experiments and from living
in a Moonbase analog. After the two EMMIHS campaigns, recommendations
were provided to ensure the success of future missions and guidelines
for other upcoming analog campaigns. Future plans: Future missions
at HI-SEAS include more EuroMoonMars IMA HI-SEAS (EMMIHS) missions,
collaborative missions with ESA, NASA, universities worldwide, and with
companies, such as SIFT and Ketone Technologies. These missions will
continue to contribute to the development and testing of technologies
and sustainable processes to lay a foundattion for creating the first
long-term settlement on the Moon. Acknowledgments: First, we would
like to thank the EMMIHS II crew (M. Musilova, S Kerber, A Wanske, J
D"Angelo, A P Castro de Paula Nunes, C R Pouwels), the Mission Control
from HI-SEAS (Andrew Cox et al.), ILEWG"s EuroMoonMars Manager B. Foing,
the Remote Support team (A. Jageli, J. Preusterink, A. Beniest,
A. Sitnikova, et al.), and A. Jageli for remote support operations of
the rover.We would also like to thank the EMMIHS II sponsors for their
generous support: Ruag Space, Capable BV, Kurtz Ersa, dB Matik AG,
Tridonic GmbH CoKG, and the Brazilian Space Agency (AEB).References:[1]
Hawaii Space Exploration Analog and Simulation, https://hi-seas.org[2]
Musilova M, Rogers H, Foing B, Sirikan N. et al. (2019), EMM IMA
HI-SEAS campaign February 2019, EPSC-DPS2019-1152[3] Foing, B. H.;
EuroMoonMars 2018-2019 Team, EuroMoonMars Instruments, Research,
Field Campaigns, and Activities 2017-2019; 2019LPI....50.3090[4]
Sirikan, N., Foing, B., Musilova, M., Weert, A., M. Mulder, A.,
Pothier, B., Burstein, J., & Rogers, H. (2019). EuroMoonMars IMA
HI-SEAS 2019 Campaign: An Engineering Perspective on a Moon Base, the
International Astronautical Congress, 21-25 October 2019. Washington
DC, United States.[5] Musilova, Michaela, Henk Rogers, and Bernard
Foing. "Analogue research performed at the HI-SEAS research station
in Hawaii." Geophysical Research Abstracts. Vol. 21. 2019. [6]
International MoonBase Alliance, https://moonbasealliance.com/
Title: How to Build Moon Bases
Authors: Rogers, Henk; Musilova, Michaela; Romo, Rodrigo; Ponthieux,
Vincent Paul; Foing, Bernard
Bibcode: 2020EPSC...14.1026R
Altcode:
The time for humans to return to the Moon is upon us. This time we
will not just go to the moon to collect some rocks and to leave only
footprints. This time we will build permanent settlements and colonize
the Moon. Our plan is to enable the building of international Moon
settlements. There are numerous space agencies, companies and research
institutions working on building rockets that will carry payload to
the moon but what we do when we get there has mainly been focused on
small scale rover based exploration. It is high time we started the
work of designing and building human lunar settlements. The idea is to
gather all of the space agencies, companies and research institutions
to work in one place where they can combine forces and robotically
build prototype Moon structures and landing pads on Earth, with the
goal of creating robots that will be sent to the Moon to create
human settlements. The group of participants who will carry out
the Research & Development is called the IMA (the International
MoonBase Alliance). Accomplishments to date: HI-SEAS (the Hawai"i -
Space Exploration Analog and Simulation): We held five long duration
Mars missions with NASA and the University of Hawaii in a habitat we
designed and built on Mauna Loa, an active volcano and the biggest
mountain in the world (by volume) on the Big Island of Hawaii. Each
mission comprised of 6 crew staying in a 110 sq m (1,200" sq. ft.) dome
to test crew selection and crew psychology (Figure 1). If during the
mission crew members left the habitat, that was considered an "Extra
Vehicular Activity" (EVA). EVAs were conducted according to strict EVA
rules with crew wearing analog spacesuits. All communications from the
habitat to the rest of the world were delayed 20 minutes each way to
simulate the lag in communicating with Mars. The missions varied between
4 to 12 months in length. Figure 1: The HI-SEAS habitat. In the last few
years, we have pivoted from NASA Mars missions to IMA Moon missions,
which are shorter in duration (from weeks or days). These missions
are more about giving a larger group of people practical "off-world"
experience and about testing research experiments and technologies
needed to build a lunar settlement (Figure 2). We have built a
"Mission Control" facility. We are testing new and much improved
EVA suits equipped with 3D cameras and head-up displays to better
communicate with Mission Control. Figure 2: HI-SEAS lunar mission
crewmembers performing an EVA in a lava tube. PISCES (the Pacific
International Space Center for Exploration Systems): PISCES is a
State of Hawaii R&D group. We have worked with NASA to sinter
powdered Hawaii lava rock (96% the same chemistry as lunar regolith)
into building materials stronger than specialty concrete. We created
"pavers" which we deployed into a landing pad using a rover and tested
it with a mounted rocket engine (Figures 3 & 4). Rodrigo Romo
who heads up PISCES, spent 6 months in Biosphere 2 giving us a wealth
of information about sealed self-sustaining environments. Figure 3:
PISCES rover testing. Figure 4: PISCES rocket engine test. IMS (the
International MoonBase Summit): We held the first IMS in October of
2017. 100 scientists, engineers, designers, economists, legislators,
astronauts and students, gathered in Hawaii to brainstorm the first
permanent lunar settlement. Out of this gathering was created the
IMA. We published our findings in a book called "Mahina", the word for
Moon in Hawaiian. It is our plan to build a first Moon Settlement and
call it "Mahina Lani" or "Moon Heaven". The plan going forward: IMA
(the International MoonBase Alliance): The IMA plan calls for a 1,000
acre "lunar landscape" campus on which we will build lunar structure
prototypes. We are now in phase one on a much smaller scale. We are
building a sealed windowless 12 meter (40") diameter dome with an
airlock. Our plan is to build it out of layers of "radiation proof"
cement and use spherical projection systems to simulate windows and
other desirable features. We plan to conduct a series of experiments
with different internal configurations to simulate crew quarters,
mission control, engineering bays, food growing facilities, meeting
rooms, common areas, mess halls, recycling centers and entertainment
spaces. The IMA vision is to send robots to the Moon that will 3D print
structures that will be occupied by humans when the time comes. The
focus will be on using ISRU (In Situ Resource Utilization) to build
self sustaining lunar settlements (Space Ports). The oceanic rock
of Hawaii ideal because it is the closest simile to lunar regolith
that's we can find on Earth. Hawaii is also a melting pot of Asian and
American cultures, so it"s the perfect place for cooperation by and
between American and Asian space settlement efforts. Let"s all work
together and build a permanent lunar settlement, a MoonBase, by the
end of this decade, "not because it"s easy, but because it"s hard"
(quote by John F. Kennedy).
Title: Combining Kepler, TESS and ground based data for characterising
exoplanets and stellar activity
Authors: Foing, Victoria; Heras, Ana; Foing, Bernard
Bibcode: 2020EPSC...14.1097F
Altcode:
This work compares the information obtained from TESS and Kepler
lightcurves, and integrates information obtained from ground based
observatories. We apply Machine learning methods for modelling
stellar and instrumental systematics in lightcurves because they
can quickly identify patterns in data without prior knowledge of
the functional form. We use a Gaussian Process to model the stellar
activity, background granulation, and transit signals simultaneously
because we expect that using a multi-component model can improve
planetary characterisation. This work seeks to address the following
questions:RQ1: How accurately can we model the stellar activity
and transit signals in TESS and Kepler lightcurves with machine
learning?RQ2: To what extent can we use these models to interpret the
rotation periods and activity cycles of the stars?RQ3: To what extent
can we use these models to detrend the lightcurves and improve transit
exoplanet characterization?The model is initialized using information
from Box Least Squares, LombScargle analysis, and Autocorrelation
functions, and then Markov Chain Monte Carlo algorithms are run to fit
rotational modulation parameters and planet parameters. We compare the
results of this method across different missions (TESS and Kepler) and
compare the results of this method with results obtained from ground
based surveys. We illustrate the comparison and the astrophysical
results in the case of WASP62 and Kepler 78 targets.
Title: Radio Astronomy from a Lunar Environment Precursor Tests
Authors: Laffan Downes, Eibhlin; Foing, Bernard
Bibcode: 2020EPSC...14..799L
Altcode:
Performing radio astronomy observations from the Earth"s surface
is plagued with interference issues. The Earth and its surrounding
atmosphere, particularly our ionosphere, are massive sources of natural
interference. There are also human sources of interference. There
have been several studies attempting to solve the issues surrounding
radio observations. One such solution is to find radio-quiet zones,
such as the far side of the Moon. In his article "Farside explorer:
unique science from a mission to the farside of the moon" David Mimoun
states that the Moon is "the most radio-quiet environment in near-Earth
space." [1] The far side of the Moon is insulated from Earth's various
interference sources. This certainly makes it a great candidate for
radio astronomy. [2][3] Due to the rotation and orbiting speed of the
Moon, the same side of the Moon is always facing Earth. However, the
building of a radio antenna array on the Moon and operating it would be
costly. Therefore, tests must be prepared on Earth in advance. These
tests are performed with the EuroMoonMars project. Using the Radio
Jove receiver with dipole antennae, Solar and Jovian observations
will be performed. These observations can be compared with data from
other radio telescopes and arrays. This would allow radio astronomy
to be tested both as a concept and as a prediction tool for solar
weather. Even though the Earth is protected by our atmosphere,
the Earth is affected by solar weather. [4] The near side of the
Moon will be affected by solar weather and this could be predicted
and diagnosed by radio instruments. During the COVID-19 pandemic and
lockdown, observations have been carried out in Bray, Ireland and at
The European Space Technology and Research Centre (ESTEC) and Leiden in
the Netherlands. These locations are all at similar latitudes. Further
observations are planned in Iceland. The EuroMoonMars is launching the
CHILL-ICE campaign in 2021 and radio observations will be an integral
research topic. Experiments will be carried out to determine the angular
response and efficiency of the apparatus in a volcanic region. The rest
of the EuroMoonMars CHILL-ICE team deserve thanks for their support of
these experiments. The Earth-based apparatus contains a single dipole,
the Radio Jove receiver and a laptop to receiver processed data. The
experimental methods can be defined as follows: Graph 1: Data
recorded in Radio Skypipe software, taken on the 15th June 2020,
during reported solar prominences. References:
Title: EuroMoonMars programme & field campaigns
Authors: Foing, Bernard
Bibcode: 2020EGUGA..2220691F
Altcode:
EuroMoonMars is an ILEWG programme following up ICEUM declarations as a
collaboration between ILEWG, space agencies, academia, universities and
research institutions and industries. The ILEWG EuroMoonMars programme
includes research activities for data analysis, instruments tests and
development, field tests in MoonMars analogue, pilot projects, training
and hands-on workshops, and outreach activities. EuroMoonMars includes
a programme of grants for Young Professional Researchers. EuroMoonMars
field campaigns have been organised in specific locations of technical,
scientific and exploration interest. Field tests have been conducted
in ESTEC, EAC, at Utah MDRS station, Eifel, Rio Tinto, Iceland, La
Reunion, LunAres base at Pila Poland, and HiSEas base in Hawaii. These
were organised by ILEWG in partnership with ESTEC, VU Amsterdam,
NASA Ames, GWU in Utah MDRS (EuroGeoMars 2009, and then yearly for
EuroMoonMars 2010-2013). Other EuroMoonMars analogue field campaigns
using selected instruments from ExoGeoLab suite were conducted in
other MoonMars extreme analogues such as Eifel volcano, Rio Tinto,
Iceland, La Reunion, Hawaii. EuroMoonMars field campaigns started with
EuroGeoMars2009 (Utah MDRS, 24 Jan-1 Mar 2009) with ILEWG, ESA ESTEC,
NASA Ames, VU Amsterdam, GWU and continued with yearly EuroMoonMars
Field campaigns in Utah (2010-2014), and in other Moon-Mars terrestrial
analogues (Eifel volcanic area, Rio Tinto, Iceland, La Reunion,
LunAres base in Poland, and HiSEAS base in Hawaii ). EMMIHS campaigns
(EuroMoonMars-IMA International Moonbase Alliance- HiSEAS): EuroMoonMars
2018-19 supported field campaigns at IMA HISEAS base on Mauna Loa
volcano in Hawaii . The Hawaii - Space Exploration Analog and Simulation
(HI-SEAS) habitat is located at 8,200' (2,500 meters) in elevation
on the largest mountain in the world, Mauna Loa, on the Big Island
of Hawai'i. As of 2018, the International Moonbase Alliance (IMA), an
organization dedicated to building sustainable settlements on the Moon,
has been organising regular simulated missions to the Moon, Mars or
other planetary bodies at HI-SEAS. In 2019, the EuroMoonMars campaigns
were launched at HI-SEAS. Six scientists, engineers, journalists and
photographers spent two weeks at the HI-SEAS station performing research
relevant to both the Moon and Mars there. Furthermore, the research and
technological experiments conducted at HI-SEAS are going to be used to
help build a Moonbase in Hawai'i, and ultimately to create an actual
Moonbase on the Moon, as part of IMA's major goals. The campaigns were
remote;y supported from Blue Planet Lab (; support@ BluePlanet/IMA:
Ponthieux, Cox, Rogers, Foing et al ) & ESTEC/ILEWG/VU Amsterdam
(Ageli, Foing, Beniest, Sitnikova, Preusterink et al ) and had analog
astronaut crew: 2018 EMMIHS0 EMM-IMA-HISEAS scouting campaign May 2018 (
Crew: Rogers H&A, Foing, Wilhite, Machida); 2019 EMMIHS1 February
(crew: Musilova, Sirikan, Mulder, Weert, Burstein, Pothier); 2019
EMMIHS2 8-22 December in Moonbase, (crew: Musilova, Kerber, Castro,
Wanske, Pouwels, d'Angelo); 2020 EMMIHS3 18 Jan- 1 Feb in Moonbase,
(crew: Heemskerk M&H, Rajkakati, Musilova, Brasileiro, Edison);
2020 EMMIHS4 1-15 Feb in MoonbaseEMMIHS0, (crew: Boross, Musilova,
Neidlinger, Pantazidis, Sheini) . Other EuroMoonMars 2020 campaigns are
planned in ESTEC, Lunares Poland, Iceland, Etna (ARCHES with DLR/ESA)
& IMA HISEAS.
Title: Lunar and Mars analogue research performed at the HI-SEAS
research station in Hawaii, part of the EuroMoonMars - IMA -
HI-SEAS campaigns
Authors: Musilova, Michaela; Foing, Bernard; Beniest, Anouk; Rogers,
Henk
Bibcode: 2020EGUGA..2213646M
Altcode:
As of 2018, the International MoonBase Alliance (IMA), has been
organizing regular simulated missions to the Moon and Mars at the Hawaii
Space Exploration Analog and Simulation (HI-SEAS) habitat. HI-SEAS is a
lunar and Martian analog research station located on the active volcano
Mauna Loa in Hawaii. The missions that take place at HI-SEAS can be of
varied duration, from several days to several months, depending on the
needs of the researchers. They are open to space agencies, organizations
and companies worldwide to take part in, provided their research and
technology testing will help contribute to the exploration of the Moon
and Mars. The crews are supported by a Mission Control Center based on
the Big Island of Hawaii as well. A series of EuroMoonMars IMA HI-SEAS
(EMMIHS) missions have been taking place at HI-SEAS since 2019. These
missions bring together researchers from the European Space Agency
(ESA), IMA, the International Lunar Exploration Working Group (ILEWG),
European Space Research and Technology Centre (ESTEC), VU Amsterdam and
many other international organizations. Crews on these missions perform
geological, astrobiological and architectural research; technological
tests using drones, 3Dprinters and rovers; as well as performing
outreach and educational projects. The EMMIHS missions typically last
for two weeks each. During this time, the crew is isolated within
the HI-SEAS habitat, which they cannot leave without performing EVAs
(Extra-Vehicular Activities) in analog space-suits and with the
permission of Mission Control. The EMMIHS campaigns aim to increase
the awareness about the research and technology testing that can be
performed in analogue environments, in order to help humans become
multiplanetary species. Furthermore, the research and technological
experiments conducted at HI-SEAS are going to be used to help build
a Moon base in Hawaii, and ultimately to create an actual Moon base
on the Moon, as part of IMA's major goals. Future missions at HI-SEAS
include more EMMIHS campaigns, collaborative missions with ESA, NASA,
University of Hawaii, University of South Florida and with companies,
such as SIFT and Ketone Technologies.
Title: Personalised Dietary Plans And Health Effects On Astronauts
In Extra-Terrestrial Habitats
Authors: Chappuis, Johanna; Pouwels, Charlotte; Musilova, Michaela;
Foing, Bernard
Bibcode: 2020EGUGA..2220628C
Altcode:
Astronaut nutrition is an important aspect to consider for
extra-terrestrial missions. It encompasses microbiological risks for
humans, individual nutritional needs and the social well-being of
astronauts. During a two-week analogue astronaut mission to the Moon,
research focusing on the dietary needs and health of each crew member
was performed. A crew of six analog astronauts, from the EuroMoonMars
IMA HI-SEAS II (EMMIHS-II) mission followed a pre-prepared personal
menu based on their intolerances and daily activities. The first things
that needed to be considered was the sanitary aspect of the missions,
as it severely limits food choices. Fresh foods that are consumed on
Earth are microbiologically fragile and occupy an important conservation
space air. In order to ensure food safety and optimize storage space,
the only food taken on the EMMIHS-II mission was freezedried.Prior to
the mission, the food rations and distribution amongst crewmembers
was determined according to the average nutritional and calorific
needs of the group. To maintain a basal metabolism, a balanced
nutrition is required. A healthy and sufficient food intake is of
high importance, particularly due to the regular physical activity
each crewmember performs during Extra Vehicular Activities (EVAs) that
the crew performed daily.It was not possible to determine the actual
amount of energy consumed on a daily basis during this mission for
logistical reasons. It was also not possible to weigh out the food for
each individual crewmember, as it would have taken up too much of the
mission time. In the future, portions could be determined in terms of
"cup sizes" per person, as this would be the most realistic measure for
the preparation of freeze-dried food. Furthermore, various digestive
problems have been identified throughout this mission. Possible
explanations for these issues could be a too abrupt change of eating
habits including the lack of consumption of fresh fruits, fresh
vegetables and the lack of fiber-rich cereals. In order to avoid
this on future missions, the next strategy could be to first estimate
the dietary intake of vegetable fibre for each individual before the
mission start, in order to individually adapt the fruit and vegetable
ration recommendations.A diverse distribution of culinary recipes is
also recommended for the preparation of future missions, in order to
improve the taste of the meals for the crew. Taste is an important
part of the pleasure of eating and as a result, it heavily influences
the intake of food. This inevitably has an effect on the physical and
mental well-being of the crew.Finally, the social and psychological
aspect of food plays an important role in the mental well-being of the
astronauts. In this context, it was found that the food preparation
and meal-sharing moments enabled the team to strengthen their social
ties, which was in favour of their fulfilment. However, on the other
hand, pleasure from eating and each crewmembers' appetite did often
not correspond to this. Hence, it was found that the freezedried food
did not contribute to the emotional wellbeing of the astronauts.
Title: Food for Extra-Terrestrial Astronaut Missions on Native Soil
Authors: Pouwels, Charlotte; Wamelink, Wieger; Musilova, Michaela;
Foing, Bernard
Bibcode: 2020EGUGA..2220507P
Altcode:
Introduction: Food demand and the lack of plant nutrients are the main
reasons to establish a sustainable agricultural ecosystem on celestial
bodies, such as Mars and the Moon. Different kinds of fresh crops, grown
in a greenhouse, deliver essential macro and micro nutrients, which have
a positive impact on the well-being of humans. Thus, they will also
heavily influence the social interactions of future astronauts. Food
development is therefore one of the main activities that will need
to be established as soon as possible upon the landing of a human-led
mission on another planetary body.In addition, crops can be used for
air purification and thus oxygen production. Experimental research
has been conducted, during a two-week analogue astronaut mission
(EMMIHS-II: the second of the EuroMoonMars-IMA-HI-SEAS missions),
to grow crops, from garden cress seeds, sown in soil that resembles
the regolith on Mars and the Moon. This plant was used because it is
easy and fast to grow, which is a priority for research projects during
these short-duration missions. In addition, this research will help in
reducing compost and fertilizer payloads for upcoming space missions
involving human crewmembers.Methodology: In a remote volcanic region
in Hawai'i, United States, the geology and therefore its soil is quite
similar to the regolith on Mars and the Moon. For these reasons, the
Hawai'i Space Exploration Analog and Simulations (HI-SEAS) habitat was
constructed and is being used in this area for space-related research
purposes.In this habitat, a greenhouse setting had been built with
basic requirements for plant growth. The local soil in each of the 70
pots had pre-determined ratio's with a compost mixture: 0%, 1%, 2%,
3%, 5%, 10%, 25%, 50%, 75%, 100%. For these settings, the assumption
was made that shielding from Solar Energetic Particles (SEP) and
Galactic Cosmic Rays (GCR's) was present. These types of radiation,
and thus shielding from the radiation, would be of high relevance on
Mars and the Moon to protect the crops there from malformations and
death. Future habitats may be located in lava tubes or covered by
regolith to address these requirements.Here, the presented results
focus on the needed ratio of compost to 'Martian' simulant soil for
garden cress. The results indicate that coarse 'Martian' soil with 2%
of compost is sufficient for establishing sufficient germination and
plant growth in the first stage of plant development. This result leads
to promising expectations for other nutrient-soil ratio experiments. In
particular for the growth of potatoes and beans, as they are high in
nutrients per m3.Studies on different kinds of soil ratio's, nutrients
delivered per m3, radiation shielding and the architecture of an indoor
greenhouse setting are of significant relevance to future missions to
the Moon and Mars and thus deserve further investigation.
Title: Report from ILEWG Task Groups: Science, Technology,
human aspects, roadmaps, socio-economics, young lunar explorers,
MoonVillage, MoonMars synergies, EuroMoonMars, ArtMoonMars
Authors: Foing, Bernard
Bibcode: 2020EGUGA..2222025F
Altcode:
ILEWG has been organising since 1994 ICEUM International Conferences on
Exploration & Utilisation of the Moon with published proceedings,
and where community declarations have been prepared and endorsed by
community participants. ILEWG has co-organised and co-sponsored lunar
sessions at EGU, COSPAR, EPSC.ILEWG task groups include science,
technology, human aspects, socio-economics, young explorers and
outreach, programmatics, roadmaps and synergies with Mars exploration,
MoonBase, MoonVillage, EuroMoonMars, ArtMoonMars, Young Lunar Explorers,
ILEWG Young Professional Grantees. ILEWG has also sponsored a number of
activities, workshops, tasks groups and publications in collaborations
with other organisations: COSPAR, space agencies, IAA, IAF, EGUBesides
the discussion forums, users can also obtain information on how to
participate, as well as details on the latest news and events regarding
lunar exploration, forthcoming meetings, relevant reports and documents
of importance for the work of the ILEWG, summary descriptions of recent
and future lunar exploration projects (such as SMART-1, Chang'E1-5,
Selene Kaguya, Chandrayaan-1-2, LRO, LCROSS), GRAIL, ARTEMIS,
international lunar exploration projects) funded by various space
agencies, and basic data on the Moon itself. Activities of the related
space agencies and organizations can also be found. The ILEWG Forum also
hosts the Lunar Explorer's Society. http://www.lunarexplorers.net/The
International Lunar Exploration Working Group (ILEWG) is a public
forum sponsored by the world's space agencies to support "international
cooperation towards a world strategy for the exploration and utilization
of the Moon - our natural satellite" (International Lunar Workshop,
Beatenberg (CH), June 1994). The Forum is intended to serve three
relevant groups:Actual members of the ILEWG, i.e. delegates and
representatives of the participating Space Agencies and organizations -
allowing them to discuss and possibly harmonize their draft concepts
and plans in the spirit of the Beatenberg Declaration (see below). Team
members of the relevant space projects - allowing them to coordinate
their internal work according to the guidelines provided by the ILEWG
Charter (see below). Members of the general public and of the Lunar
Explorer's Society who are interested and wish to be informed on the
progress of the Moon projects and possibly contribute their own ideas.
https://en.wikipedia.org/wiki/International_Lunar_Exploration_Working_Grouphttps://moonbasealliance.com/ilewgILEWG
ICEUM declarations (International
Conference on Exploration & Utilisation of the Moon)
:https://ui.adsabs.harvard.edu/search/q=ilewg%20declarations&sort=date%20desc%2C%20bibcode%20desc&p_=0COSPAR
ICEUM13: Pasadena Lunar Declaration 2018
https://meetingorganizer.copernicus.org/EPSC-DPS2019/EPSC-DPS2019-874-1.pdfReport
from ILEWG and Cape Canaveral Lunar Declaration 2008
https://meetingorganizer.copernicus.org/EGU2009/EGU2009-13223.pdf
Title: Semi-privacy and Color Application as Elements of Habitability
in Concept Designs for Extra-terrestrial Habitation
Authors: Kerber, Sabrina; Wanske, Ariane; Musilova, Michaela; Foing,
Bernard
Bibcode: 2020EGUGA..2218245K
Altcode:
IntroductionConcepts for designs of extra-terrestrial habitats
are experiencing a growing importance in the space industry. New
technologies and innovative materials bring the need for novel spatial
arrangements in these habitats. Two of the most important components
to improve habitability in extra-terrestrial habitats - the situation
of privacy and color application - have been addressed in a lunar
simulation (EMMIHS-II) at the Hawaíi Space Exploration Analog and
Simulations (HI-SEAS) habitat. This analog astronaut mission was
initiated by the European Space Agency's (ESA) EuroMoonMars (EMM) and
International Lunar Exploration Working Group (ILEWG) in cooperation
with the International MoonBase Alliance (IMA).The question of
how much privacy is necessary to create a liveable environment in
an extra-terrestrial habitat has engaged space architects for the
last decades. [1] The same keen interest has been attributed to the
importance of color in guiding architectural conceptions in the often
colour-less environment of outer space. [2] Less attention has been
paid to the issue of semi-private space. Past analog astronaut missions
at the HI-SEAS facility came across not only a lack of private space
but also a scarcity of areas crew members could retreat to without
completely leaving the common space. [2] Such semi-private areas
bear great potential both from a spatial and psychological point
of view.MethodologyThe research results presented here are based on
several experiments conducted during the EMMIHS-II lunar simulation
at the HI-SEAS Mars/Moon Research Facility.Potential benefits on crew
cohesion, work effectiveness and personal mood were studied through
setting up a semi-private area and assessing its use by the crew.Further
experiments investigated the analog astronauts' reaction to disparate
color situations inside the habitat and this semi-private space.The
findings will serve as a basis for future architectural design concepts
in extra-terrestrial habitats and also offer the potential for further
investigations during future analog missions.AcknowledgementsFirst,
we would like to thank our fellow EMMIHS-II crew members (M. Musilova,
A. J. D'Angelo, A. P. Castro de Paula Nunes, C.R. Pouwels) and the
EMMIHS-II mission sponsors. In addition, our gratitude goes out to
the HI-SEAS Mission Control, ground support at ESA/ESTEC and the
ILEWG EuroMoonMars manager, Prof. B. H. Foing, for enabling this
research. References[1] K. Kennedy, S. Capps (2000). Designing Space
Habitation. Space 2000. 10.1061/40479(204)6.[2] I. Schlacht, H. Birke
(2011). Space design: Visual interface of space habitats. Personal
and Ubiquitous Computing. 15. 497-509. 10.1007/s00779-010-0326-4.[3]
S. Häuplik-Meusburger, K. Binsted et al (2017). Habitability Studies
and Full Scale Simulation Research: Preliminary themes following HISEAS
mission IV.[4] Musilova, M., Rogers, H., Foing, B.H. et al (2019). EMM
IMA HI-SEAS campaign February 2019. EPSC-DPS2019-1152.[5] EuroMoonMars
Instruments, Research, Field Campaigns and Activities 2017-2019. Foing,
B.H., EuroMoonMars 2018-2019 Team. 2019 LPI Contrib. No. 3090.
Title: The Human Factors of Additive Manufacturing on Human
Extra-Terrestrial Missions
Authors: Kerber, Sabrina; Musilova, Michaela; Foing, Bernard
Bibcode: 2020EGUGA..2220496K
Altcode:
Introduction Additive manufacturing technologies have been successfully
implemented in the concept designs for human interplanetary missions
for some years. They not only play an important role in the designs
of future-extra-terrestrial habitats, but the benefits of 3D
printing have already been successfully tested on the International
Space Station (ISS). [1] However, while such studies of in-situ
manufacturing techniques concentrate heavily on applications in the
area of engineering or on the potential of 3D printing sustenance,
they regretfully neglect to explore the potential benefits additive
manufacturing could have for the Human Factors of space exploration. [1,
2]Based on experiments during a lunar simulation at the Hawaíi Space
Exploration Analog and Simulations (HI-SEAS) habitat, this paper
investigates how additive manufacturing can improve liveability in a
space habitat.Personal objects and leisure time items are indispensable
for manned space exploration, as they greatly contribute to the
astronauts' mental health and psychosocial balance. Access to a 3D
printer bears the potential of a much greater flexibility and variety
in personal items, and could also offer the possibility to customize
leisure objects to specific needs and moods of astronauts. In addition,
through the limited payloads and possibilities of recycling everyday
objects, additive manufacturing technology offers the opportunity to
greatly enhance the sustainability the of any human extra-terrestrial
mission.Methodology In December 2019 the European Space Agency's (ESA)
EuroMoonMars (EMM) and International Lunar Exploration Working Group
(ILEWG) initiated an analog astronaut simulation in cooperation with the
International MoonBase Alliance (IMA). During this mission (EMMIHS-II -
EuroMoonMars IMA HI-SEAS) the Human Factors of Additive Manufacturing
Study was conducted as a basis for this paper. Psychological effects,
changes in mood and work effectiveness, and the possibility to create
and maintain a connection to Earth by 3D printing seasonal objects and
decorations, were assessed.The study delivered positive results about
the use of additive manufacturing from a Human Factors point of view, as
well as the confirmation of the use in engineering. The results open up
the possibilities for further studies of the Human Factors of additive
manufacturing during future analog simulations.AcknowledgementsFirst,
I would like to thank our fellow EMMIHS-II crew members (M. Musilova,
A. J. D'Angelo, A. P. Castro de Paula Nunes, C.R. Pouwels) and the
EMMIHS-II mission sponsors. In addition, my gratitude goes out
to the HI-SEAS Mission Control, ground support at ESA/ESTEC and
the ILEWG EuroMoonMars manager, Prof. B. H. Foing, for enabling
this research. References:[1] T. Prater et al (2019), Overview
of the In-Space Manufacturing Technology Portfolio, NASA & ISS
National Lab Microgravity Materials Science Workshop, Georgia, US.[2]
M. Terfansky, M. Thangavelu (2013), 3D Printing of Food for Space
Missions, California, US.[3] M. Musilova, H. Rogers, B. H. Foing et al
(2019). EMM IMA HI-SEAS campaign February 2019. EPSC-DPS2019-1152.[4]
EuroMoonMars Instruments, Research, Field Campaigns and Activities
2017-2019. B. H. Foing, EuroMoonMars 2018-2019 Team. 2019 LPI
Contrib. No. 3090.
Title: SOMA Suits
Authors: Sitnikova, A.; Glukhova, E.; Foing, B.; Ageli, J.; Noskov,
K.; Stylianou, S.; Moutaftsi, A.
Bibcode: 2020LPI....51.1649S
Altcode:
SOMA Suits project brings together students with different backgrounds
to prepare to help launch a sustainable human presence on the Moon
and beyond.
Title: EuroMoonMars IMA at HI-SEAS Campaigns in 2019: An Overview of
the Analog Missions, Upgrades to the Mission Operations, and Protocols
Authors: Musilova, M.; Foing, B.; Beniest, A.; Rogers, H.
Bibcode: 2020LPI....51.2893M
Altcode:
The EuroMoonMars campaigns at the HI-SEAS (IMA) station in Hawaii
involve performing Moon and Mars related research and technology
testing by international crews.
Title: Food for Extra-Terrestrial Astronaut Missions on Native Soil
Authors: Pouwels, C. R.; Wamelink, G. W. W.; Musilova, M.; Foing, B.
Bibcode: 2020LPI....51.1605P
Altcode:
Food demand during extra-terrestrial missions is of high
importance. Therefore, research is done on plants that grow on simulant
soil during an analogue mission.
Title: The Human Factors of Additive Manufacturing on Human
Extra-Terrestrial Missions
Authors: Kerber, S.; Musilova, M.; Foing, B. H.
Bibcode: 2020LPI....51.1986K
Altcode:
Based on a lunar simulation by the European Space Agency, the
paper investigates how 3D printing can benefit the human factors of
extra-terrestrial missions.
Title: Lunar and Martian Regolith Based Concrete as Building Blocks
for Future Human Settlements
Authors: Heemskerk, M. V.; van Westrenen, W.; Foing, B. H.
Bibcode: 2020LPI....51.2878H
Altcode:
Concept for future lunar and martian building blocks, derived from
ISRU-based concrete.
Title: Spatial Analysis of Lava Tubes for the Purpose of
Extra-Terrestrial Habitation
Authors: Wanske, A.; Kerber, S.; Musilova, M.; Foing, B. H.
Bibcode: 2020LPI....51.1890W
Altcode:
The paper aims to provide an environmental guideline for the deployment
of extra-terrestrial settlements inside of lunar lava tubes for space
architects.
Title: Emmihs-2, the Second Euromoonmars IMA Hi-Seas 2019 Campaign:
Simulated Moonbase Outlook and Outcomes - An Engineering Perspective
Authors: Nunes, A. P. C. P.; Musilova, M.; Cox, A.; Agelini, J.;
Foing, B.
Bibcode: 2020LPI....51.2405N
Altcode:
EMMIHS are field research campaigns with the aim to conduct experiments
and test technologies relevant to space exploration and extraterrestrial
habitation.
Title: EuroMoonMars, HI-SEAS 2020: Analysis of Secondary
Mineralization and IR Spectroscopy of Igneous Rocks in Lava Tubes
on Mauna Loa, Hawaii; Insights in Extraterrestrial Environments and
Future Space Exploration
Authors: Mulder, S. J.; Foing, B. H.; Weert, A. M. P.
Bibcode: 2020LPI....51.1522M
Altcode:
The study of secondary mineralization in lava tubes to understand the
formation processes of these minerals on other terrestrial bodies in
the solar system.
Title: Moon Gallery
Authors: Sitnikova, A.; Glukhova, E.; Foing, B.; Zaklynsky, A.
Bibcode: 2020LPI....51.1635S
Altcode:
Moon Gallery is an international collaborative artwork and a gallery
of ideas worth sending to the Moon.
Title: Personalised Dietary Plans and Health Effects on Astronauts
in ExtraTerrestrial Habitats
Authors: Chappuis, J.; Pouwels, C. R.; Musilova, M.; Foing, B.
Bibcode: 2020LPI....51.1510C
Altcode:
I. EMMIHS II dietary research: sanitary aspect, nutritional needs, menu;
II. Observations and solutions: food intake, digestion, taste, appetite.
Title: Testing Rover Cooperation Concepts in Moon Analog Site
Authors: Heemskerk, R. S.; Edison, K.; Atya, S.; Heemskerk, C. J. M.;
Heemskerk, M. V.; Foing, B.
Bibcode: 2020LPI....51.3035H
Altcode:
Three different rover concepts are tested for rover-rover collaboration
at a Moon analog site.
Title: Semi-Privacy and Color Application as Elements of Habitability
in Concept Designs for Extra-Terrestrial Habitation
Authors: Kerber, S.; Wanske, A.; Musilova, M.; Foing, B. H.
Bibcode: 2020LPI....51.1991K
Altcode:
Based on a lunar simulation, the paper provides architectural guidelines
for semi-privacy and color application in extra-terrestrial habitation.
Title: EMMIHS-III Mission General Overview
Authors: Rajkakati, P. D.; Heemskerk, M. V.; Foing, B. H.
Bibcode: 2020LPI....51.3051R
Altcode:
EMMIHS-III is the third EuroMoonMars analogue mission at International
Moonbase Alliance base at HI-SEAS, and will elaborate on the previous
missions.
Title: C60+ as a diffuse interstellar band
carrier; a spectroscopic story in 6 acts
Authors: Linnartz, H.; Cami, J.; Cordiner, M.; Cox, N. L. J.;
Ehrenfreund, P.; Foing, B.; Gatchell, M.; Scheier, P.
Bibcode: 2020JMoSp.36711243L
Altcode:
In 2019 it was exactly 100 years ago that the first two DIBs, diffuse
interstellar bands, were discovered by Mary Lea Heger. Today some 500 +
DIBs are known. In numerous observational, modelling and laboratory
studies, efforts have been made to identify the carriers of these
absorption features that are observed in the light of reddened stars
crossing diffuse and translucent clouds. Despite several claims over
the years that specific DIBs could be assigned to specific species,
not one of these withstood dedicated follow-up studies. An exception
is C60+. In 2015, Campbell et al. showed
that two strong bands, recorded in the laboratory around 960 nm,
coincided precisely with known DIBs and in follow-up studies three
more matches between C60+ transitions and new
observational DIB studies were claimed. Over the last four years the
evidence for C60+ as the first identified DIB
carrier - including new laboratory data and Hubble Space Telescope
observations - has been accumulating, but not all open issues have
been solved yet. This article summarizes 6 spectroscopic achievements
that sequentially contributed to what seems to become the first DIB
story with a happy end.
Title: Ionized Interstellar Buckyballs (C60+) Confirmed Using the
Hubble Space Telescope
Authors: Cordiner, M.; Cox, N.; Linnartz, H.; Cami, J.; Najarro, F.;
Proffitt, C.; Lallement, R.; Ehrenfreund, P.; Foing, B.; Gull, T.;
Sarre, P.; Charnley, S.
Bibcode: 2020AAS...23523607C
Altcode:
Ground-based high-resolution astronomical spectroscopy, combined
with new innovations in laboratory techniques at low temperatures,
has provided strong evidence for the presence of C60+ (ionized
Buckminsterfullerene) in the diffuse interstellar medium (ISM). The
attribution of two interstellar absorption bands near 0.96 microns to
electronic transitions of C60+ became quite widely accepted in 2015,
but irrefutable identification of C60+ requires a match between the
wavelengths and the strengths of all five absorption features detectable
in the laboratory and in space. Although ground-based observations
revealed likely absorptions consistent with three weaker bands at
9348, 9365 and 9428 Angstroms, follow-up observations were required
to definitively confirm their presence. Using the novel STIS-scanning
technique pioneered by our team, we obtained ultra-high signal-to-noise,
high-dispersion Hubble Space Telescope spectra of seven heavily reddened
interstellar sightlines. A primary benefit of these spectra is that
they do not suffer from contamination by telluric absorption that
afflicts ground-based observations in this part of the spectrum. We
thus obtained reliable detections of the (weak) 9365, 9428 Angstrom
and (strong) 9577 Angstrom C60+ bands. Within the uncertainties, the
band wavelengths and strength ratios in early B-type stars (suffering
from relatively little stellar contamination) were found to match
those determined in the latest laboratory experiments of Campbell et
al. (2018), so we consider this a robust identification of the 9428
A band, and conclusive confirmation of interstellar C60+.
Title: IGLUNA: ILEWG BTU Smart Ice Lab
Authors: Sitnikova, Anna; Dimova, Lyubov; Wanske, Ariane; Foing,
Bernard; Sanden, Germaine vd; Grosjean, Marius; Moritz, David;
Löffler, Martin; Schlacht, Irene
Bibcode: 2019EPSC...13.1393S
Altcode:
Mission of ILEWG BTU team in IGLUNA project is to provide scientists
with the capability to conduct examinations and measurements on ice
samples and cores, and to preserve the integrity of these for current
and future investigations. We work together with art scientists to
visualize scientific data and provide public outreach.
Title: COSPAR ICEUM13: Pasadena Lunar Declaration 2018
Authors: Foing, Bernard
Bibcode: 2019EPSC...13..874F
Altcode:
Lunar, Planetary and Space Explorers attended the 13th ILEWG
International Conference on Exploration and Utilisation of the Moon
(ICEUM13) from 16 to 20 July 2018 at COSPAR 42nd Assembly in Pasadena,
California. The Pasadena Lunar Declaration 2018 was approved by COSPAR
participants of ICEUM13A B3.3 session on Lunar science and Exploration,
COSPAR participants of ICEUM13B PEX2 Human and Robotic Exploration of
Moon, Mars and NEOs.
Title: Planetary Defence: Science, Technology & Society
Authors: Foing, Bernard
Bibcode: 2019EPSC...13.1305F
Altcode:
We need to reinforce efforts for planetary defence in Science,
Technology & Society aspects. ESA is developing a space safety
programme that includes planetary defence: "ESA has been considering
the use of space missions for asteroid risk assessment for almost
two decades. Although the chance of a major asteroid impact is low,
the potential consequences to our society could be very severe.
Title: EuroMoonMars IMA HI-SEAS 2019: Hydrous alteration of lava
flows on Mauna Loa (Hawaii) compared to Martian volcanic soils
Authors: Weert, Annelotte; Foing, Bernard; Mulder, Sebastian;
Musilova, Michaela
Bibcode: 2019EPSC...13..722W
Altcode:
In order to provide more insight in the similarities of the effects
of hydrous alteration on volcanic rocks on Mars, samples of different
lava flows from Mauna Loa (Hawaii) will be compared by measurements
of the Mars Exploration Rovers (MER).
Title: EMM IMA HI-SEAS campaign February 2019
Authors: Musilova, Michaela; Rogers, Henk; Foing, Bernard; Sirikan,
Nityaporn; Weert, Annelotte; Mulder, Sebastian; Pothier, Benjamin;
Burstein, Joshua
Bibcode: 2019EPSC...13.1152M
Altcode:
The Hawaii - Space Exploration Analog and Simulation (HI-SEAS)
habitat is located at 8,200' (2,500 meters) in elevation on the
largest mountain in the world, Mauna Loa, on the Big Island of
Hawai'i. HI-SEAS has been the home to five successful long duration
(4 to 12 month) NASA Mars simulation missions since 2013. A HI-SEAS
Mars mission involved six person crews being isolated from the
rest of humanity for long periods of time. While in the simulation,
communications with "Earth" were delayed by up to 20 minutes each
way to simulate Mars being on other side of the Sun from Earth. When
the crew left the HI-SEAS habitat, they wore analog space-suits and
they went through full extra vehicular activity (EVA) protocols to
perform their research in the simulated Martian terrain. HI-SEAS has
also been used to perform multiple shorter duration lunar simulated
missions, in collaboration with diverse organisations and companies
worldwide. As of 2018, the International Moonbase Alliance (IMA),
an organization dedicated to building sustainable settlements on the
Moon, has been organising regular simulated missions to the Moon,
Mars or other planetary bodies at HI-SEAS. The constraints for these
missions depend on which planetary body the mission is simulating to be
on. For instance, for lunar missions the time delay in communications
is only of a few seconds, which is nearly negligible for EVAs and
other activities. In 2019, the EuroMoonMars campaign was launched at
HI-SEAS, bringing together researchers from the European Space Agency,
VU Amsterdam, the International Lunar Exploration Working Group (ILEWG)
and IMA. Six scientists, engineers, journalists and photographers spent
two weeks at the HI-SEAS station performing research relevant to both
the Moon and Mars there. The campaign aims to increase the awareness
about the research and technology testing that can be performed in
analogue environments, in order to help humans become multiplanetary
species. Furthermore, the research and technological experiments
conducted at HI-SEAS are going to be used to help build a Moonbase
in Hawai'i, and ultimately to create an actual Moonbase on the Moon,
as part of IMA's major goals. Future missions at HI-SEAS include
collaborative missions with NASA's Johnson Space Center, University
of South Florida and companies such as SIFT and Ketone Technologies.
Title: Planetary Outreach Through the Arts: ArtMoonMars
Authors: Foing, Bernard; Sitnikova, Anna
Bibcode: 2019EPSC...13.1823F
Altcode:
We give an update of ArtMoonMars, Moon Village & ITACCUS (IAF
ITACCUS Committee on Socio Cultural Utilisation of Space) activities,
with emphasis on events that took place in from 2017 to 2019. The Moon
Village is an open concept proposed with the goal of a sustainable human
and robotic presence on the lunar surface as an ensemble where multiple
users can carry out multiple activities. We want to involve everybody
including Socio-cultural and Artistic aspects. Why ArtMoonMars? Artists
can convey multiple messages of the community including planetary
science, life sciences, astronomy, fundamental research, resources
utilisation, human spaceflight, peaceful cooperation, economical
development, inspiration, training & capacity building.
Title: International MoonBase Alliance: Goals and Update
Authors: Musilova, Michaela; Rogers, Henk; Foing, Bernard
Bibcode: 2019EPSC...13.1176M
Altcode:
The International MoonBase Alliance (IMA) is an international non-profit
organization, uniting leading scientists, educators, and entrepreneurs
from space agencies, academic organizations and industries worldwide
to advance the development and implementation of the work needed to
make humankind become a multi-planetary species. IMA's first major
project beyond the Earth is to build an international base on the
Moon called Mahina Lani - Hawaiian for Heaven on the Moon. Experts
around the world are being consulted to create an action plan that
will culminate with the building of Moon-base prototypes on Earth,
followed by a building an actual sustainable settlement on the Moon
in the next decade. The action plan is being built on discussions and
recommendations from the Lunar Exploration and Analysis Group (LEAG),
the European Lunar Symposium, the International Space Development
Conference, the NewSpace Symposium, the International Astronautical
Congress (IAC), and many other worldwide space forums. Figure 1:
Artistic rendition of a version of Mahina Lani on the Moon. Part of
IMA's long-term strategy is a creation of a prototype Moon-base in
Hawai'i to test all of the equipment and scientific research needed to
build Mahina Lani. The first steps have been taken to try to acquire
land on the Big Island of Hawai'i, as well as finances, partners and
other critical elements to build the prototype Moonbase. Futhermore,
the Hawaii - Space Exploration Analog and Simulation (HI-SEAS)
research facility on the Big Island, located at 8,200 feet (2,500
meters) in elevation, is also being used for technology testing and
research in preparation for the prototype Moonbase to be built. The
research includes conducting simulated missions to the Moon, such the
EMM IMA HI-SEAS campaign started in 2019.
Title: Moon Gallery: steps towards the implementation of the actual
gallery on the Moon
Authors: Sitnikova, Anna; Glukhova, Elizaveta; Foing, Bernard; Kozhina,
Daria; de Quaasteniet, Jorick; zaklynsky, Alexander; Kuiper, Mary
Bibcode: 2019EPSC...13.1362S
Altcode:
Moon Gallery is an international collaborative artwork and a gallery
of ideas worth sending to the Moon. Moon Gallery intends to launch 100
artifacts to the Moon within the compact format of 10 x 10 x 1cm plate
on a lunar lander as early as 2022. In this multi-case tray gallery
we are developing culture for future interplanetary society. What are
the ideas we want to promote into the future? What are the ideas we
want to leave behind?
Title: VUSE, VU Science Experiments as student project performed at
IGLUNA, a human Moon-Ice habitat simulation.
Authors: de Winter, Bram; Heemskerk, Marc; Foing, Bernard; Daeter,
Marjolein
Bibcode: 2019EPSC...13..781D
Altcode:
To explore the possibilities of performing science when building a
human habitat on the Moon, a group of students from VU Amsterdam,
the Netherlands started VUSE, VU Science Experiments and this group
is participating in IGLUNA, organized by the Swiss Space Center
and ESA_Lab. This project is a simulation of a human habitat at
the South-Pole of the Moon. VUSE is designed and tested to combining
glaciology, geology, life science experiments, astrobiology and analog
simulation planning into one science package. During a 16-day campaign
the team will perform these experiment, with the goal of providing a
showcase of science that could be done within in Moon-Ice habitat and
a research to the history of the glacier. VUSE is building on work and
experience of previous student groups at the ILEWG Euromoonmars group.
Title: Horizon 2061: Infrastructures, services & collaborative
programs
Authors: Foing, Bernard
Bibcode: 2019EPSC...13.1596F
Altcode:
We shall give a preliminary synthesis of the discussions and
recommendations that took place within Horizon 2061 initiative and
workshops, concerning the Horizon 2061 pillar 4: Infrastructures,
services and collaborative programs.
Title: Using Martian and Lunar Soils as Building Blocks for Future
Habitats
Authors: Heemskerk, Marc; van Westrenen, Wim; Foing, Bernard
Bibcode: 2019EPSC...13.1825H
Altcode:
Using Martian and lunar soils to construct concrete building blocks,
which can be used to provide habitable constructions while on
extraterrestrial surface. Multiple soil simulants have been tested,
results will be published at the EPSC.
Title: SMART-1 Highlights & Apollo Celebration
Authors: Foing, Bernard
Bibcode: 2019EPSC...13..824F
Altcode:
SMART-1 results have been relevant for lunar science and exploration,
in relation with previous missions (Apollo, Luna) and subsequent
missions (Kaguya, Chang'E1-2, Chandrayaan-1, LRO, LCROSS, GRAIL,
LADEE, Chang'E3-4 and future landers). We present SMART-1 highlights
that celebrate APOLLO legacy after 50 years. SMART-1 was the first
in the programme of ESA's Small Missions for Advanced Research and
Technology. Its first objective has been achieved to demonstrate
Solar Electric Primary Propulsion (SEP) for future Cornerstones
(such as Bepi-Colombo) and to test new technologies for spacecraft
and instruments.
Title: 14-month isolation in Antarctica: research experience in a
a space-analogue environment
Authors: Müller, Hanno; Schlacht, Irene Lia; Foing, Bernard
Bibcode: 2019EPSC...13.1835M
Altcode:
Presented are the personal experience of a 14-month isolation mission
in Antarctica and selected scientific results about the temporal
evolution of surface air temperature and ozone partial pressure above
Neumayer Station.
Title: Interstellar Fullerenes
Authors: Cox, Nick; Foing, Bernard
Bibcode: 2019EPSC...13.1640C
Altcode:
In this contribution we present an overview of recent results on the
detection and study of fullerenes (and related organic compounds) in
the diffuse-to-translucent interstellar medium. The results pertain
primarily to new observations of interstellar targets obtained with
both ground and space-based facilities operating in the optical and
infrared wavelength domains. Perspectives for future studies are given.
Title: Goals and first results from MDRS IESL Crew 205
Authors: Grulich, Maria; Alotaibi, Ghanim; Blackburn, Hannah;
Hadland, Nathan; Larrea Brito, Natalia; Masaitis, David; Robson,
Daniel; Triviño, Verónica; Foing, Bernard
Bibcode: 2019EGUGA..2118660G
Altcode:
The International Emerging Space Leaders (IESLs) Crew 205 is composed by
eight outstanding international space young professionals and students,
who together, fulfilled a Mars analog mission from February 9th to
24th at MDRS in 2019. The IESL's Crew is an interdisciplinary and
multicultural team including members from Kuwait, Spain, Germany,
the U.K. and the U.S. During the two-week rotation, the crew will
simulate a mission to the Red Planet. The team conducted multiple
research projects relevant to space exploration in areas such as
in-situ resources utilization, human behavior, leadership and teamwork,
astronomy, geology, EVA optimization, and science outreach. The research
is done in collaboration with ILEWG and ESTEC in the Netherlands. In
addition to these research projects, the crew was also in charge of the
maintenance of MDRS facilities and daily operations of the station. This
mission also ultimately contribute to a better understanding of the
requirements, benefits and challenges of international teams in future
manned missions. This paper explains the results of the different
researches conducted during the two weeks mission.
Title: IGLUNA - Habitat in Ice: An ESA_Lab project hosted by the SSC
Authors: Benavides, Tatiana; Heemskerk, Marc; Foing, Bernard; De
Winter, Bram
Bibcode: 2019EGUGA..2117807B
Altcode:
IGLUNA is the first ESA_Lab interuniversity demonstrator project, and
is hosted by the Swiss Space Centre (SSC) with the vision to create
an analogue habitat inside lunar ice caps. 18 student teams from 9
countries across Europe will develop modular demonstrators that will
be constructed and tested in the field test in June 2019. This field
test will be conducted inside the moon-like extreme environment of
the Glacier Palace inside the Matterhorn glacier from 17 - 30 June
2019. During these two weeks, all the student demonstrators will
be combined to make a 36m2 human habitat. The Glacier Palace will
be open for the public during the tests, so that visitors have the
opportunity to observe or even participate in the experiments. Building
a habitat in ice on the moon has several large advantages; besides
not having to bring a large, pressurized habitable structure, water
(ice) is a great insulator for cosmic radiation and radiation from
the Sun. Furthermore, a close proximity of water is of high priority
to enlarge the chances of human survival, as water is essential for
life, but it can also be used to produce oxygen, as fuel, and energy
storage. Lastly, building a covered or subterranean on the moon also
protects against micrometeorites or dust storms from landing rockets
or large nearby impacts [1]. Besides the protection inside the polar
crater from heat from the sun, the exact opposite goes for the crater
rims. There are several points known on the south pole of the moon
where the sun shines for over 90% of the time during a lunar year,
meaning that a solar power facility is able to almost constantly
produce energy for a nearby lying facility [2-3]. Having a lunar
habitat inside a crater on the south pole of the moon thus seems
to be the most viable option for a near-future semi-permanent human
habitat. To inspire students to think about this habitat and increase
international relations and experience with designing a lunar habitat,
is the main goal of IGLUNA. IGLUNA: Being the demonstrator pilot
project of the ESA_Lab initiative, IGLUNA aims to inspire students
to participate in a space project by designing a lunar ice habitat
and foster international collaboration between the next generation of
space experts. IGLUNA builds on the experience of EuroMoonMars research
programme and analogue field campaigns involving young professionals
[4]. With the analogue base inside a (terrestrial) glacier, IGLUNA will
provide public outreach and raise international awareness, by improving
education about the durability and self-sustainability of space
missions. IGLUNA will also function as a test for future (spacefaring)
missions [1]. Acknowledgements: We acknowledge the IGLUNA coordinators
at the SSC (including T.Benavides, O.Kirchhoff, K.Kunstmann, D.Bass,
Y.Delessert). Besides, we would like to thank Prof. Bernard Foing
for his outstanding expertise and personal support for IGLUNA. We
would like to thank the VUSE team (including M.Heemskerk, B.deWinter,
M.Daeter, et al.), and recent ILEWG and EuroMoonMars-teams. References:
[1] SSC,https://www.spacecenter.ch/igluna/media/ , [2] B.Foing
(2005)https://www.astrobio.net/news-exclusive/peaks-of-eternal-light/
, [3] D.B.JBussey (2010), [4] B.Foing et al
https://www.hou.usra.edu/meetings/leag2017/pdf/5073.pdf
Title: Analogue research performed at the HI-SEAS research station
in Hawaii
Authors: Musilova, Michaela; Rogers, Henk; Foing, Bernard
Bibcode: 2019EGUGA..2115007M
Altcode:
The Hawaii - Space Exploration Analog and Simulation (HI-SEAS)
habitat is located at 8,200' (2,500 meters) in elevation on the
largest mountain in the world, Mauna Loa, on the Big Island of
Hawai'i. HI-SEAS has been the home to five successful long duration
(4 to 12 month) NASA Mars simulation missions since 2013. A HI-SEAS
Mars mission involved six person crews being isolated from the
rest of humanity for long periods of time. While in the simulation,
communications with "Earth" were delayed by up to 20 minutes each
way to simulate Mars being on other side of the Sun from Earth. When
the crew left the HI-SEAS habitat, they wore analog space-suits and
they went through full extra vehicular activity (EVA) protocols to
perform their research in the simulated Martian terrain. HI-SEAS has
also been used to perform multiple shorter duration lunar simulated
missions, in collaboration with diverse organisations and companies
worldwide. As of 2018, the International Moonbase Alliance (IMA),
an organization dedicated to building sustainable settlements on the
Moon, has been organising regular simulated missions to the Moon,
Mars or other planetary bodies at HI-SEAS. The constraints for these
missions depend on which planetary body the mission is simulating to be
on. For instance, for lunar missions the time delay in communications
is only of a few seconds, which is nearly negligible for EVAs and other
activities. The research and technological experiments conducted at
HI-SEAS are going to be used to help build a Moonbase in Hawai'i, and
ultimately to create an actual Moonbase on the Moon. Future missions at
HI-SEAS include collaborative missions with the European Space Agency,
NASA's Johnson Space Center, University of South Florida and companies
such as SIFT and Ketone Technologies.
Title: Confirming Interstellar C60 + Using
the Hubble Space Telescope
Authors: Cordiner, M. A.; Linnartz, H.; Cox, N. L. J.; Cami, J.;
Najarro, F.; Proffitt, C. R.; Lallement, R.; Ehrenfreund, P.; Foing,
B. H.; Gull, T. R.; Sarre, P. J.; Charnley, S. B.
Bibcode: 2019ApJ...875L..28C
Altcode: 2019arXiv190408821C
Recent advances in laboratory spectroscopy lead to the claim of ionized
Buckminsterfullerene (C{}60+) as the carrier of
two diffuse interstellar bands (DIBs) in the near-infrared. However,
irrefutable identification of interstellar C{}60+
requires a match between the wavelengths and the expected strengths
of all absorption features detectable in the laboratory and in
space. Here we present Hubble Space Telescope (HST) spectra of
the region covering the C{}60+ 9348, 9365,
9428, and 9577 Å absorption bands toward seven heavily reddened
stars. We focus in particular on searching for the weaker laboratory
C{}60+ bands, the very presence of which has been
a matter for recent debate. Using the novel STIS-scanning technique to
obtain ultra-high signal-to-noise spectra without contamination from
telluric absorption that afflicted previous ground-based observations,
we obtained reliable detections of the (weak) 9365, 9428 Å and (strong)
9577 Å C{}60+ bands. The band wavelengths and
strength ratios are sufficiently similar to those determined in the
latest laboratory experiments that we consider this the first robust
identification of the 9428 Å band, and a conclusive confirmation of
interstellar {{{C}}}60+.
Title: Concept and field reconnaissance for a Semi-Permanent
Moon-Analogue Habitat Inside a Lava Tube in Iceland
Authors: Heemskerk, Marc; Daeter, Marjolein; Foing, Bernard;
Sitnikova, Anna
Bibcode: 2019EGUGA..2117503H
Altcode:
Finding the best terrestrial moon-analogue mission sites is of
utmost importance in the preparation for future, manned, lunar
missions. During these moon-analogue field tests, many problems
that the astronauts will encounter during the actual mission will
be discovered. The current moon-analogue bases can only represent
a part of the conditions to be found around the most likely first
semi-permanent living quarters on the moon. Bringing large structures
to the moon will take up a prohibitively large amount of energy and
time, and with that, money. Using existing structures on the lunar
surface, might thus be the most logical and durable solution. Looking
into utilizing already existing features on the moon, one can think
of three main ways to construct a livable habitat. ISRU-housing, ice
habitats and lava tube habitats. ISRU-housing, by making concrete,
sintering regolith, or covering inflatable housing, can be a great way
to insulate and design large spaces on the Moon [1], but often requires
(heavy) machinery and the use of regolith may harm the astronauts
[2]. Utilizing the ice extracted from repositories on the lunar South
pole, with the close proximity of water and 'peaks of eternal light',
alleviates the problem of having to use heavy machinery and avoids
potentially dangerous regolith. The lunar ice resources however, are
preserved in polar craters with abundances of few % and temperatures
of -220 oC; this will bring large isolation problems, as also shown
by the IGLUNA project [3]. A third option would be to build living
quarters inside the lava tubes, as recently discovered on the borders
of the mares and the highland regions. On the Moon, lava tubes will
have an average temperature of about -20 oC, which suggests that
relatively little heating is needed to make a comfortable living
space inside a lava tube and, as they can be many meters deep, they
will protect the inhabitants from harmful radiation, temperature
changes, and micrometeorites. In September 2018, a team from ILEWG
EuroMoonMars programme [4] has visited three lava tubes on Iceland;
Raufarholshellir, Surtshellir, and Stefanshellir. Raufarholshellir is
the most touristic lava cave of Iceland, which makes it more suitable
for public outreach, but less suited for researching the psychological
aspects of the isolation. Stefanshellir and Surtshellir are almost
connected, but Stefanshellir goes deeper into the lava field and has
a more maze-like structure, making Stefanshellir the most attractive
choice for a lunar analogue base. One of the main objectives of a longer
duration Iceland moon-analogue mission as part of ILEWG EuroMoonMars
Iceland campaign 2019 will be: Is it possible to harvest enough energy,
safely store it and use it to make a local, pressurized environment
that is suited for living? Other objectives that can be reached within
an Iceland moon-analogue base are ISRU-based, such as extracting water
from dehydrating rocks [5], 3D printing building material, or soil
fertility studies. [1] B.Dunbar, E.Mahoney(2018) https://nasa.gov/isru
[2] T.E.Bell(2006), Air and Space magazine [3] T.Benavides, O.Kirchoff
et al.,(2018), https://www.spacecenter.ch/igluna/ [4] B.Foing et
al https://www.hou.usra.edu/meetings/leag2017/pdf/5073.pdf [5]
T.John,(2014), AGU, 2014AGUFM.H31P..02J
Title: International Lunar Decade and UN Sustainable Development Goals
Authors: Beldavs, Vidvus; Foing, bernard
Bibcode: 2019EGUGA..2118653B
Altcode:
The International Lunar Decade (ILD) is proposed as a framework
for international cooperation in lunar exploration and development
from 2021-2030 modeled on the International Geophysical Year (IGY -
1957-8) that marked the dawn of the space age with satellites launched
by the U.S.S.R. and the US. As with IGY the global initiative will
be coordinated by a small secretariat with countries, international
organizations such as COSPAR, NGOs, universities, cities and regions,
and private firms participating. ILD is intended to open opportunities
for small and developing countries to take part as well as the larger
spacefaring countries that are already actively involved in lunar
exploration. The ILD fits well with the goals and the approach of
the UN Space 2030 initiative that is presently under development by
UN COPUOS which is preparing a a plan for Space 2030 with UN General
Assembly approval expected at the 2020 Session. The ILD is intended to
lead to sustainable presence on the Moon by 2030. The ILD framework
will enable the development of policies for use of lunar resources
as well as to govern operations on the Moon by multiple parties. The
ILD framework will also enable joint development of shared energy and
logistics infrastructure as well as public outreach programs worldwide
as well as information sharing. A concept will be presented for
cooperation between the European Union and the African Union and their
member states and state and regional organizations towards advancing
sustainable development thru cooperation in space technology and space
operations as a model for cooperation between advanced and developing
countries. The dimension of lunar exploration and lunar development and
the potential for technology transfer to meet sustainable development
on Earth will be highlighted.
Title: Growth of an Aesthetic Organism in the Moon Gallery After
One Year
Authors: Zaklynsky, A.; Sitnikova, A.; Glukhova, E.; Foing, B.
Bibcode: 2019LPI....50.2563Z
Altcode:
An international collaborative artwork and a gallery of ideas to be
sent to the Moon in 2022 within a compact format of 10 x 10 cm petri
dish-like structure.
Title: Conservative Radiation Countermeasures in Response to Space
Radiation Effects on the Lunar South Pole
Authors: van der Sanden, G. A.; Foing, B. H.
Bibcode: 2019LPI....50.2346V
Altcode:
We present a quantitative estimation of the ionizing radiation
environment and countermeasures for a manned operation to the lunar
South Pole-Aitken Basin.
Title: Characterization of Mars and Moon Microbial Life Through
Terrestrial Analogue Field Research
Authors: Clement, T. V. M.; de Winter, B.; Foing, B. H.; Heemskerk,
M. V.; VUSE Igluna Team
Bibcode: 2019LPI....50.2445C
Altcode:
VUSE team of IGLUNA is designing experiments to look for microbial life
on Moon and Mars. For this, spectrometry, microscopy, and sequencing
will be used.
Title: VUSE, VU Science Experiments at Igluna, a Science Showcase
for a Moon Ice Habitat
Authors: de Winter, B.; Heemskerk, M.; Clement, T.; Foing, B.;
Benavides, T.; Vu Amsterdam Igluna Team; ILEWG Team; Swiss Space Center
Bibcode: 2019LPI....50.1588D
Altcode:
VU Science Experiments (VUSE) is part of IGLUNA, a Moon-ice simulation
habitat. VUSE researches the history of the glacier with ice core
analysis and field data.
Title: WATER-II Mission Concept: Water Extraction Mission Based on
WATER-I and OSIRIS-Rex
Authors: Albers, B.; de Winter, B.; Foing, B. H.; Molag, K.
Bibcode: 2019LPI....50.3205A
Altcode:
Inspired by OSIRIS-REx and Hayabusa2, a group of students from VU
Amsterdam propose a water extraction asteroid mission, WATER-II as
follow-up to OSIRIS-REx.
Title: EuroMoonMars Instruments, Research, Field Campaigns, and
Activities 2017-2019
Authors: Foing, B. H.; EuroMoonMars 2018-2019 Team
Bibcode: 2019LPI....50.3090F
Altcode:
"EuroMoonMars" is an evolving pilot research programme with instruments,
investigations, facilities, field campaigns for MoonMars science
and workforce.
Title: Chemical Sample Analysis for the IGLUNA Project
Authors: Vaessen, G. C.; de Winter, B.; Heemskerk, M. V.; Foing, B. H.
Bibcode: 2019LPI....50.2664V
Altcode:
Description of experiments that can aid the chemical analysis of
geological samples for the IGLUNA project.
Title: EuroMoonMars 2018-2019 and VUSE IgLuna: External Exploration
of the Moon Village
Authors: Korthouwer, R. B.; de Winter, B.; Heemskerk, M.; Daeter,
M.; Foing, B. H.
Bibcode: 2019LPI....50.2475K
Altcode:
The external exploration components of an external lander and drones
of the EuroMoonMars 2018/2019 VUSE IGLUNA.
Title: Geology and Astrobiology Instruments Suite for IGLUNA's VU
Science Experiments (VUSE)
Authors: Daeter, M. I.; Heemskerk, M. V.; De Winter, B.; Foing, B. H.;
VU Amsterdam Igluna Team
Bibcode: 2019LPI....50.2530D
Altcode:
Application, testing, and instrument definition for the VU Science
Experiments (VUSE) IGLUNA team.
Title: Concept for a Semi-Permanent Moon-Analogue Habitat Inside a
Lava Tube
Authors: Heemskerk, M. V.; Daeter, M. I.; Foing, B. H.; Gasser, M.;
Feucht, C. M.
Bibcode: 2019LPI....50.1693H
Altcode:
Concept for a moon-analogue lava tube habitat in Iceland, capable of
hosting short to midterm duration analogue missions.
Title: SMART-1 Highlights and Tribute to Apollo Legacy
Authors: Foing, B. H.; Racca, G.; Marini, A.; Camino, O.; Koschny,
D.; Frew, D.; Volp, J.; Josset, J. L.; Beauvivre, S.; Shkuratov, Y.;
Muinonen, K.; Mall, U.; Nathues, A.; Grande, M.; Kellett, B.; Pinet,
P.; Chevrel, S.; Cerroni, P.; Barucci, M. A.; Erard, S.; Despan, D.;
Shevchenko, V.; McMannamon, P.; Borst, A.; Ellouzi, M.; Grieger, B.;
Almeida, M.; Besse, S.; Ehrenfreund, P.; Veillet, C.; Burchell, M.;
Stooke, P.
Bibcode: 2019LPI....50.3036F
Altcode:
Celebrating APOLLO legacy after 50 years, we present SMART-1 highlights
relevant for lunar science, exploration, and inspiration towards
Moon Village.
Title: Geology and Astrobiology Research and Data Analysis for Igluna
Authors: Beentjes, D.; de Winter, B.; Heemskerk, M. V.; Foing, B.
Bibcode: 2019LPI....50.2614B
Altcode:
VUSE project is focused on research in/on a glacier: To construct the
history of the glacier and to conduct experiments, simulating a moon
habitat, with IGLUNA.
Title: VUSE Life Science Experiments: Growing Plants in a Moon-Ice
Habitat
Authors: van Bloois, S., J.; de Winter, B.; Foing, B.; Heemskerk,
M.; VU Amsterdam Igluna Team
Bibcode: 2019LPI....50.2415V
Altcode:
VUSE (VU Science Experiments) to test growing plants under dry and
cold conditions for testing the survival of plants inside a glacier.
Title: Subprojects HCAM, RCAM, FDB, and GHIS from the Igluna Project
Authors: Berg, M. J. R.; de Winter, B.; Foing, B. H.; Heemskerk, M. V.
Bibcode: 2019LPI....50.2687B
Altcode:
The subprojects HCAM, RCAM, FDB, and GHIS are part of the IGLUNA
project. This project simulates a habitat on the south pole of the
Moon. Collaboration with ESA.
Title: Igluna Project: Glaciology Research Goals
Authors: Albers, B.; de Winter, B.; Heemskerk, M.; Foing, B.;
Igluna Team
Bibcode: 2019LPI....50.1336A
Altcode:
The IGLUNA project is developing a simulation habitat in ice. In this
habitat, scientific research will take place, for example, glaciology.
Title: Hydrous Alteration of Lava Flows on Mauna Loa (Hawaii)
Compared to Mars Volcanic Soils
Authors: Weert, A. M. P.; Foing, B. H.; Rogers, H.; Musilova, M.;
Gonzalez, Y.
Bibcode: 2019LPI....50.1633W
Altcode:
Samples from Hawaii will be compared to martian rocks, to provide more
insight in the effects of hydrous alteration of volcanic rocks on Mars.
Title: IGLUNA - Habitat in Ice: An ESA_Lab Project Hosted by the
Swiss Space Center
Authors: Heemskerk, M. V.; Benavides, T.; Foing, B. H.; De Winter,
B.; Daeter, M. I.; Beentjes, D.; Kruijver, A.
Bibcode: 2019LPI....50.2416H
Altcode:
IGLUNA is the first ESA_Lab interuniversity demonstrator project,
and is hosted by the SSC with the vision to create an analogue habitat
inside lunar ice caps.
Title: EuroMoonMars Outreach Activities
Authors: Grosjean, M.; Sitnikova, A.; Foing, B.; Preusterink, J.;
De Winter, B.; Heemskerk, M.; Daeter, M.; Berg, M.; Bas Korthouwer,
R.; Vaessen, G.; Van Bloois, S.; Brouwers, I.; Kruijver, A.; Albers,
B.; Gellings, M. C.; Tomic, A.; Beentjes, D.
Bibcode: 2019LPI....50.2414G
Altcode:
EuroMoonMars is an ILEWG program since 2009 gathering projects for
research and field campaigns with young professionals. Here are the
communication activities.
Title: Instruments and Power Supply for Igluna, VU Science Experiments
Authors: Kruijver, A.; Dingemans, A.; Foing, B.; de Winter, B.;
Heemskerk, M.
Bibcode: 2019LPI....50.2869K
Altcode:
A report on the technical necessities for the scientific instruments
and tools used for IGLUNA in Zermatt, Switzerland (June 2019);
VUSE Division.
Title: Smart Ice Lab, ILEWG - Igluna Project
Authors: Sitnikova, A.; Sanden, G. v. d.; Foing, B.; Benavides,
T.; Grosjean, M.; Moritz, D.; Löffler, M.; Dimova, L.; Wanske, A.;
Schlacht, I.
Bibcode: 2019LPI....50.2066S
Altcode:
ILEWG role to facilitate scientific experiments during IGLUNA lunar
mission. IGLUNA is the first ESA_Lab interuniversity demonstrator
project.
Title: Limits of Life and the Habitability of Mars: The ESA Space
Experiment BIOMEX on the ISS
Authors: de Vera, Jean-Pierre; Alawi, Mashal; Backhaus, Theresa;
Baqué, Mickael; Billi, Daniela; Böttger, Ute; Berger, Thomas;
Bohmeier, Maria; Cockell, Charles; Demets, René; de la Torre Noetzel,
Rosa; Edwards, Howell; Elsaesser, Andreas; Fagliarone, Claudia;
Fiedler, Annelie; Foing, Bernard; Foucher, Frédéric; Fritz,
Jörg; Hanke, Franziska; Herzog, Thomas; Horneck, Gerda; Hübers,
Heinz-Wilhelm; Huwe, Björn; Joshi, Jasmin; Kozyrovska, Natalia;
Kruchten, Martha; Lasch, Peter; Lee, Natuschka; Leuko, Stefan; Leya,
Thomas; Lorek, Andreas; Martínez-Frías, Jesús; Meessen, Joachim;
Moritz, Sophie; Moeller, Ralf; Olsson-Francis, Karen; Onofri, Silvano;
Ott, Sieglinde; Pacelli, Claudia; Podolich, Olga; Rabbow, Elke; Reitz,
Günther; Rettberg, Petra; Reva, Oleg; Rothschild, Lynn; Garcia Sancho,
Leo; Schulze-Makuch, Dirk; Selbmann, Laura; Serrano, Paloma; Szewzyk,
Ulrich; Verseux, Cyprien; Wadsworth, Jennifer; Wagner, Dirk; Westall,
Frances; Wolter, David; Zucconi, Laura
Bibcode: 2019AsBio..19..145D
Altcode:
BIOMEX (BIOlogy and Mars EXperiment) is an ESA/Roscosmos space exposure
experiment housed within the exposure facility EXPOSE-R2 outside
the Zvezda module on the International Space Station (ISS). The
design of the multiuser facility supports—among others—the
BIOMEX investigations into the stability and level of degradation of
space-exposed biosignatures such as pigments, secondary metabolites,
and cell surfaces in contact with a terrestrial and Mars analog
mineral environment. In parallel, analysis on the viability of the
investigated organisms has provided relevant data for evaluation of the
habitability of Mars, for the limits of life, and for the likelihood
of an interplanetary transfer of life (theory of lithopanspermia). In
this project, lichens, archaea, bacteria, cyanobacteria, snow/permafrost
algae, meristematic black fungi, and bryophytes from alpine and polar
habitats were embedded, grown, and cultured on a mixture of martian and
lunar regolith analogs or other terrestrial minerals. The organisms and
regolith analogs and terrestrial mineral mixtures were then exposed to
space and to simulated Mars-like conditions by way of the EXPOSE-R2
facility. In this special issue, we present the first set of data
obtained in reference to our investigation into the habitability of
Mars and limits of life. This project was initiated and implemented
by the BIOMEX group, an international and interdisciplinary consortium
of 30 institutes in 12 countries on 3 continents. Preflight tests for
sample selection, results from ground-based simulation experiments,
and the space experiments themselves are presented and include a
complete overview of the scientific processes required for this space
experiment and postflight analysis. The presented BIOMEX concept could
be scaled up to future exposure experiments on the Moon and will serve
as a pretest in low Earth orbit.
Title: Lunar electrical power utility: Key to lunar development
Authors: Beldavs, Vidvuds; Vjaters, Janis; Dunlop, David; Crisafulli,
Jim; Foing, Bernard
Bibcode: 2018EPSC...12..616B
Altcode:
The International Lunar Decade (2020-2030) represents a global
commitment to permanent return to the Moon. This commitment makes
feasible long term projects such as the Lunar Power Utility, which is
intended to accelerate lunar development much as the availability of
electrical power has accelerated economic development on Earth.
Title: Towards the International Lunar Decade
Authors: Beldavs, Vidvuds; Dunlop, David; Crisafulli, Jim; Foing,
Bernard
Bibcode: 2018EPSC...12..268B
Altcode:
The International Lunar Decade 2020-2030 provides a framework
to maximize international benefits from lunar exploration and
development. It is a global program modeled on the International
Geophysical Year of 1957-8
Title: EuroMoonMars 2018 Workshop: Lunar Analogue simulations
Authors: Clavé, Elise; Foing, Bernard; Dubois, Louis; Sanden, Germaine
vd; Krainski, Mateusz; Grulich, Maria; Sitnikova, Anna; Cinelli,
Illaria; Zaklinsky, Alexander; Rodrigues, Jocelino; Michalik, Daniel
Bibcode: 2018EPSC...12..660C
Altcode:
During the annual EuroMoonMars Workshop at ESA/ESTEC, two Lunar
Analogue simulations were held. Three teams were involved: two crews
and the Ground Control Center (GCC). The first simulation was result
oriented, to demonstrate the functioning of different technologies
on the ExoGeoLab lander (robotic test bench), in the ExoHabitat and
in the Exobiology Laboratory. The second simulation was to allow
attendees to discover the concept of analogue simulations or train
them for other campaigns.
Title: EarthMoonMars Village Update 2018
Authors: Foing, Bernard
Bibcode: 2018EPSC...12..602F
Altcode:
We give an update of Moon Village (MV) and EarthMoonMars activities,
with emphasis on events that took place in 2017-2018. The Moon
Village is an open concept proposed with the goal of a sustainable
human and robotic presence on the lunar surface as an ensemble where
multiple users can carry out multiple activities. Multiple goals of
the Moon Village include planetary science, life sciences, astronomy,
fundamental re-search, resources utilisation, human spaceflight,
peaceful cooperation, economical development, inspiration, training
& capacity building.
Title: Ground Control Center during Analogue simulation for
EuroMoonMars 2018 Workshop
Authors: Clavé, Elise; Foing, Bernard; Dubois, Louis; Sanden,
Germaine vd
Bibcode: 2018EPSC...12..673C
Altcode:
During the annual EuroMoonMars Workshop at ESA/ESTEC, two Lunar Analogue
simulations were held. Three teams were involved: two crews and the
Ground Control Center (GCC). The aim of the Ground Control Center is
to assist the crews in their different activities. It requires a very
efficient communication as well as technical experts able to answer
the different questions the crews might have.
Title: EuroMoonMars Workshop 2018: a pilot study on a semi-autonomous
laboratory module for analogue simulations
Authors: van der Sanden, Germaine; Foing, Bernard; Clavé, Elise;
Dubois, Louis
Bibcode: 2018EPSC...12.1247V
Altcode:
EuroMoonMars is a pilot research programme that functions as one of the
small building blocks towards human or robotic habitation of the Moon,
Mars, Phobos, or asteroids. Its annual program is concerned with the
development of its Robotic Test Bench (ExoGeoLab), Habitation module
(Exohab) and Laboratory module (Exolab) at the European Space Research
and Technology Centre of the European Space Agency, Noordwijk, NL
(ESA-ESTEC). EuroMoonMars2018 Laboratory module: The laboratory module
functioned as a sub-system in a bigger-picture with the ExoGeoLab,
the Exohabitat, and the Ground Control Center. The laboratory crew
consisted of a crew commander, scientific officer, biomedical engineer,
food designer and visual artist. The laboratory is a prototype for
functional experimentation.
Title: SpectroLab: a planetary spectroscopic test bench in a Cube
Authors: Clavé, Elise; Foing, Bernard; Dubois, Louis; van der Sanden,
Germaine
Bibcode: 2018EPSC...12...62C
Altcode:
The idea of SpectroLab is to build an easy-to-move test bench, which
could be used in different environments: on a Lunar lander, with a
robotic arm to bring the samples to analyse, or in extra-terrestrial
facilities etc. To do so, the format of SpectroLab is inspired by a
2U CubeSat. It will contain a visible spectrometer, a movable sample
holder, an illumination system and a camera. It will be controllable
remotely a part of the ExoGeoLab lander.
Title: From Westworld to Moon World on Grindhouse Radio
Authors: James, Matthew; Foing, Bernard; Adragna, Kim; Kucmierowski,
William 'Brimstone'; Zambito, Stephen 'Zambo'; Greer, Tom
Bibcode: 2018EPSC...12.1246J
Altcode:
A national radio broadcast featuring space scientist Bernard
Foing, Westworld actress Claire Unabia and artist Matthew
James discussing the possibilities of space travel and MoonMars
Village habitation with Brimstone and the cast of Grindhouse radio.
https://www.iheart.com/podcast/53-The-Grindhouse-Radio-27408283/episode/5-17-18-marty-grabstein-and-the-unabia-29343533/
Title: Pop Culture and Planetary Studies
Authors: James, Matthew; Foing, Bernard
Bibcode: 2018EPSC...12.1227J
Altcode:
We examine the role of man in space through the lens of pop
culture. From the earliest incarnation of science fiction through the
modern-day blockbuster what role does planetary exploration play in
building the myths and dreams of the future?
Title: Global Science Operas: Moon Village (2017), Oceans &
Climate (2018)
Authors: Ben Horin, Oded; Foing, Bernard; Robberstadt, Janne; van
der Sanden, Germaine
Bibcode: 2018EPSC...12.1244B
Altcode:
We shall report the worldwide highlights of GSO 2017 Moon Village. The
Global Science Opera GSO vision is to produce annual Global Science
Opera productions during which a global community will explore
interwoven science, art and technology within a creative and democratic
inquiry process.
Title: Experimental Training and Capacity Building: EuroMoonMars
Workshops and Field Simulations 2016-2018
Authors: Foing, Bernard H.
Bibcode: 2018cosp...42E1085F
Altcode:
The ILEWG/COSPAR EuroMoonMars programme conducted in 2016-2018
a series of workshops and field analogue missions where students
and professionals all over the world became one space crew. Young
professionals joined the team as scientists, engineers or as
education/outreach experts in process of simulating real life and work
on the MoonMars ExoHab and ExoLab laboratories, and in order to develop
experience, training and capacity building. Goals: The EuroMoonMars
mission simulations in ESTEC 2017 and 2018 set a few key goals: First
of all the participants had been developing and testing equipments,
experiments, investigations, and procedures.Secondly they developed
their own communication protocol between the Mission Control Center,
the ExoLab and the ExoHab from both technical and verbal sides aimed to
standardize and facilitate the communication. Thirdly, they performed
evaluation of ergonomics of all units and the equipment needed to
complete the mission. And finally, samples were collected from the
surface for analysis in the MoonMars labs. All above was the subject
of a training program in the process of learning astronaut's daily
performance.
Title: Mars Analogue Samples Lab & Field Spectral Analysis
Authors: Foing, Bernard H.
Bibcode: 2018cosp...42E1083F
Altcode:
We have analysed a set of Mars Analogue samples from field campaigns
and from a petrological collection. We have acquired samples from
Utah Mars Desert Research station, Eifel volcano region, Iceland,
Hawaii, La Reunion and Tenerife. Several spectroscopy analyses in
the UV/VIS spectrum were performed using the remotely controlled
USB4000 spectrometer in the laboratory and during field campaigns. The
EuroMoonMars campaigns were rehearsed at ESTEC for feasibility. We
also used other diagnostic techniques.Spectroscopy of rocks, water,
organics in the lab: The focus of these analyses (Vos et al 2017) was
the detectability of certain elements known to influence the UV/VIS
spectrum such as transitional metals, but also the influence on the
spectrum of minerals, water, organics and volatiles. The influence of
water was measured in accordance with known water absorption bands
at 739 and 836 nm, and mineral or rock analyses signatures. We also
investigated spectral biomarkers.Background on ExoGeoLab lander: The
field spectroscopy was also performed during a campaign in the Eifel
volcanic area in Germany at an outcrop near the Laacher See. The outcrop
consisted of volcanic deposits from the Laacher See eruption from
approximatly 13,000 years ago. During the campaign four analogue EVAs
were performed and we collected geological samples brought to the lander
for remote spectrometry analyses.We thank participants and collaborators
for ILEWG EuroMoonMars 2016, 2017 and 2018 campaigns. References: [0]
Foing B. H. et al. (2011) Special Issue of Inl J of Astrobiology , 10,
IJA.; [1] Ehrenfreund et al. (2011) (IJA 2011, 10 (3), 239; [2] Stoker
C. et al (2011) IJA 2011, 10 (3), 269; [3] Kotler et al. (2011) IJA
2011, 10 (3), 221; [4] Groemer G. et al. (2010) LPSC 41, Abstract 1680
[5] Foing B. H. et al. (2014) LPSC 45, Abstract 2675 [6] Foing B. H. et
al. (2016) LPSC 47, Abstract 2719 [7] Batenburg P. et al. (2016) LPSC
47, Abstract 2798 [8] Offringa M.S.et al (2016) LPSC 47, Abstract 2522;
[9] Kamps O.M..et al (2016) LPSC 47, Abstract 2508
Title: MOON GALLERY : An Educational Program to build Strategies
for implementing An International Art Gallery on the Moon.
Authors: Zaklynsky, Alexander; Foing, Bernard H.; Sitnikova, Anna
Bibcode: 2018cosp...42E3807Z
Altcode:
Introduction - A short History of Art on the Moon:The Moon Museum
is a small ceramic wafer three-quarters of an inchby half an inch in
size. The artists with works in the "museum" are RobertRauschenberg,
David Novros, John Chamberlain, Claes Oldenburg,Forrest Myers and
Andy Warhol.- https://en.wikipedia.org/wiki/Moon_MuseumFallen
Astronaut: 8.5 cm aluminium sculpture by Paul Van Hoeydonck.-
https://en.wikipedia.org/wiki/Fallen_AstronautA Gallery on the Moon
project: Concept:- An international collaborative art work and Moon
villagepromotion structure.- A crowd sourced online gallery of images
created by aninternational group of participants.- A 10 by 10 cm patch
of Lunar Rover exterior paneling isone intended venue for this Gallery.-
A robust online presence, promotion structure and disseminationof
information/teaching materials related to the programalong with the
potential of realising an art work on the moon.Format:A 10 x 10 cm
square can be split into 100 cels of 1 cm x 1 cm.It can be split
into even more equal sizes down to the pixel. Ahi definition 10 x
10 cm printed image could have 1000 x 1000pixels. That is 1 million
pixels. The current initiative is to defineand develop the aesthetic
approach to this structure.Digital Format:Through an online interactive
web platform individuals couldinput their designs into the grid. Over
a set time period andwith multiple submissions from the public a
variation of designscould be collected into an archive representing a
broadspectrum of aesthetic approaches to a set of guidelinesProject
outline/structure:1] Research , concept development, collection of
informative materials.2] Design & Implementation of website &
international call for artisticproposals/submissions.3] Selection
Process of submitted works and management of aestheticorganism
online.4] Potential implementation of gallery on the moon via ESA
lunar roveror other craft destined for the moon.Project Abstract:The
Moon Gallery is a proposal for defining and promoting theevolution
of an aesthetic organism. The three main componentsof this project
are research , collaboration and archive.The Research component is
directed toward the developmentof context , informative materials and
structure for the promotionof a call for artistic submissions. The
Collaborationcomponent is the implementation of the online creative
tooland website designed for collecting submissions and showinga
realtime evolution of the 'aesthetic organism'. The Archivecomponent
is both the dissemination of an online resource ofimages and artist
proposals along with a possibly randomselection of proposals fabricated
into an actual material installationon the moon surface in the 10
x 10 cm grid format.What is an 'aesthetic organism'. A petri dish
is good for growingbacteria cultures while a website is good at
growing visualcultures. The 10 cm x 10 cm grid structure along with
an onlinesignup and submit image structure could develop a largeamount
of submissions over time with good promotion. Eachsection of the grid
relates to both the biological concept ofcells and the understanding
of perspective. As the grid is filledwith more and more input /
imagery, the more it evolves. Overtime an expanding stack of grids
will create a 3d space ofaesthetic intentions. What can we find out
by such a constructionof content. What is there to gain from studying
the outcomesof such a visual social experiment? At the very leastthe
intention of this endeavour is to raise awareness and interestin space
and the moon village project along with attemptingto develop a program
which can have the potential toinspire new explorers of the imagination,
perspective andspace through a collaborative, interactive and evolving
webproject.Additional Information - Current progress:This Initiative
of implementing a strategy for an International Art Gallery on the
Moon is in a preliminary phase of sketching out ideas and methods while
building a resource of information and developing a platform on the web
for an international call to participate. In February 2018 Sitnikova
and Zaklynsky have participated in meetings at Estec with MoonVillage
Colleagues and have begun preparations for collaborations. Sitnikova
and Zaklynsky have initiated the residency with the MoonVillage project
at Estec and will be working at Estec on a weekly basis for the next 6
months to year. We have tentatively scheduled presentations at The Royal
Academy of Art and Willem De Konig Academy to engage younger artists
into the project. We are in Planning stage for developing a series of
presentations and Lectures at Pulchri Studio in Den Haag from May 19
to June 12, 2018. The Moon Gallery Project has been accepted into the
6th European Lunar Symposium in Toulouse, France. We have also begun a
collaboration with the EuroMoonMars Team to develop a test launch of the
general moon gallery project and to explore its physical implementation
and interaction with moon villagers.Connected to the research and
conceptual development of this initiative we are producing a series
of large scale 2 x 2 m paintings which utilise custom built drawing
machines. These paintings will show a study of the grid format mentioned
previously in various abstractions. We will also use these machines to
plot the paths of satellites around the earth with via a collaboration
with computer programmers at Estec. An Exhibition of this work along
with a presentation on the initiatives development will be presented at
Pulchri Studio in Den Haag on the 19th of May and run until June 12th,
2018. - http://pulchri.nl/Other inspirations / conceptual-structural
guides:The Magic Square - https://en.wikipedia.org/wiki/Magic_squareMap
of the moon: - https://moontrek.jpl.nasa.gov/Interactive Web Art Models:
Generative & Crowdsourcing.http://www.thesheepmarket.com/
http://www.swarmsketch.com/Galileo
experiment on the Moon: The Hammer Feather
Drop.https://history.nasa.gov/alsj/a15/a15.clsout3.htmlReferences:[1]
The "Moon Village" Concept and
Initiative.https://www.hou.usra.edu/meetings/leag2016/pdf/5084.pdf[2]
Space is the Place - MoonVillage ArtScience
Residency.http://meetingorganizer.copernicus.org/EPSC2017/EPSC2017-982.pdf[3]
Launch Your Design With Cheops -
Art&Science@ESA.http://blogs.esa.int/artscience/2017/11/02/launch-your-design-with-cheops/
Visual Material:The below images and art work show an evolution in
concepts of perspective and space. The invention of techniques to
aid in the accurate reproductionof our landscape and environment
led to philosophical advancements in concepts of our aesthetic
and spiritual nature on one hand while on the other itled to the
ability of our species to infer a map of the observable universe
we exist in. Our perspective has taken us from the terrestrial to
the celestial whilesolidifying the understanding of our place in
between. The images aim to illustrate the evolution of our human
perspective and our capacity for the explorationof the space within
and around us.[1]Brunelleschi's mirror. Filippo Brunelleschi was
one of the founding fathers of the Renaissance and is generally
known for developing this technique forlinear perspective in art.
https://en.wikipedia.org/wiki/Filippo_Brunelleschihttp://farm5.static.flickr.com/4147/5051886066_86dd4b1b00.jpg[2]Wassily
Kandinsky (Russian, 1866-1944). Thirty (Trente),
1937. Oil on canvas. 31 7/8 x 39 5/16 in. (81 x 100
cm). Musée national d'art moderne, CentrePompidou,
Paris. http://www.wassilykandinsky.net/work-273.php[3]Ellsworth
Kelly, 1951. Spectrum Colors Arranged by Chance II, Collage on paper.
http://www.tate.org.uk/context-comment/articles/sixty-years-full-intensity[4]Sloan
Digital Sky Survey map of the known universe. At this scale, no
stars are visible. Individual galaxies like the Milky Way are also
invisible. Only clusters of galaxies, super clusters and filaments
containing millions of galaxies can be seen. http://www.sdss.org/
Title: Space Fullerenes, PAHs & Diffuse Interstellar Bands
Authors: Foing, Bernard H.
Bibcode: 2018cosp...42E1088F
Altcode:
C60 was discovered in 1985 from a mass spectrometer peak by Kroto,
Curl, Smalley & al, for which they got the Nobel Prize in Chemistry
in 1996. It was then produced in macroscopic quantities by Kratschmer
et al in 1990, that allowed to confirm the structure of soccer ball
geometry, and started a revolution in research and application,
to the delight of chemists, physicists, astronomers, architects
and UEFA-FIFA fans. In 1994 Foing & Ehrenfreund reported the
discovery of two near IR diffuse bands coincident with C60+ bands,
with abundance of up to 0.5 % of cosmic carbon .The interstellar bands
detected at OHP observatory at 9577 and 9632 A were consistent with
C60+ spectra in frozen matrix lab measured in 1992 by D'Hendecourt,
Fostiropoulos and Léger and other groups. The DIBs assignment as C60+,
largest (and most beautiful) interstellar molecule was celebrated by
H. Kroto, and confirmed in subsequent observations (ESO, CFHT, etc.. and
recently by latest near gas phase laboratory experiments.The quest for
fullerenes, PAHs and large organics in space and Diffuse Interstellar
Bands (DIBs) research has advanced since 20 years. DIB observational
surveys, DIB families, correlations and environment dependences,
resolved substructures indicative of rotational contours by large
molecules. DIBs carriers have been linked with large organic molecules
observed in the interstellar medium such as IR bands (assigned to PAHs,
with some new bands detected by Spitzer assigned to fullerenes, Cami
et al 2010 ), Extended Red Emission or recently detected Anomalous
Microwave Emission (AME). Fullerenes and PAHs have been proposed to
explain some DIBs and specific molecules were searched. These could
be present in various dehydrogenation and ionisation conditions, for
example fully dehydrogenated (Vuong, Foing 2000), in a form similar to
graphenes (Nobel prize Physics 2010). Infrared measurements confirm the
presence of vibrational bands of fullerene compounds in circumstellar
environments. Ground based astronomical surveys confirmed the C60+
band detection, and allow to use fullerenes as probes of interstellar
processes and environments. Experiments in the laboratory and in space
(on FOTON BIOPAN, ISS EXPOSE, OREO Cubes) allow to measure the survival
and by-products of these molecules. References: Kroto H. et al 1985,
C60: Buckminsterfullerene. Nature. 318 (6042): 162; Kratschmer W. et
al 1990 Solid C60: a new form of carbon Nature 347, 354 - 358; Foing,
B. Ehrenfreund, P. 1994 Natur 369, 296; Foing, B. Ehrenfreund, P. 1997
AA317, L59; Foing, B. Ehrenfreund, P. 1995 ASSL202, 65; Ehrenfreund,
P., Foing, B. H. 1997 AdSpR19, 1033; Galazutdinov, G. A. et al. 2000
MNRAS317, 750; Tuairisg, S. O. et al. 2000 AAS142, 225; Ruiterkamp,
R. et al. 2005 AA 432, 515; Vuong, M. H. Foing, B. H 2000 AA 363,
L5; Cami J. et al 2010, Science 329; 1180 Bryson, K. L., Peeters, Z.,
Salama, F., Foing, B., Ehrenfreund, P. et al. 2011 AdSpR 48, 1980;
Title: Report to COSPAR PEX from International Lunar Exploration
Working Group (ILEWG) and MoonVillage Workshops
Authors: Foing, Bernard H.
Bibcode: 2018cosp...42E1087F
Altcode:
The International Lunar Exploration Working Group (ILEWG) was
established in April 1995 at a meeting in Hamburg, Germany. As
established in its charter, this working group reports to COSPAR and is
charged with developing an international strategy for the exploration
of the Moon. It discusses coordination between missions, and a road
map for future international lunar exploration and utilisa-tion. It
fosters information exchange or potential and real future lunar robotic
and human missions, as well as for new scientific and exploration
information about the Moon. We give a report on ILEWG community
activities, refer to COSPAR and ILEWG ICEUM and lunar conferences
and declarations [1-18].Ongoing ILEWG priorities from ICEUM 11 and
follow-up events include:1. Science and exploration(recommendations will
be discussed at COSPAR B3.1 Lunar science and exploration session)
2. Technologies and resources - A number of robotic missions to
the Moon are now undertaken independently by various nations, with
a degree of exchange of information and co-ordination. That should
increase towards real co-operation, still allowing areas of competition
for keeping the process active, cost-effective and faster. - Lunar
landers, pressurized lunar rover projects as presented from Europe,
Asia and America are important steps that can create opportunities for
international collaboration, within a coordinated village of robotic
precursors and assistants to crew missions. - We have to think about
development, modernization of existing navigation capabilities, and
provision of lunar positioning, navigation and data relay assets to
support future robotic and human exploration. New concepts and new
methods for transportation have attracted much attention and are of
great potential.3. Infrastructures and human aspects- It is recommended
to have technical sessions and activities dealing with different
aspects of human adaptation to space environments, the modeling of
sub-systems, microbial protection and use of inflatable technologies-
While the Moon is the best and next logical step in human exploration,
we should make best use of the space stations as stepping stones for
exploration and human spaceflight beyond Low Earth Orbit. - Further
research is needed on lunar dust aspects in regard to humans and
interaction with habitats. We note high interest in CELSS for Moon
and Mars bases, and recommend further research and development. - We
recommend the development and use of terrestrial analogues research
sites and facilities, for technology demonstrations, comparative
geology and human performance research, and public engagement. We
endorse the proposal of development of world analogue sites for
international Moon-Mars analogue research.4. Moon, Space, Society and
Young Explorers- We consider that the current legal regime as set out
in the Outer Space Treaty and the Moon agreement are satisfactory for
current and future missions, but may require further clarification for
future exploration. Issues of transparency and security will need to
be addressed.- Great things are happening for Young Lunar Explorers,
with inspiring missions and hands-on activities as coordinated by
ILEWG. Lunar exploration is encouraging students of all ages to pursue
higher education. - More possibilities for participatory engagement
should be offered to the society for example via interdisciplinary
activities with the humanities.- We appreciate the work from COSPAR
panel on Exploration PEX that should be shared further.- Continued
cooperation should be enforced at all levels. The space community
feels strongly that joining the forces of space faring nations to
explore the Moon should be seriously implemented, with the views
of expanding a Global Robotic Village and building in the long run
a Manned International Lunar Base." ILEWG has further integrated
its activities with COSPAR, and developed a series of programmes
to allow exchange of data, payload opportunities, collaborations on
lunar missions, young lunar explorers grants for research projects,
field campaigns and conference participation. ILEWG has also supported
a number of MoonVillage workshops and events in 2016-2018. This will
be reported in PEX1 session concerning the international coordination
of space activities, and in PEX2 concerning the synergy between human
exploration of Moon, Mars & NEOS.References: [1] 1st International
Lunar Workshop, Balsiger H. et al., Editors, European Space Agency,
1994. ESA-SP-1170. [2] 2nd International Lunar Workshop, Kyoto,
H. Mizutani, editor, Japan Space Forum Publisher, 1997. [3] 3rd
International Lunar Workshop, Moscow 1998, E. Galimov, editor. [4]
ICEUM4, ESTEC, 2000, ESA SP-462, B.H. Foing & M. Perry, editors. [5]
ICEUM5, Hawaii Nov 2003, Durst S.M. et al, Editors, Vol 108, 1-576
pp, Science and Technology Series, American Astronautical Society,
2004. [6] ICEUM6, Udaipur 2004, Bhandari N., Editor, Journal Earth
System Science, India, 114, No6, Dec 2005, pp. 573-841. [7] ICEUM7,
Toronto Sept 2005, sci.esa.int/ilewg. [8] ICEUM8, Beijing July 2006,
Journal of Chinese Society of Astronautics, Vol. 28 Sup., 2007, Ji W.,
Editor. [9] ICEUM9, Sorrento, Italy, Foing B., Espinasse S., Kosters G.,
Editors. http://sci.esa.int/iceum9, Dec. 2007), [11] Ehrenfreund, P.,
Foing, B.H., Cellino, A. Editors, The Moon and Near Earth Objects, ASR
Vol 37, 1, 2006. [12] Foing, B.H. et al editors, 'Astronomy and Space
Science from the Moon', ASR 14, 6, 1994. [13] Ip W.-H., Foing, B.H.,
Masson Ph.L., editors, The Moon and Mars, ASR Vol 23, 11, 1999. [14]
Foing, B.H. et al, editor, Lunar Exploration, Plan-etary and Space
Science, Vol 50, 14-15, 2002. [15] Foing, B.H., Heather, D. editors,
'Lunar Exploration 2000', ASR Vol 30, Nr 8, 2002. [16] Huntress,
W. et al 'The next steps in exploring deep space - A cosmic study by
the IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377. [17]
http://sci.esa.int/ilewg/43654-declaration-iceum10-leag-srr-florida-2008/
[18] Ehrenfreund P. et al (COSPAR planetary exploration panel report)
2012, ASR Vol 49, Nr 1, pp. 2-48.
Title: Flash oral presentation of posters ( 2 minutes /posters)
Authors: Foing, Bernard H.
Bibcode: 2018cosp...42E1089F
Altcode:
Flash oral presentation of posters ( 2 minutes /posters)Lunar science
and exploration are having a renaissance with as many as twelve missions
(and 18 vehicles) sent to Moon during the last "International Lunar
decade". This session is aimed at discussing new progress in lunar
science from recent missions, latest science results, newer insight
into our understanding of Moon, modelling and synthesis of different
scientific data, future missions, and science questions. It will include
inv ited, contributed, and poster papers. Papers on new lunar mission
concepts, instrumentation for the future missions, the upcoming lunar
decade of landers and lunar robotic village, and preparations for human
lunar exploration are also welcome in this session. COSPAR-18-B3.1
will also be ICEUM13A, part of the 13th International Conference on
Exploration and Utilisation of the Moon from the ILEWG ICEUM series
started in 1994.
Title: EarthMoonMars Village Worldwide Activities
Authors: Foing, Bernard H.
Bibcode: 2018cosp...42E1086F
Altcode:
We give an update of Moon Village (MV) and MoonMars activities,
with emphasis on events that took place in 2017 and 2018. The Moon
Village is an open concept proposed with the goal of a sustainable
human and robotic presence on the lunar surface as an ensemble where
multiple users can carry out multiple activities. [1-3] .Why a Moon
Village? Multiple goals of the Moon Village include planetary science,
life sciences, astronomy, fundamental research, resources utilisation,
human spaceflight, peaceful cooperation, economical development,
inspiration, training and capacity building.Moon Village 2017
international events:- Global Space Congress Abu Dhabi UAE 30 Jan-1
Feb- UN COPUOS Action team on Exploration 5-7 Feb 2017- UN COSPAR explo
workshop Vienna 25 April, 22 May- European Lunar Symposium & New
Views of Moon , Muenster 2-4 May (HH, CN)- ISDC ST Louis (with ESA
DG J. Woerner) 1-2 June - GLEX Global Exploration Conf Beijing 6-8
June- Concordia U Montreal MVWS 11-12 Aug (M-P B.)- Global Hands on
Universe , Bowling Green 16-17 Aug- Nashville Adventure Sci Center,
Eclipse 19-21 Aug (JI)- EPSC European Planetary Science Congress
Riga, Moon Village Science, Explo. Technology Foresight 18-21 Sep-
Adelaide Australia IAC Intl Astronautical Congress A3 exploration
symposium & plenaries 25-29 Sept- Hawaii International Moon Base
Alliance 1-4 Oct (HR)- Columbia, LEAG Lunar Expl. Analysis Group
10-11 oct - Bremen Space Tech 24-26 Oct - ISU MVA MVWS 19-21 Nov
(GR, CW, JM, AK)- ESLAB ESTEC Extreme Habitable Worlds 4-8 Dec
(ESN)- MoonVillage Global Science Opera (performance over 15
countries including ESTEC event) 13 Dec (O. B.-O.)We shall also
give highlights of 2018 EarthMoonMars Village events.Perspectives:
A number of activities are planned. The EarthMoonMars Village will
rely both on automatic, robotic and human-tendered structures to
achieve sustainable surface operations serving multiple purposes on
an open-architecture basis.*AcknowledgementsWe thank Prof J. Woerner
(ESA DG) for energizing the concept of MoonVillage. *We acknowledge
co-conveners of MoonVillage Workshops and ILEWG EuroMoonMars field
campaigns in 2016, 2017 and 2018 (including C. Jonglez, V.Guinet,
M.Monnerie, A. Kleinschneider, A. Kapoglou, A. Kolodziejczyk,
M. Harasymczuk, I. Schlacht, C. Heinicke, D. Esser, M.Grulich,
T. Siruguet, H.Vos, M.Mirino, D.Sokolsky, J.Blamont, A.Lillo,
P. Evellin, L. Authier, A. Blanc, C. Chahla, A. Tomic, M. Mirino,
I. Schlacht, S. Hettrich, T. Pacher ) and participants to these
events. We thank A.Cowley, C. Haigneré, P. Messina, G. Ortega,
S.Cristoforetti, D. Binns, M. Landgraf, M. Trovatello, ESA colleagues
involved in MoonVillage related activities. We acknowledge organisers of
MoonVillage & related community workshops (identified by initials
in calendar of events and including N.Verschoor, S. Lizy-Destrez,
S. Hettrich, H. Gassabian, J.Cami, V. Foing, J.L.Moro, H. Lakk,
I. Schlacht, I. Sisaid, E.Garcia Bourne, P-A. Joumel, L. Ferreira,
Taisik Lee, J. Silk, A.Decadi, A. Wendler, M. Wilde, T. Pacher,
M-P.Boucher, H.Hiesinger, C. Sallaberger, L. Ming,J. Ivey,
V. Beldavs, H. Rogers, J. Crisafulli , C. Neal, G. Reibaldi,
C. Welch, J. Mankins, A. Kapoglou, E. Sefton-Nash, O. Ben-Horin and
others) . We thank colleagues from ILEWG, Young Lunar Explorers,
the International Lunar Decade Group, the Moon Village Association
and Moon Village International Support Group and "MoonVillagers"
at large. References [1] Jan Wörner, Driving #MoonVillage
http://www.iafastro.org/events/iac/iac-2015/plenaryprogramme/the-moon-a-continent-and-a-gateway-for-ourfuture/
(IAC 2015)
[2]http://www.iafastro.org/events/iac/iac2016/globalnetworking-forum/making-the-moon-village-and-marsjourney-accessible-and-affordable-for-all/
(IAC 2016) ; [3] B. Foing et al , Highlights from
Moon Village Workshop, held at ESTEC in December 2015,
http://www.hou.usra.edu/meetings/lpsc2016/pdf/2719.pdf,
http://www.hou.usra.edu/meetings/lpsc2016/pdf/2798.pdf [4]
P. Ehrenfreund et al. "Toward a Global Space Exploration
Program: A Stepping Stone Approach" (Adv Space Research, 49,
n°1, January 2012), prepared by COSPAR Panel on Exploration
(PEX) [5] http://www.lpi.usra.edu/leag/GER_2011.pdf;
[6] http://sci.esa.int/ilewg/47170-gluc-iceum11-
beijing-2010lunar-declaration/; [7]
http://www.lpi.usra.edu/meetings/leagilewg2008/ [8]
http://sci.esa.int/ilewg/41506-iceum9-sorrento- 2007-lunar-declaration/
[9] National Research Council (2007), The Scientific Context
for Exploration of the Moon [10] P. Ehrenfreund , B.H. Foing,
A. Cellino Editors, The Moon and Near Earth Objects), ASR 37, 1,
pp 1-192, 2006 [11] http://sci.esa.int/ilewg/38863-iceum8-beijing-
2006declaration/[12] W. Huntress, D. Stetson, R. Farquhar,
J. Zimmerman, B. Clark, W. O'Neil, R. Bourke & B. Foing,'The
next steps in exploring deep space - A cosmic study by the
IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377
[13]http://sci.esa.int/ilewg/38178-iceum7-toronto-2005-declaration/
[14] H. Balsiger et al. Eds, Intl Lunar Workshop, 1994 May 31-June
3, Beatenberg, Switzerland. 1994. ESA-SP-1170[15] R.M. Bonnet
et al, 'Mission to the Moon, Europe's Priorities for Scientific
Exploration & Utilisation of the Moon'1992 ESA SP-1150 [16]
http://www.iafastro.org/events/iaf-spring-meetings/spring-meetings-2016/[17]
https://www.spacesymposium.org/[18]
http://www.egu2016.eu/http://meetingorganizer.copernicus.org/EGU2016/session/20378[19]
https://els2016.arc.nasa.gov/[20] https://nesf2016.arc.nasa.gov/[21]
https://www.cospar-assembly.org/abstractcd/COSPAR-16/[22]
https://www.iac2016.org/,[23]
http://www.hou.usra.edu/meetings/leag2016/presentations/[24]
http://newworlds2016.space/[25]
http://www.stx.ox.ac.uk/happ/events/history-moon[26]
https://www.cranfield.ac.uk/events/events-2016/manufacturing-2075#[27-36]
Moon Village talks & workshops at ESA Centres[37-44] Moon Village
workshops organised with community[45] Foing, B. H. 2017, LPI48,
2746[46] Harasymczuk, M. et al 2017, LPI48, 2997[47] Ko_odziejczyk,
A. M et al 2017, LPICo2041, 5069[48] Authier L. et al 2017, LPICo2041,
5071[49] Foing, B. H. et al 2017, LPICo2041, 5073[50] Lillo, A et al
2017, LPICo2041, 5079
Title: Introduction to Lunar Science and Exploration
Authors: Foing, Bernard H.
Bibcode: 2018cosp...42E1084F
Altcode:
This session will address: - Recent lunar results: geochemistry,
geophysics in the context of open planetary science and exploration-
Synthesis of results from SMART-1, Kaguya, Chang'e 1, 2 and 3,
Chandrayaan-1, LCROSS, LADEE, Lunar Reconnaissance Orbiter and,
Artemis and GRAIL- Goals and Status of missions under preparation:
orbiters, Luna-Glob, Google Lunar X Prize, Luna Resurs polar lander,
SLIM, Chandrayaan2, Chang'E 4 and 5, Lunar Resource Prospector,
Future landers, Lunar sample return missions- Precursor missions,
instruments and investigations for landers, rovers, sample return,
and human cis-lunar activities and human lunar surface sorties-
Preparation for International Lunar Decade: databases, instruments,
missions, terrestrial field campaigns, support studies- ILEWG and Global
Exploration roadmaps towards a global robotic/human Moon village -
Strategic Knowledge Gaps, and key science Goals relevant to Lunar Global
Exploration Lunar science and exploration are developing further with
new and exciting missions being developed by China, the US, Japan,
India, Russia, Korea and Europe, and with new stakeholders. Space
exploration builds on international collaboration. COSPAR and its
ILEWG International Lunar Exploration Working Group (created in
1994) have fostered collaboration between lunar missions. A flotilla
of lunar orbiters has flown in the last international lunar decade
(SMART-1, Kaguya, Chang'E 1 and 2, Chandrayaan-1, LCROSS, LRO, GRAIL,
LADEE). Chinese Chang'E 3 lander and Yutu rover. Upcoming other landers
from 2018 (GLXP, Chang'E 4 and 5, SLIM, Luna , LRP) will constitute
a Robotic Village on the Moon.
Title: Synergies and interaction between Space-Architecture, Analogue
habitats & Sustainability
Authors: Van der Sanden, Germaine; Foing, Bernard H.; Dubois, Louis
Bibcode: 2018cosp...42E3502V
Altcode:
According to ESA's Director General Johann-Dietrich Wörner, a habitable
station on the Lunar surface is the next step in reaching more distant
destinations in deep space. Planetary habitats have also been proposed
for Mars, asteroids or even the martian satellite, Phobos. The core
idea of a planetary habitats deals with people working and living
together at the same place. Simultaneously, it's a metaphor for
international collaboration, a global community, which brings multiple
actors together in our endeavors for future space exploration. The
main research question is whether it is possible to form a new three
spherical model that aims to identify the three interacting components,
which constitutes positive human integration in a planetary world. This
research investigates the synergies and intersection between the
following three pillars: I) Space architecture, II) Analogue habitat
experimentation on Earth and III) Sustainability. I) Space Architecture
is a critical component in the development of the lunar habitat. The
interdisciplinary field of Space Architecture draws from a variety of
fields such as engineering, architecture, design, human factor design,
space sciences, medicine, psychology and the arts. Therefore, it is
simultaneously technical, humanistic, scientific and artistic. II)
Analogue habitats are an important extension of the field of Space
Architecture, despite taking microgravity out of the equation. These
missions are designed in extreme environments on Earth, in order
to simulate the physical similarities of a space environment. III)
The creation of a sustainable and livable habitat on a resource-poor
surface can provide the perfect case study to innovate and come up
with creative solutions that will eventually make the Earth a better
place.A three spherical model is created based on the perception of
interconnectivity and system thinking. The aim is to explore whether
these three pillars are critical for positive human integration in the
moon environment, or are too simplistic. We will present a six-month
investigation into the different compartments, how they interact and
how they form a synthesis. These three components are designed in
such a way that they provide feedback loops in order to positively
stimulate each other. At last, new study recommendations are given
for further research and framing of this discourse.
Title: Rationale and concepts for robotic and human outposts on Phobos
Authors: Witasse, Olivier; Foing, Bernard H.; Sefton-Nash, Elliot
Bibcode: 2018cosp...42E3679W
Altcode:
A concept of a permanent station on the martian moons is under
study. Such mission can serve several purposes: (a) positioning system,
(b) data relay stations for Mars surface assets or for interplanetary
missions, (c) monitoring of the Mars environment, (d) scientific
investigations of Mars and its moons, and (e) investigation for
in-situ resources exploitation and precursory human or robotic based
station. It can serve also as a Martian moon and Mars webcam. We show
here a preliminary mission concept, with some applications in the
study of the Mars environment
Title: PEX2 session panel wrap-up
Authors: Foing, Bernard H.
Bibcode: 2018cosp...42E1090F
Altcode:
PEX2 session panel wrap-up The session COSPAR-18-PEX.2: "Human
Exploration on the Moon, Mars and NEOs", co-sponsored by Commissions B,
F will include solicited and contributed talks and poster/interactive
presentations. It will also be part of the 13th International Conference
on Exploration and Utilisation of the Moon ICEUM13B from the ILEWG
ICEUM series started in 1994. It will address various themes and
COSPAR communities: Sci ences (of, on, from) the Moon enabled by
humans; Research from cislunar and libration points; From robotic
villages to international lunar bases; Research from Mars &
NEOs outposts; Humans to Phobos/Deimos, Mars and NEOs; Challenges
and preparatory technologies, field research operations; Human and
robotic partnerships and precursor missions; Resource utilisation,
life support and sustainable exploration; Stakeholders for human
exploration. One half-day session will be dedicated to a workshop
format and meetings/reports of task groups: Science, Technology,
Agencies, Robotic village, Human bases, Moon & Mars Villages,
Society & Commerce, Outreach, Young Explorers. COSPAR has provided
through Commissions, Panels and Working Groups (such as ILEWG, IMEWG)
an international forum for supporting and promoting the robotic and
human exploration of the Moon, Mars and NEOS.
Title: The EDIBLES survey II. The detectability of
C60+ bands
Authors: Lallement, R.; Cox, N. L. J.; Cami, J.; Smoker, J.; Farhang,
A.; Elyajouri, M.; Cordiner, M. A.; Linnartz, H.; Smith, K. T.;
Ehrenfreund, P.; Foing, B. H.
Bibcode: 2018A&A...614A..28L
Altcode: 2018arXiv180200369L
Gas phase spectroscopic laboratory experiments for the
buckminsterfullerene cation C60+ have resulted
in accurate rest wavelengths for five C60+
transitions that have been compared with diffuse interstellar bands
(DIBs) in the near infra-red. Detecting these in astronomical spectra
is difficult because of the strong contamination of ground-based
spectra by atmospheric water vapor, to the presence of weak and
shallow stellar lines and/or blending with other weak DIBs. The
detection of the two strong bands has been claimed by several teams,
and the three additional and weaker bands have been detected in a few
sources. Certain recent papers have argued against the identification
of C60+ based on spectral analyses claiming (i)
a large variation in the ratio of the equivalent widths of the 9632
and 9577 Å bands, (ii) a large redshift of the 9632 Å band for the
Orion star HD 37022, and (iii) the non-detection of the weaker 9428
Å DIB. Here we address these three points: (i) We show that the model
stellar line correction for the 9632 Å DIB overestimates the difference
between the strengths of the lines in giant and dwarf star spectra,
casting doubts on the conclusions about the ratio variability. (ii)
Using high quality stellar spectra from the ESO Diffuse Interstellar
Bands Large Exploration Survey (EDIBLES), recorded with the ESO/Paranal
Ultraviolet Echelle Spectrograph (UVES) in about the same atmospheric
conditions, we find no wavelength shift in the 9632 Å band toward
HD 37022. (iii) Using EDIBLES spectra and data from the Echelle
SpectroPolarimetric Device for the Observation of Stars (ESPaDOnS)
at CFHT we show that the presence of a weak 9428 Å band cannot be
ruled out, even in the same observations that a previous study claimed
it was not present.
Title: The Complex Geomorphology of Neukum Crater on Mars
Authors: Tirsch, Daniela; Jaumann, Ralf; Adeli, Solmaz; Berhardt,
Hannes; Bishop, Janice L.; Fanara, Lida; Gross, Christoph; Gwinner,
Klaus; Hauber, Ernst; Head, James W.; Hiesinger, Harald; Michael,
Gregory; Muller, Jan-Peter; Poulet, Francois; Reiss, Dennis; Williams,
David A.; Pinet, Patrick; Foing, Bernard; McCord, Tom
Bibcode: 2018EGUGA..20.1959T
Altcode:
Neukum Crater, located at about 28°E/45°S at Noachis Terra on
Mars, contains various geomorphological features that indicate a
diverse geological history forming the crater during the past up to
4 Ga years. Most prominent features of this 102 km-crater are the
large dark dune field and the two pits on its floor. The basaltic
composition of the dunes sands, enriched in high-calcium pyroxenes,
does not differ from the overall composition of the dark dunes found
in various places elsewhere on Mars. Avalanches of the dune slip
faces evidence recent seasonal mass movement processes within the
dune field. Aeolian processes also left its traces in the form of
countless dust devil tracks widespread on the crater floor as well as
in the form of transverse aeolian ridges within the pits. These pits,
also found in some neighbouring craters, act as geological windows to
the subsurface and might have contributed as sources of the dark dune
materials of this region. Moraine-like features and mass movements
in smoothed terrain along the crater wall whiteness an era of active
glacial and periglacial processes at Neukum crater. Superposed ejecta
onto these landforms allow determining the minimum age of the features
and constraining the timing of geological processes.
Title: Overview of Moon Village Global Activities & Lunar
Explorers Tribute
Authors: Foing, Bernard
Bibcode: 2018EGUGA..2018534F
Altcode:
The Moon Village is an open concept proposed with the goal of a
sustainable human and robotic pres-ence on the lunar surface as an
ensemble where multiple users can carry out multiple activities. [1-3]
With special tribute to Apollo 16 & 17 astronauts J. Young,
E. Cernan and lunar explorers, we give an update of Moon Village (MV)
activities, with emphasis on events that took place in 2017. Why a Moon
Village? Multiple goals of the Moon Village include planetary science,
life sciences, astronomy, fundamental research, resources utilisation,
human spaceflight, peaceful cooperation, economical development,
inspiration, training & capacity building. How did the Moon
Village start? ESA director general has revitalized and enhanced the
original concept of MoonVillage discussed in the last decade. Space
exploration builds on international collaboration. COSPAR and its
ILEWG International Lunar Exploration Working Group (created in
1994) have fostered collaboration between lunar missions [4-8]. A
flotilla of lunar orbiters has flown in the last international
lunar decade (SMART-1, Kaguya, Chang'E1 &2, Chandrayaan-1,
LCROSS, LRO, GRAIL, LADEE). Chinese Chang'E 3 lander and Yutu
rover. Upcoming other landers from 2018 (GLXP, Chang'E 4 & 5,
SLIM, Luna , LRP) will constitute a Robotic Village on the Moon. In
2017, Moon Village Workshops MVWS or sessions were also conducted at
international symposia or in collaboration with specific universities
or institutes. *Acknowledgements We thank Prof J. Woerner (ESA DG) for
energizing the concept of MoonVillage. *We acknowledge co-conveners
of MoonVillage Workshops and ILEWG EuroMoonMars field campaigns
in 2016 and 2017 (including C. Jonglez, V.Guinet, M.Monnerie,
A. Kleinschneider, A. Kapoglou, A. Kolodziejczyk, M. Harasymczuk,
I. Schlacht, C. Heinicke, D. Esser, M.Grulich, T. Siruguet, H.Vos,
M.Mirino, D.Sokolsky, J.Blamont, A.Lillo, P. Evellin, L. Authi-er,
A. Blanc, C. Chahla, A. Tomic, M. Mirino, I. Schlacht, S. Hettrich,
T. Pacher ) and participants to these events. We thank A.Cowley,
C. Haigneré, P. Messina, G. Ortega, S.Cristoforetti, D. Binns,
M. Landgraf, M. Trovatello, ESA colleagues involved in MoonVillage
related activities. We acknowledge organisers of MoonVillage &
related community workshops (identified by initials in calendar of
events and including N.Verschoor, S. Lizy-Destrez, S. Hettrich,
H. Gassabian, J.Cami, V. Foing, J.L.Moro, H. Lakk, I. Schlacht,
I. Sisaid, E.Garcia Bourne, P-A. Joumel, L. Ferreira, Taisik Lee,
J. Silk, A.Decadi, A. Wendler, M. Wilde, T. Pacher, M-P.Boucher,
H.Hiesinger, C. Sallaberger, L. Ming, J. Ivey, V. Beldavs, H. Rogers,
J. Crisafulli , C. Neal, G. Reibaldi, C. Welch, J. Mankins, A. Kapoglou,
E. Sefton-Nash, O. Ben-Horin and others) . We thank colleagues from
ILEWG, Young Lunar Explorers, the International Lunar Decade Group,
the Moon Village Association and Moon Village International Support
Group and "MoonVillagers" at large.
Title: Time and Light Perception in Analogs in Lunares Habitat
Authors: Kołodziejczyk, A. M.; Harasymczuk, M.; Orzechowski, L.;
Waśniowski, A.; Foing, B.
Bibcode: 2018LPI....49.1862K
Altcode:
Lunares facility is designed to investigate optimal for physiology
and health lighting conditions for future Moon and Mars human space
missions.
Title: GLACE Mission Concept: Ganymede's Life and Curious Exploration
Mission
Authors: Dijkstra, H. E.; van der Sanden, G. A. H. F.; Peters, S.;
Zepper, J.; Branchetti, M.; van Westrenen, W.; Foing, B. H.
Bibcode: 2018LPI....49.1058D
Altcode:
Here we present a concept mission for a third Jovian mission: GLACE
Ganymede's Life and Curious Exploration Mission is a follow-up mission
on the JUICE mission.
Title: The ESO Diffuse Interstellar Band Large Exploration Survey
(EDIBLES)
Authors: Cami, J.; Cox, N. L.; Farhang, A.; Smoker, J.; Elyajouri,
M.; Lallement, R.; Bacalla, X.; Bhatt, N. H.; Bron, E.; Cordiner,
M. A.; de Koter, A. .; Ehrenfreund, P.; Evans, C.; Foing, B. H.;
Javadi, A.; Joblin, C.; Kaper, L.; Khosroshahi, H. G.; Laverick, M.;
Le Petit, F. .; Linnartz, H.; Marshall, C. C.; Monreal-Ibero, A.;
Mulas, G.; Roueff, E.; Royer, P.; Salama, F.; Sarre, P. J.; Smith,
K. T.; Spaans, M.; van Loon, J. T. .; Wade, G.
Bibcode: 2018Msngr.171...31C
Altcode:
The ESO Diffuse Interstellar Band Large Exploration Survey (EDIBLES)
is a Large Programme that is collecting high-signal-to-noise (S/N)
spectra with UVES of a large sample of O and B-type stars covering
a large spectral range. The goal of the programme is to extract a
unique sample of high-quality interstellar spectra from these data,
representing different physical and chemical environments, and to
characterise these environments in great detail. An important component
of interstellar spectra is the diffuse interstellar bands (DIBs),
a set of hundreds of unidentified interstellar absorption lines. With
the detailed line-of-sight information and the high-quality spectra,
EDIBLES will derive strong constraints on the potential DIB carrier
molecules. EDIBLES will thus guide the laboratory experiments necessary
to identify these interstellar “mystery molecules”, and turn DIBs
into powerful diagnostics of their environments in our Milky Way
Galaxy and beyond. We present some preliminary results showing the
unique capabilities of the EDIBLES programme.
Title: Preparing a Lunar Rover Mission in the Framework of Analogue
Planetary Research
Authors: Pacher, T.; Hazadi, M.; Juhász, K.; Pathy, M.; Foing, B.
Bibcode: 2018LPI....49.2282P
Altcode:
Team Puli reports on various APR missions to test its mission planning
and operational procedures, mission hardware prototypes and Mission
Control Software.
Title: OCEANUS Mission Design
Authors: Heemskerk, M. V.; De Zeeuw, G.; Foing, B. H.; Van Westrenen,
W.
Bibcode: 2018LPI....49.1871H
Altcode:
As part of a joint course by ESA at the Vrije Universiteit Amsterdam,
Bsc Geology students designed a mission to Europa, including objectives,
flightplan, payload, budget, etc.
Title: Design and Operations of Environmental Analogs in Lunares
Habitat
Authors: Kołodziejczyk, A. M.; Harasymczuk, M.; Kraiński, M.;
Orzechowski, L.; Waśniowski, A.; de Lillo, A.; Foing, B.
Bibcode: 2018LPI....49.1909K
Altcode:
Establishing habitat Lunares was one of the fastest realization
of this kind in the world. It was created to run lunar and martian
environmental analogs.
Title: Improvements and Telecontrol of the Exogeolab Lander in
Analogue Environments
Authors: Lillo, A.; Foing, B. H.; Van Der Sanden, G.; Dubois, L.;
Clavé, E.; Evellin, P.; Kołodziejczyk, A.; Jonglez, C.; Heinicke,
C.; Harasymczuk, M.; Authier, L.; Blanc, A.; Chahla, C.; Tomic, A.;
Mirino, M.; Schlacht, I.; Hettrich, S.; Pacher, T.
Bibcode: 2018LPI....49.1242L
Altcode:
The ExoGeoLab Lander is a small class prototype deployed at LunAres
analogue station to investigate cooperation between telerobotics and
astronauts' EVAs.
Title: WATER-I Mission Concept: Water-Rich Asteroid Technological
Extraction Research
Authors: Molag, K.; de Winter, B.; Toorenburgh, Z.; Versteegh,
B. G. Z.; van Westrenen, W.; du Pau, K.; Knecht, E.; Borsten, D.;
Foing, B. H.
Bibcode: 2018LPI....49.1950M
Altcode:
The WATER-I mission will be a follow-up of NASA's OSIRIS-REx mission
and aims to extract water from a C-type asteroid to use it as fuel to
return to Earth.
Title: MoonVillage Worldwide Activities: Update for LPSC 2018 and
Apollo 16/17 Tribute
Authors: Foing, B. H.; Kolodziejczyk, A. M.; Heinicke, C.; Lillo,
A.; Schlacht, I.; Kapoglou, A.; Harasymczuk, M.; Verschoor, N.;
Lizy-Destrez, S.; Hettrich, S.; Gassabian, H.; Cami, J.; Foing, V.;
Moro, J. L.; Garcia Bourne, E.; Joumel, P. A.; Ferreira, L.; Lee,
T. S.; Silk, J.; Decadi, A.; Wendler, A.; Wilde, M.; Pacher, T.;
Boucher, M. P.; Ivey, J.; Beldavs, V.; Rogers, H.; Crisafulli, J.;
Reibaldi, G.; Welch, C.; Ben-Horin, O.
Bibcode: 2018LPI....49.1988F
Altcode:
The Moon Village is an open concept for a sustainable surface human
and robotic presence with multiple users. We report on 2017 events,
with special tribute to Apollo 16 and 17.
Title: SMART-1 technology, scientific results and heritage for future
space missions
Authors: Foing, B. H.; Racca, G.; Marini, A.; Koschny, D.; Frew, D.;
Grieger, B.; Camino-Ramos, O.; Josset, J. L.; Grande, M.; Smart-1
Science; Technology Working Team
Bibcode: 2018P&SS..151..141F
Altcode:
ESA's SMART-1 mission to the Moon achieved record firsts such as:
1) first Small Mission for Advanced Research and Technology; with
spacecraft built and integrated in 2.5 years and launched 3.5 years
after mission approval; 2) first mission leaving the Earth orbit using
solar power alone; 3) most fuel effective mission (60 L of Xenon) and
longest travel (13 months) to the Moon!; 4) first ESA mission reaching
the Moon and first European views of lunar poles; 5) first European
demonstration of a wide range of new technologies: Li-Ion modular
battery, deep-space communications in X- and Ka-bands, and autonomous
positioning for navigation; 6) first lunar demonstration of an infrared
spectrometer and of a Swept Charge Detector Lunar X-ray fluorescence
spectrometer; 7) first ESA mission with opportunity for lunar science,
elemental geochemistry, surface mineralogy mapping, surface geology and
precursor studies for exploration; 8) first controlled impact landing
on the Moon with real time observations campaign; 9) first mission
supporting goals of the International Lunar Exploration Working
Group (ILEWG) in technical and scientific exchange, international
collaboration, public and youth engagement; 10) first mission preparing
the ground for ESA collaboration in Chandrayaan-1, Chang' E1 and future
international lunar exploration. We review SMART-1 highlights
and new results that are relevant to the preparation for future lunar
exploration. The technology and methods had impact on space research
and applications. Recent SMART-1 results are relevant to topics on: 1)
the study of properties of the lunar dust, 2) impact craters and ejecta,
3) the study of illumination, 4) radio observations and science from the
Moon, 5) support to future missions, 6) identifying and characterising
sites for exploration and exploitation. On these respective topics,
we discuss recent SMART-1 results and challenges. We also discuss the
use of SMART-1 publications library. The SMART-1 archive observations
have been used to support the goals of ILEWG. SMART-1 has been
useful to prepare for Kaguya, Chandrayaan-1, Chang'E 1, the US Lunar
Reconnaissance Orbiter, the LCROSS impact, future lunar landers and
upcoming missions, and to contribute towards objectives of the Moon
Village and future exploration.
Title: VizieR Online Data Catalog: The ESO DIBs Large Exploration
Survey (Cox+, 2017)
Authors: Cox, N. L. J.; Cami, J.; Farhang, A.; Smoker, J.;
Monreal-Ibero, A.; Lallement, R.; Sarre, P. J.; Marshall, C. C. M.;
Smith, K. T.; Evans, C. J.; Royer, P.; Linnartz, H.; Cordiner, M. A.;
Joblin, C.; van Loon, J. T.; Foing, B. H.; Bhatt, N. H.; Bron, E.;
Elyajouri, M.; de Koter, A.; Ehrenfreund, P.; Javadi, A.; Kaper, L.;
Khosroshadi, H. G.; Laverick, M.; Le Petit, F.; Mulas, G.; Roueff,
E.; Salama, F.; Spaans, M.
Bibcode: 2018yCat..36060076C
Altcode:
We constructed a statistically representative survey sample that probes
a wide range of interstellar environment parameters including reddening
E(B-V), visual extinction AV, total-to-selective extinction
ratio RV, and molecular hydrogen fraction fH2. EDIBLES provides the community with optical (~305-1042nm) spectra
at high spectral resolution (R~70000 in the blue arm and 100000 in the
red arm) and high signal-to-noise (S/N; median value ~500-1000), for a
statistically significant sample of interstellar sightlines. Many of
the >100 sightlines included in the survey already have auxiliary
available ultraviolet, infrared and/or polarisation data on the dust
and gas components. (2 data files).
Title: 2017 EuroMoonMars Analog Habitat Preparation at ESTEC
Authors: Evellin, P.; Foing, B. H.; Lillo, A.; Kołodziejczyk, A.;
Authier, L.; Blanc, A.; Chahla, C.; Tomic, A.
Bibcode: 2017LPICo2041.5075E
Altcode:
The 2017 EuroMoonMars analog habitat aims at testing viable concepts
of laboratories and habitats to optimize the scientific results of the
first crew members of the MoonVillage. The focus is made on developing
and testing breakthrough experiments.
Title: Remote Operation of the ExoGeoLab Lander at ESTEC and
Lunares Base
Authors: Lillo, A.; Foing, B. H.; Evellin, P.; Kołodziejczyk, A.;
Jonglez, C.; Heinicke, C.; Harasymczuk, M.; Authier, L.; Blanc,
A.; Chahla, C.; Tomic, A.; Mirino, M.; Schlacht, I.; Hettrich, S.;
Pacher, T.
Bibcode: 2017LPICo2041.5079L
Altcode:
The ExoGeoLab Lander is a prototype developed to demonstrate joint
use of remote operation and EVA astronaut work in analogue lunar
environment. It was recently deployed in the new analogue base Lunares
in Poland and controlled from ESA ESTEC center.
Title: Logistics for MoonMars Simulation Habitats: ExoHab ESTEC and
LunAres Poland
Authors: Blanc, A.; Authier, L.; Foing, B. H.; Lillo, A.; Evellin,
P.; Kołodziejczyk, A.; Heinicke, C.; Harasymczuk, M.; Chahla, C.;
Tomic, A.; Hettrich, S.
Bibcode: 2017LPICo2041.5072B
Altcode:
ILEWG developed within EuroMoonMars research programme since 2008 a
Mobile Laboratory Habitat (ExoHab) at ESTEC. Its organization led to
logistic concerns our team had to work on. We contributed also to the
installation of LunAres in Poland.
Title: The ESO Diffuse Interstellar Bands Large Exploration Survey
(EDIBLES) . I. Project description, survey sample, and quality
assessment
Authors: Cox, Nick L. J.; Cami, Jan; Farhang, Amin; Smoker, Jonathan;
Monreal-Ibero, Ana; Lallement, Rosine; Sarre, Peter J.; Marshall,
Charlotte C. M.; Smith, Keith T.; Evans, Christopher J.; Royer, Pierre;
Linnartz, Harold; Cordiner, Martin A.; Joblin, Christine; van Loon,
Jacco Th.; Foing, Bernard H.; Bhatt, Neil H.; Bron, Emeric; Elyajouri,
Meriem; de Koter, Alex; Ehrenfreund, Pascale; Javadi, Atefeh; Kaper,
Lex; Khosroshadi, Habib G.; Laverick, Mike; Le Petit, Franck; Mulas,
Giacomo; Roueff, Evelyne; Salama, Farid; Spaans, Marco
Bibcode: 2017A&A...606A..76C
Altcode: 2017arXiv170801429C
The carriers of the diffuse interstellar bands (DIBs) are largely
unidentified molecules ubiquitously present in the interstellar medium
(ISM). After decades of study, two strong and possibly three weak
near-infrared DIBs have recently been attributed to the C60^+
fullerene based on observational and laboratory measurements. There is
great promise for the identification of the over 400 other known DIBs,
as this result could provide chemical hints towards other possible
carriers. In an effort tosystematically study the properties of
the DIB carriers, we have initiated a new large-scale observational
survey: the ESO Diffuse Interstellar Bands Large Exploration Survey
(EDIBLES). The main objective is to build on and extend existing DIB
surveys to make a major step forward in characterising the physical
and chemical conditions for a statistically significant sample of
interstellar lines-of-sight, with the goal to reverse-engineer key
molecular properties of the DIB carriers. EDIBLES is a filler Large
Programme using the Ultraviolet and Visual Echelle Spectrograph at
the Very Large Telescope at Paranal, Chile. It is designed to provide
an observationally unbiased view of the presence and behaviour of
the DIBs towards early-spectral-type stars whose lines-of-sight
probe the diffuse-to-translucent ISM. Such a complete dataset will
provide a deep census of the atomic and molecular content, physical
conditions, chemical abundances and elemental depletion levels for
each sightline. Achieving these goals requires a homogeneous set of
high-quality data in terms of resolution (R 70 000-100 000), sensitivity
(S/N up to 1000 per resolution element), and spectral coverage (305-1042
nm), as well as a large sample size (100+ sightlines). In this first
paper the goals, objectives and methodology of the EDIBLES programme
are described and an initial assessment of the data is provided.
Title: Scientific Outreach of the Lunar Expedition I.0 in the Lunares
Habitat in Poland
Authors: Kołodziejczyk, A. M.; Rudolf, A.; Gocyła, M.; Młyńczak,
M.; Wierzejska, E.; Waśniowski, A.; Davidova, L.; Konorski, P.;
Słonina, M.; Budzyń, D.; Kuźma, J.; Ambroszkiewicz, G.; Harasymczuk,
M.; Foing, B. H.
Bibcode: 2017LPICo2041.5069K
Altcode:
Lunares is a chronobiological laboratory to perform advanced studies
on humans in controlled MoonMars conditions. Results from The Lunar
Expedition I.0 reveal unique properties of the base for future human
spaceflight investigation.
Title: Live from the Moon ExoLab: EuroMoonMars Simulation at
ESTEC 2017
Authors: Neklesa, A.; Foing, B. H.; Lillo, A.; Evellin, P.;
Kołodziejczyk, A.; Jonglez, C.; Heinicke, C.; Harasymczuk, M.;
Authier, L.; Blanc, A.; Chahla, C.; Tomic, A.; Mirino, M.; Schlacht,
I.; Hettrich, S.; Pacher, T.
Bibcode: 2017LPICo2041.5083N
Altcode:
Space enthusiasts simulated the landing on the Moon having pre-landed
Habitat ExoHab, ExoLab 2.0, supported by the control centre on Earth. We
give here the first-hand experience from a reporter (A.N.) who joined
the space crew.
Title: ILEWG EuroMoonMars Research, Technology, and Field Simulation
Campaigns
Authors: Foing, B. H.; Lillo, A.; Evellin, P.; Kołodziejczyk,
A.; Heinicke, C.; Harasymczuk, M.; Authier, L.; Blanc, A.; Chahla,
C.; Tomic, A.; Mirino, M.; Schlacht, I.; Hettrich, S.; Pacher, T.;
Maller, L.; Decadi, A.; Villa-Massone, J.; Preusterink, J.; Neklesa,
A.; Barzilay, A.; Volkova, T.
Bibcode: 2017LPICo2041.5073F
Altcode:
ILEWG developed since 2008, "EuroMoonMars" pilot research with a Robotic
Test Bench (ExoGeoLab) and a Mobile Laboratory Habitat (ExoHab) at
ESTEC. Field campaigns were e.g. in ESTEC, EAC, at Utah MDRS, Eifel,
and LunAres base at Pila Poland in 2017.
Title: MoonMars Astronaut and CapCom Protocols: ESTEC and LunAres
PMAS Simulations
Authors: Authier, L.; Blanc, A.; Foing, B. H.; Lillo, A.; Evellin,
P.; Kołodziejczyk, A.; Heinicke, C.; Harasymczuk, M.; Chahla, C.;
Tomic, A.; Hettrich, S.; PMAS Astronauts
Bibcode: 2017LPICo2041.5071A
Altcode:
ILEWG developed since 2008 a Mobile Laboratory Habitat (ExoHab) at
ESTEC which was tested during a short simulation in July. It was a
foretaste of the PMAS mission on 31 July-14 August in LunAres base at
Pila, with mission control in Torun, Poland.
Title: King on the Moon/King on Mars / Exploring Space - Creating
Space
Authors: Verschoor, N.; Foing, B. H.
Bibcode: 2017EPSC...11..980V
Altcode:
The main goal of the practice 'King on the Moon' and 'King on Mars'
is the search for new areas to discover and to develop. You examine
issues and generate solutions to explore and take possession of new
public/private spaces.
Title: International Lunar Decade Status
Authors: Beldavs, VZ; Crisafulli, J.; Dunlop, D.; Foing, B.
Bibcode: 2017EPSC...11..199B
Altcode:
The International Lunar Decade is a global decadal event designed
to provide a framework for strategically directed international
cooperation for permanent return to the Moon. To be launched July 20,
2019, the 50th anniversary of the giant leap for mankind marked by
Neil Armstrong's first step on the Moon, the ILD launch will include
events around the world to celebrate space exploration, science, and
the expansion of humanity into the Solar System. The ILD framework
links lunar exploration and space sciences with the development of
enabling technologies, infrastructure, means of financing, laws
and policies aimed at lowering the costs and risks of venturing
into space. Dramatically reduced costs will broaden the range of
opportunities available in space and widen access to space for more
states, companies and people worldwide. The ILD is intended to bring
about the efflorescence of commercial business based on space resources
from the Moon, asteroids, comets and other bodies in the Solar System.
Title: Space is the Place - MoonVillage ArtScience Residency
Authors: Foing, B. H.; de Wilde, F.
Bibcode: 2017EPSC...11..982F
Altcode:
Space and Moon-Mars Exploration Through Art offers you a MoonVillage
Artscience Residency workshop dream ticket to ESTEC the technical
heart of ESA, the European Space Agency.
Title: Prelude to MoonVillage: Science and Innovation
Authors: Foing, B. H.
Bibcode: 2017EPSC...11..991F
Altcode:
We shall discuss the science goals, innovation, status of upcoming
missions in the context of elaborating the concept of a Moon Village
with the goal of a sustainable human presence and activity on the
lunar surface .
Title: MoonVillage Technology Foresight Workhop
Authors: Foing, B. H.
Bibcode: 2017EPSC...11..983F
Altcode:
We shall have a Technology foresight workshop in the context of
elaborating the concept of a Moon Village with the goal of a sustainable
human presence and activity on the lunar surface as an ensemble where
multiple users can carry out multiple activities.
Title: Telerobotics control of ExoGeoLab lander instruments
Authors: Lillo, A.; Foing, B. H.
Bibcode: 2017EPSC...11..666L
Altcode:
This document is about the improvement of the autonomy and capabilities
of the prototype lander ExoGeoLab, designed to host remote controlled
instruments for analogue Moon/Mars manned missions. Accent is put on
new exploration capabilities for the lander to reduce the need for EVA.
Title: MoonVillage: Frame & Opportunity for Space Economy
Authors: Foing, B. H.
Bibcode: 2017EPSC...11..990F
Altcode:
We shall discuss the frame and opportunity for space economy in the
context of elaborating the concept of a Moon Village with the goal of
a sustainable human presence and activity on the lunar surface as an
ensemble where multiple users can carry out multiple activities. This
enterprise can federate all interested Nations and partners, in
particular from terrestrial and non space commercial sectors .
Title: MaMBA - a functional Moon and Mars Base Analog
Authors: Heinicke, C.; Foing, B.
Bibcode: 2017EPSC...11..814H
Altcode:
Despite impressive progress in robotic exploration of celestial bodies,
robots are believed to never reach the effectiveness and efficiency of
a trained human. Consequently, ESA proposes to build an international
Moon Village in roughly 15 years and NASA plans for the first manned
mission to Mars shortly after. One of the challenges still remaining
is the need for a shelter, a habitat which allows human spacefarers
to safely live and work on the surface of a celestial body. Although a
number of prototype habitats has been built during the last decades and
inhabited for various durations (e.g. MDRS, FMARS, HI-SEAS, M.A.R.S.),
these habitats are typically equipped for studies on human factors
and would not function in an extraterrestrial environment. Project
MaMBA (Moon and Mars Base Analog) aims to build the first functional
habitat based on the lessons learned from intermediate and long duration
missions at the mentioned habitats. The habitat will serve for testing
technologies like life support, power systems, and interplanetary
communication. Special attention will be given to the development
of the geoscience laboratory module. Crews will live and work inside
the habitat to ensure its functionality.
Title: Earth as a Tool for Astrobiology—A European Perspective
Authors: Martins, Zita; Cottin, Hervé; Kotler, Julia Michelle;
Carrasco, Nathalie; Cockell, Charles S.; de la Torre Noetzel, Rosa;
Demets, René; de Vera, Jean-Pierre; d'Hendecourt, Louis; Ehrenfreund,
Pascale; Elsaesser, Andreas; Foing, Bernard; Onofri, Silvano; Quinn,
Richard; Rabbow, Elke; Rettberg, Petra; Ricco, Antonio J.; Slenzka,
Klaus; Stalport, Fabien; ten Kate, Inge L.; van Loon, Jack J. W. A.;
Westall, Frances
Bibcode: 2017SSRv..209...43M
Altcode: 2017SSRv..tmp...54M
Scientists use the Earth as a tool for astrobiology by analyzing
planetary field analogues (i.e. terrestrial samples and field sites
that resemble planetary bodies in our Solar System). In addition,
they expose the selected planetary field analogues in simulation
chambers to conditions that mimic the ones of planets, moons and Low
Earth Orbit (LEO) space conditions, as well as the chemistry occurring
in interstellar and cometary ices. This paper reviews the ways the
Earth is used by astrobiologists: (i) by conducting planetary field
analogue studies to investigate extant life from extreme environments,
its metabolisms, adaptation strategies and modern biosignatures; (ii)
by conducting planetary field analogue studies to investigate extinct
life from the oldest rocks on our planet and its biosignatures;
(iii) by exposing terrestrial samples to simulated space or
planetary environments and producing a sample analogue to investigate
changes in minerals, biosignatures and microorganisms. The European
Space Agency (ESA) created a topical team in 2011 to investigate
recent activities using the Earth as a tool for astrobiology
and to formulate recommendations and scientific needs to improve
ground-based astrobiological research. Space is an important tool for
astrobiology (see Horneck et al. in Astrobiology, 16:201-243, 2016;
Cottin et al., 2017), but access to space is limited. Complementing
research on Earth provides fast access, more replications and higher
sample throughput. The major conclusions of the topical team and
suggestions for the future include more scientifically qualified
calls for field campaigns with planetary analogy, and a centralized
point of contact at ESA or the EU for the organization of a survey
of such expeditions. An improvement of the coordinated logistics,
infrastructures and funding system supporting the combination of
field work with planetary simulation investigations, as well as an
optimization of the scientific return and data processing, data storage
and data distribution is also needed. Finally, a coordinated EU or ESA
education and outreach program would improve the participation of the
public in the astrobiological activities.
Title: Searching for Interstellar {{\rm{C}}}_{60}^{+} Using a New
Method for High Signal-to-noise HST/STIS Spectroscopy
Authors: Cordiner, M. A.; Cox, N. L. J.; Lallement, R.; Najarro, F.;
Cami, J.; Gull, T. R.; Foing, B. H.; Linnartz, H.; Lindler, D. J.;
Proffitt, C. R.; Sarre, P. J.; Charnley, S. B.
Bibcode: 2017ApJ...843L...2C
Altcode: 2017arXiv170401501C
Due to recent advances in laboratory spectroscopy, the first optical
detection of a very large molecule has been claimed in the diffuse
interstellar medium (ISM): {{{C}}}60+ (ionized
Buckminsterfullerene). Confirming the presence of this molecule
would have significant implications regarding the carbon budget
and chemical complexity of the ISM. Here we present results from a
new method for ultra-high signal-to-noise ratio (S/N) spectroscopy
of background stars in the near-infrared (at wavelengths of 0.9-1
μm), using the Hubble Space Telescope (HST) Imaging Spectrograph
(STIS) in a previously untested “STIS scan” mode. The use
of HST provides the crucial benefit of eliminating the need for
error-prone telluric-correction methods in the part of the spectrum
where the {{{C}}}60+ bands lie and where the
terrestrial water vapor contamination is severe. Our STIS spectrum
of the heavily reddened B0 supergiant star BD+63 1964 reaches an
unprecedented S/N for this instrument (∼600-800), allowing the
detection of the diffuse interstellar band (DIB) at 9577 Å attributed
to {{{C}}}60+, as well as new DIBs in the
near-IR. Unfortunately, the presence of overlapping stellar lines,
and the unexpected weakness of the {{{C}}}60+
bands in this sightline, prevents conclusive detection of the weaker
{{{C}}}60+ bands. A probable correlation
between the 9577 Å DIB strength and interstellar radiation
field is identified, which suggests that more strongly irradiated
interstellar sightlines will provide the optimal targets for future
{{{C}}}60+ searches.
Title: Update from Moon Village Workshops and Studies
Authors: Foing, B. H.
Bibcode: 2017LPICo1988.6043F
Altcode:
We report on Moon Village workshops that gathered multi-disciplinary
professionals to discuss Moon habitat design, science and technology
potentials of the Moon Village, and engaging stakeholders. We also
report studies and activities that followed.
Title: Using Lunar Regolith for Organics: Plant Growth Test Using
Soil Analogues
Authors: Kołodziejczyk, A.; Vos, H. C.; Harasymczuk, M.; Kraiński,
M.; Foing, B. H.
Bibcode: 2017LPICo1988.6041K
Altcode:
Plant development depends on environmental factors such light, humidity
and temperature, seed quality, contaminations, and soil type. We study
the use of lunar regolith simulants from Eifel volcanic region on the
growth of plants.
Title: Traverse velocity maps for human exploration
Authors: Heinicke, Christiane; Johnston, Carmel; Sefton-Nash, Elliot;
Foing, Bernard
Bibcode: 2017EGUGA..19..698H
Altcode:
It is often proposed that humans are more effective and efficient
in conducting exploratory work during planetary missions than
rovers. However, even humans are hindered by the restrictions of
their suits and by necessary precautions to ensure the astronauts'
safety. During the 12-month simulation at the Hawaii Space Exploration
Analog and Simulation facility, several members of the six-person crew
conducted a large number of exploratory expeditions under conditions
similar to a Mars crew. Over the course of 145 extra-vehicular
activities (EVAs), they traversed several thousand kilometers of various
types of terrain. The actual walking speeds of the crew members have
been correlated with different properties of the terrain as determined
from field excursions and remote sensing. The resulting terrain and
velocity maps can be used both for ground truthing of satellite imagery,
and potential EVA planning on celestial bodies.
Title: Introduction to EGU session "Lunar Science and Exploration
Towards Moon Village"
Authors: Foing, Bernard
Bibcode: 2017EGUGA..1912260F
Altcode:
The EGU PS2.2 session "Lunar Science and Exploration" Towards Moon
Village" will address: - Recent lunar results: geochemistry, geophysics
in the context of open planetary science and exploration - Synthesis of
results from SMART-1, Kaguya, Chang'e 1, 2 and 3, Chandrayaan-1, LCROSS,
LADEE, Lunar Reconnaissance Orbiter and, Artemis and GRAIL - Goals
and Status of missions under preparation: orbiters, Luna-Glob, Google
Lunar X Prize, Luna Resurs polar lander, SLIM, Chandrayaan2, Chang'E
4 & 5, Lunar Resource Prospector, Future landers, Lunar sample
return missions - Precursor missions, instruments and investigations
for landers, rovers, sample return, and human cis-lunar activities
and human lunar surface sorties - Preparation for International Lunar
Decade: databases, instruments, missions, terrestrial field campaigns,
support studies - ILEWG and Global Exploration roadmaps towards a
global robotic/human Moon village - Strategic Knowledge Gaps, and key
science Goals relevant to Lunar Global Exploration Lunar science and
exploration are developing further with new and exciting missions being
developed by China, the US, Japan, India, Russia, Korea and Europe,
and with new stakeholders. The Moon Village is an open concept proposed
by ESA DG with the goal of a sustainable human and robotic presence
on the lunar surface as an ensemble where multiple users can carry
out multiple activities. Multiple goals of the Moon Village include
planetary science, life sciences, astronomy, fundamental research,
resources utilisation, human spaceflight, peaceful cooperation,
economical development, inspiration, training and capacity building. ESA
director general has revitalized and enhanced the original concept of
MoonVillage discussed in the last decade. Space exploration builds on
international collaboration. COSPAR and its ILEWG International Lunar
Exploration Working Group (created in 1994) have fostered collaboration
between lunar missions [4-8]. A flotilla of lunar orbiters has flown
in the last international lunar decade (SMART-1, Kaguya, Chang'Eal1
&2, Chandrayaan-1, LCROSS, LRO, GRAIL, LADEE). Chinese Chang'E
3 lander and Yutu rover, and upcoming 2017 other landers from 2017
(GLXP, Chang'E 4 & 5, SLIM, Luna , LRP) will constitute a Robotic
Village on the Moon. A number of MoonVillage talks and/or interactive
jam sessions have been conducted at International workshops and symposia
2016. Moon Village Workshops were held at ESA centres: they were held
with senior experts as well as Young ESA professionals to discuss
general topics and specific issues ( habitat design, technology,
science and precursor missions; public and stakeholder engagement)
. Many workshops were complemented with ILEWG EuroMoonMars simulation
campaigns. Moon Village Workshops or Jam sessions were also conducted at
international symposia or in collaboration with specific universities
or institutes. The PS2.2 session will include invited and contributed
talks as well as a panel discussion and interactive posters with short
oral introduction. Acknowledgements We thank Prof J. Woerner (ESA
DG) for energizing the concept of MoonVillage. We thank co-conveners
of MoonVillage Workshops and ILEWG EuroMoonMars field campaigns in
2016 (including C. Jonglez, V.Guinet, M.Monnerie, A. Kleinschneider,
A. Kapoglou, A. Kolodziejczyk, M. Harasymczuk, I. Schlacht, C. Heinicke,
D. Esser, M.Grulich, T. Siruguet, H.Vos, M.Mirino, D.Sokolsky,
J.Blamont) and participants to these events. We thank A.Cowley,
C. Haigneré, P. Messina, G. Ortega, S.Cristoforetti, ESA colleagues
involved in MoonVillage related activities. We thank colleagues
from ILEWG, Young Lunar Explorers, the International Lunar Decade
Group, the Moon Village Association and Moon Village Support Groups
and "MoonVillagers" at large. [1] Jan Wörner, Driving #MoonVillage
http://www.iafastro.org/events/iac/iac-2015/plenaryprogramme/the-moon-a-continent-and-a-gateway-for-ourfuture/
(IAC 2015, Jerusalem);
[2]http://www.iafastro.org/events/iac/iac2016/globalnetworking-forum/making-the-moon-village-and-marsjourney-accessible-and-affordable-for-all/
(IAC 2016) ; [3] B. Foing et al , Highlights from
Moon Village Workshop, held at ESTEC in December 2015,
http://www.hou.usra.edu/meetings/lpsc2016/pdf/2719.pdf,
http://www.hou.usra.edu/meetings/lpsc2016/pdf/2798.pdf [4]
P. Ehrenfreund et al. "Toward a Global Space Exploration Program:
A Stepping Stone Approach" (Advances in Space Research, 49,
n°1, January 2012), prepared by COSPAR Panel on Exploration
(PEX) [5] http://www.lpi.usra.edu/leag/GER_2011.pdf;
[6] http://sci.esa.int/ilewg/47170-gluc-iceum11-
beijing-2010lunar-declaration/; [7]
http://www.lpi.usra.edu/meetings/leagilewg2008/
[8] http://sci.esa.int/ilewg/41506-iceum9-sorrento-
2007-lunar-declaration/ [9] National Research Council (2007), The
Scientific Context for Exploration of the Moon [10] P. Ehrenfreund ,
B.H. Foing, A. Cellino Editors, The Moon and Near Earth Objects),
Advances in Space Research, Volume 37, Issue 1, pp 1-192,
2006 [11] http://sci.esa.int/ilewg/38863-iceum8-beijing-
2006declaration/ [12] W. Huntress, D. Stetson, R. Farquhar,
J. Zimmerman, B. Clark, W. O'Neil, R. Bourke& B. Foing,'The
next steps in exploring deep space - A cosmic study by the
IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377
[13]http://sci.esa.int/ilewg/38178-iceum7-toronto-2005-declaration/
[14] H. Balsiger et al. Eds, International Lunar Workshop, 1994 May
31-June 3, Beatenberg, Switzerland. Proceedings. Ed. European Space
Agency, 1994. ESA-SP-1170 [15] R.M. Bonnet et al, 'Mission to the
Moon, Europe's Priorities for Scientific Exploration and Utilisation
of the Moon', European Space Agency, ESA SP-1150, June 1992 [16]
http://www.iafastro.org/events/iaf-spring-meetings/spring-meetings-2016/
[17] https://www.spacesymposium.org/ [18] http://www.egu2016.eu/
http://meetingorganizer.copernicus.org/EGU2016/session/20378 [19]
https://els2016.arc.nasa.gov/ [20] https://nesf2016.arc.nasa.gov/
[21] https://www.cospar-assembly.org/abstractcd/COSPAR-16/
[22] https://www.iac2016.org/, [23]
http://www.hou.usra.edu/meetings/leag2016/presentations/
[24] http://newworlds2016.space/ [25]
http://www.stx.ox.ac.uk/happ/events/history-moon [26]
https://www.cranfield.ac.uk/events/events-2016/manufacturing-2075#
Title: Proposal MaMBA - Moon and Mars Base Analog
Authors: Heinicke, Christiane; Foing, Bernard
Bibcode: 2017EGUGA..19..572H
Altcode:
Despite impressive progress in robotic exploration of celestial bodies,
robots are believed to never reach the effectiveness and efficiency of
a trained human. Consequently, ESA proposes to build an international
Moon Village in roughly 15 years and NASA plans for the first manned
mission to Mars shortly after. One of the challenges still remaining
is the need for a shelter, a habitat which allows human spacefarers
to safely live and work on the surface of a celestial body. Although
various prototype habitats have been built and inhabited during the
last decade, they typically share two fundamental flaws: First, they
usually consist of a single space, which may become uninhabitable after
depressurization due to just one single catastrophic event. Second,
none of the habitats provides shielding against radiation, one of
the major health concerns for spacefaring crews. Project MaMBA will
address these two problems at the root and build an underground habitat
comprised of five connected, but independent modules. The habitat will
serve for testing technologies like life support, power systems, and
interplanetary communication. Special attention will be given to the
development of the geoscience laboratory module. In addition to the
technological aspects, the envisioned habitat will serve as a unique
test ground for studies on the effects of underground habitation on
a crew.
Title: Analogue Simulation of human and psychosocial factors for
MoonMars bases
Authors: Davidová, Lucie; Foing, Bernard
Bibcode: 2017EGUGA..19.1092D
Altcode:
Several courageous plans regarding future human space exploration have
been proposed. Both main future targets, ESA's Moon village, as well
as journey to Mars represent huge challenge for humans. Appropriate
research on psychological aspects of humans in extreme conditions
is needed. Analogue simulations represent valuable source of
information that help us to understand how to provide an adequate
support to astronauts in specific conditions of isolation and limited
resources. The psychosocial investigation was designed to builds on
combination of several methods based on subjective as well as objective
assessments, namely observation, sociomapping, content analysis of
interviews etc. Research on several simulations provided lessons
learned and various insights. The attention was paid particularly
to the interpersonal interactions among crew members, intragroup as
well as intergroup communication, cooperation, and performance. This
comprehensive approach enables early detection of hidden structures
and potential insufficiencies of an astronaut team. The sociomapping
of interpersonal communication as well as analysis of interviews with
participants revealed insufficiencies especially in communication
between the analogue astronauts and mission control. Another important
finding was gain by investigation of the relationship between the
astronaut crew and mission control. Astronauts low trust to mission
control can have a great negative impact to the performance and
well-being of astronauts. The findings of the psychosocial studies
are very important for designing astronaut training and planning
future mission.
Title: MoonMars Base in Poland: a Simulation Habitat and Laboratory
for Research
Authors: Kolodziejczyk, Agata; Gocyla, Michal; Harasymczuk, Matt;
Krainski, Mateusz; Nawrot, Adam; Orzechowski, Leszek; Wszolek, Bogdan;
Vos, Heleen; Foing, Bernard
Bibcode: 2017EGUGA..19.1601K
Altcode:
Analog simulation missions are notable steps of real space exploration
missions, where the hardware, along with the psychological behavior, the
scientific and geological experiments, and operations, are scrutinized
and conducted in a simulated environment to prepare astronauts and
space agencies for actual missions. Here we present the newly built
MoonMars base in Poland to investigate human-robotic relations during
long-term planetary missions. We apply novel tele-medicine solutions,
novel architecture design, life-sustaining systems and novel methods
of planning and working to simulate not only "the beginning of life"
in the habitat but also "a need to transform". The aim of the project
is to facilitate and to speed up development of space education in
Europe. Particularly, we are interested to enroll students, engineers
and PhD students for realization of their individual projects in the
frame of their master and doctoral programmes.
Title: VIS/NIR reflectance and fluorescence spectrometric studies of
minerals, water, organics and biomarkers in MoonMars analogue samples
Authors: Vos, Heleen; Foing, Bernard; Kołodziejczyk, Agata; Vago,
Jorge; Harasymczuk, Matt
Bibcode: 2017EGUGA..19.1537V
Altcode:
This study focuses on the detection and characterisation of elements,
minerals, volatiles and organics using reflectance spectrometry. The
goal is to create a calibration method to enable the use of
spectrometers on analogue Moon/Mars missions and on a lander. For this
study we use measurements that are done in the VIS and NIR spectrum,
as well as fluorescence using different spectrometers. The first
part of the study consists of measurements that are performed in a
laboratory to create a calibration method. Different rock samples and
soils are analysed and the reflectance and absorption of minerals,
water, organics and biomarkers are measured. Also the influence of
the grain size, light source and surroundings is being determined. An
experiment on the reflectance spectra of plant growth in different soils
is also done to determine the possibilities of detecting the presence
of chlorophyll and other biomarkers, and to diagnose the growth and
health of a plant. This analysis can result in a monitoring method for
a Moon greenhouse, but also for general surface analysis. Using VIS and
NIR spectrometry has a couple of advantages, one being the fact that
measurements require no sample preparation, and also the small size
of the spectrometer makes it an easy tool for different analyses on
board space missions. However, VIS and NIR spectroscopy have detection
limits which makes only certain characteristics detectable. Besides
laboratory measurements, the different spectroscopy methods are tested
during a field campaign in the Eifel, Germany. During this campaign
we can determine the functionality of the spectrometer in the field
and on a lander and the problems that can rise when a spectrometer is
controlled from a distant or by a person who is not trained in using
spectroscopy. These laboratory and field measurements can help in
the scientific preparation for instruments on ExoMars rover, future
MoonMars lander missions and for the MoonVillage.
Title: Laboratory Spectroscopy of Minerals, Water, Organics,
and Biomarkers
Authors: Vos, H. C.; Kołodziejczyk, A.; Harasymczuk, M.; Vargo, J.;
Foing, B. H.
Bibcode: 2017LPI....48.2419V
Altcode:
Results from laboratory spectroscopy in the UV/VIS spectrum of minerals,
water, and organics.
Title: Operational Issues for Geological Analog Simulation EVA at
Eifel Volcanic Region: ILEWG EuroMoonMars
Authors: Harasymczuk, M.; Foing, B. H.; Kołodziejczyk, A.; Vos,
H.; Krainski, M.; Davidová, L.; Mirino, M.; Casini, A.; Eifel ILEWG
Euromoonmars 2016 Team
Bibcode: 2017LPI....48.2997H
Altcode:
During EVA simulations in Eifel area, ESA and ILEWG collaborators
tested the human-robotic partnership, EVA procedures, and schedule
for geological sampling.
Title: Field Spectroscopy, Imaging, and Sampling at the Eifel
MoonMars Analogue
Authors: Vos, H. C.; Harasymczuk, M.; Kołodziejczyk1, A.; Krainski,
M.; Davidová, L.; Mirino, M.; Casini, A.; Foing, B. H.
Bibcode: 2017LPI....48.2359V
Altcode:
Comparison of field spectroscopy data in the UV/VIS spectrum with
laboratory spectroscopy data to improve future field analyses.
Title: Moon Village Activities Update
Authors: Foing, B. H.; Jonglez, C.; Guinet, V.; Monnerie, M.;
Kleinschneider, A. M.; Kapoglou, A.; Kolodziejczyk, A.; Harasymczuk,
M.; Schlacht, I.; Heinicke, C.; Esser, D.; Vos, H.; Siruguet, T.;
Sokolsky, D.; Cowley, A.; Moon Village Workshops Co-Organisers
Bibcode: 2017LPI....48.2746F
Altcode:
We give an update on Moon Village open concept towards sustainable
human and robotic activities on the lunar surface with multiple use
by multiple users.
Title: Exploration of Planetary Crusts: A Human/Robotic Exploration
Design Reference Campaign to the Lunar Orientale Basin
Authors: Head, J. W.; Pieters, C.; Scott, D.; Johnson, B.; Potter,
R.; Hoffman, J.; Foing, B.; Zelenyi, L.; Mitrofanov, I.; Marov, M.;
Basilevsky, A.; Ivanov, M.; Jaumann, R.; Xiao, L.; Haruyama, J.;
Ohtake, M.; Senthil Kumar, P.; Aharonson, O.
Bibcode: 2017LPICo1989.8170H
Altcode:
By 2050 we need to be working on fundamental scientific problems in an
integrated fashion to provide insights into early planetary processes
by exploring and characterizing the crust of the Moon.
Title: The "Moon Village" Concept and Initiative
Authors: Woerner, J.; Foing, B.; Moon Village International Support
Group
Bibcode: 2016LPICo1960.5084W
Altcode:
ESA is elaborating the concept of a Moon Village with the goal of a
sustainable human presence and activity on the lunar surface as an
ensemble where multiple users can carry out multiple activities.
Title: Towards a Moon Village : Community Workshops Highlights
Authors: Foing, Bernard H.
Bibcode: 2016cosp...41E.610F
Altcode:
A series of Moon Village Workshops were organised at ESTEC and at ILEWG
community events in 2015 and 2016. They gathered a multi-disciplinary
group of professionals from all around the world to discuss their ideas
about the concept of a Moon Village, the vision of ESA's Director
General (DG) Jan Woerner of a permanent lunar base within the next
decades [1]. Three working groups focused on 1) Moon Habitat Design; 2)
science and technology potentials of the Moon Village, and 3) engaging
stake-holders [2-3]. Their results and recommendations are presented
in this abstract. The Moon Habitat Design group identified that the
lunar base design is strongly driven by the lunar environment, which is
characterized by high radiation, meteoroids, abrasive dust particles,
low gravity and vacuum. The base location is recommended to be near the
poles to provide optimized illumination conditions for power generation,
permanent communication to Earth, moderate temperature gradients at
the surface and interesting subjects to scientific investigations. The
abundance of nearby available resources, especially ice at the dark
bottoms of craters, can be exploited in terms of In-Situ Resources
Utilization (ISRU). The identified infrastructural requirements include
a navigation, data- & commlink network, storage facilities and
sustainable use of resources. This involves a high degree of recycling,
closed-loop life support and use of 3D-printing technology, which
are all technologies with great potential for terrestrial spin-off
applications. For the site planning of the Moon Village, proven ideas
from urban planning on Earth should be taken into account. A couple of
principles, which could improve the quality of a long-term living milieu
on the Moon, are creating spacious environments, visibility between
interior and exterior spaces, areas with flora, such as gardens and
greenhouses, establishing a sustainable community and creating social
places for astronauts to interact and relax. The proposed establishment
of the lunar base can be divided into 4 steps. First the primary
base infrastructure is laid out through robotic missions, assisted
by human tele-operations from Earth, from the lunar orbit, or via a
human-tended gateway station in one of the Earth-Moon Lagrange points
(EML-1/2). During the second phase, the first manned habitation module
will be deployed. This module contains a bare minimum of functionality
to support a small crew for a couple of months. During the third phase,
additional modules with more dedicated functions will be sent to the
Moon, in order to enhance functionality and to provide astronauts with
more space and comfort for long-term missions. In the final phase of
the lunar village, a new set of modules will be sent to the base in
order to accommodate new arriving crew members. To ensure crew safety,
the landing site for supply vessels shall be located in safe distance to
the base. Extensive utilization of autonomous or tele-operated robots
further minimizes the risk for the crew. From the very beginning,
quickly accessible emergency escape vehicles, as well as a heavily
shielded 'safe haven' module to protect the crew from solar flares,
shall be available. Sustainable moon village development would require
explorers to fully utilize and process in-situ resources, in order to
manufacture necessary equipment and create new infrastructure. Mining
activities would be performed by autonomous robotic systems and managed
by colonists from the command center. Building upon the heritage of
commercial mining activities on Earth the production would be divided
into six stages: geological exploration and mapping, mine preparation,
extraction of raw resources, processing of raw resources, separation
of minerals, storage and utilization. Additional manufacturing
techniques, such as forging, would also need to be explored so as
not to limit the production capabilities. To facilitate the progress
of the Moon Village initiative it is necessary to attract private
industry investments. Potential sources range from technology testing
in the moon environment and private R&D funding from science
and academia fields, to space tourism, and more ambitious endeavors
such as building a prototype launcher site as a ground segment for
debris de-orbiting and satellite recycling activities. The Science
and Technology team has identified key technologies and possible major
scientific disciplines for a Moon Village and ranked them by importance
and by Technology Readiness Level (TRL). In terms of basic technologies
and objectives, rover exploration, life support systems, navigation
and surveying technologies resulted to have the highest importance and
readiness. Technologies for the development of the habitats (materials,
modules connections, power supply, alternative energy technologies
and energy storage) ended up on having high importance with medium-low
technology readiness. Technologies intended to help the astronauts or
improve techniques had low-medium importance together with low-medium
TRL (e.g. space lift to transfer resources, bio cybernetic augmentation
"Exoskeleton", jumping rover, telescope). After brainstorming for
required technologies, the focus was shifted to what kinds of science
can be expected to be performed, once a functional and usable habitat
would be available. The group has categorized studies of planetary
formation and the Solar System as a highly important scientific
discipline with a medium-high TRL. Scientific areas with high-medium
importance, but low technological readiness, were found to be ISRU,
psychological effects, adaptations of life to low gravity and plant
cultivation. The physiological effects of low-gravity on the body were
considered of medium importance and readiness. The Engaging Stakeholders
working group started by identifying the main stakeholders and groups
that play a role or that could play a role towards the Moon Village
project. These stakeholders were classified on their influence towards
the program and their attitude towards it. Complex system innovations
like the Moon Village initiative often encounter stiff resistance from
intended beneficiaries and stakeholders, because they disrupt existing
behaviors, organizational structures and business models. However, if
this large-scale change is rather approached as two simultaneous and
parallel challenges - the design of the artifact in question and the
design of the intervention that brings it to life - the chances that it
will take hold will increase. Finally, the group recommended actions
to be taken by the ESA DG to engage the most direct stakeholders: The
general public should be addressed on an emotional level, human centered
design thinking and social movement design should be used to engage the
civic society. When engaging with the Moon Village stakeholders, the
emotional resonance of Moon Village's value proposition should be taken
into account as much as its scientific and technical requirements. This
involves (social) media, art and humanities and, for the long term,
also investments on education. In this way, a social excitement similar
as for the Apollo program might be triggered, which can be used by the
member states to engage with their national politicians and convince
their taxpayers of the Moon Village's benefits. ESA should invest on
the creation of a European new Space industry (similar to the one in the
U.S.) and therefore simplify their processes in order to make it easier
for the industry to invest and work with ESA with less bureaucracy. In
order to succeed in this large-scale international collaboration,
a political & legal framework needs to be established. It is
recommended to push for an International Moon Village Treaty agreement
at the U.N. and to start a conversation about the Moon Village at the
UNCOPUOS, so the delegations and member states can start providing ESA
with their political and legal inputs. The aim should be to present
a sound concept already at the ESA ministerial 2016. Conclusion:
Since a long-term human presence in the cis-lunar and lunar surface
environment is envisaged, human factors become an even more crucial
element in defining the success of the missions. Therefore, it is
very important that not only a set of technical problems is solved
to survive the harsh environment on the Moon. It is also necessary
that psychological and physiological factors will be considered in
the design of the systems, equipment and habitats. In that light, the
Moon Habitat Design group noticed a missing link between the currently
developed space technologies and the actual long-term usability by
astronauts. It is therefore critical that ESA would collaborate more
with urban planners, architects and industrial designers who provide
the expertise in creating suitable environments and products, which
are not only technically sound and functional, but also easy to use,
comfortable and aesthetically pleasing. The Science and Technology group
has in general analyzed the key challenges, technologies, objectives
and issues related to the development of a manned colony on the moon,
classifying them from an importance vs. Technology Readiness Level (TRL)
point of view. The Engaging Stakeholders working group has identified
the main stakeholders and groups that could play a role towards the
Moon Village project. These stake-holders were classified on their
influence towards the program, and their attitude towards it. One
clear conclusion was that most of the stakeholders showed a positive
view towards the Moon Village program, and that the most important
step within a short term strategy should focus on the actions to be
taken to engage stakeholders for the next ESA Ministerial to support
the program. Finally, the group came up with some recommendations
on which actions should be taken by the ESA DG to invite partners
and to engage the most direct stakeholders: ESA delegations,
media, national governments, citizens and taxpayers. References:
[1] http://sci.esa.int/ilewg/ and https://ildwg.wordpress.com/ [2]
Foing B. Moon exploration highlights and Moon Village introduction. [3]
Young Lunar Explorers Report ESTEC Moon village sessions with community
and young professionals.
Title: Eifel field operation campaign supporting Moon Mars and
NEO exploration
Authors: Kamps, Oscar; Foing, Bernard H.; Offringa, Marloes
Bibcode: 2016cosp...41E.931K
Altcode:
As follow-up on the 2009 Eifel field campaign new field tests with our
ExoGeoLab lander were conducted in November 2015 and February 2016. The
two phase campaign was used to test the usability of a mock-up lander
as test bench for experiments and its remote control in a Moon, Mars
analogue environment. In a real mission such a lander could be used in a
robotic or manned mission as scientific tool for scientists on Earth to
do preliminary study on in-situ collected rocks. This could be useful
for example for a sample return mission where scientists on Earth can
determine if sample is interesting enough for a more detailed study. The
prototype lander is one of the components of the ExoGeoLab project from
ESA and ILEWG. Several student projects have prepared the lander for
a geological field campaign in lunar and Martian analogue terrain. The
lander can be divided in three sections which are used to store several
components of the lander. The lower compartment can be used to store
a rover or used as laboratory. The middle compartment is used for the
lander computer(s), spectrometers and the associated cables. The top
plate is used for a telescope which in our case is used to observe the
environment around the lander and to guide astronauts during their
EVA. As closest volcanic are there is chosen to do the Eifel area,
Germany. Several stages of volcanism from Devon till Quaternary resulted
in a variation of rocks which is analogue to volcanic rocks from Moon,
Mars and other near Earth objects. Several topics we would like to
test were pre-defined. Functional tests and demo were performed at
European astronaut centre prior to the campaign. The latest updates with
respect to the remote control were tested. The pressurised transport
vehicle was equipped as remote base for (scientific) support during
the campaign. The new instrument set-up were tested and some spectra
were measured on collected rocks. The telescope was used to study the
environment around the lander, selecting sites of interest for EVA,
and as support for astronauts on both safety as science. From this
campaign some lessons were learned and are points of improvement for
future campaigns. One of the most important is to make the whole lander
more robust. Several times some systems were not working correctly and
someone had to repair. To make it more self-contained a stable cable
system and power supply is needed. The new set-up of the spectrometer
and sample holder seemed to work fine with the sun as illumination
source. For future campaigns there should be a good artificial source
as alternative or complement for solar illumination. The telescope
provided a good image with a lot of details of the volcanic ash
stratigraphy, but we have experienced the importance for a wider view
to have a better understanding of the context of the telescope view. An
alternative for an ad-hoc network is preferred. Four computers and two
networks seemed to interfere which made it impossible to use systems
on the lander at the same time. With the share screen function there
was some delay in controlling the computer. Next campaign we would
like to have the remote support separated from the field location so
the people which have to support astronauts have no understanding of
the area. Acknowledgment: We would like to thank people from ESTEC ,
EAC, and DLR for their support during the campaign.
Title: Human factors for the Moon: the gap in anthropometric data.
Authors: Lia Schlacht, Irene; Foing, Bernard H.; Rittweger, Joern;
Masali, Melchiorre; Stevenin, Hervé
Bibcode: 2016cosp...41E1743L
Altcode:
Since the space era began, we learned first to survive and then to live
in space. In the state of the art, we know how important human factors
research and development is to guarantee maximum safety and performance
for human missions. With the extension of the duration of space
missions, we also need to learn how habitability and comfort factors
are closely related to safety and performance. Humanities disciplines
such as design, architecture, anthropometry, and anthropology are
now involved in mission design from the start. Actual plans for
building a simulated Moon village in order to simulate and test Moon
missions are now being carried out using a holistic approach, involving
multidisciplinary experts cooperating concurrently with regard to the
interactions among humans, technology, and the environment. However,
in order to implement such plans, we need basic anthropometrical data,
which is still missing. In other words: to optimize performance,
we need to create doors and ceilings with dimensions that support
a natural human movement in the reduced gravity environment of the
Moon, but we are lacking detailed anthropometrical data on human
movement on the Moon. In the Apollo missions more than 50 years
ago, no anthropometrical studies were carried in hypogravity out as
far as we know. The necessity to collect data is very consistent
with state-of-the-art research. We still have little knowledge of
how people will interact with the Moon environment. Specifically,
it is not known exactly which posture, which kind of walking and
running motions astronauts will use both inside and outside a Moon
station. Considering recent plans for a Moon mission where humans
will spend extensive time in reduced gravity conditions, the need for
anthropometric, biomechanics and kinematics field data is a priority
in order to be able to design the right architecture, infrastructure,
and interfaces. Objective of this paper: Bring knowledge on the
relevance of anthropometrical and human factors contribution Present the ongoing research on this field Share innovative
methodologies in order to acquire feedback from other specialist. This research is aimed at reconsidering the methodologies from
the viewpoint of anthropometry and human system interaction in a
different kind of gravity and carry out new investigations that
may help to prepare for the next Moon mission, but which can also
be used for advanced applications on Earth. Experimental setups and
methodologies for achieving anthropometrical data will be described. In
particular, combined studies involving bed rest, treadmills, parabolic
flight, neutral buoyancy, and weight suspension with cables will be
presented. From a spin-off perspective, this research is also extremely
promising in terms of basic research aimed at better understanding
human physiological mechanisms ruling equilibrium, deambulation,
and related topics, which are also useful for applications on Earth.
Title: Mars Analogue Field Research and Sample Analysis
Authors: Foing, Bernard H.
Bibcode: 2016cosp...41E.611F
Altcode:
We describe results from the data analysis from a series of field
research campaigns (ILEWG EuroMoonMars campaigns 2009 to 2016) in
the Utah desert and in other extreme environments (Iceland, Eifel,
La Reunion) relevant to habitability and astrobiology in Mars
environments, and in order to help in the interpretation of Mars
missions measurements from orbit (MEX, MRO) or from the surface
(MER, MSL). We discuss results relevant to the scientific study
of the habitability factors influenced by the properties of dust,
organics, water history and the diagnostics and characterisation of
microbial life. We also discuss perspectives for the preparation of
future lander and sample return missions. We deployed at Mars Desert
Research station, Utah, a suite of instruments and techniques including
sample collection, context imaging from remote to local and microscale,
drilling, spectrometers and life sensors. We analyzed how geological and
geochemical evolution affected local parameters (mineralogy, organics
content, environment variations) and the habitability and signature of
organics and biota. We find high diversity in the composition of soil
samples even when collected in close proximity, the low abundances
of detectable PAHs and amino acids and the presence of biota of all
three domains of life with significant heterogeneity. An extraordinary
variety of putative extremophiles was observed. A dominant factor
seems to be soil porosity and lower clay-sized particle content. A
protocol was developed for sterile sampling, contamination issues,
and the diagnostics of biodiversity via PCR and DGGE analysis in soils
and rocks samples. We compare campaign results from 2009-2013 campaigns
in Utah and other sites to new measurements concerning: the comparison
between remote sensing and in-situ measurements; the study of minerals;
the detection of organics and signs of life.
Title: Traverses for lunar rovers and sample return teleoperated
from Earth or cislunar orbit
Authors: Kamps, Oscar; Foing, Bernard H.; Flahaut, Jessica
Bibcode: 2016cosp...41E.930K
Altcode:
Most interesting sites for exploration are near the poles of the
Moon where water and other ices and volatiles could be stable in the
permanent shaded regions. Several instruments on multiple orbiters have
indicated the presence of hydrogen or hydration but the relation with
the illumination conditions are not as clear. Which other variables
are involved to trap water near the poles is not known. This ignorance
makes it of high interest to do in-situ research on the Moon. ESA,
NASA and other agencies are studying a teleoperated mission from
cislunar orbit with Orion (eg. HERACLES international lunar exploration
architecture) with the possibility of long rover traverses, and human
assisted sample return. This mission concept was used for this study
on a rover traverse. This study focuses on both the North as South
Pole. The site selection for a traverse was based on the temperature map
from Diviner. Regions of interests were made as primary selection and
cover areas where the maximum temperature is lower than the sublimation
temperature of CO2. Data from neutron spectrometer from the Prospector,
and crater epoch according to the USGS were used to make a selection
of regions of interest. These selected sites where studied on their
accessibility for a rover, based on the slope map made from the LOLA
elevation model. A landing site was selected based on assumptions that
it should be at least one kilometre in diameter and have a slope lower
than 5 degrees. The temperature difference (Tmax-Tmin from the Diviner
measurements) was used select a scientifically interesting site between
the landing site and destination inside a PSR. It was thought that a
site with a temperature difference larger than 150K is interesting
to study volatile migration processes. Eventually for the traverse
planning a tool in ArcGIS was used which calculates the easiest from one
location to another where the slope is used as limiting factor. We give
the example study of rover traverse planning done for Rozhdestvenskiy
West and Amundsen crater which were both selected as most interesting
and most suitable for an in-situ, tele-operated, sample return mission.
Title: Laboratory and Field Spectroscopy of Moon analogue material
Authors: Offringa, Marloes; Foing, Bernard H.
Bibcode: 2016cosp...41E1456O
Altcode:
Samples derived from terrestrial analogue sites are studied to
gain insight into lunar processes in their geological context
(Foing, Stoker, Ehrenfreund, 2011). For this study samples from the
volcanic region of the Eifel, Germany collected during our latest
field campaigns in November 2015 and February 2016 (Foing et al.,
2010), are analyzed with a variety of spectrometers. The aim is
to obtain a database of analyzed samples that could be used as a
reference for future in situ measurements. We also use a documented
set of Moon-Mars relevant minerals curated at VU Amsterdam. We are
using systematically for all samples UV-VIS and NIR reflectance
spectrometers, and sporadically a Fourier Transform Infrared (FTIR)
spectrometer, an X-Ray Fluorescence (XRF) spectrometer and a Raman
laser spectrometer on control samples. Calibration of the UV-VIS and
NIR reflectance spectrometers is the main focus of this research in
order to obtain the clearest spectra. The calibration of the UV-VIS and
NIR reflectance spectrometers requires the use of a good light source
as well as suitable optical fibers to create a signal that covers the
widest range in wavelengths available. To eliminate noise towards the
edges of this range, multiple measurements are averaged and data is
processed by dividing the signal by reference spectra. Obtained spectra
can be tested for accuracy by comparing them with stationary laboratory
spectrometers such as the FTIR spectrometer. The Raman, UV-VIS and NIR
are also used in combination with the ExoGeoLab mock-up lander during
field campaigns (Foing, Stoker, Ehrenfreund, 2011) also brought again
to Eifel in February 2016, to prove the applicability of the equipment
in the field. Acknowledgements: we thank Dominic Doyle for ESTEC optical
lab support, Euan Monaghan (Leiden U) for FTIR measurement support, Wim
van Westrenen for access to VU samples, Oscar Kamps (Utrecht U./ESTEC),
Aidan Cowley (EAC) and Matthias Sperl (DLR) for support discussions
Title: Community Report and Recommendations from International Lunar
Exploration Working Group (ILEWG)
Authors: Foing, Bernard H.
Bibcode: 2016cosp...41E.615F
Altcode:
The International Lunar Exploration Working Group (ILEWG) was
established in April 1995 at a meeting in Hamburg, Germany. As
established in its charter, this working group reports to COSPAR
and is charged with developing an international strategy for
the exploration of the Moon. It discusses coordination between
missions, and a road map for future international lunar exploration
and utilisation. It fosters information exchange or potential and
real future lunar robotic and human missions, as well as for new
scientific and exploration information about the Moon. We refer
to COSPAR and ILEWG ICEUM and lunar conferences and declarations
[1-18], present the GLUC/ICEUM11 declaration and give a report on
ongoing relevant ILEWG community activities. ILEWG supported community
forums, ILEWG EuroMoonMars field campaigns and technology validation
activities, as well as Young Lunar Explorers events, and activities
with broad stakeholders. We discuss how lunar missions SMART-1, Kaguya,
Chang'E1&2, Chandrayaan-1, LCROSS, LRO, GRAIL, LADEE, Chang'E3 and
upcoming missions contribute to lunar exploration objectives &
roadmap towards the Moon Village. GLUC/ICEUM11 declaration: "467
International Lunar Explorers, registered delegates from 26 countries,
assembled at GLUC Global Lunar Conference including the 11th ILEWG
Conference on Exploration and Utilisation of the Moon (ICEUM11) in
Beijing. The conference engaged scientists, engineers, enthusiast
explorers, agencies and organisations in the discussion of recent
results and activities and the review of plans for exploration. Space
agencies representatives gave the latest reports on their current
lunar activities and programmes. GLUC-ICEUM11 was a truly historical
meeting that demonstrated the world-wide interest in lunar exploration,
discovery, and science. More than 400 abstracts were accepted for oral
and poster presentations in the technical sessions, organised in 32
sessions within 4 symposia: Science and Exploration; Technology and
Resource Utilisation; Infrastructure and Human aspects; Moon, Space
and Society. The latest technical achievements and results of recent
missions (SMART-1, Kaguya, Chang'E1, Chandrayaan-1, LCROSS and LRO)
were discussed at a plenary panel and technical sessions, with the
Lunar Reconnaissance Orbiter (LRO) still in operation. Chang'E1 has
generated many useful results for the community. Four plenary panel
sessions were conducted: 1. What are the plans? 2. New mission results;
3. From space stations and robotic precursors to lunar bases; 4. Moon,
Space, Society The participants summarised their findings, discussions
and recommend o continue efforts by agencies and the community on
previous ICEUM recommendations, and the continuation of the ILEWG
forum, technical groups activities and pilot projects. 1. Science and
exploration - World-wide access to raw and derived (geophysical units)
data products using consistent formats and coordinate systems will
maximize return on investment. We call to develop and implement plans
for generation, validation, and release of these data products. Data
should be made available for scientific analysis and supporting
the development and planning of future missions - There are still
Outstanding Questions: Structure and composition of crust, mantle, and
core and implications for the origin and evolution of the Earth-Moon
system; Timing, origin, and consequences of late heavy bombardment;
Impact processes and regolith evolution; Nature and origin of volatile
emplacement; Implications for resource utilization. These questions
require international cooperation and sharing of results in order
to be answered in a cost-effective manner - Ground truth information
on the lunar far side is missing and needed to address many important
scientific questions, e.g. with a sample return from South Pole- Aitken
Basin - Knowledge of the interior is poor relative to the surface, and
is needed to address a number of key questions, e.g. with International
Lunar Network for seismometry and other geophysical measurements -
Lunar missions will be driven by exploration, resource utilization,
and science; we should consider minimum science payload for every
mission, e.g., landers and rovers should carry instruments to determine
surface composition and mineralogy - It is felt important to have a
shared database about previous missions available for free, so as to
provide inputs to future missions, including a gap analysis of needed
measurements. Highly resolved global data sets are required. Autonomous
landing and hazard avoidance will depend on the best topographic map
of the Moon, achievable by combining shared data. - New topics such
as life sciences, partial gravity processes on the Moon should be
followed in relation to future exploration needs. 2. Technologies
and resources - A number of robotic missions to the Moon are now
undertaken independently by various nations, with a degree of exchange
of information and coordination. That should increase towards real
cooperation, still allowing areas of competition for keeping the process
active, cost-effective and faster. - Lunar landers, pressurized lunar
rover projects as presented from Europe, Asia and America are important
steps that can create opportunities for international collaboration,
within a coordinated village of robotic precursors and assistants to
crew missions. - We have to think about development, modernization of
existing navigation capabilities, and provision of lunar positioning,
navigation and data relay assets to support future robotic and human
exploration. New concepts and new methods for transportation have
attracted much attention and are of great potential. 3. Infrastructures
and human aspects - It is recommended to have technical sessions and
activities dealing with different aspects of human adaptation to space
environments, the modeling of sub-systems, microbial protection and
use of inflatable technologies - While the Moon is the best and next
logical step in human exploration, we should make best use of the space
stations as stepping stones for exploration and human spaceflight
beyond Low Earth Orbit. - Further research is needed on lunar dust
aspects in regard to humans and interaction with habitats. We note
high interest in CELSS for Moon and Mars bases, and recommend further
research and development. - We recommend the development and use of
terrestrial analogues research sites and facilities, for technology
demonstrations, comparative geology and human performance research,
and public engagement. We endorse the proposal of development of a site
at La Reunion for international Moon-Mars analogue research. 4. Moon,
Space, Society and Young Explorers - We consider that the current
legal regime as set out in the Outer Space Treaty and the Moon
agreement are satisfactory for current and future missions, but
may require further clarification for future exploration. Issues of
transparency and security will need to be addressed. - Great things
are happening for Young Lunar Explorers, with inspiring missions
and hands-on activities as coordinated by ILEWG. Lunar exploration
is encouraging students of all ages to pursue higher education. -
More possibilities for participatory engagement should be offered
to the society for example via interdisciplinary activities with the
humanities. - We appreciate the work from COSPAR panel on Exploration
PEX that should be shared further. - Continued cooperation should
be enforced at all levels. The space community feels strongly that
joining the forces of space faring nations to explore the Moon should
be seriously implemented, with the views of expanding a Global Robotic
Village and building in the long run a Manned International Lunar
Base. - We propose that a panel be formed through ILEWG with the help
of IAF and Chinese Society of Astronautics in cooperation with space
agencies, COSPAR and other stakeholders in order to initiate a permanent
International Space Exploration Governance Forum We, the participants
of the GLUC-ICEUM11 conference, commit to an enhanced global
cooperation towards international lunar exploration for the benefit of
humankind. Endorsed by the delegates of GLUC-ICEUM11" References: [1]
1st International Lunar Workshop, Balsiger H. et al., Editors, European
Space Agency, 1994. ESA-SP-1170. [2] 2nd International Lunar Workshop,
Kyoto, H. Mizutani, editor, Japan Space Forum Publisher, 1997. [3]
3rd International Lunar Workshop, Moscow 1998, E. Galimov, editor. [4]
ICEUM4, ESTEC, 2000, ESA SP-462, B.H. Foing & M. Perry, editors. [5]
ICEUM5, Hawaii Nov 2003, Durst S.M. et al, Editors, Vol 108, 1-576
pp, Science and Technology Series, American Astronautical Society,
2004. [6] ICEUM6, Udaipur 2004, Bhandari N., Editor, Journal Earth
System Science, India, 114, No6, Dec 2005, pp. 573-841. [7] ICEUM7,
Toronto Sept 2005, sci.esa.int/ilewg. [8] ICEUM8, Beijing July 2006,
Journal of Chinese Society of Astronautics, Vol. 28 Sup., 2007, Ji W.,
Editor. [9] ICEUM9, Sorrento, Italy, Foing B., Espinasse S., Kosters G.,
Editors. http://sci.esa.int/iceum9, Dec. 2007), [11] Ehrenfreund, P.,
Foing, B.H., Cellino, A. Editors, The Moon and Near Earth Objects, ASR
Vol 37, 1, 2006. [12] Foing, B.H. et al editors, 'Astronomy and Space
Science from the Moon', ASR 14, 6, 1994. [13] Ip W.-H., Foing, B.H.,
Masson Ph.L., editors, The Moon and Mars, ASR Vol 23, 11, 1999. [14]
Foing, B.H. et al, editor, Lunar Exploration, Planetary and Space
Science, Vol 50, 14-15, 2002. [15] Foing, B.H., Heather, D. editors,
'Lunar Exploration 2000', ASR Vol 30, Nr 8, 2002. [16] Huntress,
W. et al 'The next steps in exploring deep space - A cosmic study by
the IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377. [17]
http://sci.esa.int/ilewg/43654-declaration-iceum10-leag-srr-florida-2008/
[18] Ehrenfreund P. et al (COSPAR planetary exploration panel report)
2012, ASR Vol 49, Nr 1, pp. 2-48.
Title: COSPAR-16-B0.1/ICEUM12A: Lunar Exploration and Science
Authors: Foing, Bernard H.
Bibcode: 2016cosp...41E.612F
Altcode:
Lunar science and exploration are having a renaissance with as many
as twelve missions (and 18 vehicles) sent to Moon during the last
"International Lunar decade". This session is aimed at discussing new
progress in lunar science from recent missions, latest science results,
newer insight into our understanding of Moon, modelling and synthesis of
different scientific data, future missions, and science questions. It
will include invited, contributed, and poster papers. Papers on new
lunar mission concepts, instrumentation for the future missions,
the upcoming lunar decade of landers and lunar robotic village, and
preparations for human lunar exploration towards a "Moon Village" are
also welcome in this session. COSPAR-16-B0.1 will also be ICEUM12A,
part of the 12th International Conference on Exploration and Utilisation
of the Moon from the ILEWG ICEUM series started in 1994.
Title: Human Exploration on the Moon, Mars and NEOs: PEX.2/ICEUM12B
Authors: Foing, Bernard H.
Bibcode: 2016cosp...41E.613F
Altcode:
The session COSPAR-16-PEX.2: "Human Exploration on the Moon, Mars
and NEOs", co-sponsored by Commissions B, F will include solicited
and contributed talks and poster/interactive presentations. It will
also be part of the 12th International Conference on Exploration and
Utilisation of the Moon ICEUM12B from the ILEWG ICEUM series started in
1994. It will address various themes and COSPAR communities: - Sciences
(of, on, from) the Moon enabled by humans - Research from cislunar and
libration points - From robotic villages to international lunar bases
- Research from Mars & NEOs outposts - Humans to Phobos/Deimos,
Mars and NEOS - Challenges and preparatory technologies, field research
operations - Human and robotic partnerships and precursor missions -
Resource utilisation, life support and sustainable exploration -
Stakeholders for human exploration One half-day session will be
dedicated to a workshop format and meetings/reports of task groups:
Science, Technology, Agencies, Robotic village, Human bases, Society
& Commerce, Outreach, Young Explorers. COSPAR has provided
through Commissions, Panels and Working Groups (such as ILEWG, IMEWG)
an international forum for supporting and promoting the robotic and
human exploration of the Moon, Mars and NEOS. Proposed sponsors :
ILEWG, ISECG, IKI, ESA, NASA, DLR, CNES, ASI, UKSA, JAXA, ISRO, SRON,
CNSA, SSERVI, IAF, IAA, Lockheed Martin, Google Lunar X prize, UNOOSA
Title: Fullerenes, Organics and the Diffuse Interstellar Bands
Authors: Foing, Bernard H.
Bibcode: 2016cosp...41E.614F
Altcode:
The status of DIB research has strongly advanced since 20 years
[1], as well as the quest for fullerenes, PAHs and large organics in
space. In 1994 we reported the discovery of two near IR diffuse bands
coincident with C60+, confirmed in subsequent years [2-6] and now by
latest laboratory experiments. A number of DIB observational studies
have been published, dealing with: DIB surveys [1,7-10]; measurements
of DIB families, correlations and environment dependences [11-14];
extragalactic DIBs [15, 16]. Resolved substructures were detected
[17,18] and compared to predicted rotational contours by large molecules
[19]. Polarisation studies provided upper limits constraints [20,
21]. DIBs carriers have been linked with organic molecules observed in
the interstellar medium [22-25] such as IR bands (assigned to PAHs),
Extended Red Emission or recently detected Anomalous Microwave Emission
(AME, assigned to spinning dust) and with spectroscopic IR emission
bands measured with ISO or Spitzer. Fullerenes and PAHs have been
proposed to explain some DIBs and specific molecules were searched
in DIB spectra [eg 2-6, 26-31]. These could be present in various
dehydrogenation and ionisation conditions [32,33]. Experiments in the
laboratory and in space [eg 34-36] allow to measure the survival and
by-products of these molecules. We review DIB observational results
and their interpretation, and discuss the presence of large organics,
fullerenes, PAHs, graphenes in space. References [1] Herbig, G. 1995
ARA&A33, 19; [2] Foing, B. & Ehrenfreund, P. 1994 Natur 369,
296; [3] Foing, B. & Ehrenfreund, P. 1997 A&A317, L59; [4]
Foing, B. & Ehrenfreund, P. 1995 ASSL202, 65; [5] Ehrenfreund,
P., Foing, B. H. 1997 AdSpR19, 1033; [6] Galazutdinov, G. A. et
al. 2000 MNRAS317, 750; [7] Jenniskens, P., Desert, F.-X. 1994
A&AS106, 39; [8] Ehrenfreund, P. et al. 1997 A&A318, L28;
[9] Tuairisg, S. Ó. et al. 2000 A&AS142, 225; [10] Cox, N. et
al. 2005 A&A438, 187; [11] Cami, J. et al. 1997A&A.326, 822;
[12] Krelowski, J. et al. 1999A&A 347, 235; [13] Sonnentrucker,
P., Cami, J., Ehrenfreund, P., Foing, B. H. 1997 A&A 327, 1215;
[14] Sonnentrucker, P., Foing, B. H., Breitfellner, M., Ehrenfreund,
P. 1999 A&A 346, 936; [15] Cox, N. et al. 2007 A&A 470, 941;
[16] Ehrenfreund, P. et al. 2002 ApJ 576 L117; [17] Ehrenfreund,
P.; Foing, B. H. 1996 A&A 307 L25; [18] Sarre, P. J. et al. 1995
MNRAS.277 L41; [19] Cossart-Magos, C. & Leach, S. 1990 A&A 233,
559; [20] Cox, N. L., Ehrenfreund, P., Foing, B. H. et al. 2011 A&A
531, 25; [21] Cox, N. L., Boudin, N., Foing, B. H. et al. 2007 A&A
465, 899; [22] Ehrenfreund, P. & Charnley, S. 2000 ANRAA 38, 427;
[23] Scarrott, S. M., Watkin, S., Miles, J. R., Sarre, P. J. 1992
MNRAS 255, 11; [25] Planck Collaboration, 2011 A&A 536 20 (Planck
early results. XX.); [26] Ehrenfreund, P. et al. 1995 A&A 299;
213; [27] Ehrenfreund, P. & Foing, B. H 1995 P&SS 43, 1183;
[28] van der Zwet, G. P., Allamandola, L. J. 1985 A&A 146 76; [29]
Salama, F. et al. 1996 ApJ 458, 621; [30] Ruiterkamp, R. et al. 2005
A&A 432, 515; [31] Ruiterkamp, R. et al. 2002 A&A 390, 1153;
[32] Vuong, M. H. & Foing, B. H 2000 A&A 363, L5; [33] Le
Page, V. et al 2001 ApJS 132, 233; [34] Ehrenfreund, P et al. 2007
P&SS 55, 383; [35] Bryson, K. L., Peeters, Z., Salama, F., Foing,
B., Ehrenfreund, P. et al. 2011 AdSpR 48, 1980; [36] Mattioda, A.,
Cook, A., Ehrenfreund, P. et al. 2012 AsBio 12, 841.
Title: Lunar Polar Landing Sites
Authors: Kamps, Oscar; Foing, Bernard H.; Flahaut, Jessica
Bibcode: 2016cosp...41E.932K
Altcode:
An important step for a scientific mission is to assess on where the
mission should be conducted. This study on landing site selection
focuses on a mission to the poles of the Moon where an in-situ mission
should be conducted to answer the questions with respect to volatiles
and ices. The European interest for a mission to the poles of the Moon
is presented in the mission concept called Heracles. This mission
would be a tele-operated, sample return mission where astronauts
will controlling a rover from an Orion capsule in cislunar orbit. The
primary selection of landing sites was based on the scientific interest
of areas near the poles. The maximum temperature map from Diviner was
used to select sites where CO^2¬ should always be stable. This means
that the maximum temperature is lower than 54K which is the sublimation
temperature for CO^2¬ in lunar atmospheric pressure. Around these areas
14 potential regions of interest were selected. Further selection was
based on the epoch of the surface in these regions of interest. It was
thought that it would be of high scientific value if sites are sampled
which have another epoch than already sampled by one of the Apollo
or Luna missions. Only 6 sites on both North as South Pole could
contain stable CO^2 ¬and were older than (Pre-)Necterian. Before
a landing site and rover traverse was planned these six sites were
compared on their accessibility of the areas which could contain
stable CO^2. It was assumed that slope lower than 20^o is doable to
rove. Eventually Amundsen and Rozhdestvenskiy West were selected as
regions of interest. Assumptions for selecting landing sites was that
area should have a slope lower than 5^o, a diameter of 1km, in partial
illuminated area, and should not be isolated but inside an area which is
in previous steps marked as accessible area to rove. By using multiple
tools in ArcGIS it is possible to present the area's which were marked
as potential landing sites. The closest potential landing site to a PSR
was chosen and used to do an automatic calculation for a rover traverse
where the slope was assumed to be the limiting factor. Between the
landing site and PSR a site of interest was chosen where temperature
differences (Tmax-Tmin) is higher than 150K to study volatile migration
processes. Eventually it is concluded that Amundsen is preferred above
Rozhdestvesnkiy West because its flatter crater ground makes it easier
to select landing sites. It contains more areas where volatile migration
processes can studied and it is easier to rove.
Title: Laboratory spectroscopy of Mars Analogue materials and latest
field results from Iceland and Eifel
Authors: Offringa, Marloes; Foing, Bernard H.
Bibcode: 2016cosp...41E1458O
Altcode:
We have established a collection of samples, and measured them in
the laboratory towards a spectrometric database that could be used
as a reference for future orbital or in situ measurements. We are
using systematically for all samples UV-VIS and NIR reflectance
spectrometers, and sporadically a Fourier Transform Infrared (FTIR)
spectrometer, an X-Ray Fluorescence (XRF) spectrometer and a Raman
laser spectrometer on control samples. We also used a documented set of
Moon-Mars relevant minerals curated at VU Amsterdam, as well as samples
retrieved from Mars analogue campaigns in Utah (Foing et al., 2011,
2016), Iceland (Mid-Atlantic ridge spreading and magma-ice interaction),
La Réunion hot spot volcano and Eifel volcanic region (mixed hotspot
and melt-ascent through crust fractures) from recent campaigns in
2015 and 2016.. We discuss samples spectral diagnostics of volcanic
processes and hydrous alterations that can inform recent or upcoming
measurements from Mars orbit or in situ rovers. Acknowledgements:
we thank Dominic Doyle for ESTEC optical lab support, Euan Monaghan
(Leiden U) for FTIR measurement support, Wim van Westrenen for access
to VU samples, Oscar Kamps (Utrecht U), Aidan Cowley (EAC) and Matthias
Sperl (DLR) for support discussions
Title: Moon-Mars simulation campaign in volcanic Eifel: Remote
science support and sample analysis
Authors: Offringa, Marloes; Foing, Bernard H.; Kamps, Oscar
Bibcode: 2016cosp...41E1457O
Altcode:
Moon-Mars analogue missions using a mock-up lander that is part of
the ESA/ILEWG ExoGeoLab project were conducted during Eifel field
campaigns in 2009, 2015 and 2016 (Foing et al., 2010). In the last
EuroMoonMars2016 campaign the lander was used to conduct reconnaissance
experiments and in situ geological scientific analysis of samples, with
a payload that mainly consisted of a telescope and a UV-VIS reflectance
spectrometer. The aim of the campaign was to exhibit possibilities
for the ExoGeoLab lander to perform remotely controlled experiments
and test its applicability in the field by simulating the interaction
with astronauts. The Eifel region in Germany where the experiments
with the ExoGeoLab lander were conducted is a Moon-Mars analogue due
to its geological setting and volcanic rock composition. The research
conducted by analysis equipment on the lander could function in
support of Moon-Mars sample return missions, by providing preliminary
insight into characteristics of the analyzed samples. The set-up of the
prototype lander was that of a telescope with camera and solar power
equipment deployed on the top, the UV-VIS reflectance spectrometer
together with computers and a sample webcam were situated in the middle
compartment and to the side a sample analysis test bench was attached,
attainable by astronauts from outside the lander. An alternative light
source that illuminated the samples in case of insufficient daylight
was placed on top of the lander and functioned on solar power. The
telescope, teleoperated from a nearby stationed pressurized transport
vehicle that functioned as a base control center, attained an overview
of the sampling area and assisted the astronauts in their initial
scouting pursuits. Locations of suitable sampling sites based on these
obtained images were communicated to the astronauts, before being
acquired during a simulated EVA. Sampled rocks and soils were remotely
analyzed by the base control center, while the astronauts assisted by
placing the samples onto the sample holder and adjusting test bench
settings in order to obtain spectra. After analysis the collected
samples were documented and stored by the astronauts, before returning
to the base. Points of improvement for the EuroMoonMars2016 analog
campaign are the remote control of the computers using an established
network between the base and the lander. During following missions the
computers should preferably be operated over a larger distance without
interference. In the bottom compartment of the lander a rover is stored
that in future campaigns could replace astronaut functions by collecting
and returning samples, as well as performing adjustments to the analysis
test bench by using a remotely controlled robotic arm. Acknowledgements:
we thank Dominic Doyle for ESTEC optical lab support, Aidan Cowley (EAC)
and Matthias Sperl (DLR) for support discussions, and collaborators
from EuroMoonMars Eifel 2015-16 campaign team.
Title: The Moon Village Concept
Authors: Messina, Piero; Foing, Bernard H.; Hufenbach, Bernhard;
Haignere, Claudie; Schrogl, Kai-Uwe
Bibcode: 2016cosp...41E1286M
Altcode:
The "Moon Village" concept Space exploration is anchored in the
International Space Station and in the current and future automatic
and planetary automatic and robotic missions that pave the way for
future long-term exploration objectives. The Moon represents a prime
choice for scientific, operational and programmatic reasons and could
be the enterprise that federates all interested Nations. On these
considerations ESA is currently elaborating the concept of a Moon
Village as an ensemble where multiple users can carry out multiple
activities. The Moon Village has the ambition to serve a number of
objectives that have proven to be of interest (including astronomy,
fundamental research, resources management, moon science, etc. ) to
the space community and should be the catalyst of new alliances between
public and private entities including non-space industries. Additionally
the Moon Village should provide a strong inspirational and education
tool for the younger generations . The Moon Village will rely both
on automatic, robotic and human-tendered structures to achieve
sustainable moon surface operations serving multiple purposes on an
open-architecture basis. This Europe-inspired initiative should rally
all communities (across scientific disciplines, nations, industries)
and make it to the top of the political agendas as a the scientific
and technological undertaking but also political and inspirational
endeavour of the XXI century. The current reflections are of course
based on the current activities and plans on board the ISS and the
discussion held in international fora such as the ISECG. The paper will
present the status of these reflections, also in view of the ESA Council
at Ministerial Level 2016, and will give an overview of the on-going
activities being carried out to enable the vision of a Moon Village.
Title: Confirming interstellar C60+ using a new method for high
signal-to-noise NIR STIS spectroscopy
Authors: Cordiner, Martin A.; Cami, Jan; Charnley, Steven B.; Cox,
Nick; Foing, Bernard H.; Gull, Theodore Raymond; Joblin, Christine;
Lallement, Rosine; Linnartz, Harold; Najarro, Paco; Sarre, Peter John
Bibcode: 2016hst..prop14705C
Altcode:
Due to recent advances in laboratory spectroscopy, the first detection
of a large molecule has been claimed in the diffuse interstellar medium:
C60+ (ionized Buckminsterfullerene). If confirmed, the detection of
C60+ will constitute a major breakthrough in interstellar chemistry
and may provide, for the first time, an insight into the true chemical
complexity of the diffuse ISM. Confirming the presence of C60+ rests on
a rigorous detection of the weaker absorption lines of this molecule at
9365 and 9428 Angstroems - a region of the spectrum heavily obscured
in ground based studies due to telluric water vapour absorption. We
seek to demonstrate for the first time the feasibility of long-slit
STIS scan exposures to reach an unprecedented signal-to-noise ratio
>500 in the near-IR. These observations will eliminate the need
for error-prone telluric cancellation methods, allowing us to search
for and measure the weak C60+ features with sufficient accuracy to
confirm or reject the recently claimed C60+ discovery. If successful,
our CCD fringing reduction strategy would be a major breakthrough for
precise spectroscopic observations of various astrophysical phenomena
in this previously less well-explored wavelength region.
Title: Towards a Moon Village: Young Lunar Explorers Report
Authors: Kamps, Oscar; Foing, Bernard; Batenburg, Peter
Bibcode: 2016EGUGA..1817163K
Altcode:
Introduction: The Moon Village Workshop at ESTEC on the 14th December
2015 was organized by ILEWG/ESTEC in conjunction with the Moon 2020-2030
Symposium. It gathered a multi-disciplinary group of professionals
from all around the world to discuss their ideas about the concept of
a Moon Village, the vision of ESA's Director General (DG) Jan Woerner
of a permanent lunar base within the next decades [1]. The workshop
participants split in three working groups focusing on Moon Habitat
Design, science and technology potentials of the Moon Village, and
engaging stakeholders [2-3]. Their results and recommendations are
presented in this abstract. The Moon Habitat Design group identified
that the lunar base design is strongly driven by the lunar environment,
which is characterized by high radiation, meteoroids, abrasive dust
particles, low gravity and vacu-um. The base location is recommended
to be near the poles to provide optimized illumination conditions
for power generation, permanent communication to Earth, moderate
temperature gradients at the surface and interesting subjects
to scientific investigations. The abundance of nearby available
resources, especially ice at the dark bottoms of craters, can be
exploited in terms of In-Situ Resources Utilization (ISRU). The
identified infrastructural requirements include a navigation, data-
& commlink network, storage facilities and sustainable use of
resources. This involves a high degree of recycling, closed-loop life
support and use of 3D-printing technology, which are all technologies
with great potential for terrestrial spin-off applications. For the
site planning of the Moon Village, proven ideas from urban planning
on Earth should be taken into account. A couple of principles, which
could improve the quality of a long-term living milieu on the Moon,
are creating spacious environments, visibility between interior and
exterior spaces, areas with flora, such as gardens and greenhouses,
establishing a sustainable community and creating social places
for astronauts to interact and relax. The proposed establishment
of the lunar base can be divided into 4 steps. First the primary
base infrastructure is laid out through robotic missions, assisted
by human tele-operations from Earth, from the lunar orbit, or via a
human-tended gateway station in one of the Earth-Moon Lagrange points
(EML-1/2). During the second phase, the first manned habitation module
will be deployed. This module contains a bare minimum of functionality
to support a small crew for a couple of months. During the third phase,
additional modules with more dedicated functions will be sent to the
Moon, in order to enhance functionality and to provide astronauts with
more space and comfort for long-term missions. In the final phase of
the lunar village, a new set of modules will be sent to the base in
order to accommodate new arriving crew members. To ensure crew safety,
the landing site for supply vessels shall be located in safe distance to
the base. Extensive utilization of autonomous or tele-operated robots
further minimizes the risk for the crew. From the very beginning,
quickly accessible emergency escape vehicles, as well as a heavily
shielded 'safe haven' module to protect the crew from solar flares,
shall be available. Sustainable moon village development would require
explorers to fully utilize and process in-situ resources, in order to
manufacture necessary equipment and create new infrastructure. Mining
activities would be performed by autonomous robotic systems and managed
by colonists from the command center. Building upon the heritage of
commercial mining activities on Earth the production would be divided
into six stages: geological exploration and mapping, mine preparation,
extraction of raw resources, processing of raw resources, separation
of minerals, storage and utilization. Additional manufacturing
techniques, such as forging, would also need to be explored so as
not to limit the production capabilities. To facilitate the progress
of the Moon Village initiative it is necessary to attract private
industry investments. Potential sources range from technology testing
in the moon environment and private R&D funding from science
and academia fields, to space tourism, and more ambitious endeavors
such as building a prototype launcher site as a ground segment for
debris de-orbiting and satellite recycling activities. The Science
and Technology team has identified key technologies and possible major
scientific disciplines for a Moon Village and ranked them by importance
and by Technology Readiness Level (TRL). In terms of basic technologies
and objectives, rover exploration, life support systems, navigation
and surveying technologies resulted to have the highest importance and
readiness. Technologies for the development of the habitats (materials,
modules connections, power supply, alternative energy technologies
and energy storage) ended up on having high importance with medium-low
technology readiness. Technologies intended to help the astronauts or
improve techniques had low-medium importance together with low-medium
TRL (e.g. space lift to transfer resources, bio cybernetic augmentation
"Exoskeleton", jumping rover, telescope). After brainstorming for
required technologies, the fo-cus was shifted to what kinds of science
can be ex-pected to be performed, once a functional and usable habitat
would be available. The group has categorized studies of planetary
formation and the Solar System as a highly important scientific
discipline with a medi-um-high TRL. Scientific areas with high-medium
im-portance, but low technological readiness, were found to be ISRU,
psychological effects, adaptations of life to low gravity and plant
cultivation. The physiological effects of low-gravity on the body were
considered of medium importance and readiness. The Engaging Stakeholders
working group started by identifying the main stakeholders and groups
that play a role or that could play a role towards the Moon Village
project. These stakeholders were classified on their influence towards
the program and their attitude towards it. Complex system innovations
like the Moon Village initiative often encounter stiff resistance from
intended beneficiaries and stakeholders, because they disrupt existing
behaviors, organizational structures and business models. However,
if this large-scale change is rather approached as two simultaneous
and parallel challenges - the design of the artifact in ques-tion
and the design of the intervention that brings it to life - the
chances that it will take hold will increase. Finally, the group
recommended actions to be taken by the ESA DG to engage the most
direct stakeholders: The general public should be addressed on an
emotional level, human centered design thinking and social movement
design should be used to engage the civic society. When engaging
with the Moon Village stakeholders, the emotional resonance of Moon
Village's value proposition should be taken into account as much as
its scientific and technical requirements. This involves (social)
media, art and humanities and, for the long term, also investments on
education. In this way, a social excitement similar as for the Apollo
program might be triggered, which can be used by the member states to
engage with their national politicians and convince their taxpayers
of the Moon Village's benefits. ESA should invest on the creation of
a European new Space industry (similar to the one in the U.S.) and
therefore simplify their processes in order to make it easier for the
industry to invest and work with ESA with less bureaucracy. In order to
succeed in this large-scale international collaboration, a political
& legal framework needs to be established. It is recommended to
push for an International Moon Village Treaty agreement at the U.N. and
to start a conversation about the Moon Village at the UNCOPUOS, so
the delegations and member states can start providing ESA with their
political and legal inputs. The aim should be to present a sound concept
already at the ESA ministerial 2016. Conclusion: Since a long-term human
presence in the cis-lunar and lunar surface environment is envisaged,
human factors become an even more crucial element in defining the
success of the missions. Therefore, it is very important that not only
a set of technical problems is solved to survive the harsh environment
on the Moon. It is also necessary that psychological and physiological
factors will be considered in the design of the systems, equipment and
habitats. In that light, the Moon Habitat Design group noticed a missing
link between the currently developed space technologies and the actual
long-term usability by astronauts. It is therefore critical that ESA
would collaborate more with urban planners, architects and industrial
designers who provide the expertise in creating suitable environments
and products, which are not only technically sound and functional, but
also easy to use, comfortable and aesthetically pleasing. The Science
and Technology group has in general analyzed the key challenges,
technologies, objectives and issues related to the development of
a manned colony on the moon, classifying them from an importance
vs. Technology Readiness Level (TRL) point of view. The Engaging
Stakeholders working group has identified the main stakeholders and
groups that could play a role towards the Moon Village project. These
stake-holders were classified on their influence towards the program,
and their attitude towards it. One clear conclusion was that most of the
stakeholders showed a positive view towards the Moon Village program,
and that the most important step within a short term strategy should
focus on the actions to be taken to engage stakeholders for th next ESA
Ministerial to support the program. Finally, the group came up with some
recommendations on which actions should be taken by the ESA DG to invite
partners and to engage the most direct stakeholders: ESA delegations,
media, national governments, citizens and taxpayers. References: [1]
http://sci.esa.int/ilewg/ and https://ildwg.wordpress.com/ [2] Foing
B. Moon explora-tion highlights and Moon Village introduction. [3]
Young Lunar Explorers Report ESTEC Moon village sessions with community
and young professionals. *Organisation: Bernard Foing, ESA/ESTEC &
ILEWG, ESTEC Moon Village workshop WGs co-conveners: Peter Batenburg,
Andrea Jaime, Abigail Calzada, Angeliki Kapoglou, Chris Welch, Susanne
Pieterse, Daniel Esser, Audrey Berquand, Daniel Winter, Hanna Läkk,
Dmitri Ivanov, S Paternostro, Matias Hazadi, Oscar Kamps
Title: Towards A Moon Village: Vision and Opportunities
Authors: Foing, Bernard
Bibcode: 2016EGUGA..1815695F
Altcode:
The new DG of ESA, Jan Wörner, has expressed from the very beginning
of his duty a clear ambition towards a Moon Village, where Europe could
have a lead role. The concept of Moon Village is basically to start
with a robotic lunar village and then develop a permanent station on
the Moon with different countries and partners that can participate
and contribute with different elements, experiments, technologies,
and overall support. ESA's DG has communicated about this programme
and invited inputs from all the potential stakeholders, especially
member states, engineers, industry, scientists, innovators and diverse
representatives from the society. In order to fulfill this task, a
series of Moon Village workshops have been organized first internally
at ESA and then at international community events, and are also
planned for the coming months, to gather stakeholders to present their
ideas, their developments and their recommendations on how to put Moon
Village into the minds of Europeans, international partners and prepare
relevant actions for upcoming International Lunar Decade. Moon Village
Workshop: The Moon Village Workshop in ESTEC on the 14th December
was organized by ILEWG & ESTEC Staff Association in conjunction
with the Moon 2020-2030 Symposium. It gathered people coming from all
around the world, with many young professionals involved, as well as
senior experts and representatives, with a very well gender balanced
and multidisciplinary group. Engineers, business experts, managers,
scientists, architects, artists, students presented their views and work
done in the field of Lunar Exploration. Participants included colleagues
from ESA, SGAC Space Generation Advisory Council, NASA, and industries
such as OHB SE, TAS, Airbus DS, CGI, etc… and researchers or students
from various Universities in Europe, America, and Asia. Working groups
include: Moon Habitat Design, Science and Technology potentials on the
Moon Village, and Engaging Stakeholders. The Moon Habitat Design group
discussed principles and concepts for a minimum base that would start
with 4-10 crew, allowing a later evolution to 50 crew and elements
contributed by Moon Village partners at large. Various aspects
were assessed including habitats, laboratories, EVAs, pressurized
vehicles, core modules, inflatable extensions, power systems, life
support systems and bioreactors, ISRU using regolith, emergency,
services, medical, escape, shelters. The Science and Technology group
analyzed the importance and readiness level of technologies needed
for lunar robotic landers and for the Moon Village. The current ESA
lunar exploration activities focus on the contribution within ISS
operations barter of the ESA service module to bring Orion capsule
to the Moon starting with an automatic demonstration in 2018. It is
encouraged to consolidate this path for using the ser-vice module
for crewed missions EM2 and EM3 giving also the possibility of an ESA
astronaut, together with advanced technology, operations and science
utilization. They noted the interesting contribution of instruments,
drill, communications, and landing in support to Russian lunar polar
lander missions Luna 27. The Engaging Stakeholders working group
started by identifying the main stakeholders and groups that play a
role or that could play a role towards the Moon Village project. These
stakeholders were classified on their influence towards the programme,
and their attitude towards it. One clear conclusion was that most of the
stakeholders showed a positive view towards the Moon Village programme,
and that the most important step within a short term strategy should
focus on the actions to be taken to engage stakeholders for the next
ESA Ministerial to support the programme. Finally the group came up
with some recommendations on which should be the actions to be taken by
the ESA DG to engage the most direct stakeholders: ESA delegations,
media, national governments, citizens, taxpayers, and to invite
partners. Building on previous studies (EuroMoon, lunar polar lander)
ESA should develop a mid-class lunar lander (affordable in cost 300
Meu class), demonstrating the expertise at system level for a platform,
that could carry innovative competitive robotic payload contributed and
already with advance development from member states and international
or commercial partners. With teleoperations from Earth and cis-lunar
orbit, this will advance progress towards the next steps of Moon
Village and beyond. Recommendations: The participants encourage the
design and operations of a Moon base simulation at EAC with facility
and activities in the context of SpaceShip EAC, with the support of EAC,
DLR, ESTEC, ISU and other partners, and collaborations with other Lunar
Research Parks worldwide. It was also proposed to have an "ESTEC Moon
Village pilot project" where 20 young professional in-terns could be
hosted to work concurrently on various aspects (technology, science,
instruments platforms, Moon base design, human factors, programmatics,
outreach, community events) with links and support activities from
ESTEC senior experts, and interactions with colleagues in member
states, academia and industries . The workshop finalized with some
hands-on experiments, organized with some students demonstrating their
work on a lunar lander with tele-operated instruments and systems,
and on the measuring spectra of Moon-Mars analogue minerals. The day
ended with a refreshing lunar music session, and a networking event on
ESTEC ESCAPE where the last informal conversations marked a great wrap
up of such exciting day. Follow up Moon Village events are planned in
2016 at ESTEC, EAC and at international community venues. New means
of outreach, communications and social media must be developed. You
can follow Moon Village tweets, using #MoonVillage, and contribute
to the virtual discussions. ESA is really looking forward to engage
all stakeholders into the discussion, no matter of their background,
nationality or interest. Just let us know your views! Highlights and
recommendations can be found on https://ildwg.wordpress.com/ *Moon
Village Workshops Organisers Team: Bernard Foing (ESA/ESTEC &
ILEWG), Aidan Cowley, Guillermo Ortega, Linda van Hilten (ESA), Vid
Beldavs, David Dunlop, Jim Crisafulli (International Lunar Decade),
ESTEC Moon Village workshop 2015 WGs co-conveners: Peter Batenburg,
Andrea Jaime, Abigail Calzada, Angeliki Kapoglou, Chris Welch, Susanne
Pieterse, Daniel Esser, Audrey Berquand, Daniel Winter, Dmitri Ivanov,
Simone Paternostro, Matias Hazadi, Oscar Kamps, Marloes Offringa
Title: Site Selection and Automatically Calculated Rover Traverse
for a Lunar Teleoperated Landing Mission
Authors: Kamps, Oscar; Foing, Bernard; Flahaut, Jessica
Bibcode: 2016EGUGA..1815661K
Altcode:
With the recent interest for the Moon, and the plans from the ESA
side to do a tele-operated mission from Earth or lunar orbit, it is
important to target a well-defined location. One of the major topics
to study on the Moon is the existence and availability of volatiles
and ices. Because no lander ever visited one of the poles on the
Moon the theories with respect to water ice are only based on data
from orbiters. In a four month research project the data from the
orbiters was used for assessing potential landing sites and a rover
traverse planning. Mainly data from the Prospector and LRO were used
to select regions of interest. The prior selection was based on slope,
temperature and a geological map from the USGS. Three sites on both
the North as South Pole were used to test a proposed method for rover
traverse planning. Besides the scientific interest, the sites where
assessed on its accessibility for landing and roving. This assessment
was done based on some assumptions what would be possible for landing
and roving. For landing sites it was proposed to pick a site larger than
1km in diameter, in a (partial) illuminated area with a slope lower than
5o, which was inside an area which would be accessible for a rover. The
requirements to be selected as accessible area was a slope lower than
20o, the largest polygon which meets this requirement was chosen as
accessible area. As destination a site in the PSR was selected which
was inside the accessible area and had extremely low temperatures. The
boundary for extremely low was defined as 54K which is the sublimation
temperature of CO2 in lunar atmospheric pressure. As additional target
for the rover a site was selected where the temperature difference
would be more than 150K to study volatile migration processes. A
combination of tools in ArcGIS were used to do the site selection
and rover traverse planning. In the end Rozhdestvensky and Amundsen
were selected as most accessible and interesting. After comparing
both regions, Amundsen was preferred because of the higher temperature
variations and the flatter crater floor. The traverse was planned after
a manual selection of landing site, site of interest and destination,
which were together with a slope map the input for an automatically
calculated traverse. Some additional work is proposed with respect
to the site selection. More datasets can be used to complicate the
traverse or select other regions than Rozhdestvensky or Amundsen.
Title: Spectral analysis of lunar analogue samples
Authors: Offringa, Marloes; Foing, Bernard
Bibcode: 2016EGUGA..18.9630O
Altcode:
Analyses of samples derived from terrestrial analogue sites are used
to study lunar processes in their geological context (Foing, Stoker,
Ehrenfreund, 2011). For this study samples from the volcanic region
of the Eifel, Germany collected during field campaigns (Foing et al.,
2010), are analyzed with a variety of spectrometers. The aim is to
obtain a database of analyzed samples that could be used as a reference
for future in situ measurements. Equipment used in the laboratory
consists of a Fourier Transform Infrared (FTIR) spectrometer, an X-Ray
Fluorescence (XRF) spectrometer, a Raman laser spectrometer, as well as
UV-VIS and NIR reflectance spectrometers. The Raman, UV-VIS and NIR are
also used in combination with the EXoGeoLab mock-up lander during field
campaigns (Foing, Stoker, Ehrenfreund, 2011). Calibration of the UV-VIS
and NIR reflectance spectrometers is the main focus of this research in
order to obtain the clearest spectra. The calibration of the UV-VIS and
NIR reflectance spectrometers requires the use of a good light source
as well as suitable optical fibers to create a signal that covers the
widest range in wavelengths available. To eliminate noise towards the
edges of this range, multiple measurements are averaged and data is
processed by dividing the signal by reference spectra. Calibration
of the devices by creating a new dark and reference spectra has to
take place after every sample measurement. In this way we take into
account changes that occur in the signal due to the eating of the
devices during the measurements. Moreover, the integration time is
adjusted to obtain a clear signal without leading to oversaturation in
the reflectance spectrum. The typical integration times for the UV-VIS
reflectance spectrometer vary between 1 - 18 s, depending on the amount
of daylight during experiments. For the NIR reflectance spectrometer
the integration time resulting in the best signals is approximately
150 ms in combination with a broad spectrum light source. Together with
taking an average over ±600 measurements per sample this leads to the
best spectral signals that can be acquired with this set-up. Obtained
spectra can be tested for accuracy by comparing them with stationary
laboratory spectrometers such as the FTIR spectrometer. Future campaigns
involving the employment of the spectrometers on the ExoGeoLab lander
would prove the applicability of the equipment in the field.
Title: Laboratory Spectroscopy Measurements of Moon-Mars Analogue
Samples
Authors: Offringa, M. S.; Foing, B. H.
Bibcode: 2016LPI....47.2522O
Altcode:
Spectroscopy measurements of Moon-Mars analog samples, focused on
calibration of UV-VIS and NIR reflectance spectrometers in support of
a lunar lander mission.
Title: Highlights from MoonVillage Workshop at ESTEC, December, 2015
Authors: Foing, B. H.
Bibcode: 2016LPI....47.2719F
Altcode:
We present highlights from the ESA/ILEWG Moon Village Workshop 2015
in ESTEC addressing Moon Habitat Design, Science and Technology,
and Engaging Stakeholders.
Title: Towards a Moon Village: Results from ESTEC 2015 Workshop
Splinter Sessions
Authors: Batenburg, P.; Winter, D.; Calzada, A.; Jaime Albalat, A.;
Kleinschneider, A. M.; Welch, C.; Esser, D.; Ivanov, D.; Läkk, H.;
Kapoglou, A.; Hazadi, M.; Kamps, O.; Offringa, M.; Pieterse, S.;
Foing, B. H.
Bibcode: 2016LPI....47.2798B
Altcode:
We report on ESTEC 2015 Moon Village Workshop specific sessions on
Moon Habitat Design, science and technology potentials, and engaging
stake-holders.
Title: Lunar Polar Sites and Rover Traverse Planning for a Study on
Volatiles and Ices
Authors: Kamps, O. M.; Flahaut, J. D.; Foing, B. H.
Bibcode: 2016LPI....47.2412K
Altcode:
Results of a site selection and comparison project as preparation for
a rover traverse planning near the lunar poles for a tele-operated,
sample return mission.
Title: Preparations ExoGeoLab Lander for Lunar Analogue Field
Campaign, Eifel, Germany
Authors: Kamps, O. M.; Offringa, M. S.; Foing, B. H.
Bibcode: 2016LPI....47.2508K
Altcode:
As preparation for a lunar sample return mission we will present
results and lessons learned from a lunar analog campaign with the
ExoGeoLab lunar lander.
Title: ILEWG Report and Introduction to EPSC TP4 session on Lunar
Science and Exploration
Authors: Foing, B. H.
Bibcode: 2015EPSC...10..934F
Altcode:
We shall introduce the TP4 session on Lunar Science and Exploration and
present a status report of ILEWG/COSPAR International Lunar Exploration
Working Group to EPSC 2015.
Title: The International Lunar Decade — 2017-2029: Framework for
Concurrent Development of Enabling Technologies, Infrastructures,
Financings, and Policies for Lunar Development
Authors: Beldavs, V. Z.; Dunlop, D.; Crisafulli, J.; Foing, B.
Bibcode: 2015LPICo1863.2055B
Altcode:
The International Lunar Decade (ILD) planned for launch in 2017
provides a framework for long-term international collaboration in the
development of technologies, infrastructures, and financing mechanisms
for lunar development.
Title: Strategy for the International Lunar Decade
Authors: Beldavs, V.; Dunlop, D.; Foing, B.
Bibcode: 2015EPSC...10..917B
Altcode:
LD is a global event and process for international collaboration in
space initiated by the International Lunar Exploration Working Group
(ILEWG), the National Space Society and the National Science Centre
FOTONIKA-LV of the University of Latvia. ILD is planned for launch in
2017, the 60th anniversary of the International Geophysical Year that
marked the dawn of the space age with the launch of Sputnik. ILD is
envisioned as a decade long process of international collaboration
with lunar exploration concurrent with development of policies, key
enabling technologies and infrastructures on the Moon and in cislunar
space leading towards an eventual goal of industrial development of
the Moon and economic activity beyond Earth orbit[1]. This second
International Lunar Decade will build on the foundations of the ILD
first proposed in by the Planetary Society in 2006 at International
Conference on Exploration and Utilisation of the Moon (ICEUM), was
endorsed by ICEUM participants[3], and then by ILEWG, COSPAR and other
organizations. Starting in 2007, the work plan included a series of
recommendations for lunar exploration missions coordinated through the
ILEWG agencies and COSPAR. Advances in technology such as CubeSats and
3D printing and fundamental changes in mind-set marked by initiatives
such as the Google Lunar-X prize and asteroid mining ventures have
made industrial development of the Moon a thinkable proposition. The
ILD to be launched in 2017 is intended to set the stage for the Moon
to become a wealth generating platform for human expansion into the
solar system.ILD is being organized to engage existing organizations
involved in space collaboration such as COSPAR, COPUOS, ISECG, technical
and scientific organizations and others that address space policy,
space law, space security, governance and related concerns. Additional
organizations will be involved that deal with structures, ecosystems,
financing, economic development and health and life support and related
concerns. The Moon Treaty (1979) will be reviewed for its applicability
to the development of the international regime that will be required
to govern mining, industrial development and commercial activities
on the Moon. ILD has already been a significant topic in several
international conferences.Through this and many other conferences to
follow the initial organizers expect that key organizations will see
a role for their activities within the ILD process, endorse it and
start to shape implementation plans. This report will focus on overall
strategies for the ILD process to fully engage multiple countries and
organizations building towards a shared vision through a diversity
of scientific, technical and cultural perspectives. Public outreach
and involvement of the public, particularly youth and schools will
be an important component of the overall strategy. The activities
of the International Lunar Decade Working Group can be followed at
https://ildwg.wordpress.com .
Title: ExoLab Space Mission Simulation: Expanding life with art
& science
Authors: Schlacht, I. L.; Foing, B.; Preusterink, J. W.; Petric, E.;
Tursic, M.; Petric, S.; Pasenau, L.; Guillaume, D.; Blugerman, N.
Bibcode: 2015EPSC...10..790S
Altcode:
In the context of building a minimum autonomous modular architecture
for the Moon & extreme environments on earth, a simulation
has been performed considering also the potentiality for Art &
Science applications. In specific ExoHab and ExoLab has been equipped
as technical mockup at ESTEC for multidisciplinary mission simulation
[1,2, 3].
Title: Art & Space: the webbing projects of Eva Petrič
Authors: Petrič, E.; Schlacht, I. L.; Foing, B.
Bibcode: 2015EPSC...10..791P
Altcode:
Art is considered a form of communication often related to the
perception of personal emotion of the artist. Space is the most
extreme environment that a human could approach, this environment
affects the human body and the individual's personal perception with
metamorphosis created by factors such as, isolation, radiation and
difference of gravity. This alteration of the perception could be
viewed as a potentiality from artists to acquire and communicate new
emotions. To investigate the capacity of an artist to come faster
and closer to emotions and to communicate their feeling, a mission
simulation has been performed in the ExoLab module [1] from ILEWG [A]
on the 29th of April 2015.
Title: The International Lunar Decade Declaration
Authors: Beldavs, V.; Foing, B.; Bland, D.; Crisafulli, J.
Bibcode: 2015EPSC...10..916B
Altcode:
The International Lunar Decade Declaration was discussed at the
conference held November 9-13, 2014 in Hawaii "The Next Giant
Leap: Leveraging Lunar Assets for Sustainable Pathways to Space"
- http://2014giantleap.aerospacehawaii.info/ and accepted by a
core group that forms the International Lunar Decade Working Group
(ILDWG) that is seeking to make the proposed global event and decade
long process a reality. The Declaration will be updated from time
to time by members of the ILDWreflecting new knowledge and fresh
perspectives that bear on building a global consortium with a mission
to progress from lunar exploration to the transformation of the Moon
into a wealth gene rating platform for the expansion of humankind
into the solar system. When key organizations have endorsed the idea
and joined the effort the text of the Declaration will be considered
final. An earlier International Lunar Decade proposal was issued at
the 8th ICEUM Conference in 2006 in Beijing together with 13 specific
initiatives for lunar exploration[1,2,3]. These initiatives have
been largely implemented with coordination among the different space
agencies involved provided by the International Lunar Exploration
Working Group[2,3]. The Second International Lunar Decade from 2015
reflects current trends towards increasing involvement of commercial
firms in space, particularly seeking opportunities beyond low Earth
orbit. The central vision of the International Lunar Decade is to build
the foundations for a sustainable space economy through international
collaboration concurrently addressing Lunar exploration and building a
shared knowledge base;Policy development that enables collabo rative
research and development leading to lunar mining and industrial and
commercial development;Infrastructure on the Moon and in cislunar
space (communications, transport, energy systems, way-stations,
other) that reduces costs, lowers risks and speeds up the time to
profitable operations;Enabling technologies needed for lunar operations
(robotic and human), lunar mining, materials processing, manufacturing,
transportation, life support and other.
Title: Organics in Space: Results from SPace Exposure Platforms
and Nanosatellites
Authors: Ehrenfreund, Pascale; Foing, Bernard H.; Salama, Farid
Bibcode: 2015IAUGA..2257551E
Altcode:
A series of successful “laboratory astrophysics” experiments
performed on International Space Station (ISS) external platforms such
as EXPOSE have provided insights into the evolution of organic and
biological materials in space and planetary environments. The study
of the reactions, destruction, and longevity of organics in the space
environment is of fundamental interest. To provide an accurate outer
space environment for extended durations, exposure experiments in low
Earth orbit have been conducted in the last decades in order to examine
the consequences of actual space conditions including combinations of
solar and cosmic radiation, space vacuum, and microgravity. The O/OREOS
(Organism/ORganic Exposure to Orbital Stresses) nanosatellite studied
in situ during the 6-month primary and 1-year extended mission the
photochemical processing of selected PAHs in low Earth orbit (650 km
altitude); results were autonomously telemetered to Earth. We report
on the methods and flight preparation of samples for space exposure
platforms and results on the stability of organic thin-films. The
UV-vis degradation process of thin-films was recorded over time,
which revealed intriguing and counter-intuitive photolytic kinetics
that will be re-investigated on the ISS in a space environment.
Title: Field Research and Laboratory Sample Analysis of
Dust-Water-Organics-Life from Mars Analogue Extreme Environments
Authors: Foing, Bernard H.; Ehrenfreund, Pascale; ILEWG EuroMoonMars
Team
Bibcode: 2015IAUGA..2257650F
Altcode:
We describe results from the data analysis from a series of field
research campaigns (ILEWG EuroMoonMars campaigns 2009* to 2013) in
the extreme environment of the Utah desert relevant to habitability
and astrobiology in Mars environments, and in order to help in
the interpretation of Mars missions measurements from orbit (MEX,
MRO) or from the surface (MER, MSL). We discuss results relevant
to the scientific study of the habitability factors influenced by
the properties of dust, organics, water history and the diagnostics
and characterisation of microbial life. We also discuss perspectives
for the preparation of future lander and sample return missions. We
deployed at Mars Desert Research station, Utah, a suite of instruments
and techniques including sample collection, context imaging from
remote to local and microscale, drilling, spectrometers and life
sensors. We analyzed how geological and geochemical evolution a ected
local parameters (mineralogy, organics content, environment variations)
and the habitability and signature of organics and biota. We find high
diversity in the composition of soil samples even when collected in
close proximity, the low abundances of detectable PAHs and amino acids
and the presence of biota of all three domains of life with signi cant
heterogeneity. An extraordinary variety of putative extremophiles
was observed. A dominant factor seems to be soil porosity and lower
clay-sized particle content. A protocol was developed for sterile
sampling, contamination issues, and the diagnostics of biodiversity
via PCR and DGGE analysis in soils and rocks samples. We compare
2009 campaign results to new measurements from 2010-2013 campaigns:
comparison between remote sensing and in-situ measurements; the study
of minerals; the detection of organics and signs of life.References *
in Foing, Stoker Ehrenfreund (Editors, 2011) Astrobiology field Research
in Moon/Mars Analogue Environments", Special Issue of International
Journal of Astrobiology , IJA 2011, 10, vol. 3. 137-305Credits: ILEWG
EuroMoonMars Team
Title: SMART-1 end of life shallow regolith impact simulations
Authors: Burchell, M. J.; Cole, M. J.; Ramkissoon, N. K.;
Wozniakiewicz, P. J.; Price, M. C.; Foing, B.
Bibcode: 2015M&PS...50.1436B
Altcode: 2015M&PS..tmp..202B
The SMART-1 end-of-life impact with the lunar surface was simulated with
impacts in a two stage light-gas gun onto inclined basalt targets with
a shallow surface layer of sand. This simulated the probable impact
site, where a loose regolith will have overlaid a well consolidated
basaltic layer of rock. The impact angles used were at 5° and 10°
from the horizontal. The impact speed was ~2 km s-1 and
the projectiles were 2.03 mm diameter aluminum spheres. The sand depth
was between approximately 0.8 and 1.8 times the projectile diameter,
implying a loose lunar surface regolith of similar dimensions to the
SMART-1 spacecraft. A crater in the basement rock itself was only
observed in the impact at 10° incidence, and where the depth of loose
surface material was less than the projectile diameter, in which
case the basement rock also contained a small pit-like crater. In
all cases, the projectile ricocheted away from the impact site at a
shallow angle. This implies that at the SMART-1 impact site the crater
will have a complicated structure, with exposed basement rock and some
excavated rock displaced nearby, and the main spacecraft body itself
will not be present at the main crater.
Title: Quantifying geological processes on Mars-Results of the high
resolution stereo camera (HRSC) on Mars express
Authors: Jaumann, R.; Tirsch, D.; Hauber, E.; Ansan, V.; Di Achille,
G.; Erkeling, G.; Fueten, F.; Head, J.; Kleinhans, M. G.; Mangold,
N.; Michael, G. G.; Neukum, G.; Pacifici, A.; Platz, T.; Pondrelli,
M.; Raack, J.; Reiss, D.; Williams, D. A.; Adeli, S.; Baratoux, D.;
de Villiers, G.; Foing, B.; Gupta, S.; Gwinner, K.; Hiesinger, H.;
Hoffmann, H.; Le Deit, L.; Marinangeli, L.; Matz, K. -D.; Mertens, V.;
Muller, J. P.; Pasckert, J. H.; Roatsch, T.; Rossi, A. P.; Scholten,
F.; Sowe, M.; Voigt, J.; Warner, N.
Bibcode: 2015P&SS..112...53J
Altcode:
This review summarizes the use of High Resolution Stereo Camera (HRSC)
data as an instrumental tool and its application in the analysis of
geological processes and landforms on Mars during the last 10 years
of operation. High-resolution digital elevations models on a local
to regional scale are the unique strength of the HRSC instrument. The
analysis of these data products enabled quantifying geological processes
such as effusion rates of lava flows, tectonic deformation, discharge
of water in channels, formation timescales of deltas, geometry of
sedimentary deposits as well as estimating the age of geological
units by crater size-frequency distribution measurements. Both the
quantification of geological processes and the age determination allow
constraining the evolution of Martian geologic activity in space
and time. A second major contribution of HRSC is the discovery of
episodicity in the intensity of geological processes on Mars. This has
been revealed by comparative age dating of volcanic, fluvial, glacial,
and lacustrine deposits. Volcanic processes on Mars have been
active over more than 4 Gyr, with peak phases in all three geologic
epochs, generally ceasing towards the Amazonian. Fluvial and lacustrine
activity phases spread a time span from Noachian until Amazonian
times, but detailed studies show that they have been interrupted by
multiple and long lasting phases of quiescence. Also glacial activity
shows discrete phases of enhanced intensity that may correlate with
periods of increased spin-axis obliquity. The episodicity of geological
processes like volcanism, erosion, and glaciation on Mars reflects
close correlation between surface processes and endogenic activity as
well as orbit variations and changing climate condition.
Title: Astrochemistry: Fullerene solves an interstellar puzzle
Authors: Ehrenfreund, Pascale; Foing, Bernard
Bibcode: 2015Natur.523..296E
Altcode:
Laboratory measurements confirm that a 'buckyball' ion is responsible
for two near-infrared absorption features found in spectra of the
interstellar medium, casting light on a century-old astrochemical
mystery. See Letter p.322
Title: Small rover exploration capabilities
Authors: Salotti, Jean-Marc; Laithier, Corentin; Machut, Benoit;
Marie, Aurélien; Bruneau, Audrey; Grömer, Gernot; Foing, Bernard H.
Bibcode: 2015AdSpR..55.2484S
Altcode:
For a human mission to the Moon or Mars, an important question is to
determine the best strategy for the choice of surface vehicles. Recent
studies suggest that the first missions to Mars will be strongly
constrained and that only small unpressurized vehicles will be
available. We analyze the exploration capabilities and limitations
of small surface vehicles from the user perspective. Following the
“human centered design” paradigm, the team focused on human systems
interactions and conducted the following experiments:<ce:list - The Austrian Space Forum (OeWF) coordinated a Mars analog research
program in Morocco in February 2013. During this 23-nation expedition,
we studied surface mobility aspects in challenging terrains also to
be expected on Mars. Two test subjects in high-fidelity spacesuit
simulators and driving All-Terrain Vehicles (ATV, aka quads) had
to traverse various obstacles found in a desert region and answer
a list of questions about their vehicle, the obstacles and possible
options to go further.</ce:para> - Another member of our
team participated in the ILEWG EuroMoonMars 2013 simulation at the Mars
Desert Research Station in Utah during the same period of time. Although
the possible traverses were restricted, a similar study with analog
space suits and quads has been carried out.</ce:para> -
Other experiments have been conducted in an old rock quarry close
to Bordeaux, France. An expert in the use of quads for all types
of terrains performed a demonstration and helped us to characterize
the difficulties, the risks and advantages and drawbacks of different
vehicles and tools.</ce:para> The vehicles that will be used
on the surface of Mars have not been defined yet. Nevertheless, the
results of our project already show that using a light and unpressurized
vehicle (in the order of 150 kg) for the mobility on the Martian surface
can be a true advantage. Part of the study was dedicated to the search
for appropriate tools that could be used to make the vehicles easier
to handle, safer to use and more efficient in the field to cross an
obstacle. The final recommendation is to use winches and ramps, which
already are widely used by quad drivers. We report on the extension
of the reachable areas if such tools were available. This work
has been supported by ILEWG, EuroMoonMars and the Austrian Space Forum
(OEWF).
Title: Lunar Exploration and Science in ESA
Authors: Carpenter, James; Houdou, Bérengère; Fisackerly, Richard;
De Rosa, Diego; Patti, Bernardo; Schiemann, Jens; Hufenbach, Bernhard;
Foing, Bernard
Bibcode: 2015EGUGA..1715783C
Altcode:
ESA seeks to provide Europe with access to the lunar surface, and
allow Europeans to benefit from the opening up of this new frontier,
as part of a global endeavor. This will be best achieved through an
exploration programme which combines the strengths and capabilities
of both robotic and human explorers. ESA is preparing for future
participation in lunar exploration through a combination of human and
robotic activities, in cooperation with international partners. Future
planned activities include the contribution of key technological
capabilities to the Russian led robotic missions, Luna-Glob,
Luna-Resurs orbiter and Luna-Resurs lander. For the Luna-Resurs lander
ESA will provide analytical capabilities to compliment the Russian
led science payload, focusing on developing an characterising the
resource opportunities offered at the lunar surface. This should be
followed by the contributions at the level of mission elements to
a Lunar Polar Sample Return mission. These robotic activities are
being performed with a view to enabling a future more comprehensive
programme in which robotic and human activities are integrated to
provide the maximum benefits from lunar surface access. Activities on
the ISS and ESA participation to the US led Multi-Purpose Crew Vehicle,
which is planned for a first unmanned lunar flight in 2017, are also
important steps towards achieving this. In the frame of a broader future
international programme under discussion through the International
Space Exploration Coordination Group (ISECG) future missions are under
investigation that would provide access to the lunar surface through
international cooperation and human-robotic partnerships.
Title: The International Lunar Decade: A Giant Leap Forward in
Understanding the Moon and Opportunities for its Development
Authors: Beldavs, Vid; Atvars, Aigars; Ubelis, Arnolds; Salmins,
Kalvis; Crisafulli, Jim; Dunlop, David; Foing, Bernard
Bibcode: 2015EGUGA..1715804B
Altcode:
In 1957 at the dawn of the space age the United Nations launched
the International Geophysical Year which had a profound impact on
collaboration among scientists around the globe. Its legacy includes
several major scientific organizations as well as the beginnings
of collaboration among nations that see themselves as competitors
on Earth. The Soviet Union and the United States made many attempts
at collaboration in space while building weapons systems to destroy
each other. Space technologies have become the infrastructure for the
ubiquitous smart phone with global telecommunications, navigation,
weather forecasting, environmental monitoring, and hundreds of other
applications. In 2015, the International Year of Light, several
conferences will be held exploring the idea of an International
Lunar Decade1 An informal group, the International Lunar Decade
Working Group (ILDWG) has been formed to plan the launch of the
International Lunar Decade in 2017, the 60th Anniversary of the
International Geophysical Year. This report will cover the progress of
the ILDWG covering conferences planned, international organizations
involved and key publications. The activities of the ILDWG can be
followed at http://2014giantleap.aerospacehawaii.info/. References [1]
V. Beldavs, 2014 'The International Lunar Decade', The Space Review,
http://www.thespacereview.com/article/2431/1
Title: ILEWG report and discussion on Lunar Science and Exploration
Authors: Foing, Bernard
Bibcode: 2015EGUGA..1715788F
Altcode:
The EGU PS2.2 session "Lunar Science and Exploration" will include
oral papers and posters, and a series of discussions. Members of
ILEWG International Lunar Exploration Working Group will debate: -
Recent lunar results: geochemistry, geophysics in the context of open -
Celebrating the lunar legacy of pioneers Gerhard Neukum, Colin Pillinger
and Manfred Fuchs planetary science and exploration - Latest results
from LADEE and Chang'e 3/4 - Synthesis of results from SMART-1, Kaguya,
Chang-E1 and Chang-E2, Chandrayaan-1, Lunar Reconnaissance Orbiter and
LCROSS impactor, Artemis and GRAIL - Goals and Status of missions under
preparation: orbiters, Luna-Glob, Google Lunar X Prize, Luna Resurs,
Chang'E 5, Future landers, Lunar sample return - Precursor missions,
instruments and investigations for landers, rovers, sample return,
and human cis-lunar activities and human lunar sorties - Preparation:
databases, instruments, terrestrial field campaigns - The future
international lunar exploration programme towards ILEWG roadmap of
a global robotic village and permanent international lunar base -
The proposals for an International Lunar Decade and International
Lunar Research Parks - Strategic Knowledge Gaps, and key science Goals
relevant to Human Lunar Global Exploration Lunar science and exploration
are developing further with new and exciting missions being developed
by China, the US, Japan, India, Russia, Korea and Europe, and with
the perspective of robotic and human exploration. The session will
include invited and contributed talks as well as a panel discussion
and interactive posters with short oral introduction.
Title: A multiwavelength study of the M dwarf binary YY Geminorum
Authors: Butler, C. J.; Erkan, N.; Budding, E.; Doyle, J. G.; Foing,
B.; Bromage, G. E.; Kellett, B. J.; Frueh, M.; Huovelin, J.; Brown,
A.; Neff, J. E.
Bibcode: 2015MNRAS.446.4205B
Altcode: 2015arXiv150103930B
We review the results of the 1988 multiwavelength campaign on
the late-type eclipsing binary YY Geminorum. Observations include:
broad-band optical and near-infrared photometry, simultaneous optical
and ultraviolet (IUE) spectroscopy, X-ray (Ginga) and radio (VLA)
data. From models fitted to the optical light curves, fundamental
physical parameters have been determined together with evidence for
transient maculations (spots) located near quadrature longitudes and
intermediate latitudes. Eclipses were observed at optical, ultraviolet
and radio wavelengths. Significant drops in 6 cm radio emission near the
phases of both primary and secondary eclipse indicate relatively compact
radio emitting volumes that may lie between the binary components. IUE
observations during secondary eclipse are indicative of a uniform
chromosphere saturated with Mg II emission and an extended volume of
Lyα emission. Profile fitting of high-dispersion Hα spectra confirms
the chromospheric saturation and indicates significant Hα opacity to
heights of a few per cent of the photospheric radius. There is evidence
for an enhanced Hα emission region visible near phase 0.25-0.35
which may be associated with a large spot on the primary and with two
small optical flares which were also observed at other wavelengths:
one in microwave radiation and the other in X-rays. For both flares,
LX/Lopt is consistent with energy release in
closed magnetic structures.
Title: First results of the ORGANIC experiment on EXPOSE-R on the ISS
Authors: Bryson, K. L.; Salama, F.; Elsaesser, A.; Peeters, Z.; Ricco,
A. J.; Foing, B. H.
Bibcode: 2015IJAsB..14...55B
Altcode:
The ORGANIC experiment on EXPOSE-R spent 682 days outside the
International Space Station, providing continuous exposure to
the cosmic-, solar- and trapped-particle radiation background for
fourteen samples: 11 polycyclic aromatic hydrocarbons (PAHs) and
three fullerenes. The thin films of the ORGANIC experiment received,
during space exposure, an irradiation dose of the order of 14 000 MJ
m-2 over 2900 h of unshadowed solar illumination. Extensive
analyses were performed on the returned samples and the results
compared to ground control measurements. Analytical studies of the
returned samples included spectral measurements from the vacuum
ultraviolet to the infrared range and time-of-flight secondary ion
mass spectrometry. Limited spectral changes were observed in most
cases pointing to the stability of PAHs and fullerenes under space
exposure conditions. Furthermore, the results of these experiments
confirm the known trend in the stability of PAH species according to
molecular structure: compact PAHs are more stable than non-compact PAHs,
which are themselves more stable than PAHs containing heteroatoms,
the last category being the most prone to degradation in the space
environment. We estimate a depletion rate of the order of 85 +/- 5%
over the 17 equivalent weeks of continuous unshadowed solar exposure in
the most extreme case tetracene (smallest, non-compact PAH sample). The
insignificant spectral changes (below 10%) measured for solid films of
large or compact PAHs and fullerenes indicate a high stability under
the range of space exposure conditions investigated on EXPOSE-R.
Title: Lunar Exploration in ESA
Authors: Carpenter, J. D.; Houdou, B.; Fisackerly, F.; De Rosa, D.;
Patti, B.; Schiemann, J.; Hufenbach, B.; Foing, B.
Bibcode: 2014LPICo1820.3019C
Altcode:
We report on current ESA plans and activities in the area of lunar
exploration.
Title: VLT/X-Shooter survey of near-infrared diffuse interstellar
bands
Authors: Cox, N. L. J.; Cami, J.; Kaper, L.; Ehrenfreund, P.; Foing,
B. H.; Ochsendorf, B. B.; van Hooff, S. H. M.; Salama, F.
Bibcode: 2014A&A...569A.117C
Altcode: 2014arXiv1407.0370C
Context. The unknown identity of the diffuse interstellar band (DIB)
carriers poses one of the longest standing unresolved problems in
astrophysics. While the presence, properties, and behaviour of hundreds
of optical DIBs between 4000 Å and 9000 Å have been well established,
information on DIBs in both the ultra-violet and near-infrared (NIR)
ranges is limited.
Aims: In this paper, we present a spectral
survey of the NIR range, from 0.9 μm to 2.5 μm. Our observations were
designed to detect new DIBs, confirm previously proposed NIR DIBs,
and characterise their behaviour with respect to known line-of-sight
properties (including the optical DIBs present in our spectra).
Methods: Using the X-Shooter instrument mounted on the ESO Very Large
Telescope (VLT) we obtained medium-resolution spectra of eight known
DIB targets and one telluric reference star, from 3000 Å to 25 000
Å in one shot.
Results: In addition to the known 9577, 9632,
10 780, 11 797, and 13 175 Å NIR DIBs, we confirm 9 out of the 13
NIR DIBs that were presented by Geballe et al. (2011, Nature, 479,
200). Furthermore, we report 11 new NIR DIB candidates. The strengths
of the strongest NIR DIBs show a general correlation with reddening,
E(B - V), but with a large scatter. Several NIR DIBs are more
strongly correlated with the 5780 Å DIB strength than with E(B -
V); this is especially the case for the 15 268 Å DIB. The NIR
DIBs are strong: the summed equivalent widths of the five strongest
NIR DIBs represent a small percent of the total equivalent width of
the entire average DIB spectrum (per unit reddening). The NIR DIBs
towards the translucent cloud HD 147889 are all
weak with respect to the general trend. No direct match was found
between observed NIR DIBs and laboratory matrix-isolation spectroscopic
data of polycyclic aromatic hydrocarbons (PAHs).
Conclusions:
The strong correlation between the 5780-15 268 DIB pair implies that
(Nf)5780/(Nf)15 268 = 14. However, the reduced
strength of the 15 268 Å DIB in HD 147889 rules
out a common carrier for these two DIBs. Since the ionisation fraction
for small PAHs in this translucent cloud is known to be low compared
to diffuse clouds, the weakness of the 15 268 Å DIB suggests that an
ionised species could be the carrier of this NIR DIB. Based on
observations obtained with the VLT (ESO Programme 385.C-0720).
Title: Gale Crater Analogue Geology Studies at Multiple Scales
Authors: Foing, B. H.; Orgel, C.; Stoker, C.; Ehrenfreund, P.; Rammos,
I.; Rodrigues, L.; Svendsen, A.; Oltheten, D.; Schlacht, I.; Nebergall,
K.; Battler, M.; v'T Houd, H.; Bruneau, A.; Cross, M.; Maivald, V.;
Elsaesser, A.; Direito, S. O.; Röling, W. F.; Davies, G. R.; ILEWG
Euromoonmars 2013 Team
Bibcode: 2014LPICo1791.1462F
Altcode:
We study the terrestrial analog of Gale crater during a field campaign
(ILEWG EuroMoonMars) at MDRS, Utah to diagnose the geology at multiple
scales and help in the interpretation of measurements from orbit
(Mars Express, MRO) and Curiosity rover.
Title: Analysis Of The Returned Samples From A Space Exposure
Experiment: The ORGANIC Experiment on EXPOSE-R on the ISS
Authors: Bryson, Kathryn; Peeters, Zan; Salama, Farid; Foing, Bernard;
Ehrenfreund, Pascale; Elsaesser, Andreas; Ricco, Antonio; Jessberger,
Elmar K; Schmidt, Werner; Robert, François
Bibcode: 2014AAS...22411906B
Altcode:
The ORGANIC experiment on the multi-user facility EXPOSE-R on the
International Space Station investigated the chemical evolution,
survival, destruction, and chemical modification of PAHs and fullerenes
in space. Aromatic networks are among the most abundant organic material
in space. PAHs and fullerenes have been identified in meteorites
and are thought to be among the carriers for numerous astronomical
absorption and emission features.Thin films of selected PAHs and
fullerenes have been subjected to the low Earth orbit environment as
part of the ORGANIC experiment.EXPOSE-R with its experiment inserts was
mounted on the outside of the ISS for 682 days starting in 2009. The
samples were returned to Earth and inspected in spring 2011. The period
outside the ISS provided continuous exposure to the cosmic-, solar-,
and trapped-particle radiation background and >2500 h of unshadowed
solar illumination. All trays carry both solar-irradiation-exposed
and dark samples shielded from the UV photons, enabling discrimination
between the effects of exposure to solar photons and cosmic rays. The
samples were analyzed before exposure to the space environment with
UV-VIS and IR spectroscopy. Ground truth monitoring of additional sample
carriers was performed through UV-VIS spectroscopy at regular intervals
at NASA ARC (Bryson et al. 2011, Adv. Space Res. 48, 1980). The UV-VIS
and IR spectroscopic measurements were collected for the returned
flight samples.We report on the scientific experiment, the details of
the ground control analysis, and returned flight sample results. We
discuss how extended space exposure experiments allow to enhance our
knowledge on the evolution of organic compounds in space.
Title: ESA SMART-1 mission: review of results and legacy 10 years
after launch
Authors: Foing, Bernard
Bibcode: 2014EGUGA..1615175F
Altcode:
We review ESA's SMART-1 highlights and legacy 10 years after
launch. The SMART-1 mission to the Moon achieved record firsts such
as: 1) first Small Mission for Advanced Research and Technology;
with spacecraft built and integrated in 2.5 years and launched 3.5
years after mission approval; 2) first mission leaving the Earth
orbit using solar power alone with demonstration for future deep
space missions such as BepiColombo; 3) most fuel effective mission
(60 litres of Xenon) and longest travel (13 month) to the Moon!;
4) first ESA mission reaching the Moon and first European views
of lunar poles; 5) first European demonstration of a wide range of
new technologies: Li-Ion modular battery, deep-space communications
in X- and Ka-bands, and autonomous positioning for navigation; 6)
first lunar demonstration of an infrared spectrometer and of a Swept
Charge Detector Lunar X-ray fluorescence spectrometer ; 7) first ESA
mission with opportunity for lunar science, elemental geochemistry,
surface mineralogy mapping, surface geology and precursor studies
for exploration; 8) first controlled impact landing on the Moon with
real time observations campaign; 9) first mission supporting goals
of the ILEWG/COSPAR International Lunar Exploration Working Group in
technical and scientific exchange, international collaboration, public
and youth engagement; 10) first mission preparing the ground for ESA
collaboration in Chandrayaan-1, Chang'E1-2-3 and near-future landers,
sample return and human lunar missions. The SMART-1 technology legacy
is applicable to geostationary satellites and deep space missions
using solar electric propulsion. The SMART-1 archive observations have
been used to support scientific research and prepare subsequent lunar
missions and exploration. Most recent SMART-1 results are relevant
to topics on: 1) the study of properties of the lunar dust, 2) impact
craters and ejecta, 3) the study of illumination, 4) observations and
science from the Moon, 5) support to future missions, 6) identifying
and characterising sites for exploration and exploitation. This legacy
is relevant to the preparation for future orbiters, landers, sample
return, a global robotic village, human missions and international
lunar bases (consistent with ILEWG, COSPAR and Global Space Exploration
roadmaps). Link: http://sci.esa.int/smart-1/ References and citations:
http://scholar.google.nl/scholar?&q=smart-1+moon **We acknowledge
ESA, member states, industry and institutes for their contribution,
and the members of SMART-1 Teams: G.Racca and SMART-1 Project Team,
O. Camino and SMART-1 Operations Team, D. Frew and SMART-1 STOC,
B.H. Foing and STWT, B. Grieger, D. Koschny, J.-L. Josset, S. Beauvivre,
M. Ellouzi, S. Peters, A. Borst, E. Martellato, M. Almeida, J.Volp,
D. Heather, M. Grande, J. Huovelin, H.U. Keller, U. Mall, A. Nathues,
A. Malkki, W. Schmidt, G. Noci, Z. Sodnik, B. Kellett, P. Pinet,
S. Chevrel, P. Cerroni, M.C. de Sanctis, M.A. Barucci, S. Erard,
D. Despan, K. Muinonen, V. Shevchenko, Y. Shkuratov, P. McMannamon,
P. Ehrenfreund, C. Veillet, M. Burchell, other Co-Investigators,
associated scientists, collaborators, students and colleagues.
Title: Habitability & Astrobiology Research in Mars Terrestrial
Analogues
Authors: Foing, Bernard
Bibcode: 2014EGUGA..1615678F
Altcode:
We performed a series of field research campaigns (ILEWG EuroMoonMars)
in the extreme Utah desert relevant to Mars environments, and in order
to help in the interpretation of Mars missions measurements from orbit
(MEX, MRO) or from the surface (MER, MSL), or Moon geochemistry
(SMART-1, LRO). We shall give an update on the sample analysis
in the context of habitability and astrobiology. Methods &
Results: In the frame of ILEWG EuroMoonMars campaigns (2009 to 2013)
we deployed at Mars Desert Research station, near Hanksville Utah, a
suite of instruments and techniques [A, 1, 2, 9-11] including sample
collection, context imaging from remote to local and microscale,
drilling, spectrometers and life sensors. We analyzed how geological
and geochemical evolution affected local parameters (mineralogy,
organics content, environment variations) and the habitability and
signature of organics and biota. Among the important findings are the
diversity in the composition of soil samples even when collected in
close proximity, the low abundances of detectable PAHs and amino acids
and the presence of biota of all three domains of life with significant
heterogeneity. An extraordinary variety of putative extremophiles was
observed [3,4,9]. A dominant factor seems to be soil porosity and
lower clay-sized particle content [6-8]. A protocol was developed
for sterile sampling, contamination issues, and the diagnostics of
biodiversity via PCR and DGGE analysis in soils and rocks samples [10,
11]. We compare the 2009 campaign results [1-9] to new measurements
from 2010-2013 campaigns [10-12] relevant to: comparison between
remote sensing and in-situ measurements; the study of minerals; the
detection of organics and signs of life. Keywords: field analogue
research, astrobiology, habitability, life detection, Earth-Moon-Mars,
organics References [A] Foing, Stoker & Ehrenfreund (Editors, 2011)
"Astrobiology field Research in Moon/Mars Analogue Environments",
Special Issue of International Journal of Astrobiology , IJA 2011, 10,
vol. 3. 137-305 [1] Foing B. et al. (2011) Field astrobiology research
at Moon-Mars analogue site: Instruments and methods, IJA 2011, 10 (3),
141;[2] Clarke, J., Stoker, C. Concretions in exhumed & inverted
channels near Hanksville Utah: implications for Mars, (IJA 2011, 10
(3), 162;[3] Thiel et al., (2011) PCR-based analysis of microbial
communities during the EuroGeoMars campaign at Mars Desert Research
Station, Utah. (IJA 2011, 10 (3), 177;[4] Direito et al. (2011). A
wide variety of putative extremophiles and large beta-diversity at
the Mars Desert Research Station (Utah). (IJA 2011, 10 (3), 191;[5]
Orzechowska, G. et al (20110 analysis of Mars Analog soils using
solid Phase Microextraction, Organics solvent extraction and GCMS,
(IJA 2011, 10 (3), 209; [6] Kotler et al. (2011). Analysis of mineral
matrices of planetary soils analogs from the Utah Desert. (IJA 2011,
10 (3), 221; [7] Martins et al. (2011). Extraction of amino acids from
soils close to the Mars Desert Research Station (MDRS), Utah. (IJA
2011, 10 (3), 231; [8] Ehrenfreund et al. (2011) Astrobiology and
habitability studies in preparation for future Mars missions: trends
from investigating minerals, organics and biota. (IJA 2011, 10 (3),
239; [9] Stoker C. et al (2011) Mineralogical, Chemical, Organic &
Microbial Properties of Subsurface Soil Cores from Mars Desert Research
Station, a Phyllosilicate and Sulfate Rich Mars Analog Site, IJA 2011,
10 (3), 269; [10] Rodrigues L. et al (2014, in preparation) Preventing
biocontamination during sterile sampling; [11] Rodrigues L. et al (2014,
in preparation) Microbial diversity in MDRS rocks and soils; [12] ILEWG
EuroMoonMars Team, (2014, special issue in preparation) Results from
ILEWG EuroMoonMars campaign 2013 **Acknowledgements: B.H.Foing (1, 2,
6), C. Stoker (3), P. Ehrenfreund (4, 5), I. Rammos (2), L. Rodrigues
(2), A. Svendsen (2), D. Oltheten (2), K. Nebergall (6), M. Battler (6,
7), H. v't Houd (8), A. Bruneau (6,9), M. Cross (6,7), V. Maivald (10),
C. Orgel (6), A. Elsaesser (4), S.O.L. Direito (2,4), W.F.M. Röling
(2), G.R. Davies (2); EuroGeoMars2009 Team, DOMMEX-ILEWG EuroMoonMars
2010-2013 Teams (1) ESA/ ESTEC, Postbus 299, 2200 AG Noordwik, NL; (2)
Vrije Universiteit, Amsterdam, NL; (3) NASA Ames Research Centre; US;
(4) Leiden U. , NL; (5) Space Policy Institute, GWU, Washington D.C.,
USA; (6) ILEWG; (7) CPSX; (8) Cerberus Blackshore, ESIC Noordwijk, NL;
(9) ENSC Bordeaux; (10) DLR, Bremen
Title: Reports and recommendations from COSPAR Planetary Exploration
Committee (PEX) & International Lunar Exploration Working Group
(ILEWG)
Authors: Ehrenfreund, Pascale; Foing, Bernard
Bibcode: 2014EGUGA..1616942E
Altcode:
In response to the growing importance of space exploration,
the objectives of the COSPAR Panel on Exploration (PEX) are to
provide high quality, independent science input to support the
development of a global space exploration program while working
to safeguard the scientific assets of solar system bodies. PEX
engages with COSPAR Commissions and Panels, science foundations,
IAA, IAF, UN bodies, and IISL to support in particular national
and international space exploration working groups and the new era
of planetary exploration. COSPAR's input, as gathered by PEX, is
intended to express the consensus view of the international scientific
community and should ultimately provide a series of guidelines to
support future space exploration activities and cooperative efforts,
leading to outstanding scientific discoveries, opportunities for
innovation, strategic partnerships, technology progression, and
inspiration for people of all ages and cultures worldwide. We shall
focus on the lunar exploration aspects, where the COSPAR PEX is
building on previous COSPAR, ILEWG and community conferences. An
updated COSPAR PEX report is published and available online
(Ehrenfreund P. et al, COSPAR planetary exploration panel report,
http://www.gwu.edu/~spi/assets/COSPAR_PEX2012.pdf). We celebrate
20 years after the 1st International Conference on Exploration and
Utilisation of the Moon at Beatenberg in June 1994. The International
Lunar Exploration Working Group (ILEWG) was established the year after
in April 1995 at an EGS meeting in Hamburg, Germany. As established
in its charter, this working group reports to COSPAR and is charged
with developing an international strategy for the exploration of the
Moon (http://sci.esa.int/ilewg/ ). It discusses coordination between
missions, and a road map for future international lunar exploration
and utilisation. It fosters information exchange or potential and
real future lunar robotic and human missions, as well as for new
scientific and exploration information about the Moon. We present the
GLUC/ICEUM11 declaration (with emphasis on Science and exploration;
Technologies and resources, Infrastructures and human aspects; Moon,
Space, Society and Young Explorers) (http://sci.esa.int/iceum11). We
give a report on ongoing relevant ILEWG community activities. We discuss
how lunar missions SMART-1, Kaguya, Chang'E1&2, Chandrayaan-1,
LCROSS, LRO, GRAIL, LADEE, Chang'E3 and upcoming missions contribute
to lunar exploration objectives & roadmap.
Title: Lunar Exploration and Science in ESA
Authors: Carpenter, James; Houdou, Bérengère; Fisackerly, Richard;
De Rosa, Diego; Patti, Bernardo; Schiemann, Jens; Hufenbach, Bernhard;
Foing, Bernard
Bibcode: 2014EGUGA..1616932C
Altcode:
ESA seeks to provide Europe with access to the lunar surface, and
allow Europeans to benefit from the opening up of this new frontier,
as part of a global endeavor. This will be best achieved through an
exploration programme which combines the strengths and capabilities
of both robotic and human explorers. ESA is preparing for future
participation in lunar exploration through a combination of human and
robotic activities, in cooperation with international partners. Future
planned activities include the contribution of key technological
capabilities to the Russian led robotic missions, Luna-Glob,
Luna-Resurs orbiter and Luna-Resurs lander. For the Luna-Resurs
lander ESA will provide analytical capabilities to compliment the
already selected Russian led payload, focusing on the composition and
isotopic abundances of lunar volatiles in polar regions. This should
be followed by the contributions at the level of mission elements to
a Lunar Polar Sample Return mission. This partnership will provide
access for European investigators to the opportunities offered by
the Russian led instruments on the missions, as well as providing
Europe with a unique opportunity to characterize and utilize polar
volatile populations. Ultimately samples of high scientific value,
from as of yet unexplored and unsampled locations shall be made
available to the scientific community. These robotic activities are
being performed with a view to enabling a future more comprehensive
programme in which robotic and human activities are integrated to
provide the maximum benefits from lunar surface access. Activities on
the ISS and ESA participation to the US led Multi-Purpose Crew Vehicle,
which is planned for a first unmanned lunar flight in 2017, are also
important steps towards achieving this. All of these activities are
performed with a view to generating the technologies, capabilities,
knowledge and heritage that will make Europe an indispensable partner
in the exploration missions of the future.
Title: ESTEC/GEOVUSIE/ILEWG Planetary Student Designer Workshop:
a Teacher Training Perspective
Authors: Preusterink, J.; Foing, B. H.; Kaskes, P.
Bibcode: 2014EPSC....9..837P
Altcode:
An important role for education is to inform and create the right
skills for people to develop their own vision, using their talents to
the utmost and inspire others to learn to explore in the future. Great
effort has been taken to prepare this interactive design workshop
thoroughly. Three days in a row, starting with presentations of
Artscience The Hague to ESA colleagues, followed by a Planetary
research Symposium in Amsterdam and a student design workshop at
the end complemented a rich environment with the focus on Planetary
exploration. The design workshop was organised by GeoVUsie students,
with ESTEC and ILEWG support for tutors and inviting regional and
international students to participate in an interactive workshop to
design 5 Planetary Missions, with experts sharing their expertise and
knowhow on specific challenging items: 1. Mercury - Post BepiColombo
(with Sebastien Besse, ESA) 2. Moon South Pole Mission (with Bernard
Foing, ESA) 3. Post-ExoMars - In search for Life on Mars (with
Jorge Vago, ESA) 4. Humans in Space - Mars One investigated(with
Arno Wielders, Space Horizon) 5. Europa - life on the icy moon of
Jupiter? (with Bert Vermeersen, TU Delft. Lectures were given for
more than 150 geology students at the symposium "Moon, Mars and More"
at VU university, Amsterdam (organized by GeoVUsie earth science
students). All students were provided with information before and at
start for designing their mission. After the morning session there was
a visit to the exhibition at The Erasmus Facility - ESTEC to inspire
them even more with real artifacts of earlier and future missions into
space. After this visit they prepared their final presentations, with
original results, with innovative ideas and a good start to work out
further in the future. A telescope session for geology students had been
organized indoor due to rain. A follow-up visit to the nearby public
Copernicus observatory was planned for another clear sky occasion.
Title: Laboratory Analysis of Analogue Samples from ILEWG EuroMoonMars
campaigns
Authors: Foing, B.; Elsaesser, A.; Rodrigues, L.; Ehrenreund, P.;
Stoker, C.; Rammos, I.; Svendsen, A.; Oltheten, D.; Nebergall, K.;
Battler, M.; v't Houd, H.; Bruneau, A.; Cross, M.; Maivald, V.; Orgel,
C.; Direito, S. O. L.; Roeling, W. F. M.; Davies, G. R.
Bibcode: 2014EPSC....9..822F
Altcode:
We report on the laboratory analysis from samples obtained during
ILEWG EuroMoonMars campaigns (2009 to 2013) at Mars Desert Research
station, near Hanksville Utah. The samples were acquired, transported
and curated, and then measured in the laboratory using diverse
techniques. We shall present new measurements from latest campaigns
relevant to the study of minerals, and the detectionof organics and
signs of life.
Title: Lunar Exploration and Science Opportunities in ESA
Authors: Carpenter, J.; Houdou, B.; Fisackerly, R.; De Rosa, D.;
Schiemann, J.; Patti, B.; Foing, B.
Bibcode: 2014EPSC....9..845C
Altcode:
ESA seeks to provide Europe with access to the lunar surface, and
allow Europeans to benefit from the opening up of this new frontier,
as part of a global endeavour. This will be best achieved through an
exploration programme which combines the strengths and capabilities
of both robotic and human explorers. ESA is preparing for future
participation in lunar exploration through a combination of human and
robotic activities, in cooperation with international partners. Future
planned activities include the contribution of key technological
capabilities to the Russian led robotic missions, Luna-Glob,
Luna-Resurs orbiter and Luna-Resurs lander. For the Luna-Resurs
lander ESA will provide analytical capabilities to compliment the
already selected Russian led payload, focusing on the composition and
isotopic abundances of lunar volatiles in polar regions. This should
be followed by the contributions at the level of mission elements to
a Lunar Polar Sample Return mission. This partnership will provide
access for European investigators to the opportunities offered by
the Russian led instruments on the missions, as well as providing
Europe with a unique opportunity to characterize and utilize polar
volatile populations. Ultimately samples of high scientific value,
from as of yet unexplored and unsampled locations shall be made
available to the scientific community. These robotic activities are
being performed with a view to enabling a future more comprehensive
programme in which robotic and human activities are integrated to
provide the maximum benefits from lunar surface access. Activities on
the ISS and ESA participation to the US led Multi-Purpose Crew Vehicle,
which is planned for a first unmanned lunar flight in 2017, are also
important steps towards achieving this. All of these activities are
performed with a view to generating the technologies, capabilities,
knowledge and heritage that will make Europe an indispensible partner
in the exploration missions of the future. We report on the current
status of the European elements in this cooperative scenario, with
an emphasis on the investigations to be performed at the lunar
surface. These investigations should generate knowledge that can
be enabling for exploration in the future, and should also have a
significant fundamental scientific return.
Title: SMART-1 was travelling to the Moon, 10 years ago
Authors: Foing, B. H.
Bibcode: 2014EPSC....9..826F
Altcode:
Ten years ago, the ESA SMART-1 spacecraft was still on its way to the
Moon with lunar orbital capture achieved on 13 November 2004. We review
the legacy of SMART-1 for lunar science and exploration, applications
and for preparing future orbital and lander missions.
Title: Lunar Exploration and Science in ESA
Authors: Carpenter, J.; Houdou, B.; Fisackerly, R.; De Rosa, D.;
Patti, B.; Schiemann, J.; Hufenbach, B.; Foing, B.
Bibcode: 2014EPSC....9..840C
Altcode:
ESA seeks to provide Europe with access to the lunar surface, and
allow Europeans to benefit from the opening up of this new frontier,
as part of a global endeavor. This will be best achieved through an
exploration programme which combines the strengths and capabilities
of both robotic and human explorers. ESA is preparing for future
participation in lunar exploration through a combination of human and
robotic activities, in cooperation with international partners. Future
planned activities include the contribution of key technological
capabilities to the Russian led robotic missions, Luna-Glob,
Luna-Resurs orbiter and Luna-Resurs lander. For the Luna-Resurs
lander ESA will provide analytical capabilities to compliment the
already selected Russian led payload, focusing on the composition and
isotopic abundances of lunar volatiles in polar regions. This should
be followed by the contributions at the level of mission elements to
a Lunar Polar Sample Return mission. This partnership will provide
access for European investigators to the opportunities offered by
the Russian led instruments on the missions, as well as providing
Europe with a unique opportunity to characterize and utilize polar
volatile populations. Ultimately samples of high scientific value,
from as of yet unexplored and unsampled locations shall be made
available to the scientific community. These robotic activities are
being performed with a view to enabling a future more comprehensive
programme in which robotic and human activities are integrated to
provide the maximum benefits from lunar surface access. Activities on
the ISS and ESA participation to the US led Multi-Purpose Crew Vehicle,
which is planned for a first unmanned lunar flight in 2017, are also
important steps towards achieving this. All of these activities are
performed with a view to generating the technologies, capabilities,
knowledge and heritage that will make Europe an indispensible partner
in the exploration missions of the future. We report on the current
status of the European elements in this cooperative scenario, with
an emphasis on the investigations to be performed at the lunar
surface. These investigations should generate knowledge that can
be enabling for exploration in the future, and should also have a
significant fundamental scientific return.
Title: Lunar Team Report from a Planetary Design Workshop at ESTEC
Authors: Gray, A.; MacArthur, J.; Foing, B. H.
Bibcode: 2014EPSC....9..827G
Altcode:
On February 13, 2014, GeoVUsie, a student association for Earth science
majors at Vrijie University (VU), Amsterdam, hosted a Planetary
Sciences: Moon, Mars and More symposium. The symposium included a
learning exercise the following day for a planetary design workshop
at the European Space Research and Technology Centre (ESTEC) for
30 motivated students, the majority being from GeoVUsie with little
previous experience of planetary science. Students were split into five
teams and assigned pre-selected new science mission projects. A few
scientific papers were given to use as reference just days before the
workshop. Three hours were allocated to create a mission concept before
presenting results to the other students and science advisors. The
educational backgrounds varied from second year undergraduate students
to masters' students from mostly local universities.The lunar team
was told to design a mission to the lunar south pole, as this is a
key destination agreed upon by the international lunar scientific
community. This region has the potential to address many significant
objectives for planetary science, as the South Pole-Aitken basin has
preserved early solar system history and would help to understand
impact events throughout the solar system as well as the origin and
evolution of the Earth-Moon system, particularly if samples could be
returned. This report shows the lunar team's mission concept and reasons
for studying the origin of volatiles on the Moon as the primary science
objective [1]. Amundsen crater was selected as the optimal landing site
near the lunar south pole [2]. Other mission concepts such as RESOLVE
[3], L-VRAP [4], ESA's lunar lander studies and Luna-27 were reviewed. A
rover and drill were selected as being the most suitable architecture
for the requirements of this mission. Recommendations for future student
planetary design exercises were to continue events like this, ideally
with more time, and also to invite a more diverse range of educational
backgrounds, i.e., both engineering and science students/professionals.
Title: Field research operations and measurements from ILEWG
EuroMoonMars campaigns in Utah
Authors: Foing, B.; Stocker, C.; Ehrenfreund, P.; Battler, M.; v't
Houd, H.; Elsaesser, A.; Rammos, I.; Rodrigues, L.; Direito, S. O. L.;
Roeling, W. F. M.; Davies, G. R.
Bibcode: 2014EPSC....9..821F
Altcode:
We have conducted a s series of field researchcampaigns (ILEWG
EuroMoonMars) in the extreme environment of the Utah desert relevant
to habitability and astrobiology in Mars environments in order to help
in the interpretation of Mars missions measurements from orbit (MEX,
MRO) or from the surface (MER, MSL). We describe the field operations
and the comparison between remote sensing and in-situ data.
Title: Star Mapping with Slime Mold Physarum Polycephalum
Authors: Mihklepp, M.; Domnitch, E.; Gelfand, D.; Foing, B. H.;
van der Heide, E.
Bibcode: 2014EPSC....9..830M
Altcode:
Human curiosity and exploration towards outer space has led to many
fantastic inventions and given way to alternative scenarios about
the origins of life. In the Space Science in the Arts course together
with ESTEC with support from ILEWG. I got interested about unicellular
slime mold Physarum polycephalum. There has been and still is a lot of
research on Physarum polycephalum. This brainless eucaryotic microbe
has its smartness and external memory strategies. Physarum can navigate
through a maze made of agar using the shortest route possible when
two pieces of food are placed at two separate exits of the maze. It
can build efficient networks - Physarum created network similar to
the existing Tokyo train system. It is being used to control a robot,
in USB-sensor and in sound synthesis. Right now there is a lot of
research about using Physarum in bio-computing.
Title: Artistic Research on Freedom in Space and Science
Authors: Schelfhout, R.; Foing, B. H.; Domnich, E.; Gelfand, D.;
van der Heide., E.
Bibcode: 2014EPSC....9..829S
Altcode:
Space science in the arts. Since the earliest scientific preparations
for extraterrestrial travel at the beginning of the 20th century,
the exploration of outer space has become a quitessential framework
of the human condition and its creative manifestations. Although
the artistic pursuit of space science is still in its infancy, an
accelerated evolution is currently underway.
Title: The Martian Geomorphology as Mapped by the Mars Express
High Resolution Stereo Camera (HRSC): Implications for Geological
Processes and Climate Conditions
Authors: Jaumann, R.; Neukum, G.; Tirsch, D.; Hauber, E.; Hoffmann,
H.; Roatsch, T.; Gwinner, K.; Scholten, F.; Ansan, V.; Baratoux,
D.; DiAchille, G.; Duxbury, T.; Erkeling, G.; Foing, B.; Fueten, F.;
van Gasselt, S.; Gupta, S.; Head, J. W.; Hiesinger, H.; Ip, W. H.;
Keller, H. U.; Kleinhans, M.; Kneissl, T.; Le Deit, L.; Mangold, N.;
McCord, T. B.; Michael, G.; Muller, J. P.; Murray, J.; Pacifici, A.;
Platz, T.; Pinet, P.; Pondrelli, M.; Raack, J.; Reiss, D.; Rossi,
A. P.; Spohn, T.; Sowe, M.; Stephan, K.; Wendt, L.; Williams, D. A.;
HRSC Science Team
Bibcode: 2014LPI....45.1772J
Altcode:
After 10 years of orbiting the planet, HRSC on Mars Express has covered
about 90% of the surface in stereo and color with resolutions up to
10 m/pixel.
Title: Results from ILEWG EuroMoonMars Analogue Field Research
Campaigns
Authors: Foing, B. H.; Stoker, C.; ILEWG Euromoonmars Collaboration
Bibcode: 2014LPI....45.2675F
Altcode:
We discuss results of field analog research campaigns (ILEWG
EuroMoonMars) in support of Mars astrobiology studies, and Moon/Mars
robotic and human missions.
Title: Artistic Research on Freedom in Space and Science
Authors: Schelfhout, R.; Foing, B. H.; Domnich, E.; Gelfand, D.;
van der Heide., E.; Ilewg
Bibcode: 2014LPI....45.2808S
Altcode:
This ArtScience Research project with support from ESA/ESTEC and ILEWG
describes an artistic biodome installation as paradigm for freedom in
space and science.
Title: Exploring the Limits to Observational Diffuse Interstellar
Band Studies
Authors: Foing, B. H.
Bibcode: 2014IAUS..297...51F
Altcode:
The status of DIB research (Herbig 1995) has strongly advanced since
the DIB conference in Boulder in 1994. In the same year we reported the
discovery of two near IR diffuse bands coincident with C60
+, that was confirmed in subsequent years. Since then a
number of DIB observational studies have been published such as DIB
surveys, measurements of DIB families, correlations and environment
dependences as well as DIBs in extra-galactic sources. Resolved
substructures were measured and compared to predicted rotational
contours of large molecules. Polarisation studies provided constraints
on possible carrier molecules and upper limits. DIBs carriers have
been linked with several classes of organic molecules observed in
the interstellar medium, in particular to the UIR bands (assigned
to PAHs), the Extended Red Emission (ERE) or the recently detected
Anomalous Microwave Emission (AME, assigned to spinning dust). In
particular fullerenes and PAHs have been proposed to explain some
DIBs and specific molecules were searched for in DIB spectra. DIB
carriers could be present in various dehydrogenation and ionization
states. Experiments in the laboratory and in space contribute to our
understanding of the photo-stability of possible DIB carriers. In
summary, the status of DIB research in the last 20 years has strongly
advanced. We review DIB observational results and their interpretation
and introduce the relevant plenary discussion.
Title: X-Shooter Survey of Near-Infrared DIBs
Authors: Cox, N. L. J.; Cami, J.; Kaper, L.; Foing, B. H.; Ehrenfreund,
P.; Ochsendorf, B. B.; van Hooff, S. H. M.; Salama, F.
Bibcode: 2014IAUS..297..103C
Altcode:
We present the first results of an exploratory VLT/X-Shooter survey
of near-infrared diffuse interstellar bands (DIBs) in diffuse to
translucent interstellar clouds. These observations confirm the
presence of recently discoved NIR DIBs and provide more accurate rest
wavelengths and line widths. Example spectra are shown for the reddened,
AV ~ 10 mag, line-of-sight towards the distant binary system
4U 1907+09.
Title: Lunar Exploration and Science in ESA
Authors: Carpenter, James; Foing, Bernard H.; Fisackerly, Richard;
Houdou, Berengere; De Rosa, Diego; Patti, Bernado; Schiemann, Jens
Bibcode: 2014cosp...40E.459C
Altcode:
ESA seeks to provide Europe with access to the lunar surface, and allow
Europeans to benefit from the opening up of this new frontier, as part
of a global endeavor. This will be best achieved through an exploration
programme which combines the strengths and capabilities of both robotic
and human explorers. ESA is preparing for future participation in lunar
exploration through a combination of human and robotic activities,
in cooperation with international partners. Future planned activities
include the contribution of key technological capabilities to the
Russian led robotic missions, Luna-Glob, Luna-Resurs orbiter and
Luna-Resurs lander. For the Luna-Resurs lander ESA will provide
analytical capabilities to compliment the already selected Russian led
payload, focusing on the abundance, composition and isotopes of lunar
volatiles in polar regions, and their associated chemistry. This should
be followed by the contributions at the level of mission elements to
a Lunar Polar Sample Return mission. This partnership will provide
access for European investigators to the opportunities offered by
the Russian led instruments on the missions, as well as providing
Europe with a unique opportunity to characterise and utilise polar
volatile populations. Ultimately samples of high scientific value,
from as of yet unexplored and unsampled locations shall be made
available to the scientific community. These robotic activities are
being performed with a view to enabling a future more comprehensive
programme in which robotic and human activities are integrated to
provide the maximum benefits from lunar surface access. Activities on
the ISS and ESA participation to the US Multi-Purpose Crew Vehicle,
which is planned for a first unmanned lunar flight in 2017, are also
important steps towards achieving this. All of these activities are
performed with a view to generating the technologies, capabilities,
knowledge and heritage that will make Europe an indispensable partner
in the exploration missions of the future.
Title: Report from International Lunar Exploration Working Group
(ILEWG) to COSPAR
Authors: Foing, Bernard H.
Bibcode: 2014cosp...40E.882F
Altcode:
We refer to COSPAR and ILEWG ICEUM and lunar conferences and
declarations [1-18]. We discuss how lunar missions SMART-1, Kaguya,
Chang'E1&2, Chandrayaan-1, LCROSS, LRO, GRAIL, LADEE, Chang'E3
and upcoming missions contribute to lunar exploration objectives
& roadmap. We present the GLUC/ICEUM11 declaration and give a
report on ongoing relevant ILEWG community activities, with focus
on: “1. Science and exploration - World-wide access to raw and
derived (geophysical units) data products using consistent formats
and coordinate systems will maximize return on investment. We call to
develop and implement plans for generation, validation, and release
of these data products. Data should be made available for scientific
analysis and supporting the development and planning of future missions
- There are still Outstanding Questions: Structure and composition of
crust, mantle, and core and implications for the origin and evolution
of the Earth-Moon system; Timing, origin, and consequences of late heavy
bombardment; Impact processes and regolith evolution; Nature and origin
of volatile emplacement; Implications for resource utilization. These
questions require international cooperation and sharing of results
in order to be answered in a cost-effective manner - Ground truth
information on the lunar far side is missing and needed to address many
important scientific questions, e.g. with a sample return from South
Pole-Aitken Basin - Knowledge of the interior is poor relative to the
surface, and is needed to address a number of key questions, e.g. with
International Lunar Network for seismometry and other geophysical
measurements - Lunar missions will be driven by exploration, resource
utilization, and science; we should consider minimum science payload
for every mission, e.g., landers and rovers should carry instruments to
determine surface composition and mineralogy - It is felt important to
have a shared database about previous missions available for free, so as
to provide inputs to future missions, including a gap analysis of needed
measurements. Highly resolved global data sets are required. Autonomous
landing and hazard avoidance will depend on the best topographic map
of the Moon, achievable by combining shared data. - New topics such as
life sciences, partial gravity processes on the Moon should be followed
in relation to future exploration needs.” http://sci.esa.int/ilewg/
http://sci.esa.int/ilewg/47170-gluc-iceum11-beijing-2010lunar-declaration/
References: [1] 1st International Lunar Workshop, Balsiger H. et
al., Editors, European Space Agency, 1994. ESA-SP-1170. [2]
2nd International Lunar Workshop, Kyoto, H. Mizutani, editor,
Japan Space Forum Publisher, 1997. [3] 3rd International Lunar
Workshop, Moscow 1998, E. Galimov, editor. [4] ICEUM4, ESTEC,
2000, ESA SP-462, B.H. Foing & M. Perry, editors. [5] ICEUM5,
Hawaii Nov 2003, Durst S.M. et al, Editors, Vol 108, 1-576 pp,
Science and Technology Series, American Astronautical Society,
2004. [6] ICEUM6, Udaipur 2004, Bhandari N., Editor, Journal Earth
Sys-tem Science, India, 114, No6, Dec 2005, pp. 573-841. [7] ICEUM7,
Toronto Sept 2005, sci.esa.int/ilewg. [8] ICEUM8, Beijing July 2006,
Journal of Chinese Society of Astronautics, Vol. 28 Sup., 2007, Ji W.,
Editor. [9] ICEUM9, Sorrento, Italy, Foing B., Espinasse S., Kosters G.,
Editors. http://sci.esa.int/iceum9, Dec. 2007), [11] Ehrenfreund, P.,
Foing, B.H., Cellino, A. Editors, The Moon and Near Earth Objects, ASR
Vol 37, 1, 2006. [12] Foing, B.H. et al editors, 'Astronomy and Space
Science from the Moon', ASR 14, 6, 1994. [13] Ip W.-H., Foing, B.H.,
Masson Ph.L., editors, The Moon and Mars, ASR Vol 23, 11, 1999. [14]
Foing, B.H. et al, editor, Lunar Exploration, Planetary and Space
Science, Vol 50, 14-15, 2002. [15] Foing, B.H., Heather, D. editors,
'Lunar Exploration 2000', ASR Vol 30, Nr 8, 2002. [16] Huntress,
W. et al 'The next steps in exploring deep space - A cosmic study by
the IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377. [17]
http://sci.esa.int/ilewg/43654-declaration-iceum10-leag-srr-florida-2008/
[18] Ehrenfreund P. et al (COSPAR planetary exploration panel report)
2012, ASR Vol 49, Nr 1, pp. 2-48.
Title: Astrobiology Results from ILEWG EuroMoonMars Analogue Field
Research
Authors: Foing, Bernard H.
Bibcode: 2014cosp...40E.883F
Altcode:
We give an update on the astrobiology results from a series of field
research campaigns (ILEWG EuroMoonMars) in the extreme environment of
the Utah desert. These are relevant to prepare future lunar landers
and polar sample return missions, interpret Moon-Mars data (eg SMART1,
LRO, Mars Express, MRO, MER, MSL), study habitability and astrobiology
in Moon-Mars environments, or to test human-robotic surface EVA or base
operations. In the frame of ILEWG EuroMoonMars campaigns (2009 to 2013)
we deployed at Mars Desert Research station near Hanksville Utah, a
suite of instruments and techniques [0, 1, 2, 9-11] including sample
collection, context imaging from re-mote to local and microscale,
drilling, spectrometers and life sensors. We analyzed how geological
and geo-chemical evolution affected local parameters (mineralogy,
organics content, environment variations) and the habitability
and signature of organics and biota. Results: Among the important
findings are the diversity in the composition of soil samples even
when collected in close proximity, the low abundances of detectable
PAHs and amino acids and the presence of biota of all three domains
of life with significant heterogeneity. An extraordinary variety of
putative extremophiles was observed [3,4,9]. A dominant factor seems
to be soil porosity and lower clay-sized particle content [6-8]. A
protocol was developed for sterile sampling, contamination issues,
and the diagnostics of biodiversity via PCR and DGGE analysis in soils
and rocks samples [10, 11]. We compare the 2009 campaign results [0-9]
to new measurements from 2010-2013 campaigns relevant to: comparison
between remote sensing and in-situ measurements; the study of minerals;
the detection of organics and signs of life. We acknowledge team
members and supporting institutes: B.H. Foing (1, 2, 6), C. Stoker (3),
P. Ehrenfreund (4, 5), I. Rammos (2), L. Rodrigues (2), A. Svendsen (2),
D. Oltheten (2), I. Schlacht (2), K. Nebergall (6), M. Battler (6, 7),
H. v’t Houd (8), A. Bruneau (6,9), M. Cross (6,7), V. Maivald (10),
C. Orgel (6), A. Elsaesser (4), S.O.L. Direito (2,4), W.F.M. Röling
(2), G.R. Davies (2); EuroGeoMars2009 Team, DOMMEX-ILEWG EuroMoonMars
2010-2013 Teams (1) ESA/ ESTEC, Postbus 299, 2200 AG Noordwik, NL;
(2) Vrije Universiteit, Amsterdam, Faculty of Earth & Life
Sciences, De Boelelaan 1085, 1081 HV Amsterdam, NL; (3) NASA Ames
Research Centre; US; (4) Leiden Institute of Chemistry, NL; (5) Space
Policy Institute, GWU, Washington D.C., USA; (6) ILEWG; (7) CPSX;
(8) Cerberus Blackshore, ESIC Noordwijk, NL; (9) ENSC Bordeaux; (10)
DLR, Bremen References: Foing, Stoker & Ehrenfreund (Editors, 2011)
“Astrobiology field Research in Moon/Mars Analogue Environments”,
Special Issue of International Journal of Astrobiology , IJA 2011, 10,
vol.3. 137-305; [1] Foing B. et al. (2011) Field astrobiology research
at Moon-Mars analogue site: Instruments and methods, IJA 2011, 10 (3),
141; [2] Clarke, J., Stoker, C. Concretions in exhumed & inverte
channels near Hanksville Utah: implications for Mars, (IJA 2011, 10
(3), 162; [3] Thiel et al., (2011) PCR-based analysis of microbial
communities during the EuroGeoMars campaign at Mars Desert Research
Station, Utah. (IJA 2011, 10 (3), 177; [4] Direito et al. (2011). A
wide variety of putative extremophiles and large beta-diversity at
the Mars Desert Research Station (Utah). (IJA 2011, 10 (3), 191;
[5] Orzechowska, G. et al (20110 analysis of Mars Analog soils using
solid Phase Microextraction, Organics solvent extraction and GCMS,
(IJA 2011, 10 (3), 209; [6] Kotler et al. (2011). Analysis of mineral
matrices of planetary soils analogs from the Utah Desert. (IJA 2011,
10 (3), 221; [7] Martins et al. (2011). Extraction of amino acids from
soils close to the Mars Desert Research Station (MDRS), Utah. (IJA
2011, 10 (3), 231; [8] Ehrenfreund et al. (2011) Astrobiology and
habitability studies in preparation for future Mars missions: trends
from investigating minerals, organics and biota. (IJA 2011, 10 (3),
239; [9] Stoker C. et al (2011) Mineralogical, Chemical, Organic &
Microbial Properties of Subsurface Soil Cores from Mars Desert Research
Station, a Phyllosilicate and Sulfate Rich Mars Analog Site, IJA 2011,
10 (3), 269; [10-11] Rodrigues L. et al (2014, in preparation)
Title: Artistic Research on Freedom in Space and Science
Authors: Foing, Bernard H.; Schelfhout, Ronald; Gelfand, Dmitry;
Van der Heide, Edwin; Preusterink, Jolanda; Domnitch, Evelina
Bibcode: 2014cosp...40E.886F
Altcode:
ArtScience ESTEC: Space science in the arts. Since the earliest
scientific preparations for extra-terrestrial travel at the beginning
of the 20th century, the exploration of outer space has become a
quintessential framework of the human condition and its creative
manifestations. Although the artistic pursuit of space science
is still in its infancy, an accelerated evolution is currently
underway. Perspective: With the current state of the planet and the
development of technology, humankind has the ability to look from a
greater distance to the damage that has been done. This offers potential
in the form of early detection and prevention of disasters. Meanwhile
our aim seems to be directed away from the earth into the universe. In
the Space science in the arts project I tried to encapsulate these two
viewpoints that tend to avoid each other. We are still earthbound and
that is our basis. A tree cannot grow tall without strong roots. Space,
a promise of freedom. Line of thought: Space sounds like freedom but
to actually send people out there they have to be strapped tightly
on top of a giant missile to reach a habitat of interconnecting
tubes with very little space. It is impossible to escape protocol
with- out risking your life and the lives of astronauts have been
fixed years in advance. This is the human predicament which does not
apply to the telescopes and other devices used to reach far into the
universe. Providing information instantly the various forms of light
allow us to travel without moving. Description of the installation:
The research on freedom in space and science led to the development
of an installation that reflects the dualistic aspect which clings
to the exploration of the universe. The installation is a model
on multiple scales. You can look at the material or the feeling it
evokes as well as at the constantly changing projections. The image
is light. Inside this glass circle there is a broken dome placed over
a dark and reflective surface on which light manipulating machines
continuously alter the projected image. Development: In order to
delve deeper into the subject of freedom in space and science this
setup can serve as a vantage point. And it can offer an interactive
environment to explore notions of freedom in space and science. The
addition of a specific environment around and above the installation,
referring to the fabric of space would highly increase the impact it
has on an audience. You would then be able to immerse yourself in the
world of this settlement, somewhere in outer space. Sound, light and
projection screens will orbit the table changing the projections even
more. Triggering the imagination with every movement. Results: Freedome
has been exhibited at TecArt in Rotterdam, at ILEWG/Artscience day and
the Lunar conference at ESTEC in February 2014. The images underneath
(courtesy J. Preusterink BH Foing) depict the installation in some ways
it can be experienced http://www.youtube.com/watch?v=Qn8DHARrlU (images:
Jolanda Preusterink and Bernard Foing, from ILEWG/ESTEC/ArtScience-The
Hague workshop Space Science in the Arts) Authors: Ronald Schelfhout,
Bernard Foing, Evelina Domnitch, Dmitry Gelfand, Edwin van der Heide,
Jolanda Preusterink
Title: Outreach and capacity building activities for engaging youth
and public in Exploration
Authors: Foing, Bernard H.
Bibcode: 2014cosp...40E.885F
Altcode:
We report to the COSPAR Panel on Education and relevant community
on activities, pilot projects and results relevant for outreach
and engagement in exploration. Number of activities were developed
in the frame of the International Lunar Exploration Working Group
(ILEWG) including the participation of students in lunar symposia,
space conferences or ICEUM International Conferences on Exploration
and Utilisation of the Moon* ILEWG with support from various space
agencies, universities and institutions has organized events for young
professionals with a wide background (including scientist, engineers,
humanistic, law, art students) a Moon academy, lunar and planetary
students work-shops, technical training workshops, international observe
the Moon sessions. ILEWG has organised or sponsored participants
to a series of field training and research campaigns in Utah desert
research station, Eifel volcanic park, Iceland, Rio Tinto, La Reunion
island. Education and outreach projects used space missions data
(SMART-1 views of the Moon, Earth views from space, Mars views,
Mars crowdsourcing games, astronomy data analysis) to engage the
public in citizen science and exploration. Artistic and sociological
projects (e.g. "social lunar telescope, lunar zen garden, Moon academy,
MoonLife, MoonLife concept store, Moon republic, artscience projects,
space science in the arts, artists in residence, artists in MoonMars
base") were also initiated with artists to engage the wide public in
exploration. A number of projects have been developed with support
from ITACCUS IAF committee. We shall discuss how these pilot projects
could be expanded for the benefit of future space projects, young
professionals, the space community and the public. Acknowledgements:
we thank collaborators from ILEWG community and partner institutes
for the different projects mentioned http://sci.esa.int/ilewg/
http://sci.esa.int/ilewg/47170-gluc-iceum11-beijing-2010lunar-declaration/
Foing B., Stoker C., Ehrenfreund P., Astrobiology
field research in Moon/Mars , IJA, 10,Special Issue 03 (2011)
https://www.google.nl/?gfe_rd=cr&ei=D4MHU5CMB4ve8gfzl4DQCg#q=ilewg+euromoonmars
http://www.aliciaframis.com/Moonlife_Concept.html
http://www.artscatalyst.org/experiencelearning/detail/itaccus/
Title: Report from ILEWG to the COSPAR Panel on Exploration
Authors: Foing, Bernard H.
Bibcode: 2014cosp...40E.884F
Altcode:
The International Lunar Exploration Working Group (ILEWG) was
established in April 1995 at a meeting in Hamburg, Germany. As
established in its charter, this working group reports to COSPAR and is
charged with developing an international strategy for the exploration
of the Moon. It discusses coordination between missions, and a road
map for future international lunar exploration and utilisation. It
fosters information exchange or potential and real future lunar robotic
and human missions, as well as for new scientific and exploration
information about the Moon. ILEWG was used to feed forward results
from lunar missions such as SMART1 to the next ones, and we look now to
integrate lessons from all recent orbiters and landers, for the upcoming
landers, sample return missions, and human activities. We give a report
on ILEWG community activities, refer to COSPAR and ILEWG ICEUM and
lunar conferences and declarations [1-18], and discuss the follow-up
of GLUC/ICEUM11 declaration relevant to COSPAR PEX*. References: [1]
1st International Lunar Workshop, Balsiger H. et al., Editors, European
Space Agency, 1994. ESA-SP-1170. [2] 2nd International Lunar Workshop,
Kyoto, H. Mizutani, editor, Japan Space Forum Publisher, 1997. [3]
3rd International Lunar Workshop, Moscow 1998, E. Galimov, editor. [4]
ICEUM4, ESTEC, 2000, ESA SP-462, B.H. Foing & M. Perry, editors. [5]
ICEUM5, Hawaii Nov 2003, Durst S.M. et al, Editors, Vol 108, 1-576
pp, Science and Technology Series, American Astronautical Society,
2004. [6] ICEUM6, Udaipur 2004, Bhandari N., Editor, Journal Earth
Sys-tem Science, India, 114, No6, Dec 2005, pp. 573-841. [7] ICEUM7,
Toronto Sept 2005, sci.esa.int/ilewg. [8] ICEUM8, Beijing July 2006,
Journal of Chinese Society of Astronautics, Vol. 28 Sup., 2007, Ji W.,
Editor. [9] ICEUM9, Sorrento, Italy, Foing B., Espinasse S., Kosters G.,
Editors. http://sci.esa.int/iceum9, Dec. 2007), [11] Ehrenfreund, P.,
Foing, B.H., Cellino, A. Editors, The Moon and Near Earth Objects, ASR
Vol 37, 1, 2006. [12] Foing, B.H. et al editors, 'Astronomy and Space
Science from the Moon', ASR 14, 6, 1994. [13] Ip W.-H., Foing, B.H.,
Masson Ph.L., editors, The Moon and Mars, ASR Vol 23, 11, 1999. [14]
Foing, B.H. et al, editor, Lunar Exploration, Planetary and Space
Science, Vol 50, 14-15, 2002. [15] Foing, B.H., Heather, D. editors,
'Lunar Exploration 2000', ASR Vol 30, Nr 8, 2002. [16] Huntress,
W. et al 'The next steps in exploring deep space - A cosmic study by
the IAA', Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377. [17]
http://sci.esa.int/ilewg/43654-declaration-iceum10-leag-srr-florida-2008/
[18] Ehrenfreund P. et al (COSPAR planetary exploration panel report)
2012, ASR Vol 49, Nr 1, pp. 2-48. *Relevant extract from GLUC/ICEUM11
declaration: “467 International Lunar Explorers, registered delegates
from 26 countries, assembled at GLUC Global Lunar Conference including
the 11th ILEWG Conference on Exploration and Utilisation of the
Moon (ICEUM11) in Beijing." "1. Science and exploration (related
GLUC/ICEUM11 recommendations will be addressed at COSPAR B0.1 Lunar
science and exploration session) 2. Technologies and resources - A
number of robotic missions to the Moon are now undertaken independently
by various nations, with a degree of exchange of information and
co-ordination. That should increase towards real co-operation,
still allowing areas of competition for keeping the process active,
cost-effective and faster. - Lunar landers, pressurized lunar rover
projects as presented from Europe, Asia and America are important
steps that can create opportunities for international collaboration,
within a coordinated village of robotic precursors and assistants to
crew missions. - We have to think about development, modernization of
existing navigation capabilities, and provision of lunar positioning,
navigation and data relay assets to support future robotic and human
exploration. New concepts and new methods for transportation have
attracted much attention and are of great potential. 3. Infrastructures
and human aspects - It is recommended to have technical sessions and
activities dealing with different aspects of human adaptation to space
environments, the modeling of sub-systems, microbial protection and
use of inflatable technologies - While the Moon is the best and next
logical step in human exploration, we should make best use of the space
stations as stepping stones for exploration and human spaceflight
beyond Low Earth Orbit. - Further research is needed on lunar dust
aspects in regard to humans and interaction with habitats. We note
high interest in CELSS for Moon and Mars bases, and recommend further
research and development. - We recommend the development and use of
terrestrial analogues research sites and facilities, for technology
demonstrations, comparative geology and human performance research,
and public engagement. We endorse the proposal of development of a site
at La Reunion for international Moon-Mars analogue research. 4. Moon,
Space, Society and Young Explorers - We consider that the current legal
regime as set out in the Outer Space Treaty and the Moon agreement
are satisfactory for current and future missions, but may require
further clarification for future exploration. Issues of transparency
and security will need to be addressed. - Great things are happening
for Young Lunar Explorers, with inspiring missions and hands-on
activities as coordinated by ILEWG. Lunar exploration is encouraging
students of all ages to pursue higher education. - More possibilities
for participatory engagement should be offered to the society for
example via inter-disciplinary activities with the humanities. -
We appreciate the work from COSPAR panel on Exploration PEX that
should be shared further. - Continued cooperation should be enforced
at all levels. The space community feels strongly that joining the
forces of space faring nations to explore the Moon should be seriously
implemented, with the views of expanding a Global Robotic Village and
building in the long run a Manned International Lunar Base.” “We,
the participants of the GLUC-ICEUM11 conference, commit to an enhanced
global cooperation towards international lunar exploration for the
benefit of humankind. Endorsed by the delegates of GLUC-ICEUM11”
Title: ESTEC/Geovusie/ILEWG planetary student design workshop:
a teacher training perspective
Authors: Preusterink, Jolanda; Foing, Bernard H.; Kaskes, Pim
Bibcode: 2014cosp...40E2623P
Altcode:
An important role for education is to inform and create the right
skills for people to develop their own vision, using their talents to
the utmost and inspire others to learn to explore in the future. Great
effort has been taken to prepare this interactive design workshop
thoroughly. Three days in a row, starting with presentations of
Artscience The Hague to ESA colleagues, followed by a Planetary
research Symposium in Amsterdam and a student design workshop at
the end complemented a rich environment with the focus on Planetary
exploration. The design workshop was organised by GeoVUsie students,
with ESTEC and ILEWG support for tutors and inviting regional and
international students to participate in an interactive workshop to
design 5 Planetary Missions, with experts sharing their expertise and
knowhow on specific challenging items: 1. Mercury - Post BepiColombo
(with Sébastien Besse, ESA) 2. Moon South Pole Mission (with Bernard
Foing, ESA) 3. Post-ExoMars - In search for Life on Mars (with
Jorge Vago, ESA) 4. Humans in Space - Mars One investigated(with
Arno Wielders, Space Horizon) 5. Europa - life on the icy moon of
Jupiter? (with Bert Vermeersen, TU Delft) Lectures were given for
more than 150 geology students at the symposium “Moon, Mars and
More” at VU university, Amsterdam (organized by GeoVUsie earth
science students). All students were provided with information before
and at start for designing their mission. After the morning session
there was a visit to the exhibition at The Erasmus Facility - ESTEC
to inspire them even more with real artifacts of earlier and future
missions into space. After this visit they prepared their final
presentations, with original results, with innovative ideas and a
good start to work out further in the future. A telescope session
for geology students had been organized indoor due to rain. A
follow-up visit to the nearby public Copernicus observatory was
planned for another clear sky occasion. The interactive character
of this setting was inspirational and motivating. A good method
with vision to modernize school education and bring innovation to
educators: they are the key promoters and facilitators for change in
the culture of education. Tutors and mentors are very important to pave
the way with more modern interactive learning, including: 1. Social
Media 2. Online Learning 3. Creator Society 4. Data-driven learning
5. Virtual Assistance The great importance of emerging technologies
and their potential impact on and use in teaching, learning, and
creative inquiry in pre-college education environments offer good
prospects. The International Lunar Exploration Working Group (ILEWG)
has given support to emphasize their vision, goal to "international
cooperation towards a world strategy for the exploration and utilization
of the Moon” by organizing and facilitating students, teachers,
schools and universities with relevant material, ready to use in the
classroom and inform the greater audience. This underlines the vision
of the importance and responsibility to “draw in” education for
primary, secondary and higher education on a more regular base and to
implant space exploration on its widest scale and on a more sustainable
way in the future. Developing and building a stronger network is crucial
to gain technical personal for future Moon missions, samples return and
research on other planets, moons or asteroids. This workshop helped
to give more outreach about current space projects and will have a
follow-up. The international and cooperative character was an innovative
experience with enriching information and great promising students for
more science and future space exploration. Acknowledgements: we thank
the volunteer organiser students from VU GeoVUsie, the participants
and the tutors. A video of highlights is available on " 2. Planetary
Design student workshop organised by VU Amsterdam GeoVusie/ESTEC/ILEWG"
http://www.youtube.com/watch?v=NJxvHKcNeKo
Title: ESA SMART-1 mission: results and lessons for future lunar
exploration
Authors: Foing, Bernard H.
Bibcode: 2014cosp...40E.881F
Altcode:
We review ESA’s SMART-1 highlights and legacy 10 years after
launch. We discuss lessons for future lunar exploration and upcoming
missions. The SMART-1 mission to the Moon achieved record firsts such
as: 1) first Small Mission for Advanced Research and Technology;
with spacecraft built and integrated in 2.5 years and launched 3.5
years after mission approval; 2) first mission leaving the Earth
orbit using solar power alone with demonstration for future deep
space missions such as BepiColombo; 3) most fuel effective mission
(60 litres of Xenon) and longest travel (13 month) to the Moon!;
4) first ESA mission reaching the Moon and first European views
of lunar poles; 5) first European demonstration of a wide range of
new technologies: Li-Ion modular battery, deep-space communications
in X- and Ka-bands, and autonomous positioning for navigation; 6)
first lunar demonstration of an infrared spectrometer and of a Swept
Charge Detector Lunar X-ray fluorescence spectrometer ; 7) first ESA
mission with opportunity for lunar science, elemental geochemistry,
surface mineralogy mapping, surface geology and precursor studies
for exploration; 8) first controlled impact landing on the Moon with
real time observations campaign; 9) first mission supporting goals
of the ILEWG/COSPAR International Lunar Exploration Working Group in
technical and scientific exchange, international collaboration, public
and youth engagement; 10) first mission preparing the ground for ESA
collaboration in Chandrayaan-1, Chang’ E1-2-3 and near-future landers,
sample return and human lunar missions. The SMART-1 technology legacy is
applicable to application geostationary missions and deep space missions
using solar electric propulsion. The SMART-1 archive observations have
been used to support scientific research and prepare subsequent lunar
missions. Most recent SMART-1 results are relevant to topics on: 1) the
study of properties of the lunar dust, 2) impact craters and ejecta,
3) the study of illumination, 4) observations and science from the
Moon, 5) support to future missions, 6) identifying and characterising
sites for exploration and exploitation. These results and legacy are
relevant to the preparation for future missions, in particular in the
frame of collaboration between Russia and ESA on upcoming landers
and on a polar sample return. Also the results contribute to the
preparation for a global robotic village and international lunar
bases (consistent with ILEWG, COSPAR and Global Space Exploration
roadmaps). Link: http://sci.esa.int/smart-1/ References and citations:
http://scholar.google.nl/scholar?&q=smart-1+moon *We acknowledge
ESA, member states, industry and institutes for their contribution,
and the members of SMART-1 Teams: G.Racca and SMART-1 Project Team,
O. Camino and SMART-1 Operations Team, D. Frew and SMART-1 STOC,
B.H. Foing and STWT, B. Grieger, D. Koschny, J.-L. Josset, S. Beauvivre,
M. Ellouzi, S. Peters, A. Borst, E. Martellato, M. Almeida, J.Volp,
D. Heather, M. Grande, J. Huovelin, H.U. Keller, U. Mall, A. Nathues,
A. Malkki, W. Schmidt, G. Noci, Z. Sodnik, B. Kellett, P. Pinet,
S. Chevrel, P. Cerroni, M.C. de Sanctis, M.A. Barucci, S. Erard,
D. Despan, K. Muinonen, V. Shevchenko, Y. Shkuratov, P. McMannamon,
P. Ehrenfreund, C. Veillet, M. Burchell, other Co-Investigators,
associated scientists, collaborators, students and colleagues
Title: Fluvial sediments, concretions, evaporates at Hanksville,
Utah: An analogue field study for Gale crater, Mars
Authors: Orgel, C.; Battler, M.; Foing, B. H.; Van't Woud, H.; Maiwald,
V.; Cross, M.; Ono, A.
Bibcode: 2013EPSC....8..804O
Altcode:
On 6th August 2012, Curiosity landed in Gale crater, Mars. Initial
measurements and pictures showed sedimentary rocks that had
been deposited by fluvial activity, e.g., alluvial fan and stream
deposits. Such deposits are common in desert environments on Earth. The
goal of the ILEWG EuroMoonMars project (February 23rd-March 9th,2013)was
to conduct field studies in order to identify and study environments
that are analogous to those that Curiosity has studied and will study at
Gale crater. Several field campaigns (EuroGeoMars2009 and DOMMEX/ILEWG
EuroMoonMars from November 2009 to March 2010) had been conducted at
the Mars Desert Research Station (MDRS) [3] near Hanksville, Utah, in
the vicinity of the San Rafael swell. The aim of the ILEWG EuroMoonMars
2013 project was to identify terrestrial analog sites for Curiosity
exploration. The stratigraphy of the area consists of Jurassic and
Cretaceous strat a[5] of which the Summerville Formation, the Brushy
Basin Member of the Morrison Formation, and the Dakota Sandstone were
studied. Widespread inverted channels on Mars have been identified
through orbiter imagery data [6], e.g., at Gale crater. Concretions
also appear to be common on Mars and have been found by the Opportunity
rover at Meridiani Planum [4] and the Curiosity rover at Yellowknife
Bay (Fig. 1).
Title: SMART-1 studies of impact processes: all scales from South
Pole-Aitken basin to the SMART-1 bouncing site.
Authors: Foing, B. H.
Bibcode: 2013EPSC....8.1006F
Altcode:
We highlight some ESA SMART - 1 results on impact processes. We discuss
impact basins, the morphology of raters, the properties of central
peaks, and the study of specific impact craters of interest to ILEWG
community. We also give an update on the results from SMART-1 impact
campaign and the search for SMART-1 bouncing site and debris using
latest LRO data.
Title: SMART-1 & recent missions: results from combining data
Authors: Foing, B. H.
Bibcode: 2013EPSC....8..993F
Altcode:
We highlight some results from combined data analysis using
SMART-1 archive with other recent lunar missions. We discuss in
particular impact craters, volcanic, photometry and studies of ILEWG
sites.. SMART-1 demonstrated the use of Solar Electric Propulsion for
deep space, tested new technologies for spacecraft and instruments
miniaturisation, and provided an opportunity for science [1-12]
until impact on 3 September 2006. To date 75 refereed papers and
more than 325 conference or technical papers have been published
based on SMART-1 (see ADS & SMART-1 website sci.esa.int/smart-1
or www.esa.int/smart-1). The SMART-1 data are accessible on the ESA
Planetary Science Archive PSA [13] http://www.rssd.esa.int/psa
Title: Numerical modelling of impact crater formation associated
with isolated lunar skylight candidates on lava tubes
Authors: Martellato, E.; Foing, B. H.; Benkhoff, J.
Bibcode: 2013P&SS...86...33M
Altcode:
Skylights are openings on subsurface voids as lava tubes and
caves. Recently deep hole structures, possibly skylights, were
discovered on lunar photo images by the JAXA SELenological and
ENgineering Explorer (SELENE)-Kaguya mission, and successively confirmed
by the NASA Lunar Reconnaissance Orbiter (LRO) mission. Vertical hole
structures and possibly underlying subsurface voids have high potential
as resources for scientific study, and future unmanned and manned
activities on the Moon. One mechanism proposed for their formation is
impact cratering. The collapse of craters is due to the back spallation
phenomena on the rear surface of the lava tube roofs. Previous analysis
in this topic was based on small-scales laboratory experiments. These
have pointed out that (i) the target thickness-to-crater diameter ratio
is 0.7, and (ii) the projectile diameter-to-target thickness ratio is
0.16, at the ballistic limit once extrapolated to planetary conditions.
Title: Molecular characterization of rock microbial communities from
the Mars analogue MDRS
Authors: Rodrigues, L.; Alves, A.; Davies, G. R.; Foing, B. H.;
Stoker, C.; Clarke, J.; Correia, A.
Bibcode: 2013EPSC....8..955R
Altcode:
Several rock samples have been collected as part of a Mars field
analogue campaign (NASA DOMEX-ILEWG uroMoonMars) at Mars Desert
Research StationMDRS area (Utah Desert, USA). This report details
the microbial diversity derived from culture-independent techniques,
such as polymerase chain reaction (PCR) and denaturing gradient gel
electrophoresis (DGGE) analysis.
Title: Results from Field Research Campaigns in Earth Extreme
Environments
Authors: Foing, B. H.; Stoker, C.; Ehrenfreund, P.; Rammos, I.;
Rodrigues, L.; Svendsen, A.; Oltheten, D.; Nebergall, K.; Battler,
M.; v't Houd, H.; Bruneau, A.; Cross, M.; Maivald, V.; Orgel, C.;
Elsaesser, A.; Direito, S. O. L.; Röling, W. F. M.; Davies, G. R.
Bibcode: 2013EPSC....8..979F
Altcode:
We shall give an update on the data analysis from a series of field
research campaigns (ILEWG EuroMoonMars)in the extreme environment of
the Utah desert relevant to habitability and astrobiology in Mars
environments, and in order to help in the interpretation of Mars
missions measurements from orbit (MEX, MRO) or from the surface (MER,
MSL). Keywords: field analogue research, astrobiology, habitability,
life detection, Earth-Mars, organics
Title: The ORGANIC Experiment on EXPOSE-R on the ISS: A Space
Exposure Experiment
Authors: Bryson, Kathryn; Peeters, Z.; Salama, F.; Foing, B.;
Ehrenfreund, P.; Ricco, A.; Jessberger, E. K.; Bischoff, A.;
Breitfellner, M.; Schmidt, W.; Robert, F.
Bibcode: 2013AAS...22211411B
Altcode:
Aromatic networks are among the most abundant organic material in
space. PAHs and fullerenes have been identified in meteorites and are
thought to be among the carriers for numerous astronomical absorption
and emission features. Thin films of selected PAHs and fullerenes
have been subjected to the low Earth orbit environment as part of the
ORGANIC experiment on the multi-user facility EXPOSE-R onboard the
ISS. The ORGANIC experiment monitored the chemical evolution, survival,
destruction, and chemical modification of the samples. EXPOSE-R was
mounted on the outside of the ISS from March 10, 2009 to January 21,
2011. The samples were returned to Earth and inspected in spring
2011. The 682-day period outside the ISS provided continuous exposure
to the cosmic-, solar-, and trapped-particle radiation background
and >2500 h of unshadowed solar illumination. All trays carry both
solar-irradiation-exposed and dark samples shielded from the UV photons,
enabling discrimination between the effects of exposure to solar
photons and cosmic rays. The samples were analyzed before exposure to
the space environment with UV-VIS spectroscopy. Ground truth monitoring
of additional sample carriers was performed through UV-VIS spectroscopy
at regular intervals at NASA Ames Research Center. During the exposure
on the ISS, 2 control sample carriers were exposed with a slight time
shift in a planetary simulation chamber at the Microgravity User Support
Center at DLR. Vacuum, UV radiation, and temperature fluctuations are
simulated according to the telemetry data measured during flight. The
spectroscopic measurements of these two carriers have been performed
together with the returned flight samples. We report on the scientific
experiment, the details of the ground control analysis, and preliminary
flight sample results.
Title: Results from Archive Data From SMART-1 Combined with Recent
Missions
Authors: Foing, Bernard
Bibcode: 2013EGUGA..1513943F
Altcode:
We highlight new results from combined data analysis using SMART-1
archive with data from other recent lunar missions. We concentrate
on results obtained on the lunar farside, the poles and about the
coupling between impact, volcanic and tectonic processes. SMART-1
demonstrated the use of Solar Electric Propulsion for deep space, tested
new technologies for spacecraft and instruments miniaturisation, and
provided an opportunity for science [1-24] until impact on 3 September
2006. To date, 77 refereed papers and more than 330 conference or
technical papers have been published based on SMART-1 (see ADS on
SMART-1 scitech website). The SMART-1 data are accessible on the
ESA Planetary Science Archive PSA [13]. The lunar North and South
polar illumination was mapped and monitored over the entire year,
permitting to identify "SMART-1 peaks of quasi-eternal light", then
charcterised with subsequent missions. The surface mineralogy maps of
the central and northern parts of the South-Pole Aitken basin, was based
on Clementine and SMART-1 AMIE images for additional geomorphological
and stratigraphic information. [1] Foing etal (2001) EMP 85-523 [2]
Racca et al (2002) EMP 85-379 [3] Racca et al. (2002) PSS 50-1323 [4]
Grande et al. (2003) PSS 51-427 [5] Dunkin et al. (2003) PSS 51-435
[6] Huovelin et al. (2002) PSS 50-1345 [7] Shkuratov et al (2003)
JGRE 108-E4-1 [8] Foing et al (2003) ASR 31-2323 [9] Grande et al
(2007) PSS 55-494 [10] Pinet et al (2005) PSS 53-1309 [11] Josset etal
(2006) ASR 37-14 [12] Foing et al (2006) ASR 37-6 [13] Heather et al,
EPSC-DPS 2011-873 [13b] http://www.rssd.esa.int/psa [14] Muinonen et al
(2011) A&A531-150 [15] Souchon et al EPSC-DPS 2011-928 [16] Grieger
(2010) cosp 38-417 [17] Bussey et al (2011) LPICO-1621-5 [18] Pluchino
et al MSAItS 16-152 [19] Qiao (2011) AcASn 52, 539 [20] Vaananen et al
(2009) SolarPhys 260-479 [21] Alha et al (2012)NIMPA 664, 358 [22]
Bhattacharya et al EPSC-DPS 2011-1842 [23] Burchell et al (2010)
Icarus207-28 [24] Borst et al (2012) PSS 68, 76
Title: EuroMoonMars Field Campaign: Geology traverse planning using
orbital sub-m imagery
Authors: Svendsen, Åse; van't Woud, Hans; Samurovic, Dejan; Nebergall,
Kent; Battler, Melissa; Orgel, Csilla; Stoker, Carol; Tolboom, Iwan;
Foing, Bernard; Team EuroMoonMars
Bibcode: 2013EGUGA..1513616S
Altcode:
Most of the information we have from Moon and Mars surface, comes
from satellite observations. During the selection of landing sites and
planning of traverses on unfamiliar planetary sites, satellite images
of high resolution is crucial. But what information are we missing from
these images? What kind of surprises can be expected when exploring
an area that has only been investigated from satellite images? During
ILEWG EuroMoonMars 2013 campaign at MDRS Utah we made a comparative
study where we looked at satellite images with a spatial resolution of
50-60 cm per pixel, something that is comparable to the resolution of
MRO HiRise on Mars or LROC on the Moon. We then planned traverses at
MDRS that were as similar to geomorphological features seen at the Gale
crater as possible. Following this, we explored these traverses with
a rover, drone and walked them in a Mars EVA simulation mode, before
taking rocks and soil samples. We shal also discuss the usability of a
drone for imaging reconnaissance. The poster will present the results,
experiences and lessons learnt from this campaign concerning geological
traverse planning based on high resolution satellite images.
Title: Numerical Modeling of Raditladi and Rachmaninoff Basins
Authors: Martellato, E.; Benkhoff, J.; Preusker, F.; Cremonese, G.;
Foing, B. H.; Massironi, M.; Oberst, J.
Bibcode: 2013LPI....44.1405M
Altcode: 2013LPICo1719.1405M
We modeled with iSALE code the formation of Raditladi and Rachmaninoff,
two peak-ring basins on Mercury. We compare modeling results and
MESSENGER DTM profiles.
Title: OREOcube: ORganics Exposure in Orbit
Authors: Quinn, R.; Elsaesser, A.; Ehrenfreund, P.; Ricco, A.;
Breitenbach, A.; Chan, J.; Fresneau, A.; Alonzo, J.; Mattioda, A.;
Salama, F.; Santos, O.; Sciamma-O'Brien, E.; Cottin, H.; Dartois,
E.; d'Hendecourt, L.; Demets, R.; Foing, B.; Martins, Z.; Sephton,
M.; Spaans, M.
Bibcode: 2013LPI....44.2498Q
Altcode: 2013LPICo1719.2498Q
The OREOcube experiment will use in situ spectroscopy to study minerals
and organic compounds exposed to LEO radiation conditions on an ISS
external platform.
Title: Astrobiology, Geology and Habitability Field Studies Supporting
Mars Research
Authors: Foing, B. H.; Stoker, C.; Rodrigues, L.; Svendsen, Å.;
Rammos, I.; Zhao, T.; Mangeot, A.; Rai, B.; Zamurovic, D.; Direito, S.;
Davies, G. R.; Ehrenfreund, P.; Elsaesser, A.; Roling, W.; Martins,
Z.; Sephton, M.; Zhavaleta, J.; Thiel, C.; Orzechowska, G.; Kidd,
R.; Quinn, R.; Orgel, C.; Nebergall, K.; Battler, M.; Cross, M.;
van Woud, H.; EuroGeoMars, T.; EuroMoonMars, T.
Bibcode: 2013LPI....44.3057F
Altcode: 2013LPICo1719.3057F
We conducted field campaigns (EuroGeoMars and ILEWG EuroMoonMars)
in the Utah desert to study geology, habitability, and samples in
support of Mars-X, MRO, MER, and MSL.
Title: Preliminary studies for the ORganics Exposure in Orbit
(OREOcube) Experiment on the International Space Station
Authors: Alonzo, Jason; Fresneau, A.; Elsaesser, A.; Chan, J.;
Breitenbach, A.; Ehrenfreund, P.; Ricco, A.; Salama, F.; Mattioda,
A.; Santos, O.; Cottin, H.; Dartois, E.; d'Hendecourt, L.; Demets,
R.; Foing, B.; Martins, Z.; Sephton, M.; Spaans, M.; Quinn, R.
Bibcode: 2013AAS...22135002A
Altcode:
Organic compounds that survive in uncommon space environments are
an important astrobiology focus. The ORganics Exposure in Orbit
(OREOcube) experiment will investigate, in real time, chemical changes
in organic compounds exposed to low Earth orbit radiation conditions
on an International Space Station (ISS) external platform. OREOcube
is packaged as an identical pair of 10-cm cube instruments, each
weighing < 2 kg and containing a highly capable UV-Visible-NIR
spectrometer, a 24-sample carousel, and integral optics enabling
use of the Sun as light source for spectroscopy, along with the
electronics, microcontroller, and data storage to make each cube an
autonomous stand-alone instrument package requiring only a standard
power and data interface. We have characterized the influence of
mineralogically relevant inorganic materials on the stability,
modification, and degradation of the organic molecules under ground
laboratory experimental conditions. The results of our laboratory
experiments will be used as the basis for the selection of samples
for further investigations on the OREOcube ISS experiment. OREOcube is
an international collaboration between the European Space Agency, the
National Aeronautics and Space Administration, and University partners.
Title: Supporting Mars exploration: BIOMEX in Low Earth Orbit and
further astrobiological studies on the Moon using Raman and PanCam
technology
Authors: de Vera, Jean-Pierre; Boettger, Ute; Noetzel, Rosa de
la Torre; Sánchez, Francisco J.; Grunow, Dana; Schmitz, Nicole;
Lange, Caroline; Hübers, Heinz-Wilhelm; Billi, Daniela; Baqué,
Mickael; Rettberg, Petra; Rabbow, Elke; Reitz, Günther; Berger,
Thomas; Möller, Ralf; Bohmeier, Maria; Horneck, Gerda; Westall,
Frances; Jänchen, Jochen; Fritz, Jörg; Meyer, Cornelia; Onofri,
Silvano; Selbmann, Laura; Zucconi, Laura; Kozyrovska, Natalia; Leya,
Thomas; Foing, Bernard; Demets, René; Cockell, Charles S.; Bryce,
Casey; Wagner, Dirk; Serrano, Paloma; Edwards, Howell G. M.; Joshi,
Jasmin; Huwe, Björn; Ehrenfreund, Pascale; Elsaesser, Andreas; Ott,
Sieglinde; Meessen, Joachim; Feyh, Nina; Szewzyk, Ulrich; Jaumann,
Ralf; Spohn, Tilman
Bibcode: 2012P&SS...74..103D
Altcode:
The Low Earth Orbit (LEO) experiment Biology and Mars Experiment
(BIOMEX) is an interdisciplinary and international space research
project selected by ESA. The experiment will be accommodated on the
space exposure facility EXPOSE-R2 on the International Space Station
(ISS) and is foreseen to be launched in 2013. The prime objective of
BIOMEX is to measure to what extent biomolecules, such as pigments
and cellular components, are resistant to and able to maintain
their stability under space and Mars-like conditions. The results of
BIOMEX will be relevant for space proven biosignature definition and
for building a biosignature data base (e.g. the proposed creation
of an international Raman library). The library will be highly
relevant for future space missions such as the search for life on
Mars. The secondary scientific objective is to analyze to what extent
terrestrial extremophiles are able to survive in space and to determine
which interactions between biological samples and selected minerals
(including terrestrial, Moon- and Mars analogs) can be observed under
space and Mars-like conditions. In this context, the Moon will be an
additional platform for performing similar experiments with negligible
magnetic shielding and higher solar and galactic irradiation compared to
LEO. Using the Moon as an additional astrobiological exposure platform
to complement ongoing astrobiological LEO investigations could thus
enhance the chances of detecting organic traces of life on Mars. We
present a lunar lander mission with two related objectives: a lunar
lander equipped with Raman and PanCam instruments which can analyze the
lunar surface and survey an astrobiological exposure platform. This dual
use of testing mission technology together with geo- and astrobiological
analyses will significantly increase the science return, and support
the human preparation objectives. It will provide knowledge about
the Moon's surface itself and, in addition, monitor the stability
of life-markers, such as cells, cell components and pigments, in an
extraterrestrial environment with much closer radiation properties to
the surface of Mars. The combination of a Raman data base of these
data together with data from LEO and space simulation experiments,
will lead to further progress on the analysis and interpretation of
data that we will obtain from future Moon and Mars exploration missions.
Title: Raditladi and Rachmaninoff basins: Numerical Modelling
Authors: Martellato, E.; Benkhoff, J.; Cremonese, G.; Foing, B.;
Massironi, M.; Oberst, J.; Preusker, F.
Bibcode: 2012epsc.conf..637M
Altcode: 2012espc.conf..637M
Mercury hosts the largest population of peak-ring basins among all the
rocky planets and satellites of the Solar System. Among the database of
such structures, we take into analysis two recently imaged peak-ring
basins, Raditladi and Rachmaninoff, both located in the northern
hemisphere and about 300 km in diameter. In this work, we present
the numerical simulations carried out through the iSALE shock code,
along with the comparison with observations, in order to shed light
on the primary impactor source of these basins.
Title: Geomicrobiology associated with formation of Fe-rich accretions
in an extreme acidic environment
Authors: Rodrigues, L.; Valente, T. M.; Foing, B. H.; Davies, G. R.;
Correia, A.; Alves, A.
Bibcode: 2012epsc.conf..797R
Altcode: 2012espc.conf..797R
The abandoned mine of Valdarcas (north of Portugal) includes a small
effluent channel associated with a permanent strong acid mine drainage
(AMD) (average pH= 3.0), where Fe-rich tubular and spherical macro
concretions have been formed and can be observed in situ. Results
from biological analysis demonstrate a high phylogenetic diversity
within Bacteria domain and Fungi kingdom, and less diversity for the
Archaea domain.
Title: Some recent lunar science and exploration results using
SMART-1 archives
Authors: Foing, B. H.
Bibcode: 2012epsc.conf..586F
Altcode: 2012espc.conf..586F
We highlight some results from combined data analysis using SMART-1
archive with other recent lunar missions.
Title: Raditladi and Rachmaninoff basins: Comparative studies
Authors: Martellato, E.; Marchi, S.; Benkhoff, J.; Cremonese, G.;
Foing, B.; Giacomini, L.; Massironi, M.; Prockter, L. M.
Bibcode: 2012epsc.conf..635M
Altcode: 2012espc.conf..635M
Mercury hosts the largest population of peak-ring basins among all
the rocky planets and satellites of the Solar System. Among the
database of such structures, we take into analysis two recently
imaged peak-ring basins, Raditladi and Rachmaninoff, both located
in the northern hemisphere and about 300 km in diameter. In this
work, we present the state of art on these basins. In particular,
we focus on their differences, and the possible mechanisms or surface
properties that could have led to such a diversification between two
similar structures. This work wants to be a review of the present
knowledge on Raditladi and Rachmaninoff in the view of a subsequent
deep investigation on the impact process that led to the formation of
these basins.
Title: Results from Astrobiology Field Research Campaigns in Earth
Extreme Environments
Authors: Foing, B. H.; Rodrigues, L.; Stoker, C.; Ehrenfreund, P.;
Direto, S. O. I.; Röling, W. F. M.; Davies, G. R.; Rammos, I.; Zhao,
T.; Mangeot, A.; Pouters, W.; Rei, B.
Bibcode: 2012epsc.conf..589F
Altcode: 2012espc.conf..589F
We conducted a series of field research campaigns in the extreme
environment of the Utah desert relevant to habitability and
astrobiology research in Mars environments, and in order to help in
the interpretation of Mars missions measurements from orbit (MEX, MRO)
or from the surface (MER, MSL). Keywords: astrobiology, habitability,
life detection, field analog research, Earth-Mars, organics.
Title: Lithic microbial communities from a Mars analogue site in
Utah desert
Authors: Rodrigues, L.; Foing, B. H.; Davies, G. R.; Stoker, C.;
Clarke, J.; Correia, A.; Alves, A.
Bibcode: 2012epsc.conf..801R
Altcode: 2012espc.conf..801R
Several rock samples have been collected as part of a Mars field
analogue campaign (NASA DOMEXILEWG EuroMoonMars) at Mars Desert Research
Station (MDRS) area (Utah Desert, USA), and were analyzed with respect
to the microbial diversity they support; a culture-independent approach
resulted in DGGE band profiles descriptive of the composition of the
3 domains, Bacteria, Archaea and Eukarya.
Title: Analysis of Lava Tubes and Skylights in the Lunar Exploration
Context
Authors: Martellato, E.; Foing, B.; Benkhoff, J.
Bibcode: 2012epsc.conf..632M
Altcode: 2012espc.conf..632M
The past and current scientific activities related to the future robotic
and human exploration of the Moon have stressed the importance of lava
tubes as convenient settlements in an inhospitable planet, providing
a natural shielding to a variety of natural hazards with minimizing
costs of the construction of manned bases. The detection of lava tubes
could be favoured by the presence of skylights, which also represent
a way to access to these underground structures. In this context,
we analyze one of the proposed mechanism of skylights formation, that
is random impacts craters, by comparing cratergeometry argumentations
([11]) with numerical modelling outcomes.
Title: Surface mineralogy and stratigraphy of the lunar South
Pole-Aitken basin determined from Clementine UV/VIS and NIR data
Authors: Borst, A. M.; Foing, B. H.; Davies, G. R.; van Westrenen, W.
Bibcode: 2012P&SS...68...76B
Altcode:
The South Pole-Aitken (SPA) basin, located on the lunar far side,
is one of the oldest and largest recognised impact structures in the
solar system. The basin is a proposed site for future sample return
missions and human bases due to the unique geological environment and
its potential for preservation of water ice in areas of near-permanent
shadow. Here, we report surface mineralogy maps of the central and
northern parts of the SPA basin, based on Clementine UV/VIS and NIR
spectral data. Clementine LIDAR data and SMART-1 AMIE images provide
additional geomorphological and stratigraphic information. A noritic
mineralogical composition is identified as the deepest stratigraphic
unit exposed on the basin floor. Norite is found in nearly all central
peaks and in large topographical structures that have punched through
an upper, often basaltic or gabbroic layer, including the Leibnitz and
Apollo sub-basins. The thin layer of gabbroic/basaltic composition is
distributed over large parts of the SPA basin floor and presumably
overlays the noritic basement of apparent lower-crustal origin. Our
data do not confirm the presence of olivine-rich material in the SPA
basin, including at Olivine Hill, suggesting the mantle material was
not excavated during the basin-forming impact.
Title: Detection of Organics and Biodiversity in Terrestrial Analogue
Samples
Authors: Foing, Bernard H.
Bibcode: 2012cosp...39..552F
Altcode: 2012cosp.meet..552F
No abstract at ADS
Title: New Results and Synthesis from SMART-1
Authors: Foing, Bernard H.
Bibcode: 2012cosp...39..551F
Altcode: 2012cosp.meet..551F
We present new SMART-1 results recently published and give a synthesis
of mission highlights and legacy. SMART-1 demonstrated the use of
Solar Electric Propulsion that will be useful for Bepi-Colombo and
future deep-space missions, tested new technologies for spacecraft
and instruments miniaturisation, and provided an opportunity for
science [1-12]. The SMART-1 spacecraft operated on a science orbit
for 18 months until impact on 3 September 2006. To date, 72 refereed
papers and more than 325 conference or technical papers have been
published based on SMART-1 (see ADS on SMART-1 scitech website). The
SMART-1 data are accessible on the ESA Planetary Science Archive PSA
[13]. Recent SMART-1 published results using these archives include:
Multi-angular photometry of Mare and specific regions to diagnose
the regolith roughness and to constrain models of light re ection
and scattering [14] that can be extended to understand the surface of
other moons and asteroids; the SMART-1 impact observed from Earth was
modelled using laboratory experiments predicting the size of asymmetric
crater and ejecta [15]; the lunar North and South polar illumination
was mapped and monitored over the entire year, permitting to identify
SMART-1 peaks of quasi-eternal light" and to derive their topography
[16, 17]; SMART-1 was also used for radio occultation experiments
[18], and the X-Ray Solar Monitor data were used for activity and
are studies of the Sun as a star in conjunction with GOES AND RHESSI
[19] or to design future coronal X-ray instruments [20]. The SMART-1
archive observations have been used to support Kaguya, Chandrayaan-1,
Chang'E 1, the US Lunar Reconnaissance Orbiter, the LCROSS impact,
and to characterise potential sites relevant for lunar science and
future exploration. Credits and links: we acknowledge members of
SMART-1 Science and Technology Working Team and collaborators. SMART-1
Scitech or public websites: sci.esa.int/smart-1 or www.esa.int/smart-1
References [1] Foing etal (2001) EMP 85-523; [2] Racca et al (2002) EMP
85-379; [3] Racca et al. (2002) PSS 50-1323; [4] Grande et al. (2003)
PSS51-427; [5] Dunkin et al. (2003) PSS 51-435; [6] Huovelin et
al. (2002) PSS50-1345; [7] Shkuratov et al (2003) JGRE 108-E4-1; [8]
Foing et al (2003) ASR 31-2323; [9] Grande et al (2007) PSS 55-494;
[10] Pinet et al (2005) PSS 53-1309; [11] Josset etal (2006) ASR 37-14;
[12] Foing et al (2006) ASR 37-6; [13] http://www.rssd.esa.int/psa
[14] Muinonen et al (2011) AA 531-150; [15] Burchell et al (2010)
Icarus 207-28; 16] Grieger (2010) cosp 38-417; [17] Bussey et al (2011)
LPI CO-1621-5; [18] Pluchino et al MSAItS 16-152; [19] Vaananen et al
(2009) SolarPhys 260-479; [20] Alha et al (2012)NIMPA 664, 358
Title: Thermal degradation of organic material by portable laser
Raman spectrometry
Authors: Som, Sanjoy M.; Foing, Bernard H.
Bibcode: 2012IJAsB..11..177S
Altcode:
Raman spectrometry has been established as an instrument of choice
for studying the structure and bond type of known molecules, and
identifying the composition of unknown substances, whether geological
or biological. This versatility has led to its strong consideration for
planetary exploration. In the context of the ExoGeoLab and ExoHab pilot
projects of ESA-ESTEC & ILEWG (International Lunar Exploration
Working Group), we investigated samples of astrobiological interest
using a portable Raman spectrometer lasing at 785 nm and discuss
implications for planetary exploration. We find that biological samples
are typically best observed at wavenumbers >1100 cm-1,
but their Raman signals are often affected by fluorescence effects,
which lowers their signal-to-noise ratio. Raman signals of minerals
are typically found at wavenumbers <1100 cm-1, and
tend to be less affected by fluorescence. While higher power and/or
longer signal integration time improve Raman signals, such power
settings are detrimental to biological samples due to sample thermal
degradation. Care must be taken in selecting the laser wavelength,
power level and integration time for unknown samples, particularly if
Raman signatures of biological components are anticipated. We include
in the Appendices tables of Raman signatures for astrobiologically
relevant organic compounds and minerals.
Title: The ORGANIC Experiment on EXPOSE-R on the ISS: A Space
Exposure Experiment
Authors: Bryson, Kathryn; Peeters, Z.; Salama, F.; Foing, B.;
Ehrenfreund, P.; Ricco, A. J.; Jessberger, E.; Bischoff, A.;
Breitfellner, M.; Schmidt, W.; Robert, F.
Bibcode: 2012AAS...22020901B
Altcode:
Aromatic networks are among the most abundant organic material in
space. PAHs and fullerenes have been identified in meteorites and are
thought to be among the carriers for numerous astronomical absorption
and emission features. Thin films of selected PAHs and fullerenes
have been subjected to the low Earth orbit environment as part of
the ORGANIC experiment on the multi-user facility EXPOSE-R onboard
the International Space Station. The ORGANIC experiment monitored the
chemical evolution, survival, destruction, and chemical modification
of the samples in space environment. EXPOSE-R with its experiment
inserts was mounted on the outside of the ISS from March 10, 2009 to
January 21, 2011. The samples were returned to Earth and inspected in
spring 2011. The 682-day period outside the ISS provided continuous
exposure to the cosmic-, solar-, and trapped-particle radiation
background and >2500 h of unshadowed solar illumination. All trays
carry both solar-irradiation-exposed and dark samples shielded from the
UV photons, enabling discrimination between the effects of exposure to
solar photons and cosmic rays. The samples were analyzed before
exposure to the space environment with UV-VIS spectroscopy. Ground truth
monitoring of additional sample carriers was performed through UV-VIS
spectroscopy at regular intervals at NASA Ames Research Center. During
the exposure on the ISS, two control sample carriers were exposed
with a slight time shift in a planetary simulation chamber at the
Microgravity User Support Center (MUSC) at DLR. Vacuum, UV radiation,
and temperature fluctuations are simulated according to the telemetry
data measured during flight. The spectroscopic measurements of these
two carriers have been performed together with the returned flight
samples. We report on the scientific experiment, the details of
the ground control analysis, and preliminary flight sample results. We
discuss how extended space exposure experiments allow to enhance our
knowledge on the evolution of organic compounds in space.
Title: Contribution of eukaryotic microbial communities to the
formation of Fe-rich accretions in an extreme acidic environment
Authors: Rodrigues, L.; Valente, T.; Correia, A.; Alves, A.; Foing,
B.; Davies, G. R.
Bibcode: 2012EGUGA..1414112R
Altcode:
In the acid mine drainage of Valdarcas, northern Portugal, Fe-rich
tubular and spherical macroaccretions are directly associated with
the presence of eukaryotic microorganisms. This raises the question
whether they are biogenically-derived or the result of an abiotic
process mediated by microeukaryotic phototrophs. The drainage water
at Valdarcas is characterized by very low pH values (pH<3.5),
high metal solubility and presence of iron colloids. Mineralogical
analysis (XRD and SEM) of the precipitates indicates a mixture of
goethite, schwertmannite and jarosite. Euglenophyta and Chlorophyta
acidophilic algal were previously identified in this site. The spatial
distribution of Euglena mutabilis indicated that it has a preference
to grow up on schwertmannite-rich precipitates. Field observations
demonstrate the existence of oxygenated microenvironments created
by algal activity suggesting that algae influence iron minerals
precipitation, especially schwertmannite. The mineral-microorganism
interactions are relevant to understanding this unique and extreme
environment. Further investigations regarding the mineralogical and
chemical characterization of these deposits, and the identification
of microorganisms involved in the process could be helpful to enhance
our knowledge of past Fe formations throughout Earth's primordial
environment. It is expectable that this information will contribute to
establish a framework for recognition of biosignatures on other planets
and extraterrestrial bodies. In this study, results on the chemical
and mineralogical composition of the structures are presented. The
biological context is characterised based on observations made by
optical microscopy complemented with molecular data on the microbial
communities obtained by culture independent methods. The results
are discussed within the context of two models: the studied Fe-rich
stromatolites are microeukaryotic-mediated as described by previous
workers from similar environments or are the consequence of inorganic
precipitation of reduced iron species (Fe(III)) due to the oxygen
generated by the photosynthesis?
Title: Characterization of the particle radiation environment at
three potential landing sites on Mars using ESA’s MEREM models
Authors: McKenna-Lawlor, S.; Gonçalves, P.; Keating, A.; Morgado,
B.; Heynderickx, D.; Nieminen, P.; Santin, G.; Truscott, P.; Lei,
F.; Foing, B.; Balaz, J.
Bibcode: 2012Icar..218..723M
Altcode:
The ‘Mars Energetic Radiation Environment Models’ (dMEREM and
eMEREM) recently developed for the European Space Agency are herein used
to estimate, for the first time, background Galactic Cosmic Ray (GCR)
radiation and flare related solar energetic particle (SEP) events at
three candidate martian landing sites under conditions where particle
arrival occurred at solar minimum (December, 2006) and solar maximum
(April, 2002) during Solar Cycle 23. The three landing sites were
selected on the basis that they are characterized by significantly
different hydrological conditions and soil compositions. Energetic
particle data sets recorded on orbit at Mars at the relevant times
were incomplete because of gaps in the measurements due to operational
constraints. Thus, in the present study, comprehensive near-Earth
particle measurements made aboard the GOES spacecraft were used as
proxies to estimate the overall particle doses at each perspective
landing site, assuming in each case that the fluxes fell off as
1/r2 (where r is the helio-radial distance) and that good
magnetic connectivity always prevailed. The results indicate that the
particle radiation environment on Mars can vary according to the epoch
concerned and the landing site selected. Particle estimations obtained
using MEREM are in reasonable agreement, given the inherent differences
between the models, with the related NASA Heavy Ion-Nucleon Transport
Code for Space Radiation/HZETRN. Both sets of results indicated that,
for short (30 days) stays, the atmosphere of Mars, in the cases of
the SEPs studied and the then prevailing background galactic cosmic
radiation, provided sufficient shielding at the planetary surface to
maintain annual skin and blood forming organ/BFO dose levels below
currently accepted ionizing radiation exposure limits. The threat
of occurrence of a hard spectrum SEP during Cruise-Phase transfers
to/from Mars over 400 days, combined with the associated cumulative
effect of prolonged GCR exposure, poses an as yet unsolved hazard to
prospective onboard personnel.
Title: Subsurface Profiles of Organics Obtained by Core Drilling in
Jurassic Sediments at a Mars Analog Site in Utah
Authors: Stoker, C. R.; Clarke, J. D. A.; Valdivia-Silva, J.; Foing, B.
Bibcode: 2012LPI....43.2850S
Altcode:
We obtained rock cores (0.6-1.6 m depth) from ancient (150 m.y. old)
sediments at a Mars analog site in Utah using a prototype Mars drill. We
report the depth profile of organics from these samples to illustrate
the utility of drilling on Mars.
Title: Numerical Modeling of the Caloris Basin
Authors: Martellato, E.; Benkhoff, J.; Colangeli, L.; Foing, B.;
Marchi, S.
Bibcode: 2012LPICo1649...47M
Altcode:
No abstract at ADS
Title: Toward a global space exploration program: A stepping stone
approach
Authors: Ehrenfreund, Pascale; McKay, Chris; Rummel, John D.; Foing,
Bernard H.; Neal, Clive R.; Masson-Zwaan, Tanja; Ansdell, Megan; Peter,
Nicolas; Zarnecki, John; Mackwell, Steve; Perino, Maria Antionetta;
Billings, Linda; Mankins, John; Race, Margaret
Bibcode: 2012AdSpR..49....2E
Altcode:
In response to the growing importance of space exploration in future
planning, the Committee on Space Research (COSPAR) Panel on Exploration
(PEX) was chartered to provide independent scientific advice to
support the development of exploration programs and to safeguard the
potential scientific assets of solar system objects. In this report,
PEX elaborates a stepwise approach to achieve a new level of space
cooperation that can help develop world-wide capabilities in space
science and exploration and support a transition that will lead to
a global space exploration program. The proposed stepping stones
are intended to transcend cross-cultural barriers, leading to the
development of technical interfaces and shared legal frameworks and
fostering coordination and cooperation on a broad front. Input for
this report was drawn from expertise provided by COSPAR Associates
within the international community and via the contacts they maintain
in various scientific entities. The report provides a summary and
synthesis of science roadmaps and recommendations for planetary
exploration produced by many national and international working
groups, aiming to encourage and exploit synergies among similar
programs. While science and technology represent the core and, often,
the drivers for space exploration, several other disciplines and their
stakeholders (Earth science, space law, and others) should be more
robustly interlinked and involved than they have been to date. The
report argues that a shared vision is crucial to this linkage, and
to providing a direction that enables new countries and stakeholders
to join and engage in the overall space exploration effort. Building
a basic space technology capacity within a wider range of countries,
ensuring new actors in space act responsibly, and increasing public
awareness and engagement are concrete steps that can provide a broader
interest in space exploration, worldwide, and build a solid basis
for program sustainability. By engaging developing countries and
emerging space nations in an international space exploration program,
it will be possible to create a critical bottom-up support structure to
support program continuity in the development and execution of future
global space exploration frameworks. With a focus on stepping stones,
COSPAR can support a global space exploration program that stimulates
scientists in current and emerging spacefaring nations, and that will
invite those in developing countries to participate—pursuing research
aimed at answering outstanding questions about the origins and evolution
of our solar system and life on Earth (and possibly elsewhere). COSPAR,
in cooperation with national and international science foundations
and space-related organizations, will advocate this stepping stone
approach to enhance future cooperative space exploration efforts.
Title: The ORGANIC experiment on EXPOSE-R on the ISS: Flight sample
preparation and ground control spectroscopy
Authors: Bryson, K. L.; Peeters, Z.; Salama, F.; Foing, B.;
Ehrenfreund, P.; Ricco, A. J.; Jessberger, E.; Bischoff, A.;
Breitfellner, M.; Schmidt, W.; Robert, F.
Bibcode: 2011AdSpR..48.1980B
Altcode:
In March of 2009, the ORGANIC experiment integrated into the European
multi-user facility EXPOSE-R, containing experiments dedicated to
Astrobiology, was mounted through Extra Vehicular Activity (EVA)
externally on the International Space Station (ISS). The experiment
exposed organic samples of astronomical interest for a duration of
97 weeks (∼22 months) to the space environment. The samples that
were returned to Earth in spring 2011, received a total UV radiation
dose during their exposure including direct solar irradiation of
>2500 h, exceeding the limits of laboratory simulations. We
report flight sample preparation and pre-flight ultraviolet-visible
(UV-Vis) characterization of the ORGANIC samples, which include 11
polycyclic aromatic hydrocarbons (PAHs) and three fullerenes. The
corresponding time-dependent ground control monitoring experiments
for ORGANIC measured over ∼19 months are presented and the results
anticipated upon return of the samples are discussed. We present
the first UV-Vis spectrum of solid circobiphenyl (C 38H
16). Further, we present the first published UV-Vis
spectra of diphenanthro[9,10-b',10'-d]thiophene (C 28H
16S), dinaphtho[8,1,2-abc,2',1',8'-klm]coronene (C
36H 16), tetrabenzo[de,no,st,c'd']heptacene
(C 42H 22), and dibenzo[jk,a'b']octacene (C
40H 22) in solid phase and in solution. The
results of the ORGANIC experiment are expected to enhance our knowledge
of the evolution and degradation of large carbon-containing molecules
in space environments.
Title: Analysis of organic compounds, minerals and biota: Preparation
for future Mars life detection missions
Authors: Martins, Z.; Kotler, J. M.; Direito, S. O. L.; Sephton,
M. A.; Stoker, C.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 2011epsc.conf..709M
Altcode: 2011DPS....43..709M
In the present study we have measured the amino acid content of Mars
analogue soil samples, and related those results to the microbial and
mineralogical data of the soil samples. These were performed on soils
collected near the Mars Desert Research Station (MDRS) in the Utah
desert (Figure 1), during the EuroGeoMars 2009 campaign [2,3]. The Utah
soil displays mineralogies similar to Mars, with sedimentary deposits
of sands, evaporites, clays and gypsum [4].
Title: Microbiological contamination assessment from drilling
activities - recognition and design of prevention strategy
Authors: Rodrigues, L.; Davies, G. R.; Foing, B.; Correia, A.;
Alves, A.; Valdivia-Silva, J.; Zavaleta, J.; Stoker, C.; Wilson, D.;
Clarke, J.
Bibcode: 2011epsc.conf.1370R
Altcode: 2011DPS....43.1370R
The search for traces of extinct and extant life combined with
sub-surface sampling on Mars will be investigated for the first
time in ExoMars Exploration Mission. Sub-surface sampling will be
addressed using a robotic drill that will minimize the risk of forward
contamination. Hence the risks associated with drill contamination must
be addressed. This paper describes contamination assessment related
to dry drilling activities in Terrestrial Martian analogues.
Title: On the polarisation of the Red Rectangle optical emission bands
Authors: Cox, N. L. J.; Foing, B. H.; Cami, J.; Sarre, P. J.
Bibcode: 2011A&A...532A..46C
Altcode: 2011arXiv1105.4795C
Context. The origin of the narrow optical emission bands seen
towards the Red Rectangle is not yet understood. We investigate the
proposal that these are caused by luminescence of large carbonaceous
molecules.
Aims: We aim to measure the polarisation of the
optical narrow Red Rectangle bands (RRBs). Polarised signals of
several percent could be expected from certain asymmetric molecular
rotators.
Methods: The ESPaDOnS échelle spectrograph mounted at
the CFHT was used to obtain high-resolution optical spectropolarimetric
data of the Red Rectangle nebular emission.
Results: The RRBs
at 5800, 5850, and 6615 Å are detected in spectra of the nebular
emission 7″ and 13″ north-east from the central star. The 5826
Å and 6635 Å RRB are detected only at the position nearest to the
central star. For both positions the Stokes Q and U spectra show
no unambiguous polarisation signal in any of the RRBs. We derive an
upper limit of 0.02% line polarisation for these RRBs. A tentative
feature with peak polarisation of 0.05% is seen for the 5800 Å RRB
at 7″ offset. However, the null spectra suggest that this may be
an instrumental artefact.
Conclusions: The lack of a clear
polarisation signal for the five detected RRBs implies that if
the emission is caused by luminescence of complex organics, these
gas-phase molecular carriers are likely to have a high degree of
symmetry because they do not exhibit a Q-branch in their rotational
profile, although this may be modified by statistical effects. Based on observations obtained at the Canada-France-Hawaii Telescope
(CFHT) which is operated by the National Research Council of Canada,
the Institut National des Sciences de l'Univers of the Centre National
de la Recherche Scientique of France, and the University of Hawaii.
Title: Extraction of amino acids from soils close to the Mars Desert
Research Station (MDRS), Utah
Authors: Martins, Z.; Sephton, M. A.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 2011IJAsB..10..231M
Altcode:
Future space missions that aim to detect life should search for
molecules that are vital to all living organisms. Although the Viking
landers did not find any signs of organic molecules on Mars, signatures
of past and/or present life may still exist in the Martian regolith. In
this paper, we describe amino acid analyses performed in several Martian
analogue soil samples collected close to the Mars Desert Research
Station (MDRS), Utah, during the International Lunar Exploration
Working Group (ILEWG) EuroGeoMars campaign in February 2009. The Utah
desert around Hanksville is characterized as shale desert and is cold
and arid with an average annual temperature of 12°C. It is subjected
to wind erosion and was shaped by fluvial erosion. The data show large
differences in the total amino acid abundances between all the collected
soil samples, with values ranging from non-detectable to 100 000
parts per billion (ppb). These results are explained in the context of
mineralogical differences (namely different clay content) among the
soil samples. The data have implications for future life-detection
missions and the target mineralogy that may host biological signatures.
Title: A wide variety of putative extremophiles and large
beta-diversity at the Mars Desert Research Station (Utah)
Authors: Direito, Susana O. L.; Ehrenfreund, Pascale; Marees, Andries;
Staats, Martijn; Foing, Bernard; Röling, Wilfred F. M.
Bibcode: 2011IJAsB..10..191D
Altcode:
Humankind's innate curiosity makes us wonder whether life is or was
present on other planetary bodies such as Mars. The EuroGeoMars
2009 campaign was organized at the Mars Desert Research Station
(MDRS) to perform multidisciplinary astrobiology research. MDRS in
southeast Utah is situated in a cold arid desert with mineralogy
and erosion processes comparable to those on Mars. Insight into the
microbial community composition of this terrestrial Mars analogue
provides essential information for the search for life on Mars:
including sampling and life detection methodology optimization
and what kind of organisms to expect. Soil samples were collected
from different locations. Culture-independent molecular analyses
directed at ribosomal RNA genes revealed the presence of all three
domains of life (Archaea, Bacteria and Eukarya), but these were
not detected in all samples. Spiking experiments revealed that
this appears to relate to low DNA recovery, due to adsorption or
degradation. Bacteria were most frequently detected and showed
high alpha- and beta-diversity. Members of the Actinobacteria,
Proteobacteria, Bacteroidetes and Gemmatimonadetes phyla were found
in the majority of samples. Archaea alpha- and beta-diversity was very
low. For Eukarya, a diverse range of organisms was identified, such as
fungi, green algae and several phyla of Protozoa. Phylogenetic analysis
revealed an extraordinary variety of putative extremophiles, mainly
Bacteria but also Archaea and Eukarya. These comprised radioresistant,
endolithic, chasmolithic, xerophilic, hypolithic, thermophilic,
thermoacidophilic, psychrophilic, halophilic, haloalkaliphilic
and alkaliphilic micro-organisms. Overall, our data revealed large
difference in occurrence and diversity over short distances, indicating
the need for high-sampling frequency at similar sites. DNA extraction
methods need to be optimized to improve extraction efficiencies.
Title: Analysis of mineral matrices of planetary soil analogues from
the Utah Desert
Authors: Kotler, J. M.; Quinn, R. C.; Foing, B. H.; Martins, Z.;
Ehrenfreund, P.
Bibcode: 2011IJAsB..10..221K
Altcode:
Phyllosilicate minerals and hydrated sulphate minerals have been
positively identified on the surface of Mars. Studies conducted on
Earth indicate that micro-organisms influence various geochemical
and mineralogical transitions for the sulphate and phyllosilicate
minerals. These minerals in turn provide key nutrients to
micro-organisms and influence microbial ecology. Therefore, the
presence of these minerals in astrobiology studies of Earth-Mars
analogue environments could help scientists better understand the
types and potential abundance of micro-organisms and/or biosignatures
that may be encountered on Mars. Bulk X-ray diffraction of samples
collected during the EuroGeoMars 2009 campaign from the Mancos Shale,
the Morrison and the Dakota formations near the Mars Desert Research
Station in Utah show variable but common sedimentary mineralogy with
all samples containing quantities of hydrated sulphate minerals
and/or phyllosilicates. Analysis of the clay fractions indicate
that the phyllosilicates are interstratified illite-smectites with
all samples showing marked changes in the diffraction pattern after
ethylene glycol treatment and the characteristic appearance of a
solvated peak at ∼17 Å. The smectite phases were identified as
montmorillonite and nontronite using a combination of the X-ray
diffraction data and Fourier-Transform Infrared Spectroscopy. The
most common sulphate mineral in the samples is hydrated calcium
sulphate (gypsum), although one sample contained detectable amounts of
strontium sulphate (celestine). Carbonates detected in the samples are
variable in composition and include pure calcium carbonate (calcite),
magnesium-bearing calcium carbonate (dolomite), magnesium, iron and
manganese-bearing calcium carbonate (ankerite) and iron carbonate
(siderite). The results of these analyses when combined with organic
extractions and biological analysis should help astrobiologists and
planetary geologists better understand the potential relationships
between mineralogy and microbiology for planetary missions.
Title: Multidisciplinary integrated field campaign to an acidic
Martian Earth analogue with astrobiological interest: Rio Tinto
Authors: Gómez, F.; Walter, N.; Amils, R.; Rull, F.; Klingelhöfer,
A. K.; Kviderova, J.; Sarrazin, P.; Foing, B.; Behar, A.; Fleischer,
I.; Parro, V.; Garcia-Villadangos, M.; Blake, D.; Martin Ramos, J. D.;
Direito, S.; Mahapatra, P.; Stam, C.; Venkateswaran, K.; Voytek, M.
Bibcode: 2011IJAsB..10..291G
Altcode:
Recently reported results from latest Mars Orbiters and Rovers missions
are transforming our opinion about the red planet. That dry and
inhospitable planet reported in the past is becoming a wetter planet
with high probabilities of water existence in the past. Nowadays,
some results seem to indicate the presence of water beneath the Mars
surface. But also mineralogy studies by NASA Opportunity Rover report
iron oxides and hydroxides precipitates on Endurance Crater. Sedimentary
deposits have been identified at Meridiani Planum. These deposits
must have generated in a dune aqueous acidic and oxidizing
environment. Similarities appear when we study Rio Tinto, and acidic
river under the control of iron. The discovery of extremophiles
on Earth widened the window of possibilities for life to develop in
the Universe, and as a consequence on Mars and other planetary bodies
with astrobiological interest. The compilation of data produced by the
ongoing missions offers an interested view for life possibilities to
exist: signs of an early wet Mars and rather recent volcanic activity
as well as ground morphological characteristics that seem to be
promoted by liquid water. The discovery of important accumulations of
sulfates and the existence of iron minerals such as jarosite in rocks
of sedimentary origin has allowed specific terrestrial models to come
into focus. Río Tinto (Southwestern Spain, Iberian Pyritic Belt)
is an extreme acidic environment, product of the chemolithotrophic
activity of micro-organisms that thrive in the massive pyrite-rich
deposits of the Iberian Pyritic Belt. Some particular protective
environments should house the organic molecules and bacterial life
forms in harsh environments such as Mars surface supporting microniches
inside precipitated minerals or inside rocks. Terrestrial analogues
could help us to afford the comprehension of habitability (on other
planetary bodies). We are reporting here the multidisciplinary
study of some endolithic niches inside salt deposits used by phototrophs
for taking advantage of sheltering particular light wavelengths. These
acidic salts deposits located in Río Tinto shelter life forms that are
difficult to visualize by eye. This interdisciplinary field analogue
campaign was conducted in the framework of the CAREX FP7 EC programme.
Title: Astrobiology field research in Moon/Mars analogue environments
Authors: Foing, B. H.; Stoker, C.; Ehrenfreund, P.
Bibcode: 2011IJAsB..10..137F
Altcode:
Extreme environments on Earth often provide similar terrain conditions
to landing/operation sites on Moon and Mars. Several field campaigns
(EuroGeoMars2009 and DOMMEX/ILEWG EuroMoonMars from November 2009
to March 2010) were conducted at the Mars Desert Research Station
(MDRS) in Utah. Some of the key astrobiology results are presented
in this special issue on ‘Astrobiology field research in Moon/Mars
analogue environments’ relevant to investigate the link between
geology, minerals, organics and biota. Preliminary results from a
multidisciplinary field campaign at Rio Tinto in Spain are presented.
Title: Linear and circular spectropolarimetry of diffuse interstellar
bands
Authors: Cox, N. L. J.; Ehrenfreund, P.; Foing, B. H.; D'Hendecourt,
L.; Salama, F.; Sarre, P. J.
Bibcode: 2011A&A...531A..25C
Altcode: 2011arXiv1104.4581C
Context. The identification of the carriers of diffuse interstellar
bands (DIBs) remains one of the long-standing mysteries in
astronomy. The detection of a polarisation signal in a DIB profile
can be used to distinguish between a dust or gas-phase carrier. The
polarisation profile can give additional information on the grain
or molecular properties of the absorber.
Aims: To measure the
polarisation efficiency of the carriers of the diffuse interstellar
bands.
Methods: In order to detect and measure the linear and
circular polarisation of the DIBs we observed reddened lines of sight
showing continuum polarisation. For this study we selected two stars
HD 197770 and HD 194279. We used
high-resolution (R ~ 64 000) spectropolarimetry in the wavelength range
from 3700 to 10 480 Å with the ESPaDOnS échelle spectrograph mounted
at the CFHT.
Results: High S/N and high resolution Stokes V
(circular), Q and U (linear) spectra were obtained. We constrained upper
limits by a factor of 10 for previously observed DIBs. Furthermore,
we analysed ~30 additional DIBs for which no spectropolarimetry data
has been obtained before. This included the 9577 Å DIB and the 8621
Å DIB. The former is attributed to the C60^+ fullerene,
which could become aligned in a magnetic field. The latter shows a
tight correlation with the amount of dust in the line-of-sight and
therefore most likely may show a polarisation signal related the
aligned grains.
Conclusions: The lack of polarisation in 45
DIB profiles suggests that none of the absorption lines is induced
by a grain-type carrier. The strict upper limits, less than ~0.01%,
derived for the observed lines-of-sight imply that if DIBs are due to
gas-phase molecules these carriers have polarisation efficiencies which
are at least 6 times, and up to 300 times, smaller than those predicted
for grain-related carriers. Based on observations obtained at the
Canada-France-Hawaii Telescope (CFHT) which is operated by the National
Research Council of Canada, the Institut National des Sciences de
l'Univers of the Centre National de la Recherche Scientique of France,
and the University of Hawaii.Appendices are available in electronic form
at http://www.aanda.orgIntensity
and polarisation spectra are only available at the CDS via
anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/531/A25
Title: Lunar mare single-scattering, porosity, and surface-roughness
properties with SMART-1 AMIE
Authors: Muinonen, K.; Parviainen, H.; Näränen, J.; Josset, J. -L.;
Beauvivre, S.; Pinet, P.; Chevrel, S.; Koschny, D.; Grieger, B.;
Foing, B.; AMIE SMART-1 Team
Bibcode: 2011A&A...531A.150M
Altcode:
A novel shadowing and coherent-backscattering model is utilized in the
analysis of the single-scattering albedos and phase functions, local
surface roughness, and regolith porosity of specific lunar mare regions
imaged by the AMIE camera (Advanced Moon micro-Imager Experiment)
onboard ESA SMART-1 mission. Shadowing due to the regolith particles is
accounted via ray-tracing computations for densely-packed particulate
media with a fractional-Brownian-motion interface with free space. The
shadowing modeling allows us to derive the scattering phase function for
a ~100-μm volume element of the lunar mare regolith. The volume-element
phase function is explained by coherent-backscattering modeling, where
the fundamental single scatterers are the wavelength-scale particle
inhomogeneities or the smallest fraction of the particles on the lunar
surface. The phase function of the fundamental scatterers is expressed
as a sum of two Henyey-Greenstein terms, accounting for increased
backward scattering as well as increased forward scattering. Based on
the modeling of the AMIE lunar photometry, we conclude that most of
the lunar mare opposition effect is caused by coherent backscattering
within volume elements comparable in size to typical lunar particles,
with only a small contribution from shadowing effects.
Title: Astrobiology and habitability studies in preparation for future
Mars missions: trends from investigating minerals, organics and biota
Authors: Ehrenfreund, P.; Röling, W. F. M.; Thiel, C. S.; Quinn, R.;
Sephton, M. A.; Stoker, C.; Kotler, J. M.; Direito, S. O. L.; Martins,
Z.; Orzechowska, G. E.; Kidd, R. D.; van Sluis, C. A.; Foing, B. H.
Bibcode: 2011IJAsB..10..239E
Altcode:
Several robotic exploration missions will travel to Mars during
this decade to investigate habitability and the possible presence of
life. Field research at Mars analogue sites such as desert environments
can provide important constraints for instrument calibration,
landing site strategies and expected life detection targets. We have
characterized the mineralogy, organic chemistry and microbiology of ten
selected sample sites from the Utah desert in close vicinity to the Mars
Desert Research Station (MDRS) during the EuroGeoMars 2009 campaign
(organized by International Lunar Exploration Working Group (ILEWG),
NASA Ames and ESA ESTEC). Compared with extremely arid deserts (such
as the Atacama), organic and biological materials can be identified
in a larger number of samples and subsequently be used to perform
correlation studies. Among the important findings of this field research
campaign are the diversity in the mineralogical composition of soil
samples even when collected in close proximity, the low abundances of
detectable polycyclic aromatic hydrocarbons (PAHs) and amino acids and
the presence of biota of all three domains of life with significant
heterogeneity. An extraordinary variety of putative extremophiles,
mainly Bacteria and also Archaea and Eukarya was observed. The dominant
factor in measurable bacterial abundance seems to be soil porosity
and lower small (clay-sized) particle content. However, correlations
between many measured parameters are difficult to establish. Field
research conducted during the EuroGeoMars 2009 campaign shows that the
geological history and depositional environment of the region, as well
as the mineralogy influence the ability to detect compounds such as
amino acids and DNA. Clays are known to strongly absorb and bind organic
molecules often preventing extraction by even sophisticated laboratory
methods. Our results indicate the need for further development and
optimization of extraction procedures that release biological compounds
from host matrices to enable the effective detection of biomarkers
during future sampling campaigns on Earth and Mars.
Title: Field astrobiology research in Moon-Mars analogue environments:
instruments and methods
Authors: Foing, B. H.; Stoker, C.; Zavaleta, J.; Ehrenfreund, P.;
Thiel, C.; Sarrazin, P.; Blake, D.; Page, J.; Pletser, V.; Hendrikse,
J.; Direito, S.; Kotler, J. M.; Martins, Z.; Orzechowska, G.; Gross,
C.; Wendt, L.; Clarke, J.; Borst, A. M.; Peters, S. T. M.; Wilhelm,
M. -B.; Davies, G. R.; Davies
Bibcode: 2011IJAsB..10..141F
Altcode:
We describe the field demonstration of astrobiology instruments and
research methods conducted in and from the Mars Desert Research Station
(MDRS) in Utah during the EuroGeoMars campaign 2009 coordinated by
ILEWG, ESA/ESTEC and NASA Ames, with the contribution of academic
partners. We discuss the entire experimental approach from determining
the geological context using remote sensing, in situ measurements,
sorties with sample collection and characterization, analysis in
the field laboratory, to the post sample analysis using advanced
laboratory facilities. We present the rationale for terrestrial
field campaigns to strengthen astrobiology research and the link between
in situ and orbital remote sensing data. These campaigns are supporting
the preparation for future missions such as Mars Science Laboratory,
ExoMars or Mars Sample Return. We describe the EuroGeoMars 2009 campaign
conducted by MDRS crew 76 and 77, focused on the investigation of
surface processes in their geological context. Special emphasis was
placed on sample collection and pre-screening using in-situ portable
instruments. Science investigations included geological and geochemical
measurements as well as detection and diagnostic of water, oxidants,
organic matter, minerals, volatiles and biota. EuroGeoMars 2009
was an example of a Moon-Mars field research campaign dedicated to the
demonstration of astrobiology instruments and a specific methodology
of comprehensive measurements from selected sampling sites. We discuss
in sequence: the campaign objectives and trade-off based on science,
technical or operational constraints. This includes remote sensing
data and maps, and geological context; the monitoring of environmental
parameters; the geophysical context and mineralogy studies; geology
and geomorphology investigations; geochemistry characterization and
subsurface studies. We describe sample handling (extraction
and collection) methods, and the sample analysis of soils and rocks
performed in the MDRS laboratory using close inspection, initial
petrological characterization, microscopy, Visible-NIR spectrometry,
Raman spectrometry, X-ray diffraction/X-ray fluorescence spectrometry,
soil analysis, electrochemical and biological measurements. The
results from post-mission analysis of returned samples using advanced
facilities in collaborator institutes are described in companion
papers in this issue. We present examples of in-situ analysis, and
describe an example investigation on the exploration and analysis
of endolithic microbial mats (from reconnaissance, in-situ imaging,
sampling, local analysis to post-mission sample analysis).
Title: Human crew-related aspects for astrobiology research
Authors: Thiel, Cora S.; Pletser, Vladimir; Foing, Bernard
Bibcode: 2011IJAsB..10..255T
Altcode:
Several space agencies and exploration stakeholders have a strong
interest in obtaining information on technical and human aspects to
prepare for future extra-terrestrial planetary exploration. In this
context, the EuroGeoMars campaign, organized with support from the
International Lunar Exploration Working Group (ILEWG), the European
Space Agency (ESA), the National Aeronautics and Space Administration
(NASA) Ames Research Center and partner institutes, was conducted by
the crews 76 and 77 in February 2009 in The Mars Society's ‘Mars
Desert Research Station’ (MDRS) in Utah. The EuroGeoMars
encompasses two groups of experiments: (1) a series of field science
experiments that can be conducted from an extra-terrestrial planetary
surface in geology, biology, astronomy/astrophysics and the necessary
technology and networks to support these field investigations; (2) a
series of human crew-related investigations on crew time organization
in a planetary habitat, on the different functions and interfaces of
this habitat, and on man-machine interfaces of science and technical
equipment. This paper recalls the objective of the EuroGeoMars
project and presents the MDRS and its habitat layout. Social and
operational aspects during simulations are described. Technical and
operational aspects of biology investigations in the field and in the
habitat laboratory are discussed in detail with the focus point set
on the polymerase chain reaction (PCR)-based detection of microbial
DNA in soil samples.
Title: PCR-based analysis of microbial communities during the
EuroGeoMars campaign at Mars Desert Research Station, Utah
Authors: Thiel, Cora S.; Ehrenfreund, Pascale; Foing, Bernard; Pletser,
Vladimir; Ullrich, Oliver
Bibcode: 2011IJAsB..10..177T
Altcode:
The search for evidence of past or present life on Mars will require
the detection of markers that indicate the presence of life. Because
deoxyribonucleic acid (DNA) is found in all known living organisms,
it is considered to be a ‘biosignature’ of life. The main function
of DNA is the long-term storage of genetic information, which is
passed on from generation to generation as hereditary material. The
Polymerase Chain Reaction (PCR) is a revolutionary technique which
allows a single fragment or a small number of fragments of a DNA
molecule to be amplified millions of times, making it possible to
detect minimal traces of DNA. The compactness of the contemporary
PCR instruments makes routine sample analysis possible with a minimum
amount of laboratory space. Furthermore the technique is effective,
robust and straightforward. Our goal was to establish a routine for the
detection of DNA from micro-organisms using the PCR technique during the
EuroGeoMars simulation campaign. This took place at the Mars Society's
Mars Desert Research Station (MDRS) in Utah in February 2009 (organized
with the support of the International Lunar Exploration Working Group
(ILEWG), NASA Ames and the European Space Research and Technology
Centre (ESTEC)). During the MDRS simulation, we showed that it is
possible to establish a minimal molecular biology lab in the habitat
for the immediate on-site analysis of samples by PCR after sample
collection. Soil and water samples were taken at different locations
and soil depths. The sample analysis was started immediately after
the crew returned to the habitat laboratory. DNA was isolated from
micro-organisms and used as a template for PCR analysis of the highly
conserved ribosomal DNA to identify representatives of the different
groups of micro-organisms (bacteria, archaea and eukarya). The PCR
products were visualized by agarose gel electrophoresis and documented
by transillumination and digital imaging. The microbial diversity in
the collected samples was analysed with respect to sampling depth
and the presence or absence of vegetation. For the first time, we
have demonstrated that it is possible to perform direct on-site DNA
analysis by PCR at MDRS, a simulated planetary habitat in an extreme
environment that serves as a model for preparation and optimization
of techniques to be used for future Mars exploration.
Title: Analysis of Mars analogue soil samples using
solid-phase microextraction, organic solvent extraction and gas
chromatography/mass spectrometry
Authors: Orzechowska, G. E.; Kidd, R. D.; Foing, B. H.; Kanik, I.;
Stoker, C.; Ehrenfreund, P.
Bibcode: 2011IJAsB..10..209O
Altcode:
Polycyclic aromatic hydrocarbons (PAHs) are robust and abundant
molecules in extraterrestrial environments. They are found ubiquitously
in the interstellar medium and have been identified in extracts of
meteorites collected on Earth. PAHs are important target molecules
for planetary exploration missions that investigate the organic
inventory of planets, moons and small bodies. This study is part of
an interdisciplinary preparation phase to search for organic molecules
and life on Mars. We have investigated PAH compounds in desert soils to
determine their composition, distribution and stability. Soil samples
(Mars analogue soils) were collected at desert areas of Utah in the
vicinity of the Mars Desert Research Station (MDRS), in the Arequipa
region in Peru and from the Jutland region of Denmark. The aim of this
study was to optimize the solid-phase microextraction (SPME) method for
fast screening and determination of PAHs in soil samples. This method
minimizes sample handling and preserves the chemical integrity of the
sample. Complementary liquid extraction was used to obtain information
on five- and six-ring PAH compounds. The measured concentrations of PAHs
are, in general, very low, ranging from 1 to 60 ng g-1. The
texture of soils is mostly sandy loam with few samples being 100 %
silt. Collected soils are moderately basic with pH values of 8-9
except for the Salten Skov soil, which is slightly acidic. Although
the diverse and variable microbial populations of the samples at
the sample sites might have affected the levels and variety of PAHs
detected, SPME appears to be a rapid, viable field sampling technique
with implications for use on planetary missions.
Title: Mineralogical, chemical, organic and microbial properties of
subsurface soil cores from Mars Desert Research Station (Utah, USA):
Phyllosilicate and sulfate analogues to Mars mission landing sites
Authors: Stoker, Carol R.; Clarke, Jonathan; Direito, Susana O. L.;
Blake, David; Martin, Kevin R.; Zavaleta, Jhony; Foing, Bernard
Bibcode: 2011IJAsB..10..269S
Altcode:
We collected and analysed soil cores from four geologic units
surrounding Mars Desert Research Station (MDRS) Utah, USA, including
Mancos Shale, Dakota Sandstone, Morrison formation (Brushy Basin member)
and Summerville formation. The area is an important geochemical and
morphological analogue to terrains on Mars. Soils were analysed
for mineralogy by a Terra X-ray diffractometer (XRD), a field
version of the CheMin instrument on the Mars Science Laboratory
(MSL) mission (2012 landing). Soluble ion chemistry, total organic
content and identity and distribution of microbial populations were
also determined. The Terra data reveal that Mancos and Morrison
soils are rich in phyllosilicates similar to those observed on
Mars from orbital measurements (montmorillonite, nontronite and
illite). Evaporite minerals observed include gypsum, thenardite,
polyhalite and calcite. Soil chemical analysis shows sulfate the
dominant anion in all soils and SO4>>CO3,
as on Mars. The cation pattern Na>Ca>Mg is seen in all soils
except for the Summerville where Ca>Na. In all soils, SO4
correlates with Na, suggesting sodium sulfates are the dominant
phase. Oxidizable organics are low in all soils and range from a
high of 0.7% in the Mancos samples to undetectable at a detection
limit of 0.1% in the Morrison soils. Minerals rich in chromium and
vanadium were identified in Morrison soils that result from diagenetic
replacement of organic compounds. Depositional environment, geologic
history and mineralogy all affect the ability to preserve and detect
organic compounds. Subsurface biosphere populations were revealed to
contain organisms from all three domains (Archaea, Bacteria and Eukarya)
with cell density between 3.0×106 and 1.8×107
cells ml-1 at the deepest depth. These measurements are
analogous to data that could be obtained on future robotic or human
Mars missions and results are relevant to the MSL mission that will
investigate phyllosilicates on Mars.
Title: The ORGANIC Experiment on the ISS EXPOSE-R
Authors: Bryson, K.; Peeters, Z.; Salama, F.; Foing, B.; Ehrenfreund,
P.; Jessberger, E.; Bischoff, A.; Breitfellner, M.; Schmidt, W.
Bibcode: 2011IAUS..280P.401B
Altcode:
Polycyclic aromatic hydrocarbons (PAHs) and aromatic networks are among
the most abundant organic material in space. PAHs and fullerenes have
been identified in meteorites and are proposed as carriers for numerous
astronomical absorption and emission features. Recently the fullerenes
C60 and C70 have been discovered in a young planetary nebula, Tc 1 and
in other astronomical environments. Thin films of selected PAHs and
fullerenes have been subjected to the low Earth orbit environment as
part of the ORGANIC experiment on the multi-user facility EXPOSE-R,
which was deployed onboard the International Space Station (ISS)
in March 2009 and retrieved by extra-vehicular activity (EVA) in
January 2011. The ORGANIC experiment monitors the chemical evolution,
survival, destruction, and chemical modification of PAHs and fullerenes
exposed to solar illumination and cosmic radiation. The radiation
dose that is collected on the ISS by the samples cannot be accurately
simulated in Earth laboratories. Dark samples are shielded from the
UV photons and will enable us to differentiate between the effects of
exposure to photons and cosmic rays. The samples are monitored before
and after space exposure; ground control samples were continuously
monitored. We describe the ORGANIC experiment on the Space Station and
report on laboratory ground-control measurements in the UV-Vis-NIR
at NASA-Ames. Extended space exposure allows us to collect data on
multiple samples which can be extrapolated to other astrophysical
environments and thus greatly enhance our knowledge on the evolution
of organic compounds in space environment.
Title: Ground Control Monitoring for the Organics Experiment on the
EXPOSE-R Facility on the International Space Station
Authors: Bryson, K. L.; Salama, F.; Ehrenfreund, P.; Ricco, A. J.;
Peeters, Z.; Foing, B.; Jessberger, E.; Robert, F.; Mumma, M.
Bibcode: 2011nlaw.confC..39B
Altcode:
The Organics experiment is integrated into the multi-user facility
EXPOSER mounted on the International Space Station (ISS). In this
experiment organic samples of astronomical interest are exposed for
a long duration to the space environment and will remain 24 months
on-board the ISS before they are returned to Earth in March 2011. The
radiation dose that is collected by the samples during flight exceeds
the limits of simulations in the laboratory and the results will greatly
enhance our knowledge on the evolution of large molecules in space
environments. We describe the experimental components that are being
used on the ISS for the exposure experiments and in the laboratory
for ground-control measurements and present spectra measured in the
UV-Vis range monitoring the ground control samples.
Title: Utah Desert Analogue Sites for Mars Research and Missions
Authors: Foing, B. H.; Stoker, C.; Ehrenfreund, P.; Eurogeomars Team;
Domex Team; Euromoonmars Team
Bibcode: 2011LPICo1612.6029F
Altcode:
No abstract at ADS
Title: Bioaugmentation in growing plants for lunar bases
Authors: Zaets, I.; Burlak, O.; Rogutskyy, I.; Vasilenko, A.;
Mytrokhyn, O.; Lukashov, D.; Foing, B.; Kozyrovska, N.
Bibcode: 2011AdSpR..47.1071Z
Altcode:
Microorganisms may be a key element in a precursory scenario of growing
pioneer plants for extraterrestrial exploration. They can be used
for plant inoculation to leach nutritional elements from regolith,
to alleviate lunar stressors, as well as to decompose both lunar
rocks and the plant straw in order to form a protosoil. Bioleaching
capacities of both French marigold (Tagetes patula L.) and the
associated bacteria in contact with a lunar rock simulant (terrestrial
anorthosite) were examined using the model plant-bacteria microcosms
under controlled conditions. Marigold accumulated K, Na, Fe, Zn,
Ni, and Cr at higher concentrations in anorthosite compared to the
podzol soil. Plants inoculated with the consortium of well-defined
species of bacteria accumulated higher levels of K, Mg, and Mn, but
lower levels of Ni, Cr, Zn, Na, Ca, Fe, which exist at higher levels
in anorthosite. Bacteria also affected the Са/Mg and Fe/Mn ratios
in the biomass of marigold grown on anorthosite. Despite their growth
retardation, the inoculated plants had 15% higher weight on anorthosite
than noninoculated plants. The data suggest that the bacteria supplied
basic macro-and microelements to the model plant.
Title: Properties of Subsurface Soil Cores from Four Geologic
Provinces Surrounding Mars Desert Research Station, Utah:
Characterizing Analog Martian Soil in a Human Exploration Scenario
Authors: Stoker, C. R.; Clarke, J. D. A.; Direito, S.; Foing, B.
Bibcode: 2011LPI....42.1231S
Altcode:
We present results of analysis of sulfate-rich soil cores from Mars
analog site in Utah.
Title: Astrobiology and Habitability Studies Supporting Mars Research
and Missions
Authors: Foing, B. H.; Thiel, C.; Direito, S.; Ehrenfreund, P.; Roling,
W.; Martins, Z.; Sephton, M.; Stoker, C.; Zhavaleta, J.; Orzechowska,
G.; Kidd, R.; Quinn, R.; Kotler, M.; Eurogeomars Mdrs Team
Bibcode: 2011LPI....42.1762F
Altcode:
During EuroGeoMars 2009 campaign, we characterized the mineralogy,
organic compounds and microbiology of selected samples from different
geological sites, and established correlations (Special Issue:
“Astrobiology field research in Moon/Mars analog environments”:
IJA 2011).
Title: VizieR Online Data Catalog: Linear and circular polarisation
of diffuse interstellar bands.
Authors: Cox, N. L. J.; Ehrenfreund, P.; Foing, B. H.; D'Hendecourt,
L.; Salama, F.; Sarre, P. J.
Bibcode: 2011yCat..35310025C
Altcode: 2011yCat..35319025C
Linear and circular polarisation and total intensity spectra obtained
with ESPaDOnS at the CFHT for the two lines-of-sight towards HD197770
and HD194279. For each line-of-sight we give the average (globally
normalised) Stokes I, Q, U, and V spectra. The spectra cover the
wavelength range from 376nm to 1000nm. (2 data files).
Title: Investigation in Mars analogue habitats of the Transantarctic
Mountains of Victoria Land
Authors: de Vera, J. -P. P.; Foing, B.; Ullrich, E.; Ott, S.
Bibcode: 2010epsc.conf..145D
Altcode:
No abstract at ADS
Title: Fullerenes and Cosmic Carbon
Authors: Ehrenfreund, P.; Foing, B. H.
Bibcode: 2010Sci...329.1159E
Altcode:
No abstract at ADS
Title: Beijing Lunar Declaration 2010: A) GLUC-ICEUM11 Report and
Recommendations on Science and Exploration
Authors: Arvidson, R.; Foing, B. H.; Cohen, B.; Plescia, J.; Blamont,
J. E.; Gluc-Iceum1 Participants
Bibcode: 2010LPICo1595....3A
Altcode:
No abstract at ADS
Title: Beijing Lunar Declaration 2010: B) Technology and Resources;
Infrastructures and Human Aspects; Moon, Space and Society
Authors: Arvidson, R.; Foing, B. H.; Blamont, J. E.; Plescia, J.;
Cohen, B.; Gluc-Iceum1 Participants
Bibcode: 2010LPICo1595....4A
Altcode:
No abstract at ADS
Title: Lunar single-scattering, porosity, and surface-roughness
characteristics with SMART-1/AMIE
Authors: Näränen, J.; Parviainen, H.; Muinonen, K.; Josset, J. -L.;
Beauvivre, S.; Pinet, P.; Chevrel, S.; Koschny, D.; Grieger, B.;
Foing, B.
Bibcode: 2010els..conf..202N
Altcode:
No abstract at ADS
Title: 3D structure of the Gusev Crater region
Authors: Parker, Mirjam van Kan; Zegers, Tanja; Kneissl, Thomas;
Ivanov, Boris; Foing, Bernard; Neukum, Gerhard
Bibcode: 2010E&PSL.294..411P
Altcode:
Gusev Crater lies within the Aeolis Quadrangle of Mars at the boundary
between the northern lowlands and southern highlands. The ancient
valley Ma'adim Vallis dissects the highlands south of Gusev Crater
and is thought to have fed the crater with sediments. High Resolution
Stereo Camera data and Digital Elevation Models were used to construct a
geologic-geomorphic map (173.5-178.5° E, 10-18° S) and cross-sections,
complemented by data from Mars Orbiter Camera, Mars Orbiter Laser
Altimeter and Thermal Emission Imaging System. Three geologic domains
are recognised: the highlands in the south, Gusev Crater and lowlands
in the north. Twelve units are mapped, with thicknesses ranging
from hundred meters to several kilometres. Thicknesses of units,
and their bedding attitude, are estimated combining the geologic
map and topographic information. Relative ages are determined from
crater counts, ranging from Early Noachian for highland units to
Middle Amazonian for units in Gusev Crater and in lowlands. Episodes
of intense geologic activity (deposition, volcanism, deformation)
occur at around 4.0 Ga, 3.7 Ga, and 3.5 Ga. Comparing the geometry
of the Gusev Crater with similar sized, filled and un-filled, Martian
craters, suggests that the Columbia Hills are relics of the original
central peak of Gusev Crater.
Title: The SMART-1 lunar impact
Authors: Burchell, M. J.; Robin-Williams, R.; Foing, B. H.
Bibcode: 2010Icar..207...28B
Altcode:
The SMART-1 spacecraft impacted the Moon on 3rd September 2006 at a
speed of 2 km s -1 and at a very shallow angle of incidence
(∼1°). The resulting impact crater is too small to be viewed from
the Earth; accordingly, the general crater size and shape have been
determined here by laboratory impact experiments at the same speed and
angle of incidence combined with extrapolating to the correct size scale
to match the SMART-1 impact. This predicts a highly asymmetric crater
approximately 5.5-26 m long, 1.9-9 m wide, 0.23-1.5 m deep and 0.71-6.9
m 3 volume. Some of the excavated mass will have gone into
crater rim walls, but 0.64-6.3 m 3 would have been ejecta
on ballistic trajectories corresponding to a cloud of 2200-21,800
kg of lunar material moving away from the impact site. The shallow
Messier crater on the Moon is similarly asymmetric and is usually
taken as arising from a highly oblique impact. The light flash from
the impact and the associated ejecta plume were observed from Earth,
but the flash magnitude was not obtained, so it is not possible to
obtain the luminous efficiency of the impact event.
Title: UV and Space Exposure of Aromatic Compounds on the EXPOSE-R
Facility Onboard the International Space Station
Authors: Bryson, Kathryn; Salama, F.; Ehrenfreund, P.; Ricco, A. J.;
Peeters, Z.; Foing, B.; Jessberger, E.; Robert, F.; Mumma, M.
Bibcode: 2010AAS...21641106B
Altcode: 2010BAAS...41..820B
Aromatic networks are likely the most abundant organic material in
space. Specifically, polycyclic aromatic hydrocarbons (PAHs) and
fullerenes have been identified in meteorites and are thought to be
among the carriers for numerous astronomical absorption and emission
features. Thin films of selected PAHs and fullerenes are being subjected
to the low Earth orbit environment as part of the Organics experiment
on the multi-user facility EXPOSE-R, which has been deployed onboard
the International Space Station since March 2009 and will be retrieved
in Fall 2010. The Organics experiment monitors the chemical evolution,
survival, destruction, and chemical modification of PAHs and fullerenes
exposed to solar illumination and cosmic radiation. The radiation dose
that is collected by the samples during flight exceeds the limits of
simulations in the laboratory and will greatly enhance our knowledge on
the evolution of large molecules in space environments. Dark samples are
shielded from the UV photons and will enable us to differentiate between
the effects of exposure to photons and cosmic rays. The samples are
monitored before and after space exposure. We present spectra measured
in the UV-Vis-NIR range of ground control samples and flight samples.
Title: ExoHab Pilot Project & Field Tests for Moon-Mars Human
Laboratories
Authors: Foing, Bernard
Bibcode: 2010EGUGA..1213688F
Altcode:
We studied concepts for a minimal Moon-Mars habitat, in focussing on the
system aspects and coordinating every different part as part an evolving
architecture. We validated experimentally the Habitat and Laboratory
ExoHab concept constraints during EuroGeoMars campaign in Utah desert
research station (from 24 Jan. to 28 Feb. 2009) and EuroMoonMars/DOMMEX
campaigns in Nov 2009 and February-April 2010. We discuss from the ILEWG
ExoHab concept studies and field simulations the specifics of human
exploration, with focus on habitability and human performance. In the
ExoHab pilot concept project (supported by ILEWG, ESA NASA), we justify
the case for a scientific and exploration outpost allowing experiments,
sample analysis in laboratory (relevant to the origin and evolution of
planets and life, geophysical and geo-chemical studies, astrobiology
and life sciences, observation sciences, technology demonstration,
resource utilisation, human exploration and settlement). In this
modular concept, we consider various infra structure elements: core
habitat, Extra Vehicular activity (EVA), crew mobility, energy supply,
recycling module, communication, green house and food production,
operations. We review some studies space agencies' architecture
proposals, with landers, orbiters, rovers, habitats, surface operations
and protocols. We focus on the easiest and the soonest way in settling
a minimal base immediately operational in scientific experimentation and
exploration, but not immediately autonomous. Through a modular concept,
this outpost will be possibly evolved into a long duration or permanent
base. We will analyse the possibilities of settling such a minimal
base by means of the current and near term propulsion technology,
as a full Ariane 5 ME carrying 1.7 T of gross payload to the surface
of the Moon (Integrated Exploration Study, ESA ESTEC [1,2]). The low
solar rays incidence may permit having ice in deep craters, which
will be beneficial for the evolution of the outpost into an autonomous
base. After a robotic sample return mission, a human presence will allow
deeper research through well chosen geological samples. A polar lunar
outpost can serve to prepare for a Mars outpost: system and crew safety
aspects, use of local resources, operations on farside with limited
communication to Earth, planetary protection protocol, astrobiology and
life sciences. References: [1] Exploration Architecture Trade Report",
ESA 2008. [2] Integrated Exploration Architecture", ESA, 2008. [3]
9th ILEWG International Conference on Exploration Utilization of the
moon, 2007, sci.esa.int/ilewg [4] Schrunk et al , The Moon: Resources,
Future Development and Colonization", 1999. [5] The Moon as a Platform
for Astronomy and Space Science", B.H. Foing, ASR 14 (6), 1994. [6]
Boche-Sauvan L., Foing B (2008) MSc/ESTEC report. Co-authors, ILEWG
ExoGeoLab & ExoHab Team: B.H. Foing(1,11)*#, C. Stoker(2,11)*,
P. Ehrenfreund(10,11), L. Boche-Sauvan(1,11)*, L. Wendt(8)*, C. Gross(8,
11)*, C. Thiel(9)*, S. Peters(1,6)*, A. Borst(1,6)*, J. Zavaleta(2)*,
P. Sarrazin(2)*, D. Blake(2), J. Page(1,4,11), V. Pletser(5,11)*,
E. Monaghan(1)*, P. Mahapatra(1)#, A. Noroozi(3), P. Giannopoulos(1,11)
, A. Calzada(1,6,11), R. Walker(7), T. Zegers(1, 15) #, G. Groemer(12)#
, W. Stumptner(12)#, B. Foing(2,5), J. K. Blom(3)#, A. Perrin(14)#,
M. Mikolajczak(14)#, S. Chevrier(14)#, S. Direito(6)#, S. Voute
(18)#, A. Olmedo-Soler(17)#, T. E. Zegers(1, 18)#, D. Scheer(12)#,
K. Bickert(12)#, D. Schildhammer(12)#, B. Jantscher(1, 11, 12)#, MECA
Team(6)#, ExoGeoLab ILEWG ExoHab teams(1,4,11) EuroGeoMars team(1,4,5);
1)ESTEC/SRE-S Postbus 299, 2200 AG Noordwijk, NL, 2)NASA Ames , 3)Delft
TU , 4)ESTEC TEC Technology Dir., 5)ESTEC HSF Human Spaceflight,
6)VU Amsterdam, 7)ESTEC Education Office, 8)FU Berlin, 9)Max Planck
Goettingen, 10)Leiden/GWU , 11)ILEWG ExoHab Team, 12)Austrian Space
Forum (OEWF Innsbruck); 14) Ecole de l'Air, Salons de Provence,
15) Utrecht U., 16) MECA Team, 17) Olmedo Knowledge Systems S.L.;
* EuroGeoMars Utah crew , # ILEWG Eifel crew, EuroMoonMars/DOMMEX
Utah crew.
Title: Photosynthesis and Its Implications for Space Research
Authors: de Vera, J. P. P.; Leya, T.; Lorek, A.; Koncz, A.; de La
Torre Noetzel, R.; Kozyrovska, N.; Burlak, O.; Foing, B.
Bibcode: 2010LPICo1538.5139D
Altcode:
Photosynthesis is useful for biosignature definition, for the definition
of the habitability of a planet, for research on the likelihood of
Panspermia and for use in manned space flight missions by integration
into life supporting systems.
Title: ExoHab and EuroGeoMars Campaigns: Human Exploration and
Astrobiology
Authors: Foing, B. H.; Boche-Sauvan, L.; Stoker, C.; Ehrenfreund, P.;
Wendt, L.; Gross, C.; Thiel, C.; Peters, S.; Borst, A.; Zhavaleta,
J.; Sarrazin, P.; Blake, D.; Page, J.; Pletser, V.; Monaghan, E.;
Mahapatra, P.; Wills, D.; Noroozi, A.; Walker, R.; Zegers, T.;
Exogeolab; Exohab Team; Eurogeomars Team
Bibcode: 2010LPICo1538.5625F
Altcode:
We studied concepts for a minimal ExoHab habitat, in focussing on the
system aspects and as part of an evolving architecture. We validated
experimentally the ExoHab concept during EuroGeoMars campaign in Utah
desert research station (24 Jan. to 28 Feb. 2009).
Title: Eurogeomars Field Campaingn: Sample Analysis of Organic Matter
and Minerals
Authors: Foing, B. H.; Stoker, C.; Zhavaleta, J.; Ehrenfreund,
P.; Quinn, R.; Blake, D.; Martins, Z.; Sephton, M.; Becker, L.;
Orzechowska, G.; van Sluis, C.; Boche-Sauban, L.; Gross, C.; Thiel,
C.; Wendt, L.; Sarrazin, P.; Mahapatra, P.; Direito, S.; Roling, W.;
Eurogeomars Mdrs Team
Bibcode: 2010LPICo1538.5656F
Altcode:
A strategic search for life on Mars requires a thorough
interdisciplinary preparation phase that include the optimization of
sample analysis techniques, instrument development and calibration
and extensive terrestrial field test at Mars analog sites.
Title: Sample Collection and Analysis from CAREX Field Workshop at
Rio Tinto
Authors: Direito, S.; Foing, B. H.; Mahapatra, P.; Gomez, F.; Rull,
F.; Carex Rio Tinto 2009 Workshop
Bibcode: 2010LPICo1538.5648D
Altcode:
We described the sample collection protocol, multi- measurements
techniques and selected results (using Ramand and visible NIR
spectrometer) and interpretation from a CAREX field workshop at Rio
Tinto in september 2009.
Title: Testing Portable Raman Spectrometry for Astrobiology
Authors: Som, S. M.; Foing, B. H.; Exogeolab Team
Bibcode: 2010LPICo1538.5085S
Altcode:
We report on results of mineralogical, petrological and biological
samples using a 785nm DeltaNu Rockhound portable Raman spectrometer.
Title: The Organics Experiment on EXPOSE-R
Authors: Bryson, K. L.; Peeters, Z.; Salama, F.; Ehrenfreund, P.;
Foing, B.; Ricco, A. J.; Monaghan, E.; Willis, D.; Breitfellner, M.;
Jessberger, E.; Robert, F.; Mumma, M.
Bibcode: 2010LPICo1538.5513B
Altcode:
Thin films of selected PAHs and fullerenes are being subjected to the
low Earth orbit environment as part of the Organics experiment on the
multi-user facility EXPOSE-R onboard the International Space Station.
Title: ExoGeoLab Test Bench for Landers, Rovers and Astrobiology
Instruments
Authors: Foing, B. H.; Mahapatra, P.; Boche-Sauvan, L.; Som, S.;
Page, J.; Stoker, C.; Zhavaleta, J.; Sarrazin, P.; Blake, D.;
Poulakis, P.; Visentin, G.; Noroozi, A.; Ehrenfreund, P.; Barton,
A.; Lebreton, J. P.; Zegers, T.; Koschny, D.; Peters, S.; Borst, A.;
Monaghan, E.; Wills, D.; Thiel, C.; Wendt, L.; Gross, C.; Nijman,
F.; Pletser, V.; McKay, C.; Davies, G.; van Westrenen, W.; Batenburg,
P.; Drijkoningen, G.; Slob, E.; Gill, E.; Guglielmi, M.; Freire, M.;
Walker, R.; Exogeolab Team
Bibcode: 2010LPICo1538.5477F
Altcode:
ExoGeoLab is a Robotic Test Bench used to validate concepts and
instruments packages that could help in the technical research and
science preparation of lander and rover missions for astrobiology.
Title: ExoGeoLab Lander, Rovers and Instruments: Tests at ESTEC &
Eifel Volcanic Field
Authors: Foing, B. H.; Barton, A.; Blom, J. K.; Mahapatra, P.; Som,
S.; Jantscher, B.; Page, J.; Zegers, T.; Stoker, C.; Zavaleta, J.;
Poulakis, P.; Visentin, G.; Noroozi, A.; Ehrenfreund, P.; Mickolacjzak,
M.; Perrin, A.; Chevrier, S.; Direito, S.; Dene, A.; Voute, S.;
Olmedo, A.; Groemer, G.; Stumptner, W.; Davies, G.; van Westrenen,
W.; Koschny, D.; Lebreton, J. P.; Guglielmi, M.; Freire, M.; Walker,
R.; ILEWG Exogeolab Team; ILEWG Eifel Field Test Team
Bibcode: 2010LPI....41.1701F
Altcode:
We have built an ExoGeoLab lander demonstrator for future planetary
missions, equipped with remotely operated instruments. We tested them
at ESTEC and at an ILEWG field campaign at Eifel volcanic park in
Germany in September 2009.
Title: Geochemical Results from EuroGeoMars MDRS Utah 2009 Campaign
Authors: Borst, A.; Peters, S.; Foing, B. H.; Stoker, C.; Wendt, L.;
Gross, C.; Zavaleta, J.; Sarrazin, P.; Blake, D.; Ehrenfreund, P.;
Boche-Sauvan, L.; Page, J.; McKay, C.; Batenburg, P.; Drijkoningen,
G.; Slob, E.; Poulakis, P.; Visentin, G.; Noroozi, A.; Gill, E.;
Guglielmi, M.; Freire, M.; Walker, R.; Sabbatini, M.; Pletser,
V.; Monaghan, E.; Ernst, R.; Oosthoek, J.; Mahapatra, P.; Wills,
D.; Thiel, C.; Lebreton, J. P.; Zegers, T.; Chicarro, A.; Koschny,
D.; Vago, J.; Svedhem, H.; Davies, G.; Westenberg, A.; Edwards, J.;
Exogeolab Team; Eurogeomars Team
Bibcode: 2010LPI....41.2744B
Altcode:
We report on the geochemistry investigations during the EuroGeoMars
Campaign at the MDRS station in Utah. A total of ~150 samples from
different lithologies were analyzed using advanced and miniaturized
instruments (XRF, Raman and spectrometers).
Title: Highlights from Remote Controlled Rover for EuroGeoMars
MDRS Campaign
Authors: Hendrikse, J.; Foing, B. H.; Monaghan, E.; Stoker, C.;
Zavaleta, J.; Selch, F.; Ehrenfreund, P.; Wendt, L.; Gross, C.; Thiel,
C.; Peters, S.; Borst, A.; Sarrazin, P.; Blake, D.; Boche-Sauvan, L.;
Page, J.; Pletser, V.; Mahapatra, P.; Wills, D.; McKay, C.; Davies,
G.; van Westrenen, W.; Batenburg, P.; Drijkoningen, G.; Slob, E.;
Poulakis, P.; Visentin, G.; Noroozi, A.; Gill, E.; Guglielmi, M.;
Freire, M.; Walker, R.; Exogeolab Team; Eurogeomars Team
Bibcode: 2010LPI....41.2435H
Altcode:
The goal of the EuroGeoMars mission (from January 24 through February
28, 2009) was to validate a remote controlled rover for surface
reconnaissance and extravehicular activity support and evaluate rover
technical requirement for remote controlled reconnaissance from a
habitat and in situ support.
Title: ILEWG Eifel 2009 Campaign: Astronaut Extravehicular
Surface/Subsurface Activities and Human Aspects
Authors: Groemer, G.; Stumptner, W.; Foing, B.; Blom, J. K.; Perrin,
A.; Mikolajczak, M.; Chevrier, S.; Direito, S.; Olmedo-Soler, A.;
Zegers, T. E.; Scheer, D.; Bickert, K.; Schildhammer, D.; Jantscher,
B.; Mahapatra, P.; Meca Team
Bibcode: 2010LPI....41.1680G
Altcode:
The ILEWG organised a field campaign on 26-30 Sep 2009 with partners
in Mendig, Germany, in the volcanic Eifel region. They tested their
systems as simulation of lunar or planetary human and robotic mission
operations, and for the first time in a subterranean lavadome.
Title: The Cyborg Astrobiologist: Testing a Novelty Detection
Algorithm at the Mars Desert Research Station (MDRS), Utah
Authors: Gross, C.; Wendt, L.; McGuire, P. C.; Bonnici, A.;
Foing, B. H.; Souza-Egipsy, V.; Bose, R.; Walter, S.; Ormö, J.;
Díaz-Martínez, E.; Oesker, M.; Ontrup, J.; Haschke, R.; Ritter, H.
Bibcode: 2010LPI....41.2457G
Altcode:
Herein we present a computer vision algorithm, based in part on an
artificial neural network capable of identifying novel, previously
unseen areas of geological or astrobiological scenery.
Title: EuroGeoMars Field Campaign: Sample Analysis of Organic Matter
and Minerals
Authors: Ehrenfreund, P.; Foing, B. H.; Stoker, C.; Zavaleta,
J.; Quinn, R.; Blake, D.; Martins, Z.; Sephton, M.; Becker, L.;
Orzechowska, G.; van Sluis, C.; Boche-Sauvan, L.; Gross, C.; Thiel,
C.; Wendt, L.; Sarrazin, P.; Mahapatra, P.; Direito, S.; Roling, W.;
Eurogeomars Mdrs Team
Bibcode: 2010LPI....41.1723E
Altcode:
We report on the results of chemical, physical and astrobiological
measurements of samples collected during the EuroGeoMars campaign
at Utah Mars Desert Research Station (MDRS) in February 2009, as
interdisciplinary preparation for a strategic search for life on Mars.
Title: ILEWG ExoHab & EuroGeoMars Campaigns: Habitability &
Human Operations
Authors: Boche-Sauvan, L.; Foing, B. H.; Stoker, C.; Ehrenfreund, P.;
Wendt, L.; Gross, C.; Thiel, C.; Peters, S.; Borst, A.; Zavaleta,
J.; Sarrazin, P.; Blake, D.; Page, J.; Pletser, V.; Monaghan, E.;
Mahapatra, P.; Noroozi, A.; Giannopoulos, P.; Calzada, A.; Walker,
R.; Zegers, T.; Exogeolab; ILEWG Exohab Team; Eurogeomars Team
Bibcode: 2010LPI....41.1759B
Altcode:
We studied concepts for a minimal Moon-Mars habitat, focussing on
the system aspects and as an evolving architecture. We validated
experimentally the Habitat and Laboratory ExoHab concept constraints
during EuroGeoMars campaign in Utah desert research station.
Title: CAREX Rio Tinto Field Workshop: Instruments, Sample Collection
and Analysis
Authors: Mahapatra, P.; Foing, B.; Direito, S.; Gomez, F.; Rull, F.
Bibcode: 2010LPI....41.1374M
Altcode:
At Rio Tinto, a Mars analogue site, Raman and fibre-optic spectrometers
were successfully used to select appropriate rock and soil samples,
and detect minerals for which it is interesting to study the associated
microorganisms for innovative molecular biology techniques.
Title: Drilling on the Moon and Mars: Developing the Science Approach
for Subsurface Exploration with Human Crews
Authors: Stoker, C. R.; Zavaleta, J.; Bell, M.; Direto, S.; Foing,
B.; Blake, D.; Kim, S.
Bibcode: 2010LPI....41.2697S
Altcode:
The paper describes first results from DOMEX, an analog mission
to develop the approach for using human crews to perform science
activities on the Moon and Mars involving exploration and sampling of
the subsurface.
Title: Kombucha might be promising probiotics for consumption on
the Moon
Authors: Kozyrovska, Natalia; Foing, Bernard H.
Bibcode: 2010cosp...38..434K
Altcode: 2010cosp.meet..434K
The sanitization at permanently manned lunar bases and consuming
germ-free food in a concert with effect of lunar stressors may result
in crews disorders, including inflammatory and atopic states and
decrease of resistance to indigenous pathogens which present in human
organism in suppressed state. The administration of live microbial
supplements with presumptive health benefits on human physiology might
be reasonable solution to prevent disbacteriosis. Many of microbial
species are associated with the fermentation of dairy products,
however, they have a short self-life and so far unpractical to be used
at lunar habitation. The popular "Tea mushroom" or "Kombucha Tea" is
a probiotics proven by FDA that many people are now taking in health
promoting diets to detoxify and revitalize the organism (Danielian,
1993; Sreeramulu et al., 2001). Kombucha is composed by symbiotic
bacteria and yeasts, surrounded by a permeable membrane. The Kombucha
culture is a tiny biochemical factory, producing organic acids, amino
acids, enzymes, polyphenols, antibiotic substances, vitamins, enzymes
as well as some other products beneficial for human health. Within
the ages the Kombucha Tea has been consumed by practically all
nations in Far East and now in Eastern Europe and America due to
probiotic properties, and within this period the Kombucha microbial
ecosystem has been selected to be remarkably adaptive to culturing
conditions and resistant to adverse factors. Metagenomic approaches
in a study of microbial ecosystems will allow to reconstruct the
Kombucha microbiome and to elucidate unknown species and genes on
the base of bioinformatics programs. Compared with Kombucha wild
type, metabolically engineered strains, expected to exhibit broader
substrate specificity, utilizing sugars from waste material which will
be used for Kombucha fermentation. References 1. Danielian L.T. (1993)
Tea fungus. Publ. House "Armenia", 112 pp. 2. Palmer C., Bik E.M.,
DiGiulio D.B., Relman D.A., Brown P.O. (2007) Development of the Human
Infant Intestinal Microbiota. PLoS Biol 5(7): e177. 3. Sreeramulu G.,
Zhu Y., Knol W. (2001) Characterization of antimicrobial activity
in Kom-bucha fermentation. Acta Biotechnol. 21:49-56. 4. Versalovic
J., Relman R. (2006) How bacterial communities expand functional
repertoires. PLoS Biol 4(12): e430.
Title: The inducible CAM plants in putative lunar lander experiments
Authors: Burlak, Olexii; Zaetz, Iryna; Soldatkin, Olexii; Rogutskyy,
Ivan; Danilchenko, Boris; Mikheev, Olexander; de Vera, Jean-Pierre;
Vidmachenko, Anatolii; Foing, Bernard H.; Kozyrovska, Natalia
Bibcode: 2010cosp...38..442B
Altcode: 2010cosp.meet..442B
Precursory lunar lander experiments on growing plants in locker-based
chambers will increase our understanding of effect of lunar
conditions on plant physiology. The inducible CAM (Cras-sulacean Acid
Metabolism)-plants are reasonable model for a study of relationships
between environmental challenges and changes in plant/bacteria gene
expression. In inducible CAM-plants the enzymatic machinery for the
environmentally activated CAM switches on from a C3-to a full-CAM mode
of photosynthesis in response to any stresses (Winter et al., 2008). In
our study, Kalanchoe spp. are shown to be promising candidates for
putative lunar experiments as resistant to irradiation and desiccation,
especially after inoculation with a bacterial consortium (Boorlak
et al., 2010). Within frames of the experiment we expect to get
information about the functional activity of CAM-plants, in particular,
its organogenesis, photosystem, the circadian regulation of plant
metabolism on the base of data gaining with instrumental indications
from expression of the reporter genes fused to any genes involved in
vital functions of the plant (Kozyrovska et al., 2009). References
1. Winter K., Garcia M., Holtum J. (2008) J. Exp. Bot. 59(7):1829-1840
2. Bourlak O., Lar O., Rogutskyy I., Mikheev A., Zaets I., Chervatyuk
N., de Vera J.-P., Danilchenko A.B. Foing B.H., zyrovska N. (2010)
Space Sci. Technol. 3. Kozyrovska N.O., Vidmachenko A.P., Foing B.H. et
al. Exploration/call/estec/ESA. 2009.
Title: Moon-Mars Analogue Mission (EuroMoonMars 1 at the Mars Desert
Research Station)
Authors: Lia Schlacht, Irene; Voute, Sara; Irwin, Stacy; Foing,
Bernard H.; Stoker, Carol R.; Westenberg, Artemis
Bibcode: 2010cosp...38..475L
Altcode: 2010cosp.meet..475L
The Mars Desert Research Station (MDRS) is situated in an analogue
habitat-based Martian environment, designed for missions to determine
the knowledge and equipment necessary for successful future planetary
exploration. For this purpose, a crew of six people worked and lived
together in a closed-system environment. They performed habitability
experiments within the dwelling and conducted Extra-Vehicular Activities
(EVAs) for two weeks (20 Feb to 6 Mar 2010) and were guided externally
by mission support, called "Earth" within the simulation. Crew 91,
an international, mixed-gender, and multidisciplinary group, has
completed several studies during the first mission of the EuroMoonMars
campaign. The crew is composed of an Italian designer and human
factors specialist, a Dutch geologist, an American physicist, and
three French aerospace engineering students from Ecole de l'Air,
all with ages between 21 and 31. Each crewmember worked on personal
research and fulfilled a unique role within the group: commander,
executive officer, engineer, health and safety officer, scientist,
and journalist. The expedition focused on human factors, performance,
communication, health and safety pro-tocols, and EVA procedures. The
engineers' projects aimed to improve rover manoeuvrability, far-field
communication, and data exchanges between the base and the rover or
astronaut. The crew physicist evaluated dust control methods inside and
outside the habitat. The geologist tested planetary geological sampling
procedures. The crew designer investigated performance and overall
habitability in the context of the Mars Habitability Experiment from
the Extreme-Design group. During the mission the crew also participated
in the Food Study and in the Ethospace study, managed by external
groups. The poster will present crew dynamics, scientific results
and daily schedule from a Human Factors perspective. Main co-sponsors
and collaborators: ILEWG, ESA ESTEC, NASA Ames, Ecole de l'Air, SKOR,
Extreme-Design, Universit` di Torino, MMS TU-Berlin, Space Florida,
DAAD, Uni-a versity of Utrecht, The Mars Society.
Title: From Apollo Traverses to Future Exploration
Authors: Calzada, Mss Abigail; Voute, Sara; van Vynckt, Delphine;
Foing, Bernard H.
Bibcode: 2010cosp...38..443C
Altcode: 2010cosp.meet..443C
Historically, Apollo program is known as the first time that human
could land in other space object, in this case Earth's moon, and come
back safely to the Earth. It was the first time that humans had to
adapt geological field work to extreme conditions in space. We can
summarize the field work in a few steps: -Planning of the mission
and field training of the astronauts. -Development of instrumental
packages and reconnaissance of the area. -Geophysical measure-ments
in situ and some sampling near the Lunar Module (LM). -Various EVA's
of an average of six hours, from Apollo 15 with Lunar Rover Vehicle
(LRV) support, collecting samples and taking measurements of various
geophysical experiments. From now to future exploration we have to
focus on apply all the knowledge we have from Apollo traverses and
adapt it to the new technologies we are developing. The use of robotic
rovers can save us hours of human EVA's in the way that we can predict
the possible sites of interest before send human there. Also, the
development of a field laboratory and habitat can provide us of the
intruments necessary to do experiments without the need of a sample
return mission. We validate these traverses in EuroMoonMars campaign.
Title: The Cyborg Astrobiologist: testing a novelty detection
algorithm on two mobile exploration systems at Rivas Vaciamadrid in
Spain and at the Mars Desert Research Station in Utah
Authors: McGuire, P. C.; Gross, C.; Wendt, L.; Bonnici, A.;
Souza-Egipsy, V.; Ormö, J.; Díaz-Martínez, E.; Foing, B. H.; Bose,
R.; Walter, S.; Oesker, M.; Ontrup, J.; Haschke, R.; Ritter, H.
Bibcode: 2010IJAsB...9...11M
Altcode: 2009arXiv0910.5454M
In previous work, a platform was developed for testing computer-vision
algorithms for robotic planetary exploration. This platform consisted
of a digital video camera connected to a wearable computer for real-time
processing of images at geological and astrobiological field sites. The
real-time processing included image segmentation and the generation of
interest points based upon uncommonness in the segmentation maps. Also
in previous work, this platform for testing computer-vision algorithms
has been ported to a more ergonomic alternative platform, consisting of
a phone camera connected via the Global System for Mobile Communications
(GSM) network to a remote-server computer. The wearable-computer
platform has been tested at geological and astrobiological field sites
in Spain (Rivas Vaciamadrid and Riba de Santiuste), and the phone
camera has been tested at a geological field site in Malta. In this
work, we (i) apply a Hopfield neural-network algorithm for novelty
detection based upon colour, (ii) integrate a field-capable digital
microscope on the wearable computer platform, (iii) test this novelty
detection with the digital microscope at Rivas Vaciamadrid, (iv) develop
a Bluetooth communication mode for the phone-camera platform, in order
to allow access to a mobile processing computer at the field sites, and
(v) test the novelty detection on the Bluetooth-enabled phone camera
connected to a netbook computer at the Mars Desert Research Station in
Utah. This systems engineering and field testing have together allowed
us to develop a real-time computer-vision system that is capable, for
example, of identifying lichens as novel within a series of images
acquired in semi-arid desert environments. We acquired sequences of
images of geologic outcrops in Utah and Spain consisting of various
rock types and colours to test this algorithm. The algorithm robustly
recognized previously observed units by their colour, while requiring
only a single image or a few images to learn colours as familiar,
demonstrating its fast learning capability.
Title: SMART-1 recent results and lessons for future exploration
Authors: Foing, Bernard H.
Bibcode: 2010cosp...38..417F
Altcode: 2010cosp.meet..417F
We present recent results from SMART-1 ESA mission to the Moon published
or obtained since last COSPAR. We discuss the technology demonstration,
science and exploration results, and lessons learned for the future. We
describe SMART-1 lunar science investigations including studies of the
chemical composition of the Moon, of geophysical processes (volcanism,
tectonics, cratering, soil roughness from multi-angular photometry )
for comparative planetology. We also show high resolution studies
of recent impact sites (Kaguya, LCROSS), and of polar regions in
preparation for future exploration.
Title: Investigation of microbial diversity in a desert Mars-like
environment: Mars Desert Research Station (MDRS), Utah
Authors: Direito, Maria Susana; Staats, Martijn; Foing, Bernard H.;
Ehrenfreund, Pascale; Roling, Wilfred
Bibcode: 2010cosp...38.3327D
Altcode: 2010cosp.meet.3327D
The Utah Mars Desert Research Station (MDRS) harbours geo-morphology and
geo-processes analogues to the planet Mars. Soil samples were collected
during the EuroGeoMars campaign (from 24 January to 1 March 2009)
from different locations and depths [1]. Samples were distributed among
scientific collaborator institutes for analysis of microbial diversity,
amino acid content and degradation, content of PAH or larger organic
molecules, and respective soil properties. Our sample analysis had
the objective of characterizing the microbial communities in this Mars
analogue: DNA isolation, PCR (Polymerase Chain Reaction) using primers
for DNA amplification of Bacteria, Archaea and Eukarya ribosomal RNA
(rRNA) gene fragments, DGGE (Denaturing Gradient Gel Electrophoresis)
and clone library construction with the final aim of sequencing. Results
indicate that life is present in all the three domains of life (Archaea,
Bacteria and Eukarya), while the most diversity was found in the
domain Bacteria. Microorgan-isms are heterogeneously present and their
identities are currently investigated. The obtained information will
be later related to the other scientific analysis in order to obtain
a better understanding of this Mars analogue site, which in turn will
provide important information for the search for life on Mars. [1]
Foing, B.H. et al . (2009). Exogeolab lander/rover instruments and
EuroGeoMars MDRS campaign. LPI, 40, 2567.
Title: 3min. poster presentations of B01
Authors: Foing, Bernard H.
Bibcode: 2010cosp...38..433F
Altcode: 2010cosp.meet..433F
We give a report on recommendations from ILEWG International conferences
held at Cape Canaveral in 2008 (ICEUM10), and in Beijing in May 2010
with IAF (GLUC -ICEUM11). We discuss the different rationale for
Moon exploration. Priorities for scientific investigations include:
clues on the formation and evolution of rocky planets, accretion
and bombardment in the inner solar system, comparative planetology
processes (tectonic, volcanic, impact cratering, volatile delivery),
historical records, astrobiology, survival of organics; past, present
and future life. The ILEWG technology task group set priorities for
the advancement of instrumenta-tion: Remote sensing miniaturised
instruments; Surface geophysical and geochemistry package; Instrument
deployment and robotic arm, nano-rover, sampling, drilling; Sample
finder and collector. Regional mobility rover; Autonomy and Navigation;
Artificially intelligent robots, Complex systems. The ILEWG ExogeoLab
pilot project was developed as support for instru-ments, landers,
rovers,and preparation for cooperative robotic village. The ILEWG
lunar base task group looked at minimal design concepts, technologies
in robotic and human exploration with Tele control, telepresence,
virtual reality; Man-Machine interface and performances. The ILEWG
ExoHab pilot project has been started with support from agencies
and partners. We discuss ILEWG terrestrial Moon-Mars campaigns for
validation of technologies, research and human operations. We indicate
how Moon-Mars Exploration can inspire solutions to global Earth
sustained development: In-Situ Utilisation of resources; Establishment
of permanent robotic infrastructures, Environmental protection aspects;
Life sciences laboratories; Support to human exploration. Co-Authors:
ILEWG Task Groups on: Science, Technology, Robotic village, Lunar
Bases , Commercial and Societal aspects, Roadmap synergies with other
programmes, Public en-gagemnet and Outreach, Young Lunar Explorers.
Title: Outreach and education from EuroGeoMoonMars2009 Field Campaign
in Utah
Authors: Foing, Bernard H.
Bibcode: 2010cosp...38.3893F
Altcode: 2010cosp.meet.3893F
The goal of the EuroGeoMoonMars mission at Utah Desert Research
station(from 24 January to 28 February 2009) was to demonstrate
instruments from ExoGeoLab pilot project, to support the interpretation
of ongoing lunar and planetary missions, to validate a procedure for
surface in-situ and return science, to study human performance aspects,
and perform outreach and education projects. The EuroGeoMoonMars
campaign included four sets of objectives: 1) Technology demonstration
aspects: a set of instruments were deployed, tested, assessed,
and training was provided to scientists using them in subsequent
rotations 2) Research aspects: a series of field science and
exploration investigations were conducted in geology, geochemistry,
biology, astronomy, with synergies with space missions and research
from planetary surfaces and Earth extreme environments. 3) Human crew
related aspects, i.e. (a) evaluation of the different functions and
interfaces of a planetary habitat, (b) crew time organization in
this habitat, (c) evaluation of man-machine interfaces of science
and technical equipment; 4) Education, outreach, communications,
multi-cultural public relations Outreach, education and inspiration:
We produced written, pictures, and video materials that can be used
for education, outreach and public relations. Daily reports were posted
on the MDRS website. We had during the Technical crew preparation, the
visit of film producer Mark Arabella and film crew for a Moon related
National Geographics documentary "Earth without the Moon". Two media
crew visitors stayed also in the Hab to film our activities documenting
the operational, research, human, simulation, imaginative and fantasy
aspects of Moon-Mars-extreme Earth exploration. They contributed
a journalist report, and even performed an EVA outreach filming a
sortie to Hanksville village on Earth. Other film and journalists
visited the EuroGeoMars crew for interviews and exchange. Specific
crew reports were also prepared for some national and international
communication channels, including Plan`te Mars, RTBF, ILEWG, COSPAR,
IAF, IAA. We thank ILEWG, NASA Ames, ESA, the Mars society, VU Amsterdam
and collaborating institutes for supporting the campaign.
Title: EuroGeoMars Field Campaign: habitability studies in preparation
for future Mars missions
Authors: Ehrenfreund, Pascale; Foing, B. H.; Stoker, C.; Zhavaleta,
J.; Orzechowska, G.; Kotler, M.; Martins, Z.; Sephton, M.; Becker,
L.; Quinn, R.; van Sluis, C.; Boche-Sauvan, L.; Gross, C.; Thiel,
C.; Wendt, L.; Sarrazin, P.; Mahapatra, P.; Direito, S.; Roling, W.
Bibcode: 2010cosp...38.3299E
Altcode: 2010cosp.meet.3299E
The goal of the EuroGeoMars field campaign sponsored by ESA,
NASA and the international lunar exploration working group (ILEWG)
was to demonstrate instrument capabilities in sup-port of current
and future planetary missions, to validate a procedure for Martian
surface in-situ and return science, and to study human performance
aspects. The Mars Desert Re-search Station (MDRS) represents an ideal
basis to simulate aspects of robotic and human exploration in support
of future missions to planetary bodies. During the campaign, MDRS
Crew 77 tested X-ray diffraction and Raman instruments, and assessed
habitat and operations. Special emphasis was given to sample collection
in the geologically rich vicinity of MDRS and subsequent analysis of
organic molecules in the soil to simulate the search for bio-signatures
with field instrumentation. We describe the results of in-situ and
posterior analysis of the physical and chemical properties including
elemental composition, salt concentrations as well as carbon and amino
acid abundances. The analyses of organics and minerals show that the
subsurface mineral matrix represents a key to our understanding of
the survival of organics on Mars.
Title: EuroMoonMars Dommex (EMMD 2010): Geology results from EMMD3
in a desert Mars-like environment, Utah
Authors: van Vynckt, Delphine; Voute, Sara; Calzada, Mss Abigail;
Le Maire, Victor; Jago, Alban; de Crombrugghe, Guerric; Denies,
Jonathan; Reydam, Marc; van Vynckt, D.; Voute, Sara; Calzada, Abigail;
de Crombrugghe, G.; Denies, J.; Jago, A.; Le Maire, V.; de Lobkowicz,
I.; Mertens, A.; Reydams, M.; Foing, Bernard H.; Stoker, C.
Bibcode: 2010cosp...38..537V
Altcode: 2010cosp.meet..537V
EMMD3 Geology results : Delphine Van Vynckt Introduction: EMMD3 is
part of the JUMP Martian mission simulation conducted by stu-dents
in the Mars Desert Research Station (MDRS), a habitat installed by
the Mars Society (MS) in the Utah desert. The campaign was supported
by ILEWG International Lunar Explo-ration Working Group, ESTEC,
NASA Ames, and partners. The geology objectives of EMMD 2010 are to
study the surface and subsurface of the Jurassic-Cretaceous Earth
in Utah, to mea-sure mineral composition and to analyse the various
rocks after a sampling in EVA suit. The geological EMMD3 research is
divided in three main parts. The first one consists of developing a
sampling procedure for Martian missions; the second one concerns the
exact determination of the durations of the different steps of this
sampling procedure; the last one will study the possi-bility to work
with a rover, and the interactions human-machine. The project is in
line with the ILEWG EuroMoonMars project which coordinates several
MDRS missions, and contributes to the preparation of future Mars
sample return missions. Procedure validation: During a previous
crew rotation at the MDRS, Sara Voute (EDMM1) will finalize and
test a procedure she developed for geological missions. During our
crew rotation we will test the sampling part of that procedure into
more details. One of the objectives is to determine whether it is
understandable and usable for astronauts that are not specialized
in geology. Rover monitoring: A rover will be lent by NASA Ames to
our crew. We will study the different ways to work with such tool
in geological missions. The rover can be used as a technical support
for astronauts in outside missions. The astronauts could communicate
information (images, spectrometer scans, etc.) to the base through
the rover in order to sample efficiently. The scientists located in
the base have access to treatment tools that an astronauts in outside
mission have not and so this allows a pre-selection of the sampling
carried back. We will study also the interaction rover-astronauts in
a general way in order to determine the benefits both for the rover
and the astronauts. Moreover, we will perform exploration missions
with rover monitored remotely from the base and see the limitations of
this approach. We shall report on the science and technical results,
and implications for Earth-Mars compar-ative studies.
Title: Search for Mars climatic signal in periglacial deposits
Authors: Foing, Bernard H.
Bibcode: 2010cosp...38..503F
Altcode: 2010cosp.meet..503F
Mars has experienced large variations in its orbital parameters
throughout its history, with periodicity of 120 000 years for its
obliquity, 95 to 100,000 years for its eccentricity, and 51,000 years
for its precession (Laskar et al) . At high obliquity, signicant amount
of ice can be deposited from snow at low latitudes. This can be relevant
for understanding features from the modern Polar Layered Deposits, the
Elysium frozen sea (Murray et al 2005), or Ellas hourglass (Head et al
2005). General circulation models predict an annual net accumulation
rate of ice on the west of Tharsis volcanoes. We analysed Mars Express
images on Pavonis Mons and other periglacial deposits . By texture
analysis we could distinguish ridges, knobbies from various episodes
and relate them with geological studies. Using a glacier progression
model under different snow fall conditions according to obliquity, we
find oscillations of the glacier extents and ridges that can constrain
the past history of Martian climate. We acknowledge discussions with
A. Orsi, T. Zegers, F. Forget, J. Head, J. Laskar, S. van Gasselt,
G. Neukum Mars Express HRSC team
Title: Reflections and proposals on robotic and human exploration
of Moon; Mars, and near-Earth asteroids
Authors: Ehrenfreund, Pascale; Zarnecki, John; Mc Kay, Chris; Foing,
Bernard; Peter, Nicolas; Rummel, John; Masson-Zwaan, Tanja; Perino,
Maria A.; Macwell, Steve; Worms, Jean Claude; Billings, Linda
Bibcode: 2010cosp...38.3969E
Altcode: 2010cosp.meet.3969E
The objective of the COSPAR Panel on Exploration (PEX) is to provide the
best, independent, input to support the development of worldwide space
exploration programs and to safeguard the scientific assets of solar
system objects. In recent years, there has been ample study activity
concerning space exploration and overall international cooperation
has increased strongly. For lunar exploration, the International Lunar
Exploration Working Group (ILEWG) and the Lu-nar Exploration Analysis
Group (LEAG)—as well as other committees—represent important foci
for an even broader base of expertise. The Mars Exploration Planning
and Analysis Group (MEPAG) continues to be an excellent community
forum providing analysis for NASA and international Mars programs
represented cross-agency by the International Mars Exploration
Working Group (IMEWG). The PEX report 2010 provides a summary and
outlines synergies of existing documents and roadmaps of each of these
bodies. Additonal expertise is provided via the contacts maintained
by COSPAR's various Associates within the international community and
scientific entities. PEX also offers a stepwise approach to foster a
future international plan-etary exploration program, a system-of-systems
approach with small exploration missions that serves as preparation
for future large-scale endeavors. The PEX document is aimed to foster
transnational alliances, support joint research and educate and inspire
a new space generation.
Title: Protecting the Moon for research: ILEWG report
Authors: Foing, Bernard H.
Bibcode: 2010cosp...38.3956F
Altcode: 2010cosp.meet.3956F
We give a report on recommendations with emphasis on environment
protection, and since last COSPAR from ILEWG International conferences
Exploration and Utilisation of the Moon on held at Cape Canaveral
in 2008 (ICEUM10), and in Beijing in May 2010 with IAF (GLUC
-ICEUM11). We discuss the different rationale for Moon exploration,
as debated at ILEWG. ILEWG Science task group has listed priorities
for scientific investigations: clues on the formation and evolution
of rocky planets, accretion and bombardment in the inner solar system,
comparative planetology processes (tectonic, volcanic, impact cratering,
volatile delivery), records astrobiology, survival of organics; past,
present and future life; sciences from a biology lunar laboratory. We
discuss how to preserve Moon research potential in these areas while
operating with instruments, landers, rover during a cooperative robotic
village, and during the transition form lunar human outpost to permanent
sustainable human base. We discuss how Moon-Mars Exploration can inspire
solutions to global Earth sustained development with the trade-off of
In-Situ Utilisation of resources; Establishment of permanent robotic
infrastructures, Environmental and planetary protection aspects and
lessons for Mars; Life sciences laboratories, and support to human
exploration. Co-authors: ILEWG Task Groups on Science, Technology and
Human Lunar Bases ILEWG Reference documents: http://sci.esa.int/ilewg
-10th ILEWG Conference on Exploration and Utilisation of the Moon,
NASA Lunar Ex-ploration Analysis Group-PSace Resources Roundtable, Cape
Canaveral October 2008, pro-gramme online at http://sci.esa.int/ilewg/
-9th ILEWG Conference on Exploration and Utilisation of the Moon,
ICEUM9 Sorrento 2007, programme online at http://sci.esa.int/ilewg/
-8th ILEWG Conference on Exploration and Utilisation of the Moon,
Beijing July 2006, programme online at http://sci.esa.int/ilewg/ -The
Moon and Near Earth Objects (P. Ehrenfreund , B.H. Foing, A. Cellino
Editors), Ad-vances in Space Research, Volume 37, Issue 1, pp 1-192,
2006 -7th ILEWG Conference on Exploration and Utilisation of the Moon,
Toronto Sept 2005, Programme and Proceedings on line at www.ilewg.org,
R. Richards et al Editors -6th ILEWG Conference on Exploration and
Utilisation of the Moon, Udaipur Nov. 2004, Proceedings ( N. Bhandari
Editor), Journal Earth System Science, India, 114, No6, Dec 2005,
pp. 573-841 -5th ILEWG Conference on Exploration and Utilisation of the
Moon, Hawaii Nov 2003, Pro-ceedings ILC2005/ICEUM5 (S.M. Durst et al
Editors), Vol 108, 1-576 pp, Science and Tech-nology Series, American
Astronautical Society, 2004 -'The next steps in exploring deep space
-A cosmic study by the IAA', W. Huntress, D. Stetson, R. Farquhar,
J. Zimmerman, B. Clark, W. O'Neil, R. Bourke and B. Foing, Acta
Astronautica, Vol 58, Issues 6-7, March-April 2006, p302-377 -IAA/ESA
workshop on "Next Steps in Exploring Deep Space", ESTEC 22-23 sept. 2003
(B.H. Foing W. Huntress, conveners) Lunar Exploration, Planetary
and Space Science, Vol 50, issue 14-15, Dec 2002 (B.H. Foing al)
-ESLAB36 symposium on "Earth-like Planets and Moons", 2002, ESA-SP514,
pp. 1-356, (B.H.Foing B. Battrick, editors) -'Lunar Exploration 2000',
(B.H. Foing, D. Heather, Editors), Adv. Space Research Vol 30, Nr 8,
2002 -'Earth-Moon Relationships', Proceedings of the Conference held
in Padova, Italy at the Ac-cademia Galileiana di Scienze Lettere ed
Arti, Nov. 2000, (C. Barbieri and F. Rampazzi, Editors), in Earth,
Moon , Planets Vol. 85-86, Nos 1-3, pp 1-575, 2001 -4th International
Conference on Exploration and Utilisation of the Moon, ESTEC, 2000,
ESA SP-462 (B.H. Foing M. Perry, editors) -Investing in Space: The
Challenge for Europe. Long-Term Space Policy Committee, Second Report,
May 1999. ESA-SP-2000 -2nd International Lunar Workshop, held at Kyoto
in October 1996, Proceedings, H. Mizutani, editor, Japan Space Forum
Publisher, 1997 International Lunar Workshop, 1994 May 31-June 3,
Beatenberg, Switzerland. Proceedings. Ed. Balsiger, H. et al. European
Space Agency, 1994. ESA-SP-1170 -Astronomy and Space Science from the
Moon', Proceedings of COSPAR/IAF session at World Congress, Washington,
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Space Agency, ESA SP-1150, June 1992
Title: Automatic rock detection for in situ spectroscopy applications
on Mars
Authors: Mahapatra, Pooja; Foing, Bernard H.
Bibcode: 2010cosp...38.3504M
Altcode: 2010cosp.meet.3504M
A novel algorithm for rock detection has been developed for effectively
utilising Mars rovers, and enabling autonomous selection of target
rocks that require close-contact spectroscopic measurements. The
algorithm demarcates small rocks in terrain images as seen by cameras
on a Mars rover during traverse. This information may be used by
the rover for selection of geologically relevant sample rocks, and
(in conjunction with a rangefinder) to pick up target samples using
a robotic arm for automatic in situ determination of rock composition
and mineralogy using, for example, a Raman spectrometer. Determining
rock samples within the region that are of specific interest without
physically approaching them significantly reduces time, power and
risk. Input images in colour are converted to greyscale for intensity
analysis. Bilateral filtering is used for texture removal while
preserving rock boundaries. Unsharp masking is used for contrast
enhance-ment. Sharp contrasts in intensities are detected using Canny
edge detection, with thresholds that are calculated from the image
obtained after contrast-limited adaptive histogram equalisation of the
unsharp masked image. Scale-space representations are then generated by
convolving this image with a Gaussian kernel. A scale-invariant blob
detector (Laplacian of the Gaussian, LoG) detects blobs independently
of their sizes, and therefore requires a multi-scale approach with
automatic scale se-lection. The scale-space blob detector consists of
convolution of the Canny edge-detected image with a scale-normalised
LoG at several scales, and finding the maxima of squared LoG response
in scale-space. After the extraction of local intensity extrema,
the intensity profiles along rays going out of the local extremum
are investigated. An ellipse is fitted to the region determined by
significant changes in the intensity profiles. The fitted ellipses are
overlaid on the original Mars terrain image for a visual estimation
of the rock detection accuracy, and the number of ellipses are
counted. Since geometry and illumination have the least effect on small
rocks, the proposed algorithm is effective in detecting small rocks
(or bigger rocks at larger distances from the camera) that consist of
a small fraction of image pixels. Acknowledgements: The first author
would like to express her gratitude to the European Space Agency
(ESA/ESTEC) and the International Lunar Exploration Working Group
(ILEWG) for their support of this work.
Title: A dual bacterial culture augments Kalanchoe spp. photosynthesis
under extreme conditions
Authors: Burlak, Olexii; Rogutskyy, Ivan; Danilchenko, Boris; Mikheev,
Olexander; Zaetz, Iryna; Lorek, Andreas; Koncz, Alexander; de Vera,
Jean-Pierre; Foing, Bernard H.; Kozyrovska, Natalia
Bibcode: 2010cosp...38.3470B
Altcode: 2010cosp.meet.3470B
In consistence with conception of using microbial technology for plant
growing/protosoil for-mation for Lunar/Martian greenhouses (Kozyrovska
et al., 2004-2010), we anticipate microbes to alleviate impact of the
environmental stressors on plant development. Bacteria can augment
physiological processes in plants, for example, photosynthesis, by
regulating a hormone level and decreasing glucose sensing in planta
(Zhang et al., 2008). The study aimed to examine impact of consortium
of well-defined bacteria Klebsiella oxytoca IMBG26 and Paenibacillus
sp. IMBG150 on the CAM-plantlets Kalanhoe diagramontiana and Kalanhoe
tubiflora pho-tosynthetic activity after acute action of gamma radiation
(60Co), Near Martian ultraviolet radiation, low pressure (100 mbar), and
high concentrations of CO2 (95Plantlets of K. tubi-flora were exposed to
harmful doses of Near Martian UV radiation for 3 hours (26.53 J/cm2). A
week before experiment kalanchoe plantlets were subjected to acute
effects of ionizing radiation at doses of 30 and 70 Gy. In noninoculated
plantlets after 30 Gy the photosynthetic activity fell to 71
Title: Challenges from new lunar data: ILEWG report
Authors: Foing, Bernard H.
Bibcode: 2010cosp...38..812F
Altcode: 2010cosp.meet..812F
Recent lunar missions including Clementine, Lunar Prospector,
SMART-1, Selene Kaguya, Chang'E 1 , Chandrayaan-1 have been producing
new data in large volumes. We shall discuss the challenges in data
calibration and intercalibration, integration, the defin ition of an
accurate coordinate systems and geodesic grid, incorporation of latest
altimetry and gravimetry data. LRO Lunar Reconnaissance Orbiter and
subsequent missions will go even futher in data volume and diversity of
instruments. We shall discuss the upcoming challenges in data archiving,
management and interpretative tools, to merge orbital remote sensing
with surface data from landers and rovers for the various elements
of ILEWG lunar robotic village. Co-authors: ILEWG Task Groups on
Science, Data and Outreach Relevant ILEWG Reference documents:
http://sci.esa.int/ilewg -10th ILEWG Conference on Exploration and
Utilisation of the Moon, NASA Lunar Ex-ploration Analysis Group-Space
Resources Roundtable, Cape Canaveral October 2008, pro-gramme online
at http://sci.esa.int/ilewg/ -9th ILEWG Conference on Exploration
and Utilisation of the Moon, ICEUM9 Sorrento 2007, programme online
at http://sci.esa.int/ilewg/ -8th ILEWG Conference on Exploration
and Utilisation of the Moon, Beijing July 2006, programme online
at http://sci.esa.int/ilewg/ -7th ILEWG Conference on Exploration
and Utilisation of the Moon, Toronto Sept 2005, Programme and
Proceedings on line at www.ilewg.org, R. Richards et al Editors
-6th ILEWG Conference on Exploration and Utilisation of the Moon,
Udaipur Nov. 2004, Proceedings ( N. Bhandari Editor), Journal Earth
System Science, India, 114, No6, Dec 2005, pp. 573-841 -5th ILEWG
Conference on Exploration and Utilisation of the Moon, Hawaii Nov 2003,
Pro-ceedings ILC2005/ICEUM5 (S.M. Durst et al Editors), Vol 108, 1-576
pp, Science and Tech-nology Series, American Astronautical Society,
2004 -4th International Conference on Exploration and Utilisation of
the Moon, ESTEC, 2000, ESA SP-462 (B.H. Foing M. Perry, editors)
Title: Photospheric activity and rotation of the planet-hosting
star CoRoT-4a
Authors: Lanza, A. F.; Aigrain, S.; Messina, S.; Leto, G.; Pagano,
I.; Auvergne, M.; Baglin, A.; Barge, P.; Bonomo, A. S.; Collier
Cameron, A.; Cutispoto, G.; Deleuil, M.; de Medeiros, J. R.; Foing,
B.; Moutou, C.
Bibcode: 2009A&A...506..255L
Altcode: 2009arXiv0901.4618L
Aims: The space experiment CoRoT has recently detected a transiting hot
Jupiter in orbit around a moderately active F-type main-sequence star
(CoRoT-4a). This planetary system is of particular interest because
it has an orbital period of 9.202 days, the second longest one among
the transiting planets known to date. We study the surface rotation
and the activity of the host star during an uninterrupted sequence of
optical observations of 58 days.
Methods: Our approach is based
on a maximum entropy spot modelling technique extensively tested
by modelling the variation in the total solar irradiance. It has
been successfully applied to model the light curve of another active
star with a transiting planet observed by CoRoT, i.e., CoRoT-2a. It
assumes that stellar active regions consist of cool spots and bright
faculae, analogous to sunspots and solar photospheric faculae,
whose visibility is modulated by stellar rotation.
Results:
The modelling of the light curve of CoRoT-4a reveals three main active
longitudes with lifetimes between {∼ }30 and {∼ }60 days that rotate
quasi-synchronously with the orbital motion of the planet. The different
rotation rates of the active longitudes are interpreted in terms of
surface differential rotation, and a lower limit of 0.057 ± 0.015 is
derived for its relative amplitude. The enhancement of activity observed
close to the subplanetary longitude suggests a magnetic star-planet
interaction, although the short duration of the time series prevents us
from drawing definite conclusions.
Conclusions: The present work
confirms the quasi-synchronicity between stellar rotation and planetary
orbital motion in the CoRoT-4 system and provides a lower limit for
the surface differential rotation of the star. This information can
be important in trying to understand the formation and evolution
of this highly interesting planetary system. Moreover, there is an
indication of a possible star-planet magnetic interaction that needs
to be confirmed by future studies. Based on observations obtained
with CoRoT, a space project operated by the French Space Agency, CNES,
with partecipation of the Science Programme of ESA, ESTEC/RSSD, Austria,
Belgium, Brazil, Germany, and Spain.
Title: Transiting exoplanets from the CoRoT space
mission. VIII. CoRoT-7b: the first super-Earth with measured radius
Authors: Léger, A.; Rouan, D.; Schneider, J.; Barge, P.; Fridlund,
M.; Samuel, B.; Ollivier, M.; Guenther, E.; Deleuil, M.; Deeg, H. J.;
Auvergne, M.; Alonso, R.; Aigrain, S.; Alapini, A.; Almenara, J. M.;
Baglin, A.; Barbieri, M.; Bruntt, H.; Bordé, P.; Bouchy, F.; Cabrera,
J.; Catala, C.; Carone, L.; Carpano, S.; Csizmadia, Sz.; Dvorak,
R.; Erikson, A.; Ferraz-Mello, S.; Foing, B.; Fressin, F.; Gandolfi,
D.; Gillon, M.; Gondoin, Ph.; Grasset, O.; Guillot, T.; Hatzes, A.;
Hébrard, G.; Jorda, L.; Lammer, H.; Llebaria, A.; Loeillet, B.;
Mayor, M.; Mazeh, T.; Moutou, C.; Pätzold, M.; Pont, F.; Queloz, D.;
Rauer, H.; Renner, S.; Samadi, R.; Shporer, A.; Sotin, Ch.; Tingley,
B.; Wuchterl, G.; Adda, M.; Agogu, P.; Appourchaux, T.; Ballans, H.;
Baron, P.; Beaufort, T.; Bellenger, R.; Berlin, R.; Bernardi, P.;
Blouin, D.; Baudin, F.; Bodin, P.; Boisnard, L.; Boit, L.; Bonneau,
F.; Borzeix, S.; Briet, R.; Buey, J. -T.; Butler, B.; Cailleau, D.;
Cautain, R.; Chabaud, P. -Y.; Chaintreuil, S.; Chiavassa, F.; Costes,
V.; Cuna Parrho, V.; de Oliveira Fialho, F.; Decaudin, M.; Defise,
J. -M.; Djalal, S.; Epstein, G.; Exil, G. -E.; Fauré, C.; Fenouillet,
T.; Gaboriaud, A.; Gallic, A.; Gamet, P.; Gavalda, P.; Grolleau, E.;
Gruneisen, R.; Gueguen, L.; Guis, V.; Guivarc'h, V.; Guterman, P.;
Hallouard, D.; Hasiba, J.; Heuripeau, F.; Huntzinger, G.; Hustaix,
H.; Imad, C.; Imbert, C.; Johlander, B.; Jouret, M.; Journoud, P.;
Karioty, F.; Kerjean, L.; Lafaille, V.; Lafond, L.; Lam-Trong, T.;
Landiech, P.; Lapeyrere, V.; Larqué, T.; Laudet, P.; Lautier, N.;
Lecann, H.; Lefevre, L.; Leruyet, B.; Levacher, P.; Magnan, A.; Mazy,
E.; Mertens, F.; Mesnager, J. -M.; Meunier, J. -C.; Michel, J. -P.;
Monjoin, W.; Naudet, D.; Nguyen-Kim, K.; Orcesi, J. -L.; Ottacher,
H.; Perez, R.; Peter, G.; Plasson, P.; Plesseria, J. -Y.; Pontet, B.;
Pradines, A.; Quentin, C.; Reynaud, J. -L.; Rolland, G.; Rollenhagen,
F.; Romagnan, R.; Russ, N.; Schmidt, R.; Schwartz, N.; Sebbag, I.;
Sedes, G.; Smit, H.; Steller, M. B.; Sunter, W.; Surace, C.; Tello,
M.; Tiphène, D.; Toulouse, P.; Ulmer, B.; Vandermarcq, O.; Vergnault,
E.; Vuillemin, A.; Zanatta, P.
Bibcode: 2009A&A...506..287L
Altcode: 2009arXiv0908.0241L
Aims: We report the discovery of very shallow (Δ F/F ≈ 3.4×
10-4), periodic dips in the light curve of an active V =
11.7 G9V star observed by the CoRoT satellite, which we interpret as
caused by a transiting companion. We describe the 3-colour CoRoT
data and complementary ground-based observations that support
the planetary nature of the companion.
Methods: We used
CoRoT colours information, good angular resolution ground-based
photometric observations in- and out- of transit, adaptive optics
imaging, near-infrared spectroscopy, and preliminary results from
radial velocity measurements, to test the diluted eclipsing binary
scenarios. The parameters of the host star were derived from optical
spectra, which were then combined with the CoRoT light curve to derive
parameters of the companion.
Results: We examined all conceivable
cases of false positives carefully, and all the tests support the
planetary hypothesis. Blends with separation >0.40´´or triple
systems are almost excluded with a 8 × 10-4 risk left. We
conclude that, inasmuch we have been exhaustive, we have discovered
a planetary companion, named CoRoT-7b, for which we derive a period
of 0.853 59 ± 3 × 10-5 day and a radius of Rp
= 1.68 ± 0.09 R_Earth. Analysis of preliminary radial velocity data
yields an upper limit of 21 M_Earth for the companion mass, supporting
the finding.
Conclusions: CoRoT-7b is very likely the first
Super-Earth with a measured radius. This object illustrates what will
probably become a common situation with missions such as Kepler, namely
the need to establish the planetary origin of transits in the absence of
a firm radial velocity detection and mass measurement. The composition
of CoRoT-7b remains loosely constrained without a precise mass. A very
high surface temperature on its irradiated face, ≈1800-2600 K at the
substellar point, and a very low one, ≈50 K, on its dark face assuming
no atmosphere, have been derived. The CoRoT space mission,
launched on 27 December 2006, has been developed and is operated by
CNES, with the contribution of Austria, Belgium, Brazil, ESA, Germany,
and Spain. First CoRoT data are available to the public from the
CoRoT archive: http://idoc-corot.ias.u-psud.fr. The complementary
observations were obtained with MegaPrime/MegaCam, a joint project of
CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT) which
is operated by NRC in Canada, INSU-CNRS in France, and the University of
Hawaii; ESO Telescopes at the La Silla and Paranal Observatories under
programme ID 081.C-0413(C), DDT 282.C-5015; the IAC80 telescope operated
by the Instituto de Astrofísica de Tenerife at the Observatorio del
Teide; the Isaac Newton Telescope (INT), operated on the island of
La Palma by the Isaac Newton group in the Spanish Observatorio del
Roque de Los Muchachos of the Instituto de Astrofisica de Canarias;
and at the Anglo-Australian Telescope that have been funded by the
Optical Infrared Coordination network (OPTICON), a major international
collaboration supported by the Research Infrastructures Programme of
the European Commissions Sixth Framework Programme; Radial-velocity
observations were obtained with the SOPHIE spectrograph at the 1.93m
telescope of Observatoire de Haute Provence, France.
Title: Testing the Cyborg Astrobiologist at the Mars Desert Research
Station (MDRS), Utah
Authors: Gross, C.; Wendt, L.; McGuire, P. C.; Bonnici, A.;
Foing, B. H.; Souza-Egipsy, V.; Bose, R.; Walter, S.; Ormö, J.;
Diaz-Martinez, E.
Bibcode: 2009epsc.conf..548G
Altcode:
No abstract at ADS
Title: Synthesis of SMART-1 lunar results
Authors: Foing, B. H.
Bibcode: 2009epsc.conf..654F
Altcode:
No abstract at ADS
Title: Highlights from Remote Controlled Rover for EuroGeoMars
MDRS Campaign
Authors: Hendrikse, J.; Foing, B. H.; Monaghan, E.
Bibcode: 2009epsc.conf..588H
Altcode:
No abstract at ADS
Title: A Prototype Instrumentation System for Rover-Based Planetary
Geology
Authors: Mahapatra, P.; Foing, B.; Nijman, F.; Page, J.; Noroozi, A.
Bibcode: 2009epsc.conf..364M
Altcode:
No abstract at ADS
Title: Validation of Instruments and Robotics from
EuroGeoMars&Moon Campaign
Authors: Foing, B. H.
Bibcode: 2009epsc.conf..643F
Altcode:
No abstract at ADS
Title: Evolution of Organic Matter Studied on EXPOSE-R on the
International Space Station
Authors: Ehrenfreund, P.; Peeters, Z.; Foing, B. H.; Salama, F.;
Jessberger, E.; Robert, F.
Bibcode: 2009OLEB...39....3E
Altcode:
A crucial goal for astrobiology is to understand the evolution and
fate of organic matter in space. Organic chemistry in the universe
seems to follow common pathways: the largest fraction of carbon
in the universe is incorporated into aromatic molecules (polycyclic
aromatic hydrocarbons (PAHs), as well as solid macromolecular aromatic
structures). An opportunity to gain insights into the evolution of
aromatic molecules is provided by the multi-user facility EXPOSE-R
which will be integrated in December 2008 on the International Space
Station (ISS). The Organics experiment will expose specific PAHs
and fullerene compounds for 1 year on-board the ISS. A testflight
investigation on Biopan V was completed successfully in 2005. The
Organics experiment will monitor the chemical evolution, survival,
destruction and chemical modification of PAHs and fullerenes in space
environment. Samples are deposited in thin (~few hundred nm) films
by sublimation on MgF2 windows inside the sample cells. The samples
will be analyzed before and after exposure to space environment
with UV, visible and infrared spectroscopy and chemical analytical
techniques. Aromatic molecules are the most abundant carbonaceous
material that was delivered to the early Earth by small solar system
bodies and were recently proposed as intriguing material that could
have been involved in the transition from nonliving to living matter
during the origin of life. We discuss how data from EXPOSE-R (Organics)
and related ground-based tests are crucial to understand the evolution
of these abundant stable and ubiquitous molecules in space.
Title: Raman investigations of the EuroGeoMars Campaign
Authors: Wendt, L.; Mahapatra, P.; Gross, C.; Borst, A.; Foing, B. H.;
Exogeolab Team; Eurogeomars Team
Bibcode: 2009epsc.conf..457W
Altcode:
No abstract at ADS
Title: Outreach and education from EuroGeoMars Campaign
Authors: Foing, B. H.
Bibcode: 2009epsc.conf..641F
Altcode:
No abstract at ADS
Title: Search for radio flashes caused by collisions of meteoroids
with the moon
Authors: Volvach, A. E.; Berezhnoy, A. A.; Foing, B.; Erenfroyd, P.;
Havroshkin, O. B.; Volvach, L. N.
Bibcode: 2009KPCB...25..194V
Altcode:
No abstract at ADS
Title: Drilling on the Moon and Mars: Human Exploration Simulation
Experiments
Authors: Stoker, C.; Foing, B.; Zavaleta, J.; Clark, J.
Bibcode: 2009epsc.conf..659S
Altcode:
No abstract at ADS
Title: ExoGeoLab Test Bench for Landers, Rovers and Instruments
Authors: Foing, B. H.
Bibcode: 2009epsc.conf..639F
Altcode:
No abstract at ADS
Title: From Robotic to Human Exploration of the Moon: ILEWG roadmap
Authors: Foing, B. H.
Bibcode: 2009epsc.conf..657F
Altcode:
No abstract at ADS
Title: The Polar Maps of the Moon with AMIE/SMART-1
Authors: Despan, Daniela; Erard, S.; Barucci, A.; Josset, J. L.;
Beauvivre, S.; Koschny, D.; Almeida, M.; Grieger, B.; Foing, B.;
AMIE Team
Bibcode: 2009DPS....41.3506D
Altcode:
The AMIE camera on SMART-1, the first European lunar mission, provided a
large data set, including the north and the south pole regions. SMART-1
was in a 300 x 3000 km elliptical orbit, with perilune over the south
pole. The Moon surface displays two major types of terrain:
the bright and rugged highlands and darker, smoother plains. The
lunar north pole is in a highland region and spread out in between
three large impact craters: Peary, 88,6° N, 33° E, Hermite , 86° N,
89,9° W and Rozhdestvensky, 85,2° N, 155,4° W. The quantitative map
around the north pole shows news details of surface topography. The
floor of the Peary crater is smooth and presents only few meteoritic
bombardment formations most of them being near the rim. Similar technics
were applied to construct maps of the South pole region. The southern
highlands of the Moon are rugged and heavily cratered terrains with
geology dominated by the South pole -Aitken (SPA) basin. Abundant basin
secondary craters are scattered across the area, mostly created by the
Orientale basin impact to the west and north. A particular interest
has been carried to the topography surrounding the Shackleton crater,
which is nearly coincident with the South pole, at 89.9° latitude and
0° longitude, with 19 km diameter, according to USGS coordinates. The
AMIE mosaic of Shackleton crater spreads among 88,80 ° and 90 ° S in
latitude. The high resolution mosaic give details about the complete
rim of this crater with different illumination angles. The mosaic
of Shackleton crater was extended in a global map of the south pole
region. Eventually, the method used will be applied to mapping all areas
of interest where AMIE has provided high resolution observations. The
AMIE maps of the north and south pole of the Moon are presented.
Title: PCR-based Detection of Microbial Communities during the
EuroGeoMars MDRS Campaign
Authors: Thiel, C.; Wills, D.; Foing, B. H.
Bibcode: 2009epsc.conf..660T
Altcode:
No abstract at ADS
Title: From SMART-1 to Global Robotic Village and International
Lunar Bases
Authors: Foing, B. H.
Bibcode: 2009epsc.conf..655F
Altcode:
No abstract at ADS
Title: ExoGeoLab Test Bench for Landers, Rovers and Instruments
Authors: Foing, B. H.
Bibcode: 2009epsc.conf..637F
Altcode:
No abstract at ADS
Title: Photometric anomalies of the lunar surface studied with
SMART-1 AMIE data
Authors: Kaydash, V.; Kreslavsky, M.; Shkuratov, Yu.; Gerasimenko, S.;
Pinet, P.; Josset, J. -L.; Beauvivre, S.; Foing, B.; AMIE SMART-1 Team
Bibcode: 2009Icar..202..393K
Altcode: 2009Icar..202..393T
We present new results from the mapping of lunar photometric function
parameters using images acquired by the spacecraft SMART-1 (European
Space Agency). The source data for selected lunar areas imaged by
the AMIE camera of SMART-1 and the data processing are described. We
interpret the behavior of photometric function in terms of lunar
regolith properties. Our study reveals photometric anomalies on both
small (sub-kilometer) and large (tens of kilometers) scales. We found
the regolith mesoscale roughness of lunar swirls to be similar in Mare
Marginis, Mare Ingenii, and the surrounding terrains. Unique photometric
properties related to peculiarities of the millimeter-scale regolith
structure for the Reiner Gamma swirl are confirmed. We identified
several impact craters of subkilometer sizes as the source of
photometric anomalies created by an increase in mesoscale roughness
within the proximal crater ejecta zones. The extended ray systems
reveal differences in the photometric properties between proximal and
distant ejecta blankets. Basaltic lava flows within Mare Imbrium and
Oceanus Procellarum indicate higher regolith porosity for the redder
soils due to differences in the chemical composition of lavas.
Title: Special issue with papers from the ESLAB 2008 Symposium on
‘Cosmic Cataclysms and Life’
Authors: André, N.; Foing, B. H.; Cockell, C. S.
Bibcode: 2009IJAsB...8..145A
Altcode:
No abstract at ADS
Title: SMART-1 Results and Targets for LRO
Authors: Foing, B. H.; Koschny, D.; Grieger, B.; Josset, J. -L.;
Beauvivre, S.; Grande, M.; Huovelin, J.; Keller, H. U.; Mall, U.;
Nathues, A.; Malkki, A.; Noci, G.; Sodnik, Z.; Kellett, B.; Pinet, P.;
Chevrel, S.; Cerroni, P.; de Sanctis, M. C.; Barucci, M. A.; Erard,
S.; Despan, D.; Muinonen, K.; Shevchenko, V.; Shkuratov, Y.; Ellouzi,
M.; Peters, S.; Borst, A.; Baxkens, F.; Boche-Sauvan, L.; Mahapatra,
P.; Almeida, M.; Frew, D.; Volp, J.; Heather, D.; McMannamon, P.;
Camino, O.; Racca, G.
Bibcode: 2009LPICo1483...39F
Altcode:
No abstract at ADS
Title: Search for organics and life on Mars
Authors: Ehrenfreund, P.; Foing, B. H.
Bibcode: 2009GeCAS..73Q.320E
Altcode:
No abstract at ADS
Title: X-ray fluorescence observations of the moon by SMART-1/D-CIXS
and the first detection of Ti Kα from the lunar surface
Authors: SMART-1 Team; Swinyard, B. M.; Joy, K. H.; Kellett, B. J.;
Crawford, I. A.; Grande, M.; Howe, C. J.; Fernandes, V. A.; Gasnault,
O.; Lawrence, D. J.; Russell, S. S.; Wieczorek, M. A.; Foing, B. H.;
SMART-1 Team
Bibcode: 2009P&SS...57..744S
Altcode:
The demonstration of a compact imaging X-ray spectrometer (D-CIXS),
which flew on ESA's SMART-1 mission to the Moon ( Racca et al.,
2001; Foing et al., 2006), was designed to test innovative new
technologies for orbital X-ray fluorescence spectroscopy. D-CIXS
conducted observations of the lunar surface from January 2005
until SMART-1 impacted the Moon in September 2006. Here, we present
scientific observations made during two solar flare events and show
the first detection of Titanium Kα from the lunar surface. We discuss
the geological implications of these results. We also discuss how
experience from D-CIXS has aided the design of a similar instrument
(Chandrayaan-1 X-ray Spectrometer (C1XS)) that was launched on the
22nd October 2008 on India's Chandrayaan-1 mission to the Moon.
Title: The C1XS X-ray Spectrometer on Chandrayaan-1
Authors: Grande, M.; Maddison, B. J.; Howe, C. J.; Kellett, B. J.;
Sreekumar, P.; Huovelin, J.; Crawford, I. A.; Duston, C. L.; Smith,
D.; Anand, M.; Bhandari, N.; Cook, A.; Fernandes, V.; Foing, B.;
Gasnaut, O.; Goswami, J. N.; Holland, A.; Joy, K. H.; Kochney, D.;
Lawrence, D.; Maurice, S.; Okada, T.; Narendranath, S.; Pieters, C.;
Rothery, D.; Russell, S. S.; Shrivastava, A.; Swinyard, B.; Wilding,
M.; Wieczorek, M.
Bibcode: 2009P&SS...57..717G
Altcode:
The Chandrayaan-1 X-ray Spectrometer (C1XS) is a compact X-ray
spectrometer for the Indian Space Research Organisation (ISRO)
Chandrayaan-1 lunar mission. It exploits heritage from the D-CIXS
instrument on ESA's SMART-1 mission. As a result of detailed
developments to all aspects of the design, its performance as measured
in the laboratory greatly surpasses that of D-CIXS. In comparison
with SMART-1, Chandrayaan-1 is a science-oriented rather than a
technology mission, leading to far more favourable conditions for
science measurements. C1XS is designed to measure absolute and relative
abundances of major rock-forming elements (principally Mg, Al, Si,
Ca and Fe) in the lunar crust with spatial resolution ⩽25 FWHM km,
and to achieve relative elemental abundances of better than 10%.
Title: UV And Space Exposure Of Aromatic Compounds On The EXPOSE-R
Facility Onboard ISS
Authors: Bryson, Kathryn; Salama, F.; Enhrenfreund, P.; Ricco, A. J.;
Peeters, Z.; Foing, B. H.; Monaghan, E.; Wills, D.; Breitfellner,
M.; Jessberger, E.; Robert, F.; Mumma, M.
Bibcode: 2009AAS...21440210B
Altcode:
PAHs and fullerenes are thought to be among the carriers for numerous
astronomical absorption and emission features and have been identified
in meteorites. In addition, aromatic networks are likely the most
abundant organic material in space. Thin films of selected PAHs and
fullerenes will be subjected to the low Earth orbit environment as
part of the Organics experiment on the multi-user facility EXPOSE-R
onboard the International Space Station. EXPOSE-R will be mounted on the
International Space Station ISS in spring 2009. The Organics experiment
on EXPOSE-R will monitor the chemical evolution, survival, destruction
and chemical modification of polycyclic aromatic hydrocarbons (PAHs) and
fullerenes in space environment. The radiation dose that is collected
by the samples during flight exceeds the limits of simulations in the
laboratory and will greatly enhance our knowledge on the evolution of
large molecules in space environments. Dark samples will be shielded
from the UV photons and will enable us to differentiate between the
effects of exposure to photons and cosmic rays. In addition, the
experiment hosts pressurized and vented sample cells. All the samples
will be monitored before and after exposure to space environment. We
present spectra measured in the UV-Vis-NIR range of the flight samples
prior to space exposure.
Title: Design and Demonstration of Minimal Lunar Base
Authors: Boche-Sauvan, L.; Foing, B. H.; Exohab Team
Bibcode: 2009EGUGA..1113254B
Altcode:
Introduction: We propose a conceptual analysis of a first minimal
lunar base, in focussing on the system aspects and coordinating every
different part as part an evolving architecture [1-3]. We justify the
case for a scientific outpost allowing experiments, sample analysis
in laboratory (relevant to the origin and evolution of the Earth,
geophysical and geochemical studies of the Moon, life sciences,
observation from the Moon). Research: Research activities will be
conducted with this first settlement in: - science (of, from and
on the Moon) - exploration (robotic mobility, rover, drilling), -
technology (communication, command, organisation, automatism). Life
sciences. The life sciences aspects are considered through a life
support for a crew of 4 (habitat) and a laboratory activity with
biological experiments performed on Earth or LEO, but then without
any magnetosphere protection and therefore with direct cosmic rays
and solar particle effects. Moreover, the ability of studying the
lunar environment in the field will be a big asset before settling
a permanent base [3-5]. Lunar environment. The lunar environment
adds constraints to instruments specifications (vacuum, extreme
temperature, regolith, seism, micrometeorites). SMART-1 and other
missions data will bring geometrical, chemical and physical details
about the environment (soil material characteristics, on surface
conditions …). Test bench. To assess planetary technologies and
operations preparing for Mars human exploration. Lunar outpost
predesign modular concept: To allow a human presence on the moon
and to carry out these experiments, we will give a pre-design of a
human minimal lunar base. Through a modular concept, this base will
be possibly evolved into a long duration or permanent base. We will
analyse the possibilities of settling such a minimal base by means of
the current and near term propulsion technology, as a full Ariane 5 ME
carrying 1.7 T of gross payload to the surface of the Moon (Integrated
Exploration Study, ESA ESTEC [1,2]). We will focus on the easiest and
the soonest way in settling a minimal base immediately operational in
scientific experimentation, but not immediately autonomous. It will
prepare the next permanent lunar base by assessing its technologies,
and give scientific results about the environment. The autonomy will
be gained in the evolution of the base, and added equipment. A lunar
outpost in a polar region would allow missions longer than 14 days,
and a frequent addition of equipments. Moreover, a polar outpost will
get both advantages of far-side for simulating direct or indirect
communications to Earth and dark-side for observations. The low
solar rays incidence may permit having ice in deep craters, which
will be beneficial for the evolution of the outpost into a autonomous
base. The South Pole, by its position on the edge of the South Pole
Aitken (SPA) Basin, will allow different fast new data in analysis
mantle samples, easily reachable due to the crater morphology. These
samples will constrain the putative Late Heavy Bombarment (LHB). After
a robotic sample return mission, a human presence will allow deeper
research through well chosen geological samples [6]. In this modular
concept, we consider various infrastructure elements: core habitat,
EVA, crew mobility, energy supply, recycling module, communication,
green house and food production, operations. Many of these elements
have already been studied in space agencies' architecture proposals,
with the tech-nological possibilities of industrial partners (lunar
landers, lunar orbiter, rovers …). A deeper reflection will be
therefore done about the core habitat and the laboratory equipment,
proposing scientific priority experiments. Each element will be added
in a range considering their priority to life support in duration
[7]. Considering surface operations, protocols will be specified
in the use of certain elements. After a reflexion on the different
dependancies and priorities between these modules, a demonstration
can assess the reliability of the concept and develop the evolution
according to the practical needs. We shall also discuss experience form
the ExoHab project and EuroGeoMars cmapign at Mars Desert Research
station. References: [1] "Exploration Architecture Trade Report",
ESA, 2008, [2] "Integrated Exploration Architecture", ESA, 2008, [3]
9th ILEWG International Conference on Exploration and Utilization of
the moon, 2007, Foing et al Eds., (http://sci.esa.int/ilewg) [4] "The
Moon: Resources, Future Development and Colonization", David Schrunk,
Burton Sharpe, Bonnie Cooper and Madhu Thangavelu, 1999. [5] "The Moon
as a Platform for Astronomy and Space Science", B.H. Foing, ASR 14
(6), 1994. [6] "The Moon after Apollo, 40 Years Later: Why and what
Samples to Return ?", Johannes Geiss, Alpbach summer school 2008. [7]
"Advanced Life Support, Baseline Values and Assumptions Document",
Anthony J. Hanford, 2004
Title: EuroGeoMars mission and techniques: First results for geology
and geochemistry
Authors: Peters, S. T. M.; Borst, A.; Wendt, L.; Gross, C.; Stoker,
C.; Zhavaleta, J.; Sarrazin, P.; Slob, E.; Pletser, V.; Foing, B.
Bibcode: 2009EGUGA..1113353P
Altcode:
The EuroGeoMars expedition forms part of the European Space Agency's
ExoGeoLab research project and is a test campaign at the MDRS (Mars
Desert Research Station), which is operated by the Mars Society, in the
Utah desert, US. MDRS has yet been used by research groups of various
interest as an analogue site to the Martian environment. The goal of
this expedition is to simulate the employment of various instruments
and sample return under Martian conditions, while carrying out several
geological and biological investigations. In this paper we present
our methods and first results for the geological and geochemistry
investigations. Two main geological investigations have been carried
out, of which one includes mapping of the sequence stratigraphy and
internal structure of Quaternary alluvial fan deposits, 5 km South-West
of the MDRS. Alluvial fans are formed when a stream gradient decreases
over a relatively small area and therefore coarse-grained sediments
are being deposited. Alluvial fans on Mars are of particular interest
because they may have formed, as they do on Earth, a niche for life at
deposition time. If any was present, the sediments may contain detritus
that was transported by the river from the hinterland. Furthermore, the
internal structure and lithology represent the depositional environment,
water activity, and climatological perturbations. These three factors
provide main implications for the conditions and possibilities of
maintaining life. Mineralogical variations represent changes in the
source area of the sediments and hence possible tectonic activity. The
fan that we investigated measures 1.5 x 1.5 km and is made up of
several stratigraphic sequences that we defined by classic geological
methods. We followed the sedimentary sequences laterally using a
Ground Penetrating Radar system (GPR) and taking samples for ground
truth by drilling. All samples were analyzed on mineral content using
Raman spectroscopy and XRF (X-Ray Fluorescence) for mineralogical and
elemental analysis respectively. We created lacquer peels from several
sequences in order to sample and study sedimentary structures. The
procedure to make lacquer peels is to poor lacquer over an outcrop
and sticking the unconsolidated sediments to a piece of cloth, which
is subsequently pasted upon a hardboard plank. Another investigation
that was carried out focuses on the possibilities and restrictions to
the geologist for future fieldwork on Mars. Hence the investigators
did similar type of experiments as for the alluvial fan, wearing
spacesuits and spending restricted time outside as they would on a
Martian base. The EuroGeoMars expedition is the first in a series of
manned planetary mission simulations.
Title: ExoGeoLab Test Bench for Landers, Rovers and Instruments
Authors: Foing, B. H.
Bibcode: 2009EGUGA..1113122F
Altcode:
In the frame of ESTEC technology and research pilot project, we have
started a small pilot facility with a ExoGeoLab and a mini-Habitat,
supported by two design and control offices in the European Space
Incubator (ESI), as well as infrastructure support and manpower. We
have in addition to contribution on external instruments and manpower
from partner institutes. From this test bench and kit of ExoGeoLab
instruments, we plan to operate comprehensive instruments packages
that could help in the technical research and science preparation
of lander/rover missions studied in the frame of Cosmic Vision or
the Exploration programme. The ExoGeoLab research incubator project
includes a sequence of activities: - Data analysis and interpretation
of remote sensing data (MEX, SMART-1, VEX, Cassini-Huygens) and in-situ
(Huygens, MER) , and merging of multi-scale data sets - Procurement and
integration of geophysical, geochemical and astrobiological breadboard
instruments in an surface station and rover (ExoGeoLab) - Research
operations and exploitation of ExoGeoLab test bench for various
conceptual configurations (Moon, Mars, NEO, Titan) - Contribution
to the exploitation of surface lander results (MER, Phenix, MSL,
preparation Exomars) - Scientific simulation of planetary surfaces
using laboratory and modelling tools - Support research for definition
and design of science surface packages on the Moon, Mars, NEO, Titan
- Research support to community preparation of payload for surface
lander opportunities Specific goals and methods of ESTEC ExoGeoLab:
we have started to integrate instruments in an ExoGeoLab crossing
various techniques. The methodic steps for this hands-on research
are: 1) We have procured and adapted instruments to equip a mid-size
ExoGeoRover (made available in collaboration with ESTEC robotics
section), and a small surface station. 2) This terrestrial payload
(instruments, sensors, data handling) will be deployed, operated and
used as collaborative research pilot facility (ExoGeoLab), first tested
and operated at ESTEC, and later transportable 3) We shall perform
functional tests of these instruments, and operate them in terrestrial
conditions to correlate measurements using various techniques. 4)
We shall implement progressively the possibility of remote control of
instruments from an adjacent habitat (ExoHab 6-crew caravan recently
acquired as part of ESTEC skunks pilot project), and a remote science
desk. 5) The suite of measurements includes a comprehensive set with
telescopic imaging reconnaissance and monitoring, geophysical studies,
general geology and morphology context, geochemistry (minerals,
volatiles, organics), subsurface probe, sample extraction and
retrieval, sample analysis. 6) We shall reproduce some simulation of
diverse soil and rocks conditions (mixture of minerals, organics, ice,
penetrations of water, oxydant, organics) and diagnostics 7) We shall
use these instrument packages to characterise geological context, soil
and rock properties, 8) Science investigations will include geology,
geochemistry, measurements relevant to penetration/survival of water,
oxydant, organics, mineral and volatiles diagnostics. 9) After first
validations we shall exploit the facility for collaboration with
partners that will provide some additional guest instruments, and
perform specific investigations, 10) We shall organise field campaigns
in specific locations of scientific and exploration interest, making
use of the ExoHab habitat for logistics support and local operations
Title: A Small Lunar Rover for Reconnaissance in the Framework of
ExoGeoLab Project, System Level Design
Authors: Noroozi, A.; Ha, L.; van Dalen, P.; Maas, A.; de Raedt, S.;
Poulakis, P.; Foing, B. H.
Bibcode: 2009EGUGA..1113167N
Altcode:
Scientific research is based on accurate measurement and so depends
on the possibilities of accurate instruments. In planetary science
and exploration it is often difficult or even impossible in some cases
to gather accurate and direct information from a specified target. It
is important to gather as much information as possible to be able to
analyze and extract scientific data from them. One possibility to do
so is to send equipments to the target and perform the measurements
locally. The measurement data is then sent to base station for further
analysis. To send measurement instruments to measurement point it is
important to have a good estimation of the environmental situation
there. This information can be collected by sending a pilot rover to
the area of interest to collect visual information. The aim of this
work is to develop a tele-operated small rover, Google Lunar X-Prize
(GLXP) class, which is capable of surviving in the Moon environment
and perform reconnaissance to provide visual information to base
station of ExoGeoLab project of ESA/ESTEC. Using the state of the art
developments in electronics, software and communication technologies
allows us to achieve increase in accuracy while reducing size and power
consumption. Target mass of the rover is lees than 5 kg and its target
dimension is 300 x 60 x 80 mm3. The small size of the rover gives the
possibility of accessing places which are normally out of reach. The
required power for operation and the cost of launch is considerably
reduced compared to large rovers which makes the mission more cost
effective. The mission of the rover is to capture high resolution
images and transmit them to base station. Data link between lover and
base station is wireless and rover should supply its own energy. The
base station can be either a habitat or a relay station. The navigation
of the rover is controlled by an operator in a habitat who has a view
from the stereo camera on the rover. This stereo camera gives image
information to the base and gives the possibility for future autonomous
navigation by using three-dimensional image recognition software. As
the navigation view should have minimum delay, the resolution of
stereo camera is not very high. The rover design is divided into four
work packages. These work packages are remote imaging, remote manual
navigation, locomotion and structure, and power system. Remote imaging
work package is responsible for capturing high resolution images,
transmitting image data to base station via wireless link and store
the data for further processing. Remote manual navigation is handling
the tele-operation. It collects stereo images and navigation sensor
readouts, transmits stereo images and navigation data to base station
via wireless link, displays the image and sensor status in a real-time
fashion on operator's monitor, receives command from operator's
joystick, transfers navigation commands to rover via wireless link,
and operates the actuators accordingly. Locomotion and structure takes
care of designing the body structure and locomotion system based on
the Moon environment specifications. The target specifications of rover
locomotion system are maximum speed of 200 m/h, maximum acceleration of
0.554 m/s2, and maximum slope angle of 20Ë . The power system for
the rover includes the solar panel, batteries and power electronics
mounted on the rover. The energy storage in the rover should be able
to survive for minimum 500 m movement on the moon. Subsequently, it
should provide energy for other sub-systems to communicate, navigate
and transmit the data. Considering the harsh environmental issues on
the Moon such as dust, temperature range and radiation, it is vital for
the mission that these issues are considered in the design to correctly
dimension reliability and if necessary redundancy. Corrosion resistive
material should be used to ensure the survival of mechanical structure,
moving parts and other sensitive parts such as electronics. High
temperature variation should be considered in the design of structure
and electronics and finally electronics should be radiation protected.
Title: Characterisation of sites of astrobiology interest for Mars
landers and sample return missions
Authors: Wills, D. E. S.; Monaghan, E. P.; Foing, B. H.
Bibcode: 2009EGUGA..1111568W
Altcode:
Introduction: The aim of this work is to nominate and assess candidate
landing sites for missions of astrobiological interest to Mars. We
report in particular on science and technical criteria and our
data analysis for sites suitable for an ExoMars-class mission. This
includes information from previous missions (such as Mars Express,
MGS, Odyssey, MRO and MER rovers) on mineralogical composition,
geomorphology, evidence from past water history from imaging and
spectroscopic data, and existence of in-situ prior information from
landers and rovers (concerning evidences for volatiles, organics and
habitability conditions). Science Goals and Objectives: Firstly,
we look for morphological evidence of hydrological activity,
including sedimentary deposits (deltas, valley networks), areas
of ancient hydrothermal activity (spring deposits). Secondly, we
look for mineralogical evidence of hydrological activity, such as
phyllosilicates (formed by alteration due to water, indicate prolonged
exposure to standing water), hydrated sulphates (formed by alteration
due to water, not necessarily standing water), other water-containing
minerals. Thirdly, we prioritise Noachian terrain (during this epoch,
~3.5 billion years ago, the Martian climate may have been warmer, and
liquid water may have been stable on the surface). Finally, we look for
sites where the potential for preservation of biosignatures is high
(exposed bedrock, subsurface regions, spring sinters). Engineering
Constraints: We consider the engineering constraints placed on the
ExoMars misson. These include latitude (sufficient insolation for
power), landing altitude (sufficient atmosphere for EDL), horizontal
winds, shear, and wind turbulence (airbag free fall), radar altimeter
reflectivity (for descent and landing control), obstacles and rock
distribution (airbag landing), slopes (airbag landing), rover egress,
and rover locomotion. The Priority Sites: Out of a short-list of
ten proposed locations, we select two top priority sites and a
safe-haven. The sites chosen are Mawrth Vallis (21.6°N, 344.0°E)
and Vernal Crater (5.9°N, 355.3°E), and a safe-haven in Eastern
Meridiani (0° N, 3.7°E). The entire length of Mawrth Vallis is of
interest, not least because the source is unknown. It doesn't begin
in chaotic terrain like the majority of outflow channels. Weathered
phyllosilicates are prevalent and their variety, concentration and
surface area are currently unmatched compared to anywhere on Mars. They
exist in layered outcrops. Structures in Vernal Crater are strongly
suggestive of spring deposits, which would have a high potential
for preservation of biosignatures. Other key features of interest at
this site include probable lake-shore and regional fluvial deposits,
lacustrine layers and evidence of methane activity. Eastern Meridiani
has been nominated as a potential safe-haven. The science interest of
this site includes many diverse layers, evidence of phyllosilicates,
and excavation of underlying material by cratering. General references:
G. Neukum, R. Jaumann et al., HRSC: The High Resolution Stereo
Camera of Mars Express, in Mars Express: The scientific payload,
edited by A. Wilson, pp. 17-35, ESA, Noordwijk, The Netherlands, 2004;
R. Jaumann, G. Neukum, T. Behnke, T.C. Duxburry, K. Eichentopf, S. van
Gasselt, B. Giese, K. Gwinner, E. Hauber, H. Hoffmann, A. Hoffmeister,
U. Köhler, K.D; Matz, T.B. McCord, V. Mertens, J. Oberst, R. Pischel,
D. Reiß, E. Ress, T. Roatsch, P. Saiger, F. Scholten, G. Schwarz,
K. Stephan, M. Wählisch, and the HRSC; Co-Investigator Team: The High
Resolution Stereo Camera (HRSC) Experiment on Mars Express: Instrument
Aspects and Experiment Conduct from Interplanetary; Cruise through
Nominal Mission, Planetary and Space Science, 55, 928-952, 2007.
Title: Basic Mars Navigation System For Local Areas
Authors: Petitfils, E. -A.; Boche-Sauvan, L.; Foing, B. H.; Monaghan,
E.; Crews, Eurogeomars
Bibcode: 2009EGUGA..1113242P
Altcode:
Introduction: This project has been first set up as a basic solution
in navigation during EVA (extra-vehicular activities) in the Mars
Society Desert Research Station in the desert of Utah. The main idea
is to keep the system as simple as possible so that it can be easily
adaptable and portable. The purpose of such a device is to tell the
astronauts in EVA where they roughly are and then letting them reaching
different points in avoiding any risky way. Thus the precision needed
has not to be really high: even if it is about 50m, every astronaut can
then look on a map and be able to design a way to another point. This
navigation system will improve the safety of the EVA as it is an added
reliable orientating tool. Concept: To look at a simple way to localize
oneself, one should have a look at what has been done by mankind on
Earth. Today, everyone can think of the GPS because it's simple and
very reliable. However the infrastructure for such a system is huge
and will not be for sure available during the first missions. We can
think of course of a basic GPS using the satellites being in orbit
but this approach is not yet as simple as we would like. If we want to
keep the sky in sight, we can use the stars and the moons of Mars. Yet
this would be a good solution and we can even have a star tracker that
would give a good position according to the time of the picture. This
solution has to be kept in mind but a star tracker is quite big for
an astronaut without any rover nearby and using the sky may not be as
precise as one should expect. Another useful tool is the compass. It
has been used for centuries by sailors but on Mars, without a good
magnetic field for this purpose. But sailors also use lighthouses and
some placemarks on the land to localize themselves. This is done with
a compass, measuring the angle between a placemark and the magnetic
North. With two angles, we can then have the position of the boat. The
idea here is the same: measuring the angles between different placemarks
so that we can compute the position. But which placemarks? We have
to think about something that can be installed on Mars and is light
enough to be brought there. Balloons are really light, and in order
to place them, we need a gas as helium (or hydrogen) and also some
rope. Hydrogen is likely to be produced in situ and rope will be useful
for astronauts. So we started on a concept with some balloons around the
base, with different colors or patterns. The crew in EVA can thus know
where the base is every time they are in sight of a balloon and with at
least three balloons; they can compute their position according to the
base. Procedure of the test: During EVA, the astronauts will measure
the angle between the different balloons. The balloons are high in the
sky so they can be seen far from their location. This is particularly
important on Mars where the horizon is nearer than on Earth. The
balloons have different colors so they can be identified and we can
even think of adding an autonomous colored light under so they can be
observed during the night. With good quality balloons, we can keep them
in the sky for a few days without maintenance. Angle measurement is done
thanks to a camera. A numeric camera can have a precision of less than
0.01°/pixel, which is enough for our application. The distance between
the different balloons can easily be seen in a free picture management
software and a Matlab tool is under development for this. An algorithm
is then run and it gives the positions that fit with the observations
on a map. Simulation gave areas 20m width, which is enough for the
astronaut who has a map. The exact precision will be investigated in
situ, at the MDRS. For this first test bench, computations will be
manually done on a computer in order to validate the concept without
huge development. Afterwards, one can imagine an implementation on a
PDA brought by the astronauts. This PDA would have its own camera so
the process can be fully automatic. Such a system can also implement
other navigation system as a Martian GPS or a radio localization
system like a VOR in order to enhance the reliability of the system
and use all the advantages of each method. Acknowledgements: We thank
the ExoGeoLab, EuroGeoMars teams for support during tests, operations
and data analysis. References: [1] "ExoGeoLab Lander/Rover instruments
and EuroGeoMars MDRS campaign", B.H. Foing, LPSC abstract 2009
Title: EuroGeoMars campaign at Mars Desert Research Station: Preparing
for Future Mars Landers and Sample
Authors: Foing, B. H.; Pletser, V.; Stoker, C.; Boche-Sauvan, L.
Bibcode: 2009EGUGA..1113180F
Altcode:
Background: Surface science is one of the prime objectives of current
and future Mars, Moon, or planetary missions and encompasses a wide
range of activities from global mapping via specific studies of
localised regions until microscopic scales. The studies of rocks and
soil in situ, or with sample return missions, require the development of
systematic multi-instruments protocols, characterisation diagnostics,
and merging of data from various techniques. Both photogeology and
mineralogical wide scale mapping have been performed to some extent
previously so significant new surface science results may only come
from co-ordinated multi-instrument operations operating from the
surface. EuroGeoMars MDRS campaign: The goal of the mission (from 24
January to 1 March 2009) is to demonstrate and validate a procedure
for Martian surface in-situ and return science. This chain begins with
characterisation of the local surface and close sub-surface environment,
before moving on to sample extraction and analysis. The characterisation
stage involves a survey of a sample area in the vicinity of the MDRS
site by our geologists and other team members. This utilises satellite
and aerial photography to inform the overallmorphology and geological
unit distribution, with the specific geological and geochemical context
being provided through the use of imagers and spectrometers. Further
reconnaissance is used to plan sample-extraction EVAs at sites of
geochemical and astrobiological significance. Characterisation of
larger-scale features is conducted in-situ (for example using ground
penetrating radar to investigate the close sub-surface). Results from
these sorties inform the choice and planning of sites for surface
and sub-surface sampling. The sample extraction step - the nature
of which is dependent on the identified areas of interest - involves
standard geological tools such as rock drills and scoops etc, as well
as more specific techniques such as lacquer peels. These samples are
returned to the MDRS for analysis using microscopes and other analysis
techniques. These documented samples are afterward taken to ESTEC and
collaborators institutes for analysis by various techniques.
Title: Flexure and isostasy of lunar mascons
Authors: Peters, S. T. M.; Foing, B. H.
Bibcode: 2009EGUGA..1111546P
Altcode:
A mascon is a region of a planet's or moon's crust that contains an
excess positive gravity anomaly, indicating the presence of additional
mass in this area. Mascons on the Moon coincide with the locations of
circular basins and hence a related origin for both is likely. The
formation of a circular basin includes the excavation of the upper
parts of the crust and subsequent upwelling of the lower parts as
a result of isostatic compensation [1]. Afterwards, filling of the
basins by mare basalts leads to concentrations of dense rocks and is
hence suggested as the origin of the mascon. The present day presence
of mascons indicates that there was no subsequent isostasy leading to
downward migration of the moho and that they are hence supported by
an elastic layer on the surface of the Moon. The interaction between
mascons and this elastic shell is the main topic of our modeling. Since
they were discovered by Muller and Sjogren (1968), the origin of
mascons and their interaction with the crust became clearer. As we
point out below, several questions have however remained unsolved. Our
contribution includes the usage of recent gravity and topography models
that have not been applied in mascon studies yet. Mascons act like
a dense load on the lunar lithosphere and hence flexure it. Flexure
profiles of circular basins have been made by previous authors [2],
however, only a single-layered crust was considered until now. Our
modeling includes the two-layered crustal model preferred by Wieczorek
and Phillips (1997) which explains the gravity to topography ratios of
the lunar highlands. On the hand of previously existing data it has been
suggested that rings of negative gravity anomalies surround the mascons
[3]. Whereas this observation was first questionable, prereleases
of the high-resolution KAGUYA gravity measurements recently clearly
confirmed the presence of these features. Part of our modeling focuses
on the location and extent of the negative anomalies in respect to
the flexural depression. Furthermore we model the locations of failure
that result from flexural stresses and compare these with the observed
faults on the lunar surface, using high-resolution AMIE-images from
ESA's SMART-1 mission. We produced flexure profiles for circular basins
Humorum, Imbrium, Serenitates and Orientale, that all coincide with
mascon locations. We use a modified version of COBRA[4] for PC. The
program input and output is managed by macros included in a Microsoft
Excel file. Because the mascons have rather an axially symmetric than
elongated shape, we calculate the flexure to point loads. The gravity
and topography data that we use is provided on the web by Wieczorek
(2006) (http://www.ipgp.jussieu.fr/~wieczor). By combining the most
recent topography model [GLTM2C by Smith et al. (1997)], with the
most recent gravity model [LP150Q by Konopliv et al. (2001)], he
calculated crustal thicknesses for three model types. The first model
examines the crust as a single layer in which gravity is assumed to
result from Moho relief and Mare basalt fill. The second model has
the only difference that Bouguer correction was set to zero before
inverting for the relief along the crust-mantle interface. The third
model examines a dual-layered crust. Since crustal thickness equals
Moho depth on the Moon, we can use these different models as input for
our software. We define the characteristics of the initial situation,
i.e. height, depth and density contrast of the load before flexure. We
vary elastic parameters like elastic thickness and yield strength,
and use a Poisson's ration of 0.25 and an average Young's Modulus
of 1.1x1011 N/m2. Shearforce and bending moment are assumed to be
zero. The coming together of negative gravity anomalies related to
distinct mascons (e.g. Mare Imbrium and Mare Serenitatis) suggests
interaction of flexure. We aim to use 3D finite element models to
visualize this interaction. Furthermore we aim to include the effects
of viscous deformation of the lunar interior as a result of mascon
loading in our models. References: [1] Neumann et al., (1996), JGR, 101,
16841-16864 [2] Arkani-Hamed, (1998), 103, 3709-3739 [3] Sjogren et al.,
(1972), Science, 175, 165-168 [5] program originally based on Bodine
(1982), modifications by Zoetemeijer (2001)
Title: Report from ILEWG and Cape Canaveral Lunar Declaration 2008
Authors: Foing, B. H.
Bibcode: 2009EGUGA..1113223F
Altcode:
We shall report on the ILEWG charter, goals and activities, on
ICEUM "lunar declarations" and follow-up activities, with focus
on societal questions, and the Cape Canaveral Lunar Declaration
2008. ILEWG charter: ILEWG , the International Lunar Exploration
Working Group is a public forum created in 1994, sponsored by the
world's space agencies to support "international cooperation towards
a world strategy for the exploration and utilization of the Moon -
our natural satellite". The charter of ILEWG is: - To develop an
international strategy for the exploration of the Moon - To establish
a forum and mechanisms for the communication and coordination of
activities - To implement international coordination and cooperation
- In order to facilitate communication among all interested parties
ILEWG agrees to establish an electronic communication network for
exchange of science, technology and programmatic information related
to lunar activities ILEWG meets regularly, at least, once a year,
and leads the organization of an International Conference in order
to discuss the state of lunar exploration. Formal reports are given
at COSPAR meetings and to space agencies. ILEWG is sponsored by the
world's space agencies and is intended to serve three relevant groups:
- actual members of the ILEWG, ie delegates and repre-sentatives of
the participating Space Agencies and organizations - allowing them
to discuss and possibly harmonize their draft concepts and plans
- team members of the relevant space projects - allowing them to
coordinate their internal work according to the guidelines provided by
the Charter of the ILEWG - members of the general public and of the
Lunar Explorer's Society who are interested and wish to be informed
on the progress of the Moon projects and possibly contribute their
own ideas ILEWG activities and working groups: ILEWG task groups
include science, technology, human aspects, socio-economics, young
explorers and outreach, programmatics, roadmaps and synergies with
Mars exploration. Users can obtain information on how to participate,
as well as details on the latest news and events regarding lunar
exploration, forthcoming meetings, relevant reports and documents
of importance for the work of the ILEWG, summary descriptions of
current lunar exploration projects (such as SMART-1, Chang'E1, Selene,
Chandrayaan-1, LRO, LCROSS) funded by various space agencies, and basic
data on the Moon itself. Activities of the related space agencies and
organizations can also be found. ILEWG has been organising International
Conferences on Exploration and Utilisation of the Moon (ICEUM)
since 1994, whose proceedings are published. It has also sponsored
a number of activities, workshops, tasks groups and publications in
collabora-tions with other organisations: COSPAR, space agencies,
IAA, IAF, EGU (see references below). In accor-dance with its charter,
ILEWG reports to COSPAR, and a summary was given at Montreal COSPAR2008
on ILEWG activities conducted since the previous COSPAR2006 assembly
in Beijing. The recent ILEWG International Conference on Exploration
and Utilisation of the Moon, were held respectively in Udaipur, India
(ICEUM6, 2004), in Toronto, Canada (ICEUM7, 2005), in Beijing (ICEUM8,
2006), Sorrento (ICEUM9, 2007) and Port Canaveral (ICEUM10/LEAG/SRR,
2008 in conjunction with the NASA Lunar Exploration Analysis Groups and
Space Resources Roundtable annual meetings). We'll report on the Cape
Canaveral Lunar Declaration and on follow-up activities, in particular
in coordination with space agencies, COSPAR and IAF. References: [1]
1st International Lunar Workshop, Balsiger H. et al., Editors, European
Space Agency, 1994. ESA-SP-1170. [2] 2nd International Lunar Workshop,
Kyoto, H. Mizutani, editor, Japan Space Forum Publisher, 1997. [3]
3rd International Lunar Workshop, Moscow 1998, E. Galimov, editor. [4]
ICEUM4, ESTEC, 2000, ESA SP-462, B.H. Foing & M. Perry, editors. [5]
ICEUM5, Hawaii Nov 2003, Durst S.M. et al, Editors, Vol 108, 1-576
pp, Science and Technology Series, American Astronautical Society,
2004. [6] ICEUM6, Udaipur 2004, Bhandari N., Editor, Journal Earth
System Science, India, 114, No6, Dec 2005, pp. 573-841. [7] ICEUM7,
Toronto Sept 2005, sci.esa.int/ilewg. [8] ICEUM8, Beijing July 2006,
Journal of Chinese Society of Astronautics, Vol. 28 Sup., 2007, Ji W.,
Editor. [9] ICEUM9, Sorrento, Italy, Foing B., Espinasse S., Kosters
G., Editors. http://sci.esa.int/iceum9, Dec. 2007), [11] Ehrenfreund,
P., Foing, B.H., Cellino, A. Editors, The Moon and Near Earth Objects,
ASR Vol 37, 1, 2006. [12] Foing, B.H. et al editors, 'Astronomy and
Space Science from the Moon', ASR 14, 6, 1994. [13] Foing, B.H. et al,
editor, Lunar Exploration, Planetary and Space Science, Vol 50, 14-15,
2002. [14] Foing, B.H., Heather, D. editors, 'Lunar Exploration 2000',
ASR Vol 30, Nr 8, 2002. [15] Hunt-ress, W. et al 'The next steps in
exploring deep space - A cosmic study by the IAA', Acta Astronautica,
Vol 58, Issues 6-7, 2006, p302-377. [16] Ip W.-H., Foing, B.H., Masson
Ph.L., editors, The Moon and Mars, ASR Vol 23, 11, 1999.
Title: Lunar single-scattering, porosity, and surface-roughness
properties with SMART-1/AMIE
Authors: Parviainen, H.; Muinonen, K.; Näränen, J.; Josset, J. -L.;
Beauvivre, S.; Pinet, P.; Chevrel, S.; Koschny, D.; Grieger, B.;
Foing, B.
Bibcode: 2009EGUGA..11.7966P
Altcode:
We analyze the single-scattering albedo and phase function,
local surface roughness and regolith porosity, and the coherent
backscattering, single scattering, and shadowing contributions to
the opposition effect for specific lunar mare regions imaged by
the SMART-1/AMIE camera. We account for shadowing due to surface
roughness and mutual shadowing among the regolith particles with
ray-tracing computations for densely-packed particulate media with a
fractional-Brownian-motion interface with free space. The shadowing
modeling allows us to derive the hundred-micron-scale volume-element
scattering phase function for the lunar mare regolith. We explain
the volume-element phase function by a coherent-backscattering model,
where the single scatterers are the submicron-to-micron-scale particle
inhomogeneities and/or the smallest particles on the lunar surface. We
express the single-scatterer phase function as a sum of three
Henyey-Greenstein terms, accounting for increased backward scattering
in both narrow and wide angular ranges. The Moon exhibits an opposition
effect, that is, a nonlinear increase of disk-integrated brightness with
decreasing solar phase angle, the angle between the Sun and the observer
as seen from the object. Recently, the coherent-backscattering mechanism
(CBM) has been introduced to explain the opposition effect. CBM is
a multiple-scattering interference mechanism, where reciprocal waves
propagating through the same scatterers in opposite directions always
interfere constructively in the backward-scattering direction but with
varying interference characteristics in other directions. In addition to
CBM, mutual shadowing among regolith particles (SMp) and rough-surface
shadowing (SMr) have their effect on the behavior of the observed lunar
surface brightness. In order to accrue knowledge on the volume-element
and, ultimately, single-scattering properties of the lunar regolith,
both SMp and SMr need to be accurately accounted for. We included
four different lunar mare regions in our study. Each of these regions
covers several hundreds of square kilometers of lunar surface. When
selecting the regions, we have required that they have been imaged
by AMIE across a wide range of phase angles, including the opposition
geometry. The phase-angle range covered is 0-109 °, with incidence and
emergence angles (ι and ε) ranging within 7-87 ° and 0-53 °,
respectively. The pixel scale varies from 288m down to 29m. Biases
and dark currents were subtracted from the images in the usual way,
followed by a flat-field correction. New dark-current reduction
procedures have recently been derived from in-flight measurements to
replace the ground-calibration images . The clear filter was chosen
for the present study as it provides the largest field of view and is
currently the best-calibrated channel. Off-nadir-pointing observations
allowed for the extensive phase-angle coverage. In total, 220 images
are used for the present study. The photometric data points were
extracted as follows. First, on average, 50 sample areas of 10 Ã-
10 pixels were chosen by hand from each image. Second, the surface
normal, ι, ε, °, and α were computed for each pixel in
each sample area using the NASA/NAIF SPICE software toolkit with
the latest and corrected SMART-1/AMIE SPICE kernels. Finally, the
illumination angles and the observed intensity were averaged over
each sample area. In total, the images used in the study resulted
in approximately 11000 photometric sample points for the four mare
regions. We make use of fractional-Brownian-motion surfaces in modeling
the interface between free space and regolith and a size distribution
of spherical particles in modeling the particulate medium. We extract
the effects of the stochastic geometry from the lunar photometry
and, simultaneously, obtain the volume-element scattering phase
function of the lunar regolith locations studied. The volume-element
phase function allows us to constrain the physical properties of the
regolith particles. Based on the present theoretical modeling of the
lunar photometry from SMART-1/AMIE, we conclude that most of the lunar
mare opposition effect is caused by coherent backscattering and single
scattering within volume elements comparable to lunar particle sizes,
with only a small contribution from shadowing effects. We thus suggest
that the lunar single scatterers exhibit intensity enhancement towards
the backward scattering direction in resemblance to the scattering
characteristics experimentally measured and theoretically computed
for realistic small particles. Further interpretations of the lunar
volume-element phase function will be the subject of future research.
Title: SMART-1: Review of Lunar Highlights
Authors: Foing, B. H.; Koschny, D.; Grieger, B.; Lossett, J. -L.;
Beauvivre, S.; Grande, M.; Huovelin, J.; Keller, H. U.; Mall, U.;
Nathues, A.; Malkki, A.; Noci, G.; Sodnik, Z.; Kellett, B.; Pinet, P.;
Chevrel, S.; Cerroni, P.; de Sanctis, M. C.; Barucci, M. A.; Erard,
S.; Despan, D.; Muinonen, K.; Shevchenko, V.; Shkuratov, Y.; Ellouzi,
M.; Peters, S.; Borst, A.; Bexkens, F.; Almeida, M.; Frew, D.; Volp,
J.; Heather, D.; McMannamon, P.; Camino, O.; Racca, G.; Peters, S.
Bibcode: 2009LPI....40.2298F
Altcode:
The SMART-1 spacecraft operated from 400-3000 km for 1.5 year until
impact. We shall report at LPSC2009 on SMART-1 lunar highlights
relevant for science and exploration, in relation with subsequent
missions Kaguya, Chang'E1 and Chandrayaan-1.
Title: ExoGeoLab Lander/Rover Instruments and EuroGeoMars MDRS
Campaign
Authors: Foing, B. H.; Batenburg, P.; Drijkoningen, G.; Slob, E.;
Poulakis, P.; Visentin, G.; Page, J.; Noroozi, A.; Gill, E.; Guglielmi,
M.; Freire, M.; Walker, R.; Sabbatini, M.; Pletser, V.; Monaghan,
E.; Boche-Sauvan, L.; Ernst, R.; Oosthoek, J.; Peters, S.; Borst, A.;
Mahapatra, P.; Wills, D.; Thiel, C.; Wendt, L.; Gross, C.; Petrova,
D.; Lebreton, J. P.; Zegers, T.; Stoker, C.; Zhavaleta, J.; Sarrazin,
P.; Blake, C.; McKay, C.; Ehrenfreund, P.; Chicarro, A.; Koschny,
D.; Vago, J.; Svedhem, H.; Davies, G.; Exogeolab Team; Eurogeomars Team
Bibcode: 2009LPI....40.2567F
Altcode:
We describe ExoGeoLab a planetary surface instruments research
incubator, and the EuroGeoMars campaign at the Mars Desert Research
station aimed at validating a procedure for martian surface in-situ
and return science.
Title: Reflection Seismology Systems for Planetary Geology: First
Tests at ESTEC ExoGeoLab and MDRS, Utah
Authors: Batenburg, P. A. W.; Foing, B. H.; Drijkonigen, G. G.; Gill,
E. K. A.; Poulakis, P.; Visentin, G.; Page, J.; Pletser, V.; Peters,
S.; Borst, A.; Mahapatra, P.; Exogeolab Team; Eurogeomars Team
Bibcode: 2009LPI....40.2536B
Altcode:
The authors investigated the use of reflective seismology for Planetary
geology within ESA’s ExoGeoLab pilot project. During the EuroGeoMars
expedition tests were performed to test the influence of surface
coupling and composition on data quality.
Title: Doppler maps and surface differential rotation of EI Eri from
the MUSICOS 1998 observations
Authors: Kővári, Zs.; Washuettl, A.; Foing, B. H.; Vida, K.; Bartus,
J.; Oláh, K.; MUSICOS 98 Team
Bibcode: 2009AIPC.1094..676K
Altcode: 2009csss...15..676K; 2008arXiv0811.0348K
We present time-series Doppler images of the rapidly-rotating active
binary star EI Eri from spectroscopic observations collected during
the MUSICOS multi-site campaign in 1998, since the critical rotation
period of 1.947 days makes it impossible to obtain time-resolved images
from a single site. From the surface reconstructions a weak solar-type
differential rotation, as well as a tiny poleward meridional flow
are measured.
Title: CoRot observations of active giants: preliminary results
Authors: Gondoin, P.; Fridlund, M.; Goupil, M. J.; Baudin, F.; Samadi,
R.; Barban, C.; Belkacem, K.; Corbard, T.; Dupret, M. A.; Foing, B.;
den Hartog, R.; Lebreton, Y.; Lochard, J.; Mathias, P.; Michel, E.;
Morel, P.; Moya, A.; Palacios, A.; Zahn, J. P.
Bibcode: 2009AIPC.1094..864G
Altcode: 2009csss...15..864G
We have analysed rotation modulated light-curves of active giants
observed with CoRot using spots model. Preliminary results suggest
an increase of the surface spot coverage with decreasing rotation
period. A maximum of the surface spot coverage seems to occur on
giants with effective temperature around 5100 K. Confirmation and
interpretation of these preliminary results require groundbased
follow-up observations to measure activity indicators, to identify
binary systems, and to determine the stellar parameters and evolutionary
status of the sample giants.
Title: Magnetic activity in the photosphere of CoRoT-Exo-2a. Active
longitudes and short-term spot cycle in a young Sun-like star
Authors: Lanza, A. F.; Pagano, I.; Leto, G.; Messina, S.; Aigrain,
S.; Alonso, R.; Auvergne, M.; Baglin, A.; Barge, P.; Bonomo, A. S.;
Boumier, P.; Collier Cameron, A.; Comparato, M.; Cutispoto, G.; de
Medeiros, J. R.; Foing, B.; Kaiser, A.; Moutou, C.; Parihar, P. S.;
Silva-Valio, A.; Weiss, W. W.
Bibcode: 2009A&A...493..193L
Altcode: 2008arXiv0811.0461L
Context: The space experiment CoRoT has recently detected transits by
a hot Jupiter across the disc of an active G7V star (CoRoT-Exo-2a)
that can be considered as a good proxy for the Sun at an age of
approximately 0.5 Gyr.
Aims: We present a spot modelling of
the optical variability of the star during 142 days of uninterrupted
observations performed by CoRoT with unprecedented photometric
precision.
Methods: We apply spot modelling approaches
previously tested in the case of the Sun by modelling total solar
irradiance variations, a good proxy for the optical flux variations
of the Sun as a star. The best results in terms of mapping of the
surface brightness inhomogeneities are obtained by means of maximum
entropy regularized models. To model the light curve of CoRoT-Exo-2a,
we take into account the photometric effects of both cool spots
and solar-like faculae, adopting solar analogy.
Results: Two
active longitudes initially on opposite hemispheres are found on the
photosphere of CoRoT-Exo-2a with a rotation period of 4.522 ± 0.024
days. Their separation changes by ≈80° during the time span of the
observations. From this variation, a relative amplitude of the surface
differential rotation lower than ~1 percent is estimated. Individual
spots form within the active longitudes and show an angular velocity
~1 percent lower than that of the longitude pattern. The total spotted
area shows a cyclic oscillation with a period of 28.9 ± 4.3 days,
which is close to 10 times the synodic period of the planet as seen by
the rotating active longitudes. We discuss the effects of solar-like
faculae on our models, finding indications of a facular contribution
to the optical flux variations of CoRoT-Exo-2a being significantly
smaller than in the present Sun.
Conclusions: The implications of
such results for the internal rotation of CoRoT-Exo-2a are discussed,
based on solar analogy. A possible magnetic star-planet interaction is
suggested by the cyclic variation of the spotted area. Alternatively,
the 28.9-d cycle may be related to Rossby-type waves propagating in
the subphotospheric layers of the star. Based on observations
obtained with CoRoT, a space project operated by the French Space
Agency, CNES, with partecipation of the Science Programme of ESA,
ESTEC/RSSD, Austria, Belgium, Brazil, Germany, and Spain.
Title: ESA's Lunar Robotics Challenge
Authors: Visentin, G.; Foing, B.; Walker, R.; Galvez, A.
Bibcode: 2008LPICo1446..134V
Altcode:
No abstract at ADS
Title: SMART-1 Results and Lessons Learned for Preparing Future
Exploration
Authors: Foing, B. H.; Koschny, D.; Grieger, B.; Josset, J. -L.;
Beauvivre, S.; Grande, M.; Crawford, I.; Swinyard, B.; Huovelin, J.;
Alha, L.; Keller, H. U.; Mall, U.; Nathues, A.; Malkki, A.; Noci,
G.; Sodnik, Z.; Kellett, B.; Pinet, P.; Chevrel, S.; Cerroni, P.;
de Sanctis, M. C.; Barucci, M. A.; Erard, S.; Despan, D.; Muinonen,
K.; Naranen, J.; Shevchenko, V.; Shkuratov, Y.; Ellouzi, M.; Peters,
S.; Bexkens, F.; Borst, A.; Odum, C.; Boche-Sauvan, L.; Monaghan, E.;
Wills, D.; Almeida, M.; Frew, D.; Volp, J.; Heather, D.; McMannamon,
P.; Camino, O.; Racca, G.
Bibcode: 2008LPICo1446...55F
Altcode:
No abstract at ADS
Title: Addressing International Lunar Surface Operations
Authors: Lupisella, M.; Eppler, D.; Arnold, L.; Landis, R.; Gates, M.;
Hovland, S.; Foing, B.; Olds, J.; Depasquale, D.; Lewis, R.; Hyatt,
M.; Conley, C.; Mandl, D.; Talabac, S.; McNamara, K.; Perino, M. A.;
Alkalai, L.; Morrow, C.; Burke, J.
Bibcode: 2008LPICo1446...84L
Altcode:
No abstract at ADS
Title: High Resolution Maps of the Moon Surface with AMIE/SMART-1
Authors: Despan, D.; Erard, S.; Barucci, A.; Josset, J. -L.; Beauvivre,
S.; Chevrel, S.; Pinet, P.; Koschny, D.; Almeida, M.; Grieger, B.;
Foing, B. H.; Amie Team
Bibcode: 2008LPICo1446...48D
Altcode:
No abstract at ADS
Title: Astrobiology and Exposure Experiments from the Lunar Surface
Authors: Wills, D. E.; Foing, B.; Wills, H. H.
Bibcode: 2008LPICo1446..140W
Altcode:
No abstract at ADS
Title: Constraints on the Pre-Design of a Minimal Human Lunar Outpost
Authors: Boche-Sauvan, L.; Foing, B. H.
Bibcode: 2008LPICo1446...24B
Altcode:
No abstract at ADS
Title: Geological and Geochemical Study of South Pole-Aitken Basin
and Future Sample Return Missions
Authors: Borst, A. M.; Bexkens, F.; Foing, B. H.
Bibcode: 2008LPICo1446...26B
Altcode:
No abstract at ADS
Title: Report from ILEWG on Science and Exploration Questions
Authors: Foing, B. H.; International Lunar Exploration Working Group
Bibcode: 2008LPICo1446...54F
Altcode:
No abstract at ADS
Title: Astronomy from the Moon: Possible Science Investigations
and Precursors
Authors: Kissi-Ameyaw, J.; Monaghan, E. P.; Foing, B. H.
Bibcode: 2008LPICo1446...73K
Altcode:
No abstract at ADS
Title: Future Robotic Study of Lunar Basins: Goals for Geochemistry
and Geophysics
Authors: Peters, S. T. M.; Monaghan, M. P.; Foing, B. H.
Bibcode: 2008LPICo1446..103P
Altcode:
No abstract at ADS
Title: What Astrobiology Investigations are Needed and Possible on
the Moon?
Authors: Ehrenfreund, P.; Foing, B. H.
Bibcode: 2008LPICo1446...51E
Altcode:
No abstract at ADS
Title: Isostasy in lunar mascon areas: comparison between far side
and near side
Authors: Peters, S. T. M.; Foing, B. H.
Bibcode: 2008epsc.conf..133P
Altcode:
We have studied the isostatic response on mascon loading for impact
basins on the far side and near side to determine geophysical properties
and geodynamic processes on the Moon. We modeled the isostatic rebound
for Maria Orientale, Moscoviense and the South Pole Aitken Basin (far
side); Maria Humorum, Imbrium and Serenitates (near side). High positive
gravity anomalies on the Moon coincide with the low topography of impact
basins. It is currently accepted that this results from disruption of
the lithosphere by basin forming impacts that triggered superisostatic
uplift of the mantle. It has been observed that gravity anomalies
are lower in ancient basins as a function of time (Neumann et al.,
1998), which suggests that they are closer to isostatic equilibrium
than younger ones. Our numerical modeling includes basins of varying
ages and considers lateral variations of lithospheric properties such
as thickness and density. We used gravity data from the Clementine
mission and sample analyses from e.g. Apollo17 to determine input
values for our models. Clementine and SMART-1 images were studied for
comparison between structures on the lunar surface and those predicted
by models of mascon loading.
Title: High Resolution Maps of the Moon Surface with AMIE/SMART-1
Authors: Despan, Daniela; Erard, S.; Barucci, A.; Josset, J. L.;
Beauvivre, S.; Chevrel, S.; Pinet, P.; Koschny, D.; Almeida, M.;
Grieger, B.; Foing, B.; AMIE Team
Bibcode: 2008DPS....40.1301D
Altcode: 2008BAAS...40R.405D
The Advanced Moon micro-Imager Experiment (AMIE) on board the ESA
lunar mission Smart-1 has performed colour imaging of the lunar surface
using various filters in the visible and NIR range. This micro-camera
provided high resolution images of selected parts of the lunar surface,
including the North and South pole areas. Being give that the SMART-1
mission was in a 300km x 300km orbit with perilune over the South pole,
the coverage between the North and the South regions is different. The AMIE images were obtained using a tele-objective with 5.3° x
5.3° field of view and a sensor of 1024 x 1024 pixels. The output
images have resolution 45m/pixel at 500km, and are encoded with
10 bits/pixel. The data for the North pole were obtained at a much
higher altitude than the South pole data. From the 300 Km pericenter
altitude, the same field of view corresponds to a spatial resolution
about 27 m/pixel. The high resolution imaging of the Moon surface makes
possible detailed analysis of the morphological features and physical
characteristics of the lunar surface. In order to construct AMIE data
maps, systematic analysis and processing is being carried on using
the whole data set. Geometrical analysis of AMIE images relies on the
SPICE system: image coordinates are computed to get precise projection
at the surface, and illumination angles are computed to analyze the
photometric sequences. Using this method, high resolution mosaics were
constructed then compared to lower resolution Clementine UV-Vis and
NIR images. Maps of both North and South pole were obtained as well
as other regions of interest. Eventually, this method will be applied
in all areas where AMIE has provided high resolution observations of
the surface, typically a factor of 3 higher than the Clementine UV-Vis
camera. New results will be presented at the conference.
Title: Selecting a landing site of astrobiological interest for Mars
landers and sample return missions
Authors: Wills, D.; Monaghan, E.; Foing, B. H.
Bibcode: 2008epsc.conf..855W
Altcode:
Abstract The landscape of Mars, despite its apparent hostility to life,
is riddled with geological and mineralogical signs of past or present
hydrological activity. As such, it is a key target for astrobiological
exploration. There are, however, many factors that will need to be
considered when planning in-situ and sample return missions, if these
missions are indeed to adequately exploit the science potential of this
intriguing world. These will not only take into account the environment
of the landing site in terms of topography and ambient atmosphere etc.,
but also the geochemical make up of the surface regolith, evidence of
hydrological processes and various other considerations. The knowledge
base in all aspects of Martian science is being added to on an almost
daily basis, and the aim of this work is to combine data and studies to
nominate top priority landing locations for the search for evidence of
life on Mars. We report in particular on science and technical criteria
and our data analysis for sites of astrobiological interest. This
includes information from previous missions (such as Mars Express,
MGS, Odyssey, MRO and MER rovers) on mineralogical composition,
geomorphology, evidence from past water history from imaging and
spectroscopic data, and existence of in-situ prior information from
landers and rovers (concerning evidences for volatiles, organics
and habitability conditions). We discuss key mission objectives, and
assess what sort of sites should be targeted in the light of these. We
consider the accessibility of chosen locations, taking into account
difficulties presented in accessing the polar regions and other regions
of high altitude. We describe what additional measurements are needed,
and outline the technical and scientific operations requirements of
such in-situ landers and sample return missions. Approach In the first
step of this study we focus on the science objectives of in-situ and
sample return missions to Mars. We investigate the evidence for extinct
or extant life, propose a criteria for astrobiological interest, and
characterise landing sites in the light of this criteria. This first
step thus focuses on the question of where such missions should land,
and why. In the second step, we extend this analysis into utilising real
data to design mission scenarios for each of the proposed sites. This
further step takes into account the safety, instruments and payloads,
as well as the technological and engineering constraints of such
missions. In this way, the second step addresses the question of what
could be done, and how, once the landing sites have been chosen. In
the final step we conduct a comparative study of in-situ and sample
return missions with reference to the candidate sites.
Title: Selecting A Landing Site Of Astrobiological Interest For Mars
Landers And Sample Return Missions
Authors: Wills, Danielle; Monaghan, E.; Foing, B.
Bibcode: 2008DPS....40.1507W
Altcode: 2008BAAS...40..411W
The landscape of Mars, despite its apparent hostility to life, is
riddled with geological and mineralogical signs of past or present
hydrological activity. As such, it is a key target for astrobiological
exploration. The aim of this work is to combine data and studies
to select top priority landing locations for in-situ landers and
sample return missions to Mars. We report in particular on science and
technical criteria and our data analysis for sites of astrobiological
interest. This includes information from previous missions (such as Mars
Express, MGS, Odyssey, MRO and MER rovers) on mineralogical composition,
geomorphology, evidence from past water history from imaging and
spectroscopic data, and existence of in-situ prior information from
landers and rovers (concerning evidence for volatiles, organics
and habitability conditions). We discuss key mission objectives,
and consider the accessibility of chosen locations. We describe
what additional measurements are needed, and outline the technical
and scientific operations requirements of in-situ landers and sample
return missions to Mars.
Title: Geochemical analysis of units within the South Pole -
Aitken Basin
Authors: Borst, A. M.; Bexkens, F.; Foing, B. H.; Koschny, D.; Peters,
S. T. M.
Bibcode: 2008epsc.conf..129B
Altcode:
The South Pole - Aitken (SPA) Basin, situated on the southern
farside of the Moon, is of critical importance to unravelling the
composition and evolution of the Moon. This PreNectarian basin (
>3.9 Ga), measuring 2500 km in diameter with a depth of up to 12
km, is commonly alleged to have excavated deep into the lunar crust
(Fig. 1). Therefore the SPA Basin floor may provide a unique opportunity
to study deep seated lunar materials. However, rocks initially exposed
by the impact event have been heavily altered or hidden from view,
due to subsequent weathering and impact processes. Consequently the
identification of pristine SPA Basin floor material, which would provide
a new window into the lunar interior, has become severely complicated
[1]. Previous research using multispectral and gamma-ray data obtained
by the Clementine and Lunar Prospector missions revealed the localised
presence of noritic and gabbroic/troctolitic rocks, exposed underneath
the mixing regolith layer [2, 4]. Approach In this study we combine
structural and geochemical analyses of the SPA Basin. The research
presented here aims at improving mineralogical descriptions of mafic
rock types within the South Pole - Aitken Basin using a similar
approach as described by Tompkins and Pieters [2, 3]. Multispectral
data from Clementine ultraviolet/visible and near-infrared cameras are
used and processed in ENVI. The method relies on diagnostic shapes of
band absorptions for key mafic minerals olivine and high Ca-pyroxene,
in order to discriminate between geologic units of noritic, gabbroic
and troctolitic compositions. We synthesise our results with a
companion complementary study of the global geological structure of
the SPA Basin using Clementine altimetry and gravity data obtained by
LIDAR instruments (F. Bexkens et al., this conference). Based on both
mineralogical and structural analysis local mosaics of SMART-1 high
resolution AMIE images will be produced to provide improved geological
context for areas exposing deep crustal materials. In particular we will
discuss the Bhabha- Bose region located in central SPA Basin, which
has been previously proposed as a possible sample return landing site
[4, 5]. Ultimately this study aims to contribute to identifying target
areas of future sample return missions to ensure optimal scientific
gain. References [1] Jolliff, B.L., et al. (2002), LPSXXXIII, 1156 [2]
Pieters, C.M., et al. (1997) Geophysical Research Letters, 24, 1903-1906
[3] Tompkins, S., and Pieters, C.M. (1999). Meteor. Planet. Sci., 34(1),
25-41 [4] Pieters, C.M., et al. (2001) JGR, 106, 28,001- 28,022. [5]
Duke, M.B. (2003) Adv. Space. Res., 31, 2347- 2352. EPSC Abstracts,
Vol. 3, EPSC2008-A-00129, 2008 European Planetary Science Congress,
Author(s) 2008
Title: The global geological context and impact signatures in the
SPA basin
Authors: Bexkens, F. S.; Borst, A. M.; Foing, B. H.; Koschny, D.;
Peters, S. T. M.
Bibcode: 2008epsc.conf..130B
Altcode:
The giant South Pole - Aitken basin (SPA) is the largest recognised
impact structure in the solar system. The basin is located on the
far side of the moon and measures 3500 km in diameter, including the
outermost ringstructure [2]. It is believed to be one of the oldest
lunar structures, > 4 billion years [1]. Due to its old age and
maturity the SPA structure has been severely reworked, and primary
ejecta have been redistributed by later impacts. The smoothing effect
of later smaller impacts on original basin structure and topography
complicates studies of the primary impact signature of the basin
structure. Here, we combine Clementine and SMART-1 data to provide
additional constraints on the large-scale structure of the SPA impact
basin. The impact's outer ring is best developed on the north-eastern
side of the basin. Two possible explanations for this observation have
been brought forward: (1) The ring structure is simply best preserved
in this area because by chance it has not been reworked by later
impacts as extensively as the rest of the outer ring. (2) The SPA was
formed by an oblique impact of a low density body [2]. Such an impact
could also explain the extremely low depth-diameter ratio of the basin
[2]. Clementine LIDAR gravity and topography data are used to address
the large-scale structure of the South Pole - Aitken Basin. Using
the IDL and ENVI software gravity and topography profiles across the
SPA with different orientations have been produced and compared. The
results are also used to quantify the mass distribution as a result
of the basin forming impact and later impacts, to try and assess how
mass was distributed during and after the impact. The Clementine data
are augmented with mosaics of highresolution SMART-1 AMIE images to
improve on a detailed description of the geological context of the
SPA. One northsouth profile through the SPA will be compared with the
topography and gravity profiles. In a companion study (A.M. Borst et
al., this conference) Clementine UV/VIS and NIR images are employed to
constrain the geochemical signatures of exposed rock types within the
SPA Basin. A synthesis of our studies enables a comparison between
structure and mineralogical compositions / soil maturity, and may
lead to the identification of possible landing sites for future sample
return missions. References [1] Duke, M.B., 2003. Sample return from
the lunar south pole-aitken basin. Adv. Space. Res. Vol. 31, No. 11,
pp. 2347-2352. [2] Shevchenko, V.V., Chikmachev, V.I., Pugacheva,
S.G., 2007. Structure of the South Pole-Aitkan lunar basin. Solar
system research, Vol. 41, No 6, pp. 447-462.
Title: Large-scale spring deposits on Mars?
Authors: Rossi, Angelo Pio; Neukum, Gerhard; Pondrelli, Monica; van
Gasselt, Stephan; Zegers, Tanja; Hauber, Ernst; Chicarro, Agustin;
Foing, Bernard
Bibcode: 2008JGRE..113.8016R
Altcode: 2008JGRE..11308016R
We present a large-scale spring hypothesis for the formation of various
enigmatic light-toned deposits (LTDs) on Mars. Layered to massive LTDs
occur extensively in Valles Marineris, chaotic terrains, and several
large craters, in particular, those located in Arabia Terra. Most of
these deposits are not easily explained with either a single process or
multiple ones, either in combination or occurring sequentially. Spring
deposits can have a very wide range of internal facies and exhibit
complex architectural variations. We propose the concept of large-scale
spring deposits for explaining LTDs on Mars. Stable volcano-tectonic
settings, such as the ones typical on Mars, are compatible with a
large-scale, long-term, multistage formation of spring deposits. The
large-scale spring deposit model can explain the formation of LTDs with
a common process, although active in different times and locations,
compatible with coeval local or regional processes and deposits, such
as volcaniclastic ones. LTDs, if formed as spring deposits derived
from subsurface fluids, could potentially offer favorable conditions
both to life and to the fossilization of past life forms.
Title: SMART-1 highlights and relevant studies on early bombardment
and geological processes on rocky planets
Authors: Foing, B. H.; Racca, G. D.; Josset, J. L.; Koschny, D.;
Frew, D.; Almeida, M.; Zender, J.; Heather, D.; Peters, S.; Marini,
A.; Stagnaro, L.; Beauvivre, S.; Grande, M.; Kellett, B.; Huovelin,
J.; Nathues, A.; Mall, U.; Ehrenfreund, P.; McCannon, P.
Bibcode: 2008PhST..130a4026F
Altcode:
We present results from SMART-1 science and technology payload,
in the context of the Nobel symposium on 'Physics of Planetary
Systems'. SMART-1 is Europe' first lunar mission (Foing et al 2000 LPSC
XXXI Abstract #1677 (CDROM); Foing et al 2001 Earth, Moon Planets 85
86 523 31 Marini et al 2002 Adv. Space Res. 30 1895 900 Racca et al
2001 Earth Moon Planets 85 86 379 95, Racca et al 2002 Planet Space
Sci. 50 1323 37) demonstrating technologies for future science and
exploration missions, and providing advances in our understanding
of lunar origin and evolution, and general planetary questions. The
mission also contributes a step in developing an international program
of lunar exploration. The spacecraft, launched on 27 September 2003
as an Ariane 5 Auxiliary passenger to geostationary transfer orbit
(GTO), performed a 14-month long cruise using a tiny thrust of
electric propulsion alone, reached lunar capture in November 2004,
and lunar science orbit in March 2005. SMART-1 carried 7 hardware
experiments (Foing et al 2003 Adv. Space Res. 31 2323, Foing et al 2005
LPI/LPSC XXXVI 2404 (CDROM)) performing 10 investigations, including
3 remote-sensing instruments, used during the cruise, the mission'
nominal six-months and one-year extension in lunar science orbit. Three
remote sensing instruments, D-CIXS, SIR and AMIE, have returned data
that are relevant to a broad range of lunar studies. The mission
provided regional and global x-ray measurements of the Moon, global
high-spectral resolution NIR spectrometry, high spatial resolution
colour imaging of selected regions. The South Pole-Aitken Basin (SPA)
and other impact basins have been prime targets for studies using
the SMART-1 suite of instruments. Combined, these should aid a large
number of science studies, from bulk crustal composition and theories
of lunar origin/evolution, the global and local crustal composition,
to the search for cold traps at the lunar poles and the mapping of
potential lunar resources. We present here SMART-1 results relevant
to the study of the early bombardment and geological processes on
rocky planets. Further information and updates on the SMART-1 mission
can be found on the ESA Science and Technology web pages, at: http://sci.esa.int/smart-1/.
Title: ICEUM9 Highlights and Sorrento Lunar Declaration 2007
Authors: Foing, B. H.; Iceum9 Participants
Bibcode: 2008LPICo1415.2099F
Altcode:
We report the highlights from ICEUM9, 9th ILEWG International
Conference on the Exploration and Utilization of the Moon (Sorrento,
Italy, 23-27 July 2006) and present the "Sorrento Lunar Declaration"
endorsed unanimously by the participants (http://sci.esa.int/iceum9).
Title: Journey to the Moon: Recent results, science, future robotic
and human exploration
Authors: Foing, Bernard H.; Ehrenfreund, Pascale
Bibcode: 2008AdSpR..42..235F
Altcode:
The upcoming fleet of lunar missions, and the announcement of
new lunar exploration initiatives, show an exciting "Journey to
the Moon", covering recent results, science, future robotic and
human exploration. We review some of the questions, findings and
perspectives given in the papers included in this issue of Advances
in Space Research.
Title: ICEUM8 Highlights and Beijing Lunar Declaration 2006
Authors: Foing, B. H.; Iceum8 Participants
Bibcode: 2008LPICo1415.2106F
Altcode:
We report the highlights from ICEUM8, the 8th ILEWG International
Conference on the Exploration and Utilization of the Moon (ICEUM8,
Beijing 23-27 July 2006) and present the "Beijing Lunar Declaration"
endorsed unanimously by the participants.
Title: Beijing Lunar Declaration 2006
Authors: Foing, B. H.; Wu, J.; Iceum8 Participants
Bibcode: 2008AdSpR..42..244F
Altcode:
We report to COSPAR the "Lunar Beijing Declaration" from the
participants to The Eighth ILEWG International Conference on
the Exploration and Utilization of the Moon (ICEUM8, 23-27
July 2006). Further information can be found on ILEWG website
http://sci.esa.int/ilewg and selected 38 proceedings papers have been
published in Journal of Astronautics of Chinese Society of Astronautics,
vol. 28, Suppl., 2007.
Title: Sorrento Lunar Declaration 2007
Authors: Foing, B. H.; Espinasse, S.; Wargo, M.; di Pippo, S.;
Iceum9 Participants
Bibcode: 2008AdSpR..42..246F
Altcode:
We report to COSPAR the "Sorrento Lunar Declaration" from the
participants to the Ninth ILEWG International Conference on the
Exploration and Utilisation of the Moon (ICEUM9, Sorrento, Italy,
23-27 July 2006). Further information, abstracts and presentations
can be found on ILEWG website http://sci.esa.int/ilewg and the
conference website http://sci.esa.int/iceum9 [Foing, B., Kosters, G.,
Espinasse, S., Del Vecchio Blanco, C., Sangiovanni, G., Salatti,
M. (Eds.), Programme and Abstracts, Ninth ILEWG International
Conference on Exploration and Utilisation of the Moon, 22-26 October
2007, Sorrento, Italy, 2007; Foing, B., Espinasse, S., Kosters,
G. (Eds.), Proceedings of the Ninth ILEWG International Conference
on Exploration and Utilisation of the Moon. Available online:
<http://sci.esa.int/iceum9>, ESA/ASI/ILEWG December, 2007].
Title: Toronto Lunar Declaration 2005
Authors: Foing, B. H.; Richards, R.; Sallaberger, C.; Iceum7
Participants
Bibcode: 2008AdSpR..42..242F
Altcode:
We report to COSPAR the "Toronto Declaration" from the participants
to Seventh ILEWG International Conference on the Exploration and
Utilization of the Moon (ICEUM7, 18-23 September 2005). Further
information can be found on the ILEWG website http://sci.esa.int/ilewg.
Title: Udaipur Lunar Declaration 2004
Authors: Foing, B. H.; Bhandari, N.; Goswami, J. N.; Iceum6
Participants
Bibcode: 2008AdSpR..42..240F
Altcode:
We report to COSPAR the "Udaipur Declaration" from the participants of
Sixth ILEWG International Conference on the Exploration and Utilization
of the Moon (ICEUM6, 22-26 November 2004). Further information can be
found on the ILEWG website http://sci.esa.int/ilewg and publications in
the Journal of Earth System Science [Bhandari, N. (Ed.), Proceedings
of the International Conference on Exploration and Utilization of
the Moon 22-26 November 2004, Udaipur, Rajasthan, India. J. Earth
Syst. Sci. 114(6), 573-841, 2005].
Title: Reports to COSPAR from the International Lunar Exploration
Working Group (ILEWG)
Authors: Foing, Bernard H.
Bibcode: 2008AdSpR..42..238F
Altcode:
In accordance with its charter, the International Lunar Exploration
Working Group (ILEWG) reports to COSPAR, and a summary was given at
the Beijing COSPAR 2006 Assembly on ILEWG activities conducted since
the previous COSPAR 2004 assembly held in Paris. This included reports
from the 6th and 7th ILEWG International Conference on Exploration and
Utilization of the Moon, held respectively in Udaipur, India on 22-26
November 2004 (ICEUM6) and in Toronto, Canada on 18-23 September 2005
(ICEUM7). We give in this issue of Advances in Space Research the
"lunar declarations" from these ICEUM conferences, as well as for the
ICEUM8 conference held in Beijing immediately after the 2006 COSPAR
Assembly. One year after the COSPAR Beijing assembly, the 9th ILEWG
International Conference on Exploration and Utilization of the Moon
(ICEUM9), was held in Sorrento, Italy on 18-23 September 2007. We
report also in this issue the "Sorrento Lunar Declaration" in advance
of the ILEWG formal report to be given at the COSPAR Assembly to be
held in Montreal, Canada in July 2008.
Title: SMART-1 Lunar Highlights: Impact Craters, Basins, Tectonics
and Volcanism
Authors: Foing, B. H.; Grieger, B.; Josset, J. -L.; Beauvivre, S.;
Grande, M.; Huovelin, J.; Keller, H. U.; Mall, U.; Nathues, A.;
Malkki, A.; Noci, G.; Sodnik, Z.; Kellett, B.; Pinet, P.; Chevrel,
S.; Cerroni, P.; de Sanctis, M. C.; Barucci, M. A.; Erard, S.; Despan,
D.; Muinonen, K.; Shevchenko, V.; Shkuratov, Y.; Ellouzi, M.; Peters,
S.; Bexkens, F.; Borst, A.; Odum, C.; Boche-Sauvan, L.; Almeida, M.;
Frew, D.; Volp, J.; Heather, D.; McMannamon, P.; Camino, O.; Racca, G.
Bibcode: 2008LPICo1415.2079F
Altcode:
We shall report at the Lunar Science Workshop 2008 on SMART-1 lunar
highlights relevant for science and exploration, with emphasis on
impact craters, basins, tectonics and volcanism.
Title: Report from ILEWG to the Lunar Science Workshop 2008
Authors: Foing, B. H.; International Lunar Exploration Working Group
Bibcode: 2008LPICo1415.2090F
Altcode:
We report on activities from ILEWG, the International Lunar Exploration
Working Group, created in 1994, by the world's space agencies to support
"international cooperation towards a world strategy for the exploration
and utilization of the Moon".
Title: Astrobiology, Habitability and the Moon
Authors: Ehrenfreund, P.; Foing, B. H.
Bibcode: 2008LPICo1415.2133E
Altcode:
Lunar exploration provides a high potential to foster the objectives
of astrobiology. We review how to acquire knowledge to make the Moon
habitable (using advanced and sustained technological support), and
expand life beyond Earth planet of origin.
Title: SMART-1/Clementine Study of Humorum, Procellarum and South-Pole
Aitken Basins: Coupling Between Impacts, Volcanism and Tectonics
Authors: Peters, S. T.; Foing, B. H.; Borst, A.; Bexkens, F.; Koschny,
D.; Rossi, A.; Josset, J. L.; Beauvivre, S.; SMART-1 Amie Team
Bibcode: 2008LPICo1415.2115P
Altcode:
We have combined SMART-1 AMIE camera images with Clementine UV/VIS data
for three lunar basins (Mare Humorum, Oceanus Procellarum and South
Pole-Aitken Basin), to determine the coupling between basin origin,
tectonics and volcanism.
Title: A Cryogenic Liquid-Mirror Telescope on the Moon to Study the
Early Universe
Authors: Angel, Roger; Worden, Simon P.; Borra, Ermanno F.; Eisenstein,
Daniel J.; Foing, Bernard; Hickson, Paul; Josset, Jean-Luc; Bui Ma, Ki;
Seddiki, Omar; Sivanandam, Suresh; Thibault, Simon; van Susante, Paul
Bibcode: 2008ApJ...680.1582A
Altcode: 2008arXiv0806.2241A
We have studied the feasibility and scientific potential of zenith
observing liquid-mirror telescopes having 20-100 m diameters located
on the Moon. They would carry out deep infrared surveys to study the
distant universe and follow up discoveries made with the 6 m James Webb
Space Telescope (JWST), with more detailed images and spectroscopic
studies. They could detect objects 100 times fainter than JWST,
observing the first high-redshift stars in the early universe and their
assembly into galaxies. We explored the scientific opportunities,
key technologies, and optimum location of such telescopes. We have
demonstrated critical technologies. For example, the primary mirror
would necessitate a high-reflectivity liquid that does not evaporate
in the lunar vacuum and remains liquid at less than 100 K. We have
made a crucial demonstration by successfully coating an ionic liquid
that has negligible vapor pressure. We also successfully experimented
with a liquid mirror spinning on a superconducting bearing, as will
be needed for the cryogenic, vacuum environment of the telescope. We
have investigated issues related to lunar locations, concluding
that locations within a few kilometers of a pole are ideal for deep
sky cover and long integration times. We have located ridges and
crater rims within 0.5° of the north pole that are illuminated for
at least some sun angles during lunar winter, providing power and
temperature control. We also have identified potential problems, like
lunar dust. Issues raised by our preliminary study demand additional
in-depth analyses. These issues must be fully examined as part of a
scientific debate that we hope to start with the present article.
Title: Lunar landers and sample return: science and technologies
Authors: Foing, Bernard H.
Bibcode: 2008SPIE.6960E..09F
Altcode: 2008SPIE.6960E...7F
We review in the context of latest lunar results the case for future
lunar landers and sample returns, as discussed by various ILEWG science
and technology task groups, addressing: - ESA Lunar Polar Lander Study
(LES3) - A generic lander platform that can be adapted to sample return
or to a lunar lander /rover fetcher. - New Science opportunities from
lunar landers - Clues on mantle/lower crust (South Pole Aitken Basin),
polar ice, cometary/meteoritic record - Technology demonstration
preparation for Mars sample return - Technology demonstrator for lunar
ascent vehicle, Earth reentry, and human return vehicle Technologies
that can be developed for lunar sample return missions: entry airless
bodies, Descent and landing, robotics, Instruments, Sample acquisition,
Return and Earth reentry.
Title: SMART-1 results and future lunar exploration
Authors: Foing, Bernard H.
Bibcode: 2008SPIE.6960E..07F
Altcode: 2008SPIE.6960E...5F
We present some highlights from SMART-1's science and technology
payload, and the relevance of SMART-1 results and lessons for future
lunar exploration. SMART-1 is the first ESA mission that reached the
Moon. It is the first of Small Missions for Advanced Research and
Technology. It has fulfilled its technology objectives to demonstrate
Solar Electric Primary Propulsion (SEP) and to test new technologies
for spacecraft and instruments. After a 15-month cruise with primary
SEP and successful technology demonstration, the SMART-1 science and
exploration phase, provided first lunar orbit results. The mission
has been extended one year and ended with an impact on 3 September 2006.
Title: ILEWG technology roadmap for Moon exploration
Authors: Foing, Bernard H.
Bibcode: 2008SPIE.6960E..08F
Altcode: 2008SPIE.6960E...6F
We discuss the charter and activities of the International Lunar
Exploration Working Group (ILEWG), and give an update from the
related ILEWG task groups. We discuss the different rationale and
technology roadmap for Moon exploration, as debated in previous ILEWG
conferences. The Technology rationale includes: 1) The advancement of
instrumentation: 2) Technologies in robotic and human exploration 3)
Moon-Mars Exploration can inspire solutions to global Earth sustained
development. We finally discuss a possible roadmap for development of
technologies necessary for Moon and Mars exploration.
Title: SMART-1 Lunar Highlights
Authors: Foing, B. H.; Koschny, D.; Grieger, B.; Josset, J. -L.;
Beauvivre, S.; Grande, M.; Huovelin, J.; Keller, H. U.; Mall, U.;
Nathues, A.; Malkki, A.; Noci, G.; Sodnik, Z.; Kellett, B.; Pinet,
P.; Chevrel, S.; Cerroni, P.; de Sanctis, M. C.; Barucci, M. A.; Er
Bibcode: 2008LPI....39.1987F
Altcode:
We report on SMART-1 lunar highlights results relevant for science
and exploration. We address impact and volcanic processes. We analyse
images of lunar north and south poles, for the characterisation of
sites for future landers, rovers, and human bases.
Title: SMART-1 Lunar Science Planning
Authors: Koschny, D.; Foing, B. H.; Frew, D.; Grieger, B.; Almeida,
M.; Sarkarati, M.; Volp, J.; Josset, J. -L.; Beauvivre, S.; Grande,
M.; Huovelin, J.; Nathues, A.; Malkki, A.; Noci, G.; Kellett, B.;
Heather, D. J.; Zender, J.; McMannamon, P.; Schwehm, G.; Camino
Bibcode: 2008LPI....39.2282K
Altcode:
The SMART-1 spacecraft reached on 15 March 2005 a lunar orbit 400-3000
km for a nominal science period of six months, with a one year science
extension until impact on 3 September 2006. We report on the SMART-1
science planning methods, tools, and lessons learned.
Title: Coverage and Pointing Accuracy of SMART-1/AMIE Images
Authors: Grieger, B.; Foing, B. H.; Koschny, D.; Josset, J. L.;
Beauvivre, S.; Frew, D.; Almeida, M.; Sarkarati, M.; Volp, J.; Pinet,
P.; Chevrel, S.; Cerroni, P.; de Sanctis, M. C.; Barucci, M. A.;
Erard, S.; Despan, D.; Muinonen, K.; Shevchenko, V.; Shkuratov, Y.
Bibcode: 2008LPI....39.2221G
Altcode:
During 18 months of science operations from 400-3000 km lunar orbit,
the AMIE camera onboard the SMART-1 spacecraft acquired about 32,000
images. We report on the coverage at various resolutions (until 50
m/pixel) and the pointing accuracy.
Title: SMART-1/Clementine Study of Humorum and Procellarum Basins:
Coupling Between Impacts, Volcanism and Tectonics
Authors: Peters, S. Tm.; Foing, B. H.; Koschmy, D.; Rossi, A. P.;
Josset, J. L.; Beauvivre, S.; SMART-1 Amie Team
Bibcode: 2008LPI....39.2548P
Altcode:
We combined SMART-1 AMIE and Clementine UV/VIS data for two end-member
lunar basins to determine the coupling between basin and tectonics. For
Humorum but not Procellarum, tectonic-induced features agree well with
an idealized tectonic model.
Title: The Opposition Effect of the Moon from SMART-1 AMIE Data
Authors: Kaydash, V.; Kreslavsky, M. A.; Shkuratov, Yu.; Gerasimenko,
S.; Pinet, P.; Chevrel, S.; Josset, J. -L.; Beauvivre, S.; Foing,
B. H.; Amie SMART-1 Team
Bibcode: 2008LPI....39.1195K
Altcode:
Images obtained by the AMIE camera onboard SMART-1 spacecraft allow
access to low-phase-angle data. We use AMIE data to study the opposition
spike for lunar sites and estimate the steepness of phase function in
the phase angle range 0°-2.5°.
Title: Coverage, resolution, and calibration of SMART-1/AMIE images
Authors: Bjoern, Grieger; Foing, Bernard H.; Almeida, Miguel;
Beauvivre, Stephane; Josset, Jean-Luc; Koschny, Detlef; Dougnac,
Virgile; Martinez, Santa
Bibcode: 2008cosp...37..310B
Altcode: 2008cosp.meet..310B
The SMART-1 spacecraft was launched on 27 September 2003 end reached
its lunar baseline science orbit on 13 March 2005 for a nominal
science period of six months and one year extension. During these
18 months, the AMIE camera aboard the spacecraft acquired about 32
000 images. SMART-1 operated in an eccentric polar orbit with the
perilune close to the South pole at a minimum distance of 400 km and
an apolune distance of about 6400 km. The small but scientifically
quite interesting area south off 87° S and various spots in the
southern hemisphere are covered by the AMIE camera with a resolution
better than 50 meters per pixel. The complete Southern hemisphere is
covered with a resolution better than 100 meters per pixel. Finally,
global coverage is achieved with a resolution better than 250 meters
per pixel. Each AMIE image frame of 1024 × 1024 pixels is divided
into areas covered by four different filters and one area of 512 × 512
pixels which is uncovered. First inspections of the images had revealed
that the dark current of the CCD increased significantly during the
cruise phase when the space craft crossed the radiation belt several
times. Therefore, the dark frames acquired in the laboratory prior
to the mission are not adequate to perform the dark correction. From
the analysis of dark sky images taken during the lunar phase of the
mission, new master dark frames were estimated which have been used
to calibrate the images. We discuss the calibration of AMIE images
and present examples from different regions of the lunar surface.
Title: ILEWG roadmap Robotic and Human Lunar Exploration
Authors: Foing, Bernard H.
Bibcode: 2008cosp...37..906F
Altcode: 2008cosp.meet..906F
We shall discuss the rationale and roadmap of ongoing Moon missions, and
how they can prepare for future human exploration. Various fundamental
scientific investigations can be performed with robots and humans:
clues on the formation and evolution of rocky planets, accretion
and bombardment in the inner solar system, comparative planetology
processes (tectonic, volcanic, impact cratering, volatile delivery),
records astrobiology, survival of organics; past, present and future
life. The roadmap includes also enabling technologies that prepare
for the best syenrgies between robots and humans: Remote sensing
miniaturised instruments; Surface geophysical and geochemistry
package;Instrument deployment and robotic arm, nano-rover, sampling,
drilling; Sample finder and collector, Support equipment for astronaut
sorties; life science precursors for life support systems. We shall
adddress requirements for robotic precursor programmes, global robotic
village, technology development, resource utilisation, human aspects,
science and exploration from lunar sorties, transition towards permanent
settlements and lunar bases.
Title: Microbial community induces a plant defense system under
growing on the lunar regolith analogue
Authors: Zaetz, Irina; Mytrokhyn, Olexander; Lukashov, Dmitry;
Mashkovska, Svitlana; Kozyrovska, Natalia; Foing, Bernard H.
Bibcode: 2008cosp...37.3584Z
Altcode: 2008cosp.meet.3584Z
The lunar rock considered as a potential source of chemical elements
essential for plant nutrition, however, this substrate is of a low
bioavailability. The use of microorganisms for decomposition of silicate
rocks and stimulation of plant growth is a key idea in precursory
scenario of growing pioneer plants for a lunar base (Kozyrovska et al.,
2004; 2006; Zaetz et al., 2006). In model experiments a consortium
of well-defined plant-associated bacteria were used for growing of
French marigold (Tagetes patula L.) in anorthosite, analogous to
a lunar rock. Inoculated plants appeared better seed germination,
more fast development and also increased accumulation of K, Mg,
Mn, Co, Cu and lowered level of the toxic Zn, Ni, Cr, comparing to
control tagetes'. Bacteria regulate metal homeostasis in plants by
changing their bioavailability and by stimulating of plant defense
mechanisms. Inoculated plants were being accommodated to growth under
stress conditions on anorthosite used as a substrate. In contrast,
control plants manifested a heavy metal-induced oxidative stress,
as quantified by protein carbonyl accumulation. Depending on the
plant organ sampled and developmental stage there were increases
or loses in the antioxidant enzyme activities (guaiacol peroxidase
and glutathione-S-transferase). These changes were most evident
in inoculated plants. Production of phenolic compounds, known as
antioxidants and heavy metal chelators, is rised in variants of
inoculated marigolds. Guaiacol peroxidase plays the main role,
finally, in a reducing toxicity of heavy metals in plant leaves,
while glutathione-S-transferase and phenolics overcome stress in roots.
Title: Photometric study of the Moon with SMART-1/AMIE
Authors: Naranen, Jyri; Parviainen, Hannu; Muinonen, Karri; Josset,
Jean-Luc; Beauvivre, Stephane; Koschny, Detlef; Foing, Bernard H.;
Krieger, Bjoern; Amie Team
Bibcode: 2008cosp...37.2178N
Altcode: 2008cosp.meet.2178N
The Advanced Moon micro-Imager Experiment (AMIE) onboard the ESA
SMART-1 lunar mission performed imaging of the Moon between November
2004 and September 2006, when the mission was ended by crashing
the spacecraft into the lunar surface. AMIE was a 1024X1024 pixel
miniaturized CCD camera with three colour filters and a panchromatic
channel (clear filter). The images are of medium-to-high resolution,
e.g. at 300 km pericenter altitude the resolution was 27 m/pix. We
selected four different regions on the lunar surface imaged by
AMIE for the photometric investigation reported here. These regions
were selected so that as large phase angle coverage as possible was
available, including the opposition geometry. Each of the regions
cover a few hundred square kilometers of the lunar surface and were
imaged by AMIE several tens of times. The regions examined include,
e.g., Reiner gamma and Oceanus Procellarum near the crater Mairan. We
utilized the latest in-flight calibration data available and we also
georetrified the images to account for the aspect distortions. For
the study reported here, the panchromatic filter was chosen since it
is the best calibrated channel at the moment. The data was analyzed
by implementing a numerical light scattering model with which we
have inverted the regolith porosity and macroscopic surface roughness
properties for the target areas. The model computes the bidirectional
reflectance function using the geometric-optics approximation from a
particulate medium constrained by a self-affine fractal random fields
mimicking the regolith-covered lunar surface. Fractal description
of the surface roughness is used, since it gives a more realistic
way to model the true macroscopic surface roughness than the often
used Gaussian correlation-model. Unlike in the previous studies, the
azimuthal shadowing effects are taken into account, allowing for a more
reliable inversion of surface statistics from images with large phase
angles. In addition, we have fitted an empirical photometric function
to the data which can be used to perform photometric correction to the
images in, e.g., image mosaicking. A comparison with the results from
the relevant previous photometric studies of the Moon is given. We
end by presenting plans for future studies, especially the possible
multi-colour photometry.
Title: Diffuse Interstellar Bands and Complex Organics
Authors: Foing, Bernard H.; Ehrenfreund, Pascale; Cox, Nick
Bibcode: 2008cosp...37..904F
Altcode: 2008cosp.meet..904F
The origin of Diffuse Interstellar Bands (Herbig 1995), more than 300 in
recent surveys (O' Tuairisg et al 2000) is still a mystery. However the
measurements of sub-structures rotational contours in DIBs (Ehrenfreund
Foing 1996) indicate large molecules such as chains (12-18C), rings,
50 C PAHs or fullerenes. The distribution of DIB widths permit to
estimate a distribution of size of molecular carriers. The environment
properties of DIB carriers also indicate ionisation potentials similar
to those of cations of large carbonaceous molecules, such as large PAHs
or fullerenes (Sonnentrucker et al 1997). The correlation studies of
DIBS also indicate different carriers for the strong DIBs observed in
the visible (Cami et al 1997). Polarisation studies could also give
constraints on the carriers (Cox et al 2007). DIBS are weakened in
the low-metallicity Magellanic clouds (Ehrenfreund et al 2002, Cox
et al 2006, 2007). The detection of near IR bands at 9577 and 9632
A coinciding with laboratory transitions of C60+ (Foing, Ehrenfreund
1994, 1997) suggest that significant interstellar carbon could reside
in complex fullerene type compounds or PAHs. We report on new CFHT
Espadons observations of the C60+ and other diffuse bands.
Title: High Resolution North and South Polar Maps of the Moon with
AMIE/SMART-1
Authors: Despan, Daniela; Erard, Stephane; Beauvivre, Stephane;
Chevrel, Serge; Pinet, Patrick; Almeida, Miguel; Grieger, Bjoern;
Cerroni, Priscilla; Barucci, M. A.; Josset, Jean-Luc; Koschny, Detlef;
Foing, Bernard H.
Bibcode: 2008cosp...37..703D
Altcode: 2008cosp.meet..703D
The northern and southern polar areas maps of the Moon are obtained by
processing and mosaiking of the AMIE, SMART-1 images. The Advanced Moon
micro-Imager Experiment (AMIE) on board the ESA lunar mission Smart-1
has performed colour imaging of the lunar surface using various filters
in the visible and NIR. The low pericenter, polar orbit, allowed to
obtain high resolution images in various locations at the surface. From
the 300 km pericenter altitude, the field of view (5,3° x5,3° )
corresponds to a spatial resolution about 30 m. The 1024x1024 images
are shared by the various filters, allowing to derive mosaics of the
surface in up to 3 colors depending on pointing mode. Spot-pointing
observations and multiple observations from different orbits have
provided photometric sequences that allow to study the surface
properties in restricted areas. Geometrical analysis of the AMIE
images relies on the SPICE system: image coordinates are computed to
get precise projection at the surface, and illumination angles are
computed to analyze the photometric sequences. Images from various
orbits are first identified for each selected region of interest. These
images are then selected according to signal to noise ratio, spatial
coverage, and spatial resolution. The best images obtained with the
neutral filter are calibrated, and mosaicked using the coordinates of
the image frames corners. In the polar areas, images are selected so as
to provide the best possible viewing of surface topography, depending
on solar illumination angle, while preserving images continuity in
shadowed areas. The maps of other regions of interest are yielded:
Marius Hills, the Gruitheisen Domes, Rumker Hills, Aristarchus
Plateau. Eventually, this method will be applied in all regions
where AMIE has provided high resolution observations of the surface,
typically a factor of 3 higher than the Clementine UV-vis camera. These
regions are essentially located at latitude ranging from 80 to 40° S,
specially in the eastern hemisphere.
Title: Search for Mars climatic signal in Pavonis Mons Fan &
other periglacial deposits
Authors: Foing, Bernard H.; Forget, Francois; Pio Rossi, Angelo;
Head, James; Neukum, Gerhard
Bibcode: 2008cosp...37..903F
Altcode: 2008cosp.meet..903F
Mars has experienced large variations in its orbital parameters
through-out its history. They are calculable for the last 10
million years, with periodicity of 120 000 years for its obliquity,
95 to 100,000 years for its excentricity, and 51,000 years for its
precession, however they become undetermined beyond 20 Myr . Laskar
et al determined a standard model of Mars' insolation parameters over
4 Gyr with the most probable values 0.068 for the eccentricity and
41.80 degrees for the obliquity. At high obliquity, signicant amount
of ice can be deposited as ice at low latitudes. This can be relevant
for understanding features from the modern Polar Layered Deposits, the
Elysium frozen sea (Murray et al 2005),or Ellas hourglass (Head et al
2005). General circulation models predict an annual net accumulation
rate of ice on the west of Tharsis volcanoes. We analysed Mars Express
images obtained over orbit 946, of the west fan deposit at Pavonis
Mons. The analysis of the HRSC images shows around 15 ridges, with
interval 0.5 -4.5 km. The interaction with the under-lying surface
can be seen, indicating the overlap of different episodes. The
ridges are interpreted as drop debris on the front edge of a cold
glaciar during its slow retreat. On the other hand isotropic knobbies,
circular sub-kmscale hills are interpreted as results of fast glaciar
sublimation. By texture analysis we could distinguish ridges, knobbies
from various episodes and relate them with geological studies. For
this basic study, we choose the simplest model of glacier profile. The
bed is believed to be horizontal, and does not interfere with the
glacier. If the ridges are due to obliquity oscillation, the rate of
snow fall and sublimation depend strongly on obliquity. Indeed, with
the balance of accumulation rates and ablation rates, we can predict
oscillations of the glacier extent. We discuss how this can be used
to serach for Martian climatic signal.
Title: Synthesis of SMART-1 lunar results: Science and Exploration
Authors: Foing, Bernard H.
Bibcode: 2008cosp...37..907F
Altcode: 2008cosp.meet..907F
We shall give a synthesis on SMART-1 lunar highlights relevant for
science and exploration. The SMART-1 spacecraft reached on 15 March 2005
a lunar orbit 400-3000 km for a nominal science period of six months,
with 1 year extension until impact on 3 September 2006. SMART-1 lunar
science investigations include studies of the chemical composition of
the Moon, of geophysical processes (volcanism, tectonics, cratering,
erosion, deposition of ices and volatiles) for comparative planetology,
and high resolution studies in preparation for future steps of
lunar exploration. The mission addresses several topics such as the
accretional processes that led to the formation of rocky planets, and
the origin and evolution of the Earth-Moon system. SMART-1 AMIE camera
has been used to map sites of interest that are relevant to the study
of cataclysm bombardment, and to preview future sites for sampling
return. Lunar North polar maps and South pole repeated high resolution
images have been obtained, giving a monitoring of illumination to
map potential sites relevant for future exploration. The SMART-1
observations have been coordinated with upcoming missions. SMART-1
has been useful in the preparation of Selene Kaguya, the Indian lunar
mission Chandrayaan-1, Chinese Chang'E 1 , the US Lunar Reconnaissance
Orbiter, LCROSS, and subsequent lunar landers. SMART-1 is contributing
to prepare the next steps for exploration: survey of resources,
search for ice, monitoring polar illumination, and mapping of sites
for potential landings, international robotic villages and for future
human activities and lunar bases.
Title: SMART-1/CLEMENTINE Study of Humorum and Procellarum Basins
Authors: Carey, William; Foing, Bernard H.; Koschny, Detlef; Pio Rossi,
Angelo; Josset, Jean-Luc
Bibcode: 2008cosp...37..457C
Altcode: 2008cosp.meet..457C
A study undertaken by ESA to define a European Reference Architecture
for Space Exploration is due to be completed in September 2008. The
development of this architecture over the past twelve months has
identified a number of key capabilities, among them a lunar lander
system, which could form the basis for Europe's contribution to
the future exploration of space in collaboration with International
Partners. The focus of this paper will be on the lunar lander system,
and will present the results of an analysis of possible payloads that
could be accommodated by the lander. As the industrial study is at
the Phase 0 or Pre-Phase A level, the design of such a lander system
is at a very early stage in its development, but an estimation of the
payload capacity allows a general assessment of the types of possible
payloads that could be carried, currently this capacity is estimated
at 1.1 tonnes of gross payload mass to the lunar surface (assuming an
Ariane 5 ECA launch). An important characteristic of the lunar lander
is that it provides a versatile and flexible system for utilisation
in a broad range of lunar missions which include: - Independent
lunar exploration missions for science, technology demonstration and
research. - Delivery of logistics and cargo to support human surface
sortie missions. - Delivery of logistics to a lunar base/outpost. -
Deployment of individual infrastructure elements in support of a
lunar base/outpost. Based on the above different types of missions,
a number of configurations of "reference payload" sets are in the
process of being defined that cover specific exploration objectives
related primarily to capability demonstration, exploration enabling
research and enabled science. Aspects covered include: ISRU, robotics,
mobility, human preparation, life science and geology. This paper will
present the current status of definition of the Reference Payload sets.
Title: SMART-1 Moon impact on 3 Sept 2006: results from observation
campaign
Authors: Foing, Bernard H.
Bibcode: 2008cosp...37..905F
Altcode: 2008cosp.meet..905F
SMART-1 was launched in 2003 and orbited the Moon on a 5 hours period
until impact on 3 sept 2006. A controlled impact took place in grazing
incidence with mass of 285 kg at a velocity of 2 km/s in the Lake
of Excellence. We called the community to make predictions of impact
magnitude, cloud ejecta dynamics, exospheric effects. We also called
the ground based observers to perform coordinated measurements of
the impact. We shall discuss results from the coordinated multi-site
campaign, in particular observations from CFHT of the flash impact
and debris clouds. We shall draw lessons for future lunar impacts
including LCROSS.
Title: Lunar landers and sample return: science and exploration
Authors: Foing, Bernard H.
Bibcode: 2008cosp...37..908F
Altcode: 2008cosp.meet..908F
We present the results of a study for a lunar polar lander conducted at
ESA CDF Concurrent Design Facility and follow up activities. The goal
is to demonstrate lunar landing, survival and exploration technologies
for the future, geochemical studies of the piles, and search for
ice in permanent shadows. We describe the top objectives, mission
analysis, design and associated lander and rover. We also describe
the possible payload complement in discussion with the community. We
also describe the rationale for Lunar Sample Return missions, and
give some concept studies. Finally, we discuss the required advances
in planetary robotics, required for both the polar lunar lander and
for the sample return missions.
Title: Surface roughness and geological mapping at subhectometer
scale from the High Resolution Stereo Camera onboard Mars Express
Authors: Cord, Aurélien; Baratoux, David; Mangold, Nicolas; Martin,
Patrick; Pinet, Patrick; Greeley, Ronald; Costard, Francois; Masson,
Philippe; Foing, Bernard; Neukum, Gerhard
Bibcode: 2007Icar..191...38C
Altcode:
The quantitative measurement of surface roughness of planetary
surfaces at all scales provides insights into geological processes. A
characterization of roughness variations at the scale of a few
tens of meters is proposed that complements the analysis of local
topographic data of the martian surface at kilometer scale, as
achieved from the Mars Orbiter Laser Altimeter (MOLA) data, and at
the subcentimeter scale using photometric properties derived from
multi-angular observations. Relying on a Gabor filtering process,
an algorithm developed in the context of image classification for
the purpose of texture analysis has been adapted to handle data from
the High Resolution Stereo Camera (HRSC). The derivation of roughness
within a wavelength range of tens of meters, combined with analyses
at even longer wavelengths, gives an original view of the martian
surface. The potential of this approach is evaluated for different
examples for which the geological processes are identified and the
geological units are mapped and characterized in terms of roughness.
Title: Site Selection and Lunar Outpost: SMART-1 Results and ESA
Studies
Authors: Foing, B.
Bibcode: 2007LPICo1371.3062F
Altcode: 2007eelo.work.3062F
No abstract at ADS
Title: Geometrical Analysis of AMIE/Smart-1 Images and Applications
to Photometric Studies of the Lunar Surface
Authors: Despan, Daniela; Erard, S.; Barucci, M. A.; Josset, J. L.;
Beauvivre, S.; Chevrel, S.; Pinet, P.; Koschny, D.; Almeida, M.;
Foing, B. H.; AMIE Team
Bibcode: 2007DPS....39.2508D
Altcode: 2007BAAS...39..460D
AMIE, the Advanced Moon micro-Imager Experiment on board the ESA
lunar mission SMART-1, is an imaging system to survey the terrain in
visible and near-infrared light. AMIE provides high resolution images
obtained using a tele-objective with 5.3° x 5.3° field of view
and a sensor of 1024 x 1024 pixels. The output images have resolution
45m/pixel at 500km, and are encoded with 10 bits/pixel. From the 300 Km
pericenter altitude, the same field of view corresponds to a spatial
resolution about 30 m/pixel. The FOV is shared by various filters,
allowing to reconstruct mosaics of the surface in 3 colors, depending
on pointing mode. Spot-pointing observations provide photometric
sequences that allow to study the surface properties in restricted
areas. One of the scientific objectives of the mission is to get high
resolution imaging of the Moon surface, e.g. high latitude regions
in the southern hemisphere. In order to map the lunar surface
with AMIE, systematic analysis and processing is being carried on
using the whole data set. Geometrical analysis of AMIE images relies
on the SPICE system: image coordinates are computed to get precise
projection at the surface, and illumination angles are computed
to analyze the photometric sequences. High resolution mosaics were
constructed then compared to lower resolution Clementine UV-Vis and NIR
images. Spot-pointing sequences are used to constrain the photometric
and physical properties of surface materials in areas of interest,
based on Hapke's modeling. Optical alignment parameters in the
Spice kernels have been refined and provide absolute coordinates
in the IAU lunar frame (ULCN). They provide discrepancies with the
Clementine basemap, ranging up to some 0.1° in the equatorial regions,
as expected (e.g., Cook et al DPS 2002; Arcinal et al. EPSC 2006). A
progress report will be presented at the conference.
Title: Interstellar gas, dust and diffuse bands in the SMC
Authors: Cox, N. L. J.; Cordiner, M. A.; Ehrenfreund, P.; Kaper,
L.; Sarre, P. J.; Foing, B. H.; Spaans, M.; Cami, J.; Sofia, U. J.;
Clayton, G. C.; Gordon, K. D.; Salama, F.
Bibcode: 2007A&A...470..941C
Altcode:
Aims:In order to gain new insight into the unidentified identity of
the diffuse interstellar band (DIB) carriers, this paper describes
research into possible links between the shape of the interstellar
extinction curve (including the 2175 Å bump and far-UV rise), the
presence or absence of DIBs, and physical and chemical conditions
of the diffuse interstellar medium (gas and dust) in the Small
Magellanic Cloud (SMC).
Methods: We searched for DIB absorption
features in VLT/UVES spectra of early-type stars in the SMC whose
reddened lines-of-sight probe the diffuse interstellar medium of the
SMC. Apparent column density profiles of interstellar atomic species
(Na i, K i, Ca ii and Ti ii) are constructed to provide information on
the distribution and conditions of the interstellar gas.
Results:
The characteristics of eight DIBs detected toward the SMC wing target
AzV 456 are studied and upper limits are derived
for the DIB equivalent widths toward the SMC stars AzV
398, AzV 214, AzV 18,
AzV 65 and Sk 191. The amount of
reddening is derived for these SMC sightlines, and, using RV
and the H i column density, converted into a gas-to-dust ratio. From
the atomic column density ratios we infer an indication of the strength
of the interstellar radiation field, the titanium depletion level and
a relative measure of turbulence/quiescence. The presence or absence
of DIBs appears to be related to the shape of the extinction curve,
in particular with respect to the presence or absence of the 2175
Å feature. Our measurements indicate that the DIB characteristics
depend on the local physical conditions and chemical composition of the
interstellar medium of the SMC, which apparently determine the rate of
formation (and/or) destruction of the DIB carriers. The UV radiation
field (via photoionisation and photo-destruction) and the metallicity
(i.e. carbon abundance) are important factors in determining diffuse
band strengths which can differ greatly both between and within
galaxies. Based on observations collected with VLT/UVES at the
European Southern Observatory, Paranal, Chile (ESO programs 67.C-0281
and 71.C-0679). Tables [see full text]-[see full text] and Fig. [see
full text] are only available in electronic form at http://www.aanda.org
Title: Coupling between impacts and lunar volcanism for Humorum and
Procellarum basins
Authors: Peters, S. T. M.; Koschny, D.; Foing, B. H.
Bibcode: 2007epsc.conf..355P
Altcode:
A lot of knowledge has been obtained by ground-based observations and
previous space missions on Mare Humorum and Oceanus Procellarum, which
are a circular and irregular basin, respectively. Correlating tectonic
signatures and volcanic outflows within this area gives information on
the development of both basins; and thus on their origin of impact. By
marking different fracture patterns, paleo-stress fields occurring in
the area of both maria become visible. These stresses are believed to
be caused by the contrast in density of the solidified lava and the
anorthosite crust and therefore to be post-volcanic. The presence of
underlying topography and structures of fault systems influence the
formation of new zones of weakness within the basins. Therefore they
induce faults which do not properly reflect the stress field under which
they are formed. To exclude this distortion, only the most inner parts
of the basins are measured. Images from the AMIE-camera on SMART-1 Moon
mission were annotated for tectonic interpretation using ARC-GIS. A
volcanic outflow analysis is made using Clementine UVVIS-data: Lava
outflows from different origin were distinguished on base of their FeO
and TiO2 contents. Ages of the units were determined by cratercounting
methods from other authors. The eruptional and structural analyses
provide a model for the stratigraphic development and spatial occurrence
of the volcanic processes that flooded the maria. This model is compared
with both irregular and circular impact basins for different shape, age
and geographical positions. The results show how these impact-related
parameters influence volcanic mare evolution. With the geographical
position, also the depth and thickness of the KREEP-layer has been
taken in account.
Title: Highlights of SMART-1 Lunar Science results
Authors: Foing, B. H.
Bibcode: 2007epsc.conf..424F
Altcode:
We shall present the highlights of lunar science results from
SMART-1 payload, featuring many innovative instruments and advanced
technologies. SMART-1 lunar science investigations include studies
of the chemical composition of the Moon, of geophysical processes
(volcanism, tectonics, cratering, erosion, deposition of ices and
volatiles) for comparative planetology, and high resolution studies in
preparation for future steps of lunar exploration. The mission science
addresses several topics such as the accretional processes that led
to the formation of rocky planets, and the origin and evolution of
the Earth-Moon system.
Title: Potential rovers and payload for a future polar lunar lander
Authors: Ellouzi, M.; Foing, B.; Hovland, S.
Bibcode: 2007epsc.conf..238E
Altcode:
Lunar poles are thought of being of high interest to land on,
because they have not been explored so far, they are near regions
of quasi-eternal light, or permanent shadow for potential ices and
volatiles, they are thermally benign and are promising sites for future
human outposts and permanent bases. In order to explore the Poles,
a future landing mission would need the help of one or more rovers,
of different sizes, allowing different levels of mobility around the
landing module. They would carry on experiments, which results could
improve our knowledge of the polar areas. Therefore, we describe here
possible rovers and payload capable of meeting both technological and
scientific requirements for Moon missions to the Poles.
Title: Concept studies for lunar landers and sample return missions:
challenges for robotics
Authors: Foing, B. H.
Bibcode: 2007epsc.conf..422F
Altcode:
We present the results of a study for a lunar polar lander conducted
at ESA CDF Concurrent Design Facility and follow up activities. The
goal is to demonstrate lunar landing, survival and exploration
technologies for the future, geochemical studies of the piles, and
search for ice in permanent shadows. We describe the top objectives,
mission analysis, design and associated lander and rover. We also
describe the rationale for Lunar Sample Return missions, and give
some ongoing concept studies performed at ESA. Finally, we discuss
the required advances in planetary robotics, required for the polar
lunar lander and for the sample return missions.
Title: SMART-1 Moon impact on 3 Sept 2006: results from observation
campaign
Authors: Ehrenfreund, P.; Foing, B. H.; Veillet, C.
Bibcode: 2007epsc.conf..425E
Altcode:
SMART-1 operations ended with an impact on the lunar near-side on 3
sept 2006, adjusted in time to allow ground-based observations. The
impact took place in grazing incidence with mass of 285 kg at a
velocity of 2 km/s in the Lake of Excellence. We called the community
to make predictions of impact magnitude, cloud ejecta dynamics,
exospheric effects. We also called the ground based observers to perform
coordinated measurements of the impact. Results from the SMART-1 impact
campaign will be discussed.
Title: Science rationale and payload for lunar landers and sample
return missions
Authors: Foing, B. H.
Bibcode: 2007epsc.conf..423F
Altcode:
We present the results of a study for a lunar polar lander conducted
at ESA CDF Concurrent Design Facility and follow up activities. The
goal is to demonstrate lunar precise landing, survival and exploration
technologies for the future, geochemical studies of the poles, and
search for ice in permanent shadows. We describe the top science
objectives, the associated lander and rover, and the possible payload
complement now in discussion with the community. We also describe the
science rationale for Lunar Sample Return missions, and give update
on some ongoing concept studies performed at ESA.
Title: Search for Climatic Signal in Pavonis Mons Fan Deposits, Mars
Authors: Foing, B. H.; Orsi, A.; Cord, A.; Rossi, A.
Bibcode: 2007epsc.conf..601F
Altcode:
Introduction: Mars has experienced large variations in its orbital
parameters throughout its history. They are calculable for the last 10
million years, with periodicity of 120 000 years for its obliquity,
95 to 100 000 years for its excentricity, and 51 000 years for its
precession, however they become undetermined beyond 20 Myr [1]. Laskar
et al [2] define a standard model of Mars' insolation parameters
over 4 Gyr with the most probable values 0.068 for the eccentricity
and 41.80 degree for the obliquity. Climatic consequences: At high
obliquity, significant amount of ice can be deposited as ice at low
latitudes. General circulation models predict an annual net accumulation
rate of ice on the west of Tharsis volcanoes. Pavonis fan shaped
deposits: We analysed Mars Express images obtained over orbit 946, of
the west fan deposit at Pavonis Mons. The analysis of the HRSC images
shows around 15 ridges, with interval 0.5 - 4.5 km. The interaction
with the underlying surface can be seen, indicating the overlap of
different episodes. The ridges are interpreted as drop debris on the
front edge of a cold glaciar during its slow retreat. On the other
hand isotropic knobbies , circular sub-km-scale hills are interpreted
as results of fast glaciar sublimation. By texture analysis we could
distinguish ridges, knobbies from various episodes and relate them
with geological studies [3]. Glaciar model: For this basic study,
we choose the simplest model of glacier. The bed is believed to be
horizontal, and does not interfere with the glacier. If the ridges are
due to obliquity oscillation, the rate of snow fall and sublimation
must depend slightly on obliquity. Indeed, with accumulation rates and
ablation rates at the same order, we are able to find oscillation of the
glacier extent. We can see oscillations of the glacier extent from the
beginning. It is interesting to notice that this shape is consistent
with the observation of older outer sets of ridges, and young inner
ones. The maximum extents, which we intent to link to the position of
the ridges are organized by groups of 4 or 5. The outer ridges we see
on Pavonis Mons date back to 10-200 million years ago. We know that
the obliquity raised 5 million years ago. The recent lowering of the
obliquity could have triggered inner ridges too, but the outer ones
we see look older. To account for their formation, we have to find an
area of great variation in obliquity, allowing the glacier to form and
retreat, before 10 millions years ago. A threshold obliquity angle above
35 deg for effective ice deposition is needed to account for a glacier
older than 10 million years. Conclusions and Perspectives: Ridges in
Pavonis Mons Fan deposits could be interpreted as cold glaciar debris
tracing climate changes. Texture analysis to distinguish units and
episodes from different obliquity and climate variations. We developed
a simple qualitative glaciar progression/recession model. One needs to
better quantify ice deposition/ablation net rates vs obliquity. We find
that a 45 deg obliquity deposition threshold could better describe the
Pavonis Mons Fan deposits data. Next steps in modeling should include
the effect of topography, slopes, orientation. The geologic stratigraphy
can constrain the evolution of fan deposits [3], in conjunction with
crater counts dating and chronology . The climatic signal imprinted as
ridges could be determined over the period of large extend of glaciar,
and could permit to constrain the undetermined obliquity variations
beyond 15 Myr [2]. References: [1] Laskar et al 2002 Nature 419, 375,
[2] Laskar et al (2004, Icarus, Volume 170, Issue 2, p. 343-364. [3]
Shean, D.E., Head, J.W., Marchant, D.R. 2005, JGR, 110, E5
Title: SMART-1 Collaborations with Upcoming Lunar Missions
Authors: Foing, B. H.
Bibcode: 2007epsc.conf..444F
Altcode:
We discuss ongoing collaborations between SMART-1 and upcoming Lunar
missions (Chang'e1, Selene, Chandrayaan-1, LRO, LCROSS, future Lunar
Landers and Rovers) . This includes: - Data analysis and PSA archiving;
- Merging data between different missions; - Coordinate systems and
reference grid; - Scientific interpretation; - Survey of possible
landing sites; - Lessons from SMART-1 Impact experiment - Survey of
illumination and resources for future exploration - New miniaturised
instruments development; - Lessons from SMART-1 development; - SMART-1
science planning tool; - Public outreach and education.
Title: Search for Climatic Signal in Pavonis Mons Fan Deposits
Authors: Foing, B. H.; Orsi, A.; Cord, A.; Zegers, T.; Rossi, A.;
HRSC Co-I Team
Bibcode: 2007LPICo1353.3273F
Altcode:
We analysed Mars Express HRSC images of the west fan deposits at
Pavonis Mons. We use the deposit ridges, interpreted as drop debris
from cold glaciar slow retreat, to search for climatic signal induced
by the variations of obliquity beyond 15 Myr ago.
Title: Linear and circular polarisation of diffuse interstellar bands
Authors: Cox, N. L. J.; Boudin, N.; Foing, B. H.; Schnerr, R. S.;
Kaper, L.; Neiner, C.; Henrichs, H.; Donati, J. -F.; Ehrenfreund, P.
Bibcode: 2007A&A...465..899C
Altcode:
Context: The detection or absence of a polarisation signal in the
diffuse interstellar band (DIB) profile can possibly give important
clues on the identity of its carrier. For molecular gas-phase
carriers the effect of polarisation on its electronic transitions
depends, although uncertain how exactly, on its physical properties
(e.g. molecular structure). On the other hand, if the carriers are
grains, impurities or defects in grain mantles are also expected to
show up in the polarisation of DIBs.
Aims: Our aim is to detect
a polarisation signal in a DIB profile or to derive stricter upper
limits on the polarisation efficiency of DIB carriers.
Methods:
In order to detect and measure the linear and circular polarisation
of the DIBs we observe reddened lines of sight showing continuum
polarisation; for this study we select the stars HD
21219, HD 198478, HD
197770, HD 183143 and HD
163472. We use spectropolarimetry in the wavelength range
4480 to 6620 Å with the MuSiCoS échelle spectrograph mounted at the
Télescope Bernard Lyot.
Results: Linear polarisation spectra are
constructed in order to search for a polarisation signal in the DIB
profiles. No significant change in the linear polarisation degree is
found. We obtain a 2σ polarisation detection limit (per DIB FWHM) of
0.01-0.04% for HD 21219, 0.04-0.14% for HD
197770, 0.01-0.14% for HD 183143 and
0.01-0.14% for HD 198478, for the six investigated
DIBs. We derive upper limits for the polarisation efficiency factor
f for six strong narrow DIBs; f_max of 0.31, 0.44, 0.45, 0.18, 0.47
and 0.68 for the λλ 5780, 5797, 6196, 6284, 6379 and 6613 DIBs,
respectively. The derived detection limits are similar to those
derived by Adamson & Whittet (1995), although for more lines of
sight and more DIBs. Circular polarisation (Stokes V) spectra of high
signal-to-noise have been obtained for the first time for the 5780,
5797, 6196, 6203, 6284, 6376, 6379 and 6613 Å DIB profiles. No
circular polarisation signal is detected. The 2σV (per
0.1 Å) noise level limits are 1.0-2.5% for the DIBs in the line of
sight towards HD 197770 and 0.06-0.10% for the DIBs
towards HD 163472.
Conclusions: . The lack of
polarisation of the DIB profiles is consistent with DIB carriers that
are not directly related to solid features, like impurities in grain
mantles. However, large (carbonaceous) gas phase molecules remain
viable DIB carrier candidates. Based on observation at the
Observatoir du Pic du Midi, France with the MuSiCoS spectropolarimeter.
Title: SMART-1 Lunar Science Planning
Authors: Koschny, D.; Foing, B. H.; Frew, D.; Almeida, M.; Sarkarati,
M.; Volp, J.; Grande, M.; Huovelin, J.; Josset, J. -L.; Nathues,
A.; Malkki, A.; Noci, G.; Kellett, B.; Beauvivre, S.; Heather, D.;
Zender, J.; McMannamon, P.; Schwehm, G.; Camino, O.; Blake, R.
Bibcode: 2007LPI....38.1996K
Altcode:
The SMART-1 spacecraft reached lunar capture on 17 November 2004,
and on 15 March 2005 a lunar orbit 400-3000 km for a nominal science
period of six months, with 1 year science extension. We report on the
SMART-1 science planning methods, tools and lesson
Title: SMART-1 Mission: Highlights of Lunar Results
Authors: Foing, B. H.; Grande, M.; Huovelin, J.; Josset, J. -L.;
Keller, H. U.; Nathues, A.; Malkki, A.; Noci, G.; Kellett, B.;
Beauvivre, S.; Cerroni, P.; Pinet, P.; Makkinen, H.; Mall, U.; Almeida,
M.; Frew, D.; Volp, J.; Sarkarati, M.; Heather, D.; Koschny, D.
Bibcode: 2007LPI....38.1953F
Altcode:
The SMART-1 spacecraft reached on 15 March 2005 a lunar orbit 400-3000
km for a nominal science period of six months, with 1 year science
extension until September 2006. We shall report on highlights of lunar
science and exploration results.
Title: Radio Observations of the Moon at 3.6 cm Before and After
SMART-1 Impact
Authors: Volvach, A. E.; Berezhnoy, A. A.; Foing, B.; Ehrenfreund,
P.; Khavroshkin, O. B.; Volvach, L. N.
Bibcode: 2007LPI....38.1015V
Altcode:
Influence of SMART-1 impact on lunar radio flux at 3.6 cm was not
detected. Parameters of SMART-1 impact radio flash are estimated. Upper
limit of the intensity of radio flashes caused by meteoroid impacts
is estimated.
Title: Photometric Characterization of Selected Lunar Sites by
SMART-1 AMIE Data
Authors: Kaydash, V.; Kreslavsky, M.; Shkuratov, Yu.; Gerasimenko,
S.; Pinet, P.; Chevrel, S.; Josset, J. -L.; Beauvivre, S.; Almeida,
M.; Foing, B.
Bibcode: 2007LPI....38.1535K
Altcode:
We use images obtained in 2006 by Advanced Moon Micro-Imager Experiment
(AMIE) camera onboard SMART-1 spacecraft to access photometric
properties of selected lunar areas in the context of geological and
structural properties of the regolith.
Title: The ORGANICS experiment on BIOPAN V: UV and space exposure
of aromatic compounds
Authors: Ehrenfreund, Pascale; Ruiterkamp, Richard; Peeters, Zan;
Foing, Bernard; Salama, Farid; Martins, Zita
Bibcode: 2007P&SS...55..383E
Altcode:
We studied the stability of aromatic compounds in low Earth orbit
environment and describe the scientific results and successful flight
of the ORGANICS experiment on-board the BIOPAN V space exposure
facility. This experiment investigated the photo stability of
large organic molecules in low Earth orbit. Thin films of selected
organic molecules, such as polycyclic aromatic hydrocarbons (PAHs)
and the fullerene C 60 were subjected to the low Earth
orbit environment and the samples were monitored before and after
flight. PAHs and fullerenes have been proposed as carriers for a
number of astronomical absorption and emission features and are also
identified in meteorites. Our experiment on BIOPAN V was exposed to
a total fluence of 602.45 kJ m -2 for photons in the range
170-280 nm. The experiment was also intended as a hardware test-flight
for a long-term exposure experiment (Survival of organics in space)
on the EXPOSE facility on the International Space Station (ISS). For
the small fluence that was collected during the BIOPAN V experiment we
found little evidence of photo-destruction. The results confirm that
PAH molecules are very stable compounds in space. The small differences
in destruction rates that are expected to arise among the PAH samples
as a function of molecular size and structure will only show after
the longer irradiation fluences that are expected in the exposure
experiment on the ISS.
Title: 3D Mapping of Aram Chaos: S Record of Fracturing and Fluid
Activity
Authors: Oosthoek, J. H. P.; Zegers, T. E.; Rossi, A.; Foing, B.;
Neukum, G.; HRSC Co-Investigation Team
Bibcode: 2007LPI....38.1577O
Altcode:
Mapping of structures and stratigraphic units of Aram Chaos
was performed with HRSC data, using in particular the stereo (3D)
capabilities of HRSC. In combination with published spectral information
from TES, THEMIS and OMEGA, 3D mapping was used to deriv
Title: SMART-1 Impact Ground-based Campaign
Authors: Ehrenfreund, P.; Foing, B. H.; Veillet, C.; Wooden, D.;
Gurvits, L.; Cook, A. C.; Koschny, D.; Biver, N.; Buckley, D.; Ortiz,
J. L.; di Martino, M.; Dantowitz, R.; Cooke, B.; Reddy, V.; Wood,
M.; Vennes, S.; Albert, L.; Sugita, S.; Kasuga, T.; Meech, K.
Bibcode: 2007LPI....38.2446E
Altcode:
Based on predictions of impact magnitude and cloud ejecta dynamics,
we organized a SMART-1 ground-based observation campaign to perform
coordinated measurements of the impact. Results from the coordinated
multi-site campaign will be discussed.
Title: SMART-1 Impact Observation at the Canada-France-Hawaii
Telescope
Authors: Veillet, C.; Foing, B.
Bibcode: 2007LPI....38.1520V
Altcode:
This talk will present the current status of the processing of the
sequence of impact images obtained at CFHT, from the analysis of the
impact flash to the geometry of the plume seen spreading over the 90
seconds following the impact.
Title: The D-CIXS X-ray spectrometer on the SMART-1 mission to the
Moon—First results
Authors: Grande, M.; Kellett, B. J.; Howe, C.; Perry, C. H.; Swinyard,
B.; Dunkin, S.; Huovelin, J.; Alha, L.; D'Uston, L. C.; Maurice, S.;
Gasnault, O.; Couturier-Doux, S.; Barabash, S.; Joy, K. H.; Crawford,
I. A.; Lawrence, D.; Fernandes, V.; Casanova, I.; Wieczorek, M.;
Thomas, N.; Mall, U.; Foing, B.; Hughes, D.; Alleyne, H.; Russell,
S.; Grady, M.; Lundin, R.; Baker, D.; Murray, C. D.; Guest, J.;
Christou, A.
Bibcode: 2007P&SS...55..494G
Altcode:
The SMART-1 mission has recently arrived at the Moon. Its payload
includes D-CIXS, a compact X-ray spectrometer. SMART-1 is a technology
evaluation mission, and D-CIXS is the first of a new generation
of planetary X-ray spectrometers. Novel technologies enable new
capabilities for measuring the fluorescent yield of a planetary surface
or atmosphere which is illuminated by solar X-rays. During the extended
SMART-1 cruise phase, observations of the Earth showed strong argon
emission, providing a good source for calibration and demonstrating
the potential of the technique. At the Moon, our initial observations
over Mare Crisium show a first unambiguous remote sensing of calcium
in the lunar regolith. Data obtained are broadly consistent with
current understanding of mare and highland composition. Ground truth
is provided by the returned Luna 20 and 24 sample sets.
Title: HRSC-based Mapping and Internal Architecture of Gale Crater
(Mars)
Authors: Rossi, A. P.; Zegers, T.; Pondrelli, M.; Gwinner, K.; Hauber,
E.; Neukum, G.; Velasco, E.; Stesky, R.; Fueten, F.; Chicarro, A.;
Foing, B.
Bibcode: 2007LPI....38.1553R
Altcode:
New observations on the geomorphology and internal geometry of Gale
crater central bulge are presented. We used a new HRSC stereo-derived
DTM in order to better define morphology and layering attitude within
bulge deposits.
Title: SMART-1 Mission Overview from Launch, Lunar Orbit to Impact
Authors: Foing, B. H.; Camino, O.; Schoenmakers, J.; de Bruin, J.;
Gestal, D.; Alonso, M.; Blake, R.; Ricken, S.; Pardo, P.; Koschny,
D.; Frew, D.; Almeida, M.; Sarkarati, M.; Volp, J.; Schwehm, G.;
Josset, J. L.; Beauvivre, S.; Sodnik, Z.; Grande, M.; Keller, U.
Bibcode: 2007LPI....38.1915F
Altcode:
We shall give an overview of the SMART-1 mission, travel and operations
from launch, lunar capture, lunar science orbit to impact.
Title: The Case for Large-Scale Spring Deposits on Mars: Light-toned
Deposits in Crater Bulges, Valles Marineris and Chaos
Authors: Rossi, A. P.; Neukum, G.; Pondrelli, M.; Zegers, T.; Mason,
P.; Hauber, E.; Ori, G. G.; Fueten, F.; Oosthoek, J.; Chicarro, A.;
Foing, B.
Bibcode: 2007LPI....38.1549R
Altcode:
We investigate and propose the possibility of a common origin as spring
deposits for various materials on Mars: light-toned deposits in Valles
Marineris, crater bulges and chaotic terrains.
Title: The SMART 1 Impact Event: From the Laboratory to the Moon
Authors: Burchell, M. J.; Robin-Williams, R.; Foing, B. H.
Bibcode: 2007bget.conf...25B
Altcode:
No abstract at ADS
Title: CFHT Observation of SMART-1 Impact
Authors: Veillet, Christian; Albert, L.; Foing, B.; Ehrenfreund, P.
Bibcode: 2006DPS....38.5717V
Altcode: 2006BAAS...38.1303V
Through the use of Director’s Discretionary Time on the
Canada-France-Hawaii Telescope on top of Mauna Kea, Hawaii, an attempt
was made at observing the planned impact of the SMART-1 spacecraft. Even
though the instrumentation available on the telescope the evening of
the impact was not the best suited to the observation of such a fugitive
event, a reconnaissance at the impact site the prior evening to tune to
the observing strategy and some luck with weather and timing at impact
time allowed us to obtain a good temporal series (10-s exposure time
images every 15 seconds) of the crash area covering 17mn before the
crash and a full hour after. Observations were made with the wide-field
infrared camera WIRCam through a molecular H2 narrow-band filter. The
flash of the impact itself was captured, allowing us to independently
locate the point of impact with respect to the lunar features seen on
the Earthshine lit lunar landscape. The images taken over the minutes
following the impact provided the first ever observations of an ejecta
cloud in expansion from an impact on the Moon. The last results from
the analysis of the images of the impact itself and the subsequent
dust cloud will be presented at the time of the meeting.
Title: The Research and Scientific Support Department of ESA and CoRoT
Authors: Fridlund, M.; Beaufort, T.; Favata, F.; Foing, B.; Gimenéz,
A.; Gondoin, P.; Johlander, B.; Smit, H.; Sunter, W.; Appourchaux, T.
Bibcode: 2006ESASP1306..133F
Altcode:
No abstract at ADS
Title: SMART-1 Impact Campaign: Predictions, Observations, LCROSS
Implications
Authors: Foing, B. H.; Frew, D.; Almeida, A.; Sarkarati, M.; Volp,
J.; Racca, G.; Camino, O.; Schoenmaker, J.; Schwehm, G.; Josset,
J. L.; Beauvivre, S.; Sodnik, Z.; Cerroni, P.; Barucci, A.; Grande,
M.; Keller, U.; Nathues, A.; Muinonen, K.; Ehrenfreund, P.; Wood, M.;
Vennes, S.; Meech, K.; Taylor, C.; Hanslmeyer, A.; Vaubaillon, J.;
Khodachenko, M.; Rucker, H.; Leibundgut, B.; Hainaut, O.; Gondoin, P.;
Ortiz, J. L.; Schultz, R.; Erd, C.; SMART-1 Coordinated Observations
Group; SMART-1 Impact Prediction Group; Smart-1 Outreach; Amateur
Astronomer Coordination
Bibcode: 2006LPICo1327....9F
Altcode:
No abstract at ADS
Title: SMART-1 Implications for LCROSS: Operations and Lunar Science
Results
Authors: Foing, B. H.; Frew, D.; Almeida, M.; Koschny, D.; Volp, J.;
Josset, J. -L.; Grande, M.; Houvelin, J.; Keller, H. U.; Nathues, A.;
Malkki, A.; Noci, G.; Kellett, B.; Beauvivre, S.; Heather, D.; Zender,
J.; McMannamon, P.; Camino, O.; Colaprete, T.; Wooden, D.; Lcross Team
Bibcode: 2006LPICo1327....7F
Altcode:
No abstract at ADS
Title: Colour Images Of The Moon From Amie On Smart-1: A Preliminary
Analysys Of The Region Of Oppenheimer.
Authors: Cerroni, Priscilla; Besse, S.; De Sanctis, M. C.; Josset,
J.; Beauvivre, S.; Pinet, P.; Chevrel, S.; Barucci, M. A.; Langevin,
Y.; Koshny, D.; Almeida, M.; Foing, B.; AMIE Team
Bibcode: 2006DPS....38.5711C
Altcode: 2006BAAS...38..590C
The Advanced Moon micro-Imager Experiment (AMIE) is the imaging system
on board the ESA mission to the Moon SMART-1 which is closing towards
its end on September 3rd, 2006. During the time spent
in lunar orbit the AMIE camera provided high resolution CCD images
of selected lunar areas where it performed colour imaging through
three filters at 750, 915 and 960 nm with a maximum resolution of 27
m /pixel at the perilune of 300 km. The spectral bands have been
selected in order to allow discrimination between mafic minerals which
dominate the mare (revealed by the Fe2+ absorption feature at 950 nm)
and the anorthosite rich highland materials. Data acquired by AMIE
in push-broom modality on November 25th, 2005 for the lunar region of
Oppenheimer centered at 36 S, 194 E have been preliminarily analysed
. The ground resolution for these observations is of 73 m/px. A new
calibration has been applied to the images based on flat-fielding from
in-flight data; for the region considered three filters images have
been co-registered, colour images and band-ratio images have been
produced. An assessment of the results and a comparison with
Clementine data from the same region is presented . Spectra have been
extracted from a region in the floor of Oppenheimer and on the rim of
a crater : a comparison with spectra from Clementine yields consistent
results. Acknowledgements: P. Cerroni and M.C. De Sanctis acknowledge
the support of ASI grant I/030/05
Title: Results from SMART-1 Lunar Mission
Authors: Foing, B. H.
Bibcode: 2006IAUJD..10E...7F
Altcode:
SMART-1 is the first ESA mission that reached the Moon. It demonstrated
Solar Electric Primary Propulsion (SEP) and tested new technologies
for spacecraft and instruments. Launched on 27 Sept. 2003, as
Ariane-5 auxiliary passenger, SMART-1 has spiralled out towards
lunar capture on 15 November 2004, and then towards lunar science
orbit reached on 1 March 2005. The mission has been extended and is
due to end with an impact on 2-3 September 2006. This is permitting
science but also to prepare future international lunar exploration,
in collaboration with upcoming missions. We shall present the first
year lunar results from SMART-1's science and technology payload. The
19 kg payload includes a miniaturized high-resolution camera (AMIE),
a near-infrared point-spectrometer (SIR) for mineralogy investigation,
and a very compact X-ray spectrometer (D-CIXS) for surface elemental
composition. There is also an experiment (KaTE) aimed at demonstrating
deep-space telemetry and telecommand communications in the X and
Ka-bands, a radio-science experiment (RSIS), a deep space optical
link (Laser-Link Experiment), using the ESA Optical Ground station
in Tenerife, and the validation of a system of autonomous navigation
(OBAN) based on image processing. SMART-1 lunar science investigations
include studies of the chemical composition of the Moon, of geophysical
processes (volcanism, tectonics, cratering, erosion, deposition of ices
and volatiles) for comparative planetology, and high resolution studies
in preparation for future steps of lunar exploration. The mission
addresses several topics such as the accretional processes that led
to the formation of rocky planets, and the origin and evolution of
the Earth-Moon system.
Title: Analysis and modeling of high temporal resolution spectroscopic
observations of flares on AD Leonis
Authors: Crespo-Chacón, I.; Montes, D.; García-Alvarez, D.;
Fernández-Figueroa, M. J.; López-Santiago, J.; Foing, B. H.
Bibcode: 2006A&A...452..987C
Altcode: 2006astro.ph..2123C
We report the results of a high temporal resolution spectroscopic
monitoring of the flare star AD Leo. During 4 nights,
more than 600 spectra were taken in the optical range using the Isaac
Newton Telescope (INT) and the Intermediate Dispersion Spectrograph
(IDS). We observed a large number of short and weak flares occurring
very frequently (flare activity > 0.71 h-1). This is
consistent with the very important role that flares can play in stellar
coronal heating. The detected flares are non white-light flares and,
although most solar flares are of this kind, very few such events
have been observed previously in stars. The behaviour of different
chromospheric lines (Balmer series from Hα to H{11}, Ca II H &
K, Na I D1 and D2, He I 4026 Å and He I D3) was studied in detail
for a total of 14 flares. We estimated the physical parameters of the
flaring plasma by using a procedure that assumes a simplified slab
model of flares. All the obtained physical parameters are consistent
with previously derived values for stellar flares, and the areas -
less than 2.3% of the stellar surface - are comparable with the
size inferred for other solar and stellar flares. We studied the
relationships between the physical parameters and the area, duration,
maximum flux and energy released during the detected flares.
Title: A Lunar Liquid Mirror Telescope (LLMT) for deep-field infrared
observations near the lunar pole
Authors: Angel, Roger; Eisenstein, Dan; Sivanandam, Suresh; Worden,
Simon P.; Burge, Jim; Borra, Ermanno; Gosselin, Clément; Seddiki,
Omar; Hickson, Paul; Ma, Ki Bui; Foing, Bernard; Josset, Jean-Luc;
Thibault, Simon; Van Susante, Paul
Bibcode: 2006SPIE.6265E..1UA
Altcode: 2006SPIE.6265E..54A
We have studied the feasibility and scientific potential of a 20 - 100
m aperture astronomical telescope at the lunar pole, with its primary
mirror made of spinning liquid at less than 100K. Such a telescope,
equipped with imaging and multiplexed spectroscopic instruments for
a deep infrared survey, would be revolutionary in its power to study
the distant universe, including the formation of the first stars and
their assembly into galaxies. The LLMT could be used to follow up
discoveries made with the 6 m James Webb Space Telescope, with more
detailed images and spectroscopic studies, as well as to detect objects
100 times fainter, such as the first, high-red shift stars in the early
universe. Our preliminary analysis based on SMART-1 AMIE images shows
ridges and crater rims within 0.5° of the North Pole are illuminated
for at least some sun angles during lunar winter. Locations near these
points may prove to be ideal for the LLMT. Lunar dust deposited on
the optics or in a thin atmosphere could be problematic. An in-situ
site survey appears necessary to resolve the dust questions.
Title: The Large Magellanic Cloud: diffuse interstellar bands,
atomic lines and the local environmental conditions
Authors: Cox, N. L. J.; Cordiner, M. A.; Cami, J.; Foing, B. H.;
Sarre, P. J.; Kaper, L.; Ehrenfreund, P.
Bibcode: 2006A&A...447..991C
Altcode:
The Large Magellanic Cloud (LMC) offers a unique laboratory to study
the diffuse interstellar bands (DIBs) under conditions that are
profoundly different from those in the Galaxy. DIB carrier abundances
depend on several environmental factors, in particular the local
UV radiation field. In this paper we present measurements of twelve
DIBs in five lines of sight to early-type stars in the LMC, including
the 30 Doradus region. From the high resolution
spectra obtained with VLT/UVES we also derive environmental parameters
that characterise the local interstellar medium (ISM) in the probed
LMC clouds. These include the column density components (including
total column density) for the atomic resonance lines of Na I, Ca II,
Ti II, K I. In addition, we derive the H I column density from 21 cm
line profiles, the total-to-selective visual extinction RV
and the gas-to-dust ratio N(H I)/A_V. Furthermore, from atomic line
ratios we derive the ionisation balance and relative UV field strength
in these environments. We discuss the properties of the LMC ISM in the
context of DIB carrier formation. The behaviour of DIBs in the LMC is
compared to that of DIBs in different local environmental conditions
in the Milky Way. A key result is that in most cases the diffuse band
strengths are weak (up to factor 5) with respect to Galactic lines
of sight of comparable reddening, EB-V. In the line of
sight towards Sk -69 223 the 5780 and 5797 Å DIBs
are very similar in strength and profile to those observed towards
HD 144217, which is typical of an environment
exposed to a strong UV field. From the velocity analysis we find
that DIB carriers (towards Sk -69 243) are better
correlated with the ionised species like Ca II than with neutrals
(like Na I and CO). The most significant parameter that governs the
behaviour of the DIB carrier is the strength of the UV field.
Title: The effects of Martian near surface conditions on the
photochemistry of amino acids
Authors: ten Kate, Inge Loes; Garry, James R. C.; Peeters, Zan; Foing,
Bernard; Ehrenfreund, Pascale
Bibcode: 2006P&SS...54..296T
Altcode:
In order to understand the complex multi-parameter system of
destruction of organic material on the surface of Mars, step-by-step
laboratory simulations of processes occurring on the surface of Mars are
necessary. This paper describes the measured effects of two parameters,
a CO 2 atmosphere and low temperature, on the destruction
rate of amino acids when irradiated with Mars-like ultraviolet light
(UV). The results show that the presence of a 7 mbar CO 2
atmosphere does not affect the destruction rate of glycine, and that
cooling the sample to 210 K (average Mars temperature) lowers the
destruction rate by a factor of 7. The decrease in the destruction
rate of glycine by cooling the sample is thought to be predominantly
caused by the slower reaction kinetics. When these results are scaled to
Martian lighting conditions, cold thin films of glycine are assumed to
have half-lives of 250 h under noontime peak illumination. It has been
hypothesised that the absence of detectable native organic material in
the Martian regolith points to the presence of oxidising agents. Some
of these agents might form via the interaction of UV with compounds in
the atmosphere. Water, although a trace component of Mars' atmosphere,
is suggested to be a significant source of oxidising species. However,
gaseous CO 2 or adsorbed H 2O layers do not
influence the photodestruction of amino acids significantly in the
absence of reactive soil. Other mechanisms such as chemical processes in
the Martian regolith need to be effective for rapid organic destruction.
Title: SMART-1/AMIE Camera System
Authors: Josset, J. -L.; Beauvivre, S.; Cerroni, P.; de Sanctis, M. C.;
Pinet, P.; Chevrel, S.; Langevin, Y.; Barucci, M. A.; Plancke, P.;
Koschny, D.; Almeida, M.; Sodnik, Z.; Mancuso, S.; Hofmann, B. A.;
Muinonen, K.; Shevchenko, V.; Shkuratov, Y.; Ehrenfreund, P.; Foing,
B. H.
Bibcode: 2006LPI....37.1847J
Altcode:
The Advanced Moon micro-Imager Experiment (AMIE), on board ESA SMART-1,
the first European mission to the Moon (launched on 27th September
2003), is a camera system with scientific, technical and public outreach
oriented objectives.
Title: Widespread Periglacial Landforms in Thaumasia Highland, Mars
Authors: Rossi, A. P.; Chicarro, A. F.; Pacifici, A.; Pondrelli, M.;
Helbert, J.; Benkhoff, J.; Zegers, T.; Foing, B.; Neukum, G.
Bibcode: 2006LPI....37.1568R
Altcode:
Recent glacial and periglacial landforms appear widespread in Thaumasia
Highland. We are mapping them using HRSC data and, locally, MOC NA
and Themis VIS. We started ice stability modeling for these landforms.
Title: Preliminary Analysis of Colour Information from AMIE on Smart-1
Authors: Cerroni, P.; de Sanctis, M. C.; Josset, J. -L.; Beauvivre,
S.; Koschny, D.; Pinet, P.; Chevrel, S.; Langevin, Y.; Barucci, M. A.;
Plancke, P.; Almeida, M.; Hofmann, B. A.; Muinonen, K.; Shevchenko,
V.; Shkuratov, Yu.; Ehrenfreund, P.; Foing, B. H.
Bibcode: 2006LPI....37.1831C
Altcode:
The Advanced Moon micro-Imager Experiment (AMIE) is the imaging system
on board the ESA mission to the Moon SMART-1. We present a preliminary
assessment of push-broom data acquired during the first push-broom
orbital phase of Smart-1 mission.
Title: Amino Acid Destruction in the Martian Surface Environment
Authors: ten Kate, I. L.; Garry, J. R. C.; Peeters, Z.; Foing, B. H.;
Ehrenfreund, P.
Bibcode: 2006LPI....37.2397T
Altcode:
In this paper we present the results of experiments, in which thin
films of glycine have been irradiated with UV in a CO2 atmosphere,
and cooled to an average martian surface temperature of 210 K.
Title: ESA's SMART-1 Mission: Lunar Science Results After One Year
Authors: Foing, B. H.; Grande, M.; Huovelin, J.; Josset, J. L.; Keller,
H. U.; Nathues, A.; Malkki, A.; Noci, G.; Kellett, B.; Beauvivre, S.;
Almeida, M.; Frew, D.; Volp, J.; Heather, D.; Schwehm, G.; Koschny,
D.; Zender, J.; McMannamon, P.; Camino, O.; Racca, G. D.
Bibcode: 2006LPI....37.1920F
Altcode:
We summarise one year of SMART-1 lunar science results with the optical
camera (polar and colour high res imaging), infrared spectrometer
(mineralogy), and X-ray spectrometer (elemental composition). We
describe the plan for operations until end of mission impact in
August 2006.
Title: The next steps in exploring deep space—A cosmic study by
the IAA
Authors: Huntress, W.; Stetson, D.; Farquhar, R.; Zimmerman, J.;
Clark, B.; O'Neil, W.; Bourke, R.; Foing, B.
Bibcode: 2006AcAau..58..304H
Altcode:
This paper presents the results of an IAA cosmic study on the Next
Steps in Exploring Deep Space, the goal of which is to provide a vision
for the scientific exploration of space by humans in the first half
of the 21st Century. The study provides a roadmap for a systematic,
logical, and science-driven plan for exploration of the Solar System
and unlocking the mysteries of the Universe—a program that builds
gradually and systematically to establish a permanent presence
at each outpost along the way, and that builds the communications,
transportation and other logistical infrastructure as it proceeds. The
study suggests a set of long-term scientific goals for space exploration
that provide the context for carrying out scientific investigations
at specific destinations in space. An architecture is derived for the
space flight infrastructure required to pursue these science goals
at the specified destinations, including examination of the relevant
policy and public engagement in this enterprise.
Title: Mapping of Photometric Anomaly of Martian Surface with
HRSC Data
Authors: Kreslavsky, M. A.; Bondarenko, N. V.; Pinet, P. C.; Raitala,
J.; Foing, B. H.; Neukum, G.; Mars Express HRSC Co-Investigator Team
Bibcode: 2006LPI....37.2211K
Altcode:
We propose a practical method for mapping photometric anomaly of Mars
surface from five panchromatic HRSC channels. The method tolerates
atmospheric effect and calibration errors. We show examples of
interpretation in terms of the surface structure.
Title: Highlights of SMART-1 Lunar Science results
Authors: Foing, B. H.; SMART-1 Team
Bibcode: 2006cosp...36.3721F
Altcode: 2006cosp.meet.3721F
No abstract at ADS
Title: Highlights of SMART-1 Lunar Science results
Authors: Foing, B. H.; Smart-1 Science; Technology Working Team
Bibcode: 2006epsc.conf..653F
Altcode:
We shall present the highlights of lunar science results from SMART-1
payload, featuring many innovative instruments and advanced technologies
with a total mass of some 19 kg. SMART-1 lunar science investigations
include studies of the chemical composition of the Moon, of geophysical
processes (volcanism, tectonics, cratering, erosion, deposition of ices
and volatiles) for comparative planetology, and high resolution studies
in preparation for future steps of lunar exploration. The mission
addresses several topics such as the accretional processes that led
to the formation of rocky planets, and the origin and evolution of
the Earth-Moon system.
Title: Recent ice-related landforms at high altitude on Mars
(Thaumasia Highland)
Authors: Rossi, A. P.; Helbert, J.; Pacifici, A.; Pondrelli, M.;
Benkhoff, J.; Zegers, T.; Chicarro, A.; Foing, B.
Bibcode: 2006epsc.conf..212R
Altcode:
Pristine and deflated periglacial-like landforms are visible on HRSC
data over Thaumasia Highland, Mars. They include lineated crater/valley
fills, protalus lobes and protalus ramparts. Lineated crater/valley fill
appear to be larger in size and slightly older than protalus lobe-like
landforms in the area, suggesting a decrease in ice-related landform
development with time. The estimated age of the youngest periglacial
landforms is less than a few tens of million years, consistent with
what has been calculated for glacial/periglacial deposits in various
other regions on Mars. In order to assess the likelihood of finding ice
rich deposits within the mapped features we are using the Berlin Mars
near Surface Thermal Model (BMST). Our modeling results are consistent
with the presence of ground ice in some of the areas where we found
periglacial landforms. The most pristine looking rock glaciers mainly
occur on south facing slopes. This is consistent with modeling results
and inferred flow directions.
Title: Science objectives and first results from the SMART-1/AMIE
multicolour micro-camera
Authors: Josset, J. -L.; Beauvivre, S.; Cerroni, P.; de Sanctis, M. C.;
Pinet, P.; Chevrel, S.; Langevin, Y.; Barucci, M. A.; Plancke, P.;
Koschny, D.; Almeida, M.; Sodnik, Z.; Mancuso, S.; Hofmann, B. A.;
Muinonen, K.; Shevchenko, V.; Shkuratov, Yu.; Ehrenfreund, P.; Foing,
B. H.
Bibcode: 2006AdSpR..37...14J
Altcode:
The Advanced Moon micro-Imager Experiment (AMIE), on-board SMART-1,
the first European mission to the Moon, is an imaging system with
scientific, technical and public outreach objectives. The science
objectives are to image the lunar South Pole, permanent shadow areas
(ice deposit), eternal light (crater rims), ancient lunar non-mare
volcanism, local spectrophotometry and physical state of the lunar
surface, and to map high latitudes regions (south) mainly at far side
(South Pole Aitken basin). The technical objectives are to perform a
Laserlink experiment (detection of laser beam emitted by ESA/Tenerife
ground station), flight demonstration of new technologies and on-board
autonomy navigation. The public outreach and educational objectives
are to promote planetary exploration and space. We present here the
first results obtained during the cruise phase.
Title: Growing pioneer plants for a lunar base
Authors: Kozyrovska, N. O.; Lutvynenko, T. L.; Korniichuk, O. S.;
Kovalchuk, M. V.; Voznyuk, T. M.; Kononuchenko, O.; Zaetz, I.;
Rogutskyy, I. S.; Mytrokhyn, O. V.; Mashkovska, S. P.; Foing, B. H.;
Kordyum, V. A.
Bibcode: 2006AdSpR..37...93K
Altcode:
A precursory scenario of cultivating the first plants in a lunar
greenhouse was elaborated in frames of a conceptual study to grow plants
for a permanently manned lunar base. A prototype plant growth system
represents an ornamental plant Tagetes patula L. for growing in a lunar
rock anorthosite as a substrate. Microbial community anticipated to be
in use to support a growth and development of the plant in a substrate
of low bioavailability and provide an acceptable growth and blossoming
of T. patula under growth limiting conditions.
Title: Prelude to The Moon: Science, Technology, Utilization and
Human Exploration
Authors: Ehrenfreund, P.; Foing, B. H.
Bibcode: 2006AdSpR..37....5E
Altcode:
A COSPAR 2-day symposium was dedicated to "The Moon: Science,
Technology, Utilization and Human Exploration" at the COSPAR assembly
in Paris, on 22-23 July 2004, sponsored by Planetary (B0.3), Life
Sciences (F0.1) and Planetary Protection (PPP3) commissions, and ILEWG
International Lunar Exploration Working Group. This was very timely to
present the first results from SMART-1, the status of upcoming missions,
and the interdisciplinary, technical, programmatic aspects of future
international lunar exploration.
Title: ESA Lunar Polar Lander Study
Authors: Foing, B. H.; Hovland, S.; Lunar Polar Lander Study Team
Bibcode: 2006cosp...36.3719F
Altcode: 2006cosp.meet.3719F
No abstract at ADS
Title: NASA Lunar Exploration Programme
Authors: Foing, B. H.; Ilewg
Bibcode: 2006cosp...36.3727F
Altcode: 2006cosp.meet.3727F
No abstract at ADS
Title: Rationale and Roadmap for Moon Exploration
Authors: Foing, B. H.; ILEWG Team
Bibcode: 2006epsc.conf..651F
Altcode:
We discuss the different rationale for Moon exploration. This starts
with areas of scientific investigations: clues on the formation and
evolution of rocky planets, accretion and bombardment in the inner
solar system, comparative planetology processes (tectonic, volcanic,
impact cratering, volatile delivery), records astrobiology, survival of
organics; past, present and future life. The rationale includes also the
advancement of instrumentation: Remote sensing miniaturised instruments;
Surface geophysical and geochemistry package; Instrument deployment
and robotic arm, nano-rover, sampling, drilling; Sample finder and
collector. There are technologies in robotic and human exploration
that are a drive for the creativity and economical competitivity of
our industries: Mecha-electronics-sensors; Tele control, telepresence,
virtual reality; Regional mobility rover; Autonomy and Navigation;
Artificially intelligent robots, Complex systems, Man-Machine interface
and performances. Moon-Mars Exploration can inspire solutions to
global Earth sustained development: In-Situ Utilisation of resources;
Establishment of permanent robotic infrastructures, Environmental
protection aspects; Life sciences laboratories; Support to human
exploration. We also report on the IAA Cosmic Study on Next Steps In
Exploring Deep Space, and ongoing IAA Cosmic Studies, ILEWG/IMEWG
ongoing activities, and we finally discuss possible roadmaps for
robotic and human exploration, starting with the Moon-Mars missions
for the coming decade, and building effectively on joint technology
developments.
Title: The ORGANICS experiments on BIOPAN V: UV and space exposure
of aromatic compounds
Authors: Ehrenfreund, P.; Ruiterkamp, R.; Peeters, Z.; Foing, B.;
Salama, F.; Martins, Z.
Bibcode: 2006cosp...36.3635E
Altcode: 2006cosp.meet.3635E
We studied the stability of aromatic compounds in low Earth orbit
environment and describe the scientific results and successful flight of
the ORGANICS experiment on-board the BIOPAN V space exposure facility
This experiment investigated the photo stability of large organic
molecules in near Earth orbit Thin films of selected organic molecules
such as polycyclic aromatic hydrocarbons PAHs and the fullerene C 60
were subjected to the near Earth orbit environment and the samples
were monitored before and after flight PAHs and fullerenes have
been proposed as carriers for a number of astronomical absorption
and emission features and are also identified in meteorites Our
experiment on BIOPAN V was exposed to a total fluence of 602 45 kJ m
-2 for photons between 170 and 280 nm The experiment was also intended
as a hardware test-flight for a long-term exposure experiment on the
EXPOSE facility on the International Space Station ISS For the small
fluence that was collected during the BIOPAN V experiment we found
little evidence of photo-destruction The results confirm that PAH
molecules are very stable compounds in space
Title: Astrobiology on the Moon
Authors: Foing, B. H.
Bibcode: 2006cosp...36.3722F
Altcode: 2006cosp.meet.3722F
No abstract at ADS
Title: Rationale and robotics payload for a lunar polar lander
Authors: Foing, B.; Hovland, S.; Les3 Lander Study Team
Bibcode: 2006epsc.conf..652F
Altcode:
We present the results of a study for a lunar polar lander conducted at
ESA CDF Concurrent Design Facility until December 2005. The goal is to
demonstrate lunar landing, survival and exploration technologies for
the future, geochemical studies of the piles, and search for ice in
permanent shadows. We describe the top objectives, mission analysis,
design and associated lander and rover. We also describe the possible
payload complement in discussion with the community. The robotic
payload includes a nanorover, a regional rover with robotic arm and
drilling capability. The sensors include cameras, spectrometers and
analysis facilities.
Title: SMART-1 mission to the Moon: Status, first results and goals
Authors: Foing, B. H.; Racca, G. D.; Marini, A.; Evrard, E.; Stagnaro,
L.; Almeida, M.; Koschny, D.; Frew, D.; Zender, J.; Heather, J.;
Grande, M.; Huovelin, J.; Keller, H. U.; Nathues, A.; Josset, J. L.;
Malkki, A.; Schmidt, W.; Noci, G.; Birkl, R.; Iess, L.; Sodnik, Z.;
McManamon, P.
Bibcode: 2006AdSpR..37....6F
Altcode:
We present the first results from SMART-1's science and technology
payload. SMART-1 is Europe's first lunar mission and will provide some
significant advances to many issues currently active in lunar science,
such as our understanding of lunar origin and evolution. The mission
also contributes a step in developing an international program of
lunar exploration. The spacecraft was launched on 27 September 2003
on an Ariane 5, as an auxiliary passenger to Geostationary Transfer
Orbit (GTO), performed a 14-month long cruise using the tiny thrust
of electric propulsion alone, reached lunar capture in November
2004, and lunar science orbit in March 2005. SMART-1 carries seven
hardware experiments (performing 10 investigations, including three
remote sensing instruments, used during the cruise, the mission's
nominal six months and one year extension in lunar science orbit). The
remote sensing instruments will contribute to key planetary scientific
questions related to theories of lunar origin and evolution, the global
and local crustal composition, the search for cold traps at the lunar
poles and the mapping of potential lunar resources.
Title: Other campaign contributions TBD
Authors: Foing, B.
Bibcode: 2006epsc.conf..724F
Altcode:
No abstract at ADS
Title: SMART-1 Moon impact on 3 Sept 2006: predictions and observation
campaign
Authors: Foing, B. H.; Ehrenfreund, P.; Koschny, D.; Frew, D.;
SMART-1 Impact Campaign Team
Bibcode: 2006epsc.conf..655F
Altcode:
SMART-1 was launched in 2003 and is currently orbiting the Moon on
a 5 hours period until impact around 31 August 2006. The impact will
take place in grazing incidence with mass of 285 kg at a velocity of 2
km/s in a latitude around 37 degree south. A slight thrusting will be
operated in June to fine tune the exact time of contact. At present
possible arrival time scenarios are around 3 Sept 2006, to permit
nearside impact and adequate illumination conditions. We'll describe the
operations until impact. We called the community to make predictions of
impact magnitude, cloud ejecta dynamics, exospheric effects. We also
called the ground based observers to perform coordinated measurements
of the impact. Results from the coordinated multisite campaign will
be discussed.
Title: Other STWT contributions TBD
Authors: Foing, B.
Bibcode: 2006epsc.conf..721F
Altcode:
No abstract at ADS
Title: International lunar missions: results and implications for
astrobiologyInternational lunar missions: results and implications
for astrobiology
Authors: Foing, B. H.; Ilewg
Bibcode: 2006epsc.conf..654F
Altcode:
Results from recent lunar missions have changed our view of the
Moon. ESA SMART1 was launched in 2003 and is currently orbiting the
Moon until impact in August 2006. Lunar orbiters are readying for
launch in 2007 (Japanese SELENE, Indian Chandrayaan-1 orbiter and
the Chinese Chang'E1), as well as US Lunar Reconnaissance Orbiter
in 2008. From 2010 a series of soft lander missions to the Moon
could emplace a global robotic presence with precursor life science
experiments. The results of these missions will continue to answer
open questions about the origin of the Earth-Moon system, the early
evolution of life, the planetary environment and habitability. Lunar
geoscience studies help to understand the origin and evolution of our
unique Earth-Moon system and other rocky planets. Lunar or cislunar
telescopes on the Moon can detect and characterize if life exists
elsewhere in the universe. We can search for samples of the early
Earth on the Moon. We can use in-situ resources necessary to support
future life and human presence (e.g. water, oxygen). The Moon will
be used for life sciences, astrobiology laboratories, human bases and
biospheres that will play a key role in the future of life beyond Earth.
Title: SMART-1 Moon impact around 2-3 Sept 2006: predictions and
observation campaign
Authors: Foing, B. H.; SMART-1 Impact Campaign Team
Bibcode: 2006cosp...36.3723F
Altcode: 2006cosp.meet.3723F
No abstract at ADS
Title: Optimization of plant mineral nutrition under growth-limiting
conditions in a lunar greenhouse
Authors: Zaets, I.; Voznyuk, T.; Kovalchuk, M.; Rogutskyy, I.;
Lukashov, D.; Mytrokhyn, O.; Mashkovska, S.; Foing, B.; Kozyrovska, N.
Bibcode: 2006KosNT..12f..36Z
Altcode:
It may be assumed that the first plants in a lunar base will play a
main role in forming a protosoil of acceptable fertility needed for
purposively growing second generation plants like wheat, rice, tulips,
etc. The residues of the first-generation plants could be composted and
transformed by microorganisms into a soil-like substrate within a loop
of regenerative life support system. The lunar regolith may be used as a
substrate for plant growth at the very beginning of a mission to reduce
its cost. The use of microbial communities for priming plants will
allow one to facilitate adaption to stressful conditions and to support
the plant development under growth limiting conditions. Well-defined
plant-associated bacteria were used for growing three cultivars
to colonize French marigold (Tagetes patula L.) in anorthosite,
a substrate of low bioavailability, analogous to a lunar rock. The
consortium was composed of plant growth promoting rhizobacteria and the
bacterium Paenibacillus sp. IMBG156 which stimulated seed germination,
better plant development, and finally, the flowering of inoculated
tagetes. In contrast, control plants grew poorly in the anorthosite
and practically did not survive until flowering. Analysis of bacterial
community composition showed that all species colonized plant roots,
however, the rate of colonization depended on the allelopatic
characteristics of marigold varieties. Bacteria of consortium
were able to liberate some elements (Ca, Fe, Mn, Si, Ni, Cu, Zn)
from substrate anorthosite. Plant colonization by mixed culture of
bacterial strains resulted in the increase of accumulation of K,
Mg, Mn by the plant and in the lowering of the level of toxic metal
accumulation. It was assumed that a rationally assembled consortium of
bacterial strains promoted germination of marygold seeds and supported
the plant development under growth limiting conditions by means of
bioleaching plant essential nutritional elements and by protecting
the plant against hyperaccumulation of some toxic metals.
Title: Highlights of SMART-1 Lunar Mission
Authors: Foing, B. H.; SMART-1 Team
Bibcode: 2006cosp...36.3720F
Altcode: 2006cosp.meet.3720F
No abstract at ADS
Title: Analysis of the SMART-1 impact flash as seen from several
observatories in Spain
Authors: Ortiz, J. L.; Llorca, J.; Foing, B. H.; Koschny, D.;
Trigo-Rodriguez, J. M.; Lopez-Moreno, J. J.; Aceituno, F. J.;
Santos-Sanz, P.; Morales, N.; Moreno, F.
Bibcode: 2006epsc.conf..347O
Altcode:
The first results of our scheduled SMART-1 impact observations
from Calar Alto, Sierra Nevada and other observatories in Spain are
presented. The emphasis is made on the determination of the luminous
efficiency of the impact at different wavelength ranges from the
optical to the near infrared.
Title: Regional mapping and structural analysis of Aram Chaos area
Authors: Oosthoek, J. H. P.; Zegers, T. E.; Rossi, A. P.; Martin,
P.; Foing, B.; Neukum, G.
Bibcode: 2006epsc.conf..560O
Altcode:
Aram Chaos is a typical chaotic terrain within a ∼280 km crater
located 2.5o N and 338.5o E, in the Xanthe and Margaritifer Terrae
(XMT) region. Most large craters in the XMT region, such as the Aram
Chaos crater, formed in the Noachian Period. In the subsequent Hesperian
Period and into the Amazonian Period the XMT region has been dissected
by five of the circum-Chryse outflow channels: Shalbatana, Simud, Tiu,
Ares and Mawrth Valles. We are mapping and analysing the geology of
Aram Chaos using (1) HRSC image data from the ESA Mars Express orbiter,
(2) THEMIS and MOC image data and MOLA elevation data.. The data was
processed and map projected and incorporated in ESRI ArcGIS. HRSC
data is particularly important in this mapping study. The large swath
width, the high resolution, and the sharpness of the images combine
both context and detail in one image. In addition, HRSC anaglyphs were
incorporated in the GIS database. Using red/blue glasses, these provide
direct detailed elevation information, essential to geometry based
geological mapping. Apart from the general mapping the focus of this
study is on (1) investigating the structural and geometric relations
of the chaotic terrain and the surrounding Noachian cratered terrain,
and (2) investigating the light toned deposits in the chaotic terrain
and their relation to the chaotic terrain and outflow channels. 5
major units were distinguished: Highland terrain, Fractured highland
terrain, Intermediate chaotic terrain, Chaos floor terrain and Light
toned deposits. Inside Aram Chaos a morphologically distinct chaotic
terrain unit was mapped which also shows a distinct fault pattern. The
outflow channels were considered geomorphological units and the channel
flow boundaries and directions are shown as lines in the map. Faults
and fault blocks were mapped. On the Aram Chaos end of the channel
connecting Ares Vallis and Aram Chaos a delta-like feature is located.
Title: Planetary science: Are there active glaciers on Mars? (Reply)
Authors: Head, J. W.; Neukum, G.; Jaumann, R.; Hiesinger, H.; Hauber,
E.; Carr, M.; Masson, P.; Foing, B.; Hoffmann, H.; Kreslavsky, M.;
Werner, S.; Milkovich, S.; van Gasselt, S.; HRSC Co-Investigator Team
Bibcode: 2005Natur.438E..10H
Altcode:
Gillespie et al. concur with our interpretation that certain lobate
equatorial and mid-latitude features on Mars are due to debris-covered
glaciers formed largely during past periods of increased spin-axis
obliquity, when climate regimes favoured snow and ice accumulation
and glacial flow. They suggest that the `hourglass' deposit, dated at
more than 40 Myr old, could be active today owing to an additional
mechanism that supports ``local augmentation of accumulation from
snowfall'' without climate change on Mars. This mechanism requires
the present, or very recent, release of groundwater to the surface
to form aufeis (groundwater-fed `glaciers') where the groundwater is
generated by dewatering of hydrous compounds or melting by magmatic or
impact-generated heat. We assess whether this suggestion applies to
the deposits in question - it was previously proposed for much older
deposits in other areas of Mars. We make particular reference to the
key relationships in the accumulation zones.
Title: SMART-1 after lunar capture: First results and perspectives
Authors: Foing, B. H.; Racca, G. D.; Marini, A.; Evrard, E.; Stagnaro,
L.; Almeida, M.; Koschny, D.; Frew, D.; Zender, J.; Heather, D.;
Grande, M.; Huovelin, J.; Keller, H. U.; Nathues, A.; Josset, J. L.;
Malkki, A.; Schmidt, W.; Noci, G.; Birkl, R.; Iess, L.; Sodnik, Z.;
McManamon, P.
Bibcode: 2005JESS..114..689F
Altcode:
No abstract at ADS
Title: From Crater to Graph: Manual and Automated Crater Counting
Techniques
Authors: Plesko, C. S.; Werner, S. C.; Brumby, S. P.; Foing, B. H.;
Asphaug, E.; Neukum, G.; Team, H.; Team, I.
Bibcode: 2005AGUFM.P23A0185P
Altcode:
Impact craters are some of the most abundant, and most interesting
features on Mars. They hold a wealth of information about Martian
geology, providing clues to the relative age, local composition and
erosional history of the surface. A great deal of effort has been
expended to count and understand the nature of planetary crater
populations (Hartman and Neukum, 2001). Highly trained experts have
developed personal methods for conducting manual crater surveys. In
addition, several efforts are underway to automate this process in
order to keep up with the rapid increase in planetary surface image
data. These efforts make use of a variety of methods, including the
direct application of traditional image processing algorithms such as
the Hough transform, and recent developments in genetic programming,
an artificial intelligence-based technique, in which manual crater
surveys are used as examples to `grow' or `evolve' crater counting
algorithms. (Plesko, C. S. et al., LPSC 2005, Kim, J. R. et al., LPSC
2001, Michael, G. G. P&SS 2003, Earl, J. et al, LPSC 2005) In this
study we examine automated crater counting techniques, and compare them
with traditional manual techniques on MOC imagery, and demonstrate
capabilities for the analysis of multi-spectral and HRSC Digital
Terrain Model data as well. Techniques are compared and discussed to
define and develop a robust automated crater detection strategy.
Title: SMART-1 Mission: First Lunar Results
Authors: Foing, B. H.
Bibcode: 2005AGUFM.P51A0892F
Altcode:
The SMART-1 mission arrived in lunar science orbit in March
2005. We'll present results obtained during the nominal science
phase of the mission, using the AMIE camera for geology context,
SIR infrared spectrometer for mineralogy distrbution and the D-CIXs
X-ray spectrometer for elemental mapping. SMART-1 contributes to the
themes of geophysics(volcanism, cratering, tectonics) and geochemistry
constraints on Moon formation and evolution. It is also used for
monitoring illumination, mapping resources, and preparation of future
international lunar missions. We'll describe also the planning for the
mission extension from October 2005 to August 2006, and the involvement
of the science community.
Title: The life of stars and their planets
Authors: Catala, C.; Aerts, C.; Aigrain, S.; Antonello, E.;
Appourchaux, T.; Auvergne, M.; Baglin, A.; Barge, P.; Barstow, M. A.;
Baudin, F.; Boumier, P.; Collier Cameron, A.; Christensen-Dalsgaard,
J.; Cutispoto, G.; Deeg, H.; Deleuil, M.; Desidera, S.; Donati, J. -F.;
Favata, F.; Foing, B. H.; Gameiro, J. F.; Garcia, R.; Garrido, F.;
Horne, K.; Lanza, A. F.; Lanzafame, A. C.; Lecavelier Des Etangs,
A.; Léger, A.; Mas-Hesse, M.; Messina, S.; Micela, G.; Michel, E.;
Monteiro, M. J. P. F. G.; Mosser, B.; Noels, A.; Pagano, I.; Piotto,
G.; Poretti, E.; Rauer, H.; Roca-Cortes, T.; Rodono, M.; Rouan, D.;
Roxburgh, I.; Schneider, J.; Strassmeier, K.; Turck-Chièze, S.;
Vauclair, S.; Vidal-Madjar, A.; Weiss, W. W.; Wheatley, P.
Bibcode: 2005ESASP.588...99C
Altcode: 2005tssc.conf...99C
We lack a reliable scenario for the formation and evolution of stars
and their planetary systems, involving key factors such as magnetic
fields and turbulence. We present the case for a mission concept that
will clarify these problems and give us a global view of the evolution
of combined star and planetary systems. This will be achieved by
simultaneously addressing the search for planetary transits in front
of a large number of stars, including many nearby stars, the study of
their internal structure and evolution via asteroseismology, and that
of their magnetic activity, via UV monitoring.
Title: The advanced Moon micro-imager experiment (AMIE) on SMART-1:
Scientific goals and expected results
Authors: Pinet, P.; Cerroni, P.; Josset, J. -L.; Beauvivre, S.;
Chevrel, S.; Muinonen, K.; Langevin, Y.; Barucci, M. A.; De Sanctis,
M. C.; Shkuratov, Yu.; Shevchenko, V.; Plancke, P.; Hofmann, B. A.;
Josset, M.; Ehrenfreund, P.; Sodnik, Z.; Koschny, D.; Almeida, M.;
Foing, B.
Bibcode: 2005P&SS...53.1309P
Altcode:
The advanced Moon micro-imager experiment (AMIE) is the imaging system
on board ESA mission to the Moon SMART-1; it makes use of a miniaturised
detector and micro-processor electronics developed by SPACE X in the
frame of the ESA technical programme. The AMIE micro-imager will provide
high resolution CCD images of selected lunar areas and it will perform
colour imaging through three filters at 750, 915 and 960 nm with a
maximum resolution of 46 m/pixel at the perilune of 500 km. Specific
scientific objectives will include (1) imaging of high latitude regions
in the southern hemisphere, in particular the South Pole Aitken basin
(SPA) and the permanently shadowed regions close to the South Pole,
(2) determination of the photometric properties of the lunar surface
from observations at different phase angles (physical properties of
the regolith), (3) multi-band imaging for constraining the chemical and
mineral composition of the surface, (4) detection and characterisation
of lunar non-mare volcanic units, (5) study of lithological variations
from impact craters and implications for crustal heterogeneity. The
AMIE micro-imager will also support a Laser-link experiment to Earth,
an On Board Autonomous Navigation investigation and a Lunar libration
experiment coordinated with radio science measurements.
Title: SMART-1 Mission Overview: Lunar Results and Perspectives
Authors: Foing, B. H.; SMART-1 Team
Bibcode: 2005DPS....37.4802F
Altcode: 2005BAAS...37..731F
SMART-1 is the first ESA mission that reached the Moon. It is the
first of Small Missions for Advanced Research and Technology as
part of ESA science programme Cosmic Vision. Its objective is to
demonstrate Solar Electric Primary Propulsion (SEP) for future
Cornerstones (such as Bepi-Colombo) and to test new technologies
for spacecraft and instruments. The spacecraft was launched on 27
Sept. 2003, as Ariane-5 auxiliary passenger, left the inner radiation
belt, and spiralled out towards lunar capture on 15 November 2004,
and then towards lunar science orbit reached on 1 March 2005. The
mission has been extended until August 2006. This will permit science
but also to prepare future international lunar exploration. We shall
present an overiew of the mission, and of the first lunar results from
SMART-1's science and technology payload, featuring many innovative
instruments and advanced technologies with a total mass of some 19
kg. Besides navigation to the Moon, the technology demonstration
included an experiment (KaTE) for deep-space communications in the X
and Ka-bands, a radio-science experiment (RSIS), a deep space optical
link (Laser-Link Experiment), using the ESA Optical Ground station
in Tenerife, and the validation of a system of autonomous navigation
(OBAN). The payload includes a miniaturized high-resolution camera
(AMIE) for lunar surface imaging, a near-infrared point-spectrometer
(SIR) for lunar mineralogy investigation, and a very compact X-ray
spectrometer (D-CIXS) measuring fluorescence spectroscopy and imagery
of the Moon's surface elemental composition. SMART-1 lunar science
investigations include studies of the chemical composition of the Moon,
of geophysical processes (volcanism, tectonics, cratering, erosion,
deposition of ices and volatiles) for comparative planetology, and
high resolution studies in preparation for future steps of lunar
exploration. The mission could address several topics such as the
accretional processes that led to the formation of rocky planets,
and the origin and evolution of the Earth-Moon system.
Title: Amino acid photostability on the Martian surface
Authors: ten Kate, I. L.; Garry, J. R. C.; Peeters, Z.; Quinn, R.;
Foing, B.; Ehrenfreund, P.
Bibcode: 2005M&PS...40.1185T
Altcode:
No abstract at ADS
Title: SMART-1: Development and lessons learnt
Authors: Rathsman, Peter; Kugelberg, Joakim; Bodin, Per; Racca,
Giuseppe D.; Foing, Bernard; Stagnaro, Luca
Bibcode: 2005AcAau..57..455R
Altcode:
SMART-1 is the first of the small missions for advanced research and
technology as part of ESA's science programme “Cosmic vision”. It
was successfully launched on September 27, 2003 and is presently
traveling towards its destination, the Moon. The main objective of the
mission, to demonstrate solar electric primary propulsion for future
Cornerstones (such as Bepi-Colombo), has already been achieved. At the
time of writing the electric propulsion system has been working already
for more than 3400 h and has provided a Delta-V to the spacecraft
of more than 2500 m/s. The other technology objectives are also being
fulfilled by the verification of the proper functioning of such on-board
experiments like the X-Ka band transponder, the X-ray spectrometer,
the near IR spectrometer, the laser link, etc. The scientific objectives
are related to lunar science and will be fulfilled once the spacecraft
enters its operational lunar orbit, currently expected for January
2005. SMART-1 lunar science investigations will include studies
of the chemical composition of the Moon, of geophysical processes,
environment and high-resolution studies in preparation for future
steps of lunar exploration. SMART-1 has been an innovative mission in
many aspects and we are now drawing some preliminary conclusions about
the lessons to be learnt. The paper describes the spacecraft and the
technology elements with particular emphasis to the technology nature
of the mission. The on-board avionics employs many novel designs
for spacecraft, including a serial CAN bus for data communication,
autonomous star trackers and extensive use of auto-code generation for
implementing the attitude control system and the failure, detection,
isolation and recovery (FDIR). Finally, the orbital operation phase
currently ongoing, including the routine electric propulsion operations
and the instrument commissioning, is providing a wealth of data and
lesson-learnt useful for future autonomous planetary missions.
Title: Diffuse interstellar bands of unprecedented strength in
the line of sight towards high-mass X-ray binary 4U
1907+09
Authors: Cox, N. L. J.; Kaper, L.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 2005A&A...438..187C
Altcode:
High-resolution VLT/UVES spectra of the strongly reddened O supergiant
companion to the X-ray pulsar 4U 1907+09 provide a
unique opportunity to study the nature of the diffuse interstellar bands
(DIBs) at unprecedented strength. We detect about 180 known DIBs, of
which about 25 were listed as tentative and are now confirmed. A dozen
new DIB candidates longwards of 6900 Å are identified. We show that the
observed 5797 Å DIB strength is in line with the Galactic correlation
with reddening, whereas the 5780 Å DIB strength is relatively
weak. This indicates the contribution of denser regions, where the UV
penetration is reduced. The presence of dense cloud cores is supported
by the detection of C2 rotational transitions. Members of one DIB family
(5797, 6379 Å and 6196, 6613 Å) behave coherently, although one can
make a distinction between the two correlated pairs. The broadened
profiles of narrow DIBs are shown to be consistent with the premise
that each of the main clouds in the line of sight discerned in the
interstellar K I profile is contributing proportionally to the DIB
profile. We complement and extend the relation of DIB strength with
reddening {E}(B-V), as well as with neutral hydrogen column
density N(H I), respectively, using strongly reddened sightlines towards
another four distant HMXBs. The 5780 Å DIB, and tentatively also the
5797 and 6613 Å DIBs, are better correlated to the gas tracer H I than
to the dust tracer {E}(B-V). The resulting relationship
can be applied to any line of sight to obtain an estimate of the H
I column density. In the search for the nature of the DIB carrier,
this strongly reddened line of sight is a complementary addition to
single cloud line of sight studies.
Title: Fluid lava flows in Gusev crater, Mars
Authors: Greeley, Ronald; Foing, Bernard H.; McSween, Harry Y.;
Neukum, Gerhard; Pinet, Patrick; van Kan, Mirjam; Werner, Stephanie
C.; Williams, David A.; Zegers, Tanja E.
Bibcode: 2005JGRE..110.5008G
Altcode:
Rocks on the floor of Gusev crater are basaltic in composition,
as determined from measurements by the Mars Exploration Rover,
Spirit. On the basis of compositional data, models of the basaltic
lavas at the time of their emplacement suggest viscosities of 2.3 to 50
Pa . s (dependent on the number of phenocrysts and vesicles that were
present), which would be more fluid than terrestrial tholeiitic lavas
and comparable to mare lavas on the Moon or Archean high-Mg basalts
on Earth. Morphological data and crater counts derived from the High
Resolution Stereo Camera on Mars Express and other orbiters suggest that
the lavas flooded Gusev crater at about 3.65 b.y. and postdate older
floor materials, such as putative sediments emplaced by Ma'adim Vallis.
Title: PAH charge state distribution and DIB carriers: Implications
from the line of sight toward HD 147889
Authors: Ruiterkamp, R.; Cox, N. L. J.; Spaans, M.; Kaper, L.; Foing,
B. H.; Salama, F.; Ehrenfreund, P.
Bibcode: 2005A&A...432..515R
Altcode:
We have computed physical parameters such as density, degree of
ionization and temperature, constrained by a large observational data
set on atomic and molecular species, for the line of sight toward the
single cloud HD 147889. Diffuse interstellar bands
(DIBs) produced along this line of sight are well documented and can
be used to test the PAH hypothesis. To this effect, the charge state
fractions of different polycyclic aromatic hydrocarbons (PAHs) are
calculated in HD 147889 as a function of depth for
the derived density, electron abundance and temperature profile. As
input for the construction of these charge state distributions, the
microscopic properties of the PAHs, e.g., ionization potential and
electron affinity, are determined for a series of symmetry groups. The
combination of a physical model for the chemical and thermal balance of
the gas toward HD 147889 with a detailed treatment of
the PAH charge state distribution, and laboratory and theoretical data
on specific PAHs, allow us to compute electronic spectra of gas phase
PAH molecules and to draw conclusions about the required properties
of PAHs as DIB carriers. We find the following. 1) The variation of
the total charge state distribution of each specific class (series)
of PAH in the translucent cloud toward HD 147889
(and also of course for any other diffuse/translucent cloud)
depends strongly on the molecular symmetry and size (number of π
electrons). This is due to the strong effects of these parameters on
the ionization potential of a PAH. 2) Different wavelength regions in
the DIB spectrum are populated preferentially by different PAH charge
states depending on the underlying PAH size distribution. 3) The PAH
size distribution for HD 147889 is constrained by the
observed DIB spectrum to be Gaussian with a mean of 50 carbon atoms. 4)
For the given PAH size distribution it is possible to constrain the
total small catacondensed PAH column density along the line of sight to
HD 147889 to 2.4×1014 cm-2 by
comparing the total observed UV extinction to the strong UV absorptions
of neutral PAHs in the 2000-3000 Å region. 5) Catacondensed PAHs with
sizes above some 40 C-atoms are expected to show strong DIBS longward
of 10 000 Å. Large condensed PAHs in the series, pyrene, coronene,
ovalene, .... , on the other hand, mainly absorb between 4000 and 10
000 Å but extrapolation to even larger pericondensed PAHs in this
series also shows strong absorptions longward of 10 000 Å. 6) Only
the weak DIBs in HD 147889 could be reproduced by
a mix of small catacondensed PAHs (<50 C atoms) while for large
pericondensed PAHs (50 < C atoms < 100) the intermediate DIBs
are well reproduced. Small catacondensed PAHs cannot contribute more
than 50% of the total observed equivalent width toward HD
147889. Strong DIBs can only be reproduced by addition of
very specific PAH molecules or homologue series to the sample set
(i.e., a small number of PAHs with high oscillator strength or a large
number of PAHs with a low oscillator strength). An outline is provided
for a more general application of this method to other lines of sight,
which can be used as a pipeline to compute the spectroscopic response
of a PAH or group of PAHs in a physical environment constrained by
independent (non-DIB) observations. Based on observations made
at the European Southern Observatory, Paranal, Chile (ESO programs
67.C-0281 and 64.H-0224). Appendices A-C are only available in
electronic form at http://www.edpsciences.org
Title: Evidence from HRSC Mars Express for a Frozen Sea Close to
Mars' Equator
Authors: Murray, J. B.; Muller, J. -P.; Neukum, G.; Werner, S. C.;
Hauber, E.; Markiewicz, W. J.; Head, J. W., III; Foing, B. H.; Page,
D.; Mitchell, K. L.; Portyankina, G.; HRSC Investigator Team
Bibcode: 2005LPI....36.1741M
Altcode:
We present evidence for a presently-existing frozen sea, with surface
pack-ice, at 5° N, 150° E, age c. 5 million years. It measures c. 800
x 900 km and averages c. 45 m deep. It has probably been protected from
complete sublimation by ash and a sublimation lag of exposed sediment.
Title: ESA's SMART-1 Mission at the Moon: First Results, Status and
Next Steps
Authors: Foing, B. H.; Racca, G. D.; Grande, M.; Huovelin, J.; Josset,
J. L.; Keller, H. U.; Nathues, A.; Malkki, A.; Heather, D.; Koschny,
D.; Almeida, M.; Frew, D.; Lumb, R.; Volp, J.; Zender, J.
Bibcode: 2005LPI....36.2404F
Altcode:
ESA's SMART-1 is at the Moon! Launched by Ariane-5 in Sept. 2003,
it used primary solar electric propulsion to reach lunar capture on
17 November 2004, and to spiral down to lunar science orbit. First
data and results from the cruise approach and lunar commissioning will
be presented.
Title: Evidence from the Mars Express High Resolution Stereo Camera
for a frozen sea close to Mars' equator
Authors: Murray, John B.; Muller, Jan-Peter; Neukum, Gerhard; Werner,
Stephanie C.; van Gasselt, Stephan; Hauber, Ernst; Markiewicz, Wojciech
J.; Head, James W.; Foing, Bernard H.; Page, David; Mitchell, Karl L.;
Portyankina, Ganna; HRSC Co-Investigator Team
Bibcode: 2005Natur.434..352M
Altcode:
It is thought that the Cerberus Fossae fissures on Mars were the source
of both lava and water floods two to ten million years ago. Evidence
for the resulting lava plains has been identified in eastern Elysium,
but seas and lakes from these fissures and previous water flooding
events were presumed to have evaporated and sublimed away. Here we
present High Resolution Stereo Camera images from the European Space
Agency Mars Express spacecraft that indicate that such lakes may still
exist. We infer that the evidence is consistent with a frozen body of
water, with surface pack-ice, around 5° north latitude and 150° east
longitude in southern Elysium. The frozen lake measures about 800 ×
900km in lateral extent and may be up to 45metres deep-similar in size
and depth to the North Sea. From crater counts, we determined its age
to be 5 +/- 2 million years old. If our interpretation is confirmed,
this is a place that might preserve evidence of primitive life, if it
has ever developed on Mars.
Title: Fluid Lava Flows in Gusev Crater, Mars
Authors: Greeley, R.; Williams, D. A.; Neukum, G.; Werner, S. C.;
Zegers, T. E.; Foing, B. H.; van Kan, M.; Lanagan, P. D.; Pinet,
P. C.; Mars Express HRSC Team
Bibcode: 2005LPI....36.2094G
Altcode:
Basaltic rocks in Gusev are modeled to have viscosities of 2.3 to 50
Pa•s at the time of eruption and thus were emplaced as very fluid
flood lavas, consistent with the morphologies seen in orbiter data,
at 3.65 by based on crater counts.
Title: Mountainous Units in the Martian Gusev Highland Region:
Volcanic, Tectonic, or Impact Related?
Authors: Zegers, T. E.; van Kan, M.; Foing, B. H.; Pischel,
R.; Gwinner, K.; Scholten, F.; Werner, S. C.; Neukum, G.; HRSC
Co-Investigator Team
Bibcode: 2005LPI....36.1651Z
Altcode:
Geological mapping and structural analysis of the highland region of
Gusev crater was carried out, combining THEMIS and HRSC image data and
HRSC digital terrain models (DTM), based on HRSC stereo capabilities.
Title: Tropical to mid-latitude snow and ice accumulation, flow and
glaciation on Mars
Authors: Head, J. W.; Neukum, G.; Jaumann, R.; Hiesinger, H.; Hauber,
E.; Carr, M.; Masson, P.; Foing, B.; Hoffmann, H.; Kreslavsky, M.;
Werner, S.; Milkovich, S.; van Gasselt, S.; HRSC Co-Investigator Team
Bibcode: 2005Natur.434..346H
Altcode:
Images from the Mars Express HRSC (High-Resolution Stereo Camera)
of debris aprons at the base of massifs in eastern Hellas reveal
numerous concentrically ridged lobate and pitted features and
related evidence of extremely ice-rich glacier-like viscous flow
and sublimation. Together with new evidence for recent ice-rich rock
glaciers at the base of the Olympus Mons scarp superposed on larger
Late Amazonian debris-covered piedmont glaciers, we interpret these
deposits as evidence for geologically recent and recurring glacial
activity in tropical and mid-latitude regions of Mars during periods
of increased spin-axis obliquity when polar ice was mobilized and
redeposited in microenvironments at lower latitudes. The data indicate
that abundant residual ice probably remains in these deposits and that
these records of geologically recent climate changes are accessible
to future automated and human surface exploration.
Title: Attitude Determination of Geological Layers Using HRSC Data
and Orion Software
Authors: Fueten, F.; Stesky, R.; MacKinnon, P.; Zegers, T. E.; Hauber,
E.; Foing, B. H.; Pischel, R.; Gwinner, K.; Scholten, F.; Neukem,
G.; HRSC Co-Investigator Team
Bibcode: 2005LPI....36.1498F
Altcode:
Attitude of ILD layering in Valles Marineris, Mars, is measured using
HRSC data and Orion software.
Title: Macroscopic Texture of the Martian Surface: Application of
a Filtering Method Using Mars Express HRSC Data
Authors: Cord, A.; Martin, P.; Foing, B. H.; Jaumann, R.; Hauber,
E.; Hoffman, H.; Neukum, G.; HRSC Co-Investigator Team
Bibcode: 2005LPI....36.1615C
Altcode:
We quantify the texture of Martian surface at the scale of a few pixels
using images from HRSC (Mars Express). This can be linked with the
relative thickness of dust deposit and then with some geological and
geomorphological properties of the surface.
Title: Evolutionary History of Gusev -- The MER Landing Site --
Seen by MEX-HRSC
Authors: Werner, S. C.; Ivanov, B. A.; Neukum, G.; van Kan, M.;
Zegers, T. E.; Foing, B. H.; Greeley, R.; Williams, D. A.; HRSC
Co-Investigator Team
Bibcode: 2005LPI....36.1777W
Altcode:
The evolutionary history of Gusev and its vicinity is
discussed. Comparing Gusev--sized impact craters the level of infill
of Gusev is about 1 -- 1.5 km more than for others, possibly due to
the contribution of fluvial activity of Ma'adim Vallis.
Title: Photometric and Compositional Surface Properties of the Gusev
Crater Region, Mars, as Derived from Multi-Angle, Multi-Spectral
Investigation of Mars Express HRSC Data
Authors: Martin, P. D.; Cord, A.; Foing, B. H.; Zegers, T. E.; van Kan,
M.; Pinet, P. C.; Daydou, Y.; Hoffmann, H.; Hauber, E.; Jaumann, R.;
Neukum, G.; HRSC Co-Investigator Team
Bibcode: 2005LPI....36.1687M
Altcode:
The focus of this investigation is to use the potential of the HRSC
multi-angular and multi-spectral data sets for identifying photometric,
color and compositional units and their heterogeneity.
Title: Diurnal Variability in Martian Atmospheric Water Vapour:
Near Surface Ice Out of Equilibrium as a Source
Authors: Boettger, H. M.; Foing, B. H.; Read, P. L.; Lewis, S. R.
Bibcode: 2005LPI....36.1647B
Altcode:
We attempt to reconcile model and observationsal data from GRS and
atmospheric probes, in reference to the diurnal behaviour of atmospheric
water vapour.
Title: Evidence for Snow and Ice Accumulation Aiding Debris Flow
and Glacial Flow at Mid- to Low-Latitudes on Mars
Authors: Hiesinger, H.; Head, J. W., III; Neukum, G.; Jaumann, R.;
Hauber, E.; Carr, M. H.; Masson, Ph.; Foing, B. H.
Bibcode: 2005LPI....36.1988H
Altcode:
HRSC image data show debris aprons suggesting extremely ice-rich
glacier-like viscous flow and sublimation, and ice-rich debris-covered
glaciers suggesting geologically recurring glacial activity in low-
and mid-latitude regions.
Title: Extra-Galactic Diffuse Interstellar Bands
Authors: Cox, N.; Ehrenfreund, Pascale; Kaper, Lex; Spaans, Marco;
Foing, Bernard
Bibcode: 2005IAUS..231P.267C
Altcode: 2005IAUS..235P.267C
Diffuse Interstellar Bands (DIBs) have been observed ubiquitously
along many sight-lines probing the interstellar medium of the Milky
Way. Despite extensive efforts, their carrier(s) have not yet been
identified, although they are very likely of a carbonaceous nature
and reside in the gas phase. Possible candidates include, but are
not limited to, polycyclic aromatic hydro- carbons (PAHs), fullerenes
and carbon chains. To advance our understanding of DIB behaviour and
thus DIB carrier properties we need to study environments inherently
different from those observed in the Milky Way. Only recent advances
in instrumentation and telescope capabilities are providing us with
new exciting possibilities for extra-galactic DIB research. We
present here a selection of our recent observational results for
(extra)-galactic DIBs in the Local Group and beyond. In particular,
DIBs in the Magellanic Clouds and in the spiral galaxy NGC1448. These
first results show surprising similarities between certain DIB profiles
as well as differences in DIB behaviour. Understanding diffuse cloud
chemistry, in particular with respect to complex (carbonaceous)
molecules, is crucial to any DIB carrier identification. In this
respect, external galaxies offer a unique window as they exhibit local
interstellar conditions (such as metallicity, UV-field and gas-to-dust
ratio) very different from those observed in the Milky Way. We discuss
briefly the effect of metallicity and the gas-to-dust ratio on the
physi-chemical properties of diffuse clouds and the subsequent effects
on the PAH charge state distribution and the DIB carriers.
Title: Magellanic Diffuse Interstellar Bands and Carbon Chemistry
Authors: Ehrenfreund, P.; Cox, N.; Cami, J.; Foing, B. H.; Kaper,
L.; D'Hendecourt, L.; Maier, J. P.; Salama, F.; Sarre, P.; Snow, T.;
Sonnentrucker, P.
Bibcode: 2005HiA....13..864E
Altcode:
With the Ultraviolet Visual Echelle Spectrograph mounted at the Very
Large Telescope we have observed at unprecedented spectral resolution
the absorption spectrum toward reddened stars in the Magellanic Clouds
over the wavelength range of 3500-10500 Å. This range covers the
strong transitions associated with neutral and charged large carbon
molecules of varying sizes and structures. We report the first detection
of diffuse interstellar bands (DIBs) at 5780 and 5797 Å in the Small
Magellanic Cloud and the variation of the 6284 Å DIB toward several
targets in the Large Magellanic Cloud. The variation of DIBs in the
Magellanic Clouds compared with Galactic targets may be governed
by a combination of the different chemical processes prevailing in
low-metallicity regions and the local environmental conditions. The
analysis of high-resolution absorption spectra allows us to reveal
the global effects in the chemistry and recycling of cosmic dust in
the Magellanic clouds which are relevant for the chemical pathways
forming large organic molecules in external galaxies.
Title: First results — Lunar X-ray mapping spectrometer on smart-1
Authors: Grande, Manuel; Kellett, B.; Howe, C.; Perry, C. H.;
Swinyard, B.; Dunkin, S.; Huovenin, J.; Thomas, N.; Mall, U.; Hughes,
D.; Alleyne, H.; Russell, S.; Grady, M.; Lundin, R.; Barabash, S.;
Baker, D.; Murray, C. D.; Guest, J. E.; Crawford, I.; Casanova, I.;
Maurice, S.; Gasnault, O.; Foing, B.; Lawrence, D.; Fernandez, V.
Bibcode: 2005CIBu..163...18G
Altcode: 2005SpReT.163...18G
No abstract at ADS
Title: Wind Patterns at the Mars Exploration Rover (MER) Sites
Inferred from Mars Express HRSC and MER Images
Authors: Greeley, R.; Thompson, S.; Whelley, P.; Neukum, G.; Squyres,
S.; Sullivan, R. J.; Rafkin, S. C.; Michaels, T.; Golombek, M. P.;
Arvidson, R.; Foing, B. H.; Richter, L.; Rongxing, L.; Pinet, P.;
HRSC Science Team,.; Athena Science Team
Bibcode: 2004AGUFM.P21B..05G
Altcode:
Various wind-related features exist at the Spirit (Gusev) and
Opportunity (Sinus Meridiani) sites, including those seen from
the surface (e.g., ripples, "wind tails" associated with rocks,
and ventifacts), and from orbit (e.g., linear low-albedo patterns,
some of which change with time). The orientations of these features
suggest that formative winds at the Spirit site are from the northwest,
consistent with predictions of prevailing winds from the Mars Regional
Atmospheric Modeling System (MRAMS). Most of the aeolian features seen
from orbit at the Spirit site are dark tracks thought to represent
the passage of dust devils. HRSC images show that many tracks formed
recently, including the one on which Spirit landed; MER Microscopic
Imager data show that sands within the track zone are moderately
dust free, while sands outside the track are dusty. Thus, dark dust
devil tracks here and perhaps elsewhere on Mars are confirmed to
represent the removal of bright dust to expose a darker substrate,
which, at the Spirit site, consists of coarser-grained sands and
granules in the bedforms and silt- to fine-sand in the soils. MRAMS
suggests that strong winds occur in the afternoon in Gusev crater, a
time consistent with dust-devil formation on both Earth and Mars. At
the Meridiani site, prevailing wind-related features seen from orbit
are bright wind streaks associated with craters, the orientations of
which suggest formative winds from the northwest. Detailed mapping of
aeolian features using MER data shows that local topography (such as
craters and other depressions) at both rover sites can have a strong
influence on the inferred wind patterns. Thus, data from both orbit
and the surface are required to determine the general wind regime.
Title: Gusev Crater and Early Martian History: Clues from Mars-Express
& MGS Study
Authors: Foing, B. H.; Zegers, T. E.; van Kan, M.; Pischel, R.; Martin,
P.; Jaumann, R.; Hauber, E.; Greeley, R.; Hoffmann, H.; Neukum, G.;
HRSC Co-Investigator Team
Bibcode: 2004emge.conf.8070F
Altcode:
No abstract at ADS
Title: High Temporal Resolution Spectroscopic Observations of the
Flare Star V1054 Oph
Authors: Crespo-Chacón, Inés; Montes, David; Fernández-Figueroa,
María José; López-Santiago, Javier; García-Alvarez, David; Foing,
Bernard H.
Bibcode: 2004Ap&SS.292..697C
Altcode:
We present the results of a high temporal resolution spectroscopic
monitoring of the flare (UV Cet type) star V1054 Oph (Wolf 630AB),
classified as a dM3.5e visual binary system. Intermediate resolution
spectra have been taken during four nights (2 5 April 2001) using
the IDS spectrograph of the 2.5 m Isaac Newton Telescope (INT)
(La Palma, Canary Islands, Spain). The V1054 Oph spectra show very
strong emission lines even in its quiescent state. The analysis of the
temporal evolution of the observed emission lines (from Hβ
to H11 and the Ca II H and K lines) reveals four strong
flares and several weak flares. We have studied in detail the behaviour
of the chromospheric lines during the different phases (pre-flare,
impulsive and gradual decay) of these flares. The observed flares
last from ∼25 to 95 min. The equivalent width of the Hβ
line changes by a factor up to ∼2.3. Broad wings and asymmetric
(red-shifted) lines are observed as well.
Title: Photospheric and stellar wind variability in ɛ Ori (B0 Ia)
Authors: Prinja, R. K.; Rivinius, Th.; Stahl, O.; Kaufer, A.; Foing,
B. H.; Cami, J.; Orlando, S.
Bibcode: 2004A&A...418..727P
Altcode:
We provide direct observational evidence for a link between photospheric
activity and perturbations in the dense inner-most stellar wind regions
of the B supergiant star ɛ Ori. The results, which are relevant to
our understanding of the origin of wind structure, are based on a
multi-spectral line analysis of optical time-series data secured in
1998 using the HEROS spectrograph on the ESO Dutch 0.9-m telescope in
La Silla. A period of ∼1.9 days is consistently identified in Balmer,
He I absorption, and weak metal lines such as Si III and C II. The
primary characteristic is a large-amplitude swaying of the central
absorption trough of the line, with differential velocities in lines
formed at varying depths in the atmosphere. The variance resulting from
the ``S-wave'' velocity behaviour of the lines is constrained within ±
the projected rotation velocity (∼80 km s-1) in the weakest
absorption lines, but extends blue-ward to over -200 km s-1
in Hα. A second (superimposed) 1.9 day signal is present at more
extended blue-ward velocities (to ∼-300 km s-1) in lines
containing stronger circumstellar components. Inspection of archival
optical data from 1996 provides evidence that this modulation signal
has persisted for at least 2.5 years. Non-radial pulsational modelling
is carried out in an attempt to reproduce the key observational
characteristics of the line profile variability. Only limited success
is obtained with prograde (m=-1) modes. The principal S-wave pattern
cannot be matched by these models and remains enigmatic. Based
on observations obtained as part of the MUSICOS 98 campaign from ESO
La Silla, Chile.
Title: ESA's SMART-1 Mission to the Moon: Goals, Status and First
Results
Authors: Foing, B. H.; Racca, G. D.; Marini, A.; Grande, M.; Huovelin,
J.; Josset, J. L.; Keller, H. U.; Nathues, A.; Heather, D.; Koschny,
D.; Malkki, A.
Bibcode: 2004LPI....35.1413F
Altcode:
SMART-1 has been launched on 27 Sept. 2003. We shall report at LPSC2004
on the commissioning and first results from the spacecraft and the
instruments.
Title: Multisite observations of SU Aurigae
Authors: Unruh, Y. C.; Donati, J. -F.; Oliveira, J. M.; Collier
Cameron, A.; Catala, C.; Henrichs, H. F.; Johns-Krull, C. M.; Foing,
B.; Hao, J.; Cao, H.; Landstreet, J. D.; Stempels, H. C.; de Jong,
J. A.; Telting, J.; Walton, N.; Ehrenfreund, P.; Hatzes, A. P.;
Neff, J. E.; Böhm, T.; Simon, T.; Kaper, L.; Strassmeier, K. G.;
Granzer, Th.
Bibcode: 2004MNRAS.348.1301U
Altcode: 2004astro.ph..1081U
We present results from the 1996 Multi-Site Continuous Spectroscopy
(MUSICOS) campaign on the T Tauri star SU Aurigae. We find a 2.7-d
periodicity in the HeI (587.6 nm) line, and somewhat longer, less
well-pronounced periodicities in the Balmer lines and in Na D. Our
observations support the suggestion that the wind and infall signatures
are out of phase on SU Aur. We present Doppler images of SU Aur that
have been obtained from least-squares deconvolved profiles. Images taken
about one rotation apart show only limited overlap, in particular at low
latitudes. This is due in part to limitations in signal-to-noise ratio,
and in part to line-profile deformations that arise from short-lived
and/or non-surface features. The agreement at high latitudes is better
and suggests that at least some longer-lived features are present. The
analysis of Stokes V profiles yields a marginal magnetic field detection
during one of the phases.
Title: Noachian Martian highlands; the habitat of ancient life?
Authors: Zegers, T. E.; Conan, Y. G.; Foing, B. H.
Bibcode: 2004ESASP.545..313Z
Altcode: 2004eab..conf..313Z
No abstract at ADS
Title: Amino Acid Survival Under Ambient Martian Surface UV Lighting
Authors: Garry, J. R. C.; ten Kate, I. L.; Ruiterkamp, R.; Peeters,
Z.; Lehmann, B.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 2004LPI....35.1686G
Altcode:
Thin layers of glycine have been exposed to low ambient pressures and
ultra-violet lighting conditions similar to those on Mars. Scaling times
for sample alteration will be shown for these Mars-like conditions.
Title: Lunar Elemental Composition and Ivestigations with D-CIXS
X-Ray Mapping Spectrometer on SMART-1
Authors: Grande, M.; Dunkin, S.; Howe, C.; Browning, R.; Kellett,
B.; Perry, C. H.; Swinyard, B.; Waltham, N.; Kent, B.; Huovenin, J.;
Thomas, N.; Mal, U.; Hughes, D.; Alleyne, H.; Russell, S.; Grady,
M.; Lundin, R.; Barabash, S.; Baker, D.; Murray, C. D.; Guest, J.;
Casanova, I.; Maurice, S.; Foing, B.
Bibcode: 2004LPI....35.1519G
Altcode:
The D-CIXS Compact X-ray Spectrometer on ESA SMART-1 successfully
launched in Sept 2003 can derive 45 km resolution images of the
Moon with a spectral resolution of 185 eV, providing the first
high-resolution global map of rock forming element abundances.
Title: Geology of Noachian Martian Highlands Surrounding the Gusev
Crater
Authors: Zegers, T. E.; Conan, Y. G.; Foing, B.
Bibcode: 2004LPI....35.1767Z
Altcode:
To characterize the highland areas neighboring the Spirit landing
site we study the available visual and IR image data (THEMIS, MOC),
MOLA altimetry data and possibly new HRSC data from Mars Express.
Title: Preface To The Proceedings Of Hawaii International Lunar
Exploration Conference 2003
Authors: Foing, Bernard H.
Bibcode: 2004ilc..conf..531F
Altcode:
No abstract at ADS
Title: Europe En Route To The Moon: SMART-1 Final Preparation,
Launch And Early Flight (AAS 03-727)
Authors: Racca, G. D.; Foing, B. H.; Brinkmann, J.; de Bijl, J.;
di Napoli, L.; Estublier, D.; Evrard, E.; Grünagel, R.; Lumb, R.;
Marini, A.; Rumler, P.; Stagnaro, L.; van Dooren, J.
Bibcode: 2004ilc..conf..213R
Altcode:
No abstract at ADS
Title: High Temporal Resolution Spectra of Flare Stars
Authors: Montes, D.; Crespo-Chacón, I.; Fernández-Figueroa, M. J.;
López-Santiago, J.; García-Alvarez, D.; Foing, B. H.
Bibcode: 2004IAUS..219..910M
Altcode:
The results of a high temporal resolution spectroscopic
monitoring of the UV Cet type fare stars AD Leo and V1054 Oph are
reported. Intermediate resolution optical spectra of these stars were
taken using the IDS spectrograph of the 2.5 m Isaac Newton Telescope
(INT) of El Roque de los Muchachos Observatory (Spain) during 4 nights
(2-5 April 2001). We have obtained high temporal resolution by taking
series of spectra with short exposure times (15-300 sec) separated
only by the CCD readout time (~60 sec). The great number of spectra
observed each night has allowed us to analyse the temporal evolution of
the emission lines and to identify several fares of different intensity
and duration.
Title: Bringing the Moon and Space to the Public
Authors: Foing, B. H.; International Lunar Exploration Working Group
Bibcode: 2004cosp...35.4076F
Altcode: 2004cosp.meet.4076F
We give some examples of public outreach activities using the Moon
to engage the public in space exploration. We describe the public
relations and science communication campaign organized by ESA and
partners during the preparation of the SMART-1, and surrounding
the launch and commissioning. We also describe some P.R. activities
developed by the International Lunar Exploration Working Group (ILEWG)
and the Lunar Explorers Society (LUNEX), founded by the participants of
the 4th International Conference on the Exploration and Utilisation of
the Moon (ICEUM-4) in July 2000. We illustrate how people from diverse
backgrounds with a common interest in the exploration of the Moon and
beyond, are promoting research, exploration and outreach programmes,
by educating the public using web-based information and organising
activities or events. This provides a global structure of partnerships
that can be used to raise the awareness of the general public on
lunar, planetary and space related issues, and be used for future
actions. ILEWG: http://sci.esa.int/ilewg/ LUNEX: www.lunarexplorer.org
SMART-1: http://sci.esa.int/smart-1/
Title: Complex Organics in Interstellar Space
Authors: Foing, B.; Ehrenfreund, P.; Ruiterkamp, R.; Cox, N.
Bibcode: 2004cosp...35.4056F
Altcode: 2004cosp.meet.4056F
There are signatures of large organic molecules in the interstellar
medium, from the ultraviolet to the infrared. Some infrared emission
bands, which have been ascribed to families of large aromatic compounds
are not specific for individual identification (and for discriminating
free floating PAH molecules from loosely bound aromatics in amorphous
carbon compounds). Red fluorescence and FUV absorption have also
been ascribed to these aromatic compounds. Electronic transitions
in the visible are a key to identify free gas phase molecules. The
origin of Diffuse Interstellar Bands (Herbig 1995), more than 300 in
recent surveys (O' Tuairisg et al 2000) is still a mystery. However the
measurements of sub-structures rotational contours in DIBs (Ehrenfreund
Foing 1996) indicate large molecules such as chains (12-18C), rings,
50 C PAHs or fullerenes. The distribution of DIB widths permit to
estimate a distribution of size of molecular carriers. The environment
properties of DIB carriers also indicate ionisation potentials similar
to those of cations of large carbonaceous molecules, such as large PAHs
or fullerenes (Sonnentrucker et al 1997). The correlation studies of
DIBS also indicate different carriers for the strong DIBs observed
in the visible (Cami et al 1997). DIBS are weakened in the in the
low-metallicity Magellanic clouds (Ehrenfreund et al 2002, Cox et al
2004). The detection of near IR bands at 9577 and 9632 A coinciding
with laboratory transitions of C60+ (Foing, Ehrenfreund 1994, 1997,
Galatzudinov et al 2000 ) suggest that significant interstellar carbon
could reside in complex fullerene type compounds. These results indicate
that many different large and complex organic molecules can form
and survive in the very harsh interstellar environments. A follow up
interdisciplinary work is required between astronomical observations,
laboratory matrix and gas phase spectroscopy, theoretical work and
modelling, and active experiments in space to study the formation,
evolution, survival and transport of these complex organics.
Title: Scenario of Growing Crops on Silicates in Lunar Gargens
Authors: Kozyrovska, N.; Kovalchuk, M.; Negutska, V.; Lar, O.;
Korniichuk, O.; Alpatov, A.; Rogutskiy, I.; Kordyum, V.; Foing, B.
Bibcode: 2004cosp...35..745K
Altcode: 2004cosp.meet..745K
Self-perpetuating gardens will be a practical necessity for humans,
living in permanently manned lunar bases. A lunar garden has to
supplement less appetizing packaged food brought from the Earth,
and the ornamental plants have to serve as valuable means for
emotional relaxation of crews in a hostile lunar environment. The
plants are less prone to the inevitable pests and diseases when they
are in optimum condition, however, in lunar greenhouses there is
a threat for plants to be hosts for pests and predators. Although
the lunar rocks are microorganism free, there will be a problem
with the acquired infection (pathogens brought from the Earth) in
the substrate used for the plant growing. On the Moon pests can be
removed by total fumigation, including seed fumigation. However, such
a treatment is not required when probiotics (biocontrol bacteria) for
seed inoculation are used. A consortium of bacteria, controlling plant
diseases, provides the production of an acceptable harvest under growth
limiting factors and a threatening infection. To model lunar conditions
we have used terrestrial alumino-silicate mineral anorthosite (Malyn,
Ukraine) which served us as a lunar mineral analog for a substrate
composition. With the idea to provide a plant with some essential growth
elements siliceous bacterium Paenibacillus sp. has been isolated from
alumino-silicate mineral, and a mineral leaching has been simulated
in laboratory condition. The combination of mineral anorthosite and
siliceous bacteria, on one hand, and a consortium of beneficial bacteria
for biocontrol of plant diseases, on the other hand, are currently
used in model experiments to examine the wheat and potato growth and
production in cultivating chambers under controlled conditions.
Title: Space Science and Interdisciplinary Education
Authors: Foing, B. H.
Bibcode: 2004cosp...35.4078F
Altcode: 2004cosp.meet.4078F
The contribution of space science to an education cursus can be
conceived as a series of educational modules (each including text
books for teacher and pupil, exercises, CD-roms, observations or study
projects, kits for hands-on projects, and Internet products from space
agencies) covering different age groups (elementary 7-10, middle 10-14,
high school 15-17). These modules should not be limited to the science
teacher area, but must pervade in all topics of education the same way
as space is part of everyday life. Space agencies can contribute to
this by supporting a pilot group of teachers on sabbatical residence
to develop these modules. These teachers should cover different
European languages (e.g. English, French, German, other languages),
different educational systems experience, and different backgrounds
(Language/arts, science, history, technology). These modules could
be developed in one year, in partnership with education ministers,
publishers, for validation and production. They should be distributed
and inserted in curricula via education authorities and networks
of teachers. We list some examples of space (science) modules to be
developed, in different teachers courses for a total of about 20 hours
courses/yr, with basic modules for age group (7-10 yr) and Advanced
Modules for (10-15 yr).
Title: Gusev Crater and surrounding Highlands: preliminary HRSC
results
Authors: Foing, B. H.; Zegers, T.; Pischel, R.; Greeley, R.; Jaumann,
R.; Hoffmann, H.; Neukum, G.; HRSC Co-Investigators Team
Bibcode: 2004cosp...35.3345F
Altcode: 2004cosp.meet.3345F
We report on the preliminary analysis of data on Gusev crater and
surroundings, obtained with the Mars Express HRSC camera. The Gusev
crater lies in the northern part of the highlands that contain
the remanent magnetization.The highlands around Gusev crater are
characterized by a plateau of most likely basalt. The most conspicuous
features in the highland plateau are impact craters. Towards the
northwest of Gusev crater the plateau is transformed into a chaotic
terrain, with lower altitude. The basalt plateau rises about 2000 m
above the crater basin. It was suggested that Gusev impact depression
might have been filled with water, if available then. The brecciation
of target rocks could have resulted in a porous host rock with a large
subsurface water-rock interface that can provide sheltered conditions
for early life. To characterize the highland and the crater floor areas,
we study the new HRSC data obtained in January 2004 and compare them
to available visual and IR image data (THEMIS, MOC), TES spectroscopy
data and MOLA altimetry data. These data are also used to provide
geological context for the MER Lander Spirit that landed in the crater.
Title: The response of two amino acids to a subset of Mars' surface
conditions
Authors: Garry, J.; ten Kate, I.; Ruiterkamp, R.; Peeters, Z.; Foing,
B.; Ehrenfreund, P.
Bibcode: 2004cosp...35.4171G
Altcode: 2004cosp.meet.4171G
A multi-year project is underway to characterize and understand the
behaviour of organic molecules to the nominal average near-surface
environment of Mars. Such materials are expected to have been delivered
by meteoritic infall and studies of the longevity of organic matter
under present and past martian conditions may provide useful data to
test exobiological concepts. The use of this system as a payload test
chamber is also being pursued as an active side-issue. The project
centres around a simulation system that can accommodate objects up
to 0.2m3 in volume, and which can recreate the thermal
and UV conditions experienced by a range of martian locales. An
auxiliary chamber has been built to produce samples with a high
degree of repeatability and control. These samples have consisted of
sub-micron layers of solid glycine and beta-alanine vacuum deposited
onto silicon discs. Changes in the material content of each sample
are measured with the use of an IR transmission spectrometer with a
spectral resolution of 4cm-1, and 'forward contamination'
of these samples is lessened through the use of vacuum-tight transfer
vessels and sterile handling techniques.
Title: ESA's SMART-1 Mission: Status
Authors: Racca, G.; Foing, B. H.; SMART-1 Project Team
Bibcode: 2004cosp...35.4057R
Altcode: 2004cosp.meet.4057R
SMART-1 is the first of Small Missions for Advanced Research and
Technology as part of ESA science programme ``Cosmic Vision''. Its
objective is to demonstrate Solar Electric Primary Propulsion (SEP) for
future Cornerstones (such as Bepi-Colombo) and to test new technologies
for spacecraft and instruments. The spacecraft has been launched on 27
sept. 2003, as an Ariane-5 auxiliary passenger. SMART-1 orbit pericenter
is now outside the inner radiation belt. The current status of SMART-1
will be given at the symposium. After a 15 month cruise with primary
SEP, the SMART-1 mission is to orbit the Moon for a nominal period of
six months, with possible extension. The spacecraft will carry out a
complete programme of scientific observations during the cruise and
in lunar orbit.
Title: ESA's SMART-1 Mission Launched To The Moon: Technology And
Science Goals (AAS 03-700)
Authors: Foing, B. H.; Racca, G. D.; Marini, A.; Evrard, E.; Stagnaro,
L.; Almeida, M.; Koschny, D.; Frew, D.; Zender, J.; Heather, J.;
Grande, M.; Huovelin, J.; Keller, H. U.; Nathues, A.; Josset, J. L.;
Malkki, A.; Schmidt, W.; Noci, G.; Birkl, R.; Iess, L.; Sodnik, Z.;
McManamon, P.
Bibcode: 2004ilc..conf....3F
Altcode:
No abstract at ADS
Title: SMART-1 Payload First Results
Authors: Foing, B. H.; SMART-1 Science Technology Working Team
Bibcode: 2004cosp...35.4059F
Altcode: 2004cosp.meet.4059F
We present first results from SMART-1's science and technology payload,
with a total mass of some 19 kg, featuring many innovative instruments
and advanced technologies. A miniaturised high-resolution camera
(AMIE) for lunar surface imaging, a near-infrared point-spectrometer
(SIR) for lunar mineralogy investigation, and a very compact X-ray
spectrometer (D-CIXS) with a new type of detector and micro-collimator
which will provide fluorescence spectroscopy and imagery of the Moon's
surface elemental composition. The payload also includes an experiment
(KaTE) aimed at demonstrating deep-space telemetry and telecommand
communications in the X and Ka-bands, a radio-science experiment
(RSIS), a deep space optical link (Laser-Link Experiment), using the ESA
Optical Ground station in Tenerife, and the validation of a system of
autonomous navigation (OBAN) based on image processing. SMART-1 lunar
science investigations include studies of the chemical composition of
the Moon, of geophysical processes (volcanism, tectonics, cratering,
erosion, deposition of ices and volatiles) for comparative planetology,
and high resolution studies in preparation for future steps of lunar
exploration. The mission could address several topics such as the
accretional processes that led to the formation of rocky planets,
and the origin and evolution of the Earth-Moon system. The SMART-1
observations will be coordinated with Japanese missions Lunar-A and
SELENE, to answer open questions about comparative planetology, the
origin of the Earth --Moon system, the early evolution of life, the
planetary environment and the existence of in-situ resources necessary
to support human presence (e.g. water, oxygen). With their science and
technology results, these missions can be considered as preparatory
missions for future robotic and human exploration of the solar system.
Title: Roadmap for Future Lunar Exploration
Authors: Foing, B. H.; International Lunar Exploration Working Group
Bibcode: 2004cosp...35.4061F
Altcode: 2004cosp.meet.4061F
We discuss strategies for future lunar exploration. This includes
open science questions about comparative planetology, the origin of
the Earth --Moon system, the early evolution of life, the planetary
environment and the existence of in-situ resources necessary to support
human presence. We discuss areas of instrumentation: Remote sensing
miniaturised instruments; Surface geophysical and geochemistry package;
Instrument deployment and robotic arm, nano-rover, sampling, drilling;
Sample finder and collector. We discuss technologies in robotic
exploration: Mecha-electronics-sensors; Tele control, telepresence,
virtual reality; Regional mobility rover; Autonomy and Navigation;
Artificially intelligent robots. We compare Moon-Mars system aspects
related to In-Situ Utilisation of resources; Establishment of permanent
robotic infrastructure, Environmental protection aspects; Life sciences
laboratories; Support to human exploration. Finally, we discuss
possible roadmaps and synergies for Moon-Mars exploration, starting
with the missions for the coming decade, and building effectively on
joint technology developments.
Title: Synergies and roadmap for Moon-Mars Exploration
Authors: Foing, B. H.; Pieters, C.; Ilewg
Bibcode: 2004cosp...35.3357F
Altcode: 2004cosp.meet.3357F
There are large synergies between Moon and Mars exploration. This
includes joint areas of instrumentation: Remote sensing miniaturised
instruments; Surface geophysical and geochemistry package; Instrument
deployment and robotic arm, nano-rover, sampling, drilling; Sample
finder and collector. There are also common technologies in robotic
exploration: Mecha-electronics-sensors; Tele control, telepresence,
virtual reality; Regional mobility rover; Autonomy and Navigation;
Artificially intelligent robots. We compare Moon-Mars system aspects
related to In-Situ Utilisation of resources; Establishment of
permanent robotic infrastructure, Environmental protection aspects;
Life sciences laboratories; Support to human exploration. Finally, we
discuss possible roadmaps for exploration, starting with the Moon-Mars
missions for the coming decade, and building effectively on joint
technology developments.
Title: Microbial community in a precursory scenario of growing
Tagetes patula in a lunar greenhouse
Authors: Kozyrovska, N. O.; Korniichuk, O. S.; Voznyuk, T. M.;
Kovalchuk, M. V.; Lytvynenko, T. L.; Rogutskyy, I. S.; Mytrokhyn,
O. V.; Estrella-Liopis, V. R.; Borodinova, T. I.; Mashkovska, S. P.;
Foing, B. H.; Kordyum, V. A.
Bibcode: 2004KosNT..10e.221K
Altcode:
A confined prototype plant-microbial system is elaborated for
demonstration of growing pioneer plants in a lunar greenhouse. A
precursory scenario of growing Tagetes patula L. in a substrate
anorthosite which is similar mineralogically and chemically to lunar
silicate rocks includes the use of a microbial community. Microorganisms
served for preventive substrate colonization to avoid infection by
deleterious microorganisms as well as for bioleaching and delivering of
nutritional elements from anorthosite to plants. A model consortium of
a siliceous bacterium, biocontrol agents, and arbuscular mycorrhizal
fungi provided an acceptable growth and blossoming of Tagetes patula
L. under growth limiting factors in terrestrial conditions.
Title: MUSICOS 1998: Observations of Rotational Modulation and Flares
on the RS CVn Binary HR1099
Authors: García-Alvarez, D.; Foing, B. H.; Montes, D.; Oliveira,
J.; Doyle, J. G.; MUSICOS 98 Collaboration
Bibcode: 2003csss...12..958G
Altcode: 2001astro.ph..9235G
We present simultaneous and continuous observations of Hα, Hβ,
ion{Na}{1} D1, D2, ion{He}{1} D3
and ion{Ca}{2} H & K lines of the chromospherically active
binary HR 1099. We have observed HR 1099 for more than 3 weeks almost
continuously and monitored two flares. An increase in Hα and ion{Ca}{2}
H & K, Hβ and ion{He}{1} D3 and a strong filling-in
of the ion{Na}{1} D1, D2 during the flares are
observed. We have found that the flares took place at the same phase
(0.85) of the binary orbit, and both of them seems to occur near
the limb.
Title: MUSICOS Observations of the Chromospherically Active Binary
Star EI Eridani
Authors: Washuettl, A.; Strassmeier, K. G.; Foing, B.; MUSICOS98 Team
Bibcode: 2003csss...12.1008W
Altcode:
We present first results on spectroscopic observations of the
rapidly-rotating active binary star EI Eridani obtained during the
MUSICOS multi-site campaign in 1998. Eight sites around the globe were
involved in order to achieve surface images within a few rotations as EI
Eridani's critical rotation period of 1.945 days makes it impossible
to obtain time-resolved images from a single site. The data were
split into groups in order to obtain consecutive, independent Doppler
images. The preliminary results confirm the existence of a stable
polar spot that changes in size and shape while low-latitute spots
are found to be short lived. For the first time, it is possible to
achieve consecutive, time-resolved Doppler images for EI Eridani. A
preliminary investigation of differential rotation contradicts the
results from Hatzes & Vogt (1992).
Title: The SMART-1 Mission: Photometric Studies of the Moon with
the AMIE Camera
Authors: Shkuratov, Yu. G.; Kreslavsky, M. A.; Stankevich, D. G.;
Kaydash, V. G.; Pinet, P.; Shevchenko, V. V.; Foing, B. H.; Josset,
J. -L.
Bibcode: 2003SoSyR..37..251S
Altcode:
We describe the future SMART-1 European Space Mission whose objective
is to study the lunar surface from a polar lunar orbit. In particular,
it is anticipated that selected regions of the Moon will be photographed
using the AMIE camera with a mean spatial resolution of about 100 m in
three spectral channels (0.75, 0.92, and 0.96 μm) over a wide range of
phase angles. Since these spectral channels and the AMIE resolution are
close to those of the UVVIS camera onboard the Clementine spacecraft,
the simultaneous processing of SMART-1 and Clementine data can be
planned, for example, to obtain phase-ratio images. These images
carry information on the structural features of the lunar surface. In
particular, UVVIS/Clementine data revealed a photometric anomaly at
the Apollo-15 landing site associated with the blowing of the lunar
regolith by the lander engine. Anomalies were found in the ejection
zones of several fresh craters.
Title: Preface
Authors: Duke, Michael B.; Foing, Bernard H.
Bibcode: 2003AdSpR..31.2291D
Altcode:
No abstract at ADS
Title: SMART-1 mission to the moon: Technology and science goals
Authors: Foing, B. H.; Racca, G. D.; Marini, A.; Heather, D. J.;
Koschny, D.; Grande, M.; Huovelin, J.; Keller, H. U.; Nathues, A.;
Josset, J. L.; Malkki, A.; Schmidt, W.; Noci, G.; Birkl, R.; Iess,
L.; Sodnik, Z.; McManamon, P.
Bibcode: 2003AdSpR..31.2323F
Altcode:
SMART-1 is a technology demonstration mission for deep space solar
electrical propulsion and Technologies for the Future. SMART-1 will
be Europe's first lunar mission and will contribute to developing an
international program of lunar exploration. The spacecraft has been
readied in April 2003 for a launch in summer 2003, as an auxiliary
passenger to GTO on Ariane 5, to reach the Moon after 15 month's
cruise. SMART-1 will carry six experiments, including three remote
sensing instruments that will be used during the mission's nominal
six months in lunar orbit. These instruments will contribute to key
planetary scientific questions, related to theories of lunar origin and
evolution, the global and local crustal composition, the search for cold
traps at the lunar poles and the mapping of potential lunar resources.
Title: www.lunarexplorer.org: Educating the general public
Authors: Volp, J.; Foing, B.
Bibcode: 2003AdSpR..31.2455V
Altcode:
The Lunar Explorers Society (LUNEX) was founded by the participants of
the 4th International Conference on the Exploration and Utilisation
of the Moon (ICUEM4), which was organised under the auspices of the
International Lunar Exploration Working Group (ILEWG), and aimed to
draw together people from diverse backgrounds with a common interest
in the exploration of the Moon. At the end of the conference, a
formal ICEUM4 Declaration was drawn up detailing the recommendations
of the participants for the future of lunar exploration. LUNEX is a
society open to all Lunar Explorers and will aim to promote research,
exploration and outreach programmes that work towards the realisation
of the goals outlined in the ICEUM4 Declaration by educating the public
using web-based information and activities. LUNEX provides a global
structure that can be used to raise the awareness of the general public
on lunar related issues. We are looking for partnerships with other
Moon Societies to join efforts. For more information on the Lunar
Explorers Society, its activities, how to become an active member,
or how your organisation can work together with LUNEX, please visit
our website on www.lunarexplorer.org.
Title: The D-CIXS X-ray mapping spectrometer on SMART-1
Authors: Grande, M.; Browning, R.; Waltham, N.; Parker, D.; Dunkin,
S. K.; Kent, B.; Kellett, B.; Perry, C. H.; Swinyard, B.; Perry, A.;
Feraday, J.; Howe, C.; McBride, G.; Phillips, K.; Huovelin, J.; Muhli,
P.; Hakala, P. J.; Vilhu, O.; Laukkanen, J.; Thomas, N.; Hughes, D.;
Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Clark,
P. E.; Murray, C. D.; Guest, J.; Casanova, I.; d'Uston, L. C.; Maurice,
S.; Foing, B.; Heather, D. J.; Fernandes, V.; Muinonen, K.; Russell,
S. S.; Christou, A.; Owen, C.; Charles, P.; Koskinen, H.; Kato, M.;
Sipila, K.; Nenonen, S.; Holmstrom, M.; Bhandari, N.; Elphic, R.;
Lawrence, D.
Bibcode: 2003P&SS...51..427G
Altcode:
The D-CIXS Compact X-ray Spectrometer will provide high quality
spectroscopic mapping of the Moon, the primary science target
of the ESA SMART-1 mission. D-CIXS consists of a high throughput
spectrometer, which will perform spatially localised X-ray fluorescence
spectroscopy. It will also carry a solar monitor, to provide the direct
calibration needed to produce a global map of absolute lunar elemental
abundances, the first time this has been done. Thus it will achieve
ground breaking science within a resource envelope far smaller than
previously thought possible for this type of instrument, by exploiting
two new technologies, swept charge devices and micro-structure
collimators. The new technology does not require cold running, with
its associated overheads to the spacecraft. At the same time it will
demonstrate a radically novel approach to building a type of instrument
essential for the BepiColombo mission and potential future planetary
science targets.
Title: Scientific rationale for the D-CIXS X-ray spectrometer on
board ESA's SMART-1 mission to the Moon
Authors: Dunkin, S. K.; Grande, M.; Casanova, I.; Fernandes, V.;
Heather, D. J.; Kellett, B.; Muinonen, K.; Russell, S. S.; Browning,
R.; Waltham, N.; Parker, D.; Kent, B.; Perry, C. H.; Swinyard, B.;
Perry, A.; Feraday, J.; Howe, C.; Phillips, K.; McBride, G.; Huovelin,
J.; Muhli, P.; Hakala, P. J.; Vilhu, O.; Thomas, N.; Hughes, D.;
Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.; Baker, D.; Clark,
P. E.; Murray, C. D.; Guest, J.; d'Uston, L. C.; Maurice, S.; Foing,
B.; Christou, A.; Owen, C.; Charles, P.; Laukkanen, J.; Koskinen,
H.; Kato, M.; Sipila, K.; Nenonen, S.; Holmstrom, M.; Bhandari, N.;
Elphic, R.; Lawrence, D.
Bibcode: 2003P&SS...51..435D
Altcode:
The D-CIXS X-ray spectrometer on ESA's SMART-1 mission will provide
the first global coverage of the lunar surface in X-rays, providing
absolute measurements of elemental abundances. The instrument will
be able to detect elemental Fe, Mg, Al and Si under normal solar
conditions and several other elements during solar flare events. These
data will allow for advances in several areas of lunar science,
including an improved estimate of the bulk composition of the Moon,
detailed observations of the lateral and vertical nature of the crust,
chemical observations of the maria, investigations into the lunar
regolith, and mapping of potential lunar resources. In combination with
information to be obtained by the other instruments on SMART-1 and the
data already provided by the Clementine and Lunar Prospector missions,
this information will allow for a more detailed look at some of the
fundamental questions that remain regarding the origin and evolution
of the Moon.
Title: Status of esa smart-1 mission to the moon
Authors: Foing, B. H.; Racca, G. R.; Marini, A.; SMART-1 Technology
Working Team
Bibcode: 2003EAEJA....14857F
Altcode:
SMART-1 is the first in the programme of ESA’s Small Missions for
Advanced Research and Technology . Its objective is to demonstrate
Solar Electric Primary Propulsion (SEP) for future Cornerstones
(such as Bepi-Colombo) and to test new technologies for spacecraft
and instruments. The spacecraft has been readied for launch in spring
2003 as an Ariane-5 auxiliary passenger. After a cruise with primary
SEP, the SMART-1 mission is to orbit the Moon for a nominal period of
six months, with possible extension. The spacecraft will carry out
a complete programme of scientific observations during the cruise
and in lunar orbit. SMART-1's science payload, with a total mass
of some 19 kg, features many innovative instruments and advanced
technologies. A miniaturised high-resolution camera (AMIE) for lunar
surface imaging, a near-infrared point-spectrometer (SIR) for lunar
mineralogy investigation, and a very compact X-ray spectrometer (D-CIXS)
with a new type of detector and micro-collimator which will provide
fluorescence spectroscopy and imagery of the Moon's surface elemental
composition. The payload also includes an experiment (KaTE) aimed at
demonstrating deep-space telemetry and telecommand communications in the
X and Ka-bands, a radio-science experiment (RSIS), a deep space optical
link (Laser-Link Experiment), using the ESA Optical Ground station
in Tenerife, and the validation of a system of autonomous navigation
SMART-1 lunar science investigations include studies of the chemical
(OBAN) based on image processing. SMART-1 lunar science investigations
include studies of the chemical composition and evolution of the Moon,
of geophysical processes (volcanism, tectonics, cratering, erosion,
deposition of ices and volatiles) for comparative planetology, and
high resolution studies in preparation for future steps of lunar
exploration. The mission could address several topics such as the
accretional processes that led to the formation of planets, and the
origin of the Earth-Moon system.
Title: Mars Simulation Chamber 2 - goals , instrumentation and methods
Authors: Ehrenfreund, P.; ten Kate, I. L.; Ruiterkamp, R.; Botta,
O.; Lehmann, B.; Boudin, N.; Foing, B. H.
Bibcode: 2003EAEJA.....4298E
Altcode:
We have installed at ESTEC and instrumented a Mars Simulation Chamber
(MSC), in order to answer a range of questions on the subject of the
apparent absence of organic compounds on Mars. We shall investigate:
A. The effects of the changes of the Martian atmosphere over the history
of Mars. B. The effect of UV irradiation on organic molecules embedded
in the soil. C. The effect of oxidation on organic molecules embedded
in the soil. D. The effect of thermal cycling on the surface. E. A
combination of the above mentioned parameters. Techniques to be used
include gas analysis, environmental sensors, HPLC, spectroscopy and
other analytical techniques. We shall also assess the sensitivity
of instruments for the detection of minerals and organic compounds
of exobiological relevance in Martian analogue soils (mixed under
controlled conditions with traces of these organics). The results
concerning the simulation of complex organics on Mars, as well as
lander instrument chamber simulations will be included in a database
to serve for the interpretation of Beagle 2 data and other future Mars
missions. The results of the experiments can also provide constraints
for the observations from orbit, such as spectroscopy of minerals,
measurements of the water cycle, frost and subsurface water, the CO2
cycle, and the landing site selection. In summary, the experiments have
as a main goal to simulate various processes on organics, such as the
effects of UV radiation, diffusion, and temperature, as a function of
their depth in the soil. The specific organics will be embedded in
either porous or compact Martian soil analogues or quartz beads. In
this presentation we will concentrate on the goals, the instrumentation
and the methods, used to operate the chamber.
Title: bringing the moon to people: lunar explorers society
Authors: Foing, B. H.; Volp, J.; Almeida, M.; Heather, D.; van Susante,
P.; Lunar Explorers Society
Bibcode: 2003EAEJA....14858F
Altcode:
The Lunar Explorers Society (LUNEX) was founded by the participants
of the 4th International Conference on the Exploration and
Utilisation of the Moon (ICEUM4), held in July 2000 at the European
Space Research and Technology Centre (ESTEC) in The Netherlands. ICEUM4
was organised under the auspices of the International Lunar Exploration
Working Group (ILEWG), and aimed to draw together people from diverse
backgrounds with a common interest in the exploration of the Moon. At
the end of the conference, a formal ICEUM4 Declaration was drawn up
detailing the recommendations of the participants for the future of
lunar exploration. LUNEX will be a society open to all Lunar Explorers
and will aim to promote research, exploration and outreach programmes
that will work towards the realisation of the goals outlined in the
ICEUM4 Declaration. Following ICEUM4, a core group of active LUNEX
members was identified to begin to shape the new-born society with
guidance from ILEWG. A series of task groups have been installed to
address the key LUNEX issues, with strong participation of young lunar
explorers, and work is progressing towards the first LUNEX activities,
both at the level of the task groups and to form national chapters. The
first LUNEX convention was held in Paris in March 2001. Further
information about the Lunar Explorers Society can be found on our
Website: http://www.lunarexplorer.org.
Title: Composition of the lunar surface as will be seen from SMART-1:
A simulation using Clementine data
Authors: Shkuratov, Yuriy G.; Stankevich, Dmitriy G.; Kaydash, Vadim
G.; Omelchenko, Vitaliy V.; Pieters, Carle M.; Pinet, Patrick C.;
Chevrel, Serge D.; Daydou, Yves H.; Foing, Bernard H.; Sodnik, Zoran;
Josset, Jean-Luc; Taylor, Lawrence A.; Shevchenko, Vladislav V.
Bibcode: 2003JGRE..108.5020S
Altcode:
We present a new technique for remote sensing determination of lunar
surface composition in the context of the SMART-1 mission. The
technique is based on spectral and composition data obtained by
Lunar Soil Characterization Consortium for a few particle-size
separates of lunar soils. We map the abundance of TiO2
and FeO, pyroxene content, maturity degree (Is/FeO), and
a characteristic size of particles. Comparison of the TiO2
and FeO abundance maps with proper distributions obtained by Lucey et
al. [2000a] shows high correlation. We found also an inverse correlation
between the Is/FeO distribution and Lucey et al.'s [2000b]
parameter OM. Application of this approach shows that fresh mare crater
regolith is characterized with a higher abundance of pyroxenes, coarse
particles, and low maturity degree. The pyroxene abundance map can be
used to identify pyroclastic regions. An excess of small particles
is predicted for highland areas. We note appreciable variations of
the characteristic size of particles in mare regions. Our preliminary
results for the Reiner-γ formation show that there is no composition
anomaly for the TiO2 and FeO abundance, in agreement with
previous analyses. Our maps also indicate that the formation contains
a surface material characterized with low maturity and high degree
of crystallinity, consistent with the occurrence of immature regolith
possibly contaminated with dust.
Title: Mars Simulation Chamber 1 - preparation for Mars Express and
future Mars missions
Authors: Ehrenfreund, P.; ten Kate, I. L.; Ruiterkamp, R.; Botta,
O.; Lehmann, B.; Boudin, N.; Foing, B. H.
Bibcode: 2003EAEJA.....4277E
Altcode:
We have installed at ESTEC and instrumented a Mars Simulation Chamber
(MSC), in order to answer a range of questions on the subject of the
apparent absence of organic compounds on Mars. We shall investigate:
A. The effects of the changes of the Martian atmosphere over the history
of Mars. B. The effect of UV irradiation on organic molecules embedded
in the soil. C. The effect of oxidation on organic molecules embedded
in the soil. D. The effect of thermal cycling on the surface. E. A
combination of the above mentioned parameters. Techniques to be used
include gas analysis, environmental sensors, HPLC, spectroscopy and
other analytical techniques. We shall also assess the sensitivity
of instruments for the detection of minerals and organic compounds
of exobiological relevance in Martian analogue soils (mixed under
controlled conditions with traces of these organics). The results
concerning the simulation of complex organics on Mars, as well as
lander instrument chamber simulations will be included in a database
to serve for the interpretation of Beagle 2 data and other future Mars
missions. The results of the experiments can also provide constraints
for the observations from orbit, such as spectroscopy of minerals,
measurements of the water cycle, frost and subsurface water, the CO2
cycle, and the landing site selection. In summary, the experiments
have as a main goal to simulate various processes on organics, such as
the effects of UV radiation, diffusion, and temperature, as a function
of their depth in the soil. The specific organics will be embedded in
either porous or compact Martian soil analogues or quartz beads. In this
presentation we will concentrate on the preparation for Mars Express.
Title: Organics in space: spectroscopic characterizations
Authors: Boudin, N.; Ruiterkamp, R.; Foing, B.
Bibcode: 2003EAEJA.....6771B
Altcode:
There are signatures of large organic molecules in the interstellar
medium, from the ultraviolet to the infrared. Some infrared emission
bands, which have been ascribed to families of large aromatic compounds
are not specific for individual identification (and for discriminating
free floating PAH molecules from loosely bound aromatics in amorphous
carbon compounds). Red fluorescence and FUV absorption have also
been ascribed to these aromatic compounds. Electronic transitions
in the visible are a key to identify free gas phase molecules. The
origin of Diffuse Interstellar Bands (Herbig 1995), more than 300 in
recent surveys (O' Tuairisg et al 2000) is still a mystery. However the
measurements of sub-structures rotational contours in DIBs (Ehrenfreund
Foing 1996) indicate large molecules such as chains (12-18C), rings,
50 C PAHs or fullerenes. The distribution of DIB widths permit to
estimate a distribution of size of molecular carriers. The correlation
studies of DIBS also indicate different carriers for the strong DIBs
observed in the visible (Cami et al 1997). Finally the detection of NIR
bands at 9577 and 9632 A coinciding with laboratory transitions of C60+
(Foing, Ehrenfreund 1994, 1997, Galatzudinov et al 2000) suggest that
significant interstellar carbon could reside in complex fullerene type
compounds. These results indicate that many different large and complex
organic molecules can form and survive in the very harsh interstellar
environments. Several spectroscopic studies of these aromatics molecules
are reported and their advantages and drawbacks discussed. A follow up
interdisciplinary work is required between astronomical observations,
laboratory matrix and gas phase spectroscopy, theoretical work and
modelling, and active experiments in space to study the formation,
evolution, survival and transport of these complex organics.
Title: Simulations of Martian Surface and Subsurface Processes
Authors: ten Kate, I. L.; Ruiterkamp, R.; Botta, O.; Lehmann, B.;
Gomez Hernandez, C.; Boudin, N.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 2003LPI....34.1313T
Altcode:
Laboratory investigations on organic chemical processes occurring in
the martian surface and subsurface using a Mars Simulation Chamber.
Title: A solar-powered visit to the Moon. The SMART-1 misson
Authors: Racca, Giuseppe; Foing, Bernard
Bibcode: 2003ESABu.113...14R
Altcode:
SMART stands for Small Missions for Advanced Research in
Technology. Europe's space scientists have fitted SMART-1 with very
modern and compact sensors to map lunar minerals in greater detail
than ever before, using infrared rays. With X-rays too, it will make
the first comprehensive inventory of key chemical elements in the
lunar surface.
Title: Observing stellar activity from space
Authors: Foing, B. H.; Neiner, C.
Bibcode: 2003EAS.....9..147F
Altcode:
In this paper we present a review of the past, current and future
space missions relevant for observing stellar activity from space. In
the past, missions were focused on UV and X-ray fluxes, variability
and spectroscopy. Currently coronal spectroscopy diagnostics are
developed. HST high resolution imaging in the visible and near IR give
access to circumstellar disks and outflows. The future space missions
will concentrate on space photometry (for asteroseismology, exoplanets
search and microvariability due to activity) and interferometry (for
measuring stellar sizes and environments).
Title: Magellanic Diffuse Interstellar Bands and Carbon Chemistry
Authors: Ehrenfreund, Pascale; Cami, Jan; Foing, Bernard H.; Kaper,
Lex; Cox, Nick; Jimenez-Vicente, Jorge; Salama, Farid; Sarre, Peter;
Snow, Ted; Maier, John Paul
Bibcode: 2003IAUJD..21E...2E
Altcode:
With the Ultraviolet Visual Echelle Spectrograph mounted at the Very
Large Telescope we have observed at unprecedented spectral resolution
the absorption spectrum toward reddened stars in the Magellanic Clouds
over the wavelength range of 3500-10500 Å. This range covers the
strong transitions associated with neutral and charged large carbon
molecules of varying sizes and structures. We report the first detection
of diffuse interstellar bands (DIBs) at 5780 and 5797 Å in the Small
Magellanic Cloud and the variation of the 6284 Å DIB toward several
targets in the Large Magellanic Cloud. The variation of DIBs in the
Magellanic Clouds compared with Galactic targets may be governed
by a combination of the different chemical processes prevailing in
low-metallicity regions and the local environmental conditions. The
analysis of high-resolution absorption spectra allows us to reveal
the global effects in the chemistry and recycling of cosmic dust in
the Magellanic clouds which are relevant for the chemical pathways
forming large organic molecules in external galaxies
Title: Carbon chemistry and diffuse interstellar bands in the
Magellanic Clouds
Authors: Cox, Nick; Ehrenfreund, Pascale; Cami, Jan; Kaper, Lex; Foing,
Bernard; Cordiner, Martin; Sarre, Peter; Snow, Ted; Salama, Farid
Bibcode: 2003asdu.confE..43C
Altcode:
To unravel the carbon chemistry prevailing in (diffuse) interstellar
clouds we seek to disentangle the different environmental effects
that influence the existence and strength of the diffuse interstellar
bands (DIBs). DIBs are weak unidentified interstellar absorption bands
observed towards reddened stars. Their carriers are presently believed
to be large carbonaceous molecules (e.g PAHs). The Large and Small
Magellanic Cloud (LMC and SMC) offer a unique opportunity to link DIB
behaviour to widely varying environmental conditions (e.g. metallicity,
UV radiation field and star formation activity). This in turn imposes
useful constraints on the nature of the DIB carrier, which hopefully
leads to its much desired identification. To this aim we have
observed the absorption spectra of reddened OB stars in the Magellanic
Clouds at unprecedented high resolution (R ≅100.000) and high S/N
(>∼100) with the Ultraviolet Visual Echelle Spectrograph (UVES)
mounted at the Very Large Telescope (VLT). These spectra provide
the first observational evidence for the presence of DIBs in the SMC
(Ehrenfreund et al. 2002, ApJ, 576, L117). Analysis of the spectra
of the LMC and SMC targets indicates that a delicate balance must
exist for DIBs to be present. Noteworthy in this respect is the 30
Doradus region in the LMC in which these special conditions seem to
prevail. Of all LMC stars observed, only the two situated in the 30
Dor region have detectable DIBs. This balance appears to be strongly
dependent on the UV radiation field, which is represented by the shape
of the extinction curve (i.e. the presence of the 2200Å bump and the
steepness of the far-UV rise).
Title: Simultaneous optical and X-ray observations of flares and
rotational modulation on the RS CVn binary HR 1099 (V711 Tau) from
the MUSICOS 1998 campaign
Authors: García-Alvarez, D.; Foing, B. H.; Montes, D.; Oliveira,
J.; Doyle, J. G.; Messina, S.; Lanza, A. F.; Rodonò, M.; Abbott, J.;
Ash, T. D. C.; Baldry, I. K.; Bedding, T. R.; Buckley, D. A. H.; Cami,
J.; Cao, H.; Catala, C.; Cheng, K. P.; Domiciano de Souza, A., Jr.;
Donati, J. -F.; Hubert, A. -M.; Janot-Pacheco, E.; Hao, J. X.; Kaper,
L.; Kaufer, A.; Leister, N. V.; Neff, J. E.; Neiner, C.; Orlando, S.;
O'Toole, S. J.; Schäfer, D.; Smartt, S. J.; Stahl, O.; Telting, J.;
Tubbesing, S.
Bibcode: 2003A&A...397..285G
Altcode: 2002astro.ph.10230G
We present simultaneous and continuous observations of the Hα, Hβ,
He I D3, Na I D1, D2 doublet and the
Ca II H & K lines for the RS CVn system HR 1099. The spectroscopic
observations were obtained during the MUSICOS 1998 campaign involving
several observatories and instruments, both echelle and long-slit
spectrographs. During this campaign, HR 1099 was observed almost
continuously for more than 8 orbits of 2.8 deg. Two large optical
flares were observed, both showing an increase in the emission of Hα,
Ca II H & K, Hβ and He I D3 and a strong filling-in
of the Na I D1, D2 doublet. Contemporary
photometric observations were carried out with the robotic telescopes
APT-80 of Catania and Phoenix-25 of Fairborn Observatories. Maps
of the distribution of the spotted regions on the photosphere of
the binary components were derived using the Maximum Entropy and
Tikhonov photometric regularization criteria. Rotational modulation
was observed in Hα and He I D3 in anti-correlation with
the photometric light curves. Both flares occurred at the same binary
phase (0.85), suggesting that these events took place in the same
active region. Simultaneous X-ray observations, performed by ASM on
board RXTE, show several flare-like events, some of which correlate
well with the observed optical flares. Rotational modulation in the
X-ray light curve has been detected with minimum flux when the less
active G5 V star was in front. A possible periodicity in the X-ray
flare-like events was also found. Based on observations obtained
during the MUSICOS 98 MUlti-SIte COntinuous Spectroscopic campaign from
Observatoire de Haute-Provence, France, Kitt Peak National Observatory,
USA, ESO La Silla, Chile, Mt. Stromlo Observatory, Australia, Xinglong
National Observatory, China, Isaac Newton Telescope, Spain, Laboratório
Nacional de Astrofísica, Brazil, and South African Astronomical
Observatory, South Africa. Contemporaneous observations from Catania,
Italy and Fairborn Observatories, USA, and on data obtained with the
Rossi X-ray Timing Explorer.
Title: A survey of the PAH electronic spectra and their search in
the Interstellar Medium
Authors: Boudin, N.; Ruiterkamp, R.; Foing, B. H.
Bibcode: 2003asdu.confE.162B
Altcode:
The understanding of physical and chemical processes in the interstellar
medium is currently an important challenge for our Universe knowledge
since these processes are involved in the control of stars and planets
formation. Polycyclic Aromatic Hydrocarbons (PAHs) are now recognized
as an important constituent of the interstellar medium gaseous phase,
mainly through observations of their IR emission bands. This family of
molecules and in particular their ionic and radical derivatives seems
to be one of the most promising candidates for the identification
of the Diffuse Interstellar Bands (DIBs). These absorption bands,
observed - throughout the visible and near infrared spectral range -
over spectra of stars masked by gas cloud, were first discovered in
1922. Their spectral properties indicate that DIBs could originate
from gaseous phase carbonaceous molecules. The identification of
PAHs as molecules responsible for these bands must be done through
direct comparison with PAHs spectra recorded in conditions as close
as possible to those of the interstellar medium. An exhaustive
survey of all the literature spectra of the PAHs in the neutral or
ionic (cation and anion) forms was achieved and will be reported here,
allowing us to find some trends among the PAH spectra: for instance,
concerning the band shift due to the interaction with the matrix;
concerning the distribution of transitions of a large amount of PAH
cations, through their PhotoElectron Spectra (N. Boudin, R. Ruiterkamp
and B. H. Foing, A&A, 2003). The advantages and drawbacks of
all the experimental techniques (PhotoElectron Spectroscopy, Matrix
Isolation Spectroscopy, gas phase techniques) will be discussed. Concurrently, this large database allow us to search these laboratory
transitions in the astronomical spectra already published. A follow
up interdisciplinary work is required between astronomical observations,
laboratory matrix and gas phase spectroscopy, theoretical work and
modelling, and active experiments in space to study the formation,
evolution, survival and transport of these complex organics.
Title: ESA SMART-1 Mission to the Moon
Authors: Foing, Bernard H.; Racca, Giuseppe D.; Marini, Andrea; Grande,
Manuel; Huovelin, Juhani; Josset, Jean-Luc; Keller, Horst Uwe; Nathues,
Andreas; Koschny, Detlef; Malkki, Ansi
Bibcode: 2003IAUSS...1E..35F
Altcode:
SMART-1 is the first of ESA’s Small Missions for Advanced Research
and Technology. Its objective is to demonstrate Primary Solar Electric
Propulsion for future Cornerstones (such as Bepi-Colombo) and to test
new technologies for spacecraft and instruments. The 370 kg spacecraft
is to be launched in summer 2003 as Ariane-5 auxiliary passenger and
after a 15 month cruise is to orbit the Moon for 6 months with possible
extension. SMART-1 will carry out observations during the cruise and
in lunar orbit with a science and technology payload (19 kg total
mass): a miniaturised high-resolution camera (AMIE) a near-infrared
point-spectrometer (SIR) for lunar mineralogy a very compact X-ray
spectrometer (D-CIXS) mapping surface elemental composition a Deep Space
Communication experiment (KaTE) a radio-science investigations (RSIS)
a Laser-Link Experiment an On Board Autonomous Navigation experiment
(OBAN) and plasma sensors (SPEDE). SMART-1 will study accretional
and bombardment processes that led to the formation of rocky planets
and the origin and evolution of the Earth-Moon system. Its science
investigations include studies of the chemical composition of the
Moon of geophysical processes (volcanism tectonics cratering erosion
deposition of ices and volatiles) for comparative planetology and the
preparation for future lunar and planetary exploration.
Title: The SMART-1 X-ray solar monitor (XSM): calibrations for D-CIXS
and independent coronal science
Authors: Huovelin, J.; Alha, L.; Andersson, H.; Andersson, T.;
Browning, R.; Drummond, D.; Foing, B.; Grande, M.; Hämäläinen,
K.; Laukkanen, J.; Lämsä, V.; Muinonen, K.; Murray, M.; Nenonen,
S.; Salminen, A.; Sipilä, H.; Taylor, I.; Vilhu, O.; Waltham, N.;
Lopez-Jorkama, M.
Bibcode: 2002P&SS...50.1345H
Altcode:
The X-ray solar monitor (XSM) is a calibration instrument of the
demonstration of compact imaging X-ray spectrometer (D-CIXS) experiment,
with a separate Silicon detector unit on the SMART-1 spacecraft. The
non-imaging HPSi PIN sensor has a wide field-of-view (FOV) to enable
Sun visibility during a significant fraction of the mission lifetime,
which is essential for obtaining calibration spectra for the X-ray
fluorescence measurements by the imaging D-CIXS spectrometer. The
energy range (1- 20 keV), spectral resolution (about 250 eV at 6 keV),
and sensitivity (about 7000 cps at flux level of 10 -4
W m -2 in the range 1- 8 Å) are tuned to provide optimal
knowledge about the Solar X-ray flux on the Lunar surface, matching
well with the activating energy range for the fluorescence measured
by D-CIXS. The independent science of the XSM will also be valuable,
since the XSM energy range is very sensitive to solar flares. The
countrate during the top of an X1 flare will be about 35 times higher
than the average quiescent countrate at solar maximum. The relative
increase will be the same for an M1 flare during the SMART-1 mission,
which will be closer to the next solar minimum. Since the XSM will
observe the Sun as a star, and the energy range and spectral resolution
are close to those of present astronomical X-ray satellites (e.g.,
XMM-Newton, ASCA, Chandra), we will obtain an X-ray database of the
Sun which can be related with the stellar X-ray observations more
easily than the data from present solar X-ray instruments. In this
publication we give a detailed description of the design, performance,
and tasks of the XSM instrument, and view the science perspectives.
Title: Lunar exploration
Authors: Foing, Bernard H.
Bibcode: 2002P&SS...50.....F
Altcode:
No abstract at ADS
Title: SMART-1 mission description and development status
Authors: Racca, G. D.; Marini, A.; Stagnaro, L.; van Dooren, J.;
di Napoli, L.; Foing, B. H.; Lumb, R.; Volp, J.; Brinkmann, J.;
Grünagel, R.; Estublier, D.; Tremolizzo, E.; McKay, M.; Camino, O.;
Schoemaekers, J.; Hechler, M.; Khan, M.; Rathsman, P.; Andersson, G.;
Anflo, K.; Berge, S.; Bodin, P.; Edfors, A.; Hussain, A.; Kugelberg,
J.; Larsson, N.; Ljung, B.; Meijer, L.; Mörtsell, A.; Nordebäck,
T.; Persson, S.; Sjöberg, F.
Bibcode: 2002P&SS...50.1323R
Altcode:
SMART-1 is the first of the Small Missions for Advanced Research
in Technology of the ESA Horizons 2000 scientific programme. The
SMART-1 mission is dedicated to testing of new technologies for future
cornerstone missions, using Solar-Electric Primary Propulsion (SEPP) in
Deep Space. The chosen mission planetary target is the Moon. The target
orbit will be polar with the pericentre close to the South-Pole. The
pericentre altitude lies between 300 and 2000 km, while the apocentre
will extend to about 10,000 km. During the cruise phase, before
reaching the Moon, the spacecraft thrusting profile allows extended
periods for cruise science. The SMART-1 spacecraft will be launched in
the spring of 2003 as an auxiliary passenger on an Ariane 5 and placed
into a Geostationary Transfer Orbit (GTO). The expected launch mass is
about 370 kg, including 19 kg of payload. The selected type of SEPP is
a Hall-effect thruster called PPS-1350. The thruster is used to spiral
out of the GTO and for all orbit maneuvers including lunar capture and
descent. The trajectory has been optimised by inserting coast arcs and
the presence of the Moon's gravitational field is exploited in multiple
weak gravity assists. The Development Phase started in October 1999 and
is expected to be concluded by a Flight Acceptance Review in January
2003. The short development time for this high technology spacecraft
requires a concerted effort by industry, science institutes and ESA
centres. This paper describes the mission and the project development
status both from a technical and programmatic standpoint.
Title: MUSICOS 1998: Optical and X-rays Observations of Flares on
the RS CVn Binary HR 1099
Authors: García-Alvarez, D.; Doyle, J. G.; Foing, B. H.; Oliveira,
J. M.; Montes, D.
Bibcode: 2002ASPC..277..479G
Altcode: 2001astro.ph.10305G; 2002sccx.conf..479G
We present simultaneous and continuous observations of H_alpha, H_beta,
NaI D_1, D_2 and HeI D_3 lines of the chromospherically active binary HR
1099. We have observed HR 1099 for more than 3 weeks almost continuously
and monitored two flares. An increase in H_alpha, CaII H & K,
H_beta, HeI D_3 and HeI lambda6678 and a strong filling-in of the NaI
D_1, D_2 and MgI b triplet during one of the flares are observed. We
have found that the flares took place at the same phase (0.85) of the
binary orbit, and both of them seems to occur near the limb. Several
X-rays flares were also detected by ASM on board RXTE. Rotational
modulation in the X-rays light curve has been detected with maximum
flux when the active K1IV star is in front.
Title: Laboratory studies on complex organic molecules on Mars. Part
2 - experimental set-up and related work
Authors: ten Kate, I. L.; Ruiterkamp, R.; Botta, O.; Lehmann, B.;
Gomez Hernandez, C.; Boudin, N.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 2002ESASP.518...81T
Altcode: 2002eab..conf...81T
In 1976 the Viking missions arrived at Mars to search for traces of
extinct and extant life. Although this mission brought a range of
sophisticated instruments it neiter detected any traces of life, nor
any organic compounds in the Martian soil. Since it is still unclear
why the Viking landers did not detect any organic molecules, laboratory
experiments under simulated Martian conditions are crucial in support
of future life-seeking Mars missions. This paper describes ongoing
experiments investigating the stability of organic molecules in the
Martian soil. We present a short rationale, the experimental set-up
and approach and a description of the organic compounds that will be
used during the experiments. The research programme described in this
article is developed at the European Space Research and Technology
Centre of ESA, ESTEC and at Leiden University, in the frame of a Mars
Express Recognised Cooperating Laboratory RCL.
Title: Complex carbon chemistry and the diffuse interstellar bands
in the Magellanic Clouds
Authors: Cox, N.; Ehrenfreund, P.; Cami, J.; Jimenez-Vicente, J.;
Foing, B. H.; Kaper, L.; van der Meer, A.; D'Hendecourt, L.; Maier,
J.; Salama, F.; Sarre, P.; Snow, T.; Sonnetrucker, P.
Bibcode: 2002ESASP.518..447C
Altcode: 2002eab..conf..447C
No abstract at ADS
Title: Laboratory Calibration Studies in Support of ORGANICS on the
International Space Station: Evolution of Organic Matter in Space
Authors: Ruiterkamp, R.; Ehrenfreund, P.; Halasinski, T.; Salama,
F.; Foing, B.; Schmidt, W.
Bibcode: 2002nla..work..149R
Altcode:
This paper describes the scientific overview and current status of
ORGANICS an exposure experiment per- formed on the International
Space Station (ISS) to study the evolution of organic matter in
space (P1: P. Ehrenfreund), with supporting laboratory experiments
performed at NASA Ames. ORGANICS investigates the chemical evolution
of samples submitted to long-duration exposure to space environment
in near-Earth orbit. This experiment will provide information on the
nature, evolution, and survival of carbon species in the interstellar
medium (ISM) and in solar system targets.
Title: Laboratory studies on complex organic molecules on Mars. Part
1 - rationale
Authors: ten Kate, I. L.; Ruiterkamp, R.; Botta, O.; Lehmann, B.;
Gomez Hernandez, C.; Boudin, N.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 2002ESASP.514..293T
Altcode: 2002elpm.conf..293T
The search for organic molecules and traces of life is the future
perspective of several missions to Mars. In order to know what those
mission should be looking for, laboratory experiments under simulated
Mars conditions are necessary. Especially since the Viking mission
did not find any traces of organic compounds in the Martian soil. In
this paper the history of the search for life on Mars and the context
of our laboratory studies, are described. Furthermore it gives a short
description of the experiments. This paper is the first part of a series
of three papers. The second paper will describe the experiments and
methods, the third paper will be a status report. Both the second and
the third paper can be found in the proceedings of the Second European
Workshop on Exo/Astrobiology, ESA Special Publication SP-518.
Title: SMART-1 science experiments co-ordination
Authors: Almeida, M.; Foing, B.; Vilar, E.; Heather, D.; Koschny,
D.; Marini, A.
Bibcode: 2002ESASP.514...55A
Altcode: 2002elpm.conf...55A
SMART-1 is the first European Space Agency mission to the Moon, due
for launch in the first months of 2003. Its primary goal is to test
new technologies for space navigation and science. In its science
experiments, SMART-1 will include new, very compact experiments. This
paper aims to demonstrate some of the science experiment operations
foreseen for the mission. We describe the SMART-1 mission, its orbit
and example scenarios for imaging specific targets (such as Tycho and
Copernicus craters).
Title: Technology and science from Earth to Moon: SMART-1 experiments
and their operations
Authors: Marini, A. E.; Lumb, R.; Racca, G. D.; Foing, B. H.;
Dias-Almeida, M.
Bibcode: 2002ESASP.514...95M
Altcode: 2002elpm.conf...95M
SMART-1, the first European mission to the Moon aimed at demonstrating
the Solar Electric propulsion hosts 10 Technology and Science
experiments. The monitoring of the spacecraft plasma environment
and the thruster contamination produced by thruster is carried out
by SPEDE (Spacecraft Potential, Electron and Dust Experiment) and
EPDP (Electric Propulsion Diagnostic Package). The miniaturised
remote sensing instruments on-board SMART-1 are: AMIE (Advanced
Moon micro-Imager Experiment), D-CIXS (Demonstration of a Compact
Imaging X-ray Spectrometer), supported in its operation by XSM (X-ray
Solar Monitor), and SIR (SMART-1 Infrared Spectrometer). Technology
experiments for deep-space communications and navigation are:
KATE (Ka-Band TT&C Experiment), based on X/Kaband transponder
which also supports RSIS (Radio-Science Investigations for SMART-1),
Laser-link, demonstrating a deep-space laser communication link and OBAN
(On-Board Autonomous Navigation experiment). The Experiments will be
performed during two distinct phases of the SMART-1 mission, including
17-month Earth escape phase and a nominal 6-month operational phase
in elliptical Moon orbit. The SMART-1 STOC (Science and Technology
Operations Co-ordination) carries out the planning and co-ordination
of the Technology and science experiments.
Title: Preface (Earth-like planets and moons)
Authors: Foing, Bernard H.
Bibcode: 2002ESASP.514D...7F
Altcode: 2002elpm.confD...7F
These proceedings contain a selection of papers from 20 invited
review talks and 30 contributed oral or poster presentations given
at the ESLAB36 symposium on "Earth-like planets and moons", at ESTEC
Noordwijk on 3-8 June 2002. This covers bodies such as Earth, Mercury,
Venus, Mars, Moon, Vesta, Io, Europa, Ganymede, Callisto, Titan, Triton,
Pluto/Charon and terrestrial exoplanets. The goal is to understand their
observed similarities and differences, and give both an Earth-oriented
and a cosmic perspective. We reviewed the contribution of recent and
upcoming space missions to these studies. The programme was based
on comprehensive invited reviews, supported with interdisciplinary
contributed papers, and a large body of posters on specific results,
methods or planetary objects.
Title: Closing remarks on ESLAB36 symposium on "Earth-like planets
and moons"
Authors: Foing, Bernard H.; Organisers Of Eslab36
Bibcode: 2002ESASP.514..345F
Altcode: 2002elpm.conf..345F
We give a summary of ESLAB36 symposium on "Earth-like planets and moons"
that took place at ESTEC, Noordwijk on 3-7 June 2002. The different
sessions included: - A family portrait of Earth-like planets and moons -
The contribution of space missions for understanding Earth-like planets
and moons - Earth as a planet - Methods for comparative planetology
- Interiors, surfaces, exospheres and impact processes - Comparing
atmospheres and fluids - Earth-like planets and moons in the galaxy -
Habitable Earth-like planets and moons - ESLAB Symposium summary and
roundtable discussion - Robotic and Human exploration - Young Planetary
Explorers (YPE) special session.
Title: Lunar missions: science and exploration
Authors: Foing, Bernard H.; International Lunar Exploration Working
Group
Bibcode: 2002ESASP.514....3F
Altcode: 2002elpm.conf....3F
Results from the recent US missions "Clementine" and Lunar Prospector,
will, in the near future, be used to prepare the ESA SMART-1 and
Japanese Lunar-A and SELENE missions to the Moon. The scientific
results of these missions will continue to answer open questions about
the origin of the Earth-Moon system, the early evolution of life, the
planetary environment and the existence of in-situ resources necessary
to support human presence (e.g. water, oxygen). These science and
technology missions can be considered as precursor missions for future
human exploration of the solar system.
Title: Earth-like Planets and Moons
Authors: Foing, Bernard H.; Battrick, Bruce
Bibcode: 2002ESASP.514.....F
Altcode: 2002elpm.conf.....F
Contents: The contribution of space missions for understanding
earth-like planets and moons. Earth as a planet & space
experiments. Methods for comparative planetology. Interiors, surfaces,
exospheres and impact processes. Impact interactions with planets and
moons. Comparing atmospheres and fluids (with emphasis on Earth, Mars,
Venus, Titan, Europa). Earth-like planets and moons in the Galaxy. Young
planetary explorers (YPE).
Title: Investigating complex organic compounds in a simulated Mars
environment
Authors: ten Kate, I. L.; Ruiterkamp, R.; Botta, O.; Lehmann, B.;
Gomez Hernandez, C.; Boudin, N.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 2002IJAsB...1..387T
Altcode:
Available from http://dx.doi.org/10.1017/S1473550403001277
Title: Detection of Diffuse Interstellar Bands in the Magellanic
Clouds
Authors: Ehrenfreund, P.; Cami, J.; Jiménez-Vicente, J.; Foing, B. H.;
Kaper, L.; van der Meer, A.; Cox, N.; D'Hendecourt, L.; Maier, J. P.;
Salama, F.; Sarre, P. J.; Snow, T. P.; Sonnentrucker, P.
Bibcode: 2002ApJ...576L.117E
Altcode:
With the Ultraviolet Visual Echelle Spectrograph mounted at the Very
Large Telescope, we have observed at unprecedented spectral resolution
the absorption spectrum toward reddened stars in the Magellanic Clouds
over the wavelength range of 3500-10500 Å. This range covers the
strong transitions associated with neutral and charged large carbon
molecules of varying sizes and structures. We report the first detection
of diffuse interstellar bands (DIBs) at 5780 and 5797 Å in the Small
Magellanic Cloud and the variation of the 6284 Å DIB toward several
targets in the Large Magellanic Cloud. The variation of DIBs in the
Magellanic Clouds compared with Galactic targets may be governed
by a combination of the different chemical processes prevailing in
low-metallicity regions and the local environmental conditions. Based
on observations made at the European Southern Observatory, Paranal,
Chile (ESO program 67.C-0281).
Title: Spectroscopy of large PAHs. Laboratory studies and comparison
to the Diffuse Interstellar Bands
Authors: Ruiterkamp, R.; Halasinski, T.; Salama, F.; Foing, B. H.;
Allamandola, L. J.; Schmidt, W.; Ehrenfreund, P.
Bibcode: 2002A&A...390.1153R
Altcode:
Polycyclic Aromatic Hydrocarbons (PAHs) are thought to be the carriers
of the ubiquitous infrared emission bands (UIBs). Data from the
Infrared Space Observatory (ISO) have provided new insights into the
size distribution and the structure of interstellar PAH molecules
pointing to a trend towards larger-size PAHs. The mid-infrared
spectra of galactic and extragalactic sources have also indicated
the presence of 5-ring structures and PAH structures with attached
side groups. This paper reports for the first time the laboratory
measurement of the UV-Vis-NIR absorption spectra of a representative
set of large PAHs that have also been selected for a long duration
exposure experiment on the International Space Station ISS. PAHs with
sizes up to 600 amu, including 5-ring species and PAHs containing
heteroatoms, have been synthesized and their spectra measured using
matrix isolation spectroscopy. The spectra of the neutral species
and the associated cations and anions measured in this work are also
compared to astronomical spectra of Diffuse Interstellar Bands (DIBs).
Title: Non-radial pulsation, rotation and outburst in the Be star
omega Orionis from the MuSiCoS 1998 campaign
Authors: Neiner, C.; Hubert, A. -M.; Floquet, M.; Jankov, S.; Henrichs,
H. F.; Foing, B.; Oliveira, J.; Orlando, S.; Abbott, J.; Baldry,
I. K.; Bedding, T. R.; Cami, J.; Cao, H.; Catala, C.; Cheng, K. P.;
Domiciano de Souza, A., Jr.; Janot-Pacheco, E.; Hao, J. X.; Kaper,
L.; Kaufer, A.; Leister, N. V.; Neff, J. E.; O'Toole, S. J.; Schäfer,
D.; Smartt, S. J.; Stahl, O.; Telting, J.; Tubbesing, S.; Zorec, J.
Bibcode: 2002A&A...388..899N
Altcode:
omega Ori (HD 37490, HR
1934) is a Be star known to have presented variations. In
order to investigate the nature and origin of its short-term and
mid-term variability, a study is performed of several spectral lines
(Hα , Hdelta , ion {He}i 4471, 4713, 4921, 5876, 6678, ion {C}{ii}
4267, 6578, 6583, ion {Mg}{ii} 4481, ion {Si}{iii} 4553 and ion
{Si}{ii} 6347), based on 249 high signal-to-noise high-resolution
spectra taken with 8 telescopes over 22 consecutive nights during
the MuSiCoS (Multi SIte COntinuous Spectroscopy) campaign in
November-December 1998. The stellar parameters are revisited and
the projected rotational velocity (vsin i = 179 km s-1)
is redetermined using several methods. With the MuSiCoS 98 dataset,
a time series analysis of line-profile variations (LPVs) is performed
using the Restricted Local Cleanest (RLC) algorithm and a least squares
method. The behaviour of the velocity of the centroid of the lines,
the equivalent widths and the apparent vsini for several lines, as well
as Violet and Red components of photospheric lines affected by emission
(red ion {He}i lines, ion {Si}{ii} 6347, ion {C}{ii} 6578, 6583) are
analyzed. The non-radial pulsation (NRP) model is examined using phase
diagrams and the Fourier-Doppler Imaging (FDI) method. The LPVs are
consistent with a NRP mode with l = 2 or 3, |m| = 2 with frequency
1.03 c d-1. It is shown that an emission line outburst
occurred in the middle of the campaign. Two scenarios are proposed to
explain the behaviour of a dense cloud, temporarily orbiting around
the star with a frequency 0.46 c d-1, in relation to the
outburst. Based on observations taken during the MuSiCoS 98 campaign
at OHP (France), La Silla (ESO, Chile, ID 62.H-0270), Mount Stromlo
(Australia), Xinglong Station (China), Kitt Peak (USA), MCT/LNA (Brazil)
and INT (Isaac Newton Group, La Palma Island).
Title: Automated detection of CMEs in LASCO data
Authors: Berghmans, D.; Foing, B. H.; Fleck, B.
Bibcode: 2002ESASP.508..437B
Altcode: 2002soho...11..437B
We have developed software that autonomously detects CMEs in image
sequences from LASCO. the crux of the software is the detection of CMEs
as bright ridges in (height, time) maps using the Hough transform. The
output is a list of events, similar to the classic catalogs, with
principle angle, angular width and velocity estimation for each
CME. In contrast to catalogs assembled by human operators, these CME
detections by software can be faster, which is especially important in
the context of space weather, and possibly also more objective, as the
detection criterion is written explicitly in a program. In this paper
we describe the software and validate its performance by comparing its
output with the visually assembled CME catalogs. We discuss its present
success rate (about 75%) and prospects for improvement. Finally, we
show that the software can also reveal CMEs that have not been listed
in the catalogs. Such unreported cases might be of influence on CME
statistics and prove that also the present catalogs do not have a 100%
success rate.
Title: Preface
Authors: Foing, Bernard H.; Heather, David
Bibcode: 2002AdSpR..30.1867F
Altcode:
No abstract at ADS
Title: The D-CIXS X-ray spectrometer, and its capabilities for
lunar science
Authors: Grande, M.; Dunkin, S.; Heather, D.; Kellett, B.; Perry,
C. H.; Browning, R.; Waltham, N.; Parker, D.; Kent, B.; Swinyard,
B.; Fereday, J.; Howe, C.; Huovelin, J.; Muhli, P.; Hakala, P. J.;
Vilhu, O.; Thomas, N.; Hughes, D.; Alleyne, H.; Grady, M.; Russell,
S.; Lundin, R.; Barabash, S.; Baker, D.; Clark, P. E.; Murray, C. D.;
Christou, A.; Guest, J.; Casanova, I.; d'Uston, L. C.; Maurice, S.;
Foing, B.; Kato, M.
Bibcode: 2002AdSpR..30.1901G
Altcode:
The purpose of the D-CIXS (Demonstration of a Compact Imaging X-ray
Spectrometer) instrument on the ESA SMART-1 mission is to provide high
quality spectroscopic mapping of the Moon by imaging fluorescence
X-rays emitted from the lunar surface. In order to obtain adequate
statistics for what can be very weak sources, it is essential to have
a large effective area, while maintaining a low mass. The solution is
to make a thin, low profile detector, essentially a modern version of
"X-ray detecting paper". D-CIXS will achieve a spatial resolution on
the ground of 42km from a spacecraft at 300 km altitude, with a spectral
resolution of 200 eV or better. The instrument is based around the use
of advanced dual microstructure collimator and Swept Charge Device
X-ray detector technologies. Swept Charge Device X-ray detectors,
a novel architecture based on proven CCD technology, have the virtue
of providing superior X-ray detection and spectroscopic measurement
capabilities, while also operating at room temperature. Thus we avoid
the need for the large passive cooling radiator that was previously
required to cool large X-ray focal plane CCDs. The advanced low profile
microstructure collimation and filter design builds on expertise
developed in solid state and microwave technology to enable us to
dramatically reduce the instrument mass. The total mass of D-CIXS,
including an X-ray solar monitor is ∼4.6 kg. D-CIXS will provide the
first global map of the Moon in X-rays. During normal solar conditions,
it will be able to detect absolute elemental abundances of Fe, Mg, Al
and Si on the lunar surface, using the on-board solar monitor to obtain
a continuous measurement of the input solar spectrum. During solar flare
events, it will also be possible to detect other elements such as Ca,
Ti, V, Cr, Mn, Co, K, P and Na. The global mapping of Mg, Al and Si,
and in particular deriving Mg#, the magnesium number (MgO/[MgO+FeO]),
represents the prime goal of the D-CIXS experiment.
Title: Exoplanets and Formation of Planetary Systems: Studies With
Esa Science Missions
Authors: Foing, B. H.
Bibcode: 2002EGSGA..27.5074F
Altcode:
Several space missions from the ESA Science Horizons 2000 Programme
address key questions on the formation/evolution of planetary
systems and on the study of ex- oplanets: - How do solar systems form
? (with HST, ISO, NGST, FIRST/Herschel, Rosetta, Gaia) - Geological
evolution of terrestrial planets (with Living planet, Mars- express,
SMART-1, Venus-express, Bepi-Colombo) - History and Role of impacts
(with SMART-1, Bepi-Colombo, outer planets missions) - How to detect
other solar systems and habitable zones (with space photometry, COROT,
Eddington, Gaia, Dar- win) - Water and ices on other planets and comets
(with instruments on Mars Express, Rosetta and other planetary missions)
- Signature of biosphere and photosynthesis evolution (living Planet
missions, Darwin) We shall review how the results from these
ESA missions (and other relevant missions from other agencies) can
be exploited in synergy to advance our knowledge on the formation of
solar systems and on exoplanets.
Title: Astrobiology with ESA Science Missions
Authors: Foing, B. H.
Bibcode: 2002ASPC..269..361F
Altcode: 2002esip.conf..361F
No abstract at ADS
Title: Lunar Explorers Society: International Outreach Programme
Authors: Volp, J.; Foing, B.; ten Kate, I.; Rombaut, H.; Koppeschaar,
C.; van Susante, P.; Pachera, S.; Groemer, G.; Sanctuary, H.;
Marshall, W.
Bibcode: 2002EGSGA..27.6860V
Altcode:
"Aiming for the permanent presence of humanity on the Moon." The
Lunar Explorers Society was founded in 2000 by the attendees of the
International Conference on Exploration and Utilisation of the Moon
(ICEUM-4) held at ESTEC, Noordwijk the Netherlands. LUNEX is a society
open to all lunar explorers. Interested individuals or organisations
are invited to become members or sponsors. The main objectives of
LUNEX are: - to promote the exploration of the Moon for the benefit
of humanity. - to raise awareness of what could be achieved by
returning to the Moon - to promote international cooperation between
scientists working on Lunar missions by providing a neutral platform
for their discussions We want to reach as many people as possible,
world-wide, with our educational and outreach activities to explain
our cause and its benefits to humanity. We will give an overview
of LUNEX and the education and outreach activities under- taken and
planned by it's National Chapters. http://www.lunarexplorers.org
Title: Science Operations For Esa's Smart-1 Mission To The Moon
Authors: Almeida, M.; Foing, B.; Heather, D.; Marini, A.; Lumb, R.;
Racca, G.
Bibcode: 2002EGSGA..27.5134A
Altcode:
The primary objective of the European Space Agency's SMART-1 mission
to the Moon is to test and validate a new electric propulsion engine
for potential use on other larger ESA Cornerstone missions. However,
the SMART-1 spacecraft will also carry a number of scientific
instruments and experiments for use en-route to and in orbit about
the Moon. SMART-1's major operational constraint is that it will be
only contacted twice per week. As a result, there will be a stronger
emphasis on mid-term planning, and the spacecraft will be operated using
a large list of telecommands sent during the communication windows. This
approach leads to a higher probability of there being resource and/or
instruments conflicts. To eliminate these, two software tools were
developed: the Experiment Planning System (EPS), and the Project Test
Bed (PTB). These tools will also allow us to predict the lunar coverage
of the scien- tific instruments, and to simulate target selections.
Title: SMART-1 Technology and Science Experiments and their Operations
Authors: Marini, A.; Lumb, R.; Dias-Almeida, M.; Foing, B. H.
Bibcode: 2002iaf..confE.713M
Altcode:
SMART-1, the first European mission to the Moon, hosts 10 Technology
and science experiments run by 7 on-board instruments. The primary
objective of the mission is the demonstration of the solar electric
propulsion. Therefore the monitoring of the spacecraft plasma
environment and the contamination produced by the Stationary Plasma
thruster is a key-task, which will be carried out by two experiments
(SPEDE - Spacecraft Potential, Electron and Dust Experiment -
and EPDP - Electric propulsion diagnostic Package). SPEDE and EPDP
will contribute also to the characterisation of the near-Earth and
interplanetary plasma environment and to study the solar wind. A package
of three spectroscopy and imaging instruments has been selected to
run technology demonstration of miniaturised compact instrument for
planetary remote sensing and for carrying out valuable science at the
Moon. AMIE (Asteroid-Moon micro-Imager Experiment) is a miniature
medium-resolution (30 m at 300 km height) camera, equipped with a
fixed panchromatic and 3-colour filter, for Moon topography and imaging
support to other experiments. D-CIXS (Demonstration of a Compact Imaging
X-ray Spectrometer) is based on novel detector and filter/collimator
technologies, and will perform the first global mapping of the
lunar elemental composition, by looking at X-ray fluorescence in the
0.5-10 keV range. It is supported in its operation by XSM (X-ray Solar
Monitor) that also monitors long-term coronal X-ray emission and solar
flares. SIR is a miniature near-infrared spectrometer operating in the
0.9-2.6 μm wavelength range and will carry out mineralogical survey
of the lunar crust in a previously uncovered bandwidth. Technology
experiments for deep space communications are: The SMART-1 Instruments
have been integrated in the Spacecraft in the current year and have
undergone functional verification following environmental tests. The
Experiments will be performed during two distinct phases of the
SMART-1 mission, including: - the 17-month Earth escape phase when the
spacecraft will spiral out our planet to perform a weak - a nominal
6-month operational phase in elliptical Moon orbit with peri-centre
around the south The planning and co-ordination of the Technology and
science experiments operations is carried out at ESA/ESTEC, where an
agile service has been set up to connect and co-ordinate remotely the
technology and science experimenters and to provide the experiment
master plan to the Mission Operations Centre located at ESOC. The
SMART-1 STOC (Science and Technology Operations Co- ordination) facility
works in close synergy with the science operations teams of other ESA
Planetary missions (Rosetta, Mars Express and Bepi-Colombo), making
use of Internet communication and flexible scheduling and simulations
tools. The SMART-1 STOC supports also the mission data archiving and
is designed to provide the engineering and scientist communities with
mission data access based on the PDS (Planetary Data System) Standard.
Title: Smart-1 Project Development Status
Authors: Racca, G. D.; Foing, B. H.; SMART-1 Project Team
Bibcode: 2002EGSGA..27.1152R
Altcode:
SMART-1 is the first of the Small Missions for Advanced Research in
Technology of the ESA Horizons 2000 Science Plan. The main mission
objective of SMART-1 is to demonstrate key technologies for Bepi-Colombo
and other scientific deep-space missions. One of the key technologies
is the solar electric propulsion used as primary propulsion. The
electric propulsion will be using 1400W to transfer the 350 kg space-
craft from an Ariane-5 standard GTO to an elliptic Moon polar orbit,
10000x300 km. The total mission time is 24 months including a maximum
of 18 months transfer time. The spacecraft development entered the
detailed design and implementation phase in October 1999, under the
responsibility of the Swedish Space Corporation as prime contractor,
and the flight acceptance is targeted for the end of 2002. Apart
from the in-orbit demonstration of electric propulsion as primary
propulsion, SMART-1 is im- plementing many other enabling technologies
for deep-space missions. In addition, the spacecraft avionics design is
tailored to the low cost philosophy by enabling flexi- ble integration
of Commercial Off The Shelf (COTS) equipment. The scientific instru-
ments support the characterisation of the electric propulsion thrust
environment during the long transfer phase and detailed imaging and
spectroscopy of the lunar surface in visible, infrared and X-ray during
the Moon orbiting phase. The paper summarises the baseline mission and
spacecraft design. The main part of the paper highlights the spacecraft
design status and the assembly, integration and verification activities.
Title: Smart-1 Science Experiments Co-ordination and Expected Outputs
Authors: Almeida, M.; Foing, B.; Heather, D.; Marini, A.; Lumb, R.;
Racca, G.
Bibcode: 2002EGSGA..27.5101A
Altcode:
SMART-1 is the first European Space Agency mission to the Moon. The
primary ob- jective of the mission is to test and validate a new
electric propulsion engine for poten- tial use on other larger ESA
cornerstone missions. However the SMART-1 spacecraft will also carry
a number of scientific instruments and experiments for use en-route to
and in Orbit about the Moon. The payload comprises several instruments
and ex- periments: the Asteroid Moon Micro Imager Experiment (AMIE),
the Demonstration Compact Imaging X-ray Spectrometer (D-CIXS), the
X-ray Solar Monitor (XSM), the SMART-1 Near-Infrared Spectrometer (SIR),
the Electric Propulsion Diagnostic Package (EPDP), the Deep Space X/Ka
Band TTC Experiment (KaTE), the Radio Science Investigation for SMART-1
(RSIS), and the Spacecraft Potential, Electron and Dust Experiment
(SPEDE). During Lunar Orbit, the great majority of scientific activ-
ities will be carried out. The AMIE multispectral high resolution camera
will mainly aim to image the lunar South Pole and map the southern
regions of the Moon. D-CIXS will look for the spatial distribution
of major lunar rock types and the X-ray emission from impact of
solar wind electrons on the night-side Moon. SIR will gather data to
study the mineralogy of the lunar surface. During this phase the RSIS
experiment will also take place, using AMIE images and the high accuracy
tracking provided by KaTE to measure the lunar libration. Also in the
frame of the mission a co-ordinated utilization of the experiments
is envisaged. The Science and Technology Operations Co-Ordination
(STOC) will be in charge of this task. The STOC will, in face of the
capabilities of the experiments, advise experiments teams, to study
specific features of the Moon at the same time. The data acquired
this way, when cross-checked, will be able to produce higher value
results. The STOC will also study SMART-1 data in comparison with
former Moon data. Examples of these activities and what enhanced
science results can be obtained will be presented.
Title: SMART-1 technology preparation for future planetary missions
Authors: Marini, A. E.; Racca, G. D.; Foing, B. H.
Bibcode: 2002AdSpR..30.1895M
Altcode:
SMART-1 is the first ESA Small Mission for Advanced Research in
Technology, with the prime objective of demonstrating the use of Solar
Electric Primary Propulsion in a planetary mission. Further to this,
SMART-1 will test novel spacecraft technologies and will host six
instruments carrying out nine technology and science experiments, all
aimed at preparing future ESA Cornerstones, including the ESA Mercury
Cornerstone (now named BepiColombo) and other future planetary missions
under study, as well as solar and fundamental physics missions.
Title: Ground Support Programme For Future Mars Missions
Authors: ten Kate, I. L.; Ruiterkamp, R.; Lehmann, B.; Gomez
Hernandez, C.; Foing, B. H.; Becker, L.; Berstein, M.; Jessberger,
E.; Ehrenfreund, P.
Bibcode: 2002EGSGA..27.4768T
Altcode:
The search for organic molecules and tracers of life on Mars is the
future perspective of several Mars missions. The experimental research
programme described here in- vestigates the most abundant organic
molecules identified in solar system bodies and beyond, which may
have been exogeneously delivered to the Martian surface. A vacuum
chamber, located at ESTEC, NL, equipped with a solar simulator will be
used to collect data on the combined effects of UV photoprocessing,
atmospheric con- ditions and the presence/absence of oxidzing agents
on organic molecules. The cham- ber has a possibility of thermal
and pressure control. A window allows the attachment of UV lamps and
filters. Samples will be introduced into the chamber on a specially
designed tray. Sample trays will be filled with organic molecules
embedded in soil analogues, either porous or compact. During the
simulation in situ measurements are taken in the chamber, using
a GCMS. Samples will be retrieved with various deriva- tization
techniques. Thereafter the probes are subjected to various analyses,
such as HPLC, spectroscopy, GC, LDMS and TOF-SIMS. The results
of those simulations are part of a ground support experiment programme
for future Mars missions.
Title: Public Outreach With Smart-1
Authors: Almeida, M.; Foing, B.; Heather, D.; Marini, A.; Lumb, R.;
Racca, G.
Bibcode: 2002EGSGA..27.5132A
Altcode:
SMART-1 will be the first European Space Agency mission to the
Moon. Therefore it is possible to foresee that any public outreach
activity related to the mission can have a big impact in the media
and public in general. This expectation for a large audience carries
with it the large responsibility to create a program where is maximized
the quality, both didactic and ludic, of the public outreach products,
in order to keep the interest in the mission for a longer period. In
order to assure the good quality of these products it is important
that even when planning the mission some of the targets are selected
for its rich outreach content. This presentation will focus on some
of the public outreach activities envisaged for SMART-1 as well as
the selection of the most suitable targets for that end.
Title: Photometric studies of the Moon with AMIE/Smart-1
Authors: Shkuratov, Y.; Kreslavsky, M.; Foing, B.
Bibcode: 2002cosp...34E1510S
Altcode: 2002cosp.meetE1510S
Three different directions of photometric studies with AMIE camera of
Smart-1 mission might be possible: (1) mapping slope of phase function
to search for photometric anomalies; (2) studying the opposition
spike; and (3) detailed study of photometric function in tracking
mode of Smart-1. The first direction allows studies of photometric
anomalies related with fresh impact craters with implications for
estimates of the regolith gardening rate and projectile flux in recent
epoch; investigations of regolith structure anomalies associated with
swirls; searching for traces of geologically recent seismic events. The
second direction makes it possible to study regional variations of the
characteristic soil particle size and particle aggregate structure. The
third one (tracking mode) allows us to study subtle characteristics of
photometric function that gives information about meso-scale structure
of the lunar surface. Specific demands for the photometric studies are
the following. At least 2 i ages of the same scene are needed to provide
the firstm direction. The best choice of the phase angles: 10-20° for
one of images and 30-50° for the other one. The phase angle difference
should be >15° but < 30° One of the images can be taken from the
Clementine data set, though pairs of AMIE images are preferable. Only
Clementine images without compression losses can be used for this. Two
images of the same scene are needed to study the opposition spike. One
of them should contain the zero phase angle point. The other should be
taken at a phase angle 10 - 40° One of the images can be taken from
the Clementine data set. The tracking mode assumes taking a set of
AMIE images for the same scene while the spacecraft is moving along
its orbits. Including the zero phase angle point into the imaging
sequence would increase the scientific output of the tracking mode
series of images. Flat surface is necessary for photometric mapping with
AMIE. Regions for mapping with the highest priority are the Apollo-11,
-12, -14, and -16 landing sites; the tracking mode is desirable in
these cases. The prospective regions are also: Surveyor and Luna
landing sites, swirls, selected typical mare areas, and sites that
have been imaged with Clementine in the opposition.
Title: Space activities in exo-astrobiology
Authors: Foing, Bernard H.
Bibcode: 2002abqc.book..389F
Altcode:
A brief overview is given about astronomical (NGST, GAIA, COROT,
EDDINGTON, KEPLER and DARWIN) and planetary (CASSINI-HUYGENS, STARDUST,
ROSETTA, MARS-EXPRESS and future Mars missions, Europa missions, Moon,
Mercury missions) space missions, which will investigate astrobiological
aspects during their operation phase.
Title: Complex Organics On Mars
Authors: ten Kate, I. L.; Ruiterkamp, R.; Lehmann, B.; Gomez Hernandez,
C.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 2002EGSGA..27.4134T
Altcode:
One of the key questions in Astrobiology is to search for organic
molecules and to characterise their survival in Martian rocks and in the
Martian subsurface. The most relevant molecules in this context, which
can be studied in the laboratory are organic compounds identified in
meteorites. Among those are aliphatic and aromatic hydrocar- bons,
amino acids, polycyclic aromatic hydrocarbons (PAHs), fullerens
and kerogens. Using a Mars simulation chamber, we will study those
prebiotic and large stable car- bon compounds embedded in Martian soil
analogues. To perform the above described tasks the chamber will be
equipped with a sample tray, a solar simulator and will be able to serve
as a glovebox. The chamber will be used to validate some measurements
to be made by Beagle 2 with representative or complementary ground
instruments. The results of the simulation studies will be compiled
in a database to serve the inter- pretation of future Mars missions.
Title: An elemental abundance analysis of the mercury manganese star
HD 29647
Authors: Adelman, S. J.; Snow, T. P.; Wood, E. L.; Ivans, I. I.;
Sneden, C.; Ehrenfreund, P.; Foing, B. H.
Bibcode: 2001MNRAS.328.1144A
Altcode:
The sharp-lined mercury manganese (HgMn) star HD 29647, which is
located behind the outer envelope of the Taurus Molecular Cloud 1, is
of interest for both its stellar properties and its utility as a probe
of interstellar gas and dust along its line of sight. In this paper we
review the properties of the star, summarize its line identifications
and present an abundance analysis based on spectrograms obtained at the
McDonald Observatory and the Observatoire de Haute-Provence. This star
has elemental abundances similar to those of other HgMn stars except
that its He/H ratio is closer to solar, possibly indicating a young
age, and that it, like HR 7775, is overabundant in selected elements
including the rare earths. The stellar radial velocity, unfortunately,
closely matches that of the foreground cloud.
Title: Modelling of the Electric Propulsion Induced Plasma Environment
on SMART-1
Authors: Tajmar, M.; Gonzalez, J.; Foing, B.; Marini, A.; Noci, G.;
Laakso, H.
Bibcode: 2001ESASP.476..575T
Altcode: 2001sct..conf..575T
No abstract at ADS
Title: Characteristics of the Plasma Environment for the SMART-1
Mission
Authors: Laakso, H.; Foing, B.
Bibcode: 2001ESASP.476..601L
Altcode: 2001sct..conf..601L
No abstract at ADS
Title: The Diffuse Interstellar Bands and Organic Molecules in Space
Authors: Ehrenfreund, P.; Tuairisg, S. Ó.; Foing, B. H.;
Sonnentrucker, P.; Cami, J.
Bibcode: 2001bbbb.conf..150E
Altcode:
No abstract at ADS
Title: Exo-astrobiology with ESA space science missions
Authors: Foing, Bernard H.
Bibcode: 2001ESASP.496..121F
Altcode: 2001eab..conf..121F
Key questions of astrobiology can be addressed by several space
missions from the ESA Science Horizons 2000 Programme, such as:
How do solar and stellar systems form? (with ISO, FIRST, SMART-1,
Rosetta, Colombo, Gaia). Geological evolution of terrestrial
planets (with Living planet, Mars-express, SMART-1, Bepi-Colombo
to Mercury). Interstellar Complex organic chemistry (with ISO,
ISS/EXPOSE, FIRST, Rosetta). Co-evolution of Earth-Moon, impacts
life frustration (with SMART-1, Bepi-Colombo). How to detect other
solar systems and habitable zones (with space photometry, COROT,
Eddington, Gaia, IRSI-Darwin). Early Earth and alternative environments
(Huygens/Cassini and Mars-express). Signature of biosphere, global
biomarkers and photosynthesis evolution (living Planet missions,
Darwin). Water and exobiology on Mars (with orbiter instruments and
Beagle-2 lander on Mars-express). Study of biomarkers and delivery of
organics (with Mars-express and future missions). We shall review the
exo-astrobiology potential from these ESA missions.
Title: "Organics" experiment on the International Space Station
Authors: Ruiterkamp, Richard; Ehrenfreund, Pascale; Foing, Bernard;
Salama, Farid
Bibcode: 2001ESASP.496..137R
Altcode: 2001eab..conf..137R
In this experiment, large organics will be exposed on a long duration
radiation facility on the International Space Station. The results of
this experiment will help us to identify specific carbonaceous molecules
in the interstellar medium (ISM) and to monitor their evolution and
possible incorporation into Solar System material. The results also
allow us to make predictions concerning the survival probabilities of
specific organic species in space.
Title: ESA'S SMART-1 Mission to the Moon
Authors: Foing, B. H.; Heather, D.; Almeida, M.; Racca, G.; Marini,
A.; SMART-1 Team
Bibcode: 2001LPI....32.1787F
Altcode:
ESA's SMART-1 technology mission is to be launched at the end of
2002, to reach the Moon with Solar Electric Propulsion. Its visible
multicolour camera, near IR spectrometer, an X-ray spectrometer will
address current key questions of lunar and planetary science.
Title: Next Steps for International Lunar Exploration
Authors: Foing, B. H.; Duke, M.; Galimov, E.; Mizutani, H.; Ilewg
Bibcode: 2001LPI....32.1827F
Altcode:
We report activities and recommendations from the conferences organised
by ILEWG International Lunar Exploration Working Group. This covers
science questions, technology, data exchange, resources utilisation,
the Moon as step to Mars and solar system exploration.
Title: Outreach and Education from ESA's SMART-1 Mission to the Moon
Authors: Heather, D. J.; Foing, B. H.; van Susante, P.; Almeida, M.
Bibcode: 2001LPI....32.1983H
Altcode:
We present some of the possible outreach and education activities that
are being considered for use during ESA's SMART-1 mission to the Moon,
including 'adopt a crater', 'illuminating poles' and others. Packages
will be produced for all levels.
Title: Results and Recommendations from the International Conference
on the Exploration and Utilisation of the Moon 4 (ICEUM4)
Authors: Foing, B. H.; Heather, D. J.; Duke, M.; Racca, G.; Pieters,
C.; Mizutani, H.; Galimov, E.; Dunkin, S. K.; van Susante, P.;
Frischauf, N.; Almeida, M.; Participants, Iceum4
Bibcode: 2001LPI....32.1712F
Altcode:
We present here highlights and recommendations from the ILEWG organized
ICEUM4 meeting held in the Netherlands in July 2000
Title: Highlights from ICEUM4, the 4th International Conference on
the Exploration and Utilisation of the Moon
Authors: Foing, B. H.; Duke, M.; Galimov, E.; Mizutani, H.; Pieters,
C.; Racca, G.; Heather, D. J.; Frischauf, N.; van Susante, P.;
Almeida, M.
Bibcode: 2001EM&P...85..133F
Altcode: 1999EM&P...85..133F
The Fourth International Conference on the Exploration and Utilisation
of the Moon (ICEUM4) at ESTEC in July 2000 was organised by the
International Lunar Exploration Working Group (ILEWG) and ESA. The
conference had a broad content including future missions such as
ESA's SMART-1 mission and the Japanese Lunar-A and SELENE projects,
technology support for these missions, the recent advances in science
of the Moon, human development of the Moon, and public outreach. The
proceedings of the conference have been published as ESA Publication
ESA SP-462 and an official declaration from the conference has been
constructed from recommendations made by task groups set up at the
conference. The declaration will be used as a focus for the efforts
of the Lunar Explorers Society (LUNEX), which was founded during the
meeting. Progress will be reported at ICEUM5, to be held as part of
the World Space Congress in Houston in October 2002.
Title: MUSICOS Observations of the Chromospherically Active Binary
Star EI Eridani
Authors: Washuettl, A.; Strassmeier, K.; Foing, B.
Bibcode: 2001AGM....18..P50W
Altcode: 2001AGAb...18Q.160W
We present results on spectroscopic observations of the rapidly-rotating
active binary star EI Eridani obtained during the MUSICOS multi-site
campaign in 1998. Seven sites around the globe were involved in order
to achieve a surface image within a few rotations as EI Eridani's
critical rotation period of 1.945 days makes it impossible to
obtain time-resolved images from a single site. The data were split
into groups in order to achieve consecutive, independent Doppler
Images. Furthermore, simultaneous photospheric and chromospheric
activity monitoring was carried out.
Title: The Science Goals Of Esa's Smart-1 Mission To The Moon
Authors: Foing, B. H.; Heather, D. J.; Almeida, M.; SMART-1 Science
Technology Working Team
Bibcode: 2001EM&P...85..523F
Altcode: 1999EM&P...85..523F
SMART-1 will be Europe's first lunar mission and represents an
important step forwards in developing an international program of
lunar exploration. The spacecraft will be ready for launch in late
2002, and is designed to test new technologies for use on future
ESA cornerstone missions. In this respect, SMART-1 will also play a
vital role in developing cutting edge technologies that could be a
major part of the future of lunar and planetary science. SMART-1 will
carry three remote sensing instruments that will be used during the
mission's nominal six months in lunar orbit. These instruments will
return data that will be relevant to a broad range of lunar studies,
from bulk crustal composition and theories of lunar origin/evolution
to the search for cold traps at the lunar poles and the mapping of
potential lunar resources. With a perilune near the lunar south pole,
the South Pole-Aitken Basin (SPA) is a prime target for studies using
the SMART-1 suite of instruments.
Title: Preliminary MUSICOS 96 results on Balmer line variability on
the T Tauri star SU aurigae
Authors: Oliveira, J. M.; Unruh, Y. C.; Foing, B. H.; MUSICOS 1996
Collaboration
Bibcode: 2001AdSpR..26.1747O
Altcode:
The study of young stellar objects is essential for the further
understanding of the early evolutionary stages of the Sun and
similar low-mass stars. In this context, T Tauri stars supply valuable
information on their pre-main sequence evolution. SU Aur is a classical
T Tauri star that shows little veiling and few emission lines. The
Balmer line profiles are extremely variable, even on short time
scales. We present results from the analysis of the variability of
these spectral lines, based on a data set obtained during the world-wide
multi-site spectroscopic MUSICOS 1996 campaign. We attempt to describe
the interaction of the stellar magnetosphere and the accretion disk,
and search for the signatures of mass inflow and ejection.
Title: Smart-1: The First Time Of Europe To The Moon; Wandering in
the Earth-Moon Space
Authors: Racca, Giuseppe D.; Foing, Bernard H.; Coradini, Marcello
Bibcode: 2001EM&P...85..379R
Altcode: 1999EM&P...85..379R
After 40 years from the first lunar missions, Europe has started for
the first time the development of a mission which has the Moon as
a target. SMART-1 will be the first Western-European mission to the
Earth's satellite. The primary objective of the mission is to flight
test technology innovation for the future scientific deep-space
missions. This paper describes the mission concept, the technology
and the scientific aspects.
Title: Spectral Line Variability in the Circumstellar Environment
of the Classical T Tauri Star SU Aurigae (CD-ROM Directory:
contribs/oliveira)
Authors: Oliveira, J. M.; Foing, B. H.; Unruh, Y. C.
Bibcode: 2001ASPC..223..539O
Altcode: 2001csss...11..539O
No abstract at ADS
Title: Preliminary investigation of circumstellar emission and flares
in the fast rotating giant FK comae
Authors: Oliveira, J. M.; Foing, B. H.
Bibcode: 2001AdSpR..26.1733O
Altcode:
FK Comae is a star with some very interesting peculiarities in the
solar-stellar connection context. This star is a G5 II fast-rotating
giant and its origin and extreme (near breakup) rotational velocity
remain a puzzle. It is a perfect candidate to study solar-like activity
in extreme conditions of low gravity and magnetic configuration. We
present time-resolved spectroscopic observations obtained with the
ESA-MUSICOS spectrograph at the Isaac Newton Telescope in May 97. One
of the most interesting spectral characteristics of this star is
the presence of broad emission in the Balmer and Ca II lines. In
particular, its Hα emission seems to extend up to several stellar
radii and is erratically variable. We present monitoring of this excess
emission, interpreted as arising from giant active loop structures
and prominences. We detected flares and also continuous micro-flaring
events, that can be associated with excitation/recombination of
these magnetically confined loops. The emission present in the He
I D3 line is also a clear indication of a very active chromosphere
and corona. We report on some modelling techniques applied to the
circumstellar environment of this star. We also describe a large flare
event observed in Hα, Hβ and He I D3.
Title: Lunar Explorers Society: Goals And Activities
Authors: Foing, B.; Van Susante, P.; Almeida, M.; Heather, D.; Duke,
M.; Dunkin, S.; Lunar Explorers Society
Bibcode: 2001EM&P...85..533F
Altcode: 1999EM&P...85..533F
The Lunar Explorers Society (LUNEX) was founded by the participants
of the 4th International Conference on the Exploration and Utilisation
of the Moon (ICEUM4), held in July 2000 at the European Space Research
and Technology Centre (ESTEC) in The Netherlands. ICEUM4 was organised
under the auspices of the International Lunar Exploration Working Group
(ILEWG), and aimed to draw together people from diverse backgrounds
with a common interest in the exploration of the Moon. At the end of
the conference, a formal ICEUM4 Declaration was drawn up detailing
the recommendations of the participants for the future of lunar
exploration. LUNEX will be a society open to all Lunar Explorers and
will aim to promote research, exploration and outreach programmes
that will work towards the realisation of the goals outlined in the
ICEUM4 Declaration. Following ICEUM4, a core group of active LUNEX
members was identified to begin to shape the new-born society with
guidance from ILEWG. A series of task groups have been installed to
address the key LUNEX issues, with strong participation of young lunar
explorers, and work is progressing towards the first LUNEX activities,
both at the level of the task groups and to form national chapters. The
first LUNEX convention will be held in March 2001, starting in Paris
with the opening session, then continuing in Houston at the LPSC
and closing in Nice during the EGS-conference. Further information
about the Lunar Explorers Society can be found on our Website:
http://www.lunarexplorers.org
Title: Dehydrogenation of polycyclic aromatic hydrocarbons in the
diffuse interstellar medium
Authors: Vuong, M. H.; Foing, B. H.
Bibcode: 2000A&A...363L...5V
Altcode: 2000astro.ph.10385V
We present a model for the hydrogenation states of Polycyclic Aromatic
Hydrocarbons (PAHs) in the diffuse interstellar medium. First, we
study the abundance of hydrogenation and charge states of PAHs due
to photo-ionization, photo-dissociation in the interstellar UV field,
electron recombination and chemical reactions between PAH cations and
H or H_2. For PAH cations, we find that the dehydrogenation effects
are dominant. The hydrogenation state of PAHs depends strongly on the
H density, the size of molecule and UV field. In diffuse clouds with
low H density and normal UV radiation, PAHs containing less than 40 C
are completely or strongly dehydrogenated whereas at high H density,
they are normally hydrogenated. The partially dehydrogenated species
dominate in intermediate density clouds. PAHs above 40 C are quite
stable and are fully hydrogenated, which would favor their spectroscopic
search in near IR surveys of Diffuse Interstellar Bands (DIBs).
Title: On the identification of the C60+
interstellar features
Authors: Galazutdinov, G. A.; Krełowski, J.; Musaev, F. A.;
Ehrenfreund, P.; Foing, B. H.
Bibcode: 2000MNRAS.317..750G
Altcode:
The identity of the carriers of the diffuse interstellar bands (DIBs)
is one of the most fascinating puzzles of modern spectroscopy. Over the
last few years the number of known DIBs has grown substantially. In
this paper we discuss the two recently discovered near-infrared
weak interstellar features which have already been proposed as
fingerprints of the buckminsterfullerene [formmu2] We present and
discuss measurements of the two related DIBs within a larger sample of
reddened targets, observed with different spectrometers, telescopes
and site conditions. We provide additional arguments in favour of
the interstellar origin of the two bands. We find evidence around
the 9577-Å DIB of far-wing structures, which may affect broad-band
measurements. We estimate corrections and errors for telluric and
stellar blends, and show that the cores of the two DIBs are well
correlated with a ratio near unity within 20per cent. Finally, we
discuss their relation to the laboratory spectra of [formmu3] and the
search for two expected weaker [formmu4] transitions.
Title: The ESA SMART-1 Mission to the Moon: Goals and Science
Authors: Foing, B. H.; Racca, G. R.; SMART-1 Science and Technology
Working Team
Bibcode: 2000DPS....32.2409F
Altcode: 2000BAAS...32.1037F
SMART-1 is the first in the programme of ESA's Small Missions for
Advanced Research and Technology . Its objective is to demonstrate
Solar Electric Primary Propulsion (SEP) for future Cornerstones
(such as Bepi-Colombo) and to test new technologies for spacecraft and
instruments. The project aims to have the spacecraft ready in October
2002 for launch as an Ariane-5 auxiliary payload. After a cruise with
primary SEP, the SMART-1 mission is to orbit the Moon for a nominal
period of six months, with possible extension. The spacecraft will
carry out a complete programme of scientific observations during the
cruise and in lunar orbit. SMART-1's science payload, with a total
mass of some 15 kg, features many innovative instruments and advanced
technologies. A miniaturised high-resolution camera (AMIE) for lunar
surface imaging, a near-infrared point-spectrometer (SIR) for lunar
mineralogy investigation, and a very compact X-ray spectrometer (D-CIXS)
with a new type of detector and micro-collimator which will provide
fluorescence spectroscopy and imagery of the Moon's surface elemental
composition. The payload also includes an experiment (KaTE) aimed at
demonstrating deep-space telemetry and telecommand communications in the
X and Ka-bands, a radio-science experiment (RSIS), a deep space optical
link (Laser-Link Experiment), using the ESA Optical Ground station
in Tenerife, and the validation of a system of autonomous navigation
SMART-1 lunar science investigations include studies of the chemical
(OBAN) based on image processing. SMART-1 lunar science investigations
include studies of the chemica composition and evolution of the Moon,
of geophysical processes (volcanism, tectonics, cratering, erosion,
deposition of ices and volatiles) for comparative planetology, and
high resolution studies in preparation for future steps of lunar
exploration. The mission could address several topics such as the
accretional processes that led to the formation of planets, and the
origin of the Earth-Moon system.
Title: Magnetospheric accretion and winds on the T Tauri star SU
Aurigae. Multi-spectral line variability and cross-correlation
analysis
Authors: Oliveira, J. M.; Foing, B. H.; van Loon, J. Th.; Unruh, Y. C.
Bibcode: 2000A&A...362..615O
Altcode: 2000astro.ph..9087O
SU Aurigae is a T Tauri star that was well monitored during the MUSICOS
96 multi-site campaign. We present the results of the spectroscopic
analysis of the circumstellar environment of this star, particularly
of the Hα , Hβ , Na I D and He I D3 line profiles. The signatures of
modulated outflows and mass accretion events are analysed, as well as
transient spectral features. We compute the cross-correlation function
(CCF) of several pairs of (velocity bins in) spectral lines to better
investigate the profiles' temporal variability. We found increasing
time lags between the variability of He I D3, Na I D and Hβ . We
propose this may be understood in terms of azimuthal distortion of the
magnetic field lines due to the different rotation rates of the star
and the disk. We find the slightly blueshifted absorption features in
Hα , Hβ \ and Na I D to be anti-correlated with the accretion flow
signatures. We propose that the transient absorption features in the
blue wings of Hα , Hβ \ and Na I D (signatures of mass outflows),
and flare brightenings are related to the disruption of distorted
magnetospheric field lines. Based on observations obtained during the
MUSICOS~96 campaign in which were involved: Isaac Newton Telescope
(INT, La Palma), Observatoire de Haute Provence (OHP, France), McDonald
Observatory (MDO, USA), Beijing Astronomical Observatory (BAO, Xinglong,
China) and Canada-France-Hawaii Telescope (CFHT, Hawaii).
Title: Exploration and Utilisation of the Moon
Authors: Foing, B. H.; Perry, M.
Bibcode: 2000ESASP.462.....F
Altcode: 2000eum..conf.....F
No abstract at ADS
Title: The D-CIXS X-Ray Spectrometer on ESA's SMART-1 Mission to
the Moon
Authors: Grande, M.; Browning, R.; Dunkin, S.; Parker, D.; Kent, B.;
Kellett, B.; Perry, H. C.; Swinyard, B.; Phillips, K.; Huovenin, J.;
Thomas, N.; Hughes, D.; Alleyne, H.; Grady, M.; Lundin, R.; Barabash,
S.; Baker, D.; Murray, D. C.; Guest, J.; Casanova, I.; D'Uston, C. L.;
Maurice, S.; Foing, B.; Heather, D.; Clark, E. P.; Kato, M.
Bibcode: 2000ESASP.462...97G
Altcode: 2000eum..conf...97G
No abstract at ADS
Title: From Interstellar Dust via Comets to Life?
Authors: Ehrenfreund, Pascale; Boogert, Adwin; Enzian, Achim;
Gerakines, Perry; Foing, Bernard
Bibcode: 2000OLEB...30..342E
Altcode:
More than 120 interstellar and circumstellar molecules are currently
identified in the gas phase along with a small fraction of interstellar
dust composed of amixture of materials from various cosmic sources
(Spaans & Ehrenfreund 1999). Recent ground-based observations
and satellite data from the Infrared Space Observatory ISO have
provided revolutionary results concerning the nature of cosmic 'dust
particles. Interstellar grains act as an important catalyst in the
interstellar medium. Processes such as ultraviolet irradiation, cosmic
ray bombardment mid - temperature variations determine the grain mantle
growth and chemical evolution. The incorporation of interstellar
matter in meteorites and comets in the pre-solar nebula provides
the basis for the "cosmic dust connection" (Ehrenfreund 1999). A
comparison of interstellar and cometary dust using recent ISO data
and ground-based measurements has revealed important similarities
but also indicated that comets contain beside pristine interstellar
material, admixtures of processed material (Ehrenfreund et al. 1997,
Ehrenfreund 2000). The investigation of molecules in interstellar
clouds and comets is essential to reveal the link between dust in the
interstellar medium and in the Solar System and provides important
clues on the prebiotic chemical evolution on Earth. In space most
of the chemical evolution toward complex molecules takes place in the
solid phase, particularly accessible to laboratory simulations. We
present laboratory data relevant to ultraviolet irradiation, cosmic ray
bombardment and thermal processing of dust. This allows to reconstruct
the conditions in.the.protostellar environment and to monitor the
evolution of simple carbon bearing species to complex molecules and
aromatic networks. New results indicate in fact a lack of radiation
processing in dense clouds, which may strongly decrease the yield of
organics formed in those environments (Ehrenfreund et al. 1998). We
present studies on the outgassing properties of bright comets (such as
Hale-Bopp and Hyakutake) which are compared to recent interstellar dust
model predictions. We critically discuss whether interstellar molecules
brought by comets may act as precursors for biogenic molecules.
Title: Evolution and Survival of Complex Organics in Space
Authors: Foing, B. H.; Sonnentrucker, P.; Lasseur, C.; Ehrenfreund,
P.; O'Tuaisrig, S.; Cami, J.; Krelowski, J.
Bibcode: 2000OLEB...30..225F
Altcode:
Astronomical circumstellar and interstellar observations in the UV,
visible and infrared reveal the signature of complex carbonaceous
material. The evolution of these complex organics from stars,
interstellar medium to the early solar systems and habitable bodies,
is a key to the origin of life. We discuss the evidence for complex
organics in the interstellar medium from their spectral signature such
as UV extinction, Diffuse Interstellar Bands and Aromatic Infrared
Emission Bands. We review new information on the carriers of the
visible Diffuse Interstellar Bands. Evidence for large molecules
with 30-70 C atoms was shown for several Dills (Ehrenfreund &
Foing 1996). A statistical study indicates that carriers of Dills
are distinct molecules, though some show a family behaviour (Cami
et al. 1997). A new survey of diffuse interstellar bands reports a
population of Dills molecules enhanced in specific lines of sight (0'
Tuaisrig et al. 1999). Correlations with simple molecular species such
as CH or CH+ (Krelowski et al. 1999) or atomic species (Sonnentrucker
et al. 1999) indicate where Dill carriers reside in interstellar
clouds. New information was derived on ionisation (Sonnentrucker
et al. 1997) and double-ionisation properties which determine the
physical state and survival of these species. We discuss relevant
laboratory and theoretical studies stimulated by related astronomical
observations. Recent results are described on the search for specific
Polycyclic Aromatic Hydrocarbons, long carbon chains, fullerenes (Foing
& Ehrenfreund 1994, 1997), fulleranes and derived compounds. We
discuss how the abundances and signatures of these molecules vary in
different interstellar and circumstellar environments. We describe
constraints on the formation, evolution, ionisation, destruction,
survival of these complex organics in the interstellar medium. The
distribution of PAHs and fullerenes measured in meteorites was compared
to that derived for interstellar environments (Foing et al. 1999). Our
"Organic Matter" experiment selected to fly on the International Space
Station Exposure Facility to UV, cosmic ray, and vacuum conditions will
further investigate the evolution of complex organics in space. Finally,
we discuss some open questions on the transport and delivery of these
complex organics into the solar system and onto Earth.
Title: Exploration and Utilisation of the Moon: ICEUM4, ESTEC 10-15
July 2000
Authors: Foing, B. H.; Duke, M.; Galimov, E.; Mizutani, H.; Ilewg
Bibcode: 2000LPI....31.1757F
Altcode:
No abstract at ADS
Title: The D-CIXS X-ray Spectrometer on ESA's SMART-1 Mission to
the Moon: Science Objectives
Authors: Dunkin, S. K.; Grande, M.; Heather, D. J.; Alleyne, H.;
Casanova, I.; Clark, A. Christou P. E.; Fernandes, V. A.; Foing,
B. H.; Huovenin, J.; Kaukkanen, J.; Russell, S. S.; Kellett, B. J.;
Swinyard, B.; Vilhu, O.
Bibcode: 2000LPI....31.1648D
Altcode:
No abstract at ADS
Title: Lunar Elemental Composition and Investigations with D-CIXS
X-Ray Mapping Spectrometer on Smart-1
Authors: Grande, M.; Browning, R.; Waltham, N.; Kent, B.; Kellett,
B.; Perry, C. H.; Phillips, B. Swinyard K.; Huovenin, J.; Thomas,
N.; Livi, S.; Mal, U.; Hughes, D.; Alleyne, H.; Lundin, M. Grady R.;
Barabash, S.; Baker, D.; Murray, C. D.; Guest, J.; Dunkin, S. K.;
Maurice, I. Casanova S.; Foing, B.
Bibcode: 2000LPI....31.1442G
Altcode:
No abstract at ADS
Title: A deep echelle survey and new analysis of diffuse interstellar
bands
Authors: Tuairisg, S. Ó.; Cami, J.; Foing, B. H.; Sonnentrucker,
P.; Ehrenfreund, P.
Bibcode: 2000A&AS..142..225T
Altcode:
We report a deep survey of diffuse interstellar bands (DIBs) between
3906 Ä and 6812 Ä under consistent observing conditions toward three
very reddened and five unreddened stars. BD+63deg 1964's
line-of-sight was shown to present exceptional DIB enhancement in number
as well as in strength. The early spectral type of the star and the use
of spectra of an unreddened comparison star of the same spectral type
allowed to limit stellar line residuals. Using careful reduction and
analysis methods we discovered 60 new DIBs which are confirmed in the
reddened targets HD 183143 and BD+40deg 4220. We detected
25 possible DIBs which still await further confirmation, but we did
not detect or confirm 28 previously reported DIBs. The present survey
with 226 confirmed DIBs, measured in three targets allows a detailed
and homogeneous statistical analysis on the distribution of DIB widths
and intensities. Based on observations at Observatoire Haute Provence
with the spectrograph ELODIE Figures 6 to 40 are only available in
electronic form at http://www.edpsciences.org
Title: Status of SMART-1 ESA Mission to the Moon
Authors: Foing, B. H.; Racca, G. R.; Marini, A.; Grande, M.; Keller,
U.; Josset, J. L.; Laakso, L. Iess H.; SMART-1 Team
Bibcode: 2000LPI....31.1677F
Altcode:
No abstract at ADS
Title: Large-Scale Evolution of the Active Region NOAA 7978, 7981,
7986 Observed by Goes, Soho, and Yohkoh
Authors: Orlando, S.; Khan, J.; van Driel-Gesztelyi, L.; Thompson,
B.; Fludra, A.; Foing, B.
Bibcode: 2000AdSpR..25.1913O
Altcode:
We took part in a joint project aimed to study the large-scale
evolution of an active region from its emergence throughout its decay
for several solar rotations. Our interest focuses on the understanding
of how energy is generated, released, deposited, and transformed in
active regions. To this end, we determined physical parameters like
intensity, temperature, and emission measure of the whole active region
as a function of time for the entire period selected. We present the
preliminary results of the analysis of GOES (Geosynchronous Operational
Environmental Satellite), SOHO (Solar and Heliospheric Observatory)
and Yohkoh data of the active region named NOAA 7978, 7981, and 7986
observed between July and October 1996
Title: Multi-Site Spectroscopy on FK Comae: An Extreme Activity
Laboratory
Authors: Oliveira, J. M.; Foing, B. H.
Bibcode: 2000ASIC..544..719O
Altcode: 2000vsea.conf..719O
No abstract at ADS
Title: Flares and Large Scale Evolution of a Solar Active Region
Observed in 1996 by GOES, SOHO and YOHKOH: Implications for X-Ray
stellar Variability
Authors: Orlando, S.; van Driel-Gesztelyi, L.; Thomson, B.; Khan,
J.; Foing, B. H.
Bibcode: 2000ASIC..544..783O
Altcode: 2000vsea.conf..783O
No abstract at ADS
Title: Dynamics of Chromiospheric and Transition Region Lines Observed
with SOHO/SUMER and the GCT/Tenerife
Authors: Muglach, K.; Fleck, B.; Schühle, U.; Stolpe, F.; Foing,
B. H.; Wilhelm, K.
Bibcode: 2000AdSpR..25.1731M
Altcode:
High-resolution spectroscopic observations of the quiet Sun have been
carried out in September 1996 at the German Gregory Coudé Telescope
(GCT) in Tenerife and in May 1997 with the SUMER instrument onboard
SOHO. Time sequences of spectra in the visible and near infrared
as well as in the ultraviolet have been taken, covering a range of
heights from the solar photosphere up into the transition region. In
this contribution we present the dynamical behaviour observed at the
various heights in the solar atmosphere
Title: The Circumstellar Environment of the TTS SU Aurigae
Authors: Oliveira, J. M.; Foing, B. H.; van Loon, J. Th.
Bibcode: 2000ASPC..219..181O
Altcode: 2000astro.ph..4377O; 2000dpp..conf..181O
In this contribution we investigate how a disk determines the physical
and geometrical properties of the circumstellar environment of the T
Tauri SU Aurigae. Our model of the spectral energy distribution of this
star includes the central young star, a flat black disk and a diffuse
envelope. We also describe the inner interaction region between the
disk and the star, the magnetosphere, by analysing the accretion and
wind signatures in several spectral lines observed during the MUSICOS
96 campaign.
Title: Spectral Line Variability in the Circumstellar Environment
of the Classic al T Tauri Star SU Aurigae
Authors: Oliveira, J. M.; Foing, B. H.; Unruh, Y. C.
Bibcode: 1999astro.ph.12199O
Altcode:
SU Aurigae is a classical T Tauri star of spectral type G2. This star
was one of the scientific targets of the MUSICOS 96 multi-site campaign
that provided a wealth of high resolution cross-dispersed spectral data
with a good continuous time coverage. We present the results of the
analysis of the complex circumstellar environment of this star, with
particular regard to magnetospheric models, in which the accretion from
the disk is channelled onto the star along magnetic field lines. The
signatures of modulated outflows and mass accretion events are present
in the spectra, as well as transient spectral features. We computed
auto-correlation and cross-correlation functions to better investigate
the source of the profiles' variability. The comparison of the profiles
of different spectral lines allows us to study the footprints of events
effectively observed at different distances from the stellar surface.
Title: SMART-1 Technology and Science Experiments in Preparation of
Future Missions and ESA Cornerstones
Authors: Marini, A. E.; Racca, G. D.; Foing, B. H.; SMART-1 Project
Bibcode: 1999BAAS...31Q1592M
Altcode:
SMART-1 is the first ESA Small Mission for Advanced Research in
Technology, aimed at the demonstration of enabling technologies for
future scientific missions. SMART-1's prime technology objective is
the demonstration of the solar primary electric propulsion, a key
for future interplanetary missions. SMART-1 will use a Stationary
Plasma Thruster engine, cruising 15 months to capture a Moon polar
orbit. A gallery of images of the spacecraft is available at the web
site: http://www.estec.esa.nl/spdwww/smart1/html/11742.html SMART-1
payload aims at monitoring the electric propulsion and its spacecraft
environment and to test novel instrument technologies. The Diagnostic
Instruments include SPEDE, a spacecraft potential plasma and charged
particles detector, to characterise both spacecraft and planetary
environment, together with EPDP, a suite of sensors monitoring
secondary thrust-ions, charging and deposition effects. Innovative
spacecraft technologies will be tested on SMART-1 : Lithium batteries
and KATE, an experimental X/Ka-band deep-space transponder, to support
radio-science, to monitor the accelerations of the electric propulsion
and to test turbo-code technique, enhancing the return of scientific
data. The scientific instruments for imaging and spectrometry are:
\begin{itemize} D-CIXS, a compact X-ray spectrometer based on novel
SCD detectors and micro-structure optics, to observe X-ray celectial
objects and to perform lunar chemistry measurements. SIR, a miniaturised
quasi-monolithic point-spectrometer, operating in the Near-IR (0.9 ÷
2.4 micron), to survey the lunar crust in previously uncovered optical
regions. AMIE, a miniature camera based on 3-D integrated electronics,
imaging the Moon, and other bodies and supporting LASER-LINK and
RSIS. RSIS and LASER-LINK are investigations performed with the SMART-1
Payload: \begin{itemize} RSIS: A radio-science Experiment to validate
in-orbit determination of the libration of the celestial target,
based on high-accuracy tracking in Ka-band and imaging of a surface
landmark LASER-LINK: a demonstration of acquisition of a deep-space
laser-link from the ESA Optical Ground Station at Tenerife, validating
also the novel sub-apertured telescope designed for the mitigation of
atmospheric scintillation disturbances.
Title: SMART-1: precursor for the exploration the Solar System with
electric propulsion (Invited).
Authors: Racca, G. D.; Foing, B. H.
Bibcode: 1999BAAS...31.1107R
Altcode:
No abstract at ADS
Title: Multisite observations of surface structures on AB Doradus
in 1994 November
Authors: Collier Cameron, A.; Walter, F. M.; Vilhu, O.; Böhm, T.;
Catala, C.; Char, S.; Clarke, F. J.; Felenbok, P.; Foing, B. H.;
Ghosh, K. K.; Hao, J.; Huang, L.; Jackson, D. A.; Janot-Pacheco, E.;
Jiang, S.; Lagrange, A. -M.; Suntzeff, N.; Zhai, D. S.
Bibcode: 1999MNRAS.308..493C
Altcode:
We present time-resolved optical spectroscopy and broad-band photometry
of the rapidly rotating southern K0 dwarf star AB Doradus, obtained
during 1994 November. The data were obtained as part of a collaboration
dedicated to MUlti-SIte COntinuous Spectroscopy (MUSICOS), and entailed
coordinated observations on three continents to obtain the fullest
phase coverage possible subject to limitations of local weather
conditions. The Doppler images from the three consecutive nights
of the run show excellent mutual agreement, with a dark polar cap
and numerous intermediate- and low-latitude features. Simultaneous
optical photometry showed numerous short-duration U-band flares,
and two longer duration optical flares with durations of the order
of hours. The latter produced broad-band continuum enhancements
throughout the optical spectrum. Where simultaneous spectroscopy
was available, both types of flare were seen to have counterparts
in Hα and the Caii H line. Simultaneous time-resolved ultraviolet
spectroscopy from the Goddard High Resolution Spectrograph (GHRS)
aboard the Hubble Space Telescope, reported elsewhere, shows that at
least one of the short-duration U-band flares was also observed in Civ
with the GHRS. Time-series Hα spectra showed significant evolution
of the circumstellar prominence system over five consecutive stellar
rotations. One prominence underwent a dramatic increase in distance
from the stellar rotation axis. We speculate that this event may have
been associated with one of the long-duration flares.
Title: SMART-1: Precursor for the Exploration the Solar System with
Electric Propulsion (Invited)
Authors: Racca, G. D.; Foing, B. H.
Bibcode: 1999DPS....31.2102R
Altcode:
Deep Space exploration was initiated by a series of fly-by missions
that were propulsively and energetically modest. Therefore, the basic
energy barrier given by the use of chemical propulsion system was
not obstructive. In addition, the use of gravity assits has enabled
deep space missions with enlarged velocity increments. Unfortunately,
multiple gravity assits have the drawback to narrow drammatically
the launch windows and the cruise phases are extremely long with
obvious impacts on the operation costs. The most promising solution
for the future deep space missions is found in the use of the Electric
Propulsion (EP). Thanks to its high specific impulse, the EP enables
very high velocity increments, higher payload ratios and the use
of smaller launchers. In addition it alows to have more flexible
launch windows and ultimately reduces the cruise time. SMART-1 is a
mission to test the system aspects of primary EP. It will be launched
as an auxiliary passanger in late 2002 by an Ariane 5 rocket into a
Geo-stationary Transfer Orbit. The planetry target orbit is around the
Moon, polar, elliptical, roughly 1000 x 10000 km with perilune near
the South Pole. The Moon will be reached after a cruise of 15 to 18
months and providing a velocity increment of about 3.5 km/s by EP. The
transfer trajectory makes use of Moon resonances and Moon swing-by's to
test these techniques for future deep space missions. The EP engine is
a stationary plasma thruster, providing a relatively high thrust of 70
mN with an input power of 1350 W and with a specific impulse of 1600
s. The scientific observations of the lunar surface will be carried
out with a novel X-ray spectrometer and a low mass, very compact
IR reflectance spectrometer, together with an imaging camera. An
X-Ka-band transponder will allow to perform spaceraft tracking with
high accuracy and, comined with the camera, to test techniques for
measuring from orbt the Moon physical librations. During the cruise
phase the natural and induced plasma environment will be measured.
Title: On the nature of the H BT I infrared emission lines of
tau Scorpii
Authors: Zaal, P. A.; de Koter, A.; Waters, L. B. F. M.; Marlborough,
J. M.; Geballe, T. R.; Oliveira, J. M.; Foing, B. H.
Bibcode: 1999A&A...349..573Z
Altcode:
We present Hα , He i lambda 2.058 mu m and 6 hydrogen Brackett and
Pfund lines of tau Sco (B0.2V) obtained using the ground-based INT and
UKIRT instruments as well as satellite data from ISO. The infrared
lines all show core emission. We have investigated the formation of
these lines using sophisticated non-LTE models. The observed emission
in the most pronounced hydrogen lines, such as Bralpha and Pfalpha , is
stronger than predicted by our models. The velocities of peak emission
are blue-shifted by 5-10 km with respect to the stellar velocity. This
together with the surprisingly strong width of Bralpha and the peculiar
profile of He i lambda 2.058 suggests that shock-induced turbulent
velocity fields may be present in or somewhat above the stellar
photosphere, as has already been suggested from analysis of optical
and ultraviolet data. We derive T_eff = 32+/-2 kK from the infrared
data alone, a value consistent with previous optical analysis. The
good agreement indicates that quantitative analysis of infrared lines
alone (e.g. for hot stars in regions of high extinction) can be used
to characterize photospheres accurately. We also investigate the mass
loss of tau Sco and find an upper-limit of 6 10(-9) M_{sunyr(-1) }. A
parameter study of the infrared hydrogen and helium lines indicates
that emission may be expected in Bralpha and Pfalpha for stars with
T_eff ga 16 kK and will dominate the profiles of these lines for T_eff
ga 31 and 26 kK, respectively. He i lambda 2.058 will be in emission
for 20 la T_eff la 33 kK and He ii line profiles will contain emission
at T_eff ga 33 kK. The effect of surface gravity on these values is
small. based on data obtained with the ESA Infrared Space Observatory
(ISO), with the UK infrared telescope (UKIRT, Hawaii) and with the
Isaac Newton Telescope (INT, La Palma)
Title: On the relation between diffuse interstellar bands and simple
molecular species
Authors: Krełowski, J.; Ehrenfreund, P.; Foing, B. H.; Snow, T. P.;
Weselak, T.; Tuairisg, S. Ó.; Galazutdinov, G. A.; Musaev, F. A.
Bibcode: 1999A&A...347..235K
Altcode:
We present observations of the major diffuse interstellar bands (DIBs)
at 5780 and 5797 Ä as well as literature data and our own observations
of the violet lines of CH and CH(+) , in the lines of sight toward some
70 stars representing various degrees of the interstellar reddening. The
correlations are shown and discussed in the context of indicators such
as far-UV extinction parameters and neutral molecular abundances. The
results show that the DIBs in question (lambda lambda 5797 and 5780)
both probably form in diffuse cloud interiors, in a related regime
where CH and H_2 form. The ratio of the two DIBs correlates with CH
abundance, confirming that the lambda 5797 carrier is favoured in
enhanced molecular gas regions over the lambda 5780 carrier. The
ratio of the two DIBs correlates poorly with CH(+) abundance. Our
compilation of observational data also suggests that the DIB ratio may
be equally useful as a cloud type indicator as is R_V, the ratio of
total to selective extinction, and much more readily observed. Based on
observations obtained at the Russian Special Astrophysical Observatory
(SAO), Terskol Observatory (TER), Canada France Hawaii Telescope (CFHT),
European Southern Observatory (ESO), Observatoire de Haute-Provence
(OHP)
Title: Distribution of gas, dust and the lambda 6613 Å DIB carrier
in the Perseus OB2 association
Authors: Sonnentrucker, P.; Foing, B. H.; Breitfellner, M.;
Ehrenfreund, P.
Bibcode: 1999A&A...346..936S
Altcode:
We present a study of the spatial distribution of the lambda 6613 Ä
DIB carrier in the Perseus OB2 association based on high resolution
observations toward lines of sight representing different interstellar
environments. We determined that in the studied region, the lambda 6613
Ä DIB carrier is concentrated in two distinct clouds with velocities
of 1.4 (+/- 0.4) and 12.0 (+/- 0.9) km s(-1) . We compared the lambda
6613 Ä DIB carrier's velocity with the Na I velocity distribution
derived from our survey measurements, as well as with CO, OH, H
I and Ca Ii measurements from the literature. We conclude that the
behaviour of the carrier of the lambda 6613 Ä DIB follows the overall
expansion motion of the gas in the association. The DIB velocity is
directly linked to that of Ca Ii and H I. The DIB total column density
is proportional to the total column density of Ca Ii and H I making
those atoms good tracers of the lambda 6613 Ä DIB carrier. Those new
results support the assumption that the lambda 6613 Ä DIB would arise
from a gas phase molecule, possibly single-ionized (Sonnentrucker et
al. 1997). We also conclude that the DIB carrier is distributed in
shell structures over the whole association. We finally show from the
DIB velocity structure that the DIB carrier, gas and dust are well
mixed toward the association but that the DIB shells have an angular
extent twice larger than that of the dust. Based on observations with
OHP 1.52m Telescope and Aurelie spectrograph.
Title: Short-term spectroscopic variability in the pre-main sequence
Herbig AE star AB Aurigae during the MUSICOS 96 campaign
Authors: Catala, C.; Donati, J. F.; Böhm, T.; Landstreet, J.;
Henrichs, H. F.; Unruh, Y.; Hao, J.; Collier Cameron, A.; Johns-Krull,
C. M.; Kaper, L.; Simon, T.; Foing, B. H.; Cao, H.; Ehrenfreund, P.;
Hatzes, A. P.; Huang, L.; de Jong, J. A.; Kennelly, E. J.; ten Kulve,
E.; Mulliss, C. L.; Neff, J. E.; Oliveira, J. M.; Schrijvers, C.;
Stempels, H. C.; Telting, J. H.; Walton, N.; Yang, D.
Bibcode: 1999A&A...345..884C
Altcode:
We present results of the spectroscopic monitoring of AB Aur obtained
during the MUSICOS 96 campaign. The analysis is mainly focussed on the
He I D3 line, on the Hα line, and on a set of photospheric lines. The
star was monitored irregularly for more than 200 hours. We confirm
the high level of variability of spectral lines in AB Aur. We find
that the photospheric lines have a profile differing significantly
from a classical rotational profile. The dominant features of this
abnormal photospheric profile are a blue component, in absorption, whose
velocity is modulated with a 34hr period, and a red component, stable
in velocity but of variable intensity, with a possible periodicity
near 43 hrs. The He I D3 line exhibits two well-defined components:
a blue component, always in emission with a velocity modulated with a
45hr period, and a red component of variable intensity, alternatively
in emission and in absorption, occurring at a fixed velocity, with a
variable intensity possibly modulated with a 45 hr period. The Hα line,
showing a P Cygni profile, also exhibits pseudo-periodic variations
of its blue absorption component, but its variability appears more
complicated than that of the other lines studied here. We suggest
that the blue component of the photospheric lines is modulated by the
star's rotation, with a period of 34 hrs, due to a highly inhomogeneous
photosphere, involving significant radial flows. Our model also involves
downflows onto the stellar pole to account for the red components of the
photospheric lines and of the He I D3 line. We propose two different
interpretations of the behavior of the blue component of the He I D3
line. In the first one, this component is formed in a wind originating
from the star's equatorial regions. In this interpretation, the rotation
period of the equatorial regions of the star is 45 hrs, implying a 25%
surface differential rotation, with the pole rotating faster than the
equator. The second interpretation involves a wind originating from
a region of a circumstellar disk, at a distance of 1.6 stellar radii
from the star's center, with a rotation period of 45 hrs. We are not
able to decide which one of these two interpretations is more likely,
on the basis of the data presented here. Based on observations obtained
during the MUSICOS 96 MUlti-SIte COntinuous Spectroscopic campaign,
collected at the Canada-France Hawaii, the McDonald 2.1m, the La
Palma 2.5m Isaak Newton, the Observatoire de Haute-Provence 1.93m,
the Xinglong 2.16m, and the Ritter Observatory 1m telescopes
Title: ESA SMART-1 Mission to the Moon
Authors: Foing, B. H.; Racca, G.; SMART-1 Team
Bibcode: 1999LPI....30.2052F
Altcode:
SMART-1 is to be launched in 20001 as the first Small Mission for
Advanced Research in Technology of the ESA Scientific Programme. It
will use Primary Solar Electrical Propulsion in Deep Space and test
new technologies for future missions.
Title: Circumstellar emission and flares on FK Comae
Berenices. Analysis and modelling of Balmer and He I D3 line
variations
Authors: Oliveira, J. M.; Foing, B. H.
Bibcode: 1999A&A...343..213O
Altcode: 1999astro.ph..2010O
We present results on spectroscopic observations of the fast-rotating
active giant FK Comae, obtained mainly with the
ESA-MUSICOS spectrograph at the Isaac Newton Telescope (INT) in 1996
and 1997 and also with the Aurélie spectrograph at the Observatoire de
Haute Provence (OHP) in 1997. The profiles analysed are those of the
Balmer, Hα \ and Hβ , and He I D3 (lambda 5876 Angstroms) lines. We
analyse the Balmer line variability and phase behaviour. We confirm
these lines as highly variable, with excess emission that originates
from extended structures and exhibits clear signs of rotational
modulation. We have described the line profiles for two distinct
states of activity, using different modelling approaches. Similar
techniques were applied to the He I D3 spectra. A large flare event
lasting several days was detected in both Balmer lines and in the
He I D3 line. The energy released during this flare in Hα \ is of
the order of 10(37) erg, making it the largest Hα \ flare reported
on a cool star. Our results confirm the extreme complexity of the
circumstellar environment of FK Comae. The activity level of this
star is quite variable demanding different approaches to the line
profile analysis. Based on observations obtained at the Isaac Newton
Telescope with the ESA-MUSICOS spectrograph and at the Observatoire
de Haute Provence with the Aurélie spectrograph.
Title: New Views of Lunar Terranes with SMART-1 Expected Data
Authors: Foing, B. H.; Hoffmann, H.; Grande, M.; Josset, J. L.;
Cerroni, P.; Keller, U.; SMART-1 Team
Bibcode: 1999LPI....30.2057F
Altcode:
Experiments on the ESA SMART-1 mission will provide new global and
local data sets helpful to discriminate and characterize different lunar
"terranes" multicolor imaging at medium and high resolution.
Title: ILEWG Recommendations for Lunar Exploration
Authors: Foing, B. H.; Duke, M.; Galimov, E.; Mizutani, H.; ILEWG Team
Bibcode: 1999LPI....30.2060F
Altcode:
The International Lunar Exploration Working Group (ILEWG) was created
in 1995 with the charter: 1. To develop an international strategy for
the exploration of the Moon; 2. To establish a forum and mechanism for
the communication and coordination of activities; and 3. To implement
international coordination and cooperation.
Title: Doppler Imaging of Stellar Oscillations: Multi-Site
Observations of Epsilon Cephei
Authors: Kennelly, E. J.; Brown, T. M.; Ehrenfreund, P.; Foing,
B.; Hao, J.; Horner, S.; Korzennik, S.; Nisenson, P.; Noyes, R.;
Sonnentrucker, P.
Bibcode: 1999ASPC..185..264K
Altcode: 1999IAUCo.170..264K; 1999psrv.conf..264K
We investigate the oscillation properties of ɛ Cep using a series of
specialized techniques designed to extract and analyze time variations
in absorption line profiles. To obtain the necessary temporal coverage
for this investigation, multi-site observations were collected at
3 sites (China, France, Arizona) all equipped with high-resolution
echelle spectrographs. From these observations, we find evidence for
a very rich spectrum of modes in ɛ Cep.
Title: Observational constraints on the carriers of the Diffuse
Interstellar Bands (DIBs)
Authors: Cami, J.; Ehrenfreund, P.; Foing, B. H.
Bibcode: 1999ASIC..523..167C
Altcode: 1999fess.conf..167C
No abstract at ADS
Title: The Moon and Mars : proceedings of the B0.3 and B0.4
symposia of COSPAR Scientific Commission B which was held during
the Thirty-second COSPAR scientific assembly, Nagoya, Japan, 12-19
July, 1998
Authors: Ip, W. -H.; Foing, B. H.; Masson, Ph.
Bibcode: 1999AdSpR..23.....I
Altcode:
No abstract at ADS
Title: The ESA SMART-1 Mission to the Moon with Solar Electric
Propulsion
Authors: Foing, B. H.; Racca, G. R.
Bibcode: 1999AdSpR..23.1865F
Altcode:
SMART-1 is planned to be the first Small Mission for Advanced Research
in Technology of the ESA Scientific Programme Horizons 2000 for a
launch at the end of 2001. The mission is dedicated to the testing of
new technologies for preparing future cornerstone missions, using Solar
Electrical Propulsion in Deep Space. The mission operational lifetime
includes a 6-17 months cruise until a lunar orbit (300-10000 km) with
6 month operations. The SMART-1 spacecraft will be launched either on
Ariane 5 as auxiliary passenger or on Eurockot. The expected launch mass
is 350 kg. This allows to bring a dedicated payload with spacecraft,
instrument and electric propulsion diagnostics technologies, as well
as giving an opportunity for new lunar geophysical and geochemical
studies, and for cruise science on the way to the Moon.
Title: Circumstellar Activity and Flares in FK Comae: New Results
from the ESA MUSICOS Spectrograph on the INT
Authors: Oliveira, J. M.; Foing, B. H.
Bibcode: 1999ASPC..158..230O
Altcode: 1999ssa..conf..230O
No abstract at ADS
Title: New Estimates of Ionization Potentials of Four DIB Molecular
Carriers
Authors: Sonnentrucker, P.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 1999AdSpR..24..519S
Altcode:
We present a study of the behaviour and ionization properties of four
Diffuse Interstellar Bands (DIBs) at λλ5780, 5797, 6379 and 6613
Å. In the λλ5797, 6379 and 6613 Å DIBs, substructures have recently
been detected, indicating large gaseous molecular carriers. Studying
DIBs in regions with different physical properties in terms of UV
flux and density enables us to monitor the behaviour of the carriers
and hence to constrain their nature. As a follow-up of Sonnentrucker
et al. (1997), we add new lines of sight and generalize the results
for lines of sight with 2 or 3 clouds. This refines the Ionization
Potential estimates which are between 10 and 13 eV, hence reminiscent
of PAH or fullerence cations for those DIBs
Title: Femme: a precursor ecosystem on the moon
Authors: Paille, Ch.; Curwy, R.; Filali, R.; Lehman, B.; Dubertret,
G.; Foing, B.; Lasseur, Ch.
Bibcode: 1999AdSpR..23.1857P
Altcode:
An efficient regenerative life Support system for manned base cannot
be conceived without biological processes. Therefore since the 1960's,
numerous projects have been initiated to close, as far as possible,
the biological loop. Based on the selected concepts (i.e. carbon and/or
nitrogen cycles, microbial organisms and/or higher plants) mathematical
models have been studied and built. Unfortunately, to our knowledge
these robust models do not take into account the effects of the space
environment (i.e. reduced gravity, radiation,...). In the past, a
large number of scientific studies has been performed to understand
these effects but only a few of them have tried to quantify them. In
this paper we present a very simplified concept of an ecosystem. Its
objectives, which are compatible with a non-pressurised mission, are
on one hand to quantify microbial kinetics and on the other hand to
demonstrate the validity of several technologies and technical concepts.
Title: Preface
Authors: Fröhlich, Claus; Foing, Bernard
Bibcode: 1999AdSpR..24..135F
Altcode:
No abstract at ADS
Title: Evidence for Large Organic Molecules in the Diffuse Medium
Using Optical High Resolution Spectroscopy
Authors: Sonnentrucker, P.; Foing, B. H.; Ehrenfreund, P.
Bibcode: 1999AdSpR..24..449S
Altcode:
The Diffuse Interstellar Bands (DIBs) are absorption lines observed in
the line of sight toward reddened OB stars. Their ubiquitous detection
in space indicates chemically stable and abundant carriers. High
resolution spectroscopy led to the detection of substructures in
the line profiles of a few DIBs, indicating a gas phase molecular
origin of the carriers. Line profile studies are useful tools to
derive information on the band carriers nature. In this paper we
compared the velocity structure of the λ6613 Å DIB line profile to
the NaD1 and CaII profiles toward 6 targets of the Perseus
OB2 association
Title: Stellar seismology and variability with the COROT mission
Authors: Baglin, Annie; Foing, Bernard H.
Bibcode: 1999AdSpR..24..245B
Altcode:
The main scientific objectives for asteroseismology and the
observational strategy for the COROT photometric mission are
presented. Some indications are given on its complementary objective,
the search for extraterretrial planets, and its interest in terms of
stellar variability. COROT development in the framework of the French''
petites missions'' using the Proteus platform is described.
Title: Asteroseismology from MUSICOS multi-site campaigns
Authors: Foing, B. H.; Catala, C.; Oliveira, J. M.; Hubert, A. M.;
Floquet, M.; Hao, J. X.; Kennelly, T.; Balona, L.; Henrichs, H.;
de Jong, J.
Bibcode: 1999AdSpR..24..251F
Altcode:
For the MUSICOS international project (MUlti-SIte COntinuous
Spectroscopy), the instrument concept and multi-site operational
constraints for microvariability and asteroseismology are
discussed. Operations and results from previous MUSICOS
international campaigns in 1989, 1992, 1994, 1996 involving Pic
du Midi, Haute-Provence, South Africa, La Palma, Kitt Peak, ESO La
Silla, Hawaii, Anglo-Australian, Xinglong and other observatories are
presented. Some MUSICOS asteroseismology highlights on micro-variability
and non-radial pulsations on Be, δ Scuti, O and B, γ Dor variables are
reviewed. Perspectives for solar-type asteroseismology with multi-site
networks in support to space asteroseismology missions such as COROT,
are discussed.
Title: The Euromoon Mission: Science Exploration Goals and Model
Payload
Authors: Foing, B. H.; Euromoon Team
Bibcode: 1998LPI....29.1966F
Altcode:
No abstract at ADS
Title: Possible Mobile Surface Payload for the Euromoon Mission
Authors: Kminek, G.; Foing, B. H.; Euromoon Team
Bibcode: 1998LPI....29.1834K
Altcode:
No abstract at ADS
Title: Polar plumes and streamers from 1994 and 1998 eclipses
Authors: Foing, B. H.; Duvet, L.; Muglach, K.; Wiik, J. E.; Beaufort,
T.; Maurice, E.
Bibcode: 1998ESASP.421..273F
Altcode: 1998sjcp.conf..273F
No abstract at ADS
Title: Solar Prominence Diagnostics from November 3, 1994 Eclipse
Authors: Foing, B. H.; Wiik, J. E.; Duvet, L.; Henrich, N.; Cravatte,
S.; David, F.; Altieri, B.; Beaufort, T.; Ligot, L.; Maurice, E.
Bibcode: 1998ASPC..150..201F
Altcode: 1998IAUCo.167..201F; 1998npsp.conf..201F
No abstract at ADS
Title: MUSICOS Observations of SU AUR
Authors: Unruh, Yvonne C.; Donati, J. -F.; Balona, L.; Bohm, T.;
Cao, H.; Catala, C.; Collier Cameron, A.; Ehrenfreund, P.; Foing,
B.; Granzer, T.; Hao, J.; Hatzes, A.; Henrichs, H.; Johns-Krull,
C.; de Jong, J.; Kennelly, T.; Landstreet, J.; Morrison, N.; Mullis,
C.; Neff, J.; Oliveira, J.; Schrijvers, C.; Simon, T.; Stempels, E.;
Strassmeier, K. G.; Telting, J.; Walton, N.
Bibcode: 1998ASPC..154.2064U
Altcode: 1998csss...10.2064U
We present first results of the high-resolution observations of SU Aur
obtained through the MUSICOS network in 1996 Nov. The data set is unique
in that it gives us complete phase coverage for almost two rotation
periods of SU Aur. This is particularly valuable for T Tauri stars as
they can vary dramatically on the time scale of one rotation period.
Title: Flares and Circumstellar Material around the Fast-Rotating
Giant FK Comae
Authors: Oliveira, J. M.; Foing, B. H.; Sonnentrucker, P.; et al.
Bibcode: 1998cvsw.conf..373O
Altcode:
No abstract at ADS
Title: SMART - 1, A Precursor to Future Deep Space and Solar /
Heliospheric Missions
Authors: Foing, B.; Racca, G.; SMART-1 Team
Bibcode: 1998ESASP.417..341F
Altcode: 1998cesh.conf..341F
No abstract at ADS
Title: Balmer Line Profiles Variations in SU Aurigae from the MUSICOS
96 Multi-site Campaign
Authors: Oliveira, J. M.; Unruh, Y. C.; Foing, B. H.; MUSICOS 96
Collaboration
Bibcode: 1998Ap&SS.261..143O
Altcode: 1999Ap&SS.261..143O
No abstract at ADS
Title: Prominences and Circumstellar Emission Around FK Comae
Berenices: Balmer Line Diagnostics from MUSICOS Spectra
Authors: Oliveira, J. M.; Foing, B. H.; Gondoin, Ph.; Stempels, H. C.;
Beaufort, T.; Le Poole, R. S.; de Jong, J. A.
Bibcode: 1998ASPC..150..243O
Altcode: 1998npsp.conf..243O; 1998IAUCo.167..243O
No abstract at ADS
Title: Circumstellar Variations and Microflaring in FK Comae
Berenices: Time-Resolved Balmer Line Spectroscopy
Authors: Oliveira, J. M.; Foing, B. H.; Gondoin, Ph.; Stempels, H. C.;
Sonnentrucker, P.; Le Poole, R. S.; Ehrenfreund, P.; de Jong, J. A.;
Schrijvers, C.; Henrichs, H.; ESA-MUSICOS Collaboration
Bibcode: 1998ASPC..154.1524O
Altcode: 1998csss...10.1524O
We present results from the analysis of spectra of the fast rotating
giant FK Comae Berenices, obtained with the recently commissioned
ESA-MUSICOS spectrograph at the INT and with the Aurelie spectrograph
at the OHP. The Balmer lines broad emission is modelled as arising
from structures extending up to 4 stellar radii. The absorption
is modelled due to the presence of a shell of cold and dense gas
(solar-like filaments), near the corotation radius, covering about 20%
of the stellar disc. The extended emission is believed to arise in giant
structures reminiscent of active loops or prominences. Time resolved Hα
emission spectroscopy indicates that these structures undergo continuous
microflaring. Based on data sets from May and November 1996 and May
and June 1997, we describe different time scales for variability, from
yearly rise of activity to hourly microflares. Based on observations
with the ESA-MUSICOS spectrograph at the 2.5 m Isaac Newton Telescope,
ING Observatory, Spain and with the Aurelie spectrograph at the 1.52
m Coude Telescope, Observatoire de Haute-Provence, France
Title: 3D active regions in the solar-type giant FK Comae.
Authors: Oliveira, J. M.; Foing, B. H.; Sonnentrucker, P.; Ehrenfreund,
P.; Schrijvers, C.; Henrichs, H.
Bibcode: 1998joso.proc..170O
Altcode:
FK Com is a solar-type fast rotating giant star. The authors present
results based on several data sets obtained with the ESA-MUSICOS
spectrograph (at INT) and with Aurelie spectrograph (at OHP) in
1997. Their observations of the Hα Balmer line allow to start to
understand the 3D structure, variability and evolution of the active
regions that produce this spectral signature. The very broad emission
is interpreted as extended active loops or prominences up to 3 stellar
radii. The authors were able to analyse the contribution of phenomena
with very different timescales, from flare to micro-flaring. These
bursts of emission occur at all times in different active loops,
due to loop excitation/recombination in the stressed magnetic field.
Title: The ESA SMART-1 Mission. From laboratory to Deep Space with
Electric Propulsion
Authors: Foing, B.; SMART-1 Team
Bibcode: 1998ASSL..236..529F
Altcode: 1998lasr.conf..529F
No abstract at ADS
Title: Asteroseismology Results from the MUSICOS Network
Authors: Foing, B. H.; Catala, C.; Hubert, A. M.; Hao, J. X.; Kennelly,
E. J.; Balona, L.; Henrichs, H.; MUSICOS Team
Bibcode: 1998psrd.conf...75F
Altcode:
No abstract at ADS
Title: Results from the 3 November 1994 Solar Eclipse: Density and
Temperature Variations in Streamers and Coronal Holes
Authors: Foing, B. H.; Duvet, L.; Ligot, L.; Oliveira, J.; Beaufort,
T.; Wiik, J. E.; Altieri, B.; Henrich, N.; Cravatte, S.; Maurice, E.
Bibcode: 1998ASPC..154.1035F
Altcode: 1998csss...10.1035F
We report results from our observations of the 3 November 1994 total
solar eclipse from the North Chile altiplano. From the military base of
Putre, we used our transportable CCD camera and telescope, as well as
support photographic digitised observations from Putre and Parinacota
volcano. We obtained images from the inner to the outer corona, as well
as low-resolution spectra of prominences and of the inner corona. We
present the analysis of images and spectra of prominences in the
Balmer, He 1 and Ca 2 lines, and in the Thomson scattered continuum. The
variation of density and equivalent temperature was derived in coronal
holes (plumes and interplumes) and in equatorial streamers.
Title: Science Exploration of the Moon with the European Space Agency
SMART-1 Mission
Authors: Foing, B. H.; Racca, G.
Bibcode: 1998LPICo.957....7F
Altcode:
SMART-1, with a planned launch date of 2001, will be the first Small
Mission for Advanced Research in Technology of the ESA Scientific
Programme Horizons 2000. The mission is dedicated to the testing of
new technologies for preparing future cornerstone missions, using
solar electrical propulsion in deep space. The mission operational
lifetime contains periods for cruise phase and an orbital phase
around the Moon. The SMART-1 spacecraft launch mass is 350 kg. Two
solar-electric propulsion systems are being considered: (1) stationary
plasma thrusters (e.g., PPS-1350), which provide high thrust (70 mN)
and medium specific impulse (1600 s), and (2) ion thrusters (e.g.,
PIT-10, UK-10), which provide low thrust (20 mN) and high specific
impulse (3000 s). The SMART-1 mission will be placed in orbit around
the Moon using solar-electric propulsion. The total mass of the payload
will be between 10 and 25 kg, depending on the choice of thruster and
the exact mission scenario. Observations can also be carried out during
the cruise phase of the mission. We summarize here some science goals
(and the type of instruments which could address them) on SMART-1
Title: The diffuse interstellar bands at 5797, 6379 and 6613
Angstroms. Ionization properties of the carriers
Authors: Sonnentrucker, P.; Cami, J.; Ehrenfreund, P.; Foing, B. H.
Bibcode: 1997A&A...327.1215S
Altcode:
We present a study of the behaviour and ionization properties of
three narrow Diffuse Interstellar Bands (DIBs) at lambda lambda 5797,
6379 and 6613 Angstroms. In all three DIBs substructures have recently
been detected, indicating large gaseous molecular carriers. Studying
DIBs in regions with drastically different physical properties in
terms of UV flux and density enables us to monitor the behaviour of
the carriers and hence to constrain their nature. We observed these
three DIBs along 40 different lines-of-sight (35 program stars and
5 standard stars) consisting of HII regions, dark clouds, molecular
clouds and reflection nebulae. The DIB variations at low reddening are
explained by a new model of photoionization equilibrium of the DIB
carriers. This model takes into account the penetration depth of UV
ionizing photons throughout the cloud. The slope of the variation of
DIB strength as a function of reddening thus allows us to estimate the
effective ionization potentials of the carriers. Following this new
analysis, the carriers of the lambda 5797 and lambda 6613 Angstroms
DIBs would have ionization potentials above 10eV, reminiscent of large
PAHs or fullerenes which have a single positive charge. The estimated
ionization potential (7--9eV) of the lambda 6379 Angstroms DIB seems
to indicate a large neutral carrier. Based on observations with OHP
1.93m Telescope and Elalie spectrograph.
Title: Diffuse Interstellar Bands in single clouds: new families
and constraints on the carriers.
Authors: Cami, J.; Sonnentrucker, P.; Ehrenfreund, P.; Foing, B. H.
Bibcode: 1997A&A...326..822C
Altcode:
We present a survey of diffuse interstellar bands (DIBs) in single
clouds. High resolution and high S/N observations of DIBs towards
lines of sight representing very different environments allow to
investigate mutual correlations in a large consistent sample of
DIBs. The classification of DIBs into families is reviewed and
refined according to these results. We find that the selected 44
DIBs are due to different carriers. Two isolated families of DIBs
(λ5797 et al., λ4501 et al.) are found, which are mutually slightly
anticorrelated. The behaviour of DIBs with respect to the local UV
field is investigated using hydrogen column densities to estimate the
strength of the UV field, resulting in the hypothesis that most of the
DIB carriers are molecules sensitive to photo-ionization. With this
interpretation, the apparent division of interstellar clouds into ζ,
σ and Orion types can be understood as a sequence in strength of the
UV field. Differences in strength of the UV field between different
lines-of-sight are due to the so-called ``skin-effect'', the effective
shielding of UV radiation by the outer layers of interstellar clouds.
Title: Multi-site continuous spectroscopy. V. Rapid photospheric
variability in the Be star 48Persei from the MUSICOS 1989 campaign.
Authors: Hubert, A. M.; Floquet, M.; Hao, J. X.; Caillet, S.; Catala,
C.; Foing, B. H.; Neff, J. E.; Huang, L.; Hubert, H.; Barban, C.;
Baudrand, J.; Cao, H.; Char, S.; Chatzichristou, H.; Cuby, J. G.;
Czarny, J.; Dreux, M.; Felenbok, P.; Guerin, J.; Hron, J.; Huovelin,
J.; Jankov, S.; Jiang, S.; Le Contel, J. M.; Maitzen, H. M.; Petrov,
P.; Savanov, I.; Shcherbakov, A.; Simon, T.; Stee, P.; Tuominen, I.;
Zhai, D.
Bibcode: 1997A&A...324..929H
Altcode:
Rapid variability in the photospheric HeI 6678 line of the Be star 48Per
(HD 25940, HR 1273) has been detected from 258 high S/N CCD spectra
taken with four 1.5-2.0 meter telescopes over three consecutive nights
during the multi-site spectroscopic MUSICOS 1989 campaign. 48Per is a
rather moderate-Vsin(i) star, known to have presented slight long-term
variations in the intensity of Balmer emission lines and in the V/R
ratio. It is shown that the MUSICOS 1989 observations preceded a new
activity phase. Search for line-profile variations, hereafter lpv, was
performed with time-series analysis using two methods (TF+CLEAN and
Least-Squares) and with analysis of residuals. Weak blue-to-red and
red-to-blue moving subfeatures with the same acceleration have been
detected in the residuals. Their presence confirms that this star is
seen under a moderate angle of inclination, i~40^o^, in agreement with
estimates based on fundamental stellar parameters. A 6.04c/d frequency,
associated with the moving subfeatures mentioned above, has been firmly
established from time-series analysis and corresponds more closely,
in the frame of non-radial pulsations (NRP), to a tesseral mode
(|m|=l-1=9+/-2). Two other possible frequencies (0.85 and 2.77c/d)
have been detected but need to be confirmed with new observations
obtained over a longer time span. Despite additional spectra obtained
at Haute Provence Observatory, we could not confirm the previous value
of the orbital period or the amplitude of the radial velocity curve
of 48Per, and therefore it was premature to search for tidally-forced
oscillations.
Title: On the evolutionary status of the AB DOR + RST 137B system
Authors: Collier Cameron, A.; Foing, B. H.
Bibcode: 1997Obs...117..218C
Altcode:
No abstract at ADS
Title: Fullerenes in space
Authors: Ehrenfreund, P.; Foing, B. H.
Bibcode: 1997AdSpR..19.1033E
Altcode:
The discovery and synthesis of fullerenes led to the hypothesis that
they may be present and stable in interstellar space. Fullerenes have
been reported in an impact crater on the LDEF spacecraft. Investigations
of fullerenes in carbonaceous meteorites have yielded only small
upper limits. Fullerene compounds and their ions could be interesting
carrier molecules for some of the ``diffuse interstellar bands''
(DIBs), a long standing mystery in astronomy. We have detected two
new diffuse bands that are consistent with laboratory measurements of
the C_60^+, as first evidence for the largest molecule ever detected
in space. Criteria for this identification are discussed. The inferred
abundance (up to 0.9 % of cosmic carbon locked in C_60^+) suggests that
fullerenes may play an important role in interstellar chemistry. We
present new observations on DIB substructures consistent with fullerene
compounds, and the search for neutral C_60 in the diffuse medium.
Title: Diffuse Interstellar Bands towards BD+63 1964. A new reference
target.
Authors: Ehrenfreund, P.; Cami, J.; Dartois, E.; Foing, B. H.
Bibcode: 1997A&A...318L..28E
Altcode:
We report the discovery of a remarkable target concerning the Diffuse
Interstellar Bands (DIBs), namely BD+63 1964. The unusual high DIB
strengths in this object allow to confirm DIBs that were so far
denoted only as "probable", because of their intrinsic weakness in
most lines-of-sight. Due to specific line-of-sight conditions, the
high reddening and the early spectral type of the star, this object
is proposed as a new reference star for DIB measurements. We compared
the spectrum of BD+63 1964 to the spectrum of the well studied star
HD 183143. Line-of-sight parameters such a far UV extinction and Ca
I abundance indicate a denser environment towards BD+63 1964, which
can shield molecules efficiently from far W radiation above 6eV. The
relative enhancement of narrow DIBs in BD+63 1964 versus HD 183143 is
then discussed in the context of neutral fullerene compounds or large
PAHs. The relative weakening of broad DIBs indicate carriers with higher
photo-ionization potential and different recombination properties.
Title: New evidences for interstellar C_60_^+^.
Authors: Foing, B. H.; Ehrenfreund, P.
Bibcode: 1997A&A...317L..59F
Altcode:
The discovery and synthesis of fullerenes led to the hypothesis
that they may be present and stable in interstellar space. As first
evidence for the largest molecule ever detected in space, we have
recently detected two new diffuse interstellar bands (DIBs) in the
near-infrared that are consistent with laboratory measurements of
the C_60_ cation. The inferred abundance (up to 0.9% of cosmic carbon
locked in C_60_^+^) suggested that fullerenes may play an important
role in interstellar chemistry. We present new observations towards
HD 183143, HD 37022 and HD 80077 at 9600A from CFHT and ESO. The high
quality of the spectra confirms without doubt the presence of the two
DIBs at 9577 and 9632A and allows to measure reliably their strength,
width and band ratio. The two correlated DIBs decrease in a UV shielded
cold cloud (HD 80077) but increase in a region dominated by extreme UV
radiation (HD 37022), with a band ratio constant within errors. Both
DIBs show the same width, also consistent with a common carrier. This
width of 3cm^-1^ is compatible with rotational contours of C_60_
fullerene molecules. These results bring new evidences for C_60_^+^
in addition to the match with laboratory spectra.
Title: Effect of surface structures on integrated helioseismology
measurements
Authors: Foing, Bernard H.
Bibcode: 1997IAUJD..19E..19F
Altcode:
The presence of non-axisymmetric large scale structures on the solar
surface induces a rotational modulation of photometric and spectroscopic
measurements. This has a specific signature at selected harmonics
of the rotation frequency. We calculate the corresponding effect
in seismology measurements, in particular in the range where the g
modes are being searched. We compare this effect to data from SOHO
helioseismology instruments. Also due to the acoustic oscillation
inhibition in magnetic regions, each genuine oscillatory peak is
convolved with a side-lobe function due to the first 3 harmonics
of the rotation frequency, which affects the observed broadening,
splitting and line shapes of low-frequency p-modes.
Title: Asteroseismology Results from the MUSICOS Network
Authors: Foing, B. H.; Catala, C.; Hubert, A. M.; Hao, J. X.; Kennelly,
E. J.; Balona, L.; Henrichs, H.; MUSICOS Team
Bibcode: 1997IAUJD..24E...3F
Altcode:
MUSICOS is a project for a multisite network of high resolution
spectrometers around the world for MUlti SIte COntinuous Spectroscopy. A
major scientific goal of MUSICOS is to measure stellar non radial
pulsations, on OB, Be, delta Scuti, fast rotating stars, and ultimately
solar type star s.We highlight asteroseismology results from the MUSICOS
network obtained during different worlwide campaigns. In 1989, a record
spectroscopic monitoring (3 days, 258 spectra) of the Be star 48 Per
allowed the detection of NRP modes. In the 1992 campaign on the delta
Scuti type theta^2 Tauri, we measured the oscillation frequencies of
low degree (0-3) from velocity variations. Higher degree modes (3-10)
were measured from line-profile variations, using a two-dimensional
Fourier analysis resolving frequencies and azimuthal order. In the 1994
campaign, non radial pulsations were confirmed and sectorial retrogrades
modes were identified on the F-star variable gamma Doradus. The next
large MUSICOS campaign in November 1996 included NRP studies in delta
Scuti and hotter stars.
Title: Precursor Missions to Future Lunar Exploration
Authors: Foing, Bernard H.
Bibcode: 1997IAUJD..22E...9F
Altcode:
We shall summarize the highlights from two COSPAR symposia on "
Astronomy and Space Science from the Moon" and "Precursor Missions
to the Moon" published in Adv. Space Research Vol.14 No6 (1994) and
Vol. 18 No11 (1996). We shall focus on precursor science or technology
demonstration missions to future lunar exploration. In this context,
current studies and activities at ESA for lunar orbiters and landers
will be described.
Title: Azimuthal structures in the wind and chromosphere of the
Herbig AE star AB Aurigae. Results from the MUSICOS 1992 campaign.
Authors: Boehm, T.; Catala, C.; Donati, J. -F.; Welty, A.; Baudrand,
J.; Butler, C. J.; Carter, B.; Collier-Cameron, A.; Czarny, J.; Foing,
B.; Ghosh, K.; Hao, J.; Houdebine, E.; Huang, L.; Jiang, S.; Neff,
J. E.; Rees, D.; Semel, M.; Simon, T.; Talavera, A.; Zhai, D.; Zhao, F.
Bibcode: 1996A&AS..120..431B
Altcode:
The observations of the MUSICOS 1992 campaign concerned three scientific
programs, among which was the study of azimuthal structures in the wind
and chromosphere of the pre-main sequence Herbig Ae star AB Aur. The He
I 5876A line of AB Aur, which is formed in the expanding chromosphere
of this star, most probably in the innermost parts of its wind, was
continuously monitored at a spectral resolution of 30000 for about 4
days. The line was discovered to be variable in a spectacular way, the
profile changing from pure emission to a composite profile including a
deep absorption component in the course of a few hours. In this paper we
present strong clues that suggest a rotational modulation of the line,
with a period corresponding to the stars rotation period of 32hrs. We
confirmed the covariation of several non-photospheric spectral lines,
formed at very different radial distances of the star, which strengthens
the idea that the variability is the signature of azimuthal structures
in the wind of AB Aur, most probably due to magnetically confined
streams or loops emanating from the stellar surface. We present the
data collected during the MUSICOS 1992 campaign, but also a data set of
the He I D3 line obtained with FOE at KPNO during the years 1991-1994
and a series of IUE spectra containing the Mg II h & k UV lines
obtained one month prior to the campaign. A thorough discussion of
the possible interpretations of the spectacular variations of the He
I 5876A line is presented.
Title: The oscillation modes of θ^2^ Tauri. Results from the 1992
MUSICOS campaign.
Authors: Kennelly, E. J.; Walker, G. A. H.; Catala, C.; Foing, B. H.;
Huang, L.; Jiang, S.; Hao, J.; Zhai, D.; Zhao, F.; Neff, J. E.;
Houdebine, E. R.; Ghosh, K. K.; Charbonneau, P.
Bibcode: 1996A&A...313..571K
Altcode:
We have analyzed a series of 619 spectra of θ^2^ Tauri taken with
four telescopes over four consecutive nights during the 1992 global
MUSICOS campaign. Radial velocity variations provide information
about the oscillation frequencies of low degree (0<=l<=3),
and line-profile variations provide information on modes of higher
degree (3<=l<=10). The radial velocities were derived with
a cross-correlation technique. In addition to detecting several
frequencies found photometrically (e.g., Breger et al. 1989), we have
found two new frequencies, which implies that the oscillation spectrum
of θ^2^ Tau may not be stable. Variations within rotationally broadened
absorption lines were transformed by a Fourier-Doppler imaging analysis
into a map of apparent frequency versus apparent azimuthal order. From
this two-dimensional Fourier representation we identify some seven
oscillation modes using a genetic algorithm to explore parameter
space. While we find good agreement between the detected frequencies
and those predicted to be unstable based on the models of Dziembowski
(1990), it is still not clear why only certain modes are selected.
Title: Line profile variations in γ Doradus.
Authors: Balona, L. A.; Böhm, T.; Foing, B. H.; Ghosh, K. K.;
Janot-Pacheco, E.; Krisciunas, K.; Lagrange, A. -M.; Lawson, W. A.;
James, S. D.; Baudrand, J.; Catala, C.; Dreux, M.; Felenbok, P.;
Hearnshaw, J. B.
Bibcode: 1996MNRAS.281.1315B
Altcode: 1996astro.ph..3041B
The authors present data from high-dispersion échelle spectra and
simultaneous uvby photometry for γ Doradus. These data were obtained
from several sites during 1994 November as part of the MUSICOS-94
campaign. The star has two closely spaced periods of about 0.75 d
and is the brightest member of a new class of variable early F-type
stars. A previously suspected third period, very close to the other
two, is confirmed. Previous observations indicated that sudden changes
could be expected in the spectrum, but none was found during the
campaign. The radial velocities rule out the possibility of a close
companion. The phasing between the radial velocity and light curve
of the strongest periodic component rules out the starspot model. The
only viable mechanism for understanding the variability is non-radial
pulsation. The authors used the method of moments to identify the
modes of pulsation of the three periodic components. These appear to be
sectorial retrograde modes with spherical harmonic degrees, (l,m), as
follows: f1= (3,3), f2= (1,1) and f4=
(1,1). The angle of inclination of the star is found to be i ≅ 70°.
Title: Smallsat version of the European Moon Orbiting Observatory
(MORO)
Authors: Racca, G. D.; Foing, B. H.; Farrow, J. B.; Chaloner, C. P.
Bibcode: 1996AcAau..39..121R
Altcode:
As the third medium-class mission in the ESA's Horison 2000 science
programme, a Moon Orbiting Observatory (MORO) was proposed for global
mapping of lunar topography, mineralogy, geochemistry and gravity. The
growing need to reduce the cost of the space missions led the study
team to look for several approaches to limit the costs. It was decided
therefore to study in parallel to the baseline a smallsat version of
MORO which would just address the most important scientific issues
in complement to Clementine, Lunar Prospector and Lunar A, notably
gravimetry and high accuracy stereo imaging, topography, mineralogy
and some elemental composition detection capability. This resulted
in halving the payload mass (4∼2 kg) and reducing substantially
the spacecraft dry mass (≤300 kg). Such a small satellite can be
placed into a lunar transfer orbit directly by a number of emerging
new small-medium class launchers. The paper presents the mission and
spacecraft design and describes the areas where the smallsat approach
has allowed the largest cost reductions.
Title: MORO - Moon Orbiting Observatory. Phase A study report.
Authors: Coradini, A.; Foing, B.; Harrison, M.; Hoffmann, H.; Janle,
P.; Langevin, Y.; Milani, A.; Neukum, G.; Picardi, G.; Racca, G.;
Raitala, J.; D'Uston, C.; Waltham, N.; Wänke, H.
Bibcode: 1996moro.book.....C
Altcode:
The main scientific goals of MORO are: to constrain theories of the
Earth-Moon system formation; to study the Moon's origin, its thermal
evolution and geological history; to measure quantitatively on the
lunar surface, processes (impact craters, volcanic activity, tectonics,
erosion and volatiles) relevant for solar system studies; to survey
resources for further lunar exploration. These goals are addressed by
the MORO payload with a global geophysical and geochemical multispectral
lunar mapping instrument package of unprecedented resolution. This
Phase-A study report reflects the results of the scientific and
technical study activities.
Title: Resolved profiles of diffuse interstellar bands: evidence
fou rotational contours of gas phase molecules.
Authors: Ehrenfreund, P.; Foing, B. H.
Bibcode: 1996A&A...307L..25E
Altcode:
From high resolution and high signal to noise spectra, we resolved
two or three peak substructures and wing asymmetries in the spectral
profiles of three narrow diffuse interstellar bands (DIBs). The measured
profiles show specific similarities with calculated rotational contours
of gas phase molecular spectra, confirming the theory that gas phase
molecules are some of the DIB carriers. We measured small changes of
the profile substructures with the interstellar line of sight gas
temperature. Minor changes in the DIB widths and wings indicate a
limited geometry distortion of the molecule in the excited state. By
comparison with model calculations of polycyclic aromatic hydrocarbons
(PAHs) and fullerenes, our observations indicate that the molecular
carriers of the DIBs at 5797, 6379 and 6613A have rotational constants
smaller than 0.004cm^-1^, and would correspond to large PAH molecules
with more than 40 C atoms, chains of ~12-18 C atoms, 30 C rings or
C60 fullerene compounds.
Title: High resolution Lyalpha images obtained with the transition
region camera (TRC): a comparison with Hα observations
Authors: Wiik, J. E.; Foing, B. H.; Martens, P.; Fleck, B.;
Schmieder, B.
Bibcode: 1996AdSpR..17d.105W
Altcode: 1996AdSpR..17..105W
Comparing high spatial resolution (~ 1'') images observed in Lyalpha
with the Transition Region Camera (TRC) and in Hα at Sacramento Peak
and Meudon Observatories, we notice that some structures are well
correlated in the two lines (plages), while others are less correlated
(chromospheric network, filaments). This is an indication of the
inhomogeneous distribution of physical parameters in these structures.
Title: Magnetic Structures and Giant Flares in HR1099
Authors: Foing, B. H.; Char, S.; Ayres, T.; Catala, C.; Zhai, D. S.;
Jiang, S.; Huang, L.; Hao, J. X.; Houdebine, E.; Jankov, S.; Baudrand,
J.; Czarny, J.; Donati, J. F.; Felenbok, P.; Catalano, S.; Cutispoto,
G.; Frasca, A.; Rodono, M.; Neff, J. E.; Simon, T.; Collier-Cameron,
A.; Butler, C. J.; MUSICOS 1989 Campaign Collaboration
Bibcode: 1996mpsa.conf..283F
Altcode: 1996IAUCo.153..283F
No abstract at ADS
Title: Advances in solar and stellar physics: space studies
Authors: Foing, B. H.
Bibcode: 1996ASPC..109...31F
Altcode: 1996csss....9...31F
No abstract at ADS
Title: Moro: an european moon orbiting observatory
Authors: Foing, B. H.; Racca, G.
Bibcode: 1996AdSpR..18k..85F
Altcode: 1996AdSpR..18...85F
We present the MORO Moon Orbiting Observatory during its phase A
study. The context for ESA Intermediate mission M3 is described. We
discuss general objectives for scientific lunar studies, specific
reasons for a new orbiter around the Moon, and describe the science
objectives of MORO and the MORO instruments and mission.
Title: ESA lunar study: precursor astronomy missions to the moon
Authors: Foing, B. H.
Bibcode: 1996AdSpR..18k..43F
Altcode: 1996AdSpR..18...43F
We give a summary of the areas identified by the ESA Lunar Study
Steering Group for Scientific Exploration of the Moon in the ESA report
``Mission to the Moon''. We discuss the possible phased approach for
different scientific areas and some potential Precursor Astronomy
Missions. We give a short status of current related ESA studies.
Title: Precursor missions to the Moon. Proceedings. E1 and E1/B3
Meetings of COSPAR Scientific Commissions B and E held during the
Thirtieth COSPAR Scientific Assembly, Hamburg (Germany), 11 - 21
Jul 1994.
Authors: Foing, B. H.; Manka, R. H.
Bibcode: 1996AdSpR..18j...1F
Altcode: 1996AdSpR..18....1F
The following topics were dealt with: the Moon as a platform for
astronomy and space science, dark matter mapping with a Lunar Transit
Telescope, VLF radio astronomy, ESA lunar study, optical interferometry
from the Moon, Lunar Optical Very Large Interferometer (LOVLI), balloon
borne interferometer in the upper stratosphere, results of the MUSES-A
"HITEN" mission, and solar electric propulsion mission to the Moon.
Title: Observation and modelling of main sequence star
chromospheres. V. Ultraviolet excess emission in active M dwarfs.
Authors: Houdebine, E. R.; Mathioudakis, M.; Doyle, J. G.; Foing, B. H.
Bibcode: 1996A&A...305..209H
Altcode:
The variation in the continuum intensity (50-5000nm) of late-type
M dwarfs is investigated via two grids of model atmospheres with
different temperature minima. It is shown that the (E)UV intensity
is mostly dependent on the transition region pressure, although the
temperature minimum also plays an important role. We also observe
a significant frequency redistribution of the photospheric flux when
changing the minimum temperature, and a black-body type of emission from
the lower chromosphere. We examine the formation of the continuum and
point out that, although some differences appear for very low or very
high activity levels, in general the global picture is much alike the
Sun. We show that the UV continua are very good diagnostics of cool
dwarf atmospheres, from the temperature minimum to the transition
region. Our calculations give a good overview of the domains where
physical parameters and spectral signatures are most likely observed. We
compute the UBV(RIJKL)_J_ broad band fluxes for our models and conclude
that the chromospheric contribution should be detectable in the U
band and possibly also in the B band. We compare our calculations to
recent high resolution observations for selected stars in a narrow
spectral range ((R-I)_K_=0.875+/-0.05); we show that Hα line profiles
behave as expected, with a tight correlation between the line width
and equivalent width. Hα emission line stars show an excess in U-B
color but not in B-V. They are also more luminous than their less
active absorption line counterparts, which indicates that active dwarfs
have not yet reached the main sequence and are intermediate between T
Tauri stars and main sequence stars. The anomalously large proportion
of active stars towards late spectral types is attributed to the very
slow contraction phase for low mass stars. We calculate the fluxes in
the Extreme Ultraviolet Explorer Sn/SiO band (500-740A) and show that
they are compatible with observed upper limits. We further compare
our results for the upper activity range to pre-main sequence models
and observations. They strongly support the case for a chromospheric
contribution to Hα and the blue/UV excess for those objects (T
Tauris, naked T Tauris, YSOs). An important conclusion is that at
high pressures, corresponding to active dMe stellar atmospheres,
the chromosphere becomes a very efficient radiator at continuum
wavelengths. From log(M)~-5 (column mass), radiative losses in the
continuum rise exponentially and faster than in Hydrogen spectral lines
because of their larger optical depths. As a consequence, Hi spectral
lines have a small or negligible contribution to the total Hi (lines and
continua) and white light radiative budget. We show that the hydrogen
series dominate the radiative cooling in spectral lines (from 40% to
90%) for Hα emission line stars. The cooling in the (E)UV continuum
overwhelms the total radiative budget and is much larger than that
in outstanding chromospheric and transition region lines (e.g. CaII,
MgII, HI Lyman and Balmer). We propose this as a possible contribution
for the apparent saturation observed in some spectral lines, therefore
questioning the suggestion of saturation in magnetic activity levels.
Title: CIV 1550 transition line observations of AB Doradus with the
Hubble Space Telescope
Authors: Vilhu, O.; Muhli, P.; Huovelin, J.; Rucinski, S.; Collier
Cameron, A.; Slee, B.; Budding, E.; Banks, T.; Foing, B.; Tsuru, T.
Bibcode: 1996ASPC..109..297V
Altcode: 1996csss....9..297V
No abstract at ADS
Title: The moon as a platform for astronomy and space science
Authors: Foing, B. H.
Bibcode: 1996AdSpR..18k..17F
Altcode: 1996AdSpR..18...17F
Lunar based telescopes and observatories can provide a long term
multi-wavelength window on the Universe. We discuss some basic
constraints and specific facts regarding the use of the Moon as a
site for astronomy and space science. We assess for this use the
effects of gravity, rotation period, surface curvature, the seismic
and tidal stability, as well as the tenuous atmosphere, temperature
variations, weak magnetic fields on the Moon, micro meteorites
flux and the properties of the regolith. We discuss the thermal and
electromagnetic environments on the Moon and the properties of the
dark lunar sites for astronomical instruments. The interest of polar
lunar observatories (with eventual ice existence), the coldest sites in
the solar system, is also presented. We then summarise the respective
advantages and drawbacks of Moon-based astronomy and space science
in relation to ground based and near-Earth orbit astronomy. Finally,
we discuss the science of the Moon. We argue for the renewed interest
of lunar exploration using advanced technologies for understanding
the Earth/Moon history. The Moon is described as a test-bed for solar
system exploration. It allows both remote and in-situ measurements
for ground-truth validation of the understanding of other solar-system
bodies.
Title: Results from 3 November 1994 Solar Eclipse
Authors: Foing, B. H.; Wiik, J. E.; Henrich, N.; David, F.; Beaufort,
T.; Altieri, B.; Orosei, R.; Laureijs, R.; Metcalfe, L.; Maurice,
E.; Reuter, P.; Bois, D.
Bibcode: 1996mpsa.conf..415F
Altcode: 1996IAUCo.153..415F
No abstract at ADS
Title: ``Precursor missions to the moon'': a summary from the COSPAR
1994 symposium: (Hamburg, July 13-15, 1994)
Authors: Foing, B. H.
Bibcode: 1996AdSpR..18k...3F
Altcode: 1996AdSpR..18....3F
A symposium was dedicated to ``Precursor Missions to the Moon'' at
COSPAR in Hamburg. It included a Joint session (between the COSPAR
Planetary and Astronomy commissions) on ``Recent and Future Missions
to the Moon'', and then specific sessions on ``Precursor Astronomy
from the Moon'', ``Science of the Moon from Precursor Missions (from
Orbiters and Surface experiments)'', ``Life Sciences on the Moon'', and
``Current plans for Precursor Missions from Space Agencies''. After a
previous COSPAR 1992 symposium on ``Astronomy and Space science from
the Moon'', the goal was to concentrate on near term plans and science
projects for the Lunar Exploration and Scientific Exploitation. We
summarise here this symposium, where invited papers reviewed current
ideas and status, and selected oral contributed papers highlighted
specific proposals or related activities. Discussions allowed further
interaction about new concepts, techniques, constraints and strategies.
Title: Search for coronene and ovalene cations in the diffuse
interstellar medium.
Authors: Ehrenfreund, P.; Foing, B. H.; D'Hendecourt, L.; Jenniskens,
P.; Desert, F. X.
Bibcode: 1995A&A...299..213E
Altcode:
Recent studies suggest carbon-containing molecules as the best
candidates for the carriers of the unidentified diffuse interstellar
bands (DIBs), considering their abundance and ability to form stable
bonds in interstellar space. The spectra of the naphthalene and pyrene
cations in a neon matrix were recently reported, indicating a link
between these small polycyclic aromatic hydrocarbon (PAH) ions and some
diffuse bands. We have searched for new DIBs in the near-infrared and
around 4592A in order to identify the coronene (C_24_H_12_) and ovalene
(C_32_H_14_) cations in the diffuse medium. Due to their pericondensed
structure these molecules should be among the most stable PAHs in
the interstellar medium. The absorption spectra of both molecules
were recently measured in solid neon. We report on the search for
the bands at 9465/4592A and 9780A, and derive corresponding limits
on the presence of the coronene and ovalene cations in the diffuse
interstellar medium. From these results, we discuss a possible selective
destruction mechanism of PAHs through dication formation, and the role
of PAH compounds as possible DIB carriers.
Title: Astronomy and space science from station Moon.
Authors: Foing, Bernard H.
Bibcode: 1995JBIS...48...67F
Altcode:
Special issue: "Lunar-based astronomy".
Title: Search for fullerenes and PAHs in the diffuse interstellar
medium
Authors: Ehrenfreund, P.; Foing, B. H.
Bibcode: 1995P&SS...43.1183E
Altcode:
Recent studies suggest carbon-containing molecules as the best
candidates for carriers of the unidentified diffuse interstellar bands
(DIBs). considering their abundance and ability to form stable bonds
in interstellar space. We have searched for new DIBs in the near-IR and
have detected two new diffuse bands that are consistent with laboratory
measurements of C 60+ in a neon matrix. Criteria
for this possible identification are discussed. From these observations
and the DIB treasured absorption. we estimate that up to 0.9% of
interstellar carbon could be in the form of C 60+
We also searched for poly cyclic aromatic hydrocarbon (PAH) canons and
have derived corresponding limits for the presence of the coronene C
24H 12 and ovalene C 32H 14
cations in space. We have studied the ionization properties of these
PAH cations, which could explain their selective destruction. From
these results we discuss the role of fullerenes and PAHs as possible
DIB carriers.
Title: Highlights from the COSPAR 1992 symposium: "Astronomy and
space science from the Moon".
Authors: Foing, Bernard H.
Bibcode: 1995JBIS...48...71F
Altcode:
Special issue: "Lunar-based astronomy".
Title: Nonradial pulsations in 48 Persei: results from MUSICOS
1989 campaign
Authors: Hao, Jinxin; Lin, Huang; Catala, C.; Foing, B. H.
Bibcode: 1995mscs.conf...91H
Altcode:
No abstract at ADS
Title: Diffuse Interstellar Bands in the Near Infrared - A Dedicated
Search for Polycyclic Aromatic Hydrocarbon and Fullerene Cations
Authors: Foing, B.; Ehrenfreund, P.
Bibcode: 1995ASSL..202...65F
Altcode: 1995dib..book...65F
No abstract at ADS
Title: Results from the November 3, 1994 Total Solar Eclipse
Authors: Foing, B. H.; Wiik, J. E.; David, F.; Beauford, T.; Altieri,
B.; Orosei, R.; Laureijs, R.; Metcalfe, L.; Maurice, E.; Reuter, P.;
Bois, D.
Bibcode: 1995pist.conf..121F
Altcode:
No abstract at ADS
Title: Multi-site observations of Shoemaker-Levy 9 impacts with
Jupiter: the countdown.
Authors: Foing, B. H.
Bibcode: 1995mscs.conf..311F
Altcode:
No abstract at ADS
Title: Recherche de fullerènes et de PAHs dans le milieu
interstellaire.
Authors: Ehrenfreund, P.; Foing, B. H.
Bibcode: 1995LOHP...15....1E
Altcode:
No abstract at ADS
Title: Surface structures and white-light flares on HR 1099: review
of MUSICOS 1989 results.
Authors: Foing, B. H.; Catala, C.; Baudrand, J.; Böhm, T.; Hubert,
A. M.; Cuby, J. G.; Czarny, J.; Dreux, M.; Felenbok, P.; Zhai, D.;
Jiang, S.; Huang, L.; Hao, J.; Char, S.; Jankov, S.; Ayres, T.;
Neff, J. E.; Simon, T.; Houdebine, E. R.; Butler, C. J.; Beust, H.;
Lagrange, A. -M.; Ferlet, R.; Vidal-Madjar, A.; Vitry, R.; Cutispoto,
G.; Catalano, S.; Frasca, A.; Rodonò, M.
Bibcode: 1995mscs.conf..131F
Altcode:
No abstract at ADS
Title: A multi-wavelength campaign on YY Geminorum.
Authors: Butler, C. J.; Doyle, J. G.; Budding, E.; Foing, B.
Bibcode: 1995mscs.conf..207B
Altcode:
No abstract at ADS
Title: Multi-site continuous spectroscopy IV. Proceedings.
Authors: Lin, Huang; Disheng, Zhai; Catala, C.; Foing, B. H.
Bibcode: 1995mcsi.book.....L
Altcode:
MUSICOS stands for MUlti-SIte COntinuous Spectroscopy, and is a
project to facilitate multi-site observations in high resolution
spectroscopy. Many scientific programs related to stellar physics have a
strong need for continuous spectroscopic monitoring. The goal of MUSICOS
is to make multi-site spectroscopic observations on 2 m class telescopes
an easy and efficient operation. A three-step strategy was defined for
MUSICOS: 1. Organize multi-site, multi-wavelength campaigns, with the
existing instruments, and by using transportable fiber-fed spectrographs
on 2 m telescopes without adequate spectrographs. 2. Define, design and
build to prototype of a cheap spectrograph meeting the requirements of
the scientific programs needing multi-site observations. 3. Duplicate
this spectrograph and install the copies on telescopes of the 2 m
class around the world. The authors have now completed step 2 of this
overall strategy.
Title: General discussion on the MUSICOS project: minutes and
recommendations.
Authors: Catala, C.; Foing, B. H.
Bibcode: 1995mscs.conf..351C
Altcode:
No abstract at ADS
Title: Preparing for SOHO: results from the transition region camera
Authors: Wiik, J. E.; Foing, B. H.; Schmieder, B.; Martens, P.;
Fleck, B.
Bibcode: 1994ESASP.373..433W
Altcode: 1994soho....3..433W
No abstract at ADS
Title: Multi-site continuous spectroscopy. II. Spectrophotometry
and energy budget of exceptional white-light flares on HR1099 from
the MUSICOS 89 campaign.
Authors: Foing, B. H.; Char, S.; Ayres, T.; Catala, C.; Neff, J. E.;
Zhai, D. S.; Catalano, S.; Cutispoto, G.; Jankov, S.; Rodono, M.;
Simon, T.; Akan, C.; Aslanov, A.; Avellar, P.; Baudrand, J.; Beust,
H.; Cao, H.; Chatzichristou, H.; Cuby, J. G.; Czarny, J.; de La Reza,
R.; Dreux, M.; Felenbok, P.; Ferlet, R.; Frasca, A.; Floquet, M.;
Ghosh, K.; Guo, Z.; Guerin, J.; Hao, J. X.; Houdebine, E. R.; Huang,
L.; Hubert, A. M.; Hubert, H.; Huovelin, J.; Hron, J.; Ibanoglu, C.;
Jiang, S.; Keskin, V.; Lagrange-Henri, A. M.; Lecontel, J. M.; Li,
Q.; Mavridis, L.; Nolthenius, R.; Petrov, P.; Savanov, I.; Scherbakov,
A.; Tuominen, I.; Vidal-Madjar, A.; Zhang, R.; Zhang, X.
Bibcode: 1994A&A...292..543F
Altcode:
We report results from the December 89 multi-site continuous observing
campaign (MUSICOS 89) dedicated to the study of surface active
structures and flares on the RS CVn-type system HR1099 (=V711 Tau). This
system has been observed by up to 17 telescopes around the globe during
this campaign. We obtained complete phase coverage for Doppler imaging
of photospheric spots. Quasi-simultaneously, we observed the modulation
of Ca II K line profile due to chromospheric plage regions. At least
two exceptional white-light flares on 14 Dec. 15:00 UT and 15 Dec. 1:00
UT (the largest such optical flare episode ever reported in a RS CVn
system) were detected photometrically with typical rise and decay
times of 60-90 min, and with remarkable spectral dynamic signatures
in Hα, with longer decay time scale. Equivalent colours, temperature
excesses and projected flare areas (0.55 and 0.89 solar disc areas)
were derived for the two optical flares. We estimate the energy budget
for these two events, with respective peak intensities of radiative
losses of 1.65 and 1410^33^erg/s and integrated losses over the
white-light event duration of a few hours of 8.10^36^ and 10^38^ergs
(in the 3100-5900A range), indicating a total energy balance several
times these values. The emission was also measured in the Hα and
Hβ lines during these flares with a ratio of flare optical emission
over Balmer emission 3-4 times larger compared to other flares on
dwarfs. More than one day after the last white-light flare, part of
the flare decay phase was also measured with IUE in UV lines of low
and high excitation; the extrapolated transition region EUV losses are
found similar to the derived Balmer line losses. Both flares were shown
to occur near the limb. We derive their physical area, and estimate
their densities, column mass, and penetration depth. From Balmer line
broadening and flows, we derive a kinetic energy budget comparable to
the radiative losses. We discuss a possible magnetic energy budget
and the interpretation in terms of filament ejection occurring over
a magnetic arcade. These observations bring a new understanding and
questions about energy transport mechanisms in stellar flares.
Title: Azimuthal Structures in the Wind and Chromosphere of the
Herbig Ae-Star Ab-Aurigae - Preliminary Results from the MUSICOS-1992
Campaign
Authors: Catala, C.; Bohm, T.; Donati, J. F.; Simon, T.; Welty, A.;
Houdebine, E.; Huang, L.; Jiang, S.; Zhai, D.; Neff, J.; Foing, B. H.;
Ghosh, K.; Butler, J.; Collier-Cameron, A.; Baudrand, J.; Czarny, J.;
Zhao, F.; Talavera, A.; Kennelly, T.; Carter, B.; Rees, D.; Semel,
M.; Cutispoto, G.; Rodono, M.
Bibcode: 1994SoPh..155..185C
Altcode:
MUSICOS (for MUlti-SIte COntinuous Spectroscopy) is an international
project to facilitate and organize world-wide multi-site campaigns
in high resolution spectroscopy, in view of obtaining a complete time
coverage of various types of variable stellar phenomena.
Title: Book reviews
Authors: Hermsen, W.; Stamm, W.; Nieuwenhuijzen, H.; Plez, B.;
Koch-Miramond, L.; Schadee, A.; De Greve, J. P.; Icke, Vincent;
Kresák, Ľ.; Dekker, E.; Bonnet-Bidaud, J. -M.; Foing, B. H.
Bibcode: 1994SSRv...67..421H
Altcode:
No abstract at ADS
Title: Highlights
Authors: Foing, B. H.
Bibcode: 1994AdSpR..14f...1F
Altcode: 1994AdSpR..14....1F
No abstract at ADS
Title: The Moon as a site for astronomy and space science
Authors: Foing, B. H.
Bibcode: 1994AdSpR..14f...9F
Altcode: 1994AdSpR..14....9F
Lunar based telescopes and observatories can provide a long term
multi-wavelength window on the Universe. Here we discuss some basic
constraints and specific facts regarding the use of the Moon as a
site for astronomy and space science. We assess for this use the
effects of gravity, rotation period, surface curvature, the seismic
and tidal stability, as well as the tenuous atmosphere, temperature
variations, weak magnetic fields on the Moon, micro meteorites flux
and the properties of the regolith. We discuss the thermal and
electromagnetic environments of the Moon and the properties of the
dark lunar sites for astronomical instruments. The interest of polar
lunar observatories (with eventual ice existence), the coldest sites in
the solar system, is also presented. We then summarise the respective
advantages and drawbacks of Moon-based astronomy and space science in
relation to ground based and near-Earth orbit astronomy. Finally,
we discuss the science of the Moon. We argue for the renewed interest
of lunar exploration using advanced technologies for understanding
the Earth/Moon history. The Moon is described as a test-bed for solar
system exploration. It allows both remote and in-situ measurements
for ground-truth validation of the understanding of other solar-system
bodies.
Title: Astronomy and space science from the moon: Panel discussion
and perspectives
Authors: Foing, B. H.
Bibcode: 1994AdSpR..14f.283F
Altcode: 1994AdSpR..14..283F
The COSPAR Symposium on ``Astronomy and Space Science from the Moon'',
held at the COSPAR/IAF World Space Congress in Washington (on 31
August-3 September 1992), ended with a session on ``Scenarios for
lunar bases and observatories''. A panel discussion was organised to
address specific topics: Precursor astronomy missions Launch,
landing and transportation systems, technologies Site selection
and emplacement, resource utilisation, architectural considerations
Link with space stations, and Mars exploration programmes Human aspects, performance, protection, operations and activities
Protection of the lunar environment Biospheres on the Moon
The panel discussion, coordinate by B.H. Foing (F) included in
particular contributions from Drs Matogawa (Japan), R.M. Bonnet (ESA),
H. Balsiger (CH and ESA representative), P. Bochsler (CH), S. Volonté
(ESA), W. Mendell (NASA), W. Sadeh (USA), R. Manka (USA), B. Burke
(USA), M. Rougeron (CNES), V. Bluem (Germany) and from the general
participants. We give here a summary of these discussions. We also
include additional information for assessing the perspectives for
Lunar based activities after the COSPAR symposium.
Title: Astronomy and space science from the
Moon. Proceedings. Symposium E4 of the COSPAR 29. Plenary Meeting,
Washington, DC (USA), 28 Aug - 5 Sep 1992.
Authors: Foing, B. H.
Bibcode: 1994AdSpR..14f....F
Altcode: 1994AdSpR..14.....F
Contents: 1. Solar physics from the Moon. 2. The Moon as an
open window for astronomy. 3. Ultimate resolution and precision
astronomy from the Moon. 4. Solar system remote observations from the
Moon. 5. Solar system plasmas (Moon in situ measurements and remote
observations). 6. Lunar/Earth science. 7. Scenarios for lunar bases
and observatories.
Title: Detection of two interstellar absorption bands coincident
with spectral features of C60+
Authors: Foing, B. H.; Ehrenfreund, P.
Bibcode: 1994Natur.369..296F
Altcode:
MORE than a hundred well-defined absorption bands, arising from diffuse
gas in the interstellar medium, have been observed in the visible and
near-infrared spectra of stars 1-4. The identity of the
species responsible for these bands has remained unclear, although
many possibilities have been suggested5,6. Carbon-based
molecules ubiquitous in the interstellar medium have been widely
favoured as potential carriers of some of the diffuse interstellar
bands7-10,29 in particular, C60+
has been thought to be a promising candidate9,29. Here
we present the results of a search for C60+
in the near-infrared spectra of seven stars, based on recent
laboratory measurements of the absorption spectrum of this
species11-13. We find two diffuse bands that are coincident
(within 0.1%) with laboratory measurements on C60+
in a Ne matrix11. From this observation and the total
absorption, we estimate that 0.3-0.9% of interstellar carbon is in
the form of C60+. The molecule is very stable,
which should allow it to survive in the interstellar medium for a long
time14, but the inhibition of C60+
formation by hydrogen probably limits its abundance.
Title: Multisite continuous spectroscopy. III. Photometric analysis
and SPOT modelling of the light curves of HR 1099 before and after
the 1989 optical flares.
Authors: Zhai, D. S.; Foing, B. H.; Cutispoto, G.; Zhang, R. X.;
Catala, C.; Char, S.; Zhang, X. B.; Jankov, S.
Bibcode: 1994A&A...282..168Z
Altcode:
We present the UBV and UBV (RI)c photometry of HR 1099 (=
V711 Tau) carried out at the Beijing Astronomical Observatory and the
European Southern Observatory (ESO) (La Silla, Chile) during the second
Multisite Continuous Spectroscopy (MUSICOS) campaign in 1989. Except
for the zeropoint, the light curves at both observatories coincide with
each other and are combined to form unified light curves. A photometric
analysis is carried out by using the spot approximation based on the
Roche model. The light curves are obviously asymmetric and show an
unusual phase shift of light minimum which is different in different
wave bands. It is found that two cool and one hot spots can reconstruct
simultaneously the main characteristics of all 5 UBV (RI)c
light curves and that two adjacent spots, one cool and the other hot,
created a large temperature gradient distribution along the longitude
which is responsible for the phase shift in different wave bands. The
increase of the brightness of the binary system observed immediately
after the flare appeared to be phase-dependent and it is found to be
probably caused by the evolution of spots, especially by the hot spot.
Title: Diffuse interstellar bands in Orion. The environment dependence
of DIB strength.
Authors: Jenniskens, P.; Ehrenfreund, P.; Foing, B.
Bibcode: 1994A&A...281..517J
Altcode:
Four Diffuse Intersellar Bands (DIB) have been measured in 22 lines
of sight towards Orion and GMC214-13. The paper reports on the
environment dependence of DIB strength, using reddening, the total
extinction in the visual, and column densities of various forms of
hydrogen as indicators of line of sight conditions. In lines of sight
with small reddening, EB-V less than 0.08 mag, a weakening
of lambda(6284) and lambda(5785) is found relative to reddening (=
all matter), but no weakening relative to atomic + molecular hydrogen
(= all neural matter). This probably implies that the DIB carriers
are absent in the ionised HII medium. At higher reddening, where a
significant part of hydrogen is an molecular form, all DIBs in Orion
decrease with increasing EB-V in a similar way as is known
for the Taurus and Ophiuchus dark clouds. In Taurus, where even in low
reddened lines of sight a significant part of hydrogen is in molecular
form, lambda(6284) is weakened compared to diffuse medium values at
lower reddening than lambda (6196). In lines of sight towards the Orion
Nebula, where molecular hydrogen is mostly dissociated, lambda(6284)
is some 70% stronger, while lambda(6196) is a factor of 5 weaker than
expected from the above dependence. The results are discussed in the
context that the carrier of the diffuse bands might be a large molecule
in ionised form. The dissociation and ionisation state of hydrogen
is used as an indicator of the UV field. The results above indicate
that the lambda(6284) carrier is both ionised and destroyed by higher
energy photons than the lambda(6196) carrier, which is consistent with
a molecular carrier.
Title: The MUSICOS Network for Multi-Site Continuous Spectroscopy
Authors: Foing, B. H.; MUSICOS Collaboration; Catala, C.; Baudrand,
J.; Boehm, T.; Hubert, A. M.; Jankov, S.; Cutispoto, G.; Catalano,
S.; Pagano, I.; Rodono, M.; Umana, G.; Zhai, D. S.; Jiang, S.; Huang,
L.; Hao, J. X.; Char, S.; Houdebine, E. R.; Ayres, T.; Neff, J. E.;
Simon, T.; Butler, C. J.; Collier-Cameron, A.; Kennelly, T.; Walker,
G.; Talavera, A.
Bibcode: 1994ASPC...64..699F
Altcode: 1994csss....8..699F
No abstract at ADS
Title: Book Review: Physics of the plasma universe / Springer-Verlag,
1992
Authors: Foing, B. H.
Bibcode: 1994SSRv...67..430F
Altcode: 1994SSRv...67..430P
No abstract at ADS
Title: Multifrequency observations of AB Doradus. X-ray flaring and
rotational modulation of a young star.
Authors: Vilhu, O.; Tsuru, T.; Collier Cameron, A.; Budding, E.;
Banks, T.; Slee, B.; Ehrenfreund, P.; Foing, B. H.
Bibcode: 1993A&A...278..467V
Altcode:
X-ray observations of AB Doradus, performed by the Large Area
Counter (LAC) instrument of the GINGA satellite on January 1990, are
reported. The observations covered 5 rotations of the star (2.6 days)
during which 4 flares were detected. When added to the previously
observed EINSTEIN and EXOSAT flares, a total of 7 X-ray flares in
AB Dor have been observed so far. The flares seem to cluster around
rotational phases 0.1-0.25 and 0.6-0.75 although the statistics are
poor. The mean flare energies were around (1-3) x 1034 erg
with peak luminosities (4-6) x 1030 ergs/s. The flaring loops
were compact (ne = 1012/cu cm) and extended (1-2)
x 1010 cm above the surface. Flare masses (1018
g) and frequencies (two per day) are similar to prominence-like cloud
formations discovered previously in the star. The flare spectra can be
best-fitted either by thermal Bremstrahlung with kT = 3-6 keV or with
a power-law, with photon index gamma = 2.2-2.6. During the strongest
flare peaks AB Dor is a 10 mCrab source with a Crab-like spectrum. The
3 sigma upper limit for the 6.7 keV iron line during the flares is
somewhat smaller than predicted by thin plasma models. We discuss the
possibility of lowering the equivalent width by an extra non-thermal
continuum due to mildly relativistic electrons. Simultaneous 8.4
GHz observations during flare No. 1 gave only a marginal detection,
constraining the magnetic field strength to less than 50 Gauss if
the total X-ray continuum is non-thermal in origin. The sensitivity
was not good enough to detect any clear modulation in the X-ray light
curve, folded over the 0.514 d rotation period. Simultaneous 8.4 GHz
observations were performed with the 64 m antenna of the Australia
Telescope National Facility at Parkes and reveal a clear variability
with two maxima at phases 0.0 (spot A) and 0.5 (spot B). Nearly
simultaneous optical photometry can be modeled by a cool extended
photospheric spot at the phase 0.0 (spot A). Simultaneous H-alpha
photometry revealed a transient H-alpha absorption feature above the
spot A, trapped in co-rotation with the stellar magnetic field. All
these multifrequency data can be understood by a geometrical two spot
model. The geometry seems to have been permanent during the past 10
years, although the relative contributions of the two poles vary and
the spots are not necessarily fixed into 180 degrees apart all the
time. <This result is a new evidence against using solely the solar
analogy when interpreting data from rapidly rotating active cool stars.
Title: Dynamics of flares on late-type dMe stars. III. Kinetic energy
and mass momentum budget of a flare on AD Leonis.
Authors: Houdebine, E. R.; Foing, B. H.; Doyle, J. G.; Rodono, M.
Bibcode: 1993A&A...278..109H
Altcode:
In two previous publications (Paper I and II in this series), we
described the spectral line Doppler shifts and asymmetries observed
during a large flare on AD Leo, and interpreted those in terms of
mass motions. Here, in order to further constrain the plasma physical
properties and estimate the amount of energy released under mass
motions, we developed simple methods so as to infer lower limits to the
plasma cross-section, volume, column density, mass, average emissivity
and optical depth. This allows us to derive the first kinetic energy
and momentum budget of a stellar flare spectral signatures at visible
wavelengths. The investigation of the line flux variation along the
Balmer series indicates that up to 40% or more of the CaII H emission is
likely to arise from radiative pumping by the Balmer H-epsilon line. For
the preflare motion of the solar like 'dark filament', we estimate that
its minimum mass, kinetic energy and radius are respectively about 6.4
1013 kg, 2.7 1032 erg and 5 107 m. The
impulsive phase downward motion which attains deep photospheric layers
in 'kernels' is believed to carry a mass of only 1.3 1013 kg
and energy 2.4 1032 erg. The area/extent values we inferred
from the Balmer and the CaII lines using escape probability methods
agree well with NLTE-radiation transfer modelling. We obtain a minimum
kernel area of approximately 6 1013 sq m and an estimated
area of approximately 1014 sq m. A flaring prominence whose
spectral signature is oscillatory Doppler shifts has an estimated mass
and radius of respectively 1.2 1013 kg and 2 107
m. The minimum kinetic energy associated with its motion is about 2.9
1031 erg. We find that the kinetic energy associated with
the detected mass motions strongly depends on the localization of the
flare on the stellar disc. Ignoring or taking into account this possible
projection factor for the velocities gives a total kinetic energy of
respectively approximately 3 1030 erg and approximately
6 1032 erg (without the impulsive phase CME). The latter
figure is about a factor of 3 times more than the energy radiated in the
U-band and 2.3 times less than the 'missing energy' in the K band. This
points to an interesting aspect of stellar flare energetics, that is,
for this flare the kinetic energy may be a significant fraction of the
total energy budget. Along the same lines, our results also indicate
that possibly only a small fraction of the kinetic energy is carried by
cool plasmas and that most mass motions may occur in coronal plasmas at
a higher temperature regime. This important aspect of flare energetics
should be assessed by simultaneous observations in optical and UV/EUV
spectroscopy with a higher time resolution.
Title: Chromospheric rotational modulation in solar-like stars. I. A
method for multi-component modelling of CA II H and K spectroscopic
variability.
Authors: Char, S.; Foing, B. H.
Bibcode: 1993A&A...276...69C
Altcode:
High resolution profiles of chromospheric lines may give very valuable
information about the inhomogeneous structure and flows within
the atmosphere of late type and quiescent dwarfs. Here we present a
method for empirical modelling of the variability of Ca II H spectra,
validating some assumptions by observations of α Cen B. We developed
a multicomponent description and simulation code for the spectroscopic
modulation of fluxes, velocities, asymmetries and profiles associated
with large scale chromospheric regions on the cool stars. We present
the results and the analysis of this technique that can be applied for
estimating rotational period, or the coverage of chromospheric active
structures in solar-like stars.
Title: Chromospheric rotational modulation insolar-like
stars. II. Multi-component modelling and rotational period of alpha
Centauri B from CA II H spectroscopic variability.
Authors: Char, S.; Foing, B. H.; Beckman, J.; Garcia Lopez, R. J.;
Rebolo, R.
Bibcode: 1993A&A...276...78C
Altcode:
The K1V late-type dwarf α Cen B has been monitored to search for
spectroscopic variability in the Ca II H chromospheric line during
its rotational period. The observations were made with the Coudé
Echelle Spectrograph with the 1.4 Coudé Auxiliary Telescope at ESO,
with spectral resolution 80000. Variability in flux up to 29 % and
profile asymmetries are explained as modulation caused by discrete
structures such as solar-like plages on the star surface. An analysis
of the visibility and velocity of these structures gives a rotational
period of 43 days, in agreement with the Rossby number derived from the
Ca II chromospheric flux. A multi-component model is used to estimate
the positions and filling factors of such emissive structures. A
coherence time up to 6 months is found for the plage signature, but
gradual phase shifts and overall flux variations are observed from
year to year, providing an information on the emergence/disappearance
of active regions and on cyclic effects operating on global activity.
Title: Multi-site continuous spectroscopy. I. Overview of the MUSICOS
1989 campai
Authors: Catala, C.; Foing, B. H.; Baudrand, J.; Cao, H.; Char, S.;
Chatzichristou, H.; Cuby, J. G.; Czarny, J.; Dreux, M.; Felenbok, P.;
Floquet, M.; Geurin, J.; Huang, L.; Hubert-Delplace, A. M.; Hubert,
H.; Huovelin, J.; Jankov, S.; Jiang, S.; Li, Q.; Neff, J. E.; Petrov,
P.; Savanov, I.; Shcherbakov, A.; Simon, T.; Tuominen, I.; Zhai, D.
Bibcode: 1993A&A...275..245C
Altcode:
We describe the organization of the multi-site spectroscopic MUSICOS
1989 campaign. This international campaign involved a large number of
telescopes distributed around the world. In order to yield a complete
time coverage, we had to transport two fiber-fed spectrographs, built
at Paris-Meudon Observatory, to remote sites. Three scientific programs
were followed during this campaign: 1) search for nonradial pulsations
in the Be star 48 Per; 2) search for the signature of "co-rotating
interaction regions" in the wind of the pre-main sequence Herbig Ae
star AB Aur; 3) Doppler imaging and flare patrol for the RS CVn system
HR 1099. The goal of the campaign was to provide a continuous coverage
of these three targets in selected spectral lines. Programs 1 and 3
were successful, in the sense that the resulting duty cycle was over 80%
for 48 Per and HR 1099. On the other hand, program 2 was unsuccessful,
due to bad weather at most of the sites during the nights devoted to
AB Aur. Although the initial goal of program 2 was not achieved,
the observed spectra indicate an unusual activity level for AB Aur,
and these results are presented here, while detailed analysis of the
results of programs 1 and 3 will be published separately.
Title: Dynamics of flares on late type dMe stars. II. Mass motions
and prominence oscillations during a flare on AD Leonis.
Authors: Houdebine, E. R.; Foing, B. H.; Doyle, J. G.; Rodono, M.
Bibcode: 1993A&A...274..245H
Altcode:
On 28 March 1984 at 3:22 UT, a 2.1 magnitude flare in the U-band was
observed simultaneously in several wavelength regions, including low
resolution spectrophotometry in the wavelength range 3600-4400Å. This
flare displayed enhanced emission in chromospheric lines for a duration
of about 50 min. By studying in detail the emission line centroid
displacements and asymmetries, we discovered several new exciting
phenomena. In this paper we present evidence for complex velocity
fields. A deeper investigation of the plasma physical parameters and
the kinetic energy associated with these mass motions is discussed
by Houdebine et al. (1993). Prior to the flare onset, weak
P-Cygni profiles were observed in the Call resonance lines which
we interpret as evidence for the preflare motion of a solar like
"dark filament". The loop radius is estimated to be of the order of
5 1O7 m. During the impulsive phase, a high velocity mass
ejection was observed (Houdebine et al. 1990, Paper I) with red-shifts
in the Balmer line cores, the CaII K and HeI 4026Å. This latter event
is interpreted as the downward motion of chromospheric condensations
initiated by highly energetic particle beams (in the MeV range)
and a subsequent chromospheric evaporation. The inferred minimum
energy flux deposited by the beam in the transition region is about
9 1010 which corresponds to the energy of a large flare
on the Sun. Later during the flare, a 2.68 min periodic oscillation
occurred in the line centroids with a peak to peak amplitude up to ∼
95 km s-1. We show that it is most likely the signature
of periodic motions in a prominence that may have been initiated by
flare-born disturbances. This prominence (whose minimum radius and apex
magnetic field strength are 2 1O7m and 20G respectively)
expanded slowly during the gradual phase, and finally disrupted,
ejecting part of its mass higher in the corona. The loop disruption
signatures are well defined reversed P-Cygni profiles that are sustained
for several minutes. During the post-flare stage, we found clues for
clouds of plasma spread across the stellar disc with a minimum filling
factor of 17%.
Title: Continuous IUE Monitoring of HR 1099 Throughout Two Complete
Orbital Cycles (6 days) in December 1992
Authors: Neff, J. E.; Simon, T.; Pagano, I.; Rodono, M.; Foing, B.
Bibcode: 1993AAS...182.4604N
Altcode: 1993BAAS...25..874N
In order to map the spatial structure of a stellar atmosphere using
Doppler imaging techniques, observations of a rapidly-rotating star must
be obtained at all of its rotational phases. In order to discriminate
temporaral variability (e.g. flares) from phase-locked variability
(produced by magnetically-active regions on the stellar surface),
observations must be obtained over at least two rotational cycles. Using
the International Ultraviolet Explorer, we observed the bright RS
CVn-type system HR 1099 (V711 Tau) continuously for two contiguous
orbital/rotational cycles (period ~ 2.83 days) in December 1992. These
observations were coordinated with the 1992 campaign for Multi-Site
Continuous Spectroscopy (MUSICOS). The purpose of this campaign was
to coordinate a network of ground-based telescopes distributed around
the Earth so that moderate and high-resolution spectroscopy could be
obtained pseudo-continuously for several days. Supporting photometric
and radio observations also were obtained simultaneously. We are using
the IUE high-dispersion spectra of the Mg II h and k lines to map the
spatial structure of the stellar chromosphere and to study atmospheric
dynamics during flares. In conjunction with the IUE low-dispersion
spectra, we will be able to model the radial structure of the
chromosphere. We present preliminary results showing the rotational
modulation of the ultraviolet line fluxes and of the high-dispersion
line profiles. At least 3 transition-region flares occurred within
this 6-day interval, and our observations constrain both the rise and
decay phases of these flares. The effect of a non-uniform atmospheric
structure is subtle, but it is visible in the observed line profiles.
Title: Stellar objectives of SIMURIS
Authors: Damé, L.; Coradini, M.; Foing, B.; Rutten, R. J.; Thorne,
A.; Vial, J. C.
Bibcode: 1993MmSAI..64..345D
Altcode:
No abstract at ADS
Title: Photometric and Spectroscopic Investigation for the Optical
Rare of V711 Tau (=HR1099) in 1989
Authors: Zhai, D. S.; Foing, B. H.; Catala, C.; Zhang, R. X.
Bibcode: 1993ASPC...38..268Z
Altcode: 1993nfbs.proc..268Z
No abstract at ADS
Title: The beta Pictoris protoplanetary system. XIV. Simultaneous
observations of the CA II H and K lines: evidence for diffuse and
broad absorption features.
Authors: Ferlet, R.; Lagrange-Henri, A. -M.; Beust, H.; Vitry, R.;
Zimmermann, J. -P.; Martin, M.; Char, S.; Belmahdi, M.; Clavier,
J. -P.; Coupiac, P.; Foing, B. H.; Sevre, F.; Vidal-Madjar, A.
Bibcode: 1993A&A...267..137F
Altcode:
The sporadic circumstellar spectroscopic variations detected since
1985 towards Beta Pic have been formerly interpreted as the result
of the evaporation of small cometary-like bodies in the vicinity of
the star. To further investigate the physics of the infalling bodies,
we developed new instrumentation able to monitor simultaneously the
variability of the two Ca II H and K lines, in order to give access
to different parameters than the ones previously surveyed. Because
the instrument, whose resolving power is of the order of 10,000, is
attached to small size telescopes (one meter class) via a fiber link,
the new information is related to a more continuous survey of the lines
variability over few weeks periods. We present the detection of new
very broad and shallow absorption signatures, seen simultaneously in
the vicinity of the two Ca II lines. The results obtained confirm our
original model by showing that the variability of the events seems to
be erratic on these time scales and that the absorbing material has
to be spread quite often over areas significantly smaller than the
stellar projected surface. They further reveal the existence of more
gaseous material very close to the star, produced by the evaporation of
'body-showers', probably made of multiple smaller bodies impossible
to detect individually.
Title: The MUSICOS project: Multi-SIte COntinuous Spectroscopy
Authors: Catala, C.; Baudrand, J.; Böhm, T.; Foing, B. H.
Bibcode: 1993ASPC...40..662C
Altcode: 1993ist..proc..662C; 1993IAUCo.137..662C
No abstract at ADS
Title: RIASS Observations of AB Doradus (HD 36705)
Authors: Pagano, I.; Rodonò, M.; Cutispoto, G.; Collier Cameron, A.;
Kürster, M.; Kellett, B. J.; Bromage, G. E.; Jeffries, R.; Foing,
B.; Ehrenfreund, P.
Bibcode: 1993ASSL..183..457P
Altcode: 1993pssc.symp..457P
No abstract at ADS
Title: The SIMURIS interferometric mission: solar physics objectives
and model payload (invited paper)
Authors: Damé, L.; Coradini, M.; Foing, B.; Rutten, R. J.; Thorne,
A.; Vial, J. C.
Bibcode: 1993MmSAI..64..333D
Altcode:
No abstract at ADS
Title: Stellar Coronal Imaging
Authors: Foing, B. H.
Bibcode: 1993ASSL..183..421F
Altcode: 1993pssc.symp..421F
No abstract at ADS
Title: Tomographic/interferometric studies of active stars and
binaries.
Authors: Jankov, S.; Char, S.; Foing, Bernard H.
Bibcode: 1992ESASP.344..113J
Altcode: 1992spai.rept..113J
As for the principle of interferometric imaging, the methods of
tomographic imaging allow to spatially resolve stellar surfaces and
environments. The authors describe the principle of indirect imaging
of stellar surfaces, based on spectroscopic and photometric rotation
modulation and they show particular application and their results of
Doppler imaging of spotted stars. The common problem of regularization
of the inverse problem for the interferometric and tomographic methods
is discussed. The applicability of both methods to different phenomena
of stellar activity is compared. As a consequence it is concluded that
space interferometry and tomographic imaging methods should be used to
produce complementary results in order to have an access to phenomena
of different temporal and spatial behaviour.
Title: Prospects in stellar and galactic observations with SIMURIS.
Authors: Foing, Bernard H.
Bibcode: 1992ESASP.344..123F
Altcode: 1992spai.rept..123F
The SIMURIS instruments will be able to access non-solar objects,
with an interesting resolution for several stellar programmes in
preparation to future long baseline interferometers in Space or on
the Moon. Stellar angular diameters can be measured below the Rayleigh
resolution of the SUN interferometer. Using both SUN spatial resolution
and IFTS spectral resolution, the separations and velocity curves of
binary stars can be determined at several wavelengths. In particular
separations of binaries including Cepheids or supergiants brighter than
12 and a hotter companion brighter than 15 at 180 nm can be obtained
down to 0.1 marcsec up to 2 kpc in the Galaxy, thus allowing to solve
for the masses and distances of the components.
Title: Tomographic imaging of lete-type stars from spectroscopic
and photometricrotational modulation. I. Principle and mathematical
formulation of the method.
Authors: Jankov, S.; Foing, B. H.
Bibcode: 1992A&A...256..533J
Altcode:
The paper describes the principle of and the methods for the flux
rotational modulation imaging of late-type stars. The full mathematical
formulation of the problem of indirect stellar imaging from projections
is presented in terms of matricial formalism. The performance and
the intrinsic limitations of the method are demonstrated, using the
indirect imaging code built on the basis of the developed approach to
reconstruct an input image from a series of generated noisy spectra.
Title: Design Rationale of the Solar Ultraviolet Network / Sun
Authors: Dame, L.; Acton, L.; Bruner, M. E.; Connes, P.; Cornwell,
T. J.; Curdt, W.; Foing, B. H.; Hammer, R.; Harrison, R.; Heyvaerts,
J.; Karabin, M.; Marsch, E.; Martic, M.; Mattic, W.; Muller, R.;
Patchett, B.; Roca-Cortes, T.; Rutten, R. J.; Schmidt, W.; Title,
A. M.; Tondello, G.; Vial, J. C.; Visser, H.
Bibcode: 1992ESOC...39..995D
Altcode: 1992hrii.conf..995D
No abstract at ADS
Title: Book-Review - Helioseismology from Space
Authors: Foing, B. H.; Hoyng, P.
Bibcode: 1992SoPh..137..203F
Altcode:
No abstract at ADS
Title: The MUSICOS Network for Multi-Site Continuous Spectrophotometry
Authors: Foing, B. H.; Catala, C.; Baudrand, J.; Boehm, T.; MUSICOS
Team
Bibcode: 1992ASPC...26..637F
Altcode: 1992csss....7..637F
No abstract at ADS
Title: Spatially-Resolved Environment and Coordinated Multi-Frequency
Observations of HR 1099
Authors: Foing, B.
Bibcode: 1992iue..prop.4461F
Altcode:
No abstract at ADS
Title: Multi-site Spectroscopic Networks for the Study of Late-type
Stars (Invited)
Authors: Foing, Bernard H.; MUSICOS Team
Bibcode: 1992LNP...397..224F
Altcode: 1992sils.conf..224F
No abstract at ADS
Title: MUSICOS - multi-site continuous spectroscopy. Proceedings.
Authors: Catala, C.; Foing, B. H.
Bibcode: 1991musi.work.....C
Altcode:
Contents: 1. Scientific aim and need for multi-site observations. 2. The
MUSICOS campaign organization and operations. 3. First results from the
MUSICOS campaign. 4. Prospects for future multi-site multi-wavelength
campaigns.
Title: TRC 4: Correlation of the Tmin fine structure with the
chromospheric bright points
Authors: Martic, Milena; Dame, Luc; Bruner, M. E.; Foing, Bernard H.
Bibcode: 1991AdSpR..11e.241M
Altcode: 1991AdSpR..11..241M
Simultaneous ground based observations in the Ca II K2V
line and high resolution UV filtergrams (at λ160 nm) obtained during
the 4th rocket flight of TRC (Transition Region Camera) were used for
comparative studies of the fine structure in active regions, network,
and supergranulation cells interior. In this paper we report similar
time evolution and spatial correspondence between chromospheric cell
bright points and continuum emission form the solar Tmin region. These
results support the existence of a standing wave phenomena in the
cell interiors.
Title: A solar interferometric mission for ultrahigh resolution
imaging and spectroscopy: SIMURIS
Authors: Damé, L.; Acton, L.; Bruner, M.; Connes, P.; Cornwell, T.;
Foing, B. H.; Heyvaerts, J.; Lemaire, P.; Martić, M.; Muller, R.;
Porteneuve, J.; Roca Cortés, T.; Riehl, J.; Rutten, R.; Séchaud,
M.; Smith, P.; Thorne, A. P.; Title, A. M.; Vial, J. -C.; Visser,
H.; Weigelt, G.
Bibcode: 1991AdSpR..11a.383D
Altcode: 1991AdSpR..11..383D
SIMURIS is an interferometric investigation of the very fine structure
of the solar atmosphere from the photosphere to the corona. It was
proposed to ESA /1/, November 30 1989, for the Next Medium Size
Mission - M2, and accepted in February 1990 for an Assessment Study
in the context of the Space Station. The main scientific objectives
will be outlined, and the ambitious model payload featuring the Solar
Ultraviolet Network (SUN), a 2 m long monolithic array of 4 telescopes
of Ø20 cm, and the Imaging Fourier Transform Spectrometer (IFTS),
an UV and Visible Imaging Fourier Transform Spectrometer coupled to
a Ø40 cm Gregory, described.
Title: Solar physics at ultrahigh resolution from the space station
with the Solar Ultraviolet Network (SUN)
Authors: Damé, L.; Acton, L.; Bruner, M.; Connes, P.; Cornwell,
T.; Foing, B.; Heyvaerts, J.; Lemaire, P.; Martić, M.; Muller, R.;
Roca Cortés, T.; Riehl, J.; Rutten, R.; Title, A. M.; Vial, J. -C.;
Visser, H.; Weigelt, G.
Bibcode: 1991AdSpR..11e.267D
Altcode: 1991AdSpR..11..267D
The SUN experiment is a UV and visible Space Interferometer aimed at
ultra-high resolution in the solar atmosphere. It has been proposed
to ESA as part of the SIMURIS Mission Proposal which has recently
been accepted for an Assessment Study in the framework of the
Space Station. The 4 × 20 cm telescopes of the SUN linear array are
non-redundantly placed to cover a 2 m baseline, and the instrument makes
full use of stabilized interferometry potential, the 4 telescopes being
co-aligned and co-phased on a reference field on the sun. After a brief
outline of the scientific objectives, the concept of the instrument
is described, and its image reconstruction potential is illustrated.
Title: Effect of surface structures on integrated seismology
measurements
Authors: Foing, Bernard H.; Char, Sergio; Jankov, Slobodan
Bibcode: 1991AdSpR..11d.207F
Altcode: 1991AdSpR..11..207F
The presence of a non uniform distribution of large scale structures
on stellar surfaces (photospheric temperatures, chromospheric emission,
abundances, magnetic fields, intrinsic velocity fields or intrinsic line
profile and broadening) induces a rotational modulation of photometric
and spectroscopic measurements. In globally integrated flux,
profiles or Doppler measurements, this rotational modulation (in
amplitude and time curve) has a specific Fourier signature at selected
harmonics of the rotation frequency. We calculate the corresponding
modulation transfer signature for typical spot and plage parameters
in the solar case. We stress the need to estimate and correct such
effects from the observed power spectrum in the seismological analysis,
especially in the frequency up to the range of gravity modes. Also,
due to the oscillation inhibition in magnetic regions, the rotational
modulation of the seismological signal, has a specific Fourier signature
at the 3 first harmonics of the rotation frequency, appearing as
sidelobes around each genuine oscillatory peak that can affect the
observed broadening, splitting and line shapes of low frequency p-modes.
Title: First results from the MUSICOS 89 campaign: active surface
structures and flares on HR 1099.
Authors: Foing, B. H.; Char, S.; Jankov, S.; Catala, C.; Zhai, D. S.
Bibcode: 1991musi.work..117F
Altcode:
The authors report on the first results from the multisite continuous
campaign in December 89 (MUSICOS 89) dedicated to the study of surface
active structures and flares on the RS CVn-type system HR 1099. A
complete phase coverage was obtained for the Doppler imaging of
photospheric spots. Quasi simultaneously, the spectral modulation of
Ca II K line due to chromospheric plage regions was observed, and is
being modelled. At least two exceptional flares (the largest optical
flares reported in such RS CVn system) were detected photometrically
and with remarkable spectral signatures in H alpha.
Title: Helioseismology from space
Authors: Foing, B. H.
Bibcode: 1991AdSpR..11d....F
Altcode: 1991AdSpR..11Q....F
Status and goals in helioseismology, scientific objectives and results
of space projects, and cross-correlative studies are among the broad
topics considered. Attention is given to such topics as the search
for solar gravity modes; a statistical analysis of solar neutrino
flux variations; helioseismology with the IPHIR instrument on the
Phobos mission; and global oscillations at low frequency according
to the SOHO mission. Papers are also presented on ground-based
helioseismology networks; a new theory of umbral oscillations; the
effect of surface structures on integrated seismology measurements;
and the inferrence of solar-structure variations from photometric and
helioseismic observations.
Title: Preface
Authors: Foing, Bernard H.
Bibcode: 1991AdSpR..11d...1F
Altcode: 1991AdSpR..11Q...1F
No abstract at ADS
Title: Overview of the MUSICOS campaign organization.
Authors: Catala, C.; Foing, B. H.
Bibcode: 1991musi.work...49C
Altcode:
No abstract at ADS
Title: ESO observations with the IAP/IAS Ca II K special spectrometer
during the MUSICOS 89 campaign.
Authors: Char, S.; Foing, B.; Lemaire, P.; Lagrange, A. M.; Beust,
H.; Vidal Madjar, A.; Vitry, R.; Zimmerman, J. P.
Bibcode: 1991musi.work...69C
Altcode:
HR 1099, a highly active RS CVn star was monitored in the chromospheric
Ca II K line during the Musicos campaign. The authors used a special
spectrometer developed to monitoring variations of the Ca II lines on
stars (circumstellar absorption for β Pictoris and emissive features
on stars showing solar-like magnetic activity such as the RS CVn and
late type stars). They describe the characteristics of the instrument
and show a sample of obtained spectra for HR 1099.
Title: SIMURIS: Solar, Solar System and Stellar Interferometric
Mission for Ultrahigh Resolution Imaging and Spectroscopy
Authors: Coradini, M.; Dame, L.; Foing, B.
Bibcode: 1991ssss.book.....C
Altcode:
No abstract at ADS
Title: Rocket observations and modelling of flux-tubes
Authors: Foing, Bernard H.; Dame, Luc; Martic, Milena
Bibcode: 1991AdSpR..11e.245F
Altcode: 1991AdSpR..11..245F
The solar observations at high angular resolution have led to the
discovery that the solar magnetic field is structured in filamentary
fields at the photospheric level. Manifestations of these fluxtubes can
be diagnosed with EUV images (with the Transition Region Camera Rocket
Experiment, TRC) at 220nm in the middle photosphere, at 160nm in the
temperature minimum region or in the Ly alpha and C IV lines formed
at temperatures 20 000K and 100 000K in the transition region. In the
frame of a thin flux tube modelling of the TRC data, the vertical
variation of tube parameters and the conditions for thermalisation
in the upper photosphere are discussed. We consider constraints from
EUV observations on current models of flux-tubes and coronal loops
including non LTE calculations, dynamic and magnetic effects.
Title: Multi-site stellar networks for asteroseismology
Authors: Foing, Bernard H.; Catala, Claude; MUSICOS Team
Bibcode: 1991AdSpR..11d.159F
Altcode: 1991AdSpR..11..159F
Several scientific programmes (such as asteroseismology, stellar
rotational modulation, surface structures, Doppler imaging, variable
winds, coordinated multi-frequency observations with space satellites)
require a continuous spectroscopic and photometric coverage during
several days. Valuable continuous observations can be obtained from
multi-site networks of ground-based observatories equipped with
identical instruments, in complementarity with future facilities from
the earth poles, interplanetary probes, dedicated satellites or the
lunar base.
Title: Cooling curves of stellar flare plasmas from time resolved
optical spectroscopy.
Authors: Houdebine, E. R.; Butler, C. J.; Panagi, P. M.; Rodono, M.;
Foing, B. H.
Bibcode: 1991A&AS...87...33H
Altcode:
The relative importance of the basic phenomena that drive the emission
line fluxes during the stellar flares in the spectral range 3600 - 4400
A, is so far, still poorly known. This paper discusses the impact on
the chromosphere of the flare soft X-ray and optical/(E)UV continuum,
as well as the plasma expansion and temperature effects for emission
lines. For each spectral line, models are developed, based on the main
atomic processes taking place in the flare plasma which is assumed to
be stationary and optically thin. This preliminary model is applied to
four flares on the active dMe stars UV Ceti, Proxima Cen, and AD Leo,
to investigate the cooling of the flare plasma that emits in these
lines. The results provide convincing evidence that the line fluxes
are largely influenced by variation in temperature. By comparing the
results for diffferent spectral lines, the modeling also provides
information on the line opacities of the flare medium.
Title: Possible scenarios of coronal loops reconnection/heating
processes to be observed at high spatial resolution
Authors: Dame, L.; Heyvaerts, J.; Foing, B. H.
Bibcode: 1991AdSpR..11a.327D
Altcode: 1991AdSpR..11..327D
Recent improvements in interferometric techniques could allow to
achieve 0.01 arcsec angular resolution on the Sun, i.e. 10 km. Such
a high resolution is of direct interest to understand the coronal
loop structure since current observations at low resolution cannot
distinguish between major dissipation/heating theories which all involve
very small scale dissipating processes. Three simplified scenarios of
loop instabilities are investigated in this paper and the resulting fine
structure and contrast that they might induce on observable quantities
(temperature, density) are deduced.
Title: The imaging fourier transform spectrometer for the SIMURIS
mission
Authors: Foing, B. H.; Dame, L.; Thorne, A. P.; Lemaire, P.
Bibcode: 1991AdSpR..11a.387F
Altcode: 1991AdSpR..11..387F
The Solar Interferometric Mission for Ultrahigh Resolution Imaging and
Spectroscopy (SIMURIS) is an interferometric investigation in space
at ultraviolet and visible wavelengths aimed at reconnaissance of
solar features at angular scales from 0.3 to 0.01 arcsec. The Imaging
Fourier Transform Spectrometer (IFTS) is, with the Solar Ultraviolet
Network (SUN), one of the core instruments of the proposed SIMURIS
mission. It consists of a 40 cm Gregory telescope feeding a double
grating pre-dispersive spectrometer before entering a Fourier transform
spectrometer for a field of 10 × 10 arcsec2 at 0.3 arcsec
resolution. The SIMURIS/IFTS requires upgrading of existing FTS down
to 120 nm, with imaging capabilities. For the IFTS imaging a detector
with fast readout must be used. There are also demanding constraints
on the real time processing, and the subsequent important data rate,
and requirements on an upgraded instrument pointing system (IPS),
within the resources and capabilities of the Space Station.
Title: ESO remote control observations from Garching for the MUSICOS
'89 campaign.
Authors: Jankov, S.; Foing, B. H.
Bibcode: 1991musi.work...65J
Altcode:
In order to fulfill the task of La Silla (Chile) site in MUSICOS
'89 campaign the remote control observations were carried out at ESO,
Garching (Germany) from 14 to 16 December 1989. The Coude Auxiliary
Telescope (CAT) equipped with the Coude Echelle Spectrometer (CES)
and short camera + CCD detector, were dedicated to accomplish the RS
CVn program. Since the remote control of the CAT/CES instrumentation
is almost routinely done from the control room in ESO, Garching it was
possible to successfully accomplish the observations (Doppler Imaging
and Flare Monitoring) that need a continuous instrumental control.
Title: Fast spectroscopic variations on rapidly rotating, cool dwarfs
III. Masses of circumstellar absorbing clouds on AB Doradus.
Authors: Collier Cameron, A.; Duncan, D. K.; Ehrenfreund, P.; Foing,
B. H.; Kuntz, K. D.; Penston, M. V.; Robinson, R. D.; Soderblom, D. R.
Bibcode: 1990MNRAS.247..415C
Altcode:
We present new time-resolved Hα, Ca II H and K and Mg II h
and k spectra of the rapidly rotating KO dwarf star AB Doradus
(= HD 36705). The transient absorption features seen in the Hα
line are also present in the Ca II and Mg II resonance lines. New
techniques are developed for measuring the average strength of the
line absorption along lines-of-sight intersecting the cloud. These
techniques also give a measure of the projected cloud area. The
strength of the resonance-line absorption provides new constraints
on the column densities, projected surface areas, temperatures and
internal turbulent velocity dispersions of the circumstellar clouds
producing the absorption features. At any given time the star appears
to be surrounded by between S and 20 clouds with masses in the range
2-6 × 1017 g. The clouds appear to have turbulent internal
velocity dispersions of order 3-20 km s-1, comparable with
the random velocities of discrete filamentary structures in solar
quiescent prominences. Night-to-night changes in the amount of Ca II
resonance line absorption can be explained by changes in the amplitude
of turbulent motions in the clouds. The corresponding changes in the
total energy of the internal motions are of order 1029
erg per cloud. Changes of this magnitude could easily be activated by
the frequent energetic (∼1034 erg) X-ray flares seen on
this star.
Title: European Photon Imaging Camera (EPIC) for X-ray astronomy.
Authors: Bignami, G. F.; Villa, G. E.; Boella, G.; Bonelli, G.;
Caraveo, P.; Chiappetti, L.; Quadrini, M. E.; Di Cocco, G.; Trifoglio,
M.; Ubertini, P.; Peres, G.; Sciortino, S.; Serio, S.; Vaiana, G.;
Rothenflug, R.; Vigroux, L.; Koch, L.; Rio, Y.; Pigot, C.; Cretolle,
J.; Gabriel, A.; Foing, B.; Atteia, J. L.; Roques, J. P.; Bräuninger,
H.; Pietsch, W.; Predehl, P.; Reppin, C.; Struder, L.; Trümper, J.;
Lutz, G.; Kendziorra, E.; Staubert, R.; Holland, A. D.; Cole, R. E.;
Wells, A.; Pounds, K.; Lumb, D. A.; Pye, J.; Turner, M. J. L.; Goodall,
C. V.; Ponman, T. J.; Skinner, G. K.; Willmore, A. P.
Bibcode: 1990SPIE.1344..144B
Altcode: 1990exrg.conf..144B
ESA has selected the final payload for its "Cornerstone" mission
in X-Ray astronomy with multiple mirrors (XMM), to be flown in the
late nineties in the context of the "Horizon 2000" long term science
plan. EPIC represents the main instrument of the mission, to include
three CCD arrays in the focal planes of the three telescopes of the
spacecraft. They will be dedicated to source imaging, photometry,
spectroscopy and timing. The goals of EPIC are described.
Title: Circumstellar magnetic activity, flares and mass ejections
in young stars.
Authors: Foing, B. H.; Collier-Cameron, A.; Ehrenfreund, P.;
Houdebine, E.
Bibcode: 1990ESASP.315...53F
Altcode: 1990fspe.rept...53F
Stellar activity studies give a useful information on the early Sun
and its environment, and for estimating activity effects on the young
solar nebula. Large scale active structures can be diagnosed from their
rotational modulation signature, and reconstructed in 3 dimensions,
using tomographic or Doppler imaging techniques. Young stars undergo
violent flares associated with coronal mass ejections leading to mass
loss rates that can affect significantly the stellar environment and
even the young stellar evolution. Young stars also show large coronal
condensations, magnetically linked with the stellar surface, that can
be destabilised by occurring energetic flares. From a joint ESA/AAT/IUE
campaign, masses of such circumstellar clouds around the young star
AB Doradus were estimated. These studies allow to tackle the problems
of the link between circumstellar structures and magnetic activity and
the role of mass ejections and flares in the context of mass loss and
angular momentum braking in young stars, and early stellar evolution.
Title: Dynamics of flares on late-type dMe stars. I. Flare mass
ejections and stellar evolution.
Authors: Houdebine, E. R.; Foing, B. H.; Rodono, M.
Bibcode: 1990A&A...238..249H
Altcode:
Evidence of a high-velocity mass ejection event starting with the onset
of a particularly violent flare on the M dwarf star AD Leo is presented
and discussed. The plasma was ejected at projected line-of-sight
speeds of up to 5800 km/s. The velocity, mass, and kinetic energy of
the flow are compared to solar Coronal Mass Ejection (CME) events. The
recent and independent discovery of a strong stellar wind, probably
driven by sporadic CME events on V471 Tauri, is strongly in favor of
the present interpretation. An estimation of the ejected mass during
the observed flare event for various sets of electron temperature and
plasma opacity effects, combined with mean flare occurrence rates,
indicates that flare related mass loss may significantly affect the
normal evolution of active red-dwarfs.
Title: Solar magnetic flux-tubes and coronal loops.
Authors: Foing, B. H.
Bibcode: 1990ESASP.311....1F
Altcode: 1990plas.work....1F; 1990plap.rept....1F
High resolution observations show that the solar magnetic field is
structured in fluxtubes from the photosphere to the corona. These
tubes can be diagnosed with EUV images such as those obtained with the
Transition region Camera rocket experiment in Ly α or in different
continua. Constraints on flux tube models are presented. Observations
of loops in the corrona show the confining role of the magnetic field,
but also the coexistence of plasmas at different temperatures. Relevant
diagnostics and models of coronal loops are discussed. The study of
these magnetic structures on the sun, considered as a plasma laboratory,
is of interest for stellar magnetic fields and coronae and in other
astrophysical contexts. For discriminating between different processes
at work in fluxtubes and coronal loops, the author stresses the expected
contribution of the SOHO observatory and of the SIMURIS interferometric
project under study for ultra-high resolution.
Title: Rotational modulation and flares on RS Canum Venaticorum and
BY Draconis-type stars. XV. Observations of Proxima Centauri and
solar calibration data.
Authors: Haisch, B. M.; Butler, C. J.; Foing, B.; Rodono, M.; Giampapa,
M. S.
Bibcode: 1990A&A...232..387H
Altcode:
Results are reported from simultaneous Exosat and IUE observations
of flaring in Proxima Cen on March 2, 1985. The data are presented in
extensive tables and sample spectra and discussed in detail. The peak
emission of the soft-X-ray flare is found to be about 3 x 10 to the 27th
erg/sec, with energy about 3 x 10 to the 30th erg and an associated
increase in Mg II flux to 17,000-67,000 erg/sq cm sec, or about an
order of magnitude lower than the solar value. The presence of flare-
and microflare-related processes heating the corona is inferred.
Title: The MUSICOS Network for MUlti-SIte COntinuous Spectroscopy
Authors: Foing, Bernard; Catala, Claude; MUSICOS Team
Bibcode: 1990LNP...367..457F
Altcode: 1990psss.conf..457F
MUSICOS, (for MUlti SIte Continuous Spectroscopy) is a project for a
multisite network of high resolution spectrometers around the world
partly dedicated to continuous spectroscopy, under study in France,
with European and extra-European collaborators. This network aims to
serve the solar/stellar community (for the study of asteroseismology,
stellar rotational modulation, surface structures, Doppler imaging,
variable winds, coordinated multi-frequency observations with
space satellites...) specially for programs requiring a continuous
spectroscopic coverage around the clock during several days. A
major scientific goal of MUSICOS is to allow the study of non radial
pulsations (e.g. of OB, Be, delta Scu, fast rotating B stars) and
ultimately asteroseismological studies of solar type stars, using the
most complete continuity. This goal drives the highest constraints
on the spectrometer (high efficiency, high S/N, wavelength range over
500A, spectral stability). The first MUSICOS campaign dedicated to 3
targets in december 1989, involved sites and telescopes in Mauna Kea
(CFH and 2.2m UH), Kitt Peak Mc Math, La Silla 1.4m CAT, France 1.5m
OHP, Crimea 2.6m Shajn and China 2.16m Xinglong with two fiber-fed
spectrographs transported for this campaign at Hawaii and Xinglong. The
current MUSICOS instrument design (fiber-fed cross-dispersed echelle
spectrograph with a resolution 30000 coupled to a CCD detector,
for duplication) are described; the expected performances for
asteroseismology and the strategy for a multisite network of similar
spectrographs are presented.
Title: High Resolution Solar Physics from the Space Station with
Interferometric Techniques: The Solar Ultraviolet Network (SUN) -
Instrument &Objectives
Authors: Damé, L.; Acton, L.; Bruner, M.; Connes, P.; Cornwell, T.;
Foing, B.; Heyvaerts, J.; Jalin, R.; Lemaire, Ph.; Martic, M.; Moreau,
B.; Muller, R.; Roca Cortés, T.; Riehl, J.; Rutten, R.; Title, A. M.;
Vial, J. -C.; Visser, H.; Weigelt, G.
Bibcode: 1990PDHO....7..262D
Altcode: 1990dysu.conf..262D; 1990ESPM....6..262D
No abstract at ADS
Title: Solar-Like Magnetic Structures in Active Close Binaries
Authors: Foing, B. H.
Bibcode: 1990ASIC..319..363F
Altcode: 1990acb..proc..363F
No abstract at ADS
Title: Perspectives for Groundbased and Space Research on Active
Close Binaries
Authors: Foing, B. H.
Bibcode: 1990ASIC..319..845F
Altcode: 1990acb..proc..845F
No abstract at ADS
Title: MUSICOS: Multi-Site Continuous Spectroscopy : 2 : 1990
Authors: Catala, C.; Foing, B. H.
Bibcode: 1990mmsc.conf.....C
Altcode:
No abstract at ADS
Title: Surface structures and flares in solar-like stars
Authors: Foing, B. H.; Char, S.; Jankov, S.; Houdebine, E.
Bibcode: 1990nwus.book..213F
Altcode:
No abstract at ADS
Title: Multi-Site Spectroscopic Campaign in December 1989
Authors: Catala, C.; Foing, B. H.
Bibcode: 1989IAUC.4877....1C
Altcode: 1989IAUC.4877....0C
C. Catala and B. H. Foing write: "We are organizing a worldwide
multi-site campaign to obtain spectra with complete and continuous
time coverage over 72 hr for each of three stars: 48 Per (Dec. 7-10
UT; search for nonradial pulsations on a Be star; concentration
on He I 667.8 nm); AB Aur (Dec. 11-13; rotational modulation of
winds in a pre-main-sequence Herbig Ae star; concentration on Ca II
K); and V711 Tau = HR 1099 (Dec. 14-17; Doppler imaging of active
regions and flare monitoring on RS CVn stars; concentration on Fe I,
Ca I 643.0-643.9 nm, H-alpha, and Ca II K). The respective desired
resolutions and signal-to-noise ratios for these stars are: 40 000,
> 300; 30 000, > 50; 40 000, > 200. The telescopes currently
involved in this campaign are the University of Hawaii 2.2-m reflector,
3.6-m Canada-France-Hawaii Telescope, Kitt Peak McMath, La Silla 1.4-m
CAT, Haute Provence 1.5-m reflector, Crimea 2.6-m Shajn reflector, and
Peking Observatory 2.16-m reflector. In order to reinforce the outcome
of this campaign, we solicit additional spectroscopic and photometric
observations of these stars during and around the period mentioned
above. Multi-frequency coverage from groundbased and space facilities
in radio, infrared, visible, ultraviolet, or x-ray ranges would be
also a unique opportunity for understanding the variability due to
oscillations, instabilities, winds, active structures, or flares. Those
interested in participating should contact Claude Catala (Observatoire
de Paris, Section de Meudon, F-92195 Meudon Principal Cedex, France;
telephone 33-1-45077668; e-mail CATALA@MEUDON.SPAN) or Bernard Foing
(Space Science Department, ESA/ESTEC, P.O. Box 299, 2200 AG Noordwijk,
The Netherlands; telephone 31-1719-84958; e-mail BFOING@ESTCS1.SPAN)."
Title: Chromospheres of late-type active and quiescent dwarfs. I. an
atlas ofhigh resolution CA II H profiles.
Authors: Rebolo, R.; Garcia Lopez, R.; Beckman, J. E.; Vladilo, G.;
Foing, B. H.; Crivellari, L.
Bibcode: 1989A&AS...80..135R
Altcode:
As a result of a major program of spectral observations using the
CAT 1.4 m telescope and Coude Echelle Spectrograph at ESO, La Silla,
68 high resolution profiles of the 3968.5 A Ca H resonance line have
been obtained for 16 late type stars (dwarfs and subgiants, including
the sun) ranging from F9 to K5, selected to be representative of a
wide span of chromospheric activity. The methods, and results of a
set of reduction and analysis techniques applied to these spectra are
presented. Each wavelength scale is converted to a frame at rest with
respect to the photosphere of the star, and the flux scale is finally
transformed into units of absolute flux. A major effort was applied to
quantify the effects of the tilted baselines of the recorded spectra
on these absolute flux calibrations. The calibrated profiles are used
to extract and tabulate measured chromospheric H emission fluxes and
the velocity shifts with respect to the photosphere of the emission
cores and of the H3 self-reversals.
Title: Chromospheres of late-type active and quiescent dwarfs. II. an
activity index derived from profiles of the CA II lambda 8498 A and
lambda 8542 A triplet lines.
Authors: Foing, B. H.; Crivellari, L.; Vladilo, G.; Rebolo, R.;
Beckman, J. E.
Bibcode: 1989A&AS...80..189F
Altcode:
High resolution, high signal to noise spectral profiles of the
8498 and 8542 A lines of the Ca II infrared triplet (IRT) have been
obtained for a sample of late type dwarfs, with a wide range of levels
of chromospheric activity, in the spectral range F9 to K4/5. These
profiles, and the difference profiles for selected active and quiescent
objects of corresponding spectral type are presented. After absolute
calibration in flux, advantage is taken of the high resolution and S/N
ratios of the spectra to define several IRT indices of chromospheric
activity, for a set of bandwidths between 0.2 A and 1 A about the line
centers. Excellent correlations for active stars between the IRT and
the Ca H indices and between the respective line widths are shown,
which pertain despite the different depths of formation of the lines
in the stellar chromospheres.
Title: Solar Ultraviolet Network: an interferometric investigation
of the fundamental solar astrophysical scales
Authors: Dame, Luc; Moreau, Bernard G.; Cornwell, Timothy J.;
Visser, H.; Title, Alan M.; Acton, Loren W.; Aime, Claude; Braam,
Bart M.; Bruner, Marilyn E.; Connes, Pierre; Faucherre, Michel; Foing,
B. H.; Haisch, Bernhard M.; Hoekstra, Roel; Heyvaerts, Jean; Jalin,
Rene; Lemaire, Philippe; Martic, Milena; Muller, R.; Noens, J. C.;
Porteneuve, Jacques; Schulz-Luepertz, E.; von der Luehe, Oskar
Bibcode: 1989SPIE.1130..126D
Altcode:
The Solar UV Network (SUN) presently proposed is an interferometric
system, based on the principles of stabilized interferometry, which
will be capable of solar observations with spatial resolutions better
than 0.013 arcsec. SUN will consist of four 20-cm diameter telescopes
aligned nonredundantly on a 2-m baseline. SUN is judged to be ideally
deployable by the NASA Space Station, if implemented on a pointing
platform whose performance is of the order of the Instrument Pointing
System flown on Spacelab 2. The compact, nonredundant configuration of
SUN's telescopes will allow high-resolution imaging of a 2 x 2 arcsec
field on the solar disk.
Title: Erratum: Stellar Flare Spectral Diagnostics: Present and Future
Authors: Foing, Bernard H.
Bibcode: 1989SoPh..123..398F
Altcode:
No abstract at ADS
Title: Stellar Flare Spectral Diagnostics - Present and Future
Authors: Foing, Bernard H.
Bibcode: 1989SoPh..121..117F
Altcode: 1989IAUCo.104..117F
Stellar spectral diagnostics are of utmost importance to test
fundamental concepts of flare physics such as particle beam versus
suprathermal heating, atmospheric response, mass motions, microflaring,
statistics and recurrence of flares, flare activity and stellar
interior. We review some of these diagnostics (from photometry, optical,
and ultraviolet spectroscopy at medium- and high-spectral resolution,
X-ray, and radio observations). Specific diagnostics from line and
continuum fluxes, density sensitive lines, broadening and velocity
field effects and the comparison with semi-empirical models are also
described.
Title: Coordinated observations of a large impulsive flare on UV Ceti.
Authors: de Jager, C.; Heise, J.; van Genderen, A. M.; Foing, B. H.;
Ilyin, I. V.; Kilkenny, D. S.; Marvridis, L.; Cutispoto, G.; Rodono,
M.; Seeds, M. A.; Yuen, K. Ng.; van Driel, W.; Rabattu, X.; Zodi,
A. M.; Vilas Boas, J. W. S.; Scalise, E.; Schaal, R. E.; Kaufmann,
P.; Waelkens, C.
Bibcode: 1989A&A...211..157D
Altcode:
The characteristics of the major flare observed on UV Ceti on
Decemmber 1985 at 01:26 UT during an international observing campaign
are described. X-ray observations were obtained with Exosat in the
0.06-0.3 keV bands and 1-6 keV bands; optical photometry was obtained
in 11 wavelength bands, and spectra were recorded in the wavelength
range 3500 to 7000 A. The results of the data analysis support the
Impulsive Explosion Model proposed for stellar flares and disclose
some differences with the solar case.
Title: Electron temperatures of flare plasmas from emission line
fluxes.
Authors: Houdebine, E. R.; Butler, C. J.; Rodono, M.; Panagi, P. M.;
Foing, B. H.
Bibcode: 1989sasf.confP..59H
Altcode: 1989IAUCo.104P..59H; 1988sasf.conf...59H
The authors present spectral diagnostics for the fluxes of emission
lines, in the spectral range 3600 - 4400 Å, during the cooling phase
of stellar flares on dMe stars. Using these diagnostics, electron
temperatures have been computed for flares on AD Leonis, Proxima
Centauri and UV Ceti. This preliminary model assumes a single flare
loop containing a homogeneous, stationary optically-thin flare plasma.
Title: Spectroscopic rotational modulation associated with
chromospheric active structures.
Authors: Char, S.; Foing, Bernard H.
Bibcode: 1989mse..proc..211C
Altcode:
Several active late-type dwarfs have been monitored along their
rotational period to study the spectroscopic variability in the main
chromospheric lines. The authors analyse the Ca II H index and profile
modulation of 20% for α Cen B in terms of solar-like components of
activity (analogous to the quiet network and plage on the Sun). A
simulation of the Ca II H spectra of α Cen B based on multicomponent
features is shown, allowing to estimate the performance of methods
deriving the signature of stellar chromospheric plages from flux,
velocity and asymmetry modulation diagnostics.
Title: Spectral diagnostics of stellar flares.
Authors: Foing, B. H.
Bibcode: 1989musi.work...95F
Altcode:
No abstract at ADS
Title: Modulation rotationnelle par des structures à grande échelle:
possibilités d'application.
Authors: Foing, B. H.; Char, S.
Bibcode: 1989JAF....34Q...6F
Altcode:
No abstract at ADS
Title: A correlation between Balmer and soft X-ray emission from
stellar and solar flares.
Authors: Butler, C. J.; Rodono, M.; Foing, B. H.
Bibcode: 1989sasf.confP..21B
Altcode: 1988sasf.conf...21B; 1989IAUCo.104P..21B
Simultaneous optical spectroscopy and X-ray monitoring of stellar
and solar flares shows that a well-defined linear correlation exists
between the integrated Hγ and soft X-ray flux that extends over four
orders of magnitude. The existence of this relationship implies a
direct proportionality between the emission from the cooler and denser
regions (T ≍ 104K) responsible for Balmer lines and the
emission from the hot plasma (T ≍ 107K) responsible for
soft X-rays. The consequences are considered for (1) several models
which have been proposed for solar flares, and (2) the suggestion that
the Balmer emission results from irradiation by soft X-rays.
Title: Doppler imaging of RS CVn-type active stars.
Authors: Foing, B. H.; Jankov, S.
Bibcode: 1989musi.work...43F
Altcode:
No abstract at ADS
Title: Diagnostics spectraux d'éruptions stellaires.
Authors: Foing, B. H.
Bibcode: 1989JAF....34R...8F
Altcode:
No abstract at ADS
Title: MUSICOS - multi-site continuous spectroscopy. Proceedings.
Authors: Catala, C.; Foing, B. H.
Bibcode: 1989musi.work.....C
Altcode:
Contents: 1. Asteroseismology. 2. Variability due to
rotation. 3. Intrinsic variability and miscellaneous. 4. Instrumental
aspects.
Title: Synthesis of the scientific programs for MUSICOS.
Authors: Foing, B. H.
Bibcode: 1989musi.work..129F
Altcode:
No abstract at ADS
Title: Imagerie Doppler d'étoiles actives de type RS CVn.
Authors: Foing, B. H.; Jankov, S.
Bibcode: 1989JAF....34R...6F
Altcode:
No abstract at ADS
Title: Rotational modulation by large scale structures: possibilities
of application.
Authors: Foing, B. H.; Char, S.
Bibcode: 1989musi.work...31F
Altcode:
No abstract at ADS
Title: Simultaneous multi-wavelength observations of an intense
flare on AD Leonis.
Authors: Rodono', M.; Houdebine, E. R.; Catalano, S.; Foing, B.;
Butler, C. J.; Scaltriti, F.; Cutispoto, G.; Gary, D. E.; Gibson,
D. M.; Haisch, B. M.
Bibcode: 1989sasf.confP..53R
Altcode: 1989IAUCo.104P..53R; 1988sasf.conf...53R
The authors report on the first successful coordinated observations
of stellar flares carried out on March 28, 1984 simultaneously over
a wide range of wavelengths, from UV to microwaves, using the IUE
satellite, three ESO telescopes at La Silla (Chile) and the VLA at
Socorro (NM, USA).
Title: MUSICOS (MUlti-SIte COntinuous Spectroscopy). Objectives and
prospects for asteroseismology.
Authors: Foing, Bernard H.; Catala, C.; Felenbok, P.
Bibcode: 1988ESASP.286..665F
Altcode: 1988ssls.rept..665F
MUSICOS, a project for a multisite facility network of high
resolution spectrometers around the world partly dedicated to
continuous spectroscopy, is under study in France and with European
collaborators. This network aims to serve the solar/ stellar community
specially for programs requiring spectroscopic coverage around
the clock. A major scientific goal is to allow asteroseismological
studies using the most complete continuity. This goal drives the
highest constraints on the spectrometer (efficiency, wavelength range,
stability). The current instrument design is described; the expected
performances for asteroseismology and the organisation of the multisite
network will be discussed.
Title: GOLF: Global Oscillations at Low Frequencies for the SOHO
mission
Authors: Gabriel, A. H.; Bocchia, R.; Bonnet, R. M.; Cesarsky, C.;
Christensen-Dalsgaard, J.; Dame, L.; Delache, Ph.; Deubner, F. L.;
Foing, B.; Fossat, E.
Bibcode: 1988sohi.rept...13G
Altcode:
The GOLF (global oscillations at low frequencies) SOHO (solar
heliospheric observatory) mission is described. It aims to study
the internal structure of the Sun by measuring the spectrum of free
global oscillations. GOLF will measure both p and g mode oscillations,
with emphasis on low order long period waves which penetrate the
solar core. The instrument aims to measure frequencies between 10-7
and 6 10-3 Hz, with a sensitivity of 1 mm/s. The method involves an
extension to space of the ground based technique for measuring the mean
line-of-sight velocity of the solar surface. A sodium vapor resonance
scattering filter is used in a longitudinal magnetic field to sample the
two wings of the solar absorption line. The use of a modulating magnetic
field provides a continuous internal calibration of the sensitivity. By
adding an additional rotating polarizer, measurements are also made
of the average solar magnetic field. Efforts are made to correct the
data for the spurious effects caused by solar magnetic active regions.
Title: A correlation between Balmer and soft X-ray emission from
stellar andsolar flares.
Authors: Butler, C. J.; Rodono, M.; Foing, B. H.
Bibcode: 1988A&A...206L...1B
Altcode:
Simultaneous optical spectroscopy and X-ray monitoring of stellar
and solar flares shows that a well-defined linear correlation exists
between the integrated Hγ and soft X-ray flux that extends over four
orders of magnitude. The existence of this relationship implies a
direct proportionality between the emission from the cooler and denser
regions (T ≈ 104K) responsible for Balmer lines and the
emission from the hot plasma (T ≈ 107K) responsible for
soft X-rays. The consequences are considered for (a) several models
which have been proposed for solar flares, and (b) the suggestion that
the Balmer emission results from irradiation by soft X-rays.
Title: Solar-like Activity in Late-type Stars
Authors: Foing, Bernard H.
Bibcode: 1988IrAJ...18..257F
Altcode:
Solar active structures such as magnetic flux tubes or large-scale
active regions in the chromosphere and transition region have been
studied from images and spectra in UV continua or chromospheric lines
formed at different heights and temperatures. These active structures,
reflecting subphotospheric magnetic field and the underlying dynamo
and participating in the heating of the upper atmosphere, are also
of particular importance for the study of stellar magnetic fields,
internal dynamics, chromospheres and coronae.
Title: Improved Data Reduction Techniques for the ESO CES Plus
RETICON Spectra
Authors: Foing, B. H.; Crivellari, L.
Bibcode: 1988IAUS..132..355F
Altcode:
The authors developed routines for intensity, equivalent width, and
radial velocity measurements on CES plus Reticon spectra obtained with
the ESO 1.4 m telescope. In order to achieve the optimal recovery of
the signal, the noise has to be minimized by removing any parasitical
effect. Special care has been devoted to the correction for remanence
effects in the Reticon dark counts. Typical results are presented
and discussed.
Title: Some Constraints on Chromospheric Modelling for Solar-Type
Stars with High S/n Spectra
Authors: Foing, B. H.; Castelli, F.; Vladilo, G.; Beckman, J.
Bibcode: 1988IAUS..132..149F
Altcode:
High signal to noise spectra are required in chromospheric modelling
because chromospheric emission lines are formed in a boundary layer
under conditions of NLTE and in non-hydrostatic equilibrium, as well as
in multiple magnetically-controlled streams, with horizontal structure
on several scales, and vertical velocity fields. To obtain useable
estimates of energy dissipation with height the authors have obtained
sequences of spectra from F8 to K5 and for stars of different activity
levels. The authors outline the constraints such observations place
on models and indicate theoretical and observational difficulties.
Title: Chromospheric Velocity Fields Diagnostics from CAII and MGII
Emission Profiles
Authors: Vladilo, G.; Crivellari, B. L.; Castelli, F.; Beckman, J. E.;
Foing, B. H.
Bibcode: 1988IAUS..132..283V
Altcode:
The authors discuss the present limits to the velocity field diagnostics
in stellar chromospheres achievable with ESO CAT+CES and IUE high
resolution spectra.
Title: A Method for Calibrating, in Absolute Flux Units, CA II H
Profiles of Late Type Stars Observed at ESO
Authors: Castelli, F.; Gouttebroze, P.; Beckman, J.; Crivellari, L.;
Foing, B.
Bibcode: 1988IAUS..132..153C
Altcode:
The authors have applied to the Sun a method for calibrating, in
absolute flux units, Ca II H profiles of late-type stars. After
comparing, in the region 3948 - 3882 Å, an LTE synthetic spectrum
with the data of the solar flux atlas by Kurucz et al. (1984), they
have defined the wavelength ranges where observations agree with
computations, based on specific radiative equilibrium models and
collisional broadening parameters. By fitting in these regions the
spectrum of the moon observed at ESO with the corresponding synthetic
spectrum, the authors derived a calibration factor that enables them
to calibrate, in absolute flux units, the whole observed range.
Title: Coordinated photometry, spectroscopy and X-ray observations
of flare stars
Authors: Butler, C. J.; Doyle, J. G.; Foing, B. H.; Rodono, M.
Bibcode: 1988ASSL..143..167B
Altcode: 1988acse.conf..167B
The authors have compared the characteristics of flare activity in
UV Ceti and YZ CMi. Almost continuous variability is seen in Hγ and
U-band flux in both stars but only in UV Ceti does this correlate
strongly with soft X-rays. The relative fluxes in the Balmer emission
lines indicates higher densities in the chromospheres of these two
dMe stars as compared to the Sun.
Title: MUSICOS: Multi-Site Continuous Spectroscopy : 1 : 1988
Authors: Catala, C.; Foing, B. H.
Bibcode: 1988mmsc.conf.....C
Altcode:
No abstract at ADS
Title: Extreme ultra-violet filtergrams and X-ray spectroscopy of
active regions and flares from TRC/XSST rocket campaigns
Authors: Foing, B. H.; Martic, M.; Bonnet, R. M.; Bruner, M. E.;
Acton, L. W.; Brown, W. A.
Bibcode: 1988AdSpR...8k.153F
Altcode: 1988AdSpR...8..153F
Ultraviolet filtergrams and X ray spectra were taken by the joint
LPSP/Lockheed rocket experiment TRC/XSST during four international
campaigns involving also ground observations. XSST spectra in the
range 8 to 97A were obtained on the 13 July 1982 flare. From the EUV
filtergrams obtained by the TRC (Transition Region Camera), we could
derive calibrated fluxes in the 220nm and 160 nm continua, in the Ly
alpha and C IV lines, spanning a range of temperatures from medium
photosphere (5 000K), temperature minimum (4 200K), and transition
region (20 000 and 100 000 K). For active regions and a flare, the TRC
fluxes are compared to other data and to corresponding calculations
from semiempirical models. Finally, the scientific prospects of an
advanced TRC/XSST payload onboard future missions are discussed.
Title: Coordinated Multiband Space and Groundbased Observations of
Surface Structures and Flares on Late Type Stars
Authors: Foing, B.; Butler, C. J.; Haisch, B. M.; Linsky, J. L.;
Rodono, M.
Bibcode: 1988copa.conf..197F
Altcode:
The authors discuss the need to coordinate future synoptic observations
at all accessible wavelengths for these objects which are highly
variable on all timescales from seconds to years.
Title: Spectroscopic Variability in Late-Type Dwarfs Using High
S/n Spectra
Authors: Foing, B. H.; Beckman, J. E.; Vladilo, G.
Bibcode: 1988IAUS..132..287F
Altcode:
Monitoring of active late-type dwarfs, spectroscopically with high
resolution (λ/Δλ ≡ 105) and high S:N (>300)
round their activity cycles, principally in the Ca II H resonance
line, offers techniques to explore, (1) plage filling factors, (2)
3-dimensional chromospheric velocity fields, (3) maps of surface
activity via "Doppler Imaging". In this paper the authors deal with
the use of spectral signatures to derive plage cover.
Title: Chromospheric MG II H and K emissions free of interstellar
contamination : velocity structure in late-type dwarfs and giants.
Authors: Vladilo, G.; Molaro, P.; Crivellari, L.; Foing, B. H.;
Beckman, J. E.; Genova, R.
Bibcode: 1987A&A...185..233V
Altcode:
The authors have used high resolution IUE spectra from their own studies
and from the archive to examine the Mg II h and k chromospheric emission
cores of a sample of late-type dwarfs and giants. Sharp photospheric
absorptions were used to provide a velocity rest-frame with respect
to each stellar photosphere with the IUE-limited precision of ±4
km s-1. The knowledge of the kinematics of the local
interstellar medium (LISM) could then be used to identify cases
where either the cores or the wings, or in best circumstances both
features of the chromospheric lines were uncontaminated by LISM
absorption. The authors derive, using only LISM-free emission wings,
accurate Wilson-Bappu relations for both the h and k line, characterized
by a slope higher than in previous determinations.
Title: Diagnostics of solar coronal loops at interferometric angular
resolution
Authors: Foing, B. H.; Faucherre, M.; Dame, L.
Bibcode: 1987ESASP.273..217F
Altcode: 1987ois..work..217F
The advent of very high angular resolution (equivalent to 20 km on the
sun) for extreme ultraviolet observations would allow to diagnose the
fine structure in density and temperature of solar coronal loops. In the
framework of the variety and uncertainties of the existing theoretical
models of loops, the high angular resolution is of particular importance
to estimate the filling factor of loops by hot and cool material, to
measure radial gradients of temperature and density, to observe flows,
spatiotemporal evolution due to heating mechanisms and interaction
between loops.
Title: Flux tubes and loops in the solar chromosphere and corona.
Authors: Foing, Bernard H.
Bibcode: 1987ESASP.275...59F
Altcode: 1987sspp.symp...59F
Solar observations at high angular resolution show that the solar
magnetic field is structured in fluxtubes of 1.5 kG and less than
1 arcsec size at the photospheric level. Manifestations of these
fluxtubes can be diagnosed in the chromosphere and transition region
with EUV images in 160 nm continua or in the Ly alpha and C
IV lines formed at different heights and temperatures. The equilibrium
configuration of the fluxtubes is reviewed for different models:
thin tubes, static loops, steady flows, and numerical unstationary
simulations. In order to describe the pressure and energy balance
from the photospheric to the coronal configurations, it is necessary
to determine such parameters as the temperature, electronic density,
and velocities that will be measured with the coronal instruments on
board the Solar and Heliospheric Observatory (SOHO).
Title: CA II H emission line cores of late-type dwarfs : variability
measurements and velocity field diagnostics.
Authors: Crivellari, L.; Beckman, J. E.; Foing, B. H.; Vladilo, G.
Bibcode: 1987A&A...174..127C
Altcode:
High-resolution spectra of Alpha Cen B, Xi Boo A, 70 Oph A, and
Epsilon Ind obtained using the Coude Echelle Spectrometer and the
1.4-m Coude Auxiliary Telescope of ESO are analyzed. Variations in
the normalized fluxes for the four dwarfs are described. Position
and intensity measurements of the Ca II H features are examined. The
use of the spectra for chromospheric velocity field diagnostics is
discussed. The data reveal that it is possible to separate the effects
of plages from those due to vertical velocity fields; in some stars
the H core samples net upflow and in other net downflow; the layer
sampled by the H3 feature shows a velocity close to that defined by
the photospheric rest frame; and the H2V/H2R asymmetry is useful as
a linear measure of the chromospheric vertical velocity gradient.
Title: Structures fines chromosphériques: nouveaux résultats de
la caméra de la région de transition.
Authors: Foing, B. H.; Dame, L.; Vial, J. C.; Gouttebroze, P.; Martic,
M.; Bonnet, R. M.
Bibcode: 1987JAF....29...15F
Altcode:
No abstract at ADS
Title: La haute résolution en physique solaire: perspectives pour
l'avenir.
Authors: Damé, L.; Foing, B.; Vial, J. C.
Bibcode: 1987JAF....29...16D
Altcode:
No abstract at ADS
Title: Indirect Imaging of Active RS CVn Stars
Authors: Jankov, S.; Foing, B.
Bibcode: 1987LNP...291..528J
Altcode: 1987csss....5..528J; 1987LNP87.291..528J
The RS CVn system HR1099 has been monitored over its orbital period to
study spectroscopic variability in photospheric lines and in Ha. The
observations were made at the CAT 1.4m ESO telescope with the Coude CES
spectrometer and reticon, which permit a resolution of 105
and high S/N. The information provided by the variability of profiles,
together with the limits of the Doppler imaging methods are also
presented. Profiles are calculated with rotational broadening of
immaculate and spotted stars. A line synthesis code including a model
for the inhomogeneous temperature distribution of the primary star
allowed us to calculate a series of spectra at different orbital
phases. Different inversion algorithms were applied to test the
image reconstruction of HR1099, showing the role of such constraints
as chi-square adjustment of the spectra and maximum entropy of the
input image.
Title: High Resolution Profiles of the Ca II Infrared Triplet Lines
in Late Type Active and Quiescent Dwarfs
Authors: Foing, B. H.; Crivellari, L.; Beckman, J. E.; Castelli, F.;
Vladilo, G.
Bibcode: 1987LNP...291..158F
Altcode: 1987LNP87.291..158F; 1987csss....5..158F
In the framework of a long term programme of chromospheric modelling
of late-type dwarfs, high resolution high signal-to-noise spectral
profiles of the 8498 and 8542 A lines of the Ca II infrared triplet
(IRT) have been obtained for a sample of quiescent and active dwarfs
from spectral types F8 to K5. Line core intensity indices are related
to the stellar spectral type, effective temperature, gravity and
rotation. The Ca II IRT spectra have been calibrated to estimate the
excess chromospheric fluxes related to the activity. A relation is
derived between the fluxes measured in the line cores and the Rossby
number for the sample stars with known rotational periods. Line widths,
core and wing intensities, and the differences between active and
quiescent stars of the same spectral type are discussed.
Title: Imagerie Doppler d' étoiles actives.
Authors: Foing, B. H.; Char, S.
Bibcode: 1987JAF....29...22F
Altcode:
No abstract at ADS
Title: Lithium abundances and 7Li/6Li ratios in late-type population
I field dwarfs.
Authors: Rebolo, R.; Crivellari, L.; Castelli, F.; Foing, B.; Beckman,
J. E.
Bibcode: 1986A&A...166..195R
Altcode:
Using the Coudé Echelle Spectrograph fed by the 1.4 m Coudé Auxiliary
Telescope at ESO, La Silla, the authors have obtained a sequence of
fourteen high resolution (λ/Δλ = 105) spectra at high
signal to noise ratio, of main sequence and near main sequence objects
in the wavelength range containing the 6708 Å resonance doublet
of lithium. Using Kurucz thermal equilibrium model atmospheres, and
relying on the excellent signal to noise ratios in the spectra, they
were able to assess not only the 7Li components, but also
the weaker 6Li components of the blended doublet.
Title: New high-resolution rocket-ultraviolet filtergrams of the
solar disc
Authors: Foing, B.; Bonnet, R. -M.; Bruner, M.
Bibcode: 1986A&A...162..292F
Altcode:
A rocket-borne solar ultraviolet telescope named Transition Region
Camera was launched successfully for the third time on 13th July
1982. High quality calibrated photographic images of the sun were
obtained at Lyman alpha and in the continuum at 160 nm and 220 nm. The
angular resolution achieved is better than one arc second. A flare,
active regions, sunspots, the 8 Mm mesostructure, the chromospheric
network, bright UV grains and coronal loops were observed during the
flight. The results are presented and the evolution with height in
the solar atmosphere of the various structures observed is followed
from one wavelength to the other, showing distinct differences. The
value of the field's intensity of magnetic flux tubes is deduced from
the observations.
Title: Coordinated Exosat and spectroscopic observations of flare
stars and coronal heating
Authors: Butler, C. J.; Rodono, M.; Foing, B. H.; Haisch, B. M.
Bibcode: 1986Natur.321..679B
Altcode:
The X-ray flux of dMe stars is thought to arise from two distinct
mechanisms, one involving a continuous `quiescent' emission from a
high-temperature plasma and the other involving the dramatic flare
events which have long been known to occur on these stars. We present
here some results of simultaneous monitoring of the two flare stars, UV
Ceti and EQ Peg, with Exosat and ground-based optical spectroscopy. We
observe short-timescale variability in the 0.1-2-keV emission from both
these objects and, in the case of UV Ceti, find a strong correlation
between the soft X-ray and Hγ fluctuations. The implication is that
much of the low-level X-ray flux previously considered `quiescent'
probably originates from small flare events.
Title: Coordinated IUE and ground-based observations of stellar
flares: YZ CMi, Proxima Cen and AD Leo.
Authors: Foing, B. H.; Rodono, M.; Cutispoto, G.; Catalano, S.; Linsky,
J. L.; Gibson, D. M.; Brown, A.; Haisch, B. M.; Butler, C. J.; Byrne,
P. B.; Andrews, A. D.; Doyle, J. G.; Gary, D. E.; Henry, G. W.; Russo,
G.; Vittone, A.; Scaltriti, F.
Bibcode: 1986RMxAA..12..213F
Altcode:
Coordinated observations of stellar flares were obtained with lUE
and several ground-based facilities in March 1984.The simultaneous
observations allowed it to cover a wide range of wavelengths from ii5nm
to 6cm.We intend to study the effect ofthe observed flares at different
atmospheric heights in order to estimate the energy budget,the time
scales and the cooling processes.Our observations includetime-resolved
IUE spectroscopy at SWP(115-195nm) and LWP(190-320nm),optical
spectroscopy at the ESO 3.6m+IDS (355-440nm),high resolution
spectroscopy at the ESO 1.4m CAT+CES(653-659nm),narrow band H alpha
and wide band optical photometry, infrared photometry at 2.2microns
and microwave observations at 2,6 and 20 cm We present for some
flare events,among the results,the first detection of infrared flux
decrease -or "negative flare"-in coincidence with the flux increase
at the other wavelengths:the broadening and changes of the Balmer H
lines,He and high excitation lines;the appearance of higher members
of the Balmer serie;the enhancements of Mg II doublet and Fe II blend
(260nm);and the flare detection at 2cm and 6cm
Title: High Resolution Observations of Chromospheric Lines in
Late-Type Dwarfs
Authors: Foing, B. H.; Beckman, J.; Crivellari, L.; Galleguillos, D.
Bibcode: 1986RMxAA..12..214F
Altcode:
We obtained at the Coude Echelle Spectrometer (CES) attached to the 1.4m
CAT telescope of the European Southern Observatory ,high resolution
(R=1O0000),high signal to noise (S/N=30-20O) spectra of the Ca II H
and k,H alpha and Ca II infrared triplet lines on a sample of southern
late-type dwarfs also observed with lUE for the Mg II h and k lines
.These profiles are compared for progressive spectral types from
F8V to k5V,and for pairs of active-low active stars of the same type
and we show the variety of the core emissions and asymmetries. The
differential emission in the cores of is discussed in terms of
chromospheric heating and of coverage of these stars with active
regions.The spectral characteristics of the activity signature are
compared with observations and modelling of the profiles for solar
"plages" and active components.Some activity indicators obtained
from the Ca infrared triplet and H alpha lines are plotted versus the
spectral type,showing a lower envelope in the activity corresponding
to the quiescent stars,and the range of variation of the activity at
a given spectral type. These high resolution profiles are used as a
constraint on multi-component models of the stellar chromospheres,which
are being developed to estimate the temperature structure,the radiative
losses and the heating processes in these late-type dwarfs.
Title: Spectroscopic Observations of Comet Austin 1984I
Authors: Foing, B. H.; Festou, M.; Char, S.
Bibcode: 1986RMxAA..12..375F
Altcode:
The comet Austin (1984I) discovered on July 8, 1984 was observed at
the European Southern Observatory on July25.97UT (O.50m reflector and
Stromgren photometer),and July27.96UT(1.5m reflector, Boller &
Chivens spectrograph and image Dissector Scanner in the spectral range
500-730 nm ). Several spectra along the solar-antisolar axis have been
taken, showing the spatial extension of the species C2, NH2, Na I,
H2O+, O I lines.The central diffuse condensation of FWHM 25" , the
spatial behaviour of the previous species and the additional emitting
features included in the photometric Stromgren bands are discussed
Title: XSST/TRC rocket observations of 13 July 1982 flare.
Authors: Foing, B. H.; Bonnet, R. M.; Dame, L.; Bruner, M.; Acton,
L. W.; Brown, W. A.
Bibcode: 1986lasf.conf..319F
Altcode: 1986lasf.symp..319F
The authors analyse the UV filtergrams of the 13 July
1982 solar flare, taken by the Transition Region Camera,
during the third flight of the joint Lockheed/LPSP rocket
experiment XSST/TRC. From the calibrated intensities of the flare
components, they estimate directly the Lyα line flux (from 230 to
650×103erg cm-2s-1sr-1),
differentially the C IV line flux (from 30 to 130×103erg
cm-2s-1sr-1), and the excess of 160 nm
continuum temperature brightness (from 100 to 250K) over the underlying
plage. No detectable variation is observed in the 220-nm channel
formed in the medium photosphere. These values are small compared to
other observed or calculated equivalent quantities from Machado model
of flare F1. The authors estimate the corresponding power required to
heat the temperature minimum accordingly over the 1200 Mm2
area, to be 3.6×1025erg s-1 for this small
X-ray C6 flare, 7 minutes after the ground based observed flare maximum.
Title: New ultra-violet filtergrams and results from the transition
region camera rocket experiment
Authors: Damé, L.; Foing, B. H.; Martic, M.; Bruner, M.; Brown, W.;
Decaudin, M.; Bonnet, R. M.
Bibcode: 1986AdSpR...6h.273D
Altcode: 1986AdSpR...6..273D
The rocket-borne solar ultra-violet telescope named Transition Region
Camera (T.R.C.) was launched successfully for the fourth time on
25th october 1985. Calibrated photographic images of the sun were
obtained at Lyman alpha and in two adjacent bands at 156 nm and 169
nm. The angular resolution achieved was equivalent to 0.7 arcsec. Fine
structures in Lyman alpha were observed in the network and above
supergranular cells. From the 156 nm filtergram (including a strong C
IV contribution) and the 169 nm filtergram, we study the differential
contribution of the C IV lines and of the continuum emission, from
the quiet sun, an active region and at the limb.
Title: Multiband observations of stellar flares.
Authors: Foing, B. H.
Bibcode: 1986lasf.conf..413F
Altcode:
No abstract at ADS
Title: Spectroscopic Variability Associated with Chromospheric
Activity: The α Cen System
Authors: Foing, B.; Beckman, J.; Crivellari, L.; Vladilo, G.; Char, S.
Bibcode: 1986LNP...254..488F
Altcode: 1986csss....4..488F
No abstract at ADS
Title: Chromospheric modelling in late-type dwarfs. 2. CES (Coudé
Echelle Spectrograph) observations of active and quiescent stars.
Authors: Foing, B. H.; Beckman, J.; Crivellari, L.; Galleguillos, D.
Bibcode: 1985Msngr..41...18F
Altcode:
The characteristics of the chromospheres of late-type dwarf stars
were studied using the CoudeEchelle Spectrograph (CES) at ESO and the
IUE. The study focused on the h and k Mg II lines of F and G dwarfs. The
stability of the IUE spectra permitted calculations of averaged
absorption features and the subtraction of the Mg II lines to leave
intrinsic chromospheric and photospheric line characteristics. Stras
with Mg emission cores are very similar in their chromospheres,
while stars with Ca II cores vary greatly and exhibit more intense
emissions. The higher activity has been linked to magnetic forces which
produce spicules with diameters in the range of 1000 km. CES spectra
on the Ca II core H lines in Epsilon Eri and Alpha Cen B, active and
passive stars, respectively, show a 40 percent lower intensity in the
quiescnet star than in the active star, which has an asymmetric core
emission and a sharp central absorption with Ca IR triplet lines. The
emission features in the active stars are similar to those of the
active regions, photospheric spots, chromospheric plages and coronal
structures observed in the sun.
Title: Coordinated Multiband Observations of Stellar Flares
Authors: Rodono, M.; Foing, B. H.; Linsky, J. L.; Butler, J. C.;
Haisch, B. M.; Gary, D. E.; Gibson, D. M.
Bibcode: 1985Msngr..39....9R
Altcode:
The March 28, 1984 flare of AD Leo is characterized on the basis of
observations obtained over the spectral range from 200 nm to 20 cm using
the IUE, the VLA, and four ESO telescopes as part of a coordinated
multiband international campaign. The data are presented graphically
and discussed, with consideration of faint negative K-band events
observed simultaneously with the optical flare; an H-alpha precursor
with longer energy-release relaxation than in the U continuum; and
remarkably enhanced UV continuum, Mg II doublet, and 260-nm Fe II
blend during the last secondary optical peak.
Title: Chromospheric Modelling in Late-Type Dwarfs - Part One -
Quiescent Objects
Authors: Beckman, J.; Crivellari, L.; Foing, B.
Bibcode: 1984Msngr..38...24B
Altcode:
Attention is given to problems which arise when an attempt is made to
use observational material to clarify the mechanisms responsible for
the heating of the chromosphere in a late-type star, in order to derive
a clearer physical view of the nature of a chromosphere, its relation
to the underlying photosphere, and the overlying corona. Problems
arise in the prediction of line shapes by means of simple models,
in chromospheric inhomogeneities, in two-stream modeling, and in the
coexistence of two temperature structures. It is deemed necessary to
take the dominant role played by inhomogeneities into account, and to
ensure that any interstellar effects in the line profile data are well
and truly eliminated.
Title: Nova Sagittarii 1984
Authors: Foing, B. H.; McNaught, R.
Bibcode: 1984IAUC.4002....2F
Altcode: 1984IAUC.4002....0F
B. H. Foing, European Southern Observatory, telexes that image-tube
observations with the 1.5-m telescope and Boller and Chivens
spectrograph over 360-700 nm on Oct. 16.03 UT showed wide Balmer
emission lines and emissions of Fe II, N III and O III. Visual magnitude
estimates by R. McNaught, Coonabarabran, NSW: Oct. 10.45 UT, 13.1;
11.44, 13.2; 13.44, 13.5; 15.40, 13.5.
Title: Comet Austin (1984i)
Authors: Foing, B. H.
Bibcode: 1984IAUC.3964....3F
Altcode:
B. H. Foing, European Southern Observatory, reports: "We have observed
comet 1984i on July 25.97 (0.50-m reflector and Stromgren photometer)
and July 27.96 UT (1.5-m reflector and spectrograph covering the
range 500-730 nm). We find a central diffuse condensation of FWHM 25"
in the Stromgren channels. The C2 and NH2 spectral bands present a
similar extension. No solar-antisolar asymmetry is apparent; integrated
magnitude is equivalent to V = 6.3."
Title: Supernova in NGC 1559
Authors: Testor, G.; Foing, B. H.
Bibcode: 1984IAUC.3980....2T
Altcode: 1984IAUC.3980....0T
G. Testor and B. H. Foing, European Southern Observatory, report that
observations on Aug. 21.3 and 25.3 UT with the 1.5-m telescope (with
spectrograph and image-dissector scanner) showed a broad emission Fe II
band at 466 nm, a dip at 574 nm and an emission at H alpha, suggesting
that the supernova may be of type II (cf. IAUC 3967). The supernova
is very close to the center of the galaxy; there is a brighter object
in the field 10" west and 20" south of the galaxy's center.
Title: Coordinated IUE and ground-based observations of active stars:
flare events on YZ CMi, V1005 Ori, AD Leo and AR Lac.
Authors: Rodonò, M.; Cutispoto, G.; Catalano, S.; Linsky, J. L.;
Gibson, D. M.; Brown, A.; Haisch, B. M.; Butler, C. J.; Byrne, P. B.;
Andrews, A. D.; Doyle, J. G.; Gary, D. E.; Henry, G. W.; Russo, G.;
Vittone, A.; Scaltriti, F.; Foing, B.
Bibcode: 1984ESASP.218..247R
Altcode: 1984iue..conf..247R
Observations of stellar flares were obtained with IUE and ground-based
facilities simultaneously over a wide range of wavelengths in order
to study the effect of the flare radiation at different atmospheric
levels. Observations include time-resolved IUE and optical spectroscopy,
narrow and wide-band optical photometry, IR photometry, and microwave
observations. Results include detection of IR flux decrease, or negative
flare, in coincidence with flux increase at all other wavelengths.
Title: Characteristic structures of the solar disc observed on rocket
UV filtergrams
Authors: Foing, B.; Bonnet, R. M.
Bibcode: 1984A&A...136..133F
Altcode:
The high resolution ultraviolet filtergrams obtained with the Transition
Region Camera (a 10 cm aperture telescope equipped with broad-band
filters and a film cassette) have been statistically analyzed, using
two different methods of Fourier filtering (the Optical and the
Numerical Fourier Analysis) and autocorrelation of one-dimensional
scans of network and active disk areas. The statistical properties
and average dimensions of the structures characteristic of ultraviolet
solar filtergrams near temperature minimum are deduced. The dimensions
of the ultraviolet cell grains characteristic of the 160 nm pictures
are found to be of the order of 0.6 Mm (i.e., 0.9 arcsec with an
interdistance 1.4 Mm). The network and plage elements are brighter
and broader (about 1.0 Mm). An intermediate scale of about 8 Mm is
found in the cells which is discussed in terms of the velocity field
associated with the 3 min chromospheric oscillations. A scale of about
14 Mm is found in plage areas, which is related to the structure of
the network in active regions.
Title: On the origin of the discrete character of the solar disk
brightness in the 160 nanometer continuum
Authors: Foing, B.; Bonnet, R. M.
Bibcode: 1984ApJ...279..848F
Altcode:
The performance of the Transition Region Camera (TRC) is
evaluated with respect to spatial resolution in order to arrive
at a more refined description of the 160 nm features. The origins
of the ultraviolet-bright grains observed in the interior of the
supergranulation cells and of the bright elements that delineate the
network are investigated. It is believed that the network elements
and the cell grains have different origins. The network elements
may appear bright as a consequence of the Wilson effect at the top
of concentrated magnetic flux tubes. The magnetic field intensity
deduced on the assumption that the tubes are thermalized with their
surroundings is 120 G, which corresponds to an intensity of 1.5 kG at
the photospheric level. The cell grains cannot be of magnetic origin
because the magnetic field intensity they would require would be too
high. It is suggested that they are the trace of a local dissipation
of energy contained in periodic motions.
Title: Magnetic Flux Tubes and Local Heating in the Temperature
Minimum Region
Authors: Foing, B. H.; Bonnet, R. M.
Bibcode: 1984ssdp.conf..291F
Altcode:
The photometry and statistical analysis of 160 nm solar filtergrams
obtained by the Transition Region Camera, indicate that the solar
surface radiates at the temperature minimum a substantial portion
from features at the arcsec scale both in the network and inside
the supergranular cells. The authors investigate the origins of the
ultraviolet bright features in the cells and the network elements.
Title: The Transition Region Camera Experiment: High Resolution
Ultra-Violet Filtergrams of the Sun
Authors: Foing, B. H.; Bonnet, R. M.; Acton, L. W.; Brown, W. A.;
Bruner, M.; Decandim, M.
Bibcode: 1984ssdp.conf...99F
Altcode:
Three series of high resolution UV pictures of the Sun have been
obtained during the three flights of the Transition Region Camera
which took place on July 3, 1979, September 23, 1980 and July 13,
1982. These pictures reveal many new structures which were never
seen before on Ly alpha spectro-heliograms and on UV pictures of the
temperature minimum region. The scientific objectives, instrumentation,
flight conditions and preliminary results are described.
Title: Results from the transition region camera
Authors: Foing, B. H.; Bonnet, R. M.
Bibcode: 1984AdSpR...4h..43F
Altcode: 1984AdSpR...4...43F
Three series of high resolution ultra-violet pictures of the Sun
have been obtained during the three flights of rocket experiment
T.R.C. (Transition Region Camera) which took place on 3 July 1979,
23 September 1980 and 13 July 1982. These pictures reveal many
structures in Ly alpha and ultraviolet continua at 160 nm and 220
nm. The scientific objectives, instrumentation, flight conditions
and campaigns of simultaneous observations are described. The
contribution of T.R.C. to solar physics is discussed in the framework
of chromospheric multicomponent models, magnetic flux tubes, local
heating and periodic structures in the chromosphere.
Title: Magnetic flux tubes and local heating in the solar temperature
minimum region.
Authors: Foing, B. H.; Bonnet, R. M.; Bruner, M. E.; Acton, L. W.
Bibcode: 1983BAAS...15..620F
Altcode:
No abstract at ADS
Title: Rocket photographs of fine structure and wave patterns in
the solar temperature minimum
Authors: Bonnet, R. M.; Decaudin, M.; Foing, B.; Bruner, M.; Acton,
L. W.; Brown, W. A.
Bibcode: 1982A&A...111..125B
Altcode:
A new series of high resolution pictures of the sun has been obtained
during the second flight of the Transition Region Camera which occurred
on September 23, 1980. The qualitative analysis of the results indicates
that a substantial portion of the solar surface at the temperature
minimum radiates in non-magnetic regions and from features below 1
arcsec in size. Wave patterns are observed on the 160 nm temperature
minimum pictures. They are absent on the Lyman alpha pictures. Their
physical characteristics are compatible with those of gravitational
and acoustic waves generated by exploding granules.
Title: High Resolution UV Filtergrams of the Sun
Authors: Foing, B.; Bonnet, R. M.; Bruner, E. C.; Action, L. W.
Bibcode: 1981BAAS...13..911F
Altcode:
No abstract at ADS