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Author name code: mazzotta
ADS astronomy entries on 2022-09-14
author:"Mazzotta, Pasquale"
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Title: The Athena X-ray Integral Field Unit: a consolidated design
for the system requirement review of the preliminary definition phase
Authors: Barret, Didier; Albouys, Vincent; den Herder, Jan-Willem;
Piro, Luigi; Cappi, Massimo; Huovelin, Juhani; Kelley, Richard;
Mas-Hesse, J. Miguel; Paltani, Stéphane; Rauw, Gregor; Rozanska,
Agata; Svoboda, Jiri; Wilms, Joern; Yamasaki, Noriko; Audard, Marc;
Bandler, Simon; Barbera, Marco; Barcons, Xavier; Bozzo, Enrico;
Ceballos, Maria Teresa; Charles, Ivan; Costantini, Elisa; Dauser,
Thomas; Decourchelle, Anne; Duband, Lionel; Duval, Jean-Marc; Fiore,
Fabrizio; Gatti, Flavio; Goldwurm, Andrea; den Hartog, Roland; Jackson,
Brian; Jonker, Peter; Kilbourne, Caroline; Korpela, Seppo; Macculi,
Claudio; Mendez, Mariano; Mitsuda, Kazuhisa; Molendi, Silvano; Pajot,
François; Pointecouteau, Etienne; Porter, Frederick; Pratt, Gabriel
W.; Prêle, Damien; Ravera, Laurent; Sato, Kosuke; Schaye, Joop;
Shinozaki, Keisuke; Skup, Konrad; Soucek, Jan; Thibert, Tanguy; Vink,
Jacco; Webb, Natalie; Chaoul, Laurence; Raulin, Desi; Simionescu,
Aurora; Torrejon, Jose Miguel; Acero, Fabio; Branduardi-Raymont,
Graziella; Ettori, Stefano; Finoguenov, Alexis; Grosso, Nicolas;
Kaastra, Jelle; Mazzotta, Pasquale; Miller, Jon; Miniutti, Giovanni;
Nicastro, Fabrizio; Sciortino, Salvatore; Yamaguchi, Hiroya; Beaumont,
Sophie; Cucchetti, Edoardo; D'Andrea, Matteo; Eckart, Megan; Ferrando,
Philippe; Kammoun, Elias; Lotti, Simone; Mesnager, Jean-Michel;
Natalucci, Lorenzo; Peille, Philippe; de Plaa, Jelle; Ardellier,
Florence; Argan, Andrea; Bellouard, Elise; Carron, Jérôme; Cavazzuti,
Elisabetta; Fiorini, Mauro; Khosropanah, Pourya; Martin, Sylvain;
Perry, James; Pinsard, Frederic; Pradines, Alice; Rigano, Manuela;
Roelfsema, Peter; Schwander, Denis; Torrioli, Guido; Ullom, Joel; Vera,
Isabel; Medinaceli Villegas, Eduardo; Zuchniak, Monika; Brachet, Frank;
Lo Cicero, Ugo; Doriese, William; Durkin, Malcom; Fioretti, Valentina;
Geoffray, Hervé; Jacques, Lionel; Kirsch, Christian; Smith, Stephen;
Adams, Joseph; Gloaguen, Emilie; Hoogeveen, Ruud; van der Hulst, Paul;
Kiviranta, Mikko; van der Kuur, Jan; Ledot, Aurélien; van Leeuwen,
Bert-Joost; van Loon, Dennis; Lyautey, Bertrand; Parot, Yann; Sakai,
Kazuhiro; van Weers, Henk; Abdoelkariem, Shariefa; Adam, Thomas;
Adami, Christophe; Aicardi, Corinne; Akamatsu, Hiroki; Eleazar Merino
Alonso, Pablo; Amato, Roberta; André, Jérôme; Angelinelli, Matteo;
Anon-Cancela, Manuel; Anvar, Shebli; Atienza, Ricardo; Attard, Anthony;
Auricchio, Natalia; Balado, Ana; Bancel, Florian; Ferrari Barusso,
Lorenzo; Bernard, Vivian; Berrocal, Alicia; Blin, Sylvie; Bonino,
Donata; Bonnet, François; Bonny, Patrick; Boorman, Peter; Boreux,
Charles; Bounab, Ayoub; Boutelier, Martin; Boyce, Kevin; Brienza,
Daniele; Bruijn, Marcel; Bulgarelli, Andrea; Calarco, Simona; Callanan,
Paul; Camus, Thierry; Canourgues, Florent; Capobianco, Vito; Cardiel,
Nicolas; Castellani, Florent; Cheatom, Oscar; Chervenak, James;
Chiarello, Fabio; Clerc, Nicolas; Clerc, Laurent; Cobo, Beatriz;
Coeur-Joly, Odile; Coleiro, Alexis; Colonges, Stéphane; Corcione,
Leonardo; Coriat, Mickael; Coynel, Alexandre; Cuttaia, Francesco;
D'Ai, Antonino; D'anca, Fabio; Dadina, Mauro; Daniel, Christophe;
DeNigris, Natalie; Dercksen, Johannes; DiPirro, Michael; Doumayrou,
Eric; Dubbeldam, Luc; Dupieux, Michel; Dupourqué, Simon; Durand,
Jean Louis; Eckert, Dominique; Eiriz, Valvanera; Ercolani, Eric;
Etcheverry, Christophe; Finkbeiner, Fred; Fiocchi, Mariateresa;
Fossecave, Hervé; Franssen, Philippe; Frericks, Martin; Gabici,
Stefano; Gant, Florent; Gao, Jian-Rong; Gastaldello, Fabio; Genolet,
Ludovic; Ghizzardi, Simona; Alcacera Gil, M Angeles; Giovannini, Elisa;
Godet, Olivier; Gomez-Elvira, Javier; Gonzalez, Manuel; Gonzalez,
Raoul; Gottardi, Luciano; Granat, Dolorès; Gros, Michel; Guignard,
Nicolas; Hieltjes, Paul; Hurtado, Adolfo Jesus; Irwin, Kent; Jacquey,
Christian; Janiuk, Agnieszka; Jaubert, Jean; Jiménez, Maria; Jolly,
Antoine; Jourdan, Thierry; Julien, Sabine; Kedziora, Bartosz; Korb,
Andrew; Kreykenbohm, Ingo; König, Ole; Langer, Mathieu; Laudet,
Philippe; Laurent, Philippe; Laurenza, Monica; Lesrel, Jean; Ligori,
Sebastiano; Lorenz, Maximilian; Luminari, Alfredo; Maffei, Bruno;
Maisonnave, Océane; Marelli, Lorenzo; Massonet, Didier; Maussang,
Irwin; Gonzalo Melchor, Alejandro; Le Mer, Isabelle; Michalski,
Lea; Millerioux, Jean-Pierre; Mineo, Teresa; Minervini, Gabriele;
Molin, Alexeï; Monestes, David; Montinaro, Nicola; Mot, Baptiste;
Murat, David; Nagayoshi, Kenichiro; Nazé, Yaël; Noguès, Loïc;
Pailot, Damien; Panessa, Francesca; Parodi, Luigi; Petit, Pascal;
Piconcelli, Enrico; Pinto, Ciro; Encinas Plaza, Jose Miguel;
Poyatos, David; Prouvé, Thomas; Ptak, Andy; Puccetti, Simonetta;
Puccio, Elena; Ramon, Pascale; Reina, Manuel; Rioland, Guillaume;
Rodriguez, Louis; Roig, Anton; Rollet, Bertrand; Roncarelli, Mauro;
Roudil, Gilles; Rudnicki, Tomasz; Sanisidro, Julien; Sciortino, Luisa;
Silva, Vitor; Sordet, Michael; Soto-Aguilar, Javier; Spizzi, Pierre;
Surace, Christian; Fernández Sánchez, Miguel; Taralli, Emanuele;
Terrasa, Guilhem; Terrier, Régis; Todaro, Michela; Ubertini, Pietro;
Uslenghi, Michela; Geralt Bij de Vaate, Jan; Vaccaro, Davide; Varisco,
Salvatore; Varnière, Peggy; Vibert, Laurent; Vidriales, María;
Villa, Fabrizio; Vodopivec, Boris Martin; Volpe, Angela; de Vries,
Cor; Wakeham, Nicholas; Walmsley, Gavin; Wise, Michael; de Wit,
Martin; Woźniak, Grzegorz
2022arXiv220814562B Altcode:
The Athena X-ray Integral Unit (X-IFU) is the high resolution X-ray
spectrometer, studied since 2015 for flying in the mid-30s on the
Athena space X-ray Observatory, a versatile observatory designed to
address the Hot and Energetic Universe science theme, selected in
November 2013 by the Survey Science Committee. Based on a large format
array of Transition Edge Sensors (TES), it aims to provide spatially
resolved X-ray spectroscopy, with a spectral resolution of 2.5 eV (up
to 7 keV) over an hexagonal field of view of 5 arc minutes (equivalent
diameter). The X-IFU entered its System Requirement Review (SRR)
in June 2022, at about the same time when ESA called for an overall
X-IFU redesign (including the X-IFU cryostat and the cooling chain),
due to an unanticipated cost overrun of Athena. In this paper, after
illustrating the breakthrough capabilities of the X-IFU, we describe
the instrument as presented at its SRR, browsing through all the
subsystems and associated requirements. We then show the instrument
budgets, with a particular emphasis on the anticipated budgets of some
of its key performance parameters. Finally we briefly discuss on the
ongoing key technology demonstration activities, the calibration and the
activities foreseen in the X-IFU Instrument Science Center, and touch
on communication and outreach activities, the consortium organisation,
and finally on the life cycle assessment of X-IFU aiming at minimising
the environmental footprint, associated with the development of the
instrument. It is expected that thanks to the studies conducted so
far on X-IFU, along the design-to-cost exercise requested by ESA, the
X-IFU will maintain flagship capabilities in spatially resolved high
resolution X-ray spectroscopy, enabling most of the original X-IFU
related scientific objectives of the Athena mission to be retained
(abridged).
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Title: Feedback on radio galaxies: the cases of 3CR 318.1 and
3CR 196.1
Authors: Jimenez-Gallardo, Ana; Torresi, Eleonora; Forman, William;
Capetti, Alessandro; Sparks, Bill; Kraft, Ralph; Gilli, Roberto;
Roettgering, Huub; Liuzzo, Elisabetta; Mazzotta, Pasquale; Harwood,
Jeremy; Massaro, Francesco; Sani, Eleonora; Mazzucchelli, Chiara;
Balmaverde, Barbara; Venturi, Giacomo; Prieto, Almudena; Marconi,
Alessandro; Paggi, Alessandro; Gendron-Marsolais, Marie-Lou;
Peña-Herazo, Harold; Missaglia, Valentina; Mahatma, Vijay; Baldi,
Ranieri Diego; Tremblay, Grant; Wilkes, Belinda; Kuraszkiewicz,
Joanna; Miley, George; Ricci, Federica; Baum, Stefi; O'dea, Chris;
Lovisari, Lorenzo; van Weeren, Reinout
2022cosp...44.2328J Altcode:
Interactions between radio galaxies and their large-scale environments
are key factors to investigate the feedback processes responsible for
triggering and fuelling AGN activity. To improve our understanding of
such interactions, we carried out a multi-frequency analysis based on
the comparison between soft X-ray observations collected with Chandra
and optical datasets obtained thanks to VLT/MUSE for two radio galaxies
harbored in cool core clusters, namely: 3CR 318.1 and 3CR 196.1. These
sources are perfect examples of how radio galaxy activity can affect the
intracluster medium (ICM), showing different signatures of AGN feedback,
cold filaments, and X-ray cavities. 3CR 318.1 presents ionized gas
filaments associated with X-ray extended emission, while we observe
ionized gas spatially associated with an X-ray cavity in 3CR 196.1. The
origin of these ionized gas features remains disputed. Furthermore,
ionized gas associated with X-ray cavities has typically been seen
surrounding X-ray cavities in other radio galaxies harbored in galaxy
clusters, and not directly associated with the cavity, as is the case
for 3CR 196.1. Finally, I will also show preliminary results on the
optical-to-X-ray comparison for a selected sample of 3CR sources.
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Title: Cosmology with the SZ spectrum: Measuring the Universe's
temperature with galaxy clusters
Authors: Luzzi, Gemma; D'Angelo, Emanuele; Bourdin, Herve; De Luca,
Federico; Mazzotta, Pasquale; Oppizzi, Filippo; Polenta, Gianluca
2022EPJWC.25700028L Altcode: 2021arXiv211103427L
The hot gas in clusters of galaxies creates a distinctive spectral
distortion in the cosmic microwave background (CMB) via the
Sunyaev-Zel'dovich (SZ) effect. The spectral signature of the SZ
can be used to measure the CMB temperature at cluster redshift
(T<SUB>CMB</SUB>(z)) and to constrain the monopole of the y-type
spectral distortion of the CMB spectrum. In this work, we start
showing the measurements of T<SUB>CMB</SUB>(z) for a sample extracted
from the Second Catalog of galaxy clusters produced by Planck (PSZ2)
and containing 75 clusters selected from CHEX-MATE. Then we show the
forecasts for future CMB experiments about the constraints on the
monopole of the y-type spectral distortion of the CMB spectrum via
the spectrum of the SZ effect.
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Title: The Coma Cluster at LOFAR Frequencies. II. The Halo, Relic,
and a New Accretion Relic
Authors: Bonafede, A.; Brunetti, G.; Rudnick, L.; Vazza, F.;
Bourdin, H.; Giovannini, G.; Shimwell, T. W.; Zhang, X.; Mazzotta,
P.; Simionescu, A.; Biava, N.; Bonnassieux, E.; Brienza, M.; Brüggen,
M.; Rajpurohit, K.; Riseley, C. J.; Stuardi, C.; Feretti, L.; Tasse,
C.; Botteon, A.; Carretti, E.; Cassano, R.; Cuciti, V.; Gasperin,
F. de; Gastaldello, F.; Rossetti, M.; Rottgering, H. J. A.; Venturi,
T.; Weeren, R. J. van
2022ApJ...933..218B Altcode: 2022arXiv220301958B
We present LOw Frequency ARray observations of the Coma Cluster field at
144 MHz. The cluster hosts one of the most famous radio halos, a relic,
and a low surface brightness bridge. We detect new features that allow
us to make a step forward in the understanding of particle acceleration
in clusters. The radio halo extends for more than 2 Mpc, which is the
largest extent ever reported. To the northeast of the cluster, beyond
the Coma virial radius, we discover an arc-like radio source that could
trace particles accelerated by an accretion shock. To the west of the
halo, coincident with a shock detected in the X-rays, we confirm the
presence of a radio front, with different spectral properties with
respect to the rest of the halo. We detect a radial steepening of the
radio halo spectral index between 144 and 342 MHz, at ~30' from the
cluster center, that may indicate a non-constant re-acceleration time
throughout the volume. We also detect a mild steepening of the spectral
index toward the cluster center. For the first time, a radial change
in the slope of the radio-X-ray correlation is found, and we show that
such a change could indicate an increasing fraction of cosmic-ray versus
thermal energy density in the cluster outskirts. Finally, we investigate
the origin of the emission between the relic and the source NGC 4789,
and we argue that NGC 4789 could have crossed the shock originating
the radio emission visible between its tail and the relic.
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Title: Pressure profiles of distant Galaxy clusters with Planck-SPT
data
Authors: Oppizzi, Filippo; De Luca, Federico; Bourdin, Hervé;
Mazzotta, Pasquale; CHEX-MATE Collaboration
2022EPJWC.25700035O Altcode: 2021arXiv211102913O
We present a full set of numerical tools to extract Galaxy Cluster
pressure profiles from the joint analysis of Planck and South Pole
Telescope (SPT) observations. Pressure profiles are powerful tracers
of the thermodynamic properties and the internal structure of the
clusters. Tracing the pressure over the cosmic times allows one to
constraints the evolution of the cluster structure and the contribution
of astrophysical phenomena. SPT and Planck are complementary to
constrain the cluster structure at various spatial scales. The SPT
cluster catalogue counts 677 cluster candidates up to redshift 1.7,
it is a nearly mass-limited sample, an ideal benchmark to test cluster
evolution. We developed a pipeline to first separate the cluster signal
from the background and foreground components and then jointly fit a
parametric profile model on a combination of Planck and SPT data. We
validate our algorithm on a subsample of six clusters, common to the SPT
and the CHEX-MATE catalogues, comparing the results with the profiles
obtained from X-ray observations with XMM-Newton.
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Title: A Candle in the Wind: A Radio Filament in the Core of the
A3562 Galaxy Cluster
Authors: Giacintucci, S.; Venturi, T.; Markevitch, M.; Bourdin, H.;
Mazzotta, P.; Merluzzi, P.; Dallacasa, D.; Bardelli, S.; Sikhosana,
S. P.; Smirnov, O.; Bernardi, G.
2022ApJ...934...49G Altcode: 2022arXiv220606176G
Using a MeerKAT observation of the galaxy cluster A3562 (a member
of the Shapley supercluster), we have discovered a narrow, long and
straight, very faint radio filament, which branches out at a straight
angle from the tail of a radio galaxy located in projection near the
core of the cluster. The radio filament spans 200 kpc and aligns with
a sloshing cold front seen in the X-rays, staying inside the front
in projection. The radio spectral index along the filament appears
uniform (within large uncertainties) at α ≃ -1.5. We propose that
the radio galaxy is located outside the cold front but dips its tail
under the front. The tangential wind that blows there may stretch the
radio plasma from the radio galaxy into a filamentary structure. Some
reacceleration is needed in this scenario to keep the radio spectrum
uniform. Alternatively, the cosmic-ray electrons from that spot in the
tail can spread along the cluster magnetic field lines, straightened by
that same tangential flow, via anomalously fast diffusion. Our radio
filament can provide constraints on this process. We also uncover
a compact radio source at the brightest cluster galaxy that is 2-3
orders of magnitude less luminous than those in typical cluster central
galaxies-probably an example of a brightest cluster galaxy starved of
accretion fuel by gas sloshing.
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Title: CHEX-MATE: Morphological analysis of the sample
Authors: Campitiello, Maria Giulia; Ettori, Stefano; Lovisari, Lorenzo;
Bartalucci, Iacopo; Eckert, Dominique; Rasia, Elena; Rossetti,
Mariachiara; Gastaldello, Fabio; Pratt, Gabriel W.; Maughan, Ben;
Pointecouteau, Etienne; Sereno, Mauro; Biffi, Veronica; Borgani,
Stefano; De Luca, Federico; De Petris, Marco; Gaspari, Massimo;
Ghizzardi, Simona; Mazzotta, Pasquale; Molendi, Silvano
2022arXiv220511326C Altcode: 2022arXiv220511326G
In this work, we performed an analysis of the X-ray morphology of the
118 CHEX-MATE (Cluster HEritage project with XMM-Newton - Mass Assembly
and Thermodynamics at the Endpoint of structure formation) galaxy
clusters, with the aim to provide a classification of their dynamical
state. To investigate the link between the X-ray appearance and the
dynamical state, we considered four morphological parameters: the
surface brightness concentration, the centroid shift, and the second-
and third-order power ratios. These indicators result to be: strongly
correlated with each other, powerful in identifying the disturbed and
relaxed population, characterised by a unimodal distribution and not
strongly influenced by systematic uncertainties. In order to obtain a
continuous classification of the CHEX-MATE objects, we combined these
four parameters in a single quantity, M, which represents the grade of
relaxation of a system. On the basis of the M value, we identified the
most extreme systems of the sample, finding 15 very relaxed and 27 very
disturbed galaxy clusters. From a comparison with previous analysis
on X-ray selected samples, we confirmed that the Sunyaev-Zeldovich
(SZ) clusters tend to be more disturbed. Finally, by applying our
analysis on a simulated sample, we found a general agreement between
the observed and simulated results, with the only exception of the
concentration. This latter behaviour, is partially related to the
presence of particles with high smoothed-particle hydrodynamics density
in the central regions of the simulated clusters due to the action of
the idealised isotropic thermal Active Galactic Nuclei (AGN) feedback.
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Title: Radio footprints of a minor merger in the Shapley Supercluster:
From supercluster down to galactic scales
Authors: Venturi, T.; Giacintucci, S.; Merluzzi, P.; Bardelli, S.;
Busarello, G.; Dallacasa, D.; Sikhosana, S. P.; Marvil, J.; Smirnov,
O.; Bourdin, H.; Mazzotta, P.; Rossetti, M.; Rudnick, L.; Bernardi, G.;
Brüggen, M.; Carretti, E.; Cassano, R.; Di Gennaro, G.; Gastaldello,
F.; Kale, R.; Knowles, K.; Koribalski, B. S.; Heywood, I.; Hopkins,
A. M.; Norris, R. P.; Reiprich, T. H.; Tasse, C.; Vernstrom, T.;
Zucca, E.; Bester, L. H.; Diego, J. M.; Kanapathippillai, J.
2022A&A...660A..81V Altcode: 2022arXiv220104887V
Context. The Shapley Supercluster (⟨z⟩≈0.048) contains several
tens of gravitationally bound clusters and groups, making it an ideal
subject for radio studies of cluster mergers. <BR /> Aims: We used new
high sensitivity radio observations to investigate the less energetic
events of mass assembly in the Shapley Supercluster from supercluster
down to galactic scales. <BR /> Methods: We created total intensity
images of the full region between A3558 and A3562, from ∼230 to
∼1650 MHz, using ASKAP, MeerKAT and the GMRT, with sensitivities
ranging from ∼6 to ∼100 μJy beam<SUP>−1</SUP>. We performed
a detailed morphological and spectral study of the extended emission
features, complemented with ESO-VST optical imaging and X-ray data from
XMM-Newton. <BR /> Results: We report the first GHz frequency detection
of extremely low brightness intercluster diffuse emission on a ∼1 Mpc
scale connecting a cluster and a group, namely: A3562 and the group
SC 1329-313. It is morphologically similar to the X-ray emission in
the region. We also found (1) a radio tail generated by ram pressure
stripping in the galaxy SOS 61086 in SC 1329-313; (2) a head-tail
radio galaxy, whose tail is broken and culminates in a misaligned bar;
(3) ultrasteep diffuse emission at the centre of A3558. Finally (4), we
confirm the ultra-steep spectrum nature of the radio halo in A3562. <BR
/> Conclusions: Our study strongly supports the scenario of a flyby
of SC 1329-313 north of A3562 into the supercluster core. This event
perturbed the centre of A3562, leaving traces of this interaction in
the form of turbulence between A3562 and SC 1329-313, at the origin of
the radio bridge and eventually affecting the evolution of individual
supercluster galaxies by triggering ram pressure stripping. Our work
shows that minor mergers can be spectacular and have the potential to
generate diffuse radio emission that carries important information on
the formation of large-scale structures in the Universe.
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Title: The ultra-steep diffuse radio emission observed in the
cool-core cluster RX J1720.1+2638 with LOFAR at 54 MHz
Authors: Biava, N.; de Gasperin, F.; Bonafede, A.; Edler, H. W.;
Giacintucci, S.; Mazzotta, P.; Brunetti, G.; Botteon, A.; Brüggen,
M.; Cassano, R.; Drabent, A.; Edge, A. C.; Enßlin, T.; Gastaldello,
F.; Riseley, C. J.; Rossetti, M.; Rottgering, H. J. A.; Shimwell,
T. W.; Tasse, C.; van Weeren, R. J.
2021MNRAS.508.3995B Altcode: 2021arXiv211001629B; 2021MNRAS.tmp.2533B
Diffuse radio emission at the centre of galaxy clusters has been
observed both in merging clusters on scales of Mpc, called giant radio
haloes, and in relaxed systems with a cool-core on smaller scales,
named mini haloes. Giant radio haloes and mini haloes are thought to
be distinct classes of sources. However, recent observations have
revealed the presence of diffuse radio emission on Mpc scales in
clusters that do not show strong dynamical activity. RX J1720.1+2638
is a cool-core cluster, presenting both a bright central mini halo
and a fainter diffuse, steep-spectrum emission extending beyond the
cluster core that resembles giant radio halo emission. In this paper,
we present new observations performed with the LOw Frequency ARray
Low Band Antennas (LBA) at 54 MHz. These observations, combined
with data at higher frequencies, allow us to constrain the spectral
properties of the radio emission. The large-scale emission presents
an ultrasteep spectrum with $\alpha _{54}^{144}\sim 3.2$. The radio
emission inside and outside the cluster core have strictly different
properties, as there is a net change in spectral index and they follow
different radio-X-ray surface brightness correlations. We argue that the
large-scale diffuse emission is generated by particles re-acceleration
after a minor merger. While for the central mini halo, we suggest
that it could be generated by secondary electrons and positrons from
hadronic interactions of relativistic nuclei with the dense cool-core
gas, as an alternative to re-acceleration models.
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Title: The Cluster HEritage project with XMM-Newton: Mass Assembly and
Thermodynamics at the Endpoint of structure formation. I. Programme
overview
Authors: CHEX-MATE Collaboration; Arnaud, M.; Ettori, S.; Pratt,
G. W.; Rossetti, M.; Eckert, D.; Gastaldello, F.; Gavazzi, R.; Kay,
S. T.; Lovisari, L.; Maughan, B. J.; Pointecouteau, E.; Sereno, M.;
Bartalucci, I.; Bonafede, A.; Bourdin, H.; Cassano, R.; Duffy, R. T.;
Iqbal, A.; Maurogordato, S.; Rasia, E.; Sayers, J.; Andrade-Santos,
F.; Aussel, H.; Barnes, D. J.; Barrena, R.; Borgani, S.; Burkutean,
S.; Clerc, N.; Corasaniti, P. -S.; Cuillandre, J. -C.; De Grandi, S.;
De Petris, M.; Dolag, K.; Donahue, M.; Ferragamo, A.; Gaspari, M.;
Ghizzardi, S.; Gitti, M.; Haines, C. P.; Jauzac, M.; Johnston-Hollitt,
M.; Jones, C.; Kéruzoré, F.; Le Brun, A. M. C.; Mayet, F.; Mazzotta,
P.; Melin, J. -B.; Molendi, S.; Nonino, M.; Okabe, N.; Paltani, S.;
Perotto, L.; Pires, S.; Radovich, M.; Rubino-Martin, J. -A.; Salvati,
L.; Saro, A.; Sartoris, B.; Schellenberger, G.; Streblyanska, A.;
Tarrío, P.; Tozzi, P.; Umetsu, K.; van der Burg, R. F. J.; Vazza,
F.; Venturi, T.; Yepes, G.; Zarattini, S.
2021A&A...650A.104C Altcode: 2020arXiv201011972T
The Cluster HEritage project with XMM-Newton - Mass Assembly and
Thermodynamics at the Endpoint of structure formation (CHEX-MATE)
is a three-mega-second Multi-Year Heritage Programme to obtain X-ray
observations of a minimally-biased, signal-to-noise-limited sample of
118 galaxy clusters detected by Planck through the Sunyaev-Zeldovich
effect. The programme, described in detail in this paper, aims to study
the ultimate products of structure formation in time and mass. It
is composed of a census of the most recent objects to have formed
(Tier-1: 0.05 < z < 0.2; 2 × 10<SUP>14</SUP> M<SUB>⊙</SUB>
< M<SUB>500</SUB> < 9 × 10<SUP>14</SUP> M<SUB>⊙</SUB>),
together with a sample of the highest mass objects in the Universe
(Tier-2: z < 0.6; M<SUB>500</SUB> > 7.25 × 10<SUP>14</SUP>
M<SUB>⊙</SUB>). The programme will yield an accurate vision of the
statistical properties of the underlying population, measure how the gas
properties are shaped by collapse into the dark matter halo, uncover
the provenance of non-gravitational heating, and resolve the major
uncertainties in mass determination that limit the use of clusters for
cosmological parameter estimation. We will acquire X-ray exposures of
uniform depth, designed to obtain individual mass measurements accurate
to 15 − 20% under the hydrostatic assumption. We present the project
motivations, describe the programme definition, and detail the ongoing
multi-wavelength observational (lensing, SZ, radio) and theoretical
effort that is being deployed in support of the project.
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Title: Chandra Observations of the Planck Early Sunyaev-Zeldovich
Sample: A Reexamination of Masses and Mass Proxies
Authors: Andrade-Santos, Felipe; Pratt, Gabriel W.; Melin,
Jean-Baptiste; Arnaud, Monique; Jones, Christine; Forman, William
R.; Pointecouteau, Etienne; Bartalucci, Iacopo; Vikhlinin, Alexey;
Murray, Stephen S.; Mazzotta, Pasquale; Borgani, Stefano; Lovisari,
Lorenzo; van Weeren, Reinout J.; Kraft, Ralph P.; David, Laurence P.;
Giacintucci, Simona
2021ApJ...914...58A Altcode: 2021arXiv210307545A
Using Chandra observations, we derive the Y<SUB>X</SUB> proxy and
associated total mass measurement, ${M}_{500}^{{Y}_{{\rm{X}}}}$ , for
147 clusters with z < 0.35 from the Planck early Sunyaev-Zeldovich
catalog, and for 80 clusters with z < 0.22 from an X-ray flux-limited
sample. We reextract the Planck Y<SUB>SZ</SUB> measurements and obtain
the corresponding mass proxy, ${M}_{500}^{\mathrm{SZ}}$ , from the full
Planck mission maps, minimizing Malmquist bias due to observational
scatter. The masses reextracted using the more precise X-ray position
and characteristic size agree with the published PSZ2 values, but
yield a significant reduction in the scatter (by a factor of two)
in the ${M}_{500}^{\mathrm{SZ}}$ - ${M}_{500}^{{Y}_{{\rm{X}}}}$
relation. The slope is 0.93 ± 0.03, and the median ratio,
${M}_{500}^{\mathrm{SZ}}/{M}_{500}^{{Y}_{{\rm{X}}}}=0.91\pm
0.01$ , is within the expectations from known X-ray calibration
systematics. Y<SUB>SZ</SUB>/Y<SUB>X</SUB> is 0.88 ± 0.02,
in good agreement with predictions from cluster structure, and
implying a low level of clumpiness. In agreement with the findings
of the Planck Collaboration, the slope of the Y<SUB>SZ</SUB>-
${D}_{{\rm{A}}}^{-2}{Y}_{{\rm{X}}}$ flux relation is significantly
less than unity (0.89 ± 0.01). Using extensive simulations, we show
that this result is not due to selection effects, intrinsic scatter,
or covariance between quantities. We demonstrate analytically that
changing the Y<SUB>SZ</SUB>-Y<SUB>X</SUB> relation from apparent flux to
intrinsic properties results in a best-fit slope that is closer to unity
and increases the dispersion about the relation. The redistribution
resulting from this transformation implies that the best-fit parameters
of the ${M}_{500}^{\mathrm{SZ}}$ - ${M}_{500}^{{Y}_{{\rm{X}}}}$
relation will be sample-dependent.
---------------------------------------------------------
Title: Raining in MKW 3 s: A Chandra-MUSE Analysis of X-Ray Cold
Filaments around 3CR 318.1
Authors: Jimenez-Gallardo, A.; Massaro, F.; Balmaverde, B.; Paggi,
A.; Capetti, A.; Forman, W. R.; Kraft, R. P.; Baldi, R. D.; Mahatma,
V. H.; Mazzucchelli, C.; Missaglia, V.; Ricci, F.; Venturi, G.; Baum,
S. A.; Liuzzo, E.; O'Dea, C. P.; Prieto, M. A.; Röttgering, H. J. A.;
Sani, E.; Sparks, W. B.; Tremblay, G. R.; van Weeren, R. J.; Wilkes,
B. J.; Harwood, J. J.; Mazzotta, P.; Kuraszkiewicz, J.
2021ApJ...912L..25J Altcode: 2021arXiv210407677J
We present the analysis of X-ray and optical observations of gas
filaments observed in the radio source 3CR 318.1, associated with
NGC 5920, the brightest cluster galaxy (BCG) of MKW 3 s, a nearby
cool core galaxy cluster. This work is one of the first X-ray and
optical analyses of filaments in cool core clusters carried out
using MUSE observations. We aim at identifying the main excitation
processes responsible for the emission arising from these filaments. We
complemented the optical VLT/MUSE observations, tracing the colder gas
phase, with X-ray Chandra observations of the hotter highly ionized
gas phase. Using the MUSE observations, we studied the emission
line intensity ratios along the filaments to constrain the physical
processes driving the excitation, and, using the Chandra observations,
we carried out a spectral analysis of the gas along these filaments. We
found a spatial association between the X-ray and optical morphology
of these filaments, which are colder and have lower metal abundance
than the surrounding intracluster medium (ICM), as already seen in
other BCGs. Comparing with previous results from the literature for
other BCGs, we propose that the excitation process that is most likely
responsible for these filaments emission is a combination of star
formation and shocks, with a likely contribution from self-ionizing,
cooling ICM. Additionally, we conclude that the filaments most likely
originated from AGN-driven outflows in the direction of the radio jet.
---------------------------------------------------------
Title: Multiple AGN activity during the BCG assembly of
XDCPJ0044.0-2033 at z ∼ 1.6
Authors: Travascio, A.; Bongiorno, A.; Tozzi, P.; Fassbender, R.;
De Gasperin, F.; Cardone, V. F.; Zappacosta, L.; Vietri, G.; Merlin,
E.; Bischetti, M.; Piconcelli, E.; Duras, F.; Fiore, F.; Menci, N.;
Mazzotta, P.; Nastasi, A.
2020MNRAS.498.2719T Altcode: 2020arXiv200811132T
Undisturbed galaxy clusters are characterized by a massive and large
elliptical galaxy at their centre, i.e. the brightest cluster galaxy
(BCG). How these central galaxies form is still debated. According to
most models, a typical epoch for their assembly is $z$ ∼ 1-2. We have
performed a detailed multiwavelength analysis of the core of XMM-Newton
Distant Cluster Project (XDCP) J0044.0-2033 (XDCP0044), one of the
most massive and densest galaxy clusters currently known at redshift
$z$ ∼ 1.6, whose central galaxy population shows high star formation
compared to lower z clusters and an X-ray active galactic nuclei (AGN)
located close to its centre. SINFONI J-, H-, and KMOS YJ-, H-bands
spectroscopic data have been analysed, together with deep archival
HST photometric data in F105W, F140W, and F160W bands, Chandra X-ray,
radio JVLA data at 1-2 GHz, and ALMA band-6 observations. In the very
central region of the cluster (∼70 kpc × 70 kpc), two systems of
interacting galaxies have been identified and studied (Complex A and
B), with a total of seven confirmed cluster members. These galaxies
show perturbed morphologies and three of them show signs of AGN
activity. In particular, two type-1 AGN with typical broad lines have
been found at the centre of each complex (both of them X-ray obscured
and highly accreting with $\rm \lambda _{Edd}\sim 0.4-0.6$ ), while a
type-2 AGN has been discovered in Complex A. The AGN at the centre of
Complex B is also detected in X-ray, while the other two are spatially
related to radio emission. The three AGN provide one of the closest AGN
triple at $z$ > 1 revealed so far with a minimum (maximum) projected
distance of 10 (40) kpc. The observation of high star formation, merger
signatures, and nuclear activity in the core of XDCP0044 suggests
that all these processes are key ingredients in shaping the nascent
BCG. According to our data, XDCP0044 could form a typical massive
galaxy of $M_{\star }\sim 10^{12} \, \mathrm{M}_{\odot }$ , hosting
a black hole of $\rm 2 \times 10^8\!-\!10^9 \, \mathrm{M}_{\odot }$
, in a time-scale of the order of ∼2.5 Gyr.
---------------------------------------------------------
Title: Extracting the thermal SZ signal from heterogeneous millimeter
data sets
Authors: Bourdin, H.; Baldi, A. S.; Kozmanyan, A.; Mazzotta, P.
2020EPJWC.22800007B Altcode:
Complementarily to X-ray observations, the thermal SZ effect is a
powerful tool to probe the baryonic content of galaxy clusters from
their core to their peripheries. While contaminations by astrophysical
and instrumental backgrounds require us to scan the thermal SZ
signal across various frequencies, the multi-scale nature of cluster
morphologies require us to observe such objects at various angular
resolutions. We developed component separation algorithms that take
advantage of sparse representations to combine these heterogeneous
pieces of information, separate the thermal SZ signal from its
contaminants, detect and map the thermal SZ signal of galaxy clusters
from nearby to more distant clusters of the Planck catalogue. Spatially
weighted likelihoods allow us in particular to connect parametric
fittings of the component Spectral Energy Distribution with wavelet and
curvelet imaging, but also to combine signals registered with beams of
various width. Such techniques already allow us to detect sub-structures
in the peripheries of nearby clusters with Planck, and could be extended
to observations performed at higher angular resolutions.
---------------------------------------------------------
Title: Optical validation and characterisation of Planck PSZ1
sources at the Canary Islands observatories. II. Second year of
ITP13 observations
Authors: Barrena, R.; Ferragamo, A.; Rubiño-Martín, J. A.;
Streblyanska, A.; Aguado-Barahona, A.; Tramonte, D.; Génova-Santos,
R. T.; Hempel, A.; Lietzen, H.; Aghanim, N.; Arnaud, M.; Böhringer,
H.; Chon, G.; Dahle, H.; Douspis, M.; Lasenby, A. N.; Mazzotta, P.;
Melin, J. B.; Pointecouteau, E.; Pratt, G. W.; Rossetti, M.
2020A&A...638A.146B Altcode: 2020arXiv200407913B
We report new galaxy clusters previously unknown included in the
first Planck Sunyaev-Zeldovich (SZ) sources catalogue, the PSZ1. The
results presented here were achieved during the second year of a
two-year observational programme, the ITP13, developed at the Roque
de los Muchachos Observatory (La Palma, Spain). Using the 2.5 m Isaac
Newton telescope, the 3.5 m Telescopio Nazionale Galileo, the 4.2 m
William Herschel telescope and the 10.4 m Gran Telescopio Canarias
we characterised 75 SZ sources with low SZ significance, SZ S/N <
5.32. We performed deep optical imaging and spectroscopy in order
to associate actual galaxy clusters with the SZ Planck source. We
adopted robust criteria, based on the 2D spatial distribution,
richness, and velocity dispersions to confirm actual optical
counterparts up to z < 0.85. The selected systems are confirmed
only if they are well aligned with respect to the PSZ1 coordinate
and show high richness and high velocity dispersion. In addition,
we also inspected the Compton y-maps and SZ significance in order
to identify unrealistic detections. Following this procedure, we
identify 26 cluster counterparts associated with the SZ emission,
which means that only about 35% of the clusters considered in this
low S/N PSZ1 subsample are validated. Forty-nine SZ sources (∼65%
of this PSZ1 subset) remain unconfirmed. At the end of the ITP13
observational programme, we have studied 256 SZ sources with Dec ≥
-15° (212 of them completely unknown), finding optical counterparts
for 152 SZ sources. The ITP13 validation programme has allowed us to
update the PSZ1 purity, which is now more refined, increasing from
72% to 83% in the low SZ S/N regime. Our results are consistent with
the predicted purity curve for the full PSZ1 catalogue and with the
expected fraction of false detections caused by the non-Gaussian noise
of foreground signals. We find a strong correlation between the number
of unconfirmed sources and the thermal emission of diffuse galactic
dust at 857 GHz, thus increasing the fraction of false Planck SZ
detections at low galactic latitudes.
---------------------------------------------------------
Title: Spectral imaging of X-COP galaxy clusters with the
Sunyaev-Zel'dovich effect
Authors: Baldi, Anna Silvia; Bourdin, Hervé; Mazzotta, Pasquale
2020EPJWC.22800004B Altcode: 2019arXiv191103206B
The Sunyaev-Zel'dovich effect is the ideal probe for investigating the
outskirts of galaxy clusters. To map this signal, we apply a spectral
imaging technique which combines parametric component separation
and sparse representations. Our procedure is an improved version
of an existing algorithm, which now features a better treatment of
astrophysical contaminants, and the implementation of a new beam
deconvolution. We use the most recent frequency maps delivered by
Planck, and we consider the clusters analysed in the XMM Cluster
Outskirts Project (X-COP). In particular, we focus on the images of two
clusters which may be possibly interacting with neighbouring objects,
namely A2029 and RXCJ1825. We also highlight the advantages of the
new beam deconvolution method, through a comparison with the original
version of the imaging algorithm.
---------------------------------------------------------
Title: Spectral imaging of the thermal Sunyaev-Zel'dovich effect in
X-COP galaxy clusters: method and validation
Authors: Baldi, A. S.; Bourdin, H.; Mazzotta, P.; Eckert, D.; Ettori,
S.; Gaspari, M.; Roncarelli, M.
2019A&A...630A.121B Altcode: 2019arXiv190610013B
The imaging of galaxy clusters through the Sunyaev-Zel'dovich effect is
a valuable tool to probe the thermal pressure of the intra-cluster gas,
especially in the outermost regions where X-ray observations suffer
from photon statistics. For the first time, we produce maps of the
Comptonization parameter by applying a locally parametric algorithm for
sparse component separation to the latest frequency maps released by
Planck. The algorithm takes into account properties of real cluster data
through the two-component modelling of the spectral energy density of
thermal dust, and the masking of bright point sources. Its robustness
has been improved in the low signal-to-noise regime, thanks to the
implementation of a deconvolution of Planck beams in the chi-square
minimisation of each wavelet coefficient. We applied this procedure to
twelve low-redshift galaxy clusters detected by Planck with the highest
signal-to-noise ratio, considered in the XMM Cluster Oustkirts Project
(X-COP). Our images show the presence of anisotropic features, such
as small-scale blobs and filamentary substructures that are located in
the outskirts of a number of clusters in the sample. The significance
of their detection is established via a bootstrap-based procedure we
propose here for the first time. In particular, we present a qualitative
comparison with X-ray data for two interesting systems, namely A2029
and RXCJ1825. Our results are in agreement with the features detected
in the outskirts of the clusters in the two bands.
---------------------------------------------------------
Title: Detection of anti-correlation of hot and cold baryons in
galaxy clusters
Authors: Farahi, Arya; Mulroy, Sarah L.; Evrard, August E.; Smith,
Graham P.; Finoguenov, Alexis; Bourdin, Hervé; Carlstrom, John E.;
Haines, Chris P.; Marrone, Daniel P.; Martino, Rossella; Mazzotta,
Pasquale; O'Donnell, Christine; Okabe, Nobuhiro
2019NatCo..10.2504F Altcode: 2019arXiv190702502F
The largest clusters of galaxies in the Universe contain vast amounts of
dark matter, plus baryonic matter in two principal phases, a majority
hot gas component and a minority cold stellar phase comprising stars,
compact objects, and low-temperature gas. Hydrodynamic simulations
indicate that the highest-mass systems retain the cosmic fraction of
baryons, a natural consequence of which is anti-correlation between
the masses of hot gas and stars within dark matter halos of fixed total
mass. We report observational detection of this anti-correlation based
on 4 elements of a 9 × 9-element covariance matrix for nine cluster
properties, measured from multi-wavelength observations of 41 clusters
from the Local Cluster Substructure Survey. These clusters were selected
using explicit and quantitative selection rules that were then encoded
in our hierarchical Bayesian model. Our detection of anti-correlation is
consistent with predictions from contemporary hydrodynamic cosmological
simulations that were not tuned to reproduce this signal.
---------------------------------------------------------
Title: LoCuSS: scaling relations between galaxy cluster mass, gas,
and stellar content
Authors: Mulroy, Sarah L.; Farahi, Arya; Evrard, August E.; Smith,
Graham P.; Finoguenov, Alexis; O'Donnell, Christine; Marrone, Daniel
P.; Abdulla, Zubair; Bourdin, Hervé; Carlstrom, John E.; Démoclès,
Jessica; Haines, Chris P.; Martino, Rossella; Mazzotta, Pasquale;
McGee, Sean L.; Okabe, Nobuhiro
2019MNRAS.484...60M Altcode: 2019MNRAS.tmp....5M; 2019arXiv190111276M
We present a simultaneous analysis of galaxy cluster scaling relations
between weak-lensing mass and multiple cluster observables, across a
wide range of wavelengths, that probe both gas and stellar content. Our
new hierarchical Bayesian model simultaneously considers the selection
variable alongside all other observables in order to explicitly model
intrinsic property covariance and account for selection effects. We
apply this method to a sample of 41 clusters at 0.15 < z <
0.30, with a well-defined selection criteria based on RASS X-ray
luminosity, and observations from Chandra/XMM, SZA, Planck, UKIRT,
SDSS, and Subaru. These clusters have well-constrained weak-lensing
mass measurements based on Subaru/Suprime-Cam observations, which serve
as the reference masses in our model. We present 30 scaling relation
parameters for 10 properties. All relations probing the intracluster
gas are slightly shallower than self-similar predictions, in moderate
tension with prior measurements, and the stellar fraction decreases
with mass. K-band luminosity has the lowest intrinsic scatter with a
95th percentile of 0.16, while the lowest scatter gas probe is gas
mass with a fractional intrinsic scatter of 0.16 ± 0.03. We find
no distinction between the core-excised X-ray or high-resolution
Sunyaev-Zel'dovich relations of clusters of different central entropy,
but find with modest significance that higher entropy clusters have
higher stellar fractions than their lower entropy counterparts. We
also report posterior mass estimates from our likelihood model.
---------------------------------------------------------
Title: Universal thermodynamic properties of the intracluster medium
over two decades in radius in the X-COP sample
Authors: Ghirardini, V.; Eckert, D.; Ettori, S.; Pointecouteau, E.;
Molendi, S.; Gaspari, M.; Rossetti, M.; De Grandi, S.; Roncarelli,
M.; Bourdin, H.; Mazzotta, P.; Rasia, E.; Vazza, F.
2019A&A...621A..41G Altcode: 2018arXiv180500042G
Context. The hot plasma in a galaxy cluster is expected to be heated
to high temperatures through shocks and adiabatic compression. The
thermodynamical properties of the gas encode information on the
processes leading to the thermalization of the gas in the cluster's
potential well and on non-gravitational processes such as gas cooling,
AGN feedback, shocks, turbulence, bulk motions, cosmic rays and magnetic
field. <BR /> Aims: In this work we present the radial profiles of
the thermodynamic properties of the intracluster medium (ICM) out to
the virial radius for a sample of 12 galaxy clusters selected from
the Planck all-sky survey. We determine the universal profiles of gas
density, temperature, pressure, and entropy over more than two decades
in radius, from 0.01R<SUB>500</SUB> to 2R<SUB>500</SUB>. <BR /> Methods:
We exploited X-ray information from XMM-Newton and Sunyaev-Zel'dovich
constraints from Planck to recover thermodynamic properties out to
2R<SUB>500</SUB>. We provide average functional forms for the radial
dependence of the main quantities and quantify the slope and intrinsic
scatter of the population as a function of radius. <BR /> Results:
We find that gas density and pressure profiles steepen steadily
with radius, in excellent agreement with previous observational
results. Entropy profiles beyond R<SUB>500</SUB> closely follow the
predictions for the gravitational collapse of structures. The scatter
in all thermodynamical quantities reaches a minimum in the range [0.2 -
0.8]R<SUB>500</SUB> and increases outward. Somewhat surprisingly, we
find that pressure is substantially more scattered than temperature and
density. <BR /> Conclusions: Our results indicate that once accreting
substructures are properly excised, the properties of the ICM beyond
the cooling region (R > 0.3R<SUB>500</SUB>) follow remarkably
well the predictions of simple gravitational collapse and require few
non-gravitational corrections.
---------------------------------------------------------
Title: Deriving the Hubble constant using Planck and XMM-Newton
observations of galaxy clusters
Authors: Kozmanyan, Arpine; Bourdin, Hervé; Mazzotta, Pasquale;
Rasia, Elena; Sereno, Mauro
2019A&A...621A..34K Altcode: 2018arXiv180909560K
The possibility of determining the value of the Hubble constant using
observations of galaxy clusters in X-ray and microwave wavelengths
through the Sunyaev Zel'dovich (SZ) effect has long been known. Previous
measurements have been plagued by relatively large errors in the
observational data and severe biases induced, for example, by cluster
triaxiality and clumpiness. The advent of Planck allows us to map the
Compton parameter y, that is, the amplitude of the SZ effect, with
unprecedented accuracy at intermediate cluster-centric radii, which in
turn allows performing a detailed spatially resolved comparison with
X-ray measurements. Given such higher quality observational data,
we developed a Bayesian approach that combines informed priors on
the physics of the intracluster medium obtained from hydrodynamical
simulations of massive clusters with measurement uncertainties. We
applied our method to a sample of 61 galaxy clusters with redshifts up
to z < 0.5 observed with Planck and XMM-Newton and find H<SUB>0</SUB>
= 67 ± 3 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP>.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Clusters candidates from PSZ1
catalogue (Barrena+, 2018)
Authors: Barrena, R.; Streblyanska, A.; Ferragamo, A.; Rubino-Martin,
J. A.; Aguado-Barahona, A.; Tramonte, D.; Genova-Santos, R. T.; Hempel,
A.; Lietzen, H.; Aghanim, N.; Arnaud, M.; Bohringer, H.; Chon, G.;
Democles, J.; Dahle, H.; Douspis, M.; Lasenby, A. N.; Mazzotta, P.;
Melin, J. B.; Pointecouteau, E.; Pratt, G. W.; Rossetti, M.; van der
Burg, R. F. J.
2018yCat..36160042B Altcode:
Our reference cluster sample is PSZ1 (Planck Collaboration XXIX,
2014A&A...571A..29P, Cat. VIII/91; Planck Collaboration XXXII,
2015, Cat. J/A+A/581/A14). This catalogue includes 1227 clusters and
cluster candidates derived from SZ effect detections using all-sky maps
produced within the first 15.5 months of Planck observations. <P />All
observations were carried out at Roque de los Muchachos Observatory
(ORM) on the island of La Palma (Spain) within the framework of the
International Time Programme ITP13B-15A. The dataset was obtained in
multiple runs from August 2013 to July 2014, as part of this two-year
observing programme. <P />(1 data file).
---------------------------------------------------------
Title: Optical validation and characterization of Planck PSZ1
sources at the Canary Islands observatories. I. First year of ITP13
observations
Authors: Barrena, R.; Streblyanska, A.; Ferragamo, A.; Rubiño-Martín,
J. A.; Aguado-Barahona, A.; Tramonte, D.; Génova-Santos, R. T.;
Hempel, A.; Lietzen, H.; Aghanim, N.; Arnaud, M.; Böhringer, H.; Chon,
G.; Democles, J.; Dahle, H.; Douspis, M.; Lasenby, A. N.; Mazzotta,
P.; Melin, J. B.; Pointecouteau, E.; Pratt, G. W.; Rossetti, M.;
van der Burg, R. F. J.
2018A&A...616A..42B Altcode: 2018arXiv180305764B
We have identified new clusters and characterized previously unknown
Planck Sunyaev-Zeldovich (SZ) sources from the first Planck catalogue of
SZ sources (PSZ1). The results presented here correspond to an optical
follow-up observational programme developed during approximately one
year (2014) at Roque de los Muchachos Observatory, using the 2.5
m Isaac Newton telescope, the 3.5 m Telescopio Nazionale Galileo,
the 4.2 m William Herschel telescope and the 10.4 m Gran Telescopio
Canarias. We have characterized 115 new PSZ1 sources using deep optical
imaging and spectroscopy. We adopted robust criteria in order to
consolidate the SZ counterparts by analysing the optical richness, the
2D galaxy distribution, and velocity dispersions of clusters. Confirmed
counterparts are considered to be validated if they are rich structures,
well aligned with the Planck PSZ1 coordinate and show relatively
high velocity dispersion. Following this classification, we confirm
53 clusters, which means that 46% of this PSZ1 subsample has been
validated and characterized with this technique. Sixty-two SZ sources
(54% of this PSZ1 subset) remain unconfirmed. In addition, we find that
the fraction of unconfirmed clusters close to the galactic plane (at
|b| < 25°) is greater than that at higher galactic latitudes (|b|
> 25°), which indicates contamination produced by radio emission
of galactic dust and gas clouds on these SZ detections. In fact,
in the majority of the cases, we detect important galactic cirrus in
the optical images, mainly in the SZ target located at low galactic
latitudes, which supports this hypothesis.
---------------------------------------------------------
Title: LoCuSS: The infall of X-ray groups on to massive clusters
Authors: Haines, C. P.; Finoguenov, A.; Smith, G. P.; Babul, A.;
Egami, E.; Mazzotta, P.; Okabe, N.; Pereira, M. J.; Bianconi, M.;
McGee, S. L.; Ziparo, F.; Campusano, L. E.; Loyola, C.
2018MNRAS.477.4931H Altcode: 2018MNRAS.tmp..682H; 2017arXiv170904945H; 2018MNRAS.tmp..628H
Galaxy clusters are expected to form hierarchically in a Λ cold dark
matter (ΛCDM) universe, growing primarily through mergers with lower
mass clusters and the continual accretion of group-mass haloes. Galaxy
clusters assemble late, doubling their masses since z ∼ 0.5, and
so the outer regions of clusters should be replete with accreting
group-mass systems. We present an XMM-Newton survey to search for
X-ray groups in the infall regions of 23 massive galaxy clusters
(<M<SUB>200</SUB>> ∼ 10<SUP>15 </SUP>M<SUB>⊙</SUB>) at z
∼ 0.2, identifying 39 X-ray groups that have been spectroscopically
confirmed to lie at the cluster redshift. These groups have mass
estimates in the range 2 × 10<SUP>13</SUP>-7 × 10<SUP>14</SUP>
M<SUB>⊙</SUB>, and group-to-cluster mass ratios as low as 0.02. The
comoving number density of X-ray groups in the infall regions is
∼25× higher than that seen for isolated X-ray groups from the XXL
survey. The average mass per cluster contained within these X-ray groups
is 2.2 × 10<SUP>14 </SUP>M<SUB>⊙</SUB>, or 19 ± 5 per cent of the
mass within the primary cluster itself. We estimate that ∼10<SUP>15
</SUP>M<SUB>⊙</SUB> clusters increase their masses by 16 ± 4 per
cent between z = 0.223 and the present day due to the accretion of
groups with M<SUB>200</SUB> ≥ 10<SUP>13.2 </SUP>M<SUB>⊙</SUB>. This
represents about half of the expected mass growth rate of clusters
at these late epochs. The other half is likely to come from smooth
accretion of matter not bound within haloes. The mass function of the
infalling X-ray groups appears significantly top heavy with respect
to that of `field' X-ray systems, consistent with expectations from
numerical simulations, and the basic consequences of collapsed massive
dark matter haloes being biased tracers of the underlying large-scale
density distribution.
---------------------------------------------------------
Title: The ATHENA X-ray Integral Field Unit (X-IFU)
Authors: Barret, Didier; Lam Trong, Thien; den Herder, Jan-Willem;
Piro, Luigi; Cappi, Massimo; Houvelin, Juhani; Kelley, Richard;
Mas-Hesse, J. Miguel; Mitsuda, Kazuhisa; Paltani, Stéphane; Rauw,
Gregor; Rozanska, Agata; Wilms, Joern; Bandler, Simon; Barbera, Marco;
Barcons, Xavier; Bozzo, Enrico; Ceballos, Maria Teresa; Charles,
Ivan; Costantini, Elisa; Decourchelle, Anne; den Hartog, Roland;
Duband, Lionel; Duval, Jean-Marc; Fiore, Fabrizio; Gatti, Flavio;
Goldwurm, Andrea; Jackson, Brian; Jonker, Peter; Kilbourne, Caroline;
Macculi, Claudio; Mendez, Mariano; Molendi, Silvano; Orleanski, Piotr;
Pajot, François; Pointecouteau, Etienne; Porter, Frederick; Pratt,
Gabriel W.; Prêle, Damien; Ravera, Laurent; Sato, Kosuke; Schaye,
Joop; Shinozaki, Keisuke; Thibert, Tanguy; Valenziano, Luca; Valette,
Véronique; Vink, Jacco; Webb, Natalie; Wise, Michael; Yamasaki,
Noriko; Douchin, Françoise; Mesnager, Jean-Michel; Pontet, Bernard;
Pradines, Alice; Branduardi-Raymont, Graziella; Bulbul, Esra; Dadina,
Mauro; Ettori, Stefano; Finoguenov, Alexis; Fukazawa, Yasushi; Janiuk,
Agnieszka; Kaastra, Jelle; Mazzotta, Pasquale; Miller, Jon; Miniutti,
Giovanni; Naze, Yael; Nicastro, Fabrizio; Scioritino, Salavtore;
Simonescu, Aurora; Torrejon, Jose Miguel; Frezouls, Benoit; Geoffray,
Hervé; Peille, Philippe; Aicardi, Corinne; André, Jérôme; Daniel,
Christophe; Clénet, Antoine; Etcheverry, Christophe; Gloaguen,
Emilie; Hervet, Gilles; Jolly, Antoine; Ledot, Aurélien; Paillet,
Irwin; Schmisser, Roseline; Vella, Bruno; Damery, Jean-Charles;
Boyce, Kevin; Dipirro, Mike; Lotti, Simone; Schwander, Denis; Smith,
Stephen; Van Leeuwen, Bert-Joost; van Weers, Henk; Clerc, Nicolas;
Cobo, Beatriz; Dauser, Thomas; Kirsch, Christian; Cucchetti, Edoardo;
Eckart, Megan; Ferrando, Philippe; Natalucci, Lorenzo
2018SPIE10699E..1GB Altcode: 2018arXiv180706092B
The X-ray Integral Field Unit (X-IFU) is the high resolution X-ray
spectrometer of the ESA Athena X-ray observatory. Over a field of
view of 5' equivalent diameter, it will deliver X-ray spectra from 0.2
to 12 keV with a spectral resolution of 2.5 eV up to 7 keV on ∼ 5"
pixels. The X-IFU is based on a large format array of super-conducting
molybdenum-gold Transition Edge Sensors cooled at ∼ 90 mK, each
coupled with an absorber made of gold and bismuth with a pitch of
249 μm. A cryogenic anti-coincidence detector located underneath
the prime TES array enables the non X-ray background to be reduced. A
bath temperature of ∼ 50 mK is obtained by a series of mechanical
coolers combining 15K Pulse Tubes, 4K and 2K Joule-Thomson coolers
which pre-cool a sub Kelvin cooler made of a 3He sorption cooler
coupled with an Adiabatic Demagnetization Refrigerator. Frequency
domain multiplexing enables to read out 40 pixels in one single
channel. A photon interacting with an absorber leads to a current
pulse, amplified by the readout electronics and whose shape is
reconstructed on board to recover its energy with high accuracy. The
defocusing capability offered by the Athena movable mirror assembly
enables the X-IFU to observe the brightest X-ray sources of the sky
(up to Crab-like intensities) by spreading the telescope point spread
function over hundreds of pixels. Thus the X-IFU delivers low pile-up,
high throughput (< 50%), and typically 10 eV spectral resolution at 1
Crab intensities, i.e. a factor of 10 or more better than Silicon based
X-ray detectors. In this paper, the current X-IFU baseline is presented,
together with an assessment of its anticipated performance in terms of
spectral resolution, background, and count rate capability. The X-IFU
baseline configuration will be subject to a preliminary requirement
review that is scheduled at the end of 2018.
---------------------------------------------------------
Title: Exploring cosmic origins with CORE: Effects of observer
peculiar motion
Authors: Burigana, C.; Carvalho, C. S.; Trombetti, T.; Notari, A.;
Quartin, M.; de Gasperis, G.; Buzzelli, A.; Vittorio, N.; De Zotti, G.;
de Bernardis, P.; Chluba, J.; Bilicki, M.; Danese, L.; Delabrouille,
J.; Toffolatti, L.; Lapi, A.; Negrello, M.; Mazzotta, P.; Scott, D.;
Contreras, D.; Achúcarro, A.; Ade, P.; Allison, R.; Ashdown, M.;
Ballardini, M.; Banday, A. J.; Banerji, R.; Bartlett, J.; Bartolo,
N.; Basak, S.; Bersanelli, M.; Bonaldi, A.; Bonato, M.; Borrill, J.;
Bouchet, F.; Boulanger, F.; Brinckmann, T.; Bucher, M.; Cabella, P.;
Cai, Z. -Y.; Calvo, M.; Castellano, M. G.; Challinor, A.; Clesse,
S.; Colantoni, I.; Coppolecchia, A.; Crook, M.; D'Alessandro, G.;
Diego, J. -M.; Di Marco, A.; Di Valentino, E.; Errard, J.; Feeney,
S.; Fernández-Cobos, R.; Ferraro, S.; Finelli, F.; Forastieri, F.;
Galli, S.; Génova-Santos, R.; Gerbino, M.; González-Nuevo, J.;
Grandis, S.; Greenslade, J.; Hagstotz, S.; Hanany, S.; Handley, W.;
Hernández-Monteagudo, C.; Hervias-Caimapo, C.; Hills, M.; Hivon, E.;
Kiiveri, K.; Kisner, T.; Kitching, T.; Kunz, M.; Kurki-Suonio, H.;
Lamagna, L.; Lasenby, A.; Lattanzi, M.; Lesgourgues, J.; Liguori, M.;
Lindholm, V.; Lopez-Caniego, M.; Luzzi, G.; Maffei, B.; Mandolesi, N.;
Martinez-Gonzalez, E.; Martins, C. J. A. P.; Masi, S.; Matarrese,
S.; McCarthy, D.; Melchiorri, A.; Melin, J. -B.; Molinari, D.;
Monfardini, A.; Natoli, P.; Paiella, A.; Paoletti, D.; Patanchon, G.;
Piat, M.; Pisano, G.; Polastri, L.; Polenta, G.; Pollo, A.; Poulin,
V.; Remazeilles, M.; Roman, M.; Rubiño-Martín, J. -A.; Salvati,
L.; Tartari, A.; Tomasi, M.; Tramonte, D.; Trappe, N.; Tucker, C.;
Väliviita, J.; Van de Weijgaert, R.; van Tent, B.; Vennin, V.;
Vielva, P.; Young, K.; Zannoni, M.
2018JCAP...04..021B Altcode: 2017arXiv170405764B
We discuss the effects on the cosmic microwave background (CMB), cosmic
infrared background (CIB), and thermal Sunyaev-Zeldovich effect due to
the peculiar motion of an observer with respect to the CMB rest frame,
which induces boosting effects. After a brief review of the current
observational and theoretical status, we investigate the scientific
perspectives opened by future CMB space missions, focussing on the
Cosmic Origins Explorer (CORE) proposal. The improvements in sensitivity
offered by a mission like CORE, together with its high resolution
over a wide frequency range, will provide a more accurate estimate of
the CMB dipole. The extension of boosting effects to polarization and
cross-correlations will enable a more robust determination of purely
velocity-driven effects that are not degenerate with the intrinsic CMB
dipole, allowing us to achieve an overall signal-to-noise ratio of 13;
this improves on the Planck detection and essentially equals that
of an ideal cosmic-variance-limited experiment up to a multipole
lsimeq2000. Precise inter-frequency calibration will offer the
opportunity to constrain or even detect CMB spectral distortions,
particularly from the cosmological reionization epoch, because of
the frequency dependence of the dipole spectrum, without resorting to
precise absolute calibration. The expected improvement with respect
to COBE-FIRAS in the recovery of distortion parameters (which could
in principle be a factor of several hundred for an ideal experiment
with the CORE configuration) ranges from a factor of several up to
about 50, depending on the quality of foreground removal and relative
calibration. Even in the case of simeq1 % accuracy in both foreground
removal and relative calibration at an angular scale of 1<SUP>o</SUP>,
we find that dipole analyses for a mission like CORE will be able to
improve the recovery of the CIB spectrum amplitude by a factor simeq
17 in comparison with current results based on COBE-FIRAS. In addition
to the scientific potential of a mission like CORE for these analyses,
synergies with other planned and ongoing projects are also discussed.
---------------------------------------------------------
Title: Exploring cosmic origins with CORE: Cluster science
Authors: Melin, J. -B.; Bonaldi, A.; Remazeilles, M.; Hagstotz,
S.; Diego, J. M.; Hernández-Monteagudo, C.; Génova-Santos, R. T.;
Luzzi, G.; Martins, C. J. A. P.; Grandis, S.; Mohr, J. J.; Bartlett,
J. G.; Delabrouille, J.; Ferraro, S.; Tramonte, D.; Rubiño-Martín,
J. A.; Macìas-Pérez, J. F.; Achúcarro, A.; Ade, P.; Allison, R.;
Ashdown, M.; Ballardini, M.; Banday, A. J.; Banerji, R.; Bartolo,
N.; Basak, S.; Basu, K.; Battye, R. A.; Baumann, D.; Bersanelli, M.;
Bonato, M.; Borrill, J.; Bouchet, F.; Boulanger, F.; Brinckmann,
T.; Bucher, M.; Burigana, C.; Buzzelli, A.; Cai, Z. -Y.; Calvo,
M.; Carvalho, C. S.; Castellano, M. G.; Challinor, A.; Chluba, J.;
Clesse, S.; Colafrancesco, S.; Colantoni, I.; Coppolecchia, A.;
Crook, M.; D'Alessandro, G.; de Bernardis, P.; de Gasperis, G.; De
Petris, M.; De Zotti, G.; Di Valentino, E.; Errard, J.; Feeney, S. M.;
Fernández-Cobos, R.; Finelli, F.; Forastieri, F.; Galli, S.; Gerbino,
M.; González-Nuevo, J.; Greenslade, J.; Hanany, S.; Handley, W.;
Hervias-Caimapo, C.; Hills, M.; Hivon, E.; Kiiveri, K.; Kisner, T.;
Kitching, T.; Kunz, M.; Kurki-Suonio, H.; Lamagna, L.; Lasenby, A.;
Lattanzi, M.; Le Brun, A. M. C.; Lesgourgues, J.; Lewis, A.; Liguori,
M.; Lindholm, V.; Lopez-Caniego, M.; Maffei, B.; Martinez-Gonzalez,
E.; Masi, S.; Mazzotta, P.; McCarthy, D.; Melchiorri, A.; Molinari,
D.; Monfardini, A.; Natoli, P.; Negrello, M.; Notari, A.; Paiella,
A.; Paoletti, D.; Patanchon, G.; Piat, M.; Pisano, G.; Polastri,
L.; Polenta, G.; Pollo, A.; Poulin, V.; Quartin, M.; Roman, M.;
Salvati, L.; Tartari, A.; Tomasi, M.; Trappe, N.; Triqueneaux, S.;
Trombetti, T.; Tucker, C.; Väliviita, J.; van de Weygaert, R.; Van
Tent, B.; Vennin, V.; Vielva, P.; Vittorio, N.; Weller, J.; Young,
K.; Zannoni, M.
2018JCAP...04..019M Altcode: 2017arXiv170310456M
We examine the cosmological constraints that can be achieved with
a galaxy cluster survey with the future CORE space mission. Using
realistic simulations of the millimeter sky, produced with the latest
version of the Planck Sky Model, we characterize the CORE cluster
catalogues as a function of the main mission performance parameters. We
pay particular attention to telescope size, key to improved angular
resolution, and discuss the comparison and the complementarity of
CORE with ambitious future ground-based CMB experiments that could be
deployed in the next decade. A possible CORE mission concept with a 150
cm diameter primary mirror can detect of the order of 50,000 clusters
through the thermal Sunyaev-Zeldovich effect (SZE). The total yield
increases (decreases) by 25% when increasing (decreasing) the mirror
diameter by 30 cm. The 150 cm telescope configuration will detect
the most massive clusters (>10<SUP>14</SUP> M<SUB>solar</SUB>)
at redshift z>1.5 over the whole sky, although the exact number
above this redshift is tied to the uncertain evolution of the cluster
SZE flux-mass relation; assuming self-similar evolution, CORE will
detect 0~ 50 clusters at redshift z>1.5. This changes to 800 (200)
when increasing (decreasing) the mirror size by 30 cm. CORE will be
able to measure individual cluster halo masses through lensing of the
cosmic microwave background anisotropies with a 1-σ sensitivity of
4×10<SUP>14</SUP> M<SUB>solar</SUB>, for a 120 cm aperture telescope,
and 10<SUP>14</SUP> M<SUB>solar</SUB> for a 180 cm one. From the
ground, we estimate that, for example, a survey with about 150,000
detectors at the focus of 350 cm telescopes observing 65% of the sky
would be shallower than CORE and detect about 11,000 clusters, while
a survey with the same number of detectors observing 25% of sky with
a 10 m telescope is expected to be deeper and to detect about 70,000
clusters. When combined with the latter, CORE would reach a limiting
mass of M<SUB>500</SUB> ~ 2-3 × 10<SUP>13</SUP> M<SUB>solar</SUB>
and detect 220,000 clusters (5 sigma detection limit). Cosmological
constraints from CORE cluster counts alone are competitive with other
scheduled large scale structure surveys in the 2020's for measuring the
dark energy equation-of-state parameters w<SUB>0</SUB> and w<SUB>a</SUB>
(σ<SUB>w<SUB>0</SUB></SUB>=0.28, σ<SUB>w<SUB>a</SUB></SUB>=0.31). In
combination with primary CMB constraints, CORE cluster counts can
further reduce these error bars on w<SUB>0</SUB> and w<SUB>a</SUB>
to 0.05 and 0.13 respectively, and constrain the sum of the
neutrino masses, Σ m<SUB>ν</SUB>, to 39 meV (1 sigma). The wide
frequency coverage of CORE, 60-600 GHz, will enable measurement of
the relativistic thermal SZE by stacking clusters. Contamination
by dust emission from the clusters, however, makes constraining
the temperature of the intracluster medium difficult. The
kinetic SZE pairwise momentum will be extracted with 0S/N=7 in the
foreground-cleaned CMB map. Measurements of T<SUB>CMB</SUB>(z) using
CORE clusters will establish competitive constraints on the evolution
of the CMB temperature: (1+z)<SUP>1-β</SUP>, with an uncertainty
of σ<SUB>β</SUB> lesssim 2.7× 10<SUP>-3</SUP> at low redshift (z
lesssim 1). The wide frequency coverage also enables clean extraction
of a map of the diffuse SZE signal over the sky, substantially
reducing contamination by foregrounds compared to the Planck SZE
map extraction. Our analysis of the one-dimensional distribution of
Compton-y values in the simulated map finds an order of magnitude
improvement in constraints on σ<SUB>8</SUB> over the Planck result,
demonstrating the potential of this cosmological probe with CORE.
---------------------------------------------------------
Title: Exploring cosmic origins with CORE: Survey requirements and
mission design
Authors: Delabrouille, J.; de Bernardis, P.; Bouchet, F. R.;
Achúcarro, A.; Ade, P. A. R.; Allison, R.; Arroja, F.; Artal,
E.; Ashdown, M.; Baccigalupi, C.; Ballardini, M.; Banday, A. J.;
Banerji, R.; Barbosa, D.; Bartlett, J.; Bartolo, N.; Basak, S.;
Baselmans, J. J. A.; Basu, K.; Battistelli, E. S.; Battye, R.;
Baumann, D.; Benoít, A.; Bersanelli, M.; Bideaud, A.; Biesiada, M.;
Bilicki, M.; Bonaldi, A.; Bonato, M.; Borrill, J.; Boulanger, F.;
Brinckmann, T.; Brown, M. L.; Bucher, M.; Burigana, C.; Buzzelli,
A.; Cabass, G.; Cai, Z. -Y.; Calvo, M.; Caputo, A.; Carvalho,
C. -S.; Casas, F. J.; Castellano, G.; Catalano, A.; Challinor, A.;
Charles, I.; Chluba, J.; Clements, D. L.; Clesse, S.; Colafrancesco,
S.; Colantoni, I.; Contreras, D.; Coppolecchia, A.; Crook, M.;
D'Alessandro, G.; D'Amico, G.; da Silva, A.; de Avillez, M.; de
Gasperis, G.; De Petris, M.; de Zotti, G.; Danese, L.; Désert,
F. -X.; Desjacques, V.; Di Valentino, E.; Dickinson, C.; Diego,
J. M.; Doyle, S.; Durrer, R.; Dvorkin, C.; Eriksen, H. K.; Errard,
J.; Feeney, S.; Fernández-Cobos, R.; Finelli, F.; Forastieri, F.;
Franceschet, C.; Fuskeland, U.; Galli, S.; Génova-Santos, R. T.;
Gerbino, M.; Giusarma, E.; Gomez, A.; González-Nuevo, J.; Grandis,
S.; Greenslade, J.; Goupy, J.; Hagstotz, S.; Hanany, S.; Handley, W.;
Henrot-Versillé, S.; Hernández-Monteagudo, C.; Hervias-Caimapo, C.;
Hills, M.; Hindmarsh, M.; Hivon, E.; Hoang, D. T.; Hooper, D. C.; Hu,
B.; Keihänen, E.; Keskitalo, R.; Kiiveri, K.; Kisner, T.; Kitching,
T.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamagna, L.; Lapi,
A.; Lasenby, A.; Lattanzi, M.; Le Brun, A. M. C.; Lesgourgues, J.;
Liguori, M.; Lindholm, V.; Lizarraga, J.; Luzzi, G.; Macìas-P{érez,
J. F.; Maffei, B.; Mandolesi, N.; Martin, S.; Martinez-Gonzalez, E.;
Martins, C. J. A. P.; Masi, S.; Massardi, M.; Matarrese, S.; Mazzotta,
P.; McCarthy, D.; Melchiorri, A.; Melin, J. -B.; Mennella, A.; Mohr,
J.; Molinari, D.; Monfardini, A.; Montier, L.; Natoli, P.; Negrello,
M.; Notari, A.; Noviello, F.; Oppizzi, F.; O'Sullivan, C.; Pagano, L.;
Paiella, A.; Pajer, E.; Paoletti, D.; Paradiso, S.; Partridge, R. B.;
Patanchon, G.; Patil, S. P.; Perdereau, O.; Piacentini, F.; Piat, M.;
Pisano, G.; Polastri, L.; Polenta, G.; Pollo, A.; Ponthieu, N.; Poulin,
V.; Prêle, D.; Quartin, M.; Ravenni, A.; Remazeilles, M.; Renzi, A.;
Ringeval, C.; Roest, D.; Roman, M.; Roukema, B. F.; Rubiño-Martin,
J. -A.; Salvati, L.; Scott, D.; Serjeant, S.; Signorelli, G.;
Starobinsky, A. A.; Sunyaev, R.; Tan, C. Y.; Tartari, A.; Tasinato,
G.; Toffolatti, L.; Tomasi, M.; Torrado, J.; Tramonte, D.; Trappe,
N.; Triqueneaux, S.; Tristram, M.; Trombetti, T.; Tucci, M.; Tucker,
C.; Urrestilla, J.; Väliviita, J.; Van de Weygaert, R.; Van Tent,
B.; Vennin, V.; Verde, L.; Vermeulen, G.; Vielva, P.; Vittorio, N.;
Voisin, F.; Wallis, C.; Wandelt, B.; Wehus, I. K.; Weller, J.; Young,
K.; Zannoni, M.
2018JCAP...04..014D Altcode: 2017arXiv170604516D
Future observations of cosmic microwave background (CMB) polarisation
have the potential to answer some of the most fundamental questions
of modern physics and cosmology, including: what physical process
gave birth to the Universe we see today? What are the dark matter
and dark energy that seem to constitute 95% of the energy density of
the Universe? Do we need extensions to the standard model of particle
physics and fundamental interactions? Is the ΛCDM cosmological scenario
correct, or are we missing an essential piece of the puzzle? In this
paper, we list the requirements for a future CMB polarisation survey
addressing these scientific objectives, and discuss the design drivers
of the COREmfive space mission proposed to ESA in answer to the "M5"
call for a medium-sized mission. The rationale and options, and the
methodologies used to assess the mission's performance, are of interest
to other future CMB mission design studies. COREmfive has 19 frequency
channels, distributed over a broad frequency range, spanning the
60-600 GHz interval, to control astrophysical foreground emission. The
angular resolution ranges from 2<SUP>'</SUP> to 18<SUP>'</SUP>,
and the aggregate CMB sensitivity is about 2 μKṡarcmin. The
observations are made with a single integrated focal-plane instrument,
consisting of an array of 2100 cryogenically-cooled, linearly-polarised
detectors at the focus of a 1.2-m aperture cross-Dragone telescope. The
mission is designed to minimise all sources of systematic effects,
which must be controlled so that no more than 10<SUP>-4</SUP> of the
intensity leaks into polarisation maps, and no more than about 1%
of E-type polarisation leaks into B-type modes. COREmfive observes
the sky from a large Lissajous orbit around the Sun-Earth L2 point
on an orbit that offers stable observing conditions and avoids
contamination from sidelobe pick-up of stray radiation originating
from the Sun, Earth, and Moon. The entire sky is observed repeatedly
during four years of continuous scanning, with a combination of three
rotations of the spacecraft over different timescales. With about 50%
of the sky covered every few days, this scan strategy provides the
mitigation of systematic effects and the internal redundancy that are
needed to convincingly extract the primordial B-mode signal on large
angular scales, and check with adequate sensitivity the consistency
of the observations in several independent data subsets. COREmfive
is designed as a "near-ultimate" CMB polarisation mission which, for
optimal complementarity with ground-based observations, will perform
the observations that are known to be essential to CMB polarisation
science and cannot be obtained by any other means than a dedicated
space mission. It will provide well-characterised, highly-redundant
multi-frequency observations of polarisation at all the scales where
foreground emission and cosmic variance dominate the final uncertainty
for obtaining precision CMB science, as well as 2<SUP>'</SUP> angular
resolution maps of high-frequency foreground emission in the 300-600 GHz
frequency range, essential for complementarity with future ground-based
observations with large telescopes that can observe the CMB with the
same beamsize.
---------------------------------------------------------
Title: Cosmological hydrodynamical simulations of galaxy clusters:
X-ray scaling relations and their evolution
Authors: Truong, N.; Rasia, E.; Mazzotta, P.; Planelles, S.; Biffi,
V.; Fabjan, D.; Beck, A. M.; Borgani, S.; Dolag, K.; Gaspari, M.;
Granato, G. L.; Murante, G.; Ragone-Figueroa, C.; Steinborn, L. K.
2018MNRAS.474.4089T Altcode: 2016arXiv160700019T
We analyse cosmological hydrodynamical simulations of galaxy clusters to
study the X-ray scaling relations between total masses and observable
quantities such as X-ray luminosity, gas mass, X-ray temperature, and
Y<SUB>X</SUB>. Three sets of simulations are performed with an improved
version of the smoothed particle hydrodynamics GADGET-3 code. These
consider the following: non-radiative gas, star formation and stellar
feedback, and the addition of feedback by active galactic nuclei
(AGN). We select clusters with M<SUB>500</SUB> > 10<SUP>14</SUP>
M<SUB>⊙</SUB>E(z)<SUP>-1</SUP>, mimicking the typical selection of
Sunyaev-Zeldovich samples. This permits to have a mass range large
enough to enable robust fitting of the relations even at z ∼ 2. The
results of the analysis show a general agreement with observations. The
values of the slope of the mass-gas mass and mass-temperature relations
at z = 2 are 10 per cent lower with respect to z = 0 due to the applied
mass selection, in the former case, and to the effect of early merger
in the latter. We investigate the impact of the slope variation on
the study of the evolution of the normalization. We conclude that
cosmological studies through scaling relations should be limited to the
redshift range z = 0-1, where we find that the slope, the scatter, and
the covariance matrix of the relations are stable. The scaling between
mass and Y<SUB>X</SUB> is confirmed to be the most robust relation,
being almost independent of the gas physics. At higher redshifts,
the scaling relations are sensitive to the inclusion of AGNs which
influences low-mass systems. The detailed study of these objects will
be crucial to evaluate the AGN effect on the ICM.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Cool-core clusters with Chandra
obs. (Andrade-Santos+, 2017)
Authors: Andrade-Santos, F.; Jones, C.; Forman, W. R.; Lovisari, L.;
Vikhlinin, A.; van Weeren, R. J.; Murray, S. S.; Arnaud, M.; Pratt,
G. W.; Democles, J.; Kraft, R.; Mazzotta, P.; Bohringer, H.; Chon,
G.; Giacintucci, S.; Clarke, T. E.; Borgani, S.; David, L.; Douspis,
M.; Pointecouteau, E.; Dahle, H.; Brown, S.; Aghanim, N.; Rasia, E.
2018yCat..18430076A Altcode:
The main goal of this work is to compare the fraction of cool-core
(CC) clusters in X-ray-selected and SZ-selected samples. <P />The
first catalog of 189 SZ clusters detected by the Planck mission was
released in early 2011 (Planck Collaboration 2011, VIII/88/esz). A
Chandra XVP (X-ray Visionary Program--PI: Jones) and HRC Guaranteed
Time Observations (PI: Murray) combined to form the Chandra-Planck
Legacy Program for Massive Clusters of Galaxies. For each of the
164 ESZ Planck clusters at z<=0.35, we obtained Chandra exposures
sufficient to collect at least 10000 source counts. <P />The X-ray
sample used here is an extension of the Voevodkin & Vikhlinin
(2004ApJ...601..610V) sample. This sample contains 100 clusters
and has an effective redshift depth of z<0.3. All have Chandra
observations. Of the 100 X-ray-selected clusters, 49 are also in the
ESZ sample, and 47 are in the HIFLUGCS (Reiprich & Boehringer
2002ApJ...567..716R) catalog. <P />(2 data files).
---------------------------------------------------------
Title: Planck intermediate results. XV. A study of anomalous microwave
emission in Galactic clouds (Corrigendum)
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alves,
M. I. R.; Arnaud, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.;
Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Boulanger, F.; Burigana, C.; Cardoso, J. -F.; Casassus,
S.; Catalano, A.; Chamballu, A.; Chen, X.; Chiang, H. C.; Chiang,
L. -Y.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Colombo,
L. P. L.; Couchot, F.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies,
R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.;
Delabrouille, J.; Désert, F. -X.; Dickinson, C.; Diego, J. M.;
Donzelli, S.; Doré, O.; Dupac, X.; Enßlin, T. A.; Eriksen, H. K.;
Finelli, F.; Forni, O.; Franceschi, E.; Galeotta, S.; Ganga, K.;
Génova-Santos, R. T.; Ghosh, T.; Giard, M.; González-Nuevo, J.;
Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison,
D. L.; Helou, G.; Hernández-Monteagudo, C.; Hildebrandt, S. R.;
Hivon, E.; Hobson, M.; Hornstrup, A.; Jaffe, A. H.; Jaffe, T. R.;
Jones, W. C.; Keihänen, E.; Keskitalo, R.; Kneissl, R.; Knoche,
J.; Kunz, M.; Kurki-Suonio, H.; Lähteenmäki, A.; Lamarre, J. -M.;
Lasenby, A.; Lawrence, C. R.; Leonardi, R.; Liguori, M.; Lilje,
P. B.; Linden-Vørnle, M.; López-Caniego, M.; Macías-Pérez, J. F.;
Maffei, B.; Maino, D.; Mandolesi, N.; Marshall, D. J.; Martin, P. G.;
Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella,
A.; Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier,
L.; Morgante, G.; Mortlock, D.; Munshi, D.; Naselsky, P.; Nati, F.;
Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.;
Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Patanchon, G.; Pearson, T. J.; Peel, M.; Perdereau,
O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.;
Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.;
Rebolo, R.; Reich, W.; Reinecke, M.; Remazeilles, M.; Renault, C.;
Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini,
G.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.;
Tibbs, C. T.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Verstraete,
L.; Vielva, P.; Villa, F.; Wandelt, B. D.; Watson, R.; Wilkinson,
A.; Ysard, N.; Yvon, D.; Zacchei, A.; Zonca, A.
2018A&A...610C...1P Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Recovering galaxy cluster gas density profiles with XMM-Newton
and Chandra
Authors: Bartalucci, I.; Arnaud, M.; Pratt, G. W.; Vikhlinin,
A.; Pointecouteau, E.; Forman, W. R.; Jones, C.; Mazzotta, P.;
Andrade-Santos, F.
2017A&A...608A..88B Altcode: 2017arXiv170906570B
We examined the reconstruction of galaxy cluster radial density
profiles obtained from Chandra and XMM-Newton X-ray observations, using
high quality data for a sample of twelve objects covering a range of
morphologies and redshifts. By comparing the results obtained from the
two observatories and by varying key aspects of the analysis procedure,
we examined the impact of instrumental effects and of differences
in the methodology used in the recovery of the density profiles. We
find that the final density profile shape is particularly robust. We
adapted the photon weighting vignetting correction method developed for
XMM-Newton for use with Chandra data, and confirm that the resulting
Chandra profiles are consistent with those corrected a posteriori
for vignetting effects. Profiles obtained from direct deprojection
and those derived using parametric models are consistent at the 1%
level. At radii larger than ~6″, the agreement between Chandra and
XMM-Newton is better than 1%, confirming an excellent understanding
of the XMM-Newton PSF. Furthermore, we find no significant energy
dependence. The impact of the well-known offset between Chandra and
XMM-Newton gas temperature determinations on the density profiles is
found to be negligible. However, we find an overall normalisation offset
in density profiles of the order of ~2.5%, which is linked to absolute
flux cross-calibration issues. As a final result, the weighted ratios
of Chandra to XMM-Newton gas masses computed at R<SUB>2500</SUB>
and R<SUB>500</SUB> are r = 1.03 ± 0.01 and r = 1.03 ± 0.03,
respectively. Our study confirms that the radial density profiles
are robustly recovered, and that any differences between Chandra and
XMM-Newton can be constrained to the ~2.5% level, regardless of the
exact data analysis details. These encouraging results open the way
for the true combination of X-ray observations of galaxy clusters,
fully leveraging the high resolution of Chandra and the high throughput
of XMM-Newton.
---------------------------------------------------------
Title: Fast weak-lensing simulations with halo model
Authors: Giocoli, Carlo; Di Meo, Sandra; Meneghetti, Massimo; Jullo,
Eric; de la Torre, Sylvain; Moscardini, Lauro; Baldi, Marco; Mazzotta,
Pasquale; Metcalf, R. Benton
2017MNRAS.470.3574G Altcode: 2017arXiv170102739G
Full ray-tracing maps of gravitational lensing, constructed from N-body
simulations, represent a fundamental tool to interpret present and
future weak-lensing data. However, the limitation of computational
resources and storage capabilities severely restricts the number
of realizations that can be performed in order to accurately sample
both the cosmic shear models and covariance matrices. In this paper,
we present a halo model formalism for weak gravitational lensing that
alleviates these issues by producing weak-lensing mocks at a reduced
computational cost. Our model takes as input the halo population within
a desired light cone and the linear power spectrum of the underlined
cosmological model. We examine the contribution given by the presence
of substructures within haloes to the cosmic shear power spectrum and
quantify it to the percent level. Our method allows us to reconstruct
high-resolution convergence maps, for any desired source redshifts, of
light cones that realistically trace the matter density distribution
in the universe, account for masked area and sample selections. We
compare our analysis on the same large-scale structures constructed
using ray-tracing techniques and find very good agreements in both the
linear and non-linear regimes up to few percent levels. The accuracy
and speed of our method demonstrate the potential of our halo model
for weak-lensing statistics and the possibility to generate a large
sample of convergence maps for different cosmological models as needed
for the analysis of large galaxy redshift surveys.
---------------------------------------------------------
Title: Pressure Profiles of Distant Galaxy Clusters in the Planck
Catalogue
Authors: Bourdin, H.; Mazzotta, P.; Kozmanyan, A.; Jones, C.;
Vikhlinin, A.
2017ApJ...843...72B Altcode: 2017arXiv170702248B
Successive releases of Planck data have demonstrated the strength of
the Sunyaev-Zeldovich (SZ) effect in detecting hot baryons out to the
galaxy cluster peripheries. To infer the hot gas pressure structure
from nearby galaxy clusters to more distant objects, we developed a
parametric method that models the spectral energy distribution and
spatial anisotropies of both the Galactic thermal dust (GTD) and the
cosmic microwave background (CMB), which are combined with the cluster
SZ and dust signals. Taking advantage of the best angular resolution of
the High Frequency Instrument channels (5 arcmin) and using X-ray priors
in the innermost cluster regions that are not resolved with Planck,
this modeling allowed us to analyze a sample of 61 nearby members of
the Planck Catalogue of SZ sources (0< z< 0.5, \tilde{z}=0.15)
using the full mission data, as well as to examine a distant sample of
23 clusters (0.5< z< 1, \tilde{z}=0.56) that have been recently
followed-up with XMM-Newton and Chandra observations. We find that (I)
the average shape of the mass-scaled pressure profiles agrees with
results obtained by the Planck Collaboration in the nearby cluster
sample, and that (II) no sign of evolution is discernible between
averaged pressure profiles of the low- and high-redshift cluster
samples. In line with theoretical predictions for these halo masses
and redshift ranges, the dispersion of individual profiles relative
to a self-similar shape stays well below 10% inside r <SUB>500</SUB>
but increases in the cluster outskirts.
---------------------------------------------------------
Title: The Fraction of Cool-core Clusters in X-Ray versus SZ Samples
Using Chandra Observations
Authors: Andrade-Santos, Felipe; Jones, Christine; Forman, William R.;
Lovisari, Lorenzo; Vikhlinin, Alexey; van Weeren, Reinout J.; Murray,
Stephen S.; Arnaud, Monique; Pratt, Gabriel W.; Démoclès, Jessica;
Kraft, Ralph; Mazzotta, Pasquale; Böhringer, Hans; Chon, Gayoung;
Giacintucci, Simona; Clarke, Tracy E.; Borgani, Stefano; David, Larry;
Douspis, Marian; Pointecouteau, Etienne; Dahle, Håkon; Brown, Shea;
Aghanim, Nabila; Rasia, Elena
2017ApJ...843...76A Altcode: 2017arXiv170308690A
We derive and compare the fractions of cool-core clusters in the Planck
Early Sunyaev-Zel’dovich sample of 164 clusters with z≤slant 0.35
and in a flux-limited X-ray sample of 100 clusters with z≤slant 0.30,
using Chandra observations. We use four metrics to identify cool-core
clusters: (1) the concentration parameter, which is the ratio of the
integrated emissivity profile within 0.15 r <SUB>500</SUB> to that
within r <SUB>500</SUB>; (2) the ratio of the integrated emissivity
profile within 40 kpc to that within 400 kpc; (3) the cuspiness of
the gas density profile, which is the negative of the logarithmic
derivative of the gas density with respect to the radius, measured at
0.04 r <SUB>500</SUB>; and (4) the central gas density, measured at 0.01
r <SUB>500</SUB>. We find that the sample of X-ray-selected clusters, as
characterized by each of these metrics, contains a significantly larger
fraction of cool-core clusters compared to the sample of SZ-selected
clusters (44% ± 7% versus 28% ± 4% using the concentration parameter
in the 0.15-1.0 r <SUB>500</SUB> range, 61% ± 8% versus 36% ± 5% using
the concentration parameter in the 40-400 kpc range, 64% ± 8% versus
38% ± 5% using the cuspiness, and 53% ± 7% versus 39 ± 5% using the
central gas density). Qualitatively, cool-core clusters are more X-ray
luminous at fixed mass. Hence, our X-ray, flux-limited sample, compared
to the approximately mass-limited SZ sample, is overrepresented with
cool-core clusters. We describe a simple quantitative model that uses
the excess luminosity of cool-core clusters compared to non-cool-core
clusters at fixed mass to successfully predict the observed fraction
of cool-core clusters in X-ray-selected samples.
---------------------------------------------------------
Title: Enlighten the structure of the cluster outskirts with SZ and
X-ray observations
Authors: Mazzotta, P.
2017wprb.confE...5M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Resolving galaxy cluster gas properties at z 1 with
XMM-Newton and Chandra
Authors: Bartalucci, I.; Arnaud, M.; Pratt, G. W.; Démoclès, J.;
van der Burg, R. F. J.; Mazzotta, P.
2017A&A...598A..61B Altcode: 2016arXiv161001899B
Massive, high-redshift, galaxy clusters are useful laboratories to test
cosmological models and to probe structure formation and evolution,
but observations are challenging due to cosmological dimming and angular
distance effects. Here we present a pilot X-ray study of the five most
massive (M<SUB>500</SUB> > 5 × 10<SUP>14</SUP>M<SUB>⊙</SUB>),
distant (z ~ 1), clusters detected via the Sunyaev-Zel'Dovich
effect. We optimally combine XMM-Newton and Chandra X-ray observations
by leveraging the throughput of XMM-Newton to obtain spatially-resolved
spectroscopy, and the spatial resolution of Chandra to probe the bright
inner parts and to detect embedded point sources. Capitalising on the
excellent agreement in flux-related measurements, we present a new
method to derive the density profiles, which are constrained in the
centre by Chandra and in the outskirts by XMM-Newton. We show that the
Chandra-XMM-Newton combination is fundamental for morphological analysis
at these redshifts, the Chandra resolution being required to remove
point source contamination, and the XMM-Newton sensitivity allowing
higher significance detection of faint substructures. Measuring the
morphology using images from both instruments, we found that the
sample is dominated by dynamically disturbed objects. We use the
combined Chandra-XMM-Newton density profiles and spatially-resolved
temperature profiles to investigate thermodynamic quantities including
entropy and pressure. From comparison of the scaled profiles with the
local REXCESS sample, we find no significant departure from standard
self-similar evolution, within the dispersion, at any radius, except
for the entropy beyond 0.7 R<SUB>500</SUB>. The baryon mass fraction
tends towards the cosmic value, with a weaker dependence on mass
than that observed in the local Universe. We make a comparison with
the predictions from numerical simulations. The present pilot study
demonstrates the utility and feasibility of spatially-resolved analysis
of individual objects at high-redshift through the combination of
XMM-Newton and Chandra observations. Observations of a larger sample
will allow a fuller statistical analysis to be undertaken, in particular
of the intrinsic scatter in the structural and scaling properties of
the cluster population.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Planck Sunyaev-Zeldovich sources
(PSZ2) (Planck+, 2016)
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Barrena, R.; Bartlett, J. G.; Bartolo, N.; Battaner, E.;
Battye, R.; Benabed, K.; Benoit, A.; Benoit-Levy, A.; Bernard, J. -P.;
Bersanelli, M.; Bielewicz, P.; Bikmaev, I.; Bohringer, H.; Bonaldi,
A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bucher,
M.; Burenin, R.; Burigana, C.; Butler, R. C.; Calabrese, E.; Cardoso,
J. -F.; Carvalho, P.; Catalano, A.; Challinor, A.; Chamballu, A.;
Chary, R. -R.; Chiang, H. C.; Chon, G.; Christensen, P. R.; Clements,
D. L.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Comis, B.; Couchot,
F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Dahle, H.;
Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; De Rosa,
A.; de Zotti, G.; Delabrouille, J.; Desert, F. -X.; Dickinson, C.;
Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Dore, O.; Douspis,
M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Eisenhardt, P. R. M.;
Elsner, F.; Ensslin, T. A.; Eriksen, H. K.; Falgarone, E.; Fergusson,
J.; Feroz, F.; Ferragamo, A.; Finelli, F.; Forni, O.; Frailis, M.;
Fraisse, A. A.; Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli,
S.; Ganga, K.; Genova-Santos, R. T.; Giard, M.; Giraud-Heraud, Y.;
Gjerlow, E.; Gonzalez-Nuevo, J.; Gorski, K. M.; Grainge, K. J. B.;
Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Hansen,
F. K.; Hanson, D.; Harrison, D. L.; Hempel, A.; Henrot-Versille, S.;
Hernandez-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger,
K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jin, T.; Jones,
W. C.; Juvela, M.; Keihanen, E.; Keskitalo, R.; Khamitov, I.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lamarre, J. -M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.;
Leonardi, R.; Lesgourgues, J.; Levrier, F.; Liguori, M.; Lilje, P. B.;
Linden-Vornle, M.; Lopez-Caniego, M.; Lubin, P. M.; Macias-Perez,
J. F.; Maggio, G.; Maino, D.; Mak, D. S. Y.; Mandolesi, N.; Mangilli,
A.; Martin, P. G.; Martinez-Gonzalez, E.; Masi, S.; Matarrese, S.;
Mazzotta, P.; McGehee, P.; Mei, S.; Melchiorri, A.; Melin, J. -B.;
Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschenes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss,
A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nastasi, A.; Nati, F.;
Natoli, P.; Netterfield, C. B.; Norgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Olamaie, M.; Oxborrow, C. A.; Paci,
F.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon, G.;
Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrott, Y. C.; Perrotta,
F.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Pratt, G. W.;
Prezeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.;
Rozo, E.; Rubino-Martin, J. A.; Rumsey, C.; Rusholme, B.; Rykoff,
E. S.; Sandri, M.; Santos, D.; Saunders, R. D. E.; Savelainen, M.;
Savini, G.; Schammel, M. P.; Scott, D.; Seiffert, M. D.; Shellard,
E. P. S.; Shimwell, T. W.; Spence, R. L. D.; Stanford, S. A.; Stern,
D.; Stolyarov, V.; Stompor, R.; Streblyanska, A.; Sudiwala, R.;
Sunyaev, R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber,
J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tramonte, D.; Tristram,
M.; Tucci, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Valiviita,
J.; van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.;
Wehus, I. K.; White, S. D. M.; Wright, E. L.; Yvon, D.; Zacchei, A.;
Zonca, A.
2017yCat..35940027P Altcode:
Three pipelines are used to detect SZ clusters: two independent
implementations of the Matched Multi-Filter (MMF1 and MMF3), and
PowellSnakes (PwS). The main catalogue is constructed as the union of
the catalogues from the three detection methods. The completeness and
reliability of the catalogues have been assessed through internal and
external validation as described in section 4 of the paper. <P />(5
data files).
---------------------------------------------------------
Title: VizieR Online Data Catalog: Planck Catalogue of Galactic cold
clumps (PGCC) (Planck+, 2016)
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoit, A.; Benoit-Levy,
A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bonaldi, A.;
Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger,
F.; Bucher, M.; Burigana, C.; Butler, R. C.; Calabrese, E.; Catalano,
A.; Chamballu, A.; Chiang, H. C.; Christensen, P. R.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Combet, C.; Couchot, F.; Coulais, A.;
Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis,
R. J.; de Bernardis, P.; De Rosa, A.; de Zotti, G.; Delabrouille, J.;
Desert, F. -X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.;
Dore, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Elsner,
F.; Ensslin, T. A.; Eriksen, H. K.; Falgarone, E.; Fergusson, J.;
Fergusson, J.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.;
Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.;
Giard, M.; Giraud-Heraud, Y.; Gjerlow, E.; Gonzalez-Nuevo, J.; Gorsk,
I. K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.;
Hansen, F. K.; Hanson, D.; Harrison, D. L.; Helou, G.; Henrot-Versille,
S.; Hernandez-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon,
E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger,
K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela,
M.; Keihanen, E.; Keskitalo, R.; Kisner, T. S.; Knoche, J.; Kunz,
M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.;
Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Lesgourgues, J.; Levrier,
F.; Liguori, M.; Lilje, P. B.; Linden-Vornle, M.; Lopez-Caniego, M.;
Lubin, P. M.; Macias-Perez, J. F.; Maggio, G.; Maino, D.; Mandolesi,
N.; Mangilli, A.; Marshall, D. J.; Martin, P. G.; Martinez-Gonzalez,
E.; Masi, S.; Matarrese, S.; Mazzotta, P.; McGehee, P.; Melchiorri, A.;
Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschenes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss,
A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.;
Netterfield, C. B.; Norgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.;
Paladini, R.; Paoletti, D.; Pasian, F.; Patanchon, G.; Pearson,
T. J.; Pelkonen, V. -M.; Perdereau, O.; Perotto, L.; Perrotta, F.;
Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Pratt, G. W.;
Prezeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier,
G.; Rubino-Martin, J. A.; Rusholme, B.; Sandri, M.; Santos, D.;
Savelainen, M.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard,
E. P. S.; Spencer, L. D.; Stolyarov, V.; Sudiwala, R.; Sunyaev, R.;
Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi,
L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen,
J.; Umana, G.; Valenziano, L.; Valiviita, J.; van Tent, B.; Vielva,
P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Yvon, D.;
Zacchei, A.; Zonca, A.
2017yCat..35940028P Altcode:
The Planck Catalogue of Galactic Cold Clumps (PGCC) is a list of
13188 Galactic sources and 54 sources located in the Small and Large
Magellanic Clouds. The sources have been identified in Planck data as
sources colder than their environment. It has been built using the 48
months Planck data at 857, 545, and 353GHz combined with the 3THz IRAS
data. <P />(1 data file).
---------------------------------------------------------
Title: Planck intermediate results. XL. The Sunyaev-Zeldovich signal
from the Virgo cluster
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bonaldi, A.; Bonavera,
L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Burigana, C.; Butler,
R. C.; Calabrese, E.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.;
Chiang, H. C.; Christensen, P. R.; Churazov, E.; Clements, D. L.;
Colombo, L. P. L.; Combet, C.; Comis, B.; Couchot, F.; Coulais, A.;
Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis,
R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille,
J.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.;
Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Elsner,
F.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis,
M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Galli, S.; Ganga,
K.; Giard, M.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.;
Górski, K. M.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Hansen,
F. K.; Harrison, D. L.; Helou, G.; Hernández-Monteagudo, C.; Herranz,
D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Hornstrup, A.; Hovest,
W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.;
Jones, W. C.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.;
Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.;
Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Levrier,
F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maggio, G.; Maino, D.;
Mandolesi, N.; Mangilli, A.; Marcos-Caballero, A.; Maris, M.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta,
P.; Meinhold, P. R.; Melchiorri, A.; Mennella, A.; Migliaccio, M.;
Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky,
P.; Nati, F.; Natoli, P.; Noviello, F.; Novikov, D.; Novikov, I.;
Oppermann, N.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paoletti, D.;
Pasian, F.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Pettorino,
V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Pratt, G. W.; Prunet,
S.; Puget, J. -L.; Rachen, J. P.; Reinecke, M.; Remazeilles, M.;
Renault, C.; Renzi, A.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Rossetti, M.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.;
Sandri, M.; Santos, D.; Savelainen, M.; Savini, G.; Schaefer, B. M.;
Scott, D.; Soler, J. D.; Stolyarov, V.; Stompor, R.; Sudiwala, R.;
Sunyaev, R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber,
J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci,
M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva,
P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Weller,
J.; Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...596A.101P Altcode: 2015arXiv151105156P
The Virgo cluster is the largest Sunyaev-Zeldovich (SZ) source in the
sky, both in terms of angular size and total integrated flux. Planck's
wide angular scale and frequency coverage, together with its high
sensitivity, enable a detailed study of this big object through the
SZ effect. Virgo is well resolved by Planck, showing an elongated
structure that correlates well with the morphology observed from X-rays,
but extends beyond the observed X-ray signal. We find good agreement
between the SZ signal (or Compton parameter, y<SUB>c</SUB>) observed
by Planck and the expected signal inferred from X-ray observations and
simple analytical models. Owing to its proximity to us, the gas beyond
the virial radius in Virgo can be studied with unprecedented sensitivity
by integrating the SZ signal over tens of square degrees. We study the
signal in the outskirts of Virgo and compare it with analytical models
and a constrained simulation of the environment of Virgo. Planck data
suggest that significant amounts of low-density plasma surround Virgo,
out to twice the virial radius. We find the SZ signal in the outskirts
of Virgo to be consistent with a simple model that extrapolates the
inferred pressure at lower radii, while assuming that the temperature
stays in the keV range beyond the virial radius. The observed signal
is also consistent with simulations and points to a shallow pressure
profile in the outskirts of the cluster. This reservoir of gas at large
radii can be linked with the hottest phase of the elusivewarm/hot
intergalactic medium. Taking the lack of symmetry of Virgo into
account, we find that a prolate model is favoured by the combination
of SZ and X-ray data, in agreement with predictions. Finally, based
on the combination of the same SZ and X-ray data, we constrain the
total amount of gas in Virgo. Under the hypothesis that the abundance
of baryons in Virgo is representative of the cosmic average, we also
infer a distance for Virgo of approximately 18 Mpc, in good agreement
with previous estimates.
---------------------------------------------------------
Title: Planck 2015 results. IV. Low Frequency Instrument beams and
window functions
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Ashdown,
M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Bartolo, N.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy,
A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bock, J. J.;
Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Bucher, M.; Burigana, C.; Butler, R. C.; Calabrese, E.;
Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Christensen, P. R.;
Colombi, S.; Colombo, L. P. L.; Crill, B. P.; Curto, A.; Cuttaia, F.;
Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.;
Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac,
X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.;
Fergusson, J.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi,
E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Giard, M.;
Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.;
Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.;
Harrison, D. L.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt,
S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest,
W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.;
Juvela, M.; Keihänen, E.; Keskitalo, R.; Kiiveri, K.; Kisner, T. S.;
Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lähteenmäki, A.; Lamarre,
J. -M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Leahy, J. P.;
Leonardi, R.; Lesgourgues, J.; Levrier, F.; Liguori, M.; Lilje,
P. B.; Linden-Vørnle, M.; Lindholm, V.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; Maggio, G.; Maino, D.; Mandolesi,
N.; Mangilli, A.; Maris, M.; Martin, P. G.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Mazzotta, P.; McGehee, P.; Meinhold,
P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.;
Mitra, S.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi,
D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Novikov, D.; Novikov, I.; Paci, F.;
Pagano, L.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.;
Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino,
V.; Piacentini, F.; Pierpaoli, E.; Pietrobon, D.; Pointecouteau, E.;
Polenta, G.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renzi, A.;
Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Scott,
D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Stolyarov,
V.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Tuovinen, J.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent,
B.; Vassallo, T.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.;
Watson, R.; Wehus, I. K.; Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...594A...4P Altcode: 2015arXiv150201584P
This paper presents the characterization of the in-flight beams,
the beam window functions, and the associated uncertainties for the
Planck Low Frequency Instrument (LFI). The structure of the paper
is similar to that presented in the 2013 Planck release; the main
differences concern the beam normalization and the delivery of the
window functions to be used for polarization analysis. The in-flight
assessment of the LFI main beams relies on measurements performed during
observations of Jupiter. By stacking data from seven Jupiter transits,
the main beam profiles are measured down to -25 dB at 30 and 44 GHz,
and down to -30 dB at 70 GHz. It has been confirmed that the agreement
between the simulated beams and the measured beams is better than 1%
at each LFI frequency band (within the 20 dB contour from the peak,
the rms values are 0.1% at 30 and 70 GHz; 0.2% at 44 GHz). Simulated
polarized beams are used for the computation of the effective beam
window functions. The error budget for the window functions is estimated
from both main beam and sidelobe contributions, and accounts for the
radiometer band shapes. The total uncertainties in the effective beam
window functions are 0.7% and 1% at 30 and 44 GHz, respectively (at
ℓ ≈ 600); and 0.5% at 70 GHz (at ℓ ≈ 1000).
---------------------------------------------------------
Title: Planck 2015 results. II. Low Frequency Instrument data
processings
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Ashdown,
M.; Aumont, J.; Baccigalupi, C.; Ballardini, M.; Banday, A. J.;
Barreiro, R. B.; Bartolo, N.; Basak, S.; Battaglia, P.; Battaner,
E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J. -P.;
Bersanelli, M.; Bielewicz, P.; Bock, J. J.; Bonaldi, A.; Bonavera,
L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bucher, M.; Burigana,
C.; Butler, R. C.; Calabrese, E.; Cardoso, J. -F.; Castex, G.;
Catalano, A.; Chamballu, A.; Christensen, P. R.; Colombi, S.; Colombo,
L. P. L.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies,
R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.;
Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli,
S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.;
Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Fergusson, J.; Finelli,
F.; Forni, O.; Frailis, M.; Franceschet, C.; Franceschi, E.; Frejsel,
A.; Galeotta, S.; Galli, S.; Ganga, K.; Giard, M.; Giraud-Héraud,
Y.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.;
Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison,
D. L.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.;
Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest,
W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.;
Juvela, M.; Keihänen, E.; Keskitalo, R.; Kiiveri, K.; Kisner, T. S.;
Knoche, J.; Krachmalnicoff, N.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Lattanzi, M.;
Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Levrier,
F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; Lindholm, V.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maggio, G.;
Maino, D.; Mandolesi, N.; Mangilli, A.; Maris, M.; Martin, P. G.;
Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.;
McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella,
A.; Migliaccio, M.; Mitra, S.; Montier, L.; Morgante, G.; Morisset, N.;
Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati,
F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Novikov,
D.; Novikov, I.; Oppermann, N.; Paci, F.; Pagano, L.; Paoletti, D.;
Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Peel, M.;
Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini,
F.; Pierpaoli, E.; Pietrobon, D.; Pointecouteau, E.; Polenta, G.;
Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renzi, A.; Rocha, G.;
Romelli, E.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Scott,
D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Stolyarov,
V.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Tucci, M.; Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.;
Valiviita, J.; Van Tent, B.; Vassallo, T.; Vielva, P.; Villa, F.;
Wade, L. A.; Wandelt, B. D.; Watson, R.; Wehus, I. K.; Wilkinson,
A.; Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...594A...2P Altcode: 2015arXiv150201583P
We present an updated description of the Planck Low Frequency
Instrument (LFI) data processing pipeline, associated with the 2015
data release. We point out the places where our results and methods
have remained unchanged since the 2013 paper and we highlight the
changes made for the 2015 release, describing the products (especially
timelines) and the ways in which they were obtained. We demonstrate
that the pipeline is self-consistent (principally based on simulations)
and report all null tests. For the first time, we present LFI maps in
Stokes Q and U polarization. We refer to other related papers where
more detailed descriptions of the LFI data processing pipeline may be
found if needed.
---------------------------------------------------------
Title: Planck 2015 results. VI. LFI mapmaking
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Ashdown,
M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Bartolo, N.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy,
A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bonaldi, A.;
Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bucher, M.;
Burigana, C.; Butler, R. C.; Calabrese, E.; Cardoso, J. -F.; Catalano,
A.; Chamballu, A.; Chary, R. -R.; Christensen, P. R.; Colombi, S.;
Colombo, L. P. L.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.;
Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli,
S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.;
Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Fergusson, J.; Finelli,
F.; Forni, O.; Frailis, M.; Franceschi, E.; Frejsel, A.; Galeotta,
S.; Galli, S.; Ganga, K.; Giard, M.; Giraud-Héraud, Y.; Gjerløw,
E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio,
A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D. L.;
Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger,
K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Juvela, M.; Keihänen,
E.; Keskitalo, R.; Kiiveri, K.; Kisner, T. S.; Knoche, J.; Kunz, M.;
Kurki-Suonio, H.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.;
Lattanzi, M.; Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; Lesgourgues,
J.; Levrier, F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
Lindholm, V.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maggio, G.; Maino, D.; Mandolesi, N.; Mangilli, A.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.;
McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.;
Migliaccio, M.; Mitra, S.; Montier, L.; Morgante, G.; Mortlock, D.;
Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli,
P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Novikov, D.; Novikov,
I.; Paci, F.; Pagano, L.; Paoletti, D.; Partridge, B.; Pasian, F.;
Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrotta,
F.; Pettorino, V.; Pierpaoli, E.; Pietrobon, D.; Pointecouteau, E.;
Polenta, G.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renzi, A.;
Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Scott,
D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Stolyarov,
V.; Stompor, R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.;
Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Tucci, M.; Tuovinen, J.; Valenziano, L.; Valiviita, J.; Van Tent,
B.; Vassallo, T.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.;
Watson, R.; Wehus, I. K.; Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...594A...6P Altcode: 2015arXiv150201585P
This paper describes the mapmaking procedure applied to Planck Low
Frequency Instrument (LFI) data. The mapmaking step takes as input
the calibrated timelines and pointing information. The main products
are sky maps of I, Q, and U Stokes components. For the first time, we
present polarization maps at LFI frequencies. The mapmaking algorithm
is based on a destriping technique, which is enhanced with a noise
prior. The Galactic region is masked to reduce errors arising from
bandpass mismatch and high signal gradients. We apply horn-uniform
radiometer weights to reduce the effects of beam-shape mismatch. The
algorithm is the same as used for the 2013 release, apart from small
changes in parameter settings. We validate the procedure through
simulations. Special emphasis is put on the control of systematics,
which is particularly important for accurate polarization analysis. We
also produce low-resolution versions of the maps and corresponding
noise covariance matrices. These serve as input in later analysis steps
and parameter estimation. The noise covariance matrices are validated
through noise Monte Carlo simulations. The residual noise in the map
products is characterized through analysis of half-ring maps, noise
covariance matrices, and simulations.
---------------------------------------------------------
Title: Planck 2015 results. XXVIII. The Planck Catalogue of Galactic
cold clumps
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.;
Barreiro, R. B.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.;
Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Boulanger, F.; Bucher, M.; Burigana, C.; Butler, R. C.; Calabrese,
E.; Catalano, A.; Chamballu, A.; Chiang, H. C.; Christensen,
P. R.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet,
C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.;
Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Désert, F. -X.; Dickinson,
C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.;
Ducout, A.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.;
Eriksen, H. K.; Falgarone, E.; Fergusson, J.; Finelli, F.; Forni, O.;
Frailis, M.; Fraisse, A. A.; Franceschi, E.; Frejsel, A.; Galeotta,
S.; Galli, S.; Ganga, K.; Giard, M.; Giraud-Héraud, Y.; Gjerløw,
E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Gudmundsson, J. E.; Hansen, F. K.; Hanson, D.; Harrison,
D. L.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.;
Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.;
Keskitalo, R.; Kisner, T. S.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.;
Lagache, G.; Lamarre, J. -M.; Lasenby, A.; Lattanzi, M.; Lawrence,
C. R.; Leonardi, R.; Lesgourgues, J.; Levrier, F.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Maggio, G.; Maino, D.; Mandolesi, N.; Mangilli,
A.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.;
Matarrese, S.; Mazzotta, P.; McGehee, P.; Melchiorri, A.; Mendes, L.;
Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, M. -A.;
Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi,
D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Pelkonen,
V. -M.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.;
Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski,
S.; Pointecouteau, E.; Polenta, G.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.; Ristorcelli,
I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Savini,
G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.;
Stolyarov, V.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Umana, G.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.;
Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Yvon, D.; Zacchei, A.;
Zonca, A.
2016A&A...594A..28P Altcode: 2015arXiv150201599P
We present the Planck Catalogue of Galactic Cold Clumps (PGCC),
an all-sky catalogue of Galactic cold clump candidates detected by
Planck. This catalogue is the full version of the Early Cold Core
(ECC) catalogue, which was made available in 2011 with the Early
Release Compact Source Catalogue (ERCSC) and which contained 915
high signal-to-noise sources. It is based on the Planck 48-month
mission data that are currently being released to the astronomical
community. The PGCC catalogue is an observational catalogue consisting
exclusively of Galactic cold sources. The three highest Planck bands
(857, 454, and 353 GHz) have been combined with IRAS data at 3 THz to
perform a multi-frequency detection of sources colder than their local
environment. After rejection of possible extragalactic contaminants,
the PGCC catalogue contains 13188 Galactic sources spread across the
whole sky, I.e., from the Galactic plane to high latitudes, following
the spatial distribution of the main molecular cloud complexes. The
median temperature of PGCC sources lies between 13 and 14.5 K,
depending on the quality of the flux density measurements, with a
temperature ranging from 5.8 to 20 K after removing the sources with
the top 1% highest temperature estimates. Using seven independent
methods, reliable distance estimates have been obtained for 5574
sources, which allows us to derive their physical properties such
as their mass, physical size, mean density, and luminosity.The PGCC
sources are located mainly in the solar neighbourhood, but also up
to a distance of 10.5 kpc in the direction of the Galactic centre,
and range from low-mass cores to large molecular clouds. Because of
this diversity and because the PGCC catalogue contains sources in very
different environments, the catalogue is useful for investigating the
evolution from molecular clouds to cores. Finally, it also includes
54 additional sources located in the Small and Large Magellanic Clouds.
---------------------------------------------------------
Title: Planck 2015 results. XXVII. The second Planck catalogue of
Sunyaev-Zeldovich sources
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Barrena, R.; Bartlett, J. G.; Bartolo, N.; Battaner, E.;
Battye, R.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard,
J. -P.; Bersanelli, M.; Bielewicz, P.; Bikmaev, I.; Böhringer, H.;
Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Bucher, M.; Burenin, R.; Burigana, C.; Butler, R. C.; Calabrese,
E.; Cardoso, J. -F.; Carvalho, P.; Catalano, A.; Challinor, A.;
Chamballu, A.; Chary, R. -R.; Chiang, H. C.; Chon, G.; Christensen,
P. R.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet,
C.; Comis, B.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.;
Cuttaia, F.; Dahle, H.; Danese, L.; Davies, R. D.; Davis, R. J.;
de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.;
Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole,
H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.;
Efstathiou, G.; Eisenhardt, P. R. M.; Elsner, F.; Enßlin, T. A.;
Eriksen, H. K.; Falgarone, E.; Fergusson, J.; Feroz, F.; Ferragamo,
A.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi,
E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Génova-Santos,
R. T.; Giard, M.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo,
J.; Górski, K. M.; Grainge, K. J. B.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Gudmundsson, J. E.; Hansen, F. K.; Hanson, D.; Harrison,
D. L.; Hempel, A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.;
Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Jaffe,
A. H.; Jaffe, T. R.; Jin, T.; Jones, W. C.; Juvela, M.; Keihänen, E.;
Keskitalo, R.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby,
A.; Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Lesgourgues,
J.; Levrier, F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maggio,
G.; Maino, D.; Mak, D. S. Y.; Mandolesi, N.; Mangilli, A.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta,
P.; McGehee, P.; Mei, S.; Melchiorri, A.; Melin, J. -B.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss,
A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nastasi, A.; Nati, F.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Olamaie, M.; Oxborrow, C. A.; Paci,
F.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon, G.;
Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrott, Y. C.; Perrotta,
F.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.;
Rozo, E.; Rubiño-Martín, J. A.; Rumsey, C.; Rusholme, B.; Rykoff,
E. S.; Sandri, M.; Santos, D.; Saunders, R. D. E.; Savelainen, M.;
Savini, G.; Schammel, M. P.; Scott, D.; Seiffert, M. D.; Shellard,
E. P. S.; Shimwell, T. W.; Spencer, L. D.; Stanford, S. A.; Stern, D.;
Stolyarov, V.; Stompor, R.; Streblyanska, A.; Sudiwala, R.; Sunyaev,
R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tramonte, D.; Tristram, M.;
Tucci, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Valiviita, J.; Van
Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus,
I. K.; White, S. D. M.; Wright, E. L.; Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...594A..27P Altcode: 2015arXiv150201598P
We present the all-sky Planck catalogue of Sunyaev-Zeldovich (SZ)
sources detected from the 29 month full-mission data. The catalogue
(PSZ2) is the largest SZ-selected sample of galaxy clusters yet produced
and the deepest systematic all-sky surveyof galaxy clusters. It
contains 1653 detections, of which 1203 are confirmed clusters with
identified counterparts in external data sets, and is the first
SZ-selected cluster survey containing >10<SUP>3</SUP> confirmed
clusters. We present a detailed analysis of the survey selection
function in terms of its completeness and statistical reliability,
placing a lower limit of 83% on the purity. Using simulations, we find
that the estimates of the SZ strength parameter Y<SUB>5R500</SUB>are
robust to pressure-profile variation and beam systematics, but accurate
conversion to Y<SUB>500</SUB> requires the use of prior information
on the cluster extent. We describe the multi-wavelength search for
counterparts in ancillary data, which makes use of radio, microwave,
infra-red, optical, and X-ray data sets, and which places emphasis
on the robustness of the counterpart match. We discuss the physical
properties of the new sample and identify a population of low-redshift
X-ray under-luminous clusters revealed by SZ selection. These objects
appear in optical and SZ surveys with consistent properties for their
mass, but are almost absent from ROSAT X-ray selected samples.
---------------------------------------------------------
Title: Planck 2015 results. I. Overview of products and scientific
results
Authors: Planck Collaboration; Adam, R.; Ade, P. A. R.; Aghanim, N.;
Akrami, Y.; Alves, M. I. R.; Argüeso, F.; Arnaud, M.; Arroja, F.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Ballardini, M.; Banday,
A. J.; Barreiro, R. B.; Bartlett, J. G.; Bartolo, N.; Basak, S.;
Battaglia, P.; Battaner, E.; Battye, R.; Benabed, K.; Benoît, A.;
Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bertincourt, B.;
Bielewicz, P.; Bikmaev, I.; Bock, J. J.; Böhringer, H.; Bonaldi, A.;
Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.;
Bucher, M.; Burenin, R.; Burigana, C.; Butler, R. C.; Calabrese, E.;
Cardoso, J. -F.; Carvalho, P.; Casaponsa, B.; Castex, G.; Catalano,
A.; Challinor, A.; Chamballu, A.; Chary, R. -R.; Chiang, H. C.;
Chluba, J.; Chon, G.; Christensen, P. R.; Church, S.; Clemens, M.;
Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Comis,
B.; Contreras, D.; Couchot, F.; Coulais, A.; Crill, B. P.; Cruz, M.;
Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de
Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis,
J. -M.; Désert, F. -X.; Di Valentino, E.; Dickinson, C.; Diego, J. M.;
Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout,
A.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Eisenhardt, P. R. M.;
Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Fantaye,
Y.; Farhang, M.; Feeney, S.; Fergusson, J.; Fernandez-Cobos, R.; Feroz,
F.; Finelli, F.; Florido, E.; Forni, O.; Frailis, M.; Fraisse, A. A.;
Franceschet, C.; Franceschi, E.; Frejsel, A.; Frolov, A.; Galeotta, S.;
Galli, S.; Ganga, K.; Gauthier, C.; Génova-Santos, R. T.; Gerbino, M.;
Ghosh, T.; Giard, M.; Giraud-Héraud, Y.; Giusarma, E.; Gjerløw, E.;
González-Nuevo, J.; Górski, K. M.; Grainge, K. J. B.; Gratton, S.;
Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Hamann, J.; Handley,
W.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Heavens, A.; Helou,
G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Huang, Z.; Huffenberger, K. M.; Hurier, G.; Ilić, S.;
Jaffe, A. H.; Jaffe, T. R.; Jin, T.; Jones, W. C.; Juvela, M.; Karakci,
A.; Keihänen, E.; Keskitalo, R.; Khamitov, I.; Kiiveri, K.; Kim, J.;
Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Krachmalnicoff, N.;
Kunz, M.; Kurki-Suonio, H.; Lacasa, F.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Langer, M.; Lasenby, A.; Lattanzi, M.; Lawrence,
C. R.; Le Jeune, M.; Leahy, J. P.; Lellouch, E.; Leonardi, R.;
León-Tavares, J.; Lesgourgues, J.; Levrier, F.; Lewis, A.; Liguori,
M.; Lilje, P. B.; Lilley, M.; Linden-Vørnle, M.; Lindholm, V.; Liu,
H.; López-Caniego, M.; Lubin, P. M.; Ma, Y. -Z.; Macías-Pérez,
J. F.; Maggio, G.; Maino, D.; Mak, D. S. Y.; Mandolesi, N.; Mangilli,
A.; Marchini, A.; Marcos-Caballero, A.; Marinucci, D.; Maris, M.;
Marshall, D. J.; Martin, P. G.; Martinelli, M.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Mazzotta, P.; McEwen, J. D.; McGehee,
P.; Mei, S.; Meinhold, P. R.; Melchiorri, A.; Melin, J. -B.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Mikkelsen, K.; Millea, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Molinari, D.; Moneti, A.; Montier,
L.; Moreno, R.; Morgante, G.; Mortlock, D.; Moss, A.; Mottet, S.;
Münchmeyer, M.; Munshi, D.; Murphy, J. A.; Narimani, A.; Naselsky,
P.; Nastasi, A.; Nati, F.; Natoli, P.; Negrello, M.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; Olamaie, M.; Oppermann, N.; Orlando, E.; Oxborrow, C. A.; Paci,
F.; Pagano, L.; Pajot, F.; Paladini, R.; Pandolfi, S.; Paoletti,
D.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Peel,
M.; Peiris, H. V.; Pelkonen, V. -M.; Perdereau, O.; Perotto, L.;
Perrott, Y. C.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pogosyan, D.;
Pointecouteau, E.; Polenta, G.; Popa, L.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Racine, B.; Reach, W. T.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi,
A.; Ristorcelli, I.; Rocha, G.; Roman, M.; Romelli, E.; Rosset,
C.; Rossetti, M.; Rotti, A.; Roudier, G.; Rouillé d'Orfeuil, B.;
Rowan-Robinson, M.; Rubiño-Martín, J. A.; Ruiz-Granados, B.; Rumsey,
C.; Rusholme, B.; Said, N.; Salvatelli, V.; Salvati, L.; Sandri,
M.; Sanghera, H. S.; Santos, D.; Saunders, R. D. E.; Sauvé, A.;
Savelainen, M.; Savini, G.; Schaefer, B. M.; Schammel, M. P.; Scott,
D.; Seiffert, M. D.; Serra, P.; Shellard, E. P. S.; Shimwell, T. W.;
Shiraishi, M.; Smith, K.; Souradeep, T.; Spencer, L. D.; Spinelli,
M.; Stanford, S. A.; Stern, D.; Stolyarov, V.; Stompor, R.; Strong,
A. W.; Sudiwala, R.; Sunyaev, R.; Sutter, P.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.;
Texier, D.; Toffolatti, L.; Tomasi, M.; Tornikoski, M.; Tramonte,
D.; Tristram, M.; Troja, A.; Trombetti, T.; Tucci, M.; Tuovinen, J.;
Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, F.;
Vassallo, T.; Vibert, L.; Vidal, M.; Viel, M.; Vielva, P.; Villa, F.;
Wade, L. A.; Walter, B.; Wandelt, B. D.; Watson, R.; Wehus, I. K.;
Welikala, N.; Weller, J.; White, M.; White, S. D. M.; Wilkinson, A.;
Yvon, D.; Zacchei, A.; Zibin, J. P.; Zonca, A.
2016A&A...594A...1P Altcode: 2015arXiv150201582P
The European Space Agency's Planck satellite, which is dedicated
to studying the early Universe and its subsequent evolution, was
launched on 14 May 2009. It scanned the microwave and submillimetre
sky continuously between 12 August 2009 and 23 October 2013. In
February 2015, ESA and the Planck Collaboration released the second
set of cosmology products based ondata from the entire Planck
mission, including both temperature and polarization, along with a
set of scientific and technical papers and a web-based explanatory
supplement. This paper gives an overview of the main characteristics of
the data and the data products in the release, as well as the associated
cosmological and astrophysical science results and papers. The data
products include maps of the cosmic microwave background (CMB), the
thermal Sunyaev-Zeldovich effect, diffuse foregrounds in temperature
and polarization, catalogues of compact Galactic and extragalactic
sources (including separate catalogues of Sunyaev-Zeldovich clusters
and Galactic cold clumps), and extensive simulations of signals and
noise used in assessing uncertainties and the performance of the
analysis methods. The likelihood code used to assess cosmological
models against the Planck data is described, along with a CMB lensing
likelihood. Scientific results include cosmological parameters derived
from CMB power spectra, gravitational lensing, and cluster counts,
as well as constraints on inflation, non-Gaussianity, primordial
magnetic fields, dark energy, and modified gravity, and new results
on low-frequency Galactic foregrounds.
---------------------------------------------------------
Title: Shapley Supercluster Survey: ram-pressure stripping versus
tidal interactions in the Shapley supercluster
Authors: Merluzzi, P.; Busarello, G.; Dopita, M. A.; Haines, C. P.;
Steinhauser, D.; Bourdin, H.; Mazzotta, P.
2016MNRAS.460.3345M Altcode: 2016arXiv160506329M
We present two new examples of galaxies undergoing transformation in the
Shapley supercluster core. These low-mass (M_{star }∼ 0.4-1× 10^{10}
M<SUB>⊙</SUB>) galaxies are members of the two clusters SC 1329-313 (z
∼ 0.045) and SC 1327-312 (z ∼ 0.049). Integral-field spectroscopy
complemented by imaging in the ugriK bands and in Hα narrow band
is used to disentangle the effects of tidal interaction (TI) and
ram-pressure stripping (RPS). In both galaxies, SOS 61086 and SOS 90630,
we observe one-sided extraplanar ionized gas extending respectively
∼30 and ∼41 kpc in projection from their discs. The galaxies'
gaseous discs are truncated, and the kinematics of the stellar and gas
components are decoupled, supporting the RPS scenario. The emission
of the ionized gas extends in the direction of a possible companion
for both galaxies suggesting a TI. The overall gas velocity field of
SOS 61086 is reproduced by ad hoc N-body/hydrodynamical simulations of
RPS acting almost face-on and starting ∼250 Myr ago, consistent with
the age of the young stellar populations. A link between the observed
gas stripping and the cluster-cluster interaction experienced by SC
1329-313 and A3562 is suggested. Simulations of ram pressure acting
almost edge-on are able to fully reproduce the gas velocity field of
SOS 90630, but cannot at the same time reproduce the extended tail of
outflowing gas. This suggests that an additional disturbance from a
TI is required. This study adds a piece of evidence that RPS may take
place in different environments with different impacts and witnesses
the possible effect of cluster-cluster merger on RPS.
---------------------------------------------------------
Title: The evolution of galaxy groups and clusters
Authors: Mazzotta, Pasquale
2016cosp...41E1271M Altcode:
The Athena mission will implement the Hot and Energetic Universe science
theme which poses the question of How does ordinary matter assemble into
the large-scale structures we see today?. Groups and Galaxy clusters
are key laboratories to understand the role of the various physical
processes governing the baryonic matter from the kilo-parsec scale
of super-massive black holes to the mega-parsec one of the clusters
outskirts on assembling and evolving large scale structures. We will
focus on the study of the galaxy groups and clusters evolution with the
Athen a mission. We will review the status of current constraints in
light of the newest results obtained from state of the art cosmological
simulations and will discuss the perspectives out to the mission launch
time in 2028.
---------------------------------------------------------
Title: Comparing Cool Cores in the Planck SZ Selected Samples of
Clusters of Galaxies with Cool Cores in X-ray Selected Cluster Samples
Authors: Jones, Christine; Santos, Felipe A.; Forman, William R.;
Kraft, Ralph P.; Lovisari, Lorenzo; Arnaud, Monique; Mazzotta,
Pasquale; Van Weeren, Reinout J.; Churazov, Eugene; Ferrari, Chiara;
Borgani, Stefano; Chandra-Planck Collaboration
2016AAS...22811004J Altcode:
The Planck mission provided a representative sample of clusters of
galaxies over the entire sky. With completed Chandra observations
of 165 Planck ESZ and cosmology sample clusters at z<0.35, we can
now characterize each cluster in terms of its X-ray luminosity, gas
temperature, gas mass, total mass, gas entropy, gas central cooling
time, presence of active AGN, gas cavities, radio emission, and cluster
morphology. In this presentation we compare the percentages of cool
core and non-cool core clusters in the Planck-selected clusters with the
percentages in X-ray selected cluster samples. We find a significantly
smaller percentage of cool core clusters in the Planck sample than in
X-ray selected cluster samples. We will discuss the primary reasons for
this smaller percentage of cool-core clusters in the Planck-selected
cluster sample than in X-ray-selected samples.
---------------------------------------------------------
Title: Discovery of an exceptionally bright giant arc at z = 2.369,
gravitationally lensed by the Planck cluster PSZ1 G311.65-18.48
Authors: Dahle, H.; Aghanim, N.; Guennou, L.; Hudelot, P.; Kneissl,
R.; Pointecouteau, E.; Beelen, A.; Bayliss, M.; Douspis, M.; Nesvadba,
N.; Hempel, A.; Gronke, M.; Burenin, R.; Dole, H.; Harrison, D.;
Mazzotta, P.; Sunyaev, R.
2016A&A...590L...4D Altcode:
As part of an all-sky follow-up of the Planck catalogue of
Sunyaev-Zeldovich (SZ) cluster candidates detected in the first
14 months of data, we are observing cluster candidates in the
southern sky in the optical imaging and spectroscopy through an
ESO Large Programme. Inspection of ESO New Technology Telescope
(NTT) R-and z-band imaging data from our programme has revealed an
unusually large and bright arc in the field of PSZ1 G311.65-18.48. We
establish the basic photometric and morphological properties of the
arc and provide conclusive evidence for the gravitational lensing
nature of this object. Guided by the NTT images, we have obtained
a long-slit spectrum with IMACS on the Magellan-I Baade Telescope,
covering a part of the arc and the brightest cluster galaxy of PSZ1
G311.65-18.48. Our imaging data confirm the presence of a galaxy
cluster coinciding (within 0.´6) with the position of the Planck
SZ source. The arc is separated by ~30″ from the brightest cluster
galaxy, which closely coincides with the center of curvature of the
arc. A photometric analysis yields integrated (Vega) magnitudes of
(R,z,J,K<SUB>s</SUB>) = (17.82,17.38,16.75,15.43) for the arc, more
than one magnitude brighter than any previously known lensed arc at z ~
2-3. The arc is a vigorously star-forming galaxy at z = 2.369, while the
Planck SZ cluster lens is at z = 0.443.Even when allowing for lensing
magnifications as high as μ = 100 still leads to the conclusion that
the source galaxy is among the intrinsically most luminous normal
(I.e., non-AGN) galaxies known at z ~ 2-3. <P />FITS files of all
the reduced images are only available at the CDS via anonymous ftp to
<A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
(<A href="http://130.79.128.5">http://130.79.128.5</A>) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/590/L4">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/590/L4</A>
---------------------------------------------------------
Title: Selecting background galaxies in weak-lensing analysis of
galaxy clusters
Authors: Formicola, I.; Radovich, M.; Meneghetti, M.; Mazzotta, P.;
Grado, A.; Giocoli, C.
2016MNRAS.458.2776F Altcode: 2016MNRAS.tmp..285F; 2016arXiv160305690F
In this paper, we present a new method to select the faint, background
galaxies used to derive the mass of galaxy clusters by weak lensing. The
method is based on the simultaneous analysis of the shear signal, that
should be consistent with zero for the foreground, unlensed galaxies,
and of the colours of the galaxies: photometric data from the COSMic
evOlution Survey are used to train the colour selection. In order to
validate this methodology, we test it against a set of state-of-the-art
image simulations of mock galaxy clusters in different redshift
[0.23-0.45] and mass [0.5-1.55 × 10<SUP>15</SUP> M<SUB>⊙</SUB>]
ranges, mimicking medium-deep multicolour imaging observations
[e.g. Subaru, Large Binocular Telescope]. The performance of our
method in terms of contamination by unlensed sources is comparable to a
selection based on photometric redshifts, which however requires a good
spectral coverage and is thus much more observationally demanding. The
application of our method to simulations gives an average ratio between
estimated and true masses of ∼0.98 ± 0.09. As a further test, we
finally apply our method to real data, and compare our results with
other weak-lensing mass estimates in the literature: for this purpose,
we choose the cluster Abell 2219 (z = 0.228), for which multiband
(BVRi) data are publicly available.
---------------------------------------------------------
Title: Planck intermediate results. XXXI. Microwave survey of Galactic
supernova remnants
Authors: Planck Collaboration; Arnaud, M.; Ashdown, M.;
Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.;
Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.; Bernard,
J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Brogan, C. L.; Burigana, C.; Cardoso,
J. -F.; Catalano, A.; Chamballu, A.; Chiang, H. C.; Christensen,
P. R.; Colombi, S.; Colombo, L. P. L.; Crill, B. P.; Curto, A.;
Cuttaia, F.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Désert, F. -X.; Dickinson, C.;
Diego, J. M.; Donzelli, S.; Doré, O.; Dupac, X.; Enßlin, T. A.;
Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.;
Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giraud-Héraud,
Y.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.;
Hansen, F. K.; Harrison, D. L.; Hernández-Monteagudo, C.; Herranz,
D.; Hildebrandt, S. R.; Hobson, M.; Holmes, W. A.; Huffenberger,
K. M.; Jaffe, A. H.; Jaffe, T. R.; Keihänen, E.; Keskitalo, R.;
Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio,
H.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Lawrence,
C. R.; Leonardi, R.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Maino, D.; Maris, M.; Marshall,
D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.;
Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio,
M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.;
Noviello, F.; Novikov, D.; Novikov, I.; Oppermann, N.; Oxborrow,
C. A.; Pagano, L.; Pajot, F.; Paladini, R.; Pasian, F.; Peel, M.;
Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Popa, L.;
Pratt, G. W.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Reich,
W.; Reinecke, M.; Remazeilles, M.; Renault, C.; Rho, J.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier,
G.; Rusholme, B.; Sandri, M.; Savini, G.; Scott, D.; Stolyarov, V.;
Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi,
L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.;
Wade, L. A.; Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...586A.134P Altcode: 2014arXiv1409.5746P
The all-sky Planck survey in 9 frequency bands was used to search
for emission from all 274 known Galactic supernova remnants. Of
these, 16 were detected in at least two Planck frequencies. The
radio-through-microwave spectral energy distributions were compiled to
determine the mechanism for microwave emission. In only one case, IC
443, is there high-frequency emission clearly from dust associated with
the supernova remnant. In all cases, the low-frequency emission is from
synchrotron radiation. As predicted for a population of relativistic
particles with energy distribution that extends continuously to high
energies, a single power law is evident for many sources, including the
Crab and PKS 1209-51/52. A decrease in flux density relative to the
extrapolation of radio emission is evident in several sources. Their
spectral energy distributions can be approximated as broken power
laws, S<SUB>ν</SUB> ∝ ν<SUP>-α</SUP>, with the spectral index,
α, increasing by 0.5-1 above a break frequency in the range 10-60
GHz. The break could be due to synchrotron losses.
---------------------------------------------------------
Title: Planck intermediate results. XXXIII. Signature of the magnetic
field geometry of interstellar filaments in dust polarization maps
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alves,
M. I. R.; Arnaud, M.; Arzoumanian, D.; Aumont, J.; Baccigalupi, C.;
Banday, A. J.; Barreiro, R. B.; Bartolo, N.; Battaner, E.; Benabed,
K.; Benoit-Lévy, A.; Bernard, J. -P.; Berné, O.; Bersanelli, M.;
Bielewicz, P.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Boulanger, F.; Bracco, A.; Burigana, C.; Calabrese,
E.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Chiang, H. C.;
Christensen, P. R.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.;
Combet, C.; Couchot, F.; Crill, B. P.; Curto, A.; Cuttaia, F.;
Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.;
Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Elsner,
F.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Ferrière, K.;
Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi,
E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Ghosh, T.;
Giard, M.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.;
Górski, K. M.; Gregorio, A.; Gruppuso, A.; Guillet, V.; Hansen,
F. K.; Hanson, D.; Harrison, D. L.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.;
Jones, W. C.; Juvela, M.; Keskitalo, R.; Kisner, T. S.; Knoche, J.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.;
Lawrence, C. R.; Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maffei, B.; Mandolesi, N.; Mangilli, A.; Maris, M.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta,
P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati,
F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; Oppermann, N.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Pasian, F.; Perrotta, F.; Pettorino, V.; Piacentini,
F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Pratt, G. W.; Puget, J. -L.; Rachen,
J. P.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi,
A.; Ricciardi, S.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti,
M.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.;
Savelainen, M.; Savini, G.; Scott, D.; Soler, J. D.; Stolyarov, V.;
Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi,
L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Valenziano,
L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.;
Wandelt, B. D.; Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...586A.136P Altcode: 2014arXiv1411.2271P
Planck observations at 353 GHz provide the first fully sampled maps of
the polarized dust emission towards interstellar filaments and their
backgrounds (I.e., the emission observed in the surroundings of the
filaments). The data allow us to determine the intrinsic polarization
properties of the filaments and therefore to provide insight into the
structure of their magnetic field (B). We present the polarization
maps of three nearby (several parsecs long) star-forming filaments
of moderate column density (N<SUB>H</SUB> about 10<SUP>22</SUP>
cm<SUP>-2</SUP>): Musca, B211, and L1506. These three filaments are
detected above the background in dust total and polarized emission. We
use the spatial information to separate Stokes I, Q, and U of the
filaments from those of their backgrounds, an essential step in
measuring the intrinsic polarization fraction (p) and angle (ψ) of each
emission component. We find that the polarization angles in the three
filaments (ψ<SUB>fil</SUB>) are coherent along their lengths and not
the same as in their backgrounds (ψ<SUB>bg</SUB>). The differences
between ψ<SUB>fil</SUB> and ψ<SUB>bg</SUB> are 12° and 54° for
Musca and L1506, respectively, and only 6° in the case of B211. These
differences forMusca and L1506 are larger than the dispersions of ψ,
both along the filaments and in their backgrounds. The observed changes
of ψ are direct evidence of variations of the orientation of the
plane of the sky (POS) projection of the magnetic field. As in previous
studies, we find a decrease of several per cent in p with N<SUB>H</SUB>
from the backgrounds to the crest of the filaments. We show that the
bulk of the drop in p within the filaments cannot be explained by random
fluctuations of the orientation of the magnetic field because they
are too small (σ<SUB>ψ</SUB>< 10°). We recognize the degeneracy
between the dust alignment efficiency (by, e.g., radiative torques)
and the structure of the B-field in causing variations in p, but we
argue that the decrease in p from the backgrounds to the filaments
results in part from depolarization associated with the 3D structure
of the B-field: both its orientation in the POS and with respect to
the POS. We do not resolve the inner structure of the filaments,
but at the smallest scales accessible with Planck (~0.2 pc), the
observed changes of ψ and p hold information on the magnetic field
structure within filaments. They show that both the mean field and
its fluctuations in the filaments are different from those of their
backgrounds, which points to a coupling between the matter and the
B-field in the filament formation process.
---------------------------------------------------------
Title: LoCuSS: Testing hydrostatic equilibrium in galaxy clusters
Authors: Smith, G. P.; Mazzotta, P.; Okabe, N.; Ziparo, F.; Mulroy,
S. L.; Babul, A.; Finoguenov, A.; McCarthy, I. G.; Lieu, M.; Bahé,
Y. M.; Bourdin, H.; Evrard, A. E.; Futamase, T.; Haines, C. P.; Jauzac,
M.; Marrone, D. P.; Martino, R.; May, P. E.; Taylor, J. E.; Umetsu, K.
2016MNRAS.456L..74S Altcode: 2015arXiv151101919S
We test the assumption of hydrostatic equilibrium in an X-ray luminosity
selected sample of 50 galaxy clusters at 0.15 < z < 0.3 from
the Local Cluster Substructure Survey (LoCuSS). Our weak-lensing
measurements of M<SUB>500</SUB> control systematic biases to sub-4 per
cent, and our hydrostatic measurements of the same achieve excellent
agreement between XMM-Newton and Chandra. The mean ratio of X-ray
to lensing mass for these 50 clusters is β_X= 0.95± 0.05, and for
the 44 clusters also detected by Planck, the mean ratio of Planck mass
estimate to LoCuSS lensing mass is β_P= 0.95± 0.04. Based on a careful
like-for-like analysis, we find that LoCuSS, the Canadian Cluster
Comparison Project, and Weighing the Giants agree on β_P ≃ 0.9-0.95
at 0.15 < z < 0.3. This small level of hydrostatic bias disagrees
at ∼5σ with the level required to reconcile Planck cosmology results
from the cosmic microwave background and galaxy cluster counts.
---------------------------------------------------------
Title: Planck intermediate results. XXXII. The relative orientation
between the magnetic field and structures traced by interstellar dust
Authors: Planck Collaboration; Adam, R.; Ade, P. A. R.; Aghanim, N.;
Alves, M. I. R.; Arnaud, M.; Arzoumanian, D.; Ashdown, M.; Aumont, J.;
Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartolo, N.; Battaner,
E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.;
Bielewicz, P.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Boulanger, F.; Bracco, A.; Burigana, C.; Butler, R. C.;
Calabrese, E.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Chiang,
H. C.; Christensen, P. R.; Colombi, S.; Colombo, L. P. L.; Combet,
C.; Couchot, F.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.;
Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli,
S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.;
Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Ferrière,
K.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi,
E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga, K.; Ghosh, T.; Giard,
M.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gregorio,
A.; Gruppuso, A.; Guillet, V.; Hansen, F. K.; Hanson, D.; Harrison,
D. L.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest, W.;
Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jones,
W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.;
Lamarre, J. -M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Leonardi,
R.; Levrier, F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta,
P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.;
Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante, G.;
Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Natoli, P.;
Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.;
Oppermann, N.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paoletti,
D.; Pasian, F.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino,
V.; Piacentini, F.; Piat, M.; Plaszczynski, S.; Pointecouteau, E.;
Polenta, G.; Ponthieu, N.; Popa, L.; Pratt, G. W.; Prunet, S.; Puget,
J. -L.; Rachen, J. P.; Reach, W. T.; Reinecke, M.; Remazeilles, M.;
Renault, C.; Ristorcelli, I.; Rocha, G.; Roudier, G.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.;
Soler, J. D.; Spencer, L. D.; Stolyarov, V.; Sudiwala, R.; Sunyaev,
R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.;
Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Wiesemeyer,
H.; Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...586A.135P Altcode: 2014arXiv1409.6728P
The role of the magnetic field in the formation of the filamentary
structures observed in the interstellar medium (ISM) is a debated
topic owing to the paucity of relevant observations needed to test
existing models. The Planck all-sky maps of linearly polarized emission
from dust at 353 GHz provide the required combination of imaging and
statistics to study the correlation between the structures of the
Galactic magnetic field and of interstellar matter over the whole
sky, both in the diffuse ISM and in molecular clouds. The data reveal
that structures, or ridges, in the intensity map have counterparts
in the Stokes Q and/or U maps. We focus our study on structures at
intermediate and high Galactic latitudes, which cover two orders of
magnitude in column density, from 10<SUP>20</SUP> to 10<SUP>22</SUP>
cm<SUP>-2</SUP>. We measure the magnetic field orientation on the
plane ofthe sky from the polarization data, and present an algorithm to
estimate the orientation of the ridges from the dust intensity map. We
use analytical models to account for projection effects. Comparing
polarization angles on and off the structures, we estimate the mean
ratio between the strengths of the turbulent and mean components of
the magnetic field to be between 0.6 and 1.0, with a preferred value
of 0.8. We find that the ridges are usually aligned with the magnetic
field measured on the structures. This statistical trend becomes
more striking for increasing polarization fraction and decreasing
column density. There is no alignment for the highest column density
ridges. We interpret the increase in alignment with polarization
fraction as a consequence of projection effects. We present maps to
show that the decrease in alignment for high column density is not due
to a loss of correlation between the distribution of matter and the
geometry of the magnetic field. In molecular complexes, we also observe
structures perpendicular to the magnetic field, which, statistically,
cannot be accounted for by projection effects. This first statistical
study of the relative orientation between the matter structures and
the magnetic field in the ISM points out that, at the angular scales
probed by Planck, the field geometry projected on the plane of the
sky is correlated with the distribution of matter. In the diffuse ISM,
the structures of matter are usually aligned with the magnetic field,
while perpendicular structures appear in molecular clouds. We discuss
our results in the context of models and MHD simulations, which attempt
to describe the respective roles of turbulence, magnetic field, and
self-gravity in the formation of structures in the magnetized ISM.
---------------------------------------------------------
Title: Planck intermediate results. XXX. The angular power spectrum
of polarized dust emission at intermediate and high Galactic latitudes
Authors: Planck Collaboration; Adam, R.; Ade, P. A. R.; Aghanim, N.;
Arnaud, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Bartlett, J. G.; Bartolo, N.; Battaner, E.; Benabed, K.;
Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.;
Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Boulanger, F.; Bracco, A.; Bucher, M.; Burigana, C.; Butler, R. C.;
Calabrese, E.; Cardoso, J. -F.; Catalano, A.; Challinor, A.; Chamballu,
A.; Chary, R. -R.; Chiang, H. C.; Christensen, P. R.; Clements,
D. L.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Couchot, F.;
Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies,
R. D.; Davis, R. J.; de Bernardis, P.; de Zotti, G.; Delabrouille,
J.; Delouis, J. -M.; Désert, F. -X.; Dickinson, C.; Diego, J. M.;
Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.;
Dunkley, J.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.;
Eriksen, H. K.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis, M.;
Fraisse, A. A.; Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli,
S.; Ganga, K.; Ghosh, T.; Giard, M.; Giraud-Héraud, Y.; Gjerløw,
E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Guillet, V.; Hansen, F. K.; Hanson, D.; Harrison, D. L.;
Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz,
D.; Hivon, E.; Hobson, M.; Holmes, W. A.; Huffenberger, K. M.; Hurier,
G.; Jaffe, A. H.; Jaffe, T. R.; Jewell, J.; Jones, W. C.; Juvela, M.;
Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.;
Knox, L.; Krachmalnicoff, N.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lamarre, J. -M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.;
Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Levrier, F.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Mangilli,
A.; Maris, M.; Martin, P. G.; Martínez-González, E.; Masi, S.;
Matarrese, S.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss,
A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.;
Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Pratt, G. W.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Remazeilles,
M.; Renault, C.; Renzi, A.; Ricciardi, S.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rouillé d'Orfeuil,
B.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.;
Savelainen, M.; Savini, G.; Scott, D.; Soler, J. D.; Spencer, L. D.;
Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Vibert, L.; Vielva, P.;
Villa, F.; Wade, L. A.; Wandelt, B. D.; Watson, R.; Wehus, I. K.;
White, M.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...586A.133P Altcode: 2014arXiv1409.5738P
The polarized thermal emission from diffuse Galactic dust is the
main foreground present in measurements of the polarization of the
cosmic microwave background (CMB) at frequencies above 100 GHz. In
this paper we exploit the uniqueness of the Planck HFI polarization
data from 100 to 353 GHz to measure the polarized dust angular power
spectra C<SUB>ℓ</SUB><SUP>EE</SUP> and C<SUB>ℓ</SUB><SUP>BB</SUP>
over the multipole range 40 <ℓ< 600 well away from the Galactic
plane. These measurements will bring new insights into interstellar dust
physics and allow a precise determination of the level of contamination
for CMB polarization experiments. Despite the non-Gaussian and
anisotropic nature of Galactic dust, we show that general statistical
properties of the emission can be characterized accurately over large
fractions of the sky using angular power spectra. The polarization
power spectra of the dust are well described by power laws in multipole,
C<SUB>ℓ</SUB> ∝ ℓ<SUP>α</SUP>, with exponents α<SUP>EE,BB</SUP>
= -2.42 ± 0.02. The amplitudes of the polarization power spectra vary
with the average brightness in a way similar to the intensity power
spectra. The frequency dependence of the dust polarization spectra is
consistent with modified blackbody emission with β<SUB>d</SUB> = 1.59
and T<SUB>d</SUB> = 19.6 K down to the lowest Planck HFI frequencies. We
find a systematic difference between the amplitudes of the Galactic B-
and E-modes, C<SUB>ℓ</SUB><SUP>BB</SUP>/C<SUB>ℓ</SUB><SUP>EE</SUP> =
0.5. We verify that these general properties are preserved towards high
Galactic latitudes with low dust column densities. We show that even
in the faintest dust-emitting regions there are no "clean" windows in
the sky where primordial CMB B-mode polarization measurements could be
made without subtraction of foreground emission. Finally, we investigate
the level of dust polarization in the specific field recently targeted
by the BICEP2 experiment. Extrapolation of the Planck 353 GHz data
to 150 GHz gives a dust power 𝒟<SUB>ℓ</SUB><SUP>BB</SUP> ≡
ℓ(ℓ+1)C<SUB>ℓ</SUB><SUP>BB</SUP>/(2π) of 1.32 × 10<SUP>-2</SUP>
μK<SUB>CMB</SUB><SUP>2</SUP> over the multipole range of the primordial
recombination bump (40 <ℓ< 120); the statistical uncertainty
is ± 0.29 × 10<SUP>-2</SUP> μK<SUB>CMB</SUB><SUP>2</SUP> and
there is an additional uncertainty (+0.28, -0.24) × 10<SUP>-2</SUP>
μK<SUB>CMB</SUB><SUP>2</SUP> from the extrapolation. This level is
the same magnitude as reported by BICEP2 over this ℓ range, which
highlights the need for assessment of the polarized dust signal even
in the cleanest windows of the sky.
---------------------------------------------------------
Title: Planck intermediate results. XXIX. All-sky dust modelling
with Planck, IRAS, and WISE observations
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alves,
M. I. R.; Aniano, G.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Barreiro, R. B.; Bartolo, N.; Battaner, E.;
Benabed, K.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.;
Bielewicz, P.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill,
J.; Bouchet, F. R.; Boulanger, F.; Burigana, C.; Butler, R. C.;
Calabrese, E.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Chiang,
H. C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Colombo,
L. P. L.; Couchot, F.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese,
L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.;
de Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dole,
H.; Donzelli, S.; Doré, O.; Douspis, M.; Draine, B. T.; Ducout,
A.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen,
H. K.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse,
A. A.; Franceschi, E.; Frejsel, A.; Galeotta, S.; Galli, S.; Ganga,
K.; Ghosh, T.; Giard, M.; Gjerløw, E.; González-Nuevo, J.; Górski,
K. M.; Gregorio, A.; Gruppuso, A.; Guillet, V.; Hansen, F. K.; Hanson,
D.; Harrison, D. L.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Holmes, W. A.; Hovest, W.;
Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jones,
W. C.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.;
Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.;
Lasenby, A.; Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Levrier,
F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi,
N.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy,
J. A.; Naselsky, P.; Natoli, P.; Nørgaard-Nielsen, H. U.; Novikov,
D.; Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini,
R.; Paoletti, D.; Pasian, F.; Perdereau, O.; Perotto, L.; Perrotta,
F.; Pettorino, V.; Piacentini, F.; Piat, M.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Pratt, G. W.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ristorcelli, I.; Rocha,
G.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.;
Santos, D.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Sudiwala, R.;
Sunyaev, R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber,
J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci,
M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva,
P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Ysard, N.;
Yvon, D.; Zacchei, A.; Zonca, A.
2016A&A...586A.132P Altcode: 2014arXiv1409.2495P; 2014arXiv1409.2495A
We present all-sky modelling of the high resolution Planck, IRAS,
and WISE infrared (IR) observations using the physical dust model
presented by Draine & Li in 2007 (DL, ApJ, 657, 810). We study the
performance and results of this model, and discuss implications for
future dust modelling. The present work extends the DL dust modelling
carried out on nearby galaxies using Herschel and Spitzer data to
Galactic dust emission. We employ the DL dust model to generate maps
of the dust mass surface density Σ<SUB>M<SUB>d</SUB></SUB>, the
dust optical extinction A<SUB>V</SUB>, and the starlight intensity
heating the bulk of the dust, parametrized by U<SUB>min</SUB>. The
DL model reproduces the observed spectral energy distribution (SED)
satisfactorily over most of the sky, with small deviations in the
inner Galactic disk and in low ecliptic latitude areas, presumably
due to zodiacal light contamination. In the Andromeda galaxy (M31),
the present dust mass estimates agree remarkably well (within 10%)
with DL estimates based on independent Spitzer and Herschel data. We
compare the DL optical extinction A<SUB>V</SUB> for the diffuse
interstellar medium (ISM) with optical estimates for approximately 2
× 10<SUP>5</SUP> quasi-stellar objects (QSOs) observed inthe Sloan
Digital Sky Survey (SDSS). The DL A<SUB>V</SUB> estimates are larger
than those determined towards QSOs by a factor of about 2, which
depends on U<SUB>min</SUB>. The DL fitting parameter U<SUB>min</SUB>,
effectively determined by the wavelength where the SED peaks, appears
to trace variations in the far-IR opacity of the dust grains per unit
A<SUB>V</SUB>, and not only in the starlight intensity. These results
show that some of the physical assumptions of the DL model will need
to be revised. To circumvent the model deficiency, we propose an
empirical renormalization of the DL A<SUB>V</SUB> estimate, dependent
of U<SUB>min</SUB>, which compensates for the systematic differences
found with QSO observations. This renormalization, made to match the
A<SUB>V</SUB> estimates towards QSOs, also brings into agreement the DL
A<SUB>V</SUB> estimates with those derived for molecular clouds from the
near-IR colours of stars in the 2 micron all sky survey (2MASS). The
DL model and the QSOs data are also used to compress the spectral
information in the Planck and IRAS observations for the diffuse ISM
to a family of 20 SEDs normalized per A<SUB>V</SUB>, parameterized by
U<SUB>min</SUB>, which may be used to test and empirically calibrate
dust models. The family of SEDs and the maps generated with the DL
model are made public in the Planck Legacy Archive.
---------------------------------------------------------
Title: Spectral Imaging of Galaxy Clusters with Planck
Authors: Bourdin, H.; Mazzotta, P.; Rasia, E.
2015ApJ...815...92B Altcode: 2016arXiv160106323B
The Sunyaev-Zeldovich (SZ) effect is a promising tool for detecting
the presence of hot gas out to the galaxy cluster peripheries. We
developed a spectral imaging algorithm dedicated to the SZ observations
of nearby galaxy clusters with Planck, with the aim of revealing
gas density anisotropies related to the filamentary accretion of
materials, or pressure discontinuities induced by the propagation of
shock fronts. To optimize an unavoidable trade-off between angular
resolution and precision of the SZ flux measurements, the algorithm
performs a multi-scale analysis of the SZ maps as well as of other
extended components, such as the cosmic microwave background (CMB)
anisotropies and the Galactic thermal dust. The demixing of the SZ
signal is tackled through kernel-weighted likelihood maximizations. The
CMB anisotropies are further analyzed through a wavelet analysis,
while the Galactic foregrounds and SZ maps are analyzed via a curvelet
analysis that best preserves their anisotropic details. The algorithm
performance has been tested against mock observations of galaxy
clusters obtained by simulating the Planck High Frequency Instrument
and by pointing at a few characteristic positions in the sky. These
tests suggest that Planck should easily allow us to detect filaments
in the cluster peripheries and detect large-scale shocks in colliding
galaxy clusters that feature favorable geometry.
---------------------------------------------------------
Title: A Multi-wavelength Mass Analysis of RCS2 J232727.6-020437,
A ∼3 × 10<SUP>15</SUP> M<SUB>⊙</SUB> Galaxy Cluster at z = 0.7
Authors: Sharon, K.; Gladders, M. D.; Marrone, D. P.; Hoekstra,
H.; Rasia, E.; Bourdin, H.; Gifford, D.; Hicks, A. K.; Greer, C.;
Mroczkowski, T.; Barrientos, L. F.; Bayliss, M.; Carlstrom, J. E.;
Gilbank, D. G.; Gralla, M.; Hlavacek-Larrondo, J.; Leitch, E.;
Mazzotta, P.; Miller, C.; Muchovej, S. J. C.; Schrabback, T.; Yee,
H. K. C.; RCS-Team
2015ApJ...814...21S Altcode: 2015arXiv150307188S
We present an initial study of the mass and evolutionary state of a
massive and distant cluster, RCS2 J232727.6-020437. This cluster, at z
= 0.6986, is the richest cluster discovered in the RCS2 project. The
mass measurements presented in this paper are derived from all
possible mass proxies: X-ray measurements, weak-lensing shear,
strong lensing, Sunyaev-Zel’dovich effect decrement, the velocity
distribution of cluster member galaxies, and galaxy richness. While
each of these observables probe the mass of the cluster at a different
radius, they all indicate that RCS2 J232727.6-020437 is among the
most massive clusters at this redshift, with an estimated mass of
{M}<SUB>200</SUB>∼ 3× {10}<SUP>15</SUP>{h}<SUB>70</SUB><SUP>-1</SUP>
{M}<SUB>⊙ </SUB>. In this paper, we demonstrate that the various
observables are all reasonably consistent with each other to within
their uncertainties. RCS2 J232727.6-020437 appears to be well
relaxed—with circular and concentric X-ray isophotes, with a cool
core, and no indication of significant substructure in extensive
galaxy velocity data. <P />Based on observations obtained with :
MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the
Canada-France-Hawaii Telescope (CFHT) which is operated by the National
Research Council (NRC) of Canada, the Institut National des Science de
l’Univers of the Centre National de la Recherche Scientifique (CNRS)
of France, and the University of Hawaii; the NASA/ESA Hubble Space
Telescope (HST), obtained from the data archive at the Space Telescope
Institute. STScI is operated by the association of Universities for
Research in Astronomy, Inc. under the NASA contract NAS 5-2655; the
6.5 m Magellan telescopes located at Las Campanas Observatory, Chile;
---------------------------------------------------------
Title: Hot coronae around spiral galaxies: Probing the first
principles of galaxy formation
Authors: Bogdán, Ákos; Forman, William; Volgelsberger, Mark;
Mazzotta, Pasquale; Kraft, Ralph; Joes, Christine; Churazov, Eugene;
Bourdin, Hervé
2015xrvw.confE...5B Altcode:
The presence of hot gaseous coronae in the dark matter halos
of massive spiral galaxies is a fundamental prediction of all
structure formation models. Yet these coronae remained unexplored for
several decades, thereby posing a serious challenge to observers and
theorists. Although several X-ray coronae have been detected around
nearby massive spiral galaxies in the past few years, we still lack
a comprehensive picture. X-ray Surveyor will provide the much needed
breakthrough. Specifically, X-ray Surveyor will characterize the hot
coronae in unprecedented details, explore their evolution as a function
of redshift, which in turn will constrain the physical processes that
play an essential role in galaxy formation from the early Universe to
the present epoch.
---------------------------------------------------------
Title: Planck intermediate results. XXVIII. Interstellar gas and
dust in the Chamaeleon clouds as seen by Fermi LAT and Planck
Authors: Planck Collaboration; Fermi Collaboration; Ade, P. A. R.;
Aghanim, N.; Aniano, G.; Arnaud, M.; Ashdown, M.; Aumont, J.;
Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartolo, N.; Battaner,
E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.;
Bielewicz, P.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Boulanger, F.; Burigana, C.; Butler, R. C.; Calabrese,
E.; Cardoso, J. -F.; Casandjian, J. M.; Catalano, A.; Chamballu,
A.; Chiang, H. C.; Christensen, P. R.; Colombo, L. P. L.; Combet,
C.; Couchot, F.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.;
Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Désert, F. -X.; Dickinson, C.; Diego, J. M.;
Digel, S. W.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout,
A.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen,
H. K.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse,
A. A.; Franceschi, E.; Frejsel, A.; Fukui, Y.; Galeotta, S.; Galli,
S.; Ganga, K.; Ghosh, T.; Giard, M.; Gjerløw, E.; González-Nuevo,
J.; Górski, K. M.; Gregorio, A.; Grenier, I. A.; Gruppuso, A.;
Hansen, F. K.; Hanson, D.; Harrison, D. L.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon,
E.; Hobson, M.; Holmes, W. A.; Hovest, W.; Huffenberger, K. M.;
Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.;
Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.;
Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Levrier, F.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris,
M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi,
S.; Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella,
A.; Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier,
L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky,
P.; Natoli, P.; Nørgaard-Nielsen, H. U.; Novikov, D.; Novikov, I.;
Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.;
Pasian, F.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.;
Piacentini, F.; Piat, M.; Plaszczynski, S.; Pointecouteau, E.; Polenta,
G.; Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.;
Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault,
C.; Ristorcelli, I.; Rocha, G.; Roudier, G.; Rusholme, B.; Sandri,
M.; Santos, D.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Strong,
A. W.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski, A. -S.;
Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Tibaldo, L.; Toffolatti,
L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.; Valenziano, L.;
Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.;
Wandelt, B. D.; Wehus, I. K.; Yvon, D.; Zacchei, A.; Zonca, A.
2015A&A...582A..31P Altcode: 2014arXiv1409.3268P; 2015A&A...582A..31A
The nearby Chamaeleon clouds have been observed in γ rays by the
Fermi Large Area Telescope (LAT) and in thermal dust emission by
Planck and IRAS. Cosmic rays and large dust grains, if smoothly
mixed with gas, can jointly serve with the H i and <SUP>12</SUP>CO
radio data to (i) map the hydrogen column densities, N<SUB>H</SUB>,
in the different gas phases, in particular at the dark neutral medium
(DNM) transition between the H i-bright and CO-bright media; (ii)
constrain the CO-to-H<SUB>2</SUB> conversion factor, X<SUB>CO</SUB>;
and (iii) probe the dust properties per gas nucleon in each phase and
map their spatial variations across the clouds. We have separated
clouds at local, intermediate, and Galactic velocities in H i and
<SUP>12</SUP>CO line emission to model in parallel the γ-ray intensity
recorded between 0.4 and 100 GeV; the dust optical depth at 353 GHz,
τ<SUB>353</SUB>; the thermal radiance of the large grains; and an
estimate of the dust extinction, A<SUB>VQ</SUB>, empirically corrected
for the starlight intensity. The dust and γ-ray models have been
coupled to account for the DNM gas. The consistent γ-ray emissivity
spectra recorded in the different phases confirm that the GeV-TeV
cosmic rays probed by the LAT uniformly permeate all gas phases up to
the <SUP>12</SUP>CO cores. The dust and cosmic rays both reveal large
amounts of DNM gas, with comparable spatial distributions and twice
as much mass as in the CO-bright clouds. We give constraints on the H
i-DNM-CO transitions for five separate clouds. CO-dark H<SUB>2</SUB>
dominates the molecular columns up to A<SUB>V</SUB> ≃ 0.9 and its
mass often exceeds the one-third of the molecular mass expected by
theory. The corrected A<SUB>VQ</SUB> extinction largely provides the
best fit to the total gas traced by the γ rays. Nevertheless, we
find evidence for a marked rise in A<SUB>VQ</SUB>/N<SUB>H</SUB> with
increasing N<SUB>H</SUB> and molecular fraction, and with decreasing
dust temperature. The rise in τ<SUB>353</SUB>/N<SUB>H</SUB> is even
steeper. We observe variations of lesser amplitude and orderliness
for the specific power of the grains, except for a coherent decline
by half in the CO cores. This combined information suggests grain
evolution. We provide average values for the dust properties per
gas nucleon in the different phases. The γ rays and dust radiance
yield consistent X<SUB>CO</SUB> estimates near 0.7 × 10<SUP>20</SUP>
cm<SUP>-2</SUP> K<SUP>-1</SUP> km<SUP>-1</SUP> s. The A<SUB>VQ</SUB> and
τ<SUB>353</SUB> tracers yield biased values because of the large rise
in grain opacity in the CO clouds. These results clarify a recurrent
disparity in the γ-ray versus dust calibration of X<SUB>CO</SUB>,
but they confirm the factor of 2 difference found between the
X<SUB>CO</SUB> estimates in nearby clouds and in the neighbouring
spiral arms. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424955/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck intermediate results. XXV. The Andromeda galaxy as
seen by Planck
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Bartolo, N.; Battaner, E.; Battye, R.; Benabed, K.; Bendo,
G. J.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Burigana, C.; Butler, R. C.; Calabrese, E.; Cardoso, J. -F.;
Catalano, A.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, H. C.;
Christensen, P. R.; Clements, D. L.; Colombo, L. P. L.; Combet,
C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.;
Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.;
Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.;
Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Finelli,
F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Frejsel,
A.; Galeotta, S.; Ganga, K.; Giard, M.; Giraud-Héraud, Y.; Gjerløw,
E.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso,
A.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Henrot-Versillé,
S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.;
Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.;
Huffenberger, K. M.; Hurier, G.; Israel, F. P.; Jaffe, A. H.;
Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo,
R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.;
Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Levrier, F.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Madden, S.; Maffei, B.; Maino, D.; Mandolesi,
N.; Maris, M.; Martin, P. G.; Martínez-González, E.; Masi, S.;
Matarrese, S.; Mazzotta, P.; Mendes, L.; Mennella, A.; Migliaccio,
M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati,
F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.;
Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Partridge, B.; Pasian, F.; Pearson, T. J.; Peel, M.;
Perdereau, O.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi,
S.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier,
G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.;
Scott, D.; Spencer, L. D.; Stolyarov, V.; Sudiwala, R.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.;
Wade, L. A.; Wandelt, B. D.; Watson, R.; Wehus, I. K.; Yvon, D.;
Zacchei, A.; Zonca, A.
2015A&A...582A..28P Altcode: 2014arXiv1407.5452P; 2014arXiv1407.5452A
The Andromeda galaxy (M 31) is one of a few galaxies that has
sufficient angular size on the sky to be resolved by the Planck
satellite. Planck has detected M 31 in all of its frequency bands, and
has mapped out the dust emission with the High Frequency Instrument,
clearly resolving multiple spiralarms and sub-features. We examine the
morphology of this long-wavelength dust emission as seen by Planck,
including a study of its outermost spiral arms, and investigate the
dust heating mechanism across M 31. We find that dust dominating
the longer wavelength emission (≳0.3 mm) is heated by the diffuse
stellar population (as traced by 3.6 μm emission), with the dust
dominating the shorter wavelength emission heated by a mix of the
old stellar population and star-forming regions (as traced by 24 μm
emission). We also fit spectral energy distributions for individual
5' pixels and quantify the dust properties across the galaxy, taking
into account these different heating mechanisms, finding that there
is a linear decrease in temperature with galactocentric distance for
dust heated by the old stellar population, as would be expected, with
temperatures ranging from around 22 K in the nucleus to 14 K outside
of the 10 kpc ring. Finally, we measure the integrated spectrum of
the whole galaxy, which we find to be well-fitted with a global dust
temperature of (18.2 ± 1.0) K with a spectral index of 1.62 ± 0.11
(assuming a single modified blackbody), and a significant amount of
free-free emission at intermediate frequencies of 20-60 GHz, which
corresponds to a star formation rate of around 0.12 M<SUB>⊙</SUB>
yr<SUP>-1</SUP>. We find a 2.3σ detection of the presence of spinning
dust emission, with a 30 GHz amplitude of 0.7 ± 0.3 Jy, which is in
line with expectations from our Galaxy.
---------------------------------------------------------
Title: Planck intermediate results. XXVI. Optical identification
and redshifts of Planck clusters with the RTT150 telescope
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.;
Barreiro, R. B.; Barrena, R.; Bartolo, N.; Battaner, E.; Benabed,
K.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.;
Bikmaev, I.; Böhringer, H.; Bonaldi, A.; Bonavera, L.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Burenin, R.; Burigana, C.; Butler, R. C.;
Calabrese, E.; Carvalho, P.; Catalano, A.; Chamballu, A.; Chiang,
H. C.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements, D. L.;
Colombo, L. P. L.; Comis, B.; Couchot, F.; Curto, A.; Cuttaia, F.;
Dahle, H.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.;
de Rosa, A.; de Zotti, G.; Delabrouille, J.; Diego, J. M.; Dole, H.;
Doré, O.; Douspis, M.; Ducout, A.; Dupac, X.; Efstathiou, G.; Elsner,
F.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Flores-Cacho, I.;
Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Frejsel, A.;
Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard,
M.; Gilfanov, M.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo,
J.; Górski, K. M.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison,
D. L.; Hempel, A.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.;
Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo,
R.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz,
M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.;
Lattanzi, M.; Lawrence, C. R.; Leonardi, R.; Levrier, F.; Liguori,
M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; Maino, D.; Mandolesi, N.; Maris, M.;
Martin, P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.;
Mazzotta, P.; Melin, J. -B.; Mendes, L.; Mennella, A.; Migliaccio,
M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati,
F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Novikov, D.; Novikov, I.;
Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.;
Perdereau, O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini,
F.; Piat, M.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.;
Polenta, G.; Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi,
S.; Ristorcelli, I.; Rocha, G.; Roman, M.; Rosset, C.; Rossetti, M.;
Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Scott,
D.; Spencer, L. D.; Stolyarov, V.; Sudiwala, R.; Sunyaev, R.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Valenziano, L.;
Valiviita, J.; Van Tent, B.; Vibert, L.; Vielva, P.; Villa, F.; Wade,
L. A.; Wandelt, B. D.; Wehus, I. K.; Yvon, D.; Zacchei, A.; Zonca, A.
2015A&A...582A..29P Altcode: 2014arXiv1407.6663P
We present the results of approximately three years of observations
of Planck Sunyaev-Zeldovich (SZ) sources with the Russian-Turkish 1.5
m telescope (RTT150), as a part of the optical follow-up programme
undertaken by the Planck collaboration. During this time period
approximately 20% of all dark and grey clear time available at
the telescope was devoted to observations of Planck objects. Some
observations of distant clusters were also done at the 6 m Bolshoi
Telescope Alt-azimutalnyi (BTA) of the Special Astrophysical Observatory
of the Russian Academy of Sciences. In total, deep, direct images of
more than one hundred fields were obtained in multiple filters. We
identified 47 previously unknown galaxy clusters, 41 of which are
included in the Planck catalogue of SZ sources. The redshifts of
65 Planck clusters were measured spectroscopically and 14 more were
measured photometrically. We discuss the details of cluster optical
identifications and redshift measurements. We also present new
spectroscopic redshifts for 39 Planck clusters that were not included
in the Planck SZ source catalogue and are published here for the
first time.
---------------------------------------------------------
Title: Planck intermediate results. XXVII. High-redshift infrared
galaxy overdensity candidates and lensed sources discovered by Planck
and confirmed by Herschel-SPIRE
Authors: Planck Collaboration; Aghanim, N.; Altieri, B.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.;
Barreiro, R. B.; Bartolo, N.; Battaner, E.; Beelen, A.; Benabed, K.;
Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bethermin, M.;
Bielewicz, P.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Boulanger, F.; Burigana, C.; Calabrese, E.; Canameras, R.; Cardoso,
J. -F.; Catalano, A.; Chamballu, A.; Chary, R. -R.; Chiang, H. C.;
Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.; Crill,
B. P.; Curto, A.; Danese, L.; Dassas, K.; Davies, R. D.; Davis, R. J.;
de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Diego,
J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.;
Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Falgarone, E.;
Flores-Cacho, I.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi,
E.; Frejsel, A.; Frye, B.; Galeotta, S.; Galli, S.; Ganga, K.; Giard,
M.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.;
Gruppuso, A.; Guéry, D.; Hansen, F. K.; Hanson, D.; Harrison, D. L.;
Helou, G.; Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hovest, W.; Huffenberger, K. M.; Hurier,
G.; Jaffe, A. H.; Jaffe, T. R.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lamarre, J. -M.; Lasenby, A.; Lattanzi, M.; Lawrence, C. R.;
Le Floc'h, E.; Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; MacKenzie, T.; Maffei, B.; Mandolesi, N.; Maris, M.; Martin,
P. G.; Martinache, C.; Martínez-González, E.; Masi, S.; Matarrese,
S.; Mazzotta, P.; Melchiorri, A.; Mennella, A.; Migliaccio, M.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy,
J. A.; Natoli, P.; Negrello, M.; Nesvadba, N. P. H.; Novikov, D.;
Novikov, I.; Omont, A.; Pagano, L.; Pajot, F.; Pasian, F.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat,
M.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Popa, L.;
Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ristorcelli, I.; Rocha,
G.; Roudier, G.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.;
Scott, D.; Spencer, L. D.; Stolyarov, V.; Sunyaev, R.; Sutton, D.;
Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Tristram, M.; Tucci, M.; Umana, G.; Valenziano, L.; Valiviita, J.;
Valtchanov, I.; Van Tent, B.; Vieira, J. D.; Vielva, P.; Wade, L. A.;
Wandelt, B. D.; Wehus, I. K.; Welikala, N.; Zacchei, A.; Zonca, A.
2015A&A...582A..30P Altcode: 2015arXiv150308773P
We have used the Planck all-sky submillimetre and millimetre maps
to search for rare sources distinguished by extreme brightness, a
few hundred millijanskies, and their potential for being situated at
high redshift. These "cold" Planck sources, selected using the High
Frequency Instrument (HFI) directly from the maps and from the Planck
Catalogue of Compact Sources (PCCS), all satisfy the criterion of having
their rest-frame far-infrared peak redshifted to the frequency range
353-857 GHz. This colour-selection favours galaxies in the redshift
range z = 2-4, which we consider as cold peaks in the cosmic infrared
background. With a 4.´5 beam at the four highest frequencies, our
sample is expected to include overdensities of galaxies in groups or
clusters, lensed galaxies, and chance line-of-sight projections. We
perform a dedicated Herschel-SPIRE follow-up of 234 such Planck
targets, finding a significant excess of red 350 and 500μm sources, in
comparison to reference SPIRE fields. About 94% of the SPIRE sources in
the Planck fields are consistent with being overdensities of galaxies
peaking at 350μm, with 3% peaking at 500μm, and none peaking at
250μm. About 3% are candidate lensed systems, all 12 of which have
secure spectroscopic confirmations, placing them at redshifts z>
2.2. Only four targets are Galactic cirrus, yielding a success rate
in our search strategy for identifying extragalactic sources within
the Planck beam of better than 98%. The galaxy overdensities are
detected with high significance, half of the sample showing statistical
significance above 10σ. The SPIRE photometric redshifts of galaxies
in overdensities suggest a peak at z ≃ 2, assuming a single common
dust temperature for the sources of T<SUB>d</SUB> = 35 K. Under this
assumption, we derive an infrared (IR) luminosity for each SPIRE
source of about 4 × 10<SUP>12</SUP>L<SUB>⊙</SUB>, yielding star
formation rates of typically 700 M<SUB>⊙</SUB> yr<SUP>-1</SUP>. If
the observed overdensities are actual gravitationally-bound structures,
the total IR luminosity of all their SPIRE-detected sources peaks at
4 × 10<SUP>13</SUP>L<SUB>⊙</SUB>, leading to total star formation
rates of perhaps 7 × 10<SUP>3</SUP>M<SUB>⊙</SUB> yr<SUP>-1</SUP>
per overdensity. Taken together, these sources show the signatures
of high-z (z> 2) protoclusters of intensively star-forming
galaxies. All these observations confirm the uniqueness of our
sample compared to reference samples and demonstrate the ability
of the all-skyPlanck-HFI cold sources to select populations of
cosmological and astrophysical interest for structure formation
studies. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424790/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Evolution of Entropy Profiles in Simulated Clusters
Authors: Rasia, Elena; Troung, Nhut; Borgani, Stefano; Planelles,
Susana; Biffi, Veronica; Murante, Giuseppe; Mazzotta, Pasquale;
Bourdin, Herve
2015eheu.conf...18R Altcode:
Our new set of simulations reproduce the observed dichotomy betweencool
core and non-cool core clusters. The objects, simulated with an improved
hydrodynamical scheme and a new BH feedback prescription, areconsisten
with their observation regarding the entropy, temperature,gas density,
metallicity profiles. In this presentation we will focus on the entropy
profiles and its evolution. Forecasts for Athena'sobservations will
be drawn.
---------------------------------------------------------
Title: Planck 2013 results. XXXII. The updated Planck catalogue of
Sunyaev-Zeldovich sources
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Aussel, H.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Barrena, R.; Bartelmann, M.; Bartlett, J. G.; Battaner,
E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J. -P.;
Bersanelli, M.; Bielewicz, P.; Bikmaev, I.; Bobin, J.; Bock, J. J.;
Böhringer, H.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Bridges, M.; Bucher, M.; Burenin, R.; Burigana, C.; Butler, R. C.;
Cardoso, J. -F.; Carvalho, P.; Catalano, A.; Challinor, A.; Chamballu,
A.; Chary, R. -R.; Chen, X.; Chiang, H. C.; Chiang, L. -Y.; Chon,
G.; Christensen, P. R.; Churazov, E.; Church, S.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Comis, B.; Couchot, F.; Coulais, A.;
Crill, B. P.; Curto, A.; Cuttaia, F.; Da Silva, A.; Dahle, H.; Danese,
L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de
Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Démoclès, J.; Désert,
F. -X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli,
S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Eriksen, H. K.; Feroz, F.; Ferragamo, A.; Finelli, F.; Flores-Cacho,
I.; Forni, O.; Frailis, M.; Franceschi, E.; Fromenteau, S.; Galeotta,
S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; Giardino, G.;
Gilfanov, M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski,
K. M.; Grainge, K. J. B.; Gratton, S.; Gregorio, A.; Groeneboom, N.,
E.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D.; Hempel,
A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Hurley-Walker, N.;
Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.;
Keskitalo, R.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.;
Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.;
Leahy, J. P.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.;
Li, C.; Liddle, A.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish,
C. J.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall,
D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Matthai, F.; Mazzotta, P.; Mei, S.; Meinhold, P. R.;
Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella, A.; Migliaccio,
M.; Mikkelsen, K.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy,
J. A.; Naselsky, P.; Nastasi, A.; Nati, F.; Natoli, P.; Nesvadba,
N. P. H.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Olamaie, M.; Osborne,
S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.;
Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto,
L.; Perrott, Y. C.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli,
E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rowan-Robinson,
M.; Rubiño-Martín, J. A.; Rumsey, C.; Rusholme, B.; Sandri, M.;
Santos, D.; Saunders, R. D. E.; Savini, G.; Schammel, M. P.; Scott,
D.; Seiffert, M. D.; Shellard, E. P. S.; Shimwell, T. W.; Spencer,
L. D.; Starck, J. -L.; Stolyarov, V.; Stompor, R.; Streblyanska, A.;
Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.;
Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Tramonte, D.; Tristram, M.; Tucci, M.; Tuovinen, J.;
Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.;
Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt,
B. D.; White, M.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2015A&A...581A..14P Altcode: 2015arXiv150200543P
We update the all-sky Planck catalogue of 1227 clusters and cluster
candidates (PSZ1) published in March 2013, derived from detections
of the Sunyaev-Zeldovich (SZ) effect using the first 15.5 months of
Planck satellite observations. As an addendum, we deliver an updated
version of the PSZ1 catalogue, reporting the further confirmation of
86 Planck-discovered clusters. In total, the PSZ1 now contains 947
confirmed clusters, of which 214 were confirmed as newly discovered
clusters through follow-up observations undertaken by the Planck
Collaboration. The updated PSZ1 contains redshifts for 913 systems, of
which 736 (~ 80.6%) are spectroscopic, and associated mass estimates
derived from the Y<SUB>z</SUB> mass proxy. We also provide a new
SZ quality flag for the remaining 280 candidates. This flag was
derived from a novel artificial neural-network classification
of the SZ signal. Based on this assessment, the purity of the
updated PSZ1 catalogue is estimated to be 94%. In this release, we
provide the full updated catalogue and an additional readme file
with further information on the Planck SZ detections. <P />The
catalogue is only available at the CDS via anonymous ftp to <A
href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
(ftp://130.79.128.5) or via <A
href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/581/A14">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/581/A14</A>
---------------------------------------------------------
Title: VizieR Online Data Catalog: Updated Planck catalogue PSZ1
(Planck+, 2015)
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Aussel, H.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Barrena, R.; Bartelmann, M.; Bartlett, J. G.; Battaner, E.;
Benabed, K.; Benoit, A.; Benoit-Levy, A.; Bernard, J. -P.; Bersanelli,
M.; Bielewicz, P.; Bikmaev, I.; Bobin, J.; Bock, J. J.; Bohringer,
H.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bridges,
M.; Bucher, M.; Burenin, R.; Burigana, C.; Butler, R. C.; Cardoso,
J. -F.; Carvalho, P.; Catalano, A.; Challinor, A.; Chamballu, A.;
Chary, R. -R.; Chen, X.; Chiang, H. C.; Chiang, L. -Y.; Chon, G.;
Christensen, P. R.; Churazov, E.; Church, S.; Clements, D. L.; Colombi,
S.; Colombo, L. P. L.; Comis, B.; Couchot, F.; Coulais, A.; Crill,
B. P.; Curto, A.; Cuttaia, F.; da Silva, A.; Dahle, H.; Danese, L.;
Davies, R. D.; Davis, R. J.; de Bernardis, P.; De Rosa, A.; de Zotti,
G.; Delabrouille, J.; Delouis, J. -M.; Democles, J.; Desert, F. -X.;
Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Dore,
O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enslin, T. A.; Eriksen,
H. K.; Feroz, F.; Ferragamo, A.; Finelli, F.; Flores-Cacho, I.;
Forni, O.; Frailis, M.; Franceschi, E.; Fromenteau, S.; Galeotta, S.;
Ganga, K.; Genova-Santos, R. T.; Giard, M.; Giardino, G.; Gilfanov,
M.; Giraud-Heraud, Y.; Gonzalez-Nuevo, J.; Gorski, K. M.; Grainge,
K. J. B.; Gratton, S.; Gregorio, A.; Groeneboom, N. E.; Gruppuso, A.;
Hansen, F. K.; Hanson, D.; Harrison, D.; Hempel, A.; Henrot-Versille,
S.; Hernandez-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.;
Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.;
Huffenberger, K. M.; Hurier, G.; Hurley-Walker, N.; Jaffe, A. H.;
Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihanen, E.; Keskitalo,
R.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lahteenmaki, A.; Lamarre,
J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leahy, J. P.;
Leonardi, R.; Leon-Tavares, J.; Lesgourgues, J.; Li, C.; Liddle,
A.; Liguori, M.; Lilje, P. B.; Linden-Vornle, M.; Lopez-Caniego,
M.; Lubin, P. M.; Macias-Perez, J. F.; MacTavish, C. J.; Maffei,
B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martinez-Gonzalez, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; Mei, S.; Meinhold, P. R.; Melchiorri, A.;
Melin, J. -B.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mikkelsen,
K.; Mitra, S.; Miville-Deschenes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.;
Nastasi, A.; Nati, F.; Natoli, P.; Nesvadba, N. P. H.; Netterfield,
C. B.; Norgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; O'Dwyer, I. J.; Olamaie, M.; Osborne, S.; Oxborrow, C. A.; Paci,
F.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon,
G.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrott, Y. C.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.;
Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa,
L.; Poutanen, T.; Pratt, G. W.; Prezeau, G.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorce, I.; Rocha, G.;
Rosset, C.; Roudier, G.; Rowan-Robinson, M.; Rubino-Martin, J. A.;
Rumsey, C.; Rusholme, B.; Sandri, M.; Santos, D.; Saunders, R. D. E.;
Savini, G.; Schammel, M. P.; Scott, D.; Seiffert, M. D.; Shellard,
E. P. S.; Shimwel, T. W.; Spencer, L. D.; Starck, J. -L.; Stolyarov,
V.; Stompor, R.; Streblyanska, A.; Sudiwala, R.; Sunyaev, R.; Sureau,
F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tramonte,
D.; Tristram, M.; Tucci, M.; Tuovinen, J.; Turler, M.; Umana, G.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Vibert, L.; Vielva,
P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; White, M.;
White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2015yCat..35810014P Altcode:
The updated Planck catalogue of SZ sources is available
at PLA (http://www.sciops.esa.int/index.php?page=
Planck<SUB>Legacy</SUB>Archive&project=planck) and the SZ cluster
database (http://szcluster-db.ias.u-psud.fr). The updated PSZ1 gathers
in a single table all the entries of the delivered catalogue mainly
based on the Planck data and the entries of the external validation
information based on ancillary data (Appendices B and C of Planck
Collaboration et al. (2014A&A...571A..29P, Cat. VIII/91),
respectively). It also contains additional entries. <P />The updated
catalogue contains, when available, cluster external identifications8
and consolidated redshifts. We added two new entries: the redshift
type and the bibliographic reference. <P />(2 data files).
---------------------------------------------------------
Title: Planck intermediate results. XXIV. Constraints on variations
in fundamental constants
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J. -P.;
Bersanelli, M.; Bielewicz, P.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Burigana, C.; Butler, R. C.; Calabrese, E.; Chamballu, A.;
Chiang, H. C.; Christensen, P. R.; Clements, D. L.; Colombo, L. P. L.;
Couchot, F.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis,
R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.;
Diego, J. M.; Dole, H.; Doré, O.; Dupac, X.; Enßlin, T. A.; Eriksen,
H. K.; Fabre, O.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.;
Galeotta, S.; Galli, S.; Ganga, K.; Giard, M.; González-Nuevo, J.;
Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson,
D.; Harrison, D. L.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe,
A. H.; Jones, W. C.; Keihänen, E.; Keskitalo, R.; Kneissl, R.;
Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lamarre, J. -M.; Lasenby,
A.; Lawrence, C. R.; Leonardi, R.; Lesgourgues, J.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Mandolesi, N.; Maris, M.; Martin, P. G.;
Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta, P.;
Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Menegoni, E.; Mennella,
A.; Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier,
L.; Morgante, G.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky,
P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.;
Novikov, D.; Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.;
Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa,
L.; Pratt, G. W.; Prunet, S.; Rachen, J. P.; Rebolo, R.; Reinecke, M.;
Remazeilles, M.; Renault, C.; Ricciardi, S.; Ristorcelli, I.; Rocha,
G.; Roudier, G.; Rusholme, B.; Sandri, M.; Savini, G.; Scott, D.;
Spencer, L. D.; Stolyarov, V.; Sudiwala, R.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Uzan, J. -P.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.;
Wade, L. A.; Yvon, D.; Zacchei, A.; Zonca, A.
2015A&A...580A..22P Altcode: 2014arXiv1406.7482A
Any variation in the fundamental physical constants, more particularly
in the fine structure constant, α, or in the mass of the electron,
m<SUB>e</SUB>, affects the recombination history of the Universe
and cause an imprint on the cosmic microwave background angular
power spectra. We show that the Planck data allow one to improve the
constraint on the time variation of the fine structure constant at
redshift z ~ 10<SUP>3</SUP> by about a factor of 5 compared to WMAP
data, as well as to break the degeneracy with the Hubble constant,
H<SUB>0</SUB>. In addition to α, we can set a constraint on the
variation in the mass of the electron, m<SUB>e</SUB>, and in the
simultaneous variation of the two constants. We examine in detail
the degeneracies between fundamental constants and the cosmological
parameters, in order to compare the limits obtained from Planck and
WMAP and to determine the constraining power gained by including other
cosmological probes. We conclude that independent time variations
of the fine structure constant and of the mass of the electron are
constrained by Planck to Δα/α = (3.6 ± 3.7) × 10<SUP>-3</SUP>
and Δm<SUB>e</SUB>/m<SUB>e</SUB> = (4 ± 11) × 10<SUP>-3</SUP> at the
68% confidence level. We also investigate the possibility of a spatial
variation of the fine structure constant. The relative amplitude of a
dipolar spatial variation in α (corresponding to a gradient across
our Hubble volume) is constrained to be δα/α = (-2.4 ± 3.7) ×
10<SUP>-2</SUP>. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424496/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck intermediate results. XXIII. Galactic plane emission
components derived from Planck with ancillary data
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alves,
M. I. R.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.;
Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed,
K.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.;
Bobin, J.; Bonaldi, A.; Bond, J. R.; Bouchet, F. R.; Boulanger, F.;
Burigana, C.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Chiang,
H. C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Colombo,
L. P. L.; Combet, C.; Couchot, F.; Crill, B. P.; Cuttaia, F.; Danese,
L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de
Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Donzelli,
S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.;
Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Ghosh, T.; Giard,
M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski,
K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D. L.;
Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe,
A. H.; Jaffe, T. R.; Jones, W. C.; Keihänen, E.; Keskitalo, R.;
Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.;
Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Lawrence,
C. R.; Leonardi, R.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maino,
D.; Mandolesi, N.; Martin, P. G.; Martínez-González, E.; Masi,
S.; Massardi, M.; Matarrese, S.; Mazzotta, P.; Meinhold, P. R.;
Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.;
Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante, G.;
Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.;
Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.;
Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Pasian, F.; Pearson, T. J.; Peel, M.; Perdereau, O.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.;
Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa,
L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach,
W. T.; Rebolo, R.; Reich, W.; Reinecke, M.; Remazeilles, M.; Renault,
C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini,
G.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Strong, A. W.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco,
D.; Terenzi, L.; Tibbs, C. T.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Tucci, M.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis,
J.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Watson, R.;
Yvon, D.; Zacchei, A.; Zonca, A.
2015A&A...580A..13P Altcode: 2014arXiv1406.5093P
Planck data when combined with ancillary data provide a unique
opportunity to separate the diffuse emission components of the inner
Galaxy. The purpose of the paper is to elucidate the morphology of the
various emission components in the strong star-formation region lying
inside the solar radius and to clarify the relationship between the
various components. The region of the Galactic plane covered is l =
300° → 0° → 60° wherestar-formation is highest and the emission
is strong enough to make meaningful component separation. The latitude
widths in this longitude range lie between 1° and 2°, which correspond
to FWHM z-widths of 100-200 pc at a typical distance of 6 kpc. The
four emission components studied here are synchrotron, free-free,
anomalous microwave emission (AME), and thermal (vibrational) dust
emission. These components are identified by constructing spectral
energy distributions (SEDs) at positions along the Galactic plane using
the wide frequency coverage of Planck (28.4-857 GHz) in combination
with low-frequency radio data at 0.408-2.3 GHz plus WMAP data at 23-94
GHz, along with far-infrared (FIR) data from COBE-DIRBE and IRAS. The
free-free component is determined from radio recombination line (RRL)
data. AME is found to be comparable in brightness to the free-free
emission on the Galactic plane in the frequency range 20-40 GHz with a
width in latitude similar to that of the thermal dust; it comprises 45
± 1% of the total 28.4 GHz emission in the longitude range l = 300°
→ 0° → 60°. The free-free component is the narrowest, reflecting
the fact that it is produced by current star-formation as traced by
the narrow distribution of OB stars. It is the dominant emission on
the plane between 60 and 100 GHz. RRLs from this ionized gas are used
to assess its distance, leading to a free-free z-width of FWHM ≈ 100
pc. The narrow synchrotron component has a low-frequency brightness
spectral index β<SUB>synch</SUB> ≈ -2.7 that is similar to the broad
synchrotron component indicating that they are both populated by the
cosmic ray electrons of the same spectral index. The width of this
narrow synchrotron component is significantly larger than that of the
other three components, suggesting that it is generated in an assembly
of older supernova remnants that have expanded to sizes of order 150
pc in 3 × 10<SUP>5</SUP> yr; pulsars of a similar age have a similar
spread in latitude. The thermal dust is identified in the SEDs with
average parameters of T<SUB>dust</SUB> = 20.4 ± 0.4 K, β<SUB>FIR</SUB>
= 1.94 ± 0.03 (> 353 GHz), and β<SUB>mm</SUB> = 1.67 ± 0.02 (<
353 GHz). The latitude distributions of gamma-rays, CO, and the emission
in high-frequency Planck bands have similar widths, showing that they
are all indicators of the total gaseous matter on the plane in the
inner Galaxy. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424434/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: A weak lensing analysis of the PLCK G100.2-30.4 cluster
Authors: Radovich, M.; Formicola, I.; Meneghetti, M.; Bartalucci,
I.; Bourdin, H.; Mazzotta, P.; Moscardini, L.; Ettori, S.; Arnaud,
M.; Pratt, G. W.; Aghanim, N.; Dahle, H.; Douspis, M.; Pointecouteau,
E.; Grado, A.
2015A&A...579A...7R Altcode: 2015arXiv150502887R
We present a mass estimate of the Planck-discovered cluster PLCK
G100.2-30.4, derived from a weak lensing analysis of deep Subaru griz
images. We perform a careful selection of the background galaxies using
the multi-band imaging data, and undertake the weak lensing analysis
on the deep (1 h) r -band image. The shape measurement is based on the
Kaiser-Squires-Broadhurst algorithm; we adopt the PSFex software to
model the point spread function (PSF) across the field and correct for
this in the shape measurement. The weak lensing analysis is validated
through extensive image simulations. We compare the resulting weak
lensing mass profile and total mass estimate to those obtained from our
re-analysis of XMM-Newton observations, derived under the hypothesis
of hydrostatic equilibrium. The total integrated mass profiles agree
remarkably well, within 1σ across their common radial range. A mass
M<SUB>500</SUB> ~ 7 × 10<SUP>14</SUP>M<SUB>⊙</SUB> is derived for
the cluster from our weak lensing analysis. Comparing this value to that
obtained from our reanalysis of XMM-Newton data, we obtain a bias factor
of (1-b) = 0.8 ± 0.1. This is compatible within 1σ with the value of
(1-b) obtained in Planck 2015 from the calibration of the bias factor
using newly available weak lensing reconstructed masses. <P />Based
on data collected at Subaru Telescope (University of Tokyo).
---------------------------------------------------------
Title: Planck intermediate results. XXII. Frequency dependence of
thermal emission from Galactic dust in intensity and polarization
Authors: Planck Collaboration; Ade, P. A. R.; Alves, M. I. R.; Aniano,
G.; Armitage-Caplan, C.; Arnaud, M.; Atrio-Barandela, F.; Aumont, J.;
Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed,
K.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.;
Bock, J. J.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.;
Burigana, C.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Chiang,
H. C.; Colombo, L. P. L.; Combet, C.; Couchot, F.; Coulais, A.; Crill,
B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.;
de Bernardis, P.; de Zotti, G.; Delabrouille, J.; Désert, F. -X.;
Dickinson, C.; Diego, J. M.; Donzelli, S.; Doré, O.; Douspis, M.;
Dunkley, J.; Dupac, X.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.;
Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.;
Galeotta, S.; Ganga, K.; Ghosh, T.; Giard, M.; González-Nuevo, J.;
Górski, K. M.; Gregorio, A.; Gruppuso, A.; Guillet, V.; Hansen, F. K.;
Harrison, D. L.; Helou, G.; Hernández-Monteagudo, C.; Hildebrandt,
S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Jaffe,
A. H.; Jaffe, T. R.; Jones, W. C.; Keihänen, E.; Keskitalo, R.;
Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.;
Leahy, J. P.; Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maffei, B.; Magalhães, A. M.; Maino, D.; Mandolesi, N.; Maris,
M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi,
S.; Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella,
A.; Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier,
L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky,
P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Noviello, F.; Novikov,
D.; Novikov, I.; Oppermann, N.; Oxborrow, C. A.; Pagano, L.; Pajot,
F.; Paoletti, D.; Pasian, F.; Perdereau, O.; Perotto, L.; Perrotta,
F.; Piacentini, F.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Popa, L.; Pratt, G. W.; Rachen, J. P.; Reach, W. T.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rubiño-Martín,
J. A.; Rusholme, B.; Salerno, E.; Sandri, M.; Savini, G.; Scott, D.;
Spencer, L. D.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Valenziano, L.;
Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Wandelt, B. D.;
Zacchei, A.; Zonca, A.
2015A&A...576A.107P Altcode: 2014arXiv1405.0874P
Planck has mapped the intensity and polarization of the sky at microwave
frequencies with unprecedented sensitivity. We use these data to
characterize the frequency dependence of dust emission. We make use
of the Planck 353 GHz I, Q, and U Stokes maps as dust templates, and
cross-correlate them with the Planck and WMAP data at 12 frequencies
from 23 to 353 GHz, over circular patches with 10° radius. The
cross-correlation analysis is performed for both intensity and
polarization data in a consistent manner. The results are corrected for
the chance correlation between the templates and the anisotropies of the
cosmic microwave background. We use a mask that focuses our analysis on
the diffuse interstellar medium at intermediate Galactic latitudes. We
determine the spectral indices of dust emission in intensity and
polarization between 100 and 353 GHz, for each sky patch. Both indices
are found to be remarkably constant over the sky. The mean values,
1.59 ± 0.02 for polarization and 1.51 ± 0.01 for intensity, for a
mean dust temperature of 19.6 K, are close, but significantly different
(3.6σ). We determine the mean spectral energy distribution (SED) of
the microwave emission, correlated with the 353 GHz dust templates,
by averaging the results of the correlation over all sky patches. We
find that the mean SED increases for decreasing frequencies at ν< 60
GHz for both intensity and polarization. The rise of the polarization
SED towards low frequencies may be accounted for by a synchrotron
component correlated with dust, with no need for any polarization of
the anomalous microwave emission. We use a spectral model to separate
the synchrotron and dust polarization and to characterize the spectral
dependence of the dust polarization fraction. The polarization
fraction (p) of the dust emission decreases by (21 ± 6)% from 353
to 70 GHz. We discuss this result within the context of existing dust
models. The decrease in p could indicate differences in polarization
efficiency among components of interstellar dust (e.g., carbon
versus silicate grains). Our observational results provide inputs to
quantify and optimize the separation between Galactic and cosmological
polarization. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424088/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck intermediate results. XIX. An overview of the polarized
thermal emission from Galactic dust
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alina,
D.; Alves, M. I. R.; Armitage-Caplan, C.; Arnaud, M.; Arzoumanian,
D.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.;
Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.;
Bock, J. J.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.;
Bracco, A.; Burigana, C.; Butler, R. C.; Cardoso, J. -F.; Catalano,
A.; Chamballu, A.; Chary, R. -R.; Chiang, H. C.; Christensen, P. R.;
Colombi, S.; Colombo, L. P. L.; Combet, C.; Couchot, F.; Coulais,
A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.;
Davis, R. J.; de Bernardis, P.; de Gouveia Dal Pino, E. M.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Désert, F. -X.; Dickinson, C.;
Diego, J. M.; Donzelli, S.; Doré, O.; Douspis, M.; Dunkley, J.;
Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Falgarone,
E.; Ferrière, K.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse,
A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Ghosh, T.; Giard, M.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.;
Gruppuso, A.; Guillet, V.; Hansen, F. K.; Harrison, D. L.; Helou, G.;
Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.;
Holmes, W. A.; Hornstrup, A.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe,
T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.;
Leahy, J. P.; Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maffei, B.; Magalhães, A. M.; Maino, D.; Mandolesi, N.;
Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.;
Masi, S.; Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.;
Mennella, A.; Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti, A.;
Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.;
Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Noviello, F.;
Novikov, D.; Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.;
Paladini, R.; Paoletti, D.; Pasian, F.; Pearson, T. J.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pietrobon,
D.; Plaszczynski, S.; Poidevin, F.; Pointecouteau, E.; Polenta, G.;
Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.;
Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault,
C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset,
C.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.;
Savini, G.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Stompor, R.;
Sudiwala, R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber,
J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci,
M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva,
P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Zacchei, A.; Zonca, A.
2015A&A...576A.104P Altcode: 2014arXiv1405.0871P
This paper presents an overview of the polarized sky as seen by
Planck HFI at 353 GHz, which is the most sensitive Planck channel for
dust polarization. We construct and analyse maps of dust polarization
fraction and polarization angle at 1° resolution, taking into account
noise bias and possible systematic effects. The sensitivity of the
Planck HFI polarization measurements allows for the first time a
mapping of Galactic dust polarized emission on large scales, including
low column density regions. We find that the maximum observed dust
polarization fraction is high (p<SUB>max</SUB> = 19.8%), in particular
in some regions of moderate hydrogen column density (N<SUB>H</SUB>
< 2 × 10<SUP>21</SUP> cm<SUP>-2</SUP>). The polarization fraction
displays a large scatter at N<SUB>H</SUB> below a few 10<SUP>21</SUP>
cm<SUP>-2</SUP>. There is a general decrease in the dust polarization
fraction with increasing column density above N<SUB>H</SUB> ≃ 1
× 10<SUP>21</SUP> cm<SUP>-2</SUP> and in particular a sharp drop
above N<SUB>H</SUB> ≃ 1.5 × 10<SUP>22</SUP> cm<SUP>-2</SUP>. We
characterize the spatial structure of the polarization angle using
the angle dispersion function. We find that the polarization angle
is ordered over extended areas of several square degrees, separated
by filamentary structures of high angle dispersion function. These
appear as interfaces where the sky projection of the magnetic field
changes abruptly without variations in the column density. The
polarization fraction is found to be anti-correlated with the
dispersion of polarization angles. These results suggest that, at the
resolution of 1°, depolarization is due mainly to fluctuations in
the magnetic field orientation along the line of sight, rather than
to the loss of grain alignment in shielded regions. We also compare
the polarization of thermal dust emission with that of synchrotron
measured with Planck, low-frequency radio data, and Faraday rotation
measurements toward extragalactic sources. These components bear
resemblance along the Galactic plane and in some regions such as
the Fan and North Polar Spur regions. The poor match observed in
other regions shows, however, that dust, cosmic-ray electrons,
and thermal electrons generally sample different parts of the line
of sight. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424082/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck intermediate results. XX. Comparison of polarized
thermal emission from Galactic dust with simulations of MHD turbulence
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alina,
D.; Alves, M. I. R.; Aniano, G.; Armitage-Caplan, C.; Arnaud, M.;
Arzoumanian, D.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.;
Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.;
Benabed, K.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.;
Bielewicz, P.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger,
F.; Bracco, A.; Burigana, C.; Cardoso, J. -F.; Catalano, A.;
Chamballu, A.; Chiang, H. C.; Christensen, P. R.; Colombi, S.;
Colombo, L. P. L.; Combet, C.; Couchot, F.; Coulais, A.; Crill,
B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis,
R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille,
J.; Dickinson, C.; Diego, J. M.; Donzelli, S.; Doré, O.; Douspis,
M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.;
Falgarone, E.; Fanciullo, L.; Ferrière, K.; Finelli, F.; Forni, O.;
Frailis, M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga,
K.; Ghosh, T.; Giard, M.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gregorio, A.; Gruppuso, A.; Guillet, V.; Hansen,
F. K.; Harrison, D. L.; Helou, G.; Hernández-Monteagudo, C.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.;
Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl,
R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre,
J. -M.; Lasenby, A.; Lawrence, C. R.; Leonardi, R.; Levrier, F.;
Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; Maino, D.; Mandolesi, N.; Maris,
M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.;
Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.;
Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Noviello, F.; Novikov, D.;
Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paoletti, D.;
Pasian, F.; Pelkonen, V. -M.; Perdereau, O.; Perotto, L.; Perrotta,
F.; Piacentini, F.; Piat, M.; Pietrobon, D.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Popa, L.; Pratt, G. W.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Reinecke, M.; Remazeilles, M.; Renault,
C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset,
C.; Roudier, G.; Rusholme, B.; Sandri, M.; Scott, D.; Soler, J. D.;
Spencer, L. D.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.;
Wade, L. A.; Wandelt, B. D.; Zonca, A.
2015A&A...576A.105P Altcode: 2014arXiv1405.0872P
Polarized emission observed by Planck HFI at 353 GHz towards a
sample of nearby fields is presented, focusing on the statistics of
polarization fractions p and angles ψ. The polarization fractions
and column densities in these nearby fields are representative of
the range of values obtained over the whole sky. We find that: (i)
the largest polarization fractions are reached in the most diffuse
fields; (ii) the maximum polarization fraction p<SUB>max</SUB>
decreases with column density N<SUB>H</SUB> in the more opaque fields
with N<SUB>H</SUB>> 10<SUP>21</SUP> cm<SUP>-2</SUP>; and (iii) the
polarization fraction along a given line of sight is correlated with the
local spatial coherence of the polarization angle. These observations
are compared to polarized emission maps computed in simulations of
anisotropic magnetohydrodynamical turbulence in which we assume a
uniform intrinsic polarization fraction of the dust grains. We find
that an estimate of this parameter may be recovered from the maximum
polarization fraction p<SUB>max</SUB> in diffuse regions where the
magnetic field is ordered on large scales and perpendicular to the
line of sight. This emphasizes the impact of anisotropies of the
magnetic field on the emerging polarization signal. The decrease
of the maximum polarization fraction with column density in nearby
molecular clouds is well reproduced in the simulations, indicating
that it is essentially due to the turbulent structure of the magnetic
field: an accumulation of variously polarized structures along the
line of sight leads to such an anti-correlation. In the simulations,
polarization fractions are also found to anti-correlate with the angle
dispersion function 𝒮. However, the dispersion of the polarization
angle for a given polarization fraction is found to be larger in
the simulations than in the observations, suggesting a shortcoming
in the physical content of these numerical models. In summary, we
find that the turbulent structure of the magnetic field is able to
reproduce the main statistical properties of the dust polarization as
observed in a variety of nearby clouds, dense cores excluded, and that
the large-scale field orientation with respect to the line of sight
plays a major role in the quantitative analysis of these statistical
properties. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424086/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck intermediate results. XXI. Comparison of polarized
thermal emission from Galactic dust at 353 GHz with interstellar
polarization in the visible
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alina,
D.; Aniano, G.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.;
Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.;
Barreiro, R. B.; Battaner, E.; Beichman, C.; Benabed, K.; Benoit-Lévy,
A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bock, J. J.;
Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Burigana, C.;
Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Chary, R. -R.; Chiang,
H. C.; Christensen, P. R.; Colombi, S.; Colombo, L. P. L.; Combet,
C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.;
Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Désert, F. -X.; Dickinson, C.;
Diego, J. M.; Donzelli, S.; Doré, O.; Douspis, M.; Dunkley, J.;
Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Falgarone,
E.; Fanciullo, L.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse,
A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Ghosh, T.; Giard, M.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gregorio,
A.; Gruppuso, A.; Guillet, V.; Hansen, F. K.; Harrison, D. L.; Helou,
G.; Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson,
M.; Holmes, W. A.; Hornstrup, A.; Huffenberger, K. M.; Jaffe, A. H.;
Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo,
R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.;
Lawrence, C. R.; Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maffei, B.; Magalhães, A. M.; Maino, D.; Mandolesi, N.; Maris,
M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.;
Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.;
Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Noviello, F.; Novikov, D.;
Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Pasian, F.; Perdereau, O.; Perotto, L.; Perrotta, F.;
Piacentini, F.; Piat, M.; Pietrobon, D.; Plaszczynski, S.; Poidevin,
F.; Pointecouteau, E.; Polenta, G.; Popa, L.; Pratt, G. W.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.;
Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli,
I.; Rocha, G.; Rosset, C.; Roudier, G.; Rusholme, B.; Sandri, M.;
Savini, G.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Stompor, R.;
Sudiwala, R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber,
J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci,
M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva,
P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; Zonca, A.
2015A&A...576A.106P Altcode: 2014arXiv1405.0873P
The Planck survey provides unprecedented full-sky coverage of the
submillimetre polarized emission from Galactic dust. In addition to the
information on the direction of the Galactic magnetic field, this also
brings new constraints on the properties of dust. The dust grains that
emit the radiation seen by Planck in the submillimetre also extinguish
and polarize starlight in the visible. Comparison of the polarization
of the emission and of the interstellar polarization on selected
lines of sight probed by stars provides unique new diagnostics of the
emission and light scattering properties of dust, and therefore of the
important dust model parameters, composition, size, and shape. Using
ancillary catalogues of interstellar polarization and extinction of
starlight, we obtain the degree of polarization, p<SUB>V</SUB>, and
the optical depth in the V band to the star, τ<SUB>V</SUB>. Toward
these stars we measure the submillimetre polarized intensity,
P<SUB>S</SUB>, and total intensity, I<SUB>S</SUB>, in the Planck 353
GHz channel. We compare the column density measure in the visible,
E(B - V), with that inferred from the Planck product map of the
submillimetre dust optical depth and compare the polarization direction
(position angle) in the visible with that in the submillimetre. For
those lines of sight through the diffuse interstellar medium with
comparable values of the estimated column density and polarization
directions close to orthogonal, we correlate properties in the
submillimetre and visible to find two ratios, R<SUB>S /V</SUB> =
(P<SUB>S</SUB>/I<SUB>S</SUB>) / (p<SUB>V</SUB>/τ<SUB>V</SUB>) and
R<SUB>P/p</SUB> = P<SUB>S</SUB>/p<SUB>V</SUB>, the latter focusing
directly on the polarization properties of the aligned grain population
alone.We find R<SUB>S /V</SUB> = 4.2, with statistical and systematic
uncertainties 0.2 and 0.3, respectively, and R<SUB>P/p</SUB> = 5.4 MJy
sr<SUP>-1</SUP>, with uncertainties 0.2 and 0.3 MJy sr<SUP>-1</SUP>,
respectively. Our estimate of R<SUB>S /V</SUB> is compatible with
predictions based on a range of polarizing dust models that have
been developed for the diffuse interstellar medium. This estimate
provides new empirical validation of many of the common underlying
assumptions of the models, but is not yet very discriminating among
them. However, our estimate of R<SUB>P/p</SUB> is not compatible with
predictions, which are too low by a factor of about 2.5. This more
discriminating diagnostic, R<SUB>P/p</SUB>, indicates that changes to
the optical properties in the models of the aligned grain population are
required. These new diagnostics, together with the spectral dependence
in the submillimetre from Planck,will be important for constraining
and understanding the full complexity of the grain models, and for
interpreting the Planck thermal dust polarization and refinement
of the separation of this contamination of the cosmic microwave
background. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201424087/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck intermediate results. XVIII. The millimetre and
sub-millimetre emission from planetary nebulae
Authors: Planck Collaboration; Arnaud, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner,
E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli,
M.; Bielewicz, P.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Buemi, C. S.; Burigana, C.; Cardoso, J. -F.; Casassus, S.;
Catalano, A.; Cerrigone, L.; Chamballu, A.; Chiang, H. C.; Colombi,
S.; Colombo, L. P. L.; Couchot, F.; Crill, B. P.; Curto, A.; Cuttaia,
F.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de
Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Donzelli,
S.; Doré, O.; Dupac, X.; Enßlin, T. A.; Eriksen, H. K.; Finelli,
F.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard,
M.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.;
Hansen, F. K.; Harrison, D. L.; Hildebrandt, S. R.; Hivon, E.; Holmes,
W. A.; Hora, J. L.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.;
Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.;
Kisner, T. S.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.; Leonardi, R.;
Leto, P.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Martin,
P. G.; Masi, S.; Massardi, M.; Matarrese, S.; Mazzotta, P.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy,
J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Noviello, F.; Novikov,
D.; Novikov, I.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti,
D.; Peel, M.; Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat, M.;
Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Popa,
L.; Pratt, G. W.; Procopio, P.; Prunet, S.; Puget, J. -L.; Rachen,
J. P.; Reinecke, M.; Remazeilles, M.; Ricciardi, S.; Riller, T.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Scott, D.; Spencer,
L. D.; Stolyarov, V.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.;
Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Trigilio,
C.; Tristram, M.; Trombetti, T.; Tucci, M.; Umana, G.; Valiviita,
J.; Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.;
Zacchei, A.; Zijlstra, A.; Zonca, A.
2015A&A...573A...6P Altcode: 2014arXiv1403.4723P
Late stages of stellar evolution are characterized by copious mass-loss
events whose signature is the formation of circumstellar envelopes
(CSE). Planck multi-frequency measurements have provided relevant
information on a sample of Galactic planetary nebulae (PNe) in the
important and relatively unexplored observational band between 30 and
857 GHz. Planck enables the assembly of comprehensive PNe spectral
energy distributions (SEDs) from radio to far-IR frequencies. Modelling
the derived SEDs provides us with information on physical properties
of CSEs and the mass content of both main components: ionized gas,
traced by the free-free emission at cm-mm waves; and thermal dust,
traced by the millimetre and far-IR emission. In particular, the amount
of ionized gas and dust has been derived here. Such quantities have
also been estimated for the very young PN CRL 618, where the strong
variability observed in its radio and millimetre emission has previously
prevented constructing its SED. A morphological study of the Helix
Nebula was also performed. Planck maps reveal, for the first time,
the spatial distribution of the dust inside the envelope, allowing us
to identify different components, the most interesting of which is a
very extended component (up to 1 pc) that may be related to a region
where the slow expanding envelope is interacting with the surrounding
interstellar medium.
---------------------------------------------------------
Title: Shapley Supercluster Survey: Galaxy evolution from filaments
to cluster cores
Authors: Merluzzi, P.; Busarello, G.; Haines, C. P.; Mercurio, A.;
Okabe, N.; Pimbblet, K. J.; Dopita, M. A.; Grado, A.; Limatola,
L.; Bourdin, H.; Mazzotta, P.; Capaccioli, M.; Napolitano, N. R.;
Schipani, P.
2015MNRAS.446..803M Altcode: 2014arXiv1407.4628M
We present an overview of a multiwavelength survey of the Shapley
Supercluster (SSC; z ∼ 0.05) covering a contiguous area of 260
h^{-2}_{70} Mpc<SUP>2</SUP> including the supercluster core. The project
main aim is to quantify the influence of cluster-scale mass assembly
on galaxy evolution in one of the most massive structures in the local
Universe. The Shapley Supercluster Survey (ShaSS) includes nine Abell
clusters (A3552, A3554, A3556, A3558, A3559, A3560, A3562, AS0724,
AS0726) and two poor clusters (SC1327-312, SC1329-313) showing evidence
of cluster-cluster interactions. Optical (ugri) and near-infrared (K)
imaging acquired with VLT Survey Telescope and Visible and Infrared
Survey Telescope for Astronomy allow us to study the galaxy population
down to m<SUP>⋆</SUP> + 6 at the supercluster redshift. A dedicated
spectroscopic survey with AAOmega on the Anglo-Australian Telescope
provides a magnitude-limited sample of supercluster members with 80
per cent completeness at ∼m<SUP>⋆</SUP> + 3. We derive the galaxy
density across the whole area, demonstrating that all structures within
this area are embedded in a single network of clusters, groups and
filaments. The stellar mass density in the core of the SSC is always
higher than 9 × 10<SUP>9</SUP> M<SUB>⊙</SUB> Mpc<SUP>-3</SUP>,
which is ∼40× the cosmic stellar mass density for galaxies in the
local Universe. We find a new filamentary structure (∼7 Mpc long
in projection) connecting the SSC core to the cluster A3559, as well
as previously unidentified density peaks. We perform a weak-lensing
analysis of the central 1 deg<SUP>2</SUP> field of the survey obtaining
for the central cluster A3558 a mass of M_{500}=7.63_{-3.40}^{+3.88}×
10^{14} M_{⊙}, in agreement with X-ray based estimates.
---------------------------------------------------------
Title: Planck 2013 results. IV. Low Frequency Instrument beams and
window functions
Authors: Planck Collaboration; Aghanim, N.; Armitage-Caplan, C.;
Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.;
Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Cardoso,
J. -F.; Catalano, A.; Chamballu, A.; Chiang, L. -Y.; Christensen,
P. R.; Church, S.; Colombi, S.; Colombo, L. P. L.; Crill, B. P.;
Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de
Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Dickinson,
C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.;
Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli,
F.; Forni, O.; Frailis, M.; Franceschi, E.; Gaier, T. C.; Galeotta,
S.; Ganga, K.; Giard, M.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.;
Hanson, D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.;
Jaffe, T. R.; Jewell, J.; Jones, W. C.; Juvela, M.; Kangaslahti, P.;
Keihänen, E.; Keskitalo, R.; Kiiveri, K.; Kisner, T. S.; Knoche,
J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.;
Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; Lindholm, V.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall,
D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi,
M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Meinhold, P. R.;
Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.;
Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi,
D.; Naselsky, P.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen,
H. U.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Paci, F.;
Pagano, L.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.;
Perdereau, O.; Perotto, L.; Perrotta, F.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.;
Remazeilles, M.; Ricciardi, S.; Riller, T.; Rocha, G.; Rosset, C.;
Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos,
D.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.;
Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sureau, F.; Sutton, D.;
Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.;
Van Tent, B.; Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade,
L. A.; Wandelt, B. D.; Zacchei, A.; Zonca, A.
2014A&A...571A...4P Altcode: 2013arXiv1303.5065P
This paper presents the characterization of the in-flight beams,
the beam window functions, and the associated uncertainties for the
Planck Low Frequency Instrument (LFI). Knowledge of the beam profiles is
necessary for determining the transfer function to go from the observed
to the actual sky anisotropy power spectrum. The main beam distortions
affect the beam window function, complicating the reconstruction of
the anisotropy power spectrum at high multipoles, whereas the sidelobes
affect the low and intermediate multipoles. The in-flight assessment of
the LFI main beams relies on the measurements performed during Jupiter
observations. By stacking the datafrom multiple Jupiter transits,
the main beam profiles are measured down to -20 dB at 30 and 44 GHz,
and down to -25 dB at 70 GHz. The main beam solid angles are determined
to better than 0.2% at each LFI frequency band. The Planck pre-launch
optical model is conveniently tuned to characterize the main beams
independently of any noise effects. This approach provides an optical
model whose beams fully reproduce the measurements in the main beam
region, but also allows a description of the beams at power levels
lower than can be achieved by the Jupiter measurements themselves. The
agreement between the simulated beams and the measured beams is better
than 1% at each LFI frequency band. The simulated beams are used for the
computation of the window functions for the effective beams. The error
budget for the window functions is estimated from both main beam and
sidelobe contributions, and accounts for the radiometer bandshapes. The
total uncertainties in the effective beam window functions are: 2%
and 1.2% at 30 and 44 GHz, respectively (at ℓ ≈ 600), and 0.7%
at 70 GHz (at ℓ ≈ 1000).
---------------------------------------------------------
Title: Planck 2013 results. III. LFI systematic uncertainties
Authors: Planck Collaboration; Aghanim, N.; Armitage-Caplan, C.;
Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.;
Benoît, A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.;
Bielewicz, P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bonavera, L.;
Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.;
Burigana, C.; Butler, R. C.; Cardoso, J. -F.; Catalano, A.; Chamballu,
A.; Chiang, L. -Y.; Christensen, P. R.; Church, S.; Colombi, S.;
Colombo, L. P. L.; Crill, B. P.; Cruz, M.; Curto, A.; Cuttaia, F.;
Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Dick, J.; Dickinson, C.; Diego,
J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.;
Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni,
O.; Frailis, M.; Franceschi, E.; Gaier, T. C.; Galeotta, S.; Ganga,
K.; Giard, M.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.;
Hanson, D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.;
Jaffe, T. R.; Jewell, J.; Jones, W. C.; Juvela, M.; Kangaslahti, P.;
Keihänen, E.; Keskitalo, R.; Kiiveri, K.; Kisner, T. S.; Knoche,
J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.;
Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; Lindholm, V.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall,
D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri,
A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.;
Naselsky, P.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen,
H. U.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Paci,
F.; Pagano, L.; Paladini, R.; Paoletti, D.; Partridge, B.; Pasian,
F.; Patanchon, G.; Pearson, D.; Peel, M.; Perdereau, O.; Perotto,
L.; Perrotta, F.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.;
Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.;
Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Ricciardi,
S.; Riller, T.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.;
Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Scott,
D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Starck,
J. -L.; Stolyarov, V.; Stompor, R.; Sureau, F.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.;
Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.;
Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt,
B. D.; Watson, R.; Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A...3P Altcode: 2013arXiv1303.5064P
We present the current estimate of instrumental and systematic effect
uncertainties for the Planck-Low Frequency Instrument relevant to
the first release of the Planck cosmological results. We give an
overview of the main effects and of the tools and methods applied to
assess residuals in maps and power spectra. We also present an overall
budget of known systematic effect uncertainties, which are dominated
by sidelobe straylight pick-up and imperfect calibration. However,
even these two effects are at least two orders of magnitude weaker
than the cosmic microwave background fluctuations as measured in
terms of the angular temperature power spectrum. A residual signal
above the noise level is present in the multipole range ℓ < 20,
most notably at 30 GHz, and is probably caused by residual Galactic
straylight contamination. Current analysis aims to further reduce the
level of spurious signals in the data and to improve the systematic
effects modelling, in particular with respect to straylight and
calibration uncertainties.
---------------------------------------------------------
Title: Planck 2013 results. VI. High Frequency Instrument data
processing
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner,
E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J. -P.;
Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bowyer, J. W.; Bridges, M.;
Bucher, M.; Burigana, C.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.;
Chary, R. -R.; Chen, X.; Chiang, H. C.; Chiang, L. -Y.; Christensen,
P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.;
Combet, C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia,
F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de
Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert,
F. -X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré,
O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Enßlin,
T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse,
A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino,
G.; Girard, D.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski,
K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.;
Hansen, F. K.; Hanson, D.; Harrison, D.; Helou, G.; Henrot-Versillé,
S.; Herent, O.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt,
S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hou, Z.;
Hovest, W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe,
T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Le Jeune, M.; Leonardi, R.; Leroy, C.; Lesgourgues,
J.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego,
M.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei,
B.; Mandolesi, N.; Maris, M.; Marleau, F.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; McGehee, P.; Meinhold, P. R.; Melchiorri,
A.; Melot, F.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Mottet, S.; Munshi, D.; Murphy, J. A.; Naselsky,
P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen,
H. U.; North, C.; Noviello, F.; Novikov, D.; Novikov, I.; Orieux,
F.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.;
Paladini, R.; Paoletti, D.; Pasian, F.; Patanchon, G.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli,
E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Racine, B.; Reach, W. T.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.;
Rowan-Robinson, M.; Rusholme, B.; Sanselme, L.; Santos, D.; Sauvé,
A.; Savini, G.; Scott, D.; Shellard, E. P. S.; Spencer, L. D.; Starck,
J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sureau, F.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco,
D.; Techene, S.; Terenzi, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vibert, L.;
Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A...6P Altcode: 2013arXiv1303.5067P
Wedescribe the processing of the 531 billion raw data samples from
the High Frequency Instrument (HFI), which we performed to produce
six temperature maps from the first 473 days of Planck-HFI survey
data. These maps provide an accurate rendition of the sky emission at
100, 143, 217, 353, 545, and 857GHz with an angular resolution ranging
from 9.´7 to 4.´6. The detector noise per (effective) beam solid
angle is respectively, 10, 6 , 12, and 39 μK in the four lowest HFI
frequency channels (100-353GHz) and 13 and 14 kJy sr<SUP>-1</SUP>
in the 545 and 857 GHz channels. Relative to the 143 GHz channel,
these two high frequency channels are calibrated to within 5% and the
353 GHz channel to the percent level. The 100 and 217 GHz channels,
which together with the 143 GHz channel determine the high-multipole
part of the CMB power spectrum (50 <ℓ < 2500), are calibrated
relative to 143 GHz to better than 0.2%.
---------------------------------------------------------
Title: Planck 2013 results. IX. HFI spectral response
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela,
F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard,
J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Bond,
J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bridges, M.;
Bucher, M.; Burigana, C.; Cardoso, J. -F.; Catalano, A.; Challinor,
A.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, H. C.; Chiang,
L. -Y.; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.;
Colombo, L. P. L.; Combet, C.; Comis, B.; Couchot, F.; Coulais, A.;
Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; de
Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis,
J. -M.; Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dole, H.;
Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.;
Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Finelli, F.; Forni,
O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton,
S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison,
D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.; Jaffe, A. H.; Jaffe,
T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; Leroy, C.; Lesgourgues,
J.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego,
M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Mandolesi, N.;
Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.;
Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.;
McGehee, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio,
M.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky,
P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen,
H. U.; North, C.; Noviello, F.; Novikov, D.; Novikov, I.; Osborne,
S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.;
Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.;
Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski,
S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen,
T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen,
J. P.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.;
Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.;
Rusholme, B.; Santos, D.; Savini, G.; Scott, D.; Shellard, E. P. S.;
Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala,
R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber,
J. A.; Tavagnacco, D.; Terenzi, L.; Tomasi, M.; Tristram, M.; Tucci,
M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva,
P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Yvon, D.;
Zacchei, A.; Zonca, A.
2014A&A...571A...9P Altcode: 2013arXiv1303.5070P
The Planck High Frequency Instrument (HFI) spectral response was
determined through a series of ground based tests conducted with the
HFI focal plane in a cryogenic environment prior to launch. The main
goal of the spectral transmission tests was to measure the relative
spectral response (includingthe level of out-of-band signal rejection)
of all HFI detectors to a known source of electromagnetic radiation
individually. This was determined by measuring the interferometric
output of a continuously scanned Fourier transform spectrometer with
all HFI detectors. As there is no on-board spectrometer within HFI,
the ground-based spectral response experiments provide the definitive
data set for the relative spectral calibration of the HFI. Knowledge of
the relative variations in the spectral response between HFI detectors
allows for a more thorough analysis of the HFI data. The spectral
response of the HFI is used in Planck data analysis and component
separation, this includes extraction of CO emission observed within
Planck bands, dust emission, Sunyaev-Zeldovich sources, and intensity to
polarization leakage. The HFI spectral response data have also been used
to provide unit conversion and colour correction analysis tools. While
previous papers describe the pre-flight experiments conducted on the
Planck HFI, this paper focusses on the analysis of the pre-flight
spectral response measurements and the derivation of data products,
e.g. band-average spectra, unit conversion coefficients, and colour
correction coefficients, all with related uncertainties. Verifications
of the HFI spectral response data are provided through comparisons
with photometric HFI flight data. This validation includes use of HFI
zodiacal emission observations to demonstrate out-of-band spectral
signal rejection better than 10<SUP>8</SUP>. The accuracy of the HFI
relative spectral response data is verified through comparison with
complementary flight-data based unit conversion coefficients and colour
correction coefficients. These coefficients include those based upon
HFI observations of CO, dust, and Sunyaev-Zeldovich emission. General
agreement is observed between the ground-based spectral characterization
of HFI and corresponding in-flight observations, within the quoted
uncertainty of each; explanations are provided for any discrepancies.
---------------------------------------------------------
Title: Planck 2013 results. VII. HFI time response and beams
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela,
F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard,
J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Bond,
J. R.; Borrill, J.; Bouchet, F. R.; Bowyer, J. W.; Bridges, M.;
Bucher, M.; Burigana, C.; Cardoso, J. -F.; Catalano, A.; Challinor,
A.; Chamballu, A.; Chary, R. -R.; Chiang, H. C.; Chiang, L. -Y.;
Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo,
L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia,
F.; Danese, L.; Davies, R. D.; de Bernardis, P.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Diego, J. M.;
Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dunkley, J.; Dupac,
X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.;
Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Galeotta,
S.; Ganga, K.; Giard, M.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson,
J. E.; Haissinski, J.; Hansen, F. K.; Hanson, D.; Harrison, D.;
Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hou, Z.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe,
T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leonardi, R.; Leroy, C.; Lesgourgues, J.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Mandolesi, N.;
Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.;
Masi, S.; Massardi, M.; Matarrese, S.; Matsumura, T.; Matthai, F.;
Mazzotta, P.; McGehee, P.; Melchiorri, A.; Mendes, L.; Mennella,
A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy,
J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.;
Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polegre, A. M.; Polenta,
G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Roudier, G.; Rowan-Robinson, M.; Rusholme, B.; Sandri,
M.; Santos, D.; Sauvé, A.; Savini, G.; Scott, D.; Shellard, E. P. S.;
Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala,
R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber,
J. A.; Tavagnacco, D.; Terenzi, L.; Tomasi, M.; Tristram, M.; Tucci,
M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva,
P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Yvon, D.;
Zacchei, A.; Zonca, A.
2014A&A...571A...7P Altcode: 2013arXiv1303.5068P
This paper characterizes the effective beams, the effective beam window
functions and the associated errors for the Planck High Frequency
Instrument (HFI) detectors. The effective beam is theangular response
including the effect of the optics, detectors, data processing and the
scan strategy. The window function is the representation of this beam in
the harmonic domain which is required to recover an unbiased measurement
of the cosmic microwave background angular power spectrum. The HFI is
a scanning instrument and its effective beams are the convolution of:
a) the optical response of the telescope and feeds; b) the processing
of the time-ordered data and deconvolution of the bolometric and
electronic transfer function; and c) the merging of several surveys to
produce maps. The time response transfer functions are measured using
observations of Jupiter and Saturn and by minimizing survey difference
residuals. The scanning beam is the post-deconvolution angular response
of the instrument, and is characterized with observations of Mars. The
main beam solid angles are determined to better than 0.5% at each HFI
frequency band. Observations of Jupiter and Saturn limit near sidelobes
(within 5°) to about 0.1% of the total solid angle. Time response
residuals remain as long tails in the scanning beams, but contribute
less than 0.1% of the total solid angle. The bias and uncertainty in
the beam products are estimated using ensembles of simulated planet
observations that include the impact of instrumental noise and known
systematic effects. The correlation structure of these ensembles is
well-described by five error eigenmodes that are sub-dominant to sample
variance and instrumental noise in the harmonic domain. A suite of
consistency tests provide confidence that the error model represents a
sufficient description of the data. The total error in the effective
beam window functions is below 1% at 100 GHz up to multipole ℓ ~
1500, and below 0.5% at 143 and 217 GHz up to ℓ ~ 2000.
---------------------------------------------------------
Title: Planck 2013 results. VIII. HFI photometric calibration and
mapmaking
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela,
F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard,
J. -P.; Bersanelli, M.; Bertincourt, B.; Bielewicz, P.; Bobin, J.;
Bock, J. J.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.;
Bridges, M.; Bucher, M.; Burigana, C.; Cardoso, J. -F.; Catalano,
A.; Challinor, A.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang,
H. C.; Chiang, L. -Y.; Christensen, P. R.; Church, S.; Clements,
D. L.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Couchot, F.;
Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies,
R. D.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.;
Delouis, J. -M.; Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dole,
H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou,
G.; Enßlin, T. A.; Eriksen, H. K.; Filliard, C.; Finelli, F.;
Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen,
F. K.; Hanson, D.; Harrison, D.; Helou, G.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger,
K. M.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen,
E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby,
A.; Laureijs, R. J.; Lawrence, C. R.; Le Jeune, M.; Lellouch, E.;
Leonardi, R.; Leroy, C.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maffei, B.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Maurin, L.; Mazzotta, P.; McGehee, P.; Meinhold, P. R.;
Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Moreno, R.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.;
Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.;
Paci, F.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Partridge,
B.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto,
L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.;
Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget,
J. -L.; Rachen, J. P.; Reinecke, M.; Remazeilles, M.; Renault, C.;
Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Roudier, G.; Rusholme, B.; Santos, D.; Savini, G.; Scott, D.; Shellard,
E. P. S.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor, R.;
Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.;
Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Techene, S.; Terenzi,
L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.; Valenziano, L.;
Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.;
Wade, L. A.; Wandelt, B. D.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A...8P Altcode: 2013arXiv1303.5069P
This paper describes the methods used to produce photometrically
calibrated maps from the Planck High Frequency Instrument (HFI) cleaned,
time-ordered information. HFI observes the sky over a broad range
of frequencies, from 100 to 857 GHz. To obtain the best calibration
accuracy over such a large range, two different photometric calibration
schemes have to be used. The 545 and 857 GHz data are calibrated by
comparing flux-density measurements of Uranus and Neptune with models
of their atmospheric emission. The lower frequencies (below 353 GHz)
are calibrated using the solar dipole. A component of this anisotropy
is time-variable, owing to the orbital motion of the satellite in
the solar system. Photometric calibration is thus tightly linked
to mapmaking, which also addresses low-frequency noise removal. By
comparing observations taken more than one year apart in the same
configuration, we have identified apparent gain variations with
time. These variations are induced by non-linearities in the read-out
electronics chain. We have developed an effective correction to limit
their effect on calibration. We present several methods to estimate
the precision of the photometric calibration. We distinguish relative
uncertainties (between detectors, or between frequencies) and absolute
uncertainties. Absolute uncertainties lie in the range from 0.54% to 10%
from 100 to 857 GHz. We describe the pipeline used to produce the maps
from the HFI timelines, based on the photometric calibration parameters,
and the scheme used to set the zero level of the maps a posteriori. We
also discuss the cross-calibration between HFI and the SPIRE instrument
on board Herschel. Finally we summarize the basic characteristics of
the set of HFI maps included in the 2013 Planck data release.
---------------------------------------------------------
Title: Planck 2013 results. II. Low Frequency Instrument data
processing
Authors: Planck Collaboration; Aghanim, N.; Armitage-Caplan, C.;
Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana,
C.; Butler, R. C.; Cappellini, B.; Cardoso, J. -F.; Catalano, A.;
Chamballu, A.; Chen, X.; Chiang, L. -Y.; Christensen, P. R.; Church,
S.; Colombi, S.; Colombo, L. P. L.; Crill, B. P.; Cruz, M.; Curto, A.;
Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis,
P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Dickinson, C.;
Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac,
X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Falvella, M. C.;
Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.; Gaier, T. C.;
Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Héraud,
Y.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.;
Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison,
D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.;
Jewell, J.; Jones, W. C.; Juvela, M.; Kangaslahti, P.; Keihänen,
E.; Keskitalo, R.; Kiiveri, K.; Kisner, T. S.; Knoche, J.; Knox, L.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre,
J. -M.; Lasenby, A.; Lattanzi, M.; Laureijs, R. J.; Lawrence, C. R.;
Leach, S.; Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; Lindholm, V.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; Maggio, G.; Maino, D.; Mandolesi,
N.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González,
E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta,
P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.;
Migliaccio, M.; Mitra, S.; Moneti, A.; Montier, L.; Morgante, G.;
Morisset, N.; Mortlock, D.; Moss, A.; Munshi, D.; Naselsky, P.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Novikov,
D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Paci, F.; Pagano, L.;
Paladini, R.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon,
G.; Peel, M.; Perdereau, O.; Perotto, L.; Perrotta, F.; Pierpaoli,
E.; Pietrobon, D.; Plaszczynski, S.; Platania, P.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Ricciardi, S.; Riller,
T.; Robbers, G.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.;
Rubiño-Martín, J. A.; Rusholme, B.; Salerno, E.; Sandri, M.; Santos,
D.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.;
Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sureau, F.; Sutton, D.;
Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.;
Van Tent, B.; Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade,
L. A.; Wandelt, B. D.; Watson, R.; Wehus, I. K.; White, S. D. M.;
Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A...2P Altcode: 2013arXiv1303.5063P
We describe the data processing pipeline of the Planck Low Frequency
Instrument (LFI) data processing centre (DPC) to create and characterize
full-sky maps based on the first 15.5 months of operations at 30, 44,
and 70 GHz. In particular, we discuss the various steps involved in
reducing the data, from telemetry packets through to the production
of cleaned, calibrated timelines and calibrated frequency maps. Data
are continuously calibrated using the modulation induced on the
mean temperature of the cosmic microwave background radiation by the
proper motion of the spacecraft. Sky signals other than the dipole are
removed by an iterative procedure based on simultaneous fitting of
calibration parameters and sky maps. Noise properties are estimated
from time-ordered data after the sky signal has been removed, using
a generalized least squares map-making algorithm. A destriping code
(Madam) is employed to combine radiometric data and pointing information
into sky maps, minimizing the variance of correlated noise. Noise
covariance matrices, required to compute statistical uncertainties on
LFI and Planck products, are also produced. Main beams are estimated
down to the ≈- 20 dB level using Jupiter transits, which are also
used for the geometrical calibration of the focal plane.
---------------------------------------------------------
Title: Mapping the Particle Acceleration in the Cool Core of the
Galaxy Cluster RX J1720.1+2638
Authors: Giacintucci, S.; Markevitch, M.; Brunetti, G.; ZuHone, J. A.;
Venturi, T.; Mazzotta, P.; Bourdin, H.
2014ApJ...795...73G Altcode: 2014arXiv1403.2820G
We present new deep, high-resolution radio images of the diffuse
minihalo in the cool core of the galaxy cluster RX J1720.1+2638. The
images have been obtained with the Giant Metrewave Radio Telescope
at 317, 617, and 1280 MHz and with the Very Large Array at 1.5, 4.9,
and 8.4 GHz, with angular resolutions ranging from 1” to 10”. This
represents the best radio spectral and imaging data set for any
minihalo. Most of the radio flux of the minihalo arises from a bright
central component with a maximum radius of ~80 kpc. A fainter tail of
emission extends out from the central component to form a spiral-shaped
structure with a length of ~230 kpc, seen at frequencies 1.5 GHz and
below. We find indication of a possible steepening of the total radio
spectrum of the minihalo at high frequencies. Furthermore, a spectral
index image shows that the spectrum of the diffuse emission steepens
with increasing distance along the tail. A striking spatial correlation
is observed between the minihalo emission and two cold fronts visible in
the Chandra X-ray image of this cool core. These cold fronts confine the
minihalo, as also seen in numerical simulations of minihalo formation
by sloshing-induced turbulence. All these observations favor the
hypothesis that the radio-emitting electrons in cluster cool cores
are produced by turbulent re-acceleration.
---------------------------------------------------------
Title: Planck 2013 results. V. LFI calibration
Authors: Planck Collaboration; Aghanim, N.; Armitage-Caplan, C.;
Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana,
C.; Butler, R. C.; Cappellini, B.; Cardoso, J. -F.; Catalano, A.;
Chamballu, A.; Chen, X.; Chiang, L. -Y.; Christensen, P. R.; Church,
S.; Colombi, S.; Colombo, L. P. L.; Crill, B. P.; Curto, A.; Cuttaia,
F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dole,
H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.;
Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.;
Franceschi, E.; Gaier, T. C.; Galeotta, S.; Ganga, K.; Giard, M.;
Giardino, G.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.;
Hanson, D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.;
Jaffe, T. R.; Jewell, J.; Jones, W. C.; Juvela, M.; Kangaslahti, P.;
Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Knoche, J.; Knox, L.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre,
J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.;
Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Moneti, A.; Montier,
L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Naselsky, P.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Novikov,
D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Paci, F.; Pagano, L.;
Paladini, R.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon,
G.; Pearson, D.; Peel, M.; Perdereau, O.; Perotto, L.; Perrotta,
F.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Ricciardi, S.; Riller, T.; Rocha,
G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubiño-Martín, J. A.;
Rusholme, B.; Sandri, M.; Santos, D.; Scott, D.; Seiffert, M. D.;
Shellard, E. P. S.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.;
Stompor, R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.;
Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.; Umana, G.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Vielva, P.;
Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Watson, R.;
Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A...5P Altcode: 2013arXiv1303.5066P
We discuss the methods employed to photometrically calibrate the data
acquired by the Low Frequency Instrument on Planck. Our calibration is
based on a combination of the orbital dipole plus the solar dipole,
caused respectively by the motion of the Planck spacecraft with
respect to the Sun and by motion of the solar system with respect to
the cosmic microwave background (CMB) rest frame. The latter provides
a signal of a few mK with the same spectrum as the CMB anisotropies
and is visible throughout the mission. In this data releasewe rely
on the characterization of the solar dipole as measured by WMAP. We
also present preliminary results (at 44 GHz only) on the study of
the Orbital Dipole, which agree with the WMAP value of the solar
system speed within our uncertainties. We compute the calibration
constant for each radiometer roughly once per hour, in order to keep
track of changes in the detectors' gain. Since non-idealities in the
optical response of the beams proved to be important, we implemented
a fast convolution algorithm which considers the full beam response
in estimating the signal generated by the dipole. Moreover, in order
to further reduce the impact of residual systematics due to sidelobes,
we estimated time variations in the calibration constant of the 30 GHz
radiometers (the ones with the largest sidelobes) using the signal of
an internal reference load at 4 K instead of the CMB dipole. We have
estimated the accuracy of the LFI calibration following two strategies:
(1) we have run a set of simulations to assess the impact of statistical
errors and systematic effects in the instrument and in the calibration
procedure; and (2) we have performed a number of internal consistency
checks on the data and on the brightness temperature of Jupiter. Errors
in the calibration of this Planck/LFI data release are expected to be
about 0.6% at 44 and 70 GHz, and 0.8% at 30 GHz. Both these preliminary
results at low and high ℓ are consistent with WMAP results within
uncertainties and comparison of power spectra indicates good consistency
in the absolute calibration with HFI (0.3%) and a 1.4σ discrepancy
with WMAP (0.9%).
---------------------------------------------------------
Title: Planck 2013 results. XXXI. Consistency of the Planck data
Authors: Planck Collaboration; Ade, P. A. R.; Arnaud, M.; Ashdown, M.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner,
E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.;
Bielewicz, P.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Burigana, C.;
Cardoso, J. -F.; Catalano, A.; Challinor, A.; Chamballu, A.; Chiang,
H. C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Colombo,
L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia,
F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Désert, F. -X.; Dickinson, C.;
Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac,
X.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis,
M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard,
M.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio,
A.; Gruppuso, A.; Gudmundsson, J. E.; Hansen, F. K.; Hanson, D.;
Harrison, D. L.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt,
S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest,
W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.;
Keihänen, E.; Keskitalo, R.; Knoche, J.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.;
Lawrence, C. R.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.;
Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego,
M.; Lubin, P. M.; Macías-Pérez, J. F.; Maino, D.; Mandolesi,
N.; Maris, M.; Martin, P. G.; Martínez-González, E.; Masi, S.;
Matarrese, S.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss,
A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.;
Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.;
Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paoletti, D.; Partridge, B.;
Pasian, F.; Patanchon, G.; Pearson, D.; Pearson, T. J.; Perdereau, O.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.;
Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa,
L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reinecke,
M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Ristorcelli, I.;
Rocha, G.; Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri,
M.; Scott, D.; Stolyarov, V.; Sudiwala, R.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.;
Tomasi, M.; Tristram, M.; Tucci, M.; Valenziano, L.; Valiviita, J.;
Van Tent, B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.;
Wehus, I. K.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..31P Altcode: 2015arXiv150803375P
The Planck design and scanning strategy provide many levels of
redundancy that can be exploited to provide tests of internal
consistency. One of the most important is the comparison of the 70
GHz (amplifier) and 100 GHz (bolometer) channels. Based on different
instrument technologies, with feeds located differently in the focal
plane, analysed independently by different teams using different
software, and near the minimum of diffuse foreground emission, these
channels are in effect two different experiments. The 143 GHz channel
has the lowest noise level on Planck, and is near the minimum of
unresolved foreground emission. In this paper, we analyse the level
of consistency achieved in the 2013 Planck data. We concentrate on
comparisons between the 70, 100, and 143 GHz channel maps and power
spectra, particularly over the angular scales of the first and second
acoustic peaks, on maps masked for diffuse Galactic emission and for
strong unresolved sources. Difference maps covering angular scales
from 8° to 15' are consistent with noise, and show no evidence of
cosmic microwave background structure. Including small but important
corrections for unresolved-source residuals, we demonstrate agreement
(measured by deviation of the ratio from unity) between 70 and
100 GHz power spectra averaged over 70 ≤ ℓ ≤ 390 at the 0.8%
level, and agreement between 143 and 100 GHz power spectra of 0.4%
over the same ℓ range. These values are within and consistent
with the overall uncertainties in calibration given in the Planck
2013 results. We also present results based on the 2013 likelihood
analysis showing consistency at the 0.35% between the 100, 143, and
217 GHz power spectra. We analyse calibration procedures and beams to
determine what fraction of these differences can be accounted for by
known approximations or systematicerrors that could be controlled even
better in the future, reducing uncertainties still further. Several
possible small improvements are described. Subsequent analysis of the
beams quantifies the importance of asymmetry in the near sidelobes,
which was not fully accounted for initially, affecting the 70/100
ratio. Correcting for this, the 70, 100, and 143 GHz power spectra agree
to 0.4% over the first two acoustic peaks. The likelihood analysis that
produced the 2013 cosmological parameters incorporated uncertainties
larger than this. We show explicitly that correction of the missing
near sidelobe power in the HFI channels would result in shifts in the
posterior distributions of parameters of less than 0.3σ except for
A<SUB>s</SUB>, the amplitude of the primordial curvature perturbations
at 0.05 Mpc<SUP>-1</SUP>, which changes by about 1σ. We extend these
comparisons to include the sky maps from the complete nine-year mission
of the Wilkinson Microwave Anisotropy Probe (WMAP), and find a roughly
2% difference between the Planck and WMAP power spectra in the region
of the first acoustic peak.
---------------------------------------------------------
Title: Planck 2013 results. X. HFI energetic particle effects:
characterization, removal, and simulation
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner,
E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J. -P.;
Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana, C.;
Cardoso, J. -F.; Catalano, A.; Challinor, A.; Chamballu, A.; Chiang,
H. C.; Chiang, L. -Y.; Christensen, P. R.; Church, S.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.;
Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; de Bernardis, P.;
de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert,
F. -X.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.;
Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.;
Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard,
M.; Girard, D.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski,
K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson,
D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.;
Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe,
T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leonardi, R.; Leroy, C.; Lesgourgues, J.; Liguori,
M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; Mandolesi, N.; Maris, M.; Marshall,
D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee, P.; Melchiorri, A.;
Mendes, L.; Mennella, A.; Migliaccio, M.; Miniussi, A.; Mitra, S.;
Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante, G.;
Mortlock, D.; Mottet, S.; Munshi, D.; Murphy, J. A.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.;
Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.;
Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon,
G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Racine, B.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller,
T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rusholme,
B.; Sanselme, L.; Santos, D.; Sauvé, A.; Savini, G.; Scott, D.;
Shellard, E. P. S.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.;
Stompor, R.; Sudiwala, R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.;
Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Tristram, M.; Tucci, M.; Umana, G.; Valenziano, L.;
Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.;
Wade, L. A.; Wandelt, B. D.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..10P Altcode: 2013arXiv1303.5071P
We describe the detection, interpretation, and removal of the signal
resulting from interactions of high energy particles with the Planck
High Frequency Instrument (HFI). There are two types of interactions:
heating of the 0.1 K bolometer plate; and glitches in each detector time
stream. The transientresponses to detector glitch shapes are not simple
single-pole exponential decays and fall into three families. The glitch
shape for each family has been characterized empirically in flight data
and these shapes have been used to remove glitches from the detector
time streams. The spectrum of the count rate per unit energy is computed
for each family and a correspondence is made to the location on the
detector of the particle hit. Most of the detected glitches are from
Galactic protons incident on the die frame supporting the micro-machined
bolometric detectors. In the Planck orbit at L2, the particle flux is
around 5 cm<SUP>-2</SUP> s<SUP>-1</SUP> and is dominated by protons
incident on the spacecraft with energy >39 MeV, at a rate of
typically one event per second per detector. Different categories
of glitches have different signatures in the time stream. Two of the
glitch types have a low amplitude component that decays over nearly 1
s. This component produces excess noise if not properly removed from
the time-ordered data. We have used a glitch detection and subtraction
method based on the joint fit of population templates. The application
of this novel glitch subtraction method removes excess noise from the
time streams. Using realistic simulations, we find that this method
does not introduce signal bias into the Planck data.
---------------------------------------------------------
Title: Planck 2013 results. XIV. Zodiacal emission
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.;
Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger,
F.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Cardoso,
J. -F.; Catalano, A.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang,
H. C.; Chiang, L. -Y.; Christensen, P. R.; Church, S.; Clements,
D. L.; Colley, J. -M.; Colombi, S.; Colombo, L. P. L.; Couchot, F.;
Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies,
R. D.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.;
Delouis, J. -M.; Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dole,
H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.;
Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.;
Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton,
S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison,
D.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.;
Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe,
T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.;
Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs,
R. J.; Lawrence, C. R.; Leonardi, R.; Lesgourgues, J.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris,
M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi,
S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Meinhold,
P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante, G.;
Mortlock, D.; Mottet, S.; Munshi, D.; Murphy, J. A.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.;
Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; O'Sullivan,
C.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polegre, A. M.; Polenta,
G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rowan-Robinson,
M.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.;
Seiffert, M. D.; Shellard, E. P. S.; Smoot, G. F.; Spencer, L. D.;
Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sureau,
F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Tucci, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Valiviita,
J.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..14P Altcode: 2013arXiv1303.5074P
The Planck satellite provides a set of all-sky maps at nine
frequencies from 30 GHz to 857 GHz. Planets, minor bodies, and diffuse
interplanetary dust emission (IPD) are all observed. The IPD can be
separated from Galactic and other emissions because Planck views a
given point on the celestial sphere multiple times, through different
columns of IPD. We use the Planck data to investigate the behaviour of
zodiacal emission over the whole sky at sub-millimetre and millimetre
wavelengths. We fit the Planck data to find the emissivities of
the various components of the COBE zodiacal model - a diffuse cloud,
three asteroidal dust bands, a circumsolar ring, and an Earth-trailing
feature. The emissivity of the diffuse cloud decreases with increasing
wavelength, as expected from earlier analyses. The emissivities of
the dust bands, however, decrease less rapidly, indicating that the
properties of the grains in the bands are different from those in
the diffuse cloud. We fit the small amount of Galactic emission seen
through the telescope's far sidelobes, and place limits on possible
contamination of the cosmic microwave background (CMB) results from
both zodiacal and far-sidelobe emission. When necessary, the results
are used in the Planck pipeline to make maps with zodiacal emission
and far sidelobes removed. We show that the zodiacal correction to the
CMB maps is small compared to the Planck CMB temperature power spectrum
and give a list of flux densities for small solar system bodies.
---------------------------------------------------------
Title: Planck 2013 results. XXX. Cosmic infrared background
measurements and implications for star formation
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bethermin, M.; Bielewicz, P.;
Blagrave, K.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bridges, M.; Bucher,
M.; Burigana, C.; Butler, R. C.; Cardoso, J. -F.; Catalano, A.;
Challinor, A.; Chamballu, A.; Chen, X.; Chiang, H. C.; Chiang,
L. -Y.; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.;
Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.;
Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis,
P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.;
Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.;
Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi,
E.; Galeotta, S.; Ganga, K.; Ghosh, T.; Giard, M.; Giraud-Héraud,
Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio,
A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D.; Helou,
G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.;
Jones, W. C.; Juvela, M.; Kalberla, P.; Keihänen, E.; Kerp, J.;
Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz,
M.; Kurki-Suonio, H.; Lacasa, F.; Lagache, G.; Lähteenmäki, A.;
Lamarre, J. -M.; Langer, M.; Lasenby, A.; Laureijs, R. J.; Lawrence,
C. R.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.; Liguori,
M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.;
Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.;
Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.;
Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.; Paci,
F.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Partridge, B.;
Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.;
Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski,
S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen,
T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen,
J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.;
Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Roudier, G.; Rowan-Robinson, M.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.;
Seiffert, M. D.; Serra, P.; Shellard, E. P. S.; Spencer, L. D.; Starck,
J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau,
F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Tucci, M.; Tuovinen, J.; Türler, M.; Valenziano, L.; Valiviita,
J.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Welikala, N.; White, M.; White, S. D. M.; Winkel,
B.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..30P Altcode: 2013arXiv1309.0382P
We present new measurements of cosmic infrared background (CIB)
anisotropies using Planck. Combining HFI data with IRAS, the angular
auto- and cross-frequency power spectrum is measured from 143 to 3000
GHz, and the auto-bispectrum from 217 to 545 GHz. The total areas
used to compute the CIB power spectrum and bispectrum are about 2240
and 4400 deg<SUP>2</SUP>, respectively. After careful removal of the
contaminants (cosmic microwave background anisotropies, Galactic dust,
and Sunyaev-Zeldovich emission), and a complete study of systematics,
the CIB power spectrum is measured with unprecedented signal to noise
ratio from angular multipoles ℓ ~ 150 to 2500. The bispectrum due
to the clustering of dusty, star-forming galaxies is measured from
ℓ ~ 130 to 1100, with a total signal to noise ratio of around 6,
19, and 29 at 217, 353, and 545 GHz, respectively. Two approaches
are developed for modelling CIB power spectrum anisotropies. The
first approach takes advantage of the unique measurements by Planck
at large angular scales, and models only the linear part of the
power spectrum, with a mean bias of dark matter haloes hosting dusty
galaxies at a given redshift weighted by their contribution to the
emissivities. The second approach is based on a model that associates
star-forming galaxies with dark matter haloes and their subhaloes,
using a parametrized relation between the dust-processed infrared
luminosity and (sub-)halo mass. The two approaches simultaneously fit
all auto- and cross-power spectra very well. We find that the star
formation history is well constrained up to redshifts around 2, and
agrees with recent estimates of the obscured star-formation density
using Spitzer and Herschel. However, at higher redshift, the accuracy
of the star formation history measurement is strongly degraded by the
uncertainty in the spectral energy distribution of CIB galaxies. We
also find that the mean halo mass which is most efficient at hosting
star formation is log (M<SUB>eff</SUB>/M<SUB>⊙</SUB>) = 12.6 and
that CIB galaxies have warmer temperatures as redshift increases. The
CIB bispectrum is steeper than that expected from the power spectrum,
although well fitted by a power law; this gives some information about
the contribution of massive haloes to the CIB bispectrum. Finally,
we show that the same halo occupation distribution can fit all power
spectra simultaneously. The precise measurements enabled by Planck pose
new challenges for the modelling of CIB anisotropies, indicating the
power of using CIB anisotropies to understand the process of galaxy
formation.
---------------------------------------------------------
Title: Planck 2013 results. XII. Diffuse component separation
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock,
J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Boulanger, F.; Bridges, M.; Bucher, M.; Burigana, C.; Butler,
R. C.; Cardoso, J. -F.; Castex, G.; Catalano, A.; Challinor, A.;
Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, H. C.; Chiang, L. -Y.;
Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo,
L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Cruz, M.; Curto, A.;
Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.;
de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert,
F. -X.; Dickinson, C.; Diego, J. M.; Dobler, G.; Dole, H.; Donzelli,
S.; Doré, O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.;
Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Finelli, F.; Forni,
O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga,
K.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo,
J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen,
F. K.; Hanson, D.; Harrison, D. L.; Helou, G.; Henrot-Versillé,
S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.;
Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.;
Huey, G.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jewell,
J.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.;
Laureijs, R. J.; Lawrence, C. R.; Le Jeune, M.; Leach, S.; Leahy,
J. P.; Leonardi, R.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Marcos-Caballero, A.;
Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.;
Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.;
Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio,
M.; Mikkelsen, K.; Mitra, S.; Miville-Deschênes, M. -A.; Molinari, D.;
Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi,
D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; O'Dwyer, I. J.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano,
L.; Pajot, F.; Paladini, R.; Paoletti, D.; Partridge, B.; Pasian, F.;
Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrotta,
F.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Roman, M.; Rosset, C.;
Roudier, G.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme,
B.; Salerno, E.; Sandri, M.; Santos, D.; Savini, G.; Schiavon, F.;
Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Starck,
J. -L.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco,
D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.;
Van Tent, B.; Varis, J.; Viel, M.; Vielva, P.; Villa, F.; Vittorio,
N.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Wilkinson, A.; Xia,
J. -Q.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..12P Altcode: 2013arXiv1303.5072P
Planck has produced detailed all-sky observations over nine frequency
bands between 30 and 857 GHz. These observations allow robust
reconstruction of the primordial cosmic microwave background (CMB)
temperature fluctuations over nearly the full sky, as well as new
constraints on Galactic foregrounds, including thermal dust and line
emission from molecular carbon monoxide (CO). This paper describes
the component separation framework adopted by Planck for many
cosmological analyses, including CMB power spectrum determination
and likelihood construction on large angular scales, studies of
primordial non-Gaussianity and statistical isotropy, the integrated
Sachs-Wolfe effect, gravitational lensing, and searches for topological
defects. We test four foreground-cleaned CMB maps derived using
qualitatively different component separation algorithms. The quality
of our reconstructions is evaluated through detailed simulations
and internal comparisons, and shown through various tests to be
internally consistent and robust for CMB power spectrum and cosmological
parameter estimation up to ℓ = 2000. The parameter constraints on
ΛCDM cosmologies derived from these maps are consistent with those
presented in the cross-spectrum based Planck likelihood analysis. We
choose two of the CMB maps for specific scientific goals. We also
present maps and frequency spectra of the Galactic low-frequency, CO,
and thermal dust emission. The component maps are found to provide a
faithful representation of the sky, as evaluated by simulations, with
the largest bias seen in the CO component at 3%. For the low-frequency
component, the spectral index varies widely over the sky, ranging from
about β = -4 to - 2. Considering both morphology and prior knowledge
of the low frequencycomponents, the index map allows us to associate
a steep spectral index (β< -3.2) with strong anomalous microwave
emission, corresponding to a spinning dust spectrum peaking below
20 GHz, a flat index of β> -2.3 with strong free-free emission,
and intermediate values with synchrotron emission.
---------------------------------------------------------
Title: Planck 2013 results. XXV. Searches for cosmic strings and
other topological defects
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Bartolo, N.; Battaner, E.; Battye, R.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana,
C.; Butler, R. C.; Cardoso, J. -F.; Catalano, A.; Challinor, A.;
Chamballu, A.; Chiang, L. -Y.; Chiang, H. C.; Christensen, P. R.;
Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot,
F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese,
L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.;
de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.;
Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.;
Ducout, A.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Eriksen, H. K.; Fergusson, J.; Finelli, F.; Forni, O.; Frailis, M.;
Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton,
S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison,
D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Huffenberger, K. M.; Jaffe, T. R.; Jaffe, A. H.;
Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Liguori,
M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.;
Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.;
Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McEwen, J. D.;
Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Moss, A.; Munshi, D.; Naselsky, P.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.;
Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon, G.; Peiris, H. V.;
Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.;
Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.;
Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Räth, C.;
Rebolo, R.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.;
Ringeval, C.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.;
Rowan-Robinson, M.; Rusholme, B.; Sandri, M.; Santos, D.; Savini,
G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.;
Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sureau,
F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.;
Tucci, M.; Tuovinen, J.; Valenziano, L.; Valiviita, J.; Van Tent, B.;
Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt,
B. D.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..25P Altcode: 2013arXiv1303.5085P
Planck data have been used to provide stringent new constraints on
cosmic strings and other defects. We describe forecasts of the CMB
power spectrum induced by cosmic strings, calculating these from network
models and simulations using line-of-sight Boltzmann solvers. We have
studied Nambu-Goto cosmic strings, as well as field theory strings
for which radiative effects are important, thus spanning the range
of theoretical uncertainty in the underlying strings models. We have
added the angular power spectrum from strings to that for a simple
adiabatic model, with the extra fraction defined as f<SUB>10</SUB>
at multipole ℓ = 10. This parameter has been added to the standard
six parameter fit using COSMOMC with flat priors. For the Nambu-Goto
string model, we have obtained a constraint on the string tension of
Gμ/c<SUP>2</SUP> < 1.5 × 10<SUP>-7</SUP> and f<SUB>10</SUB> <
0.015 at 95% confidence that can be improved to Gμ/c<SUP>2</SUP> <
1.3 × 10<SUP>-7</SUP> and f<SUB>10</SUB> < 0.010 on inclusion
of high-ℓ CMB data. For the Abelian-Higgs field theory model we
find, Gμ<SUB>AH</SUB>/c<SUP>2</SUP>< 3.2 × 10<SUP>-7</SUP>
and f<SUB>10</SUB> < 0.028. The marginalised likelihoods for
f<SUB>10</SUB> and in the f<SUB>10</SUB>-Ω<SUB>b</SUB>h<SUP>2</SUP>
plane are also presented. We have additionally obtained comparable
constraints on f<SUB>10</SUB> for models with semilocal strings and
global textures. In terms of the effective defect energy scale these are
somewhat weaker at Gμ/c<SUP>2</SUP> < 1.1 × 10<SUP>-6</SUP>. We
have made complementarity searches for the specific non-Gaussian
signatures of cosmic strings, calibrating with all-sky Planck resolution
CMB maps generated from networks of post-recombination strings. We
have validated our non-Gaussian searches using these simulated maps
in a Planck-realistic context, estimating sensitivities of up to
ΔGμ/c<SUP>2</SUP> ≈ 4 × 10<SUP>-7</SUP>. We have obtained upper
limits on the string tension at 95% confidence of Gμ/c<SUP>2</SUP>
< 9.0 × 10<SUP>-7</SUP> with modal bispectrum estimation and
Gμ/c<SUP>2</SUP> < 7.8 × 10<SUP>-7</SUP> for real space searches
with Minkowski functionals. These are conservative upper bounds because
only post-recombination string contributions have been included in
the non-Gaussian analysis.
---------------------------------------------------------
Title: Planck 2013 results. XXI. Power spectrum and high-order
statistics of the Planck all-sky Compton parameter map
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock, J. J.;
Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bridges, M.;
Bucher, M.; Burigana, C.; Butler, R. C.; Cardoso, J. -F.; Carvalho,
P.; Catalano, A.; Challinor, A.; Chamballu, A.; Chiang, H. C.;
Chiang, L. -Y.; Christensen, P. R.; Church, S.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Comis, B.; Couchot, F.; Coulais,
A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Da Silva, A.; Danese,
L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.;
de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.;
Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.;
Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Eriksen, H. K.; Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis,
M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.;
Hanson, D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.;
Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen,
E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.;
Kunz, M.; Kurki-Suonio, H.; Lacasa, F.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.;
Leahy, J. P.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.;
Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi,
N.; Marcos-Caballero, A.; Maris, M.; Marshall, D. J.; Martin, P. G.;
Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; Melchiorri, A.; Melin, J. -B.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss,
A.; Munshi, D.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.;
Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli,
E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.;
Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli,
I.; Rocha, G.; Rosset, C.; Rossetti, M.; Roudier, G.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.;
Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Starck, J. -L.;
Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau,
F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.;
Tucci, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Valiviita, J.; Van
Tent, B.; Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..21P Altcode: 2013arXiv1303.5081P
We have constructed the first all-sky map of the thermal
Sunyaev-Zeldovich (tSZ) effect by applying specifically tailored
component separation algorithms to the 100 to 857 GHz frequency channel
maps from the Planck survey. This map shows an obvious galaxy cluster
tSZ signal that is well matched with blindly detected clusters in the
Planck SZ catalogue. To characterize the signal in the tSZ map we
have computed its angular power spectrum. At large angular scales
(ℓ < 60), the major foreground contaminant is the diffuse
thermal dust emission. At small angular scales (ℓ > 500) the
clustered cosmic infrared background and residual point sources are
the major contaminants. These foregrounds are carefully modelled and
subtracted. We thus measure the tSZ power spectrum over angular scales
0.17° ≲ θ ≲ 3.0° that were previously unexplored. The measured
tSZ power spectrum is consistent with that expected from the Planck
catalogue of SZ sources, with clear evidence of additional signal from
unresolved clusters and, potentially, diffuse warm baryons. Marginalized
band-powers of the Planck tSZ power spectrum and the best-fit model
are given. The non-Gaussianity of the Compton parameter map is further
characterized by computing its 1D probability distribution function
and its bispectrum. The measured tSZ power spectrum and high order
statistics are used to place constraints on σ<SUB>8</SUB>.
---------------------------------------------------------
Title: Planck 2013 results. XV. CMB power spectra and likelihood
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock,
J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Boulanger, F.; Bridges, M.; Bucher, M.; Burigana, C.; Butler,
R. C.; Calabrese, E.; Cardoso, J. -F.; Catalano, A.; Challinor, A.;
Chamballu, A.; Chiang, H. C.; Chiang, L. -Y.; Christensen, P. R.;
Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet,
C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia,
F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de
Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert,
F. -X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré,
O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Elsner, F.;
Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.;
Fraisse, A. A.; Franceschi, E.; Gaier, T. C.; Galeotta, S.; Galli,
S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; Gjerløw,
E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio,
A.; Gruppuso, A.; Gudmundsson, J. E.; Hansen, F. K.; Hanson, D.;
Harrison, D.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.;
Jaffe, A. H.; Jaffe, T. R.; Jewell, J.; Jones, W. C.; Juvela, M.;
Keihänen, E.; Keskitalo, R.; Kiiveri, K.; Kisner, T. S.; Kneissl,
R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Lattanzi, M.;
Laureijs, R. J.; Lawrence, C. R.; Le Jeune, M.; Leach, S.; Leahy,
J. P.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.; Liguori,
M.; Lilje, P. B.; Linden-Vørnle, M.; Lindholm, V.; López-Caniego,
M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.;
Mandolesi, N.; Marinucci, D.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese,
S.; Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.;
Mendes, L.; Menegoni, E.; Mennella, A.; Migliaccio, M.; Millea,
M.; Mitra, S.; Miville-Deschênes, M. -A.; Molinari, D.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.;
Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.;
Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.;
O'Dwyer, I. J.; Orieux, F.; Osborne, S.; Oxborrow, C. A.; Paci, F.;
Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Partridge, B.;
Pasian, F.; Patanchon, G.; Paykari, P.; Perdereau, O.; Perotto, L.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu,
N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Rahlin, A.; Rebolo, R.; Reinecke, M.;
Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ringeval, C.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rowan-Robinson,
M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Sanselme,
L.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard,
E. P. S.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor,
R.; Sudiwala, R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet,
J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Vielva, P.;
Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.;
White, M.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..15P Altcode: 2013arXiv1303.5075P
This paper presents the Planck 2013 likelihood, a complete statistical
description of the two-point correlation function of the CMB temperature
fluctuations that accounts for all known relevant uncertainties,
both instrumental and astrophysical in nature. We use this likelihood
to derive our best estimate of the CMB angular power spectrum from
Planck over three decades in multipole moment, ℓ, covering 2 ≤ ℓ
≤ 2500. The main source of uncertainty at ℓ ≲ 1500 is cosmic
variance. Uncertainties in small-scale foreground modelling and
instrumental noise dominate the error budget at higher ℓs. For ℓ
< 50, our likelihood exploits all Planck frequency channels from 30
to 353 GHz, separating the cosmological CMB signal from diffuse Galactic
foregrounds through a physically motivated Bayesian component separation
technique. At ℓ ≥ 50, we employ a correlated Gaussian likelihood
approximation based on a fine-grained set of angular cross-spectra
derived from multiple detector combinations between the 100, 143, and
217 GHz frequency channels, marginalising over power spectrum foreground
templates. We validate our likelihood through an extensive suite of
consistency tests, and assess the impact of residual foreground and
instrumental uncertainties on the final cosmological parameters. We
find good internal agreement among the high-ℓ cross-spectra with
residuals below a few μK<SUP>2</SUP> at ℓ ≲ 1000, in agreement
with estimated calibration uncertainties. We compare our results with
foreground-cleaned CMB maps derived from all Planck frequencies, as
well as with cross-spectra derived from the 70 GHz Planck map, and
find broad agreement in terms of spectrum residuals and cosmological
parameters. We further show that the best-fit ΛCDM cosmology is in
excellent agreement with preliminary PlanckEE and TE polarisation
spectra. We find that the standard ΛCDM cosmology is well constrained
by Planck from the measurements at ℓ ≲ 1500. One specific example
is the spectral index of scalar perturbations, for which we report a
5.4σ deviation from scale invariance, n<SUB>s</SUB> = 1. Increasing
the multipole range beyond ℓ ≃ 1500 does not increase our accuracy
for the ΛCDM parameters, but instead allows us to study extensions
beyond the standard model. We find no indication of significant
departures from the ΛCDM framework. Finally, we report a tension
between the Planck best-fit ΛCDM model and the low-ℓ spectrum in
the form of a power deficit of 5-10% at ℓ ≲ 40, with a statistical
significance of 2.5-3σ. Without a theoretically motivated model for
this power deficit, we do not elaborate further on its cosmological
implications, but note that this is our most puzzling finding in an
otherwise remarkably consistent data set.
---------------------------------------------------------
Title: Planck 2013 results. XVIII. The gravitational lensing-infrared
background correlation
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela,
F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Bartlett, J. G.; Basak, S.; Battaner, E.; Benabed, K.; Benoît, A.;
Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bethermin, M.;
Bielewicz, P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bridges, M.; Bucher, M.;
Burigana, C.; Butler, R. C.; Cardoso, J. -F.; Catalano, A.; Challinor,
A.; Chamballu, A.; Chiang, H. C.; Chiang, L. -Y.; Christensen,
P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.;
Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.;
Danese, L.; Davies, R. D.; de Bernardis, P.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Diego, J. M.;
Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou,
G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis,
M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.;
Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Hansen, F. K.; Hanson,
D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.;
Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe,
T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.;
Lacasa, F.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby,
A.; Laureijs, R. J.; Lawrence, C. R.; Leonardi, R.; León-Tavares,
J.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.;
Migliaccio, M.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.;
Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.;
Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.;
Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon,
G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rowan-Robinson,
M.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.;
Seiffert, M. D.; Serra, P.; Shellard, E. P. S.; Spencer, L. D.; Starck,
J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau,
F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Tucci, M.; Tuovinen, J.; Valenziano, L.; Valiviita, J.; Van Tent,
B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..18P Altcode: 2013arXiv1303.5078P
The multi-frequency capability of the Planck satellite provides
information both on the integrated history of star formation (via the
cosmic infrared background, or CIB) and on the distribution of dark
matter (via the lensing effect on the cosmic microwave background,
or CMB). The conjunction of these two unique probes allows us to
measure directly the connection between dark and luminous matter
in the high redshift (1 ≤ z ≤ 3) Universe. We use a three-point
statistic optimized to detect the correlation between these two tracers,
using lens reconstructions at 100, 143, and 217 GHz, together with CIB
measurements at 100-857 GHz. Following a thorough discussion of possible
contaminants and a suite of consistency tests, we report the first
detection of the correlation between the CIB and CMB lensing. The well
matched redshift distribution of these two signals leads to a detection
significance with a peak value of 42/19σ (statistical/statistical
+ systematics) at 545 GHz and a correlation as high as 80% across
these two tracers. Our full set of multi-frequency measurements
(both CIB auto- and CIB-lensing cross-spectra) are consistent with
a simple halo-based model, with a characteristic mass scale for the
halos hosting CIB sources of log<SUB>10</SUB>(M/M<SUB>⊙</SUB>)
= 10.5 ± 0.6. Leveraging the frequency dependence of our signal,
we isolate the high redshift contribution to the CIB, and constrain
the star formation rate (SFR) density at z ≥ 1. We measure directly
the SFR density with around 2σ significance for three redshift bins
between z = 1 and 7, thus opening a new window into the study of the
formation of stars at early times.
---------------------------------------------------------
Title: Planck 2013 results. XXIV. Constraints on primordial
non-Gaussianity
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela,
F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Bartlett, J. G.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana,
C.; Butler, R. C.; Cardoso, J. -F.; Catalano, A.; Challinor, A.;
Chamballu, A.; Chiang, H. C.; Chiang, L. -Y.; Christensen, P. R.;
Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot,
F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese,
L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de
Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Diego,
J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.;
Dunkley, J.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.;
Eriksen, H. K.; Fergusson, J.; Finelli, F.; Forni, O.; Frailis, M.;
Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giraud-Héraud,
Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio,
A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D.; Heavens,
A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.;
Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lacasa, F.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Lewis,
A.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi,
N.; Mangilli, A.; Marinucci, D.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss,
A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Peiris, H. V.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli,
E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Racine, B.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier,
G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos,
D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.;
Smith, K.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor,
R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutter, P.; Sutton, D.;
Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Tuovinen, J.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis,
J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
White, M.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..24P Altcode: 2013arXiv1303.5084P
The Planck nominal mission cosmic microwave background (CMB) maps yield
unprecedented constraints on primordial non-Gaussianity (NG). Using
three optimal bispectrum estimators, separable template-fitting
(KSW), binned, and modal, we obtain consistent values for the
primordial local, equilateral, and orthogonal bispectrum amplitudes,
quoting as our final result f<SUB>NL</SUB><SUP>local</SUP>
= 2.7 ± 5.8, f<SUB>NL</SUB><SUP>equil</SUP> = -42 ±
75, and f<SUB>NL</SUB><SUP>orth</SUP> = -25 ± 39 (68% CL
statistical). Non-Gaussianity is detected in the data; using
skew-C<SUB>ℓ</SUB> statistics we find a nonzero bispectrum from
residual point sources, and the integrated-Sachs-Wolfe-lensing
bispectrum at a level expected in the ΛCDM scenario. The results are
based on comprehensive cross-validation of these estimators on Gaussian
and non-Gaussian simulations, are stable across component separation
techniques, pass an extensive suite of tests, and are confirmed by
skew-C<SUB>ℓ</SUB>, wavelet bispectrum and Minkowski functional
estimators. Beyond estimates of individual shape amplitudes, we present
model-independent, three-dimensional reconstructions of the Planck CMB
bispectrum and thus derive constraints on early-Universe scenarios
that generate primordial NG, including general single-field models
of inflation, excited initial states (non-Bunch-Davies vacua), and
directionally-dependent vector models. We provide an initial survey of
scale-dependent feature and resonance models. These results bound both
general single-field and multi-field model parameter ranges, such as the
speed of sound, c<SUB>s</SUB> ≥ 0.02 (95% CL), in an effective field
theory parametrization, and the curvaton decay fraction r<SUB>D</SUB>
≥ 0.15 (95% CL). The Planck data significantly limit the viable
parameter space of the ekpyrotic/cyclic scenarios. The amplitude of the
four-point function in the local model τ<SUB>NL</SUB>< 2800 (95%
CL). Taken together, these constraints represent the highest precision
tests to date of physical mechanisms for the origin of cosmic structure.
---------------------------------------------------------
Title: Planck 2013 results. XXVI. Background geometry and topology
of the Universe
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock,
J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Cardoso,
J. -F.; Catalano, A.; Challinor, A.; Chamballu, A.; Chiang, H. C.;
Chiang, L. -Y.; Christensen, P. R.; Church, S.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill,
B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis,
R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.;
Delouis, J. -M.; Désert, F. -X.; Diego, J. M.; Dole, H.; Donzelli,
S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin,
T. A.; Eriksen, H. K.; Fabre, O.; Finelli, F.; Forni, O.; Frailis,
M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino,
G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.;
Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson,
D.; Harrison, D. L.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.;
Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo,
R.; Kisner, T. S.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.;
Laureijs, R. J.; Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; Leroy,
C.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; McEwen, J. D.; Melchiorri, A.; Mendes, L.;
Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, M. -A.;
Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi,
D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Peiris, H. V.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli,
E.; Pietrobon, D.; Plaszczynski, S.; Pogosyan, D.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Riazuelo, A.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.;
Rowan-Robinson, M.; Rusholme, B.; Sandri, M.; Santos, D.; Savini,
G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.;
Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sureau,
F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.;
Tucci, M.; Tuovinen, J.; Valenziano, L.; Valiviita, J.; Van Tent, B.;
Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt,
B. D.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..26P Altcode: 2013arXiv1303.5086P
The new cosmic microwave background (CMB) temperature maps from
Planck provide the highest-quality full-sky view of the surface of
last scattering available to date. This allows us to detect possible
departures from the standard model of a globally homogeneous and
isotropic cosmology on the largest scales. We search for correlations
induced by a possible non-trivial topology with a fundamental domain
intersecting, or nearly intersecting, the last scattering surface
(at comoving distance χ<SUB>rec</SUB>), both via a direct search
for matched circular patterns at the intersections and by an optimal
likelihood search for specific topologies. For the latter we consider
flat spaces with cubic toroidal (T3), equal-sided chimney (T2)
and slab (T1) topologies, three multi-connected spaces of constant
positive curvature (dodecahedral, truncated cube and octahedral)
and two compact negative-curvature spaces. These searches yield no
detection of the compact topology with the scale below the diameter
of the last scattering surface. For most compact topologies studied
the likelihood maximized over the orientation of the space relative
to the observed map shows some preference for multi-connected models
just larger than the diameter of the last scattering surface. Since
this effect is also present in simulated realizations of isotropic
maps, we interpret it as the inevitable alignment of mild anisotropic
correlations with chance features in a single sky realization; such
a feature can also be present, in milder form, when the likelihood
is marginalized over orientations. Thus marginalized, the limits
on the radius ℛ<SUB>i</SUB> of the largest sphere inscribed in
topological domain (at log-likelihood-ratio Δln ℒ > -5 relative
to a simply-connected flat Planck best-fit model) are: in a flat
Universe, ℛ<SUB>i</SUB>> 0.92χ<SUB>rec</SUB> for the T3 cubic
torus; ℛ<SUB>i</SUB>> 0.71χ<SUB>rec</SUB> for the T2 chimney;
ℛ<SUB>i</SUB>> 0.50χ<SUB>rec</SUB> for the T1 slab; and in a
positively curved Universe, ℛ<SUB>i</SUB>> 1.03χ<SUB>rec</SUB>
for the dodecahedral space; ℛ<SUB>i</SUB>> 1.0χ<SUB>rec</SUB> for
the truncated cube; and ℛ<SUB>i</SUB>> 0.89χ<SUB>rec</SUB> for the
octahedral space. The limit for a wider class of topologies, i.e., those
predicting matching pairs of back-to-back circles, among them tori and
the three spherical cases listed above, coming from the matched-circles
search, is ℛ<SUB>i</SUB>> 0.94χ<SUB>rec</SUB> at 99% confidence
level. Similar limits apply to a wide, although not exhaustive, range
of topologies. We also perform a Bayesian search for an anisotropic
global Bianchi VII<SUB>h</SUB> geometry. In the non-physical setting
where the Bianchi cosmology is decoupled from the standard cosmology,
Planck data favour the inclusion of a Bianchi component with a Bayes
factor of at least 1.5 units of log-evidence. Indeed, the Bianchi
pattern is quite efficient at accounting for some of the large-scale
anomalies found in Planck data. However, the cosmological parameters
that generate this pattern are in strong disagreement with those found
from CMB anisotropy data alone. In the physically motivated setting
where the Bianchi parameters are coupled and fitted simultaneously with
the standard cosmological parameters, we find no evidence for a Bianchi
VII<SUB>h</SUB> cosmology and constrain the vorticity of such models to
(ω/H)<SUB>0</SUB>< 8.1 × 10<SUP>-10</SUP> (95% confidence level).
---------------------------------------------------------
Title: Planck 2013 results. XXII. Constraints on inflation
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela,
F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Bartlett, J. G.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill,
J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana, C.; Butler,
R. C.; Calabrese, E.; Cardoso, J. -F.; Catalano, A.; Challinor, A.;
Chamballu, A.; Chiang, H. C.; Chiang, L. -Y.; Christensen, P. R.;
Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot,
F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.;
Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Dickinson,
C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.;
Dunkley, J.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.;
Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.;
Ganga, K.; Gauthier, C.; Giard, M.; Giardino, G.; Giraud-Héraud,
Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio,
A.; Gruppuso, A.; Hamann, J.; Hansen, F. K.; Hanson, D.; Harrison,
D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.;
Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leach, S.; Leahy, J. P.; Leonardi, R.; Lesgourgues,
J.; Lewis, A.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.;
Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, M. -A.;
Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi,
D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; O'Dwyer, I. J.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano,
L.; Pajot, F.; Paladini, R.; Pandolfi, S.; Paoletti, D.; Partridge,
B.; Pasian, F.; Patanchon, G.; Peiris, H. V.; Perdereau, O.; Perotto,
L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu,
N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Roudier, G.; Rowan-Robinson, M.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savelainen, M.; Savini,
G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.;
Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev,
R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.;
Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Tréguer-Goudineau, J.; Tristram, M.; Tucci, M.; Tuovinen, J.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Vielva, P.;
Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; White, M.;
Wilkinson, A.; Yvon, D.; Zacchei, A.; Zibin, J. P.; Zonca, A.
2014A&A...571A..22P Altcode: 2013arXiv1303.5082P
We analyse the implications of the Planck data for cosmic inflation. The
Planck nominal mission temperature anisotropy measurements, combined
with the WMAP large-angle polarization, constrain the scalar spectral
index to be n<SUB>s</SUB> = 0.9603 ± 0.0073, ruling out exact scale
invariance at over 5σ.Planck establishes an upper bound on the
tensor-to-scalar ratio of r< 0.11 (95% CL). The Planck data thus
shrink the space of allowed standard inflationary models, preferring
potentials with V”< 0. Exponential potential models, the simplest
hybrid inflationary models, and monomial potential models of degree
n ≥ 2 do not provide a good fit to the data. Planck does not find
statistically significant running of the scalar spectral index,
obtaining dn<SUB>s</SUB>/ dlnk = - 0.0134 ± 0.0090. We verify these
conclusions through a numerical analysis, which makes no slow-roll
approximation, and carry out a Bayesian parameter estimation
and model-selection analysis for a number of inflationary models
including monomial, natural, and hilltop potentials. For each model,
we present the Planck constraints on the parameters of the potential
and explore several possibilities for the post-inflationary entropy
generation epoch, thus obtaining nontrivial data-driven constraints. We
also present a direct reconstruction of the observable range of the
inflaton potential. Unless a quartic term is allowed in the potential,
we find results consistent with second-order slow-roll predictions. We
also investigate whether the primordial power spectrum contains any
features. We find that models with a parameterized oscillatory feature
improve the fit by Δχ<SUP>2</SUP><SUB>eff</SUB> ≈ 10; however,
Bayesian evidence does not prefer these models. We constrain several
single-field inflation models with generalized Lagrangians by combining
power spectrum data with Planck bounds on f<SUB>NL</SUB>. Planck
constrains with unprecedented accuracy the amplitude and possible
correlation (with the adiabatic mode) of non-decaying isocurvature
fluctuations. The fractional primordial contributions of cold dark
matter (CDM) isocurvature modes of the types expected in the curvaton
and axion scenarios have upper bounds of 0.25% and 3.9% (95% CL),
respectively. In models with arbitrarily correlated CDM or neutrino
isocurvature modes, an anticorrelated isocurvature component can
improve the χ<SUP>2</SUP><SUB>eff</SUB> by approximately 4 as a
result of slightly lowering the theoretical prediction for the ℓ
≲ 40 multipoles relative to the higher multipoles. Nonetheless,
the data are consistent with adiabatic initial conditions.
---------------------------------------------------------
Title: Planck 2013 results. XIX. The integrated Sachs-Wolfe effect
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela,
F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Bartlett, J. G.; Bartolo, N.; Battaner, E.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana,
C.; Butler, R. C.; Cardoso, J. -F.; Catalano, A.; Challinor, A.;
Chamballu, A.; Chiang, H. C.; Chiang, L. -Y.; Christensen, P. R.;
Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot,
F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.;
Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Dickinson,
C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.;
Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen,
H. K.; Fergusson, J.; Finelli, F.; Forni, O.; Fosalba, P.; Frailis, M.;
Franceschi, E.; Frommert, M.; Galeotta, S.; Ganga, K.; Génova-Santos,
R. T.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo,
J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.;
Hansen, F. K.; Hanson, D.; Harrison, D.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon,
E.; Ho, S.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.;
Huffenberger, K. M.; Ilić, S.; Jaffe, A. H.; Jaffe, T. R.; Jasche,
J.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Langer, M.; Lasenby, A.;
Laureijs, R. J.; Lawrence, C. R.; Leahy, J. P.; Leonardi, R.;
Lesgourgues, J.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.;
Maino, D.; Mandolesi, N.; Mangilli, A.; Marcos-Caballero, A.; Maris,
M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi,
S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Meinhold,
P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante, G.;
Mortlock, D.; Moss, A.; Munshi, D.; Naselsky, P.; Nati, F.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano,
L.; Pajot, F.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon,
G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Racine, B.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, A.;
Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Roudier, G.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme,
B.; Sandri, M.; Santos, D.; Savini, G.; Schaefer, B. M.; Schiavon,
F.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.;
Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev,
R.; Sureau, F.; Sutter, P.; Sutton, D.; Suur-Uski, A. -S.; Sygnet,
J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Umana, G.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Viel, M.;
Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
White, M.; Xia, J. -Q.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..19P Altcode: 2013arXiv1303.5079P
Based on cosmic microwave background (CMB) maps from the 2013
Planck Mission data release, this paper presents the detection of
the integrated Sachs-Wolfe (ISW) effect, that is, the correlation
between the CMB and large-scale evolving gravitational potentials. The
significance of detection ranges from 2 to 4σ, depending on which
method is used. We investigated three separate approaches, which
essentially cover all previous studies, and also break new ground. (i)
We correlated the CMB with the Planck reconstructed gravitational
lensing potential (for the first time). This detection was made
using the lensing-induced bispectrum between the low-ℓ and high-ℓ
temperature anisotropies; the correlation between lensing and the ISW
effect has a significance close to 2.5σ. (ii) We cross-correlated
with tracers of large-scale structure, which yielded a significance of
about 3σ, based on a combination of radio (NVSS) and optical (SDSS)
data. (iii) We used aperture photometry on stacked CMB fields at the
locations of known large-scale structures, which yielded and confirms
a 4σ signal, over a broader spectral range, when using a previously
explored catalogue, but shows strong discrepancies in amplitude and
scale when compared with expectations. More recent catalogues give
more moderate results that range from negligible to 2.5σ at most,
but have a more consistent scale and amplitude, the latter being still
slightly higher than what is expected from numerical simulations
within ΛCMD. Where they can be compared, these measurements are
compatible with previous work using data from WMAP, where these
scales have been mapped to the limits of cosmic variance. Planck's
broader frequency coverage allows for better foreground cleaning and
confirms that the signal is achromatic, which makes it preferable
for ISW detection. As a final step we used tracers of large-scale
structure to filter the CMB data, from which we present maps of the
ISW temperature perturbation. These results provide complementary and
independent evidence for the existence of a dark energy component that
governs the currently accelerated expansion of the Universe.
---------------------------------------------------------
Title: Planck 2013 results. XXIX. The Planck catalogue of
Sunyaev-Zeldovich sources
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Aussel, H.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Barrena, R.; Bartelmann, M.; Bartlett, J. G.; Battaner,
E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.; Bernard, J. -P.;
Bersanelli, M.; Bielewicz, P.; Bikmaev, I.; Bobin, J.; Bock, J. J.;
Böhringer, H.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Bridges, M.; Bucher, M.; Burenin, R.; Burigana, C.; Butler, R. C.;
Cardoso, J. -F.; Carvalho, P.; Catalano, A.; Challinor, A.; Chamballu,
A.; Chary, R. -R.; Chen, X.; Chiang, H. C.; Chiang, L. -Y.; Chon,
G.; Christensen, P. R.; Churazov, E.; Church, S.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Comis, B.; Couchot, F.; Coulais,
A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Da Silva, A.; Dahle, H.;
Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Démoclès,
J.; Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole,
H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou,
G.; Eisenhardt, P. R. M.; Enßlin, T. A.; Eriksen, H. K.; Feroz, F.;
Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi, E.;
Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard,
M.; Giardino, G.; Gilfanov, M.; Giraud-Héraud, Y.; González-Nuevo,
J.; Górski, K. M.; Grainge, K. J. B.; Gratton, S.; Gregorio, A.;
Groeneboom, N., E.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison,
D.; Hempel, A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.;
Hurley-Walker, N.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela,
M.; Keihänen, E.; Keskitalo, R.; Khamitov, I.; Kisner, T. S.; Kneissl,
R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.;
Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; León-Tavares, J.;
Lesgourgues, J.; Li, C.; Liddle, A.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris,
M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi,
S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Mei, S.;
Meinhold, P. R.; Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella,
A.; Migliaccio, M.; Mikkelsen, K.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi,
D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Nesvadba,
N. P. H.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Olamaie, M.; Osborne,
S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paoletti, D.;
Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto,
L.; Perrott, Y. C.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli,
E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rowan-Robinson,
M.; Rubiño-Martín, J. A.; Rumsey, C.; Rusholme, B.; Sandri, M.;
Santos, D.; Saunders, R. D. E.; Savini, G.; Schammel, M. P.; Scott,
D.; Seiffert, M. D.; Shellard, E. P. S.; Shimwell, T. W.; Spencer,
L. D.; Stanford, S. A.; Starck, J. -L.; Stolyarov, V.; Stompor, R.;
Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.;
Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.;
Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vibert, L.;
Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
White, M.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..29P Altcode: 2013arXiv1303.5089P
We describe the all-sky Planck catalogue of clusters and cluster
candidates derived from Sunyaev-Zeldovich (SZ) effect detections using
the first 15.5 months of Planck satellite observations. The catalogue
contains 1227 entries, making it over six times the size of the Planck
Early SZ (ESZ) sample and the largest SZ-selected catalogue to date. It
contains 861 confirmed clusters, of which 178 have been confirmed as
clusters, mostly through follow-up observations, and a further 683
are previously-known clusters. The remaining 366 have the status of
cluster candidates, and we divide them into three classes according to
the quality of evidence that they are likely to be true clusters. The
Planck SZ catalogue is the deepest all-sky cluster catalogue, with
redshifts up to about one, and spans the broadest cluster mass range
from (0.1 to 1.6) × 10<SUP>15</SUP> M<SUB>⊙</SUB>. Confirmation
of cluster candidates through comparison with existing surveys or
cluster catalogues is extensively described, as is the statistical
characterization of the catalogue in terms of completeness and
statistical reliability. The outputs of the validation process are
provided as additional information. This gives, in particular, an
ensemble of 813 cluster redshifts, and for all these Planck clusters we
also include a mass estimated from a newly-proposed SZ-mass proxy. A
refined measure of the SZ Compton parameter for the clusters with
X-ray counter-parts is provided, as is an X-ray flux for all the
Planck clusters not previously detected in X-ray surveys. <P />The
catalogue of SZ sources is available at Planck Legacy Archive and <A
href="http://www.sciops.esa.int/index.php?page=Planck_Legacy_Archive&project=planck">http://www.sciops.esa.int/index.php?page=Planck_Legacy_Archive&project=planck</A>
---------------------------------------------------------
Title: Planck 2013 results. XXIII. Isotropy and statistics of the CMB
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Bartolo, N.; Battaner, E.; Battye, R.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana, C.;
Butler, R. C.; Cardoso, J. -F.; Catalano, A.; Challinor, A.; Chamballu,
A.; Chary, R. -R.; Chiang, H. C.; Chiang, L. -Y.; Christensen, P. R.;
Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot,
F.; Coulais, A.; Crill, B. P.; Cruz, M.; Curto, A.; Cuttaia, F.;
Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.;
Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Ducout,
A.; Dupac, X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen,
H. K.; Fantaye, Y.; Fergusson, J.; Finelli, F.; Forni, O.; Frailis,
M.; Franceschi, E.; Frommert, M.; Galeotta, S.; Ganga, K.; Giard,
M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski,
K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hansen,
M.; Hanson, D.; Harrison, D. L.; Helou, G.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger,
K. M.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen,
E.; Keskitalo, R.; Kim, J.; Kisner, T. S.; Knoche, J.; Knox, L.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre,
J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leahy, J. P.;
Leonardi, R.; Leroy, C.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Mangilli, A.; Marinucci,
D.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González,
E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.;
McEwen, J. D.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella,
A.; Migliaccio, M.; Mikkelsen, K.; Mitra, S.; Miville-Deschênes,
M. -A.; Molinari, D.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock,
D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.; Paci,
F.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon, G.;
Peiris, H. V.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini,
F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pogosyan,
D.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen,
T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen,
J. P.; Racine, B.; Räth, C.; Rebolo, R.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Renzi, A.; Ricciardi, S.; Riller, T.; Ristorcelli,
I.; Rocha, G.; Rosset, C.; Rotti, A.; Roudier, G.; Rubiño-Martín,
J. A.; Ruiz-Granados, B.; Rusholme, B.; Sandri, M.; Santos, D.; Savini,
G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Souradeep, T.;
Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala,
R.; Sureau, F.; Sutter, P.; Sutton, D.; Suur-Uski, A. -S.; Sygnet,
J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Vielva, P.;
Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.;
White, M.; Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..23P Altcode: 2013arXiv1303.5083P
The two fundamental assumptions of the standard cosmological model -
that the initial fluctuations are statistically isotropic and Gaussian
- are rigorously tested using maps of the cosmic microwave background
(CMB) anisotropy from the Planck satellite. The detailed results are
based on studies of four independent estimates of the CMB that are
compared to simulations using a fiducial ΛCDM model and incorporating
essential aspects of the Planck measurement process. Deviations from
isotropy have been found and demonstrated to be robust against component
separation algorithm, mask choice, and frequency dependence. Many of
these anomalies were previously observed in the WMAP data, and are
now confirmed at similar levels of significance (about 3σ). However,
we find little evidence of non-Gaussianity, with the exception of a
few statistical signatures that seem to be associated with specific
anomalies. In particular, we find that the quadrupole-octopole alignment
is also connected to a low observed variance in the CMB signal. A
power asymmetry is now found to persist on scales corresponding
to about ℓ = 600 and can be described in the low-ℓ regime by a
phenomenological dipole modulation model. However, any primordial power
asymmetry is strongly scale-dependent and does not extend toarbitrarily
small angular scales. Finally, it is plausible that some of these
features may be reflected in the angular power spectrum of the data,
which shows a deficit of power on similar scales. Indeed, when the
power spectra of two hemispheres defined by a preferred direction
are considered separately, one shows evidence of a deficit in power,
while its opposite contains oscillations between odd and even modes
that may be related to the parity violation and phase correlations
also detected in the data. Although these analyses represent a step
forward in building an understanding of the anomalies, a satisfactory
explanation based on physically motivated models is still lacking.
---------------------------------------------------------
Title: Planck 2013 results. XIII. Galactic CO emission
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Alves, M. I. R.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.;
Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.;
Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Boulanger, F.; Bridges, M.; Bucher, M.; Burigana,
C.; Butler, R. C.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.;
Chary, R. -R.; Chen, X.; Chiang, H. C.; Chiang, L. -Y.; Christensen,
P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.;
Combet, C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.;
Cuttaia, F.; Danese, L.; Davies, R. D.; de Bernardis, P.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Dempsey, J. T.;
Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.;
Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Eriksen, H. K.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis,
M.; Franceschi, E.; Fukui, Y.; Galeotta, S.; Ganga, K.; Giard, M.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton,
S.; Gregorio, A.; Gruppuso, A.; Handa, T.; Hansen, F. K.; Hanson,
D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hily-Blant, P.; Hivon, E.; Hobson,
M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.;
Hurier, G.; Jaffe, A. H.; Jaffe, T. R.; Jewell, J.; Jones, W. C.;
Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Knoche, J.;
Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence,
C. R.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.; Liguori,
M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; Maffei, B.; Mandolesi, N.; Maris, M.;
Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.;
Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee, P.;
Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Moore,
T. J. T.; Morgante, G.; Morino, J.; Mortlock, D.; Munshi, D.; Murphy,
J. A.; Nakajima, T.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; Okuda, T.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.;
Pajot, F.; Paladini, R.; Paoletti, D.; Pasian, F.; Patanchon, G.;
Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.;
Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri,
M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard,
E. P. S.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor, R.;
Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.;
Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Thomas,
H. S.; Toffolatti, L.; Tomasi, M.; Torii, K.; Tristram, M.; Tucci,
M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent,
B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
Wehus, I. K.; Yamamoto, H.; Yoda, T.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..13P Altcode: 2013arXiv1303.5073T; 2013arXiv1303.5073P
Rotational transition lines of CO play a major role in molecular radio
astronomy as a mass tracer and in particular in the study of star
formation and Galactic structure. Although a wealth of data exists for
the Galactic plane and some well-known molecular clouds, there is no
available high sensitivity all-sky survey of CO emission to date. Such
all-sky surveys can be constructed using the Planck HFI data because
the three lowest CO rotational transition lines at 115, 230 and 345
GHz significantly contribute to the signal of the 100, 217 and 353
GHz HFI channels, respectively. Two different component separation
methods are used to extract the CO maps from Planck HFI data. The maps
obtained are then compared to one another and to existing external CO
surveys. From these quality checks the best CO maps, in terms of signal
to noise ratio and/or residual contamination by other emission, are
selected. Three different sets of velocity-integrated CO emission maps
are produced with different trade-offs between signal-to-noise, angular
resolution, and reliability. Maps for the CO J = 1 → 0, J = 2 → 1,
and J = 3 → 2 rotational transitions are presented and described in
detail. They are shown to be fully compatible with previous surveys
of parts of the Galactic plane as well as with undersampled surveys of
the high latitude sky. The Planck HFI velocity-integrated CO maps for
the J = 1 → 0, J = 2 → 1, and J = 3 →2 rotational transitions
provide an unprecedented all-sky CO view of the Galaxy. These maps
are also of great interest to monitor potential CO contamination of
the Planck studies of the cosmological microwave background.
---------------------------------------------------------
Title: Planck 2013 results. XVI. Cosmological parameters
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock,
J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Calabrese,
E.; Cappellini, B.; Cardoso, J. -F.; Catalano, A.; Challinor, A.;
Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, H. C.; Chiang, L. -Y.;
Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo,
L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia,
F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de
Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert,
F. -X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli,
S.; Doré, O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.;
Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.;
Frailis, M.; Fraisse, A. A.; Franceschi, E.; Gaier, T. C.; Galeotta,
S.; Galli, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Héraud,
Y.; Gjerløw, E.; González-Nuevo, J.; Górski, K. M.; Gratton, S.;
Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.; Haissinski, J.; Hamann,
J.; Hansen, F. K.; Hanson, D.; Harrison, D.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon,
E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hou, Z.; Hovest,
W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jewell, J.;
Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.;
Lattanzi, M.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leahy,
J. P.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.; Lewis, A.;
Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi,
N.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González,
E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta,
P.; Meinhold, P. R.; Melchiorri, A.; Melin, J. -B.; Mendes, L.;
Menegoni, E.; Mennella, A.; Migliaccio, M.; Millea, M.; Mitra, S.;
Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante, G.;
Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.;
Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne,
S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, D.;
Pearson, T. J.; Peiris, H. V.; Perdereau, O.; Perotto, L.; Perrotta,
F.; Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.; Rowan-Robinson,
M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.;
Savelainen, M.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard,
E. P. S.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor,
R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.;
Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.;
Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
Wehus, I. K.; White, M.; White, S. D. M.; Wilkinson, A.; Yvon, D.;
Zacchei, A.; Zonca, A.
2014A&A...571A..16P Altcode: 2013arXiv1303.5076P
This paper presents the first cosmological results based on Planck
measurements of the cosmic microwave background (CMB) temperature
and lensing-potential power spectra. We find that the Planck spectra
at high multipoles (ℓ ≳ 40) are extremely well described by
the standard spatially-flat six-parameter ΛCDM cosmology with a
power-law spectrum of adiabatic scalar perturbations. Within the
context of this cosmology, the Planck data determine the cosmological
parameters to high precision: the angular size of the sound horizon at
recombination, the physical densities of baryons and cold dark matter,
and the scalar spectral index are estimated to be θ<SUB>∗</SUB> =
(1.04147 ± 0.00062) × 10<SUP>-2</SUP>, Ω<SUB>b</SUB>h<SUP>2</SUP>
= 0.02205 ± 0.00028, Ω<SUB>c</SUB>h<SUP>2</SUP> = 0.1199 ± 0.0027,
and n<SUB>s</SUB> = 0.9603 ± 0.0073, respectively(note that in this
abstract we quote 68% errors on measured parameters and 95% upper
limits on other parameters). For this cosmology, we find a low value of
the Hubble constant, H<SUB>0</SUB> = (67.3 ± 1.2) km s<SUP>-1</SUP>
Mpc<SUP>-1</SUP>, and a high value of the matter density parameter,
Ω<SUB>m</SUB> = 0.315 ± 0.017. These values are in tension with recent
direct measurements of H<SUB>0</SUB> and the magnitude-redshift relation
for Type Ia supernovae, but are in excellent agreement with geometrical
constraints from baryon acoustic oscillation (BAO) surveys. Including
curvature, we find that the Universe is consistent with spatial
flatness to percent level precision using Planck CMB data alone. We
use high-resolution CMB data together with Planck to provide greater
control on extragalactic foreground components in an investigation of
extensions to the six-parameter ΛCDM model. We present selected results
from a large grid of cosmological models, using a range of additional
astrophysical data sets in addition to Planck and high-resolution CMB
data. None of these models are favoured over the standard six-parameter
ΛCDM cosmology. The deviation of the scalar spectral index from
unity isinsensitive to the addition of tensor modes and to changes
in the matter content of the Universe. We find an upper limit of
r<SUB>0.002</SUB>< 0.11 on the tensor-to-scalar ratio. There is no
evidence for additional neutrino-like relativistic particles beyond the
three families of neutrinos in the standard model. Using BAO and CMB
data, we find N<SUB>eff</SUB> = 3.30 ± 0.27 for the effective number
of relativistic degrees of freedom, and an upper limit of 0.23 eV for
the sum of neutrino masses. Our results are in excellent agreement with
big bang nucleosynthesis and the standard value of N<SUB>eff</SUB> =
3.046. We find no evidence for dynamical dark energy; using BAO and CMB
data, the dark energy equation of state parameter is constrained to be
w = -1.13<SUB>-0.10</SUB><SUP>+0.13</SUP>. We also use the Planck data
to set limits on a possible variation of the fine-structure constant,
dark matter annihilation and primordial magnetic fields. Despite the
success of the six-parameter ΛCDM model in describing the Planck data
at high multipoles, we note that this cosmology does not provide a
good fit to the temperature power spectrum at low multipoles. The
unusual shape of the spectrum in the multipole range 20 ≲ ℓ
≲ 40 was seen previously in the WMAP data and is a real feature
of the primordial CMB anisotropies. The poor fit to the spectrum at
low multipoles is not of decisive significance, but is an "anomaly"
in an otherwise self-consistent analysis of the Planck temperature data.
---------------------------------------------------------
Title: Planck 2013 results. XVII. Gravitational lensing by large-scale
structure
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Basak, S.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit-Lévy,
A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bock,
J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Bridges, M.; Bucher, M.; Burigana, C.; Butler, R. C.; Cardoso,
J. -F.; Catalano, A.; Challinor, A.; Chamballu, A.; Chiang, H. C.;
Chiang, L. -Y.; Christensen, P. R.; Church, S.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill,
B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis,
R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Déchelette, T.;
Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Dickinson, C.;
Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dunkley,
J.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli,
F.; Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson,
J. E.; Hansen, F. K.; Hanson, D.; Harrison, D.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon,
E.; Ho, S.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.;
Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela,
M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche,
J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lavabre, A.;
Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; León-Tavares, J.;
Lesgourgues, J.; Lewis, A.; Liguori, M.; Lilje, P. B.; Linden-Vørnle,
M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Mangilli, A.; Maris, M.; Marshall,
D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi,
M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss,
A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano,
L.; Pajot, F.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon,
G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Pullen, A. R.; Rachen, J. P.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.;
Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.;
Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.;
Smith, K.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor,
R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.;
Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.;
Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; White, M.;
White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..17P Altcode: 2013arXiv1303.5077P
On the arcminute angular scales probed by Planck, the cosmic
microwave background (CMB) anisotropies are gently perturbed by
gravitational lensing. Here we present a detailed study of this
effect, detecting lensing independently in the 100, 143, and 217
GHz frequency bands with an overall significance of greater than
25σ. We use thetemperature-gradient correlations induced by lensing
to reconstruct a (noisy) map of the CMB lensing potential, which
provides an integrated measure of the mass distribution back to the
CMB last-scattering surface. Our lensing potential map is significantly
correlated with other tracers of mass, a fact which we demonstrate using
several representative tracers of large-scale structure. We estimate
the power spectrum of the lensing potential, finding generally good
agreement with expectations from the best-fitting ΛCDM model for the
Planck temperature power spectrum, showing that this measurement at z =
1100 correctly predicts the properties of the lower-redshift, later-time
structures which source the lensing potential. When combined with the
temperature power spectrum, our measurement provides degeneracy-breaking
power for parameter constraints; it improves CMB-alone constraints
on curvature by a factor of two and also partly breaks the degeneracy
between the amplitude of the primordial perturbation power spectrum and
the optical depth to reionization, allowing a measurement of the optical
depth to reionization which is independent of large-scale polarization
data. Discarding scale information, our measurement corresponds to a 4%
constraint on the amplitude of the lensing potential power spectrum,
or a 2% constraint on the root-mean-squared amplitude of matter
fluctuations at z ~ 2.
---------------------------------------------------------
Title: Planck 2013 results. XX. Cosmology from Sunyaev-Zeldovich
cluster counts
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.;
Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Barrena,
R.; Bartlett, J. G.; Battaner, E.; Battye, R.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bikmaev, I.; Blanchard, A.; Bobin, J.; Bock, J. J.; Böhringer,
H.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bourdin,
H.; Bridges, M.; Brown, M. L.; Bucher, M.; Burenin, R.; Burigana, C.;
Butler, R. C.; Cardoso, J. -F.; Carvalho, P.; Catalano, A.; Challinor,
A.; Chamballu, A.; Chary, R. -R.; Chiang, L. -Y.; Chiang, H. C.; Chon,
G.; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.;
Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.;
Cuttaia, F.; Da Silva, A.; Dahle, H.; Danese, L.; Davies, R. D.; Davis,
R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille,
J.; Delouis, J. -M.; Démoclès, J.; Désert, F. -X.; Dickinson, C.;
Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis,
M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.;
Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi,
E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.;
Hanson, D.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.;
Jaffe, T. R.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen, E.;
Keskitalo, R.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.;
Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.;
Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leahy,
J. P.; Leonardi, R.; León-Tavares, J.; Lesgourgues, J.; Liddle, A.;
Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi,
N.; Marcos-Caballero, A.; Maris, M.; Marshall, D. J.; Martin, P. G.;
Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.;
Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Melin, J. -B.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss,
A.; Munshi, D.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; Osborne, S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.;
Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli,
E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prézeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.;
Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli,
I.; Rocha, G.; Roman, M.; Rosset, C.; Roudier, G.; Rowan-Robinson, M.;
Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini,
G.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.;
Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.; Sunyaev,
R.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.;
Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.; Umana, G.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Vielva, P.; Villa, F.;
Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Weller, J.; White, M.;
White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..20P Altcode: 2013arXiv1303.5080P
We present constraints on cosmological parameters using number counts
as a function of redshift for a sub-sample of 189 galaxy clusters
from the Planck SZ (PSZ) catalogue. The PSZ is selected through the
signature of the Sunyaev-Zeldovich (SZ) effect, and the sub-sample
used here has a signal-to-noise threshold of seven, with each object
confirmed as a cluster and all but one with a redshift estimate. We
discuss the completeness of the sample and our construction of a
likelihood analysis. Using a relation between mass M and SZ signal
Y calibrated to X-ray measurements, we derive constraints on the
power spectrum amplitude σ<SUB>8</SUB> and matter density parameter
Ω<SUB>m</SUB> in a flat ΛCDM model. We test the robustness of our
estimates and find that possible biases in the Y-M relation and the
halo mass function are larger than the statistical uncertainties from
the cluster sample. Assuming the X-ray determined mass to be biased
low relative to the true mass by between zero and 30%, motivated by
comparison of the observed mass scaling relations to those from a set
of numerical simulations, we find that σ<SUB>8</SUB> = 0.75 ± 0.03,
Ω<SUB>m</SUB> = 0.29 ± 0.02, and σ<SUB>8</SUB>(Ω<SUB>m</SUB>/
0.27)<SUP>0.3</SUP> = 0.764 ± 0.025. The value of σ<SUB>8</SUB>
is degenerate with the mass bias; if the latter is fixed to a
value of 20% (the central value from numerical simulations) we find
σ<SUB>8</SUB>(Ω<SUB>m</SUB>/0.27)<SUP>0.3</SUP> = 0.78 ± 0.01 and
a tighter one-dimensional range σ<SUB>8</SUB> = 0.77 ± 0.02. We find
that the larger values of σ<SUB>8</SUB> and Ω<SUB>m</SUB> preferred
by Planck’s measurements of the primary CMB anisotropies can be
accommodated by a mass bias of about 40%. Alternatively, consistency
with the primary CMB constraints can be achieved by inclusion of
processes that suppress power on small scales relative to the ΛCDM
model, such as a component of massive neutrinos. We place our results
in the context of other determinations of cosmologicalparameters,
and discuss issues that need to be resolved in order to make further
progress in this field.
---------------------------------------------------------
Title: Planck 2013 results. XI. All-sky model of thermal dust emission
Authors: Planck Collaboration; Abergel, A.; Ade, P. A. R.; Aghanim, N.;
Alves, M. I. R.; Aniano, G.; Armitage-Caplan, C.; Arnaud, M.; Ashdown,
M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.;
Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Boulanger, F.; Bridges, M.; Bucher, M.; Burigana, C.;
Butler, R. C.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.; Chary,
R. -R.; Chiang, H. C.; Chiang, L. -Y.; Christensen, P. R.; Church, S.;
Clemens, M.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet,
C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia,
F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de
Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert,
F. -X.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré,
O.; Douspis, M.; Draine, B. T.; Dupac, X.; Efstathiou, G.; Enßlin,
T. A.; Eriksen, H. K.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis,
M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Ghosh,
T.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo,
J.; Górski, K. M.; Gratton, S.; Gregorio, A.; Grenier, I. A.;
Gruppuso, A.; Guillet, V.; Hansen, F. K.; Hanson, D.; Harrison,
D. L.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.;
Jaffe, T. R.; Jewell, J.; Joncas, G.; Jones, W. C.; Juvela, M.;
Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Knoche, J.; Knox, L.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre,
J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leonardi,
R.; León-Tavares, J.; Lesgourgues, J.; Levrier, F.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris,
M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi,
S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee,
P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.; Paci,
F.; Pagano, L.; Pajot, F.; Paladini, R.; Paoletti, D.; Pasian, F.;
Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini,
F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.;
Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.;
Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.;
Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Roudier, G.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme,
B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.;
Shellard, E. P. S.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.;
Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.;
Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Valiviita,
J.; Van Tent, B.; Verstraete, L.; Vielva, P.; Villa, F.; Vittorio,
N.; Wade, L. A.; Wandelt, B. D.; Welikala, N.; Ysard, N.; Yvon, D.;
Zacchei, A.; Zonca, A.
2014A&A...571A..11P Altcode: 2013arXiv1312.1300P; 2013arXiv1312.1300A
This paper presents an all-sky model of dust emission from the Planck
353, 545, and 857 GHz, and IRAS 100 μm data. Using a modified blackbody
fit to the data we present all-sky maps of the dust optical depth,
temperature, and spectral index over the 353-3000 GHz range. This model
is a good representation of the IRAS and Planck data at 5' between
353 and 3000 GHz (850 and 100 μm). It shows variations of the order
of 30% compared with the widely-used model of Finkbeiner, Davis, and
Schlegel. The Planck data allow us to estimate the dust temperature
uniformly over the whole sky, down to an angular resolution of 5',
providing an improved estimate of the dust optical depth compared to
previous all-sky dust model, especially in high-contrast molecular
regions where the dust temperature varies strongly at small scales
in response to dust evolution, extinction, and/or local production
of heating photons. An increase of the dust opacity at 353 GHz,
τ<SUB>353</SUB>/N<SUB>H</SUB>, from the diffuse to the denser
interstellar medium (ISM) is reported. It is associated with a
decrease in the observed dust temperature, T<SUB>obs</SUB>, that
could be due at least in part to the increased dust opacity. We also
report an excess of dust emission at H i column densities lower than
10<SUP>20</SUP> cm<SUP>-2</SUP> that could be the signature of dust in
the warm ionized medium. In the diffuse ISM at high Galactic latitude,
we report an anticorrelation between τ<SUB>353</SUB>/N<SUB>H</SUB>
and T<SUB>obs</SUB> while the dust specific luminosity, i.e., the
total dust emission integrated over frequency (the radiance) per
hydrogen atom, stays about constant, confirming one of the Planck Early
Results obtained on selected fields. This effect is compatible with
the view that, in the diffuse ISM, T<SUB>obs</SUB> responds to spatial
variations of the dust opacity, due to variations of dust properties,
in addition to (small) variations of the radiation field strength. The
implication is that in the diffuse high-latitude ISM τ<SUB>353</SUB>
is not as reliable a tracer of dust column density as we conclude
it is in molecular clouds where the correlation of τ<SUB>353</SUB>
with dust extinction estimated using colour excess measurements on
stars is strong. To estimate Galactic E(B - V) in extragalactic fields
at high latitude we develop a new method based on the thermal dust
radiance, instead of the dust optical depth, calibrated to E(B - V)
using reddening measurements of quasars deduced from Sloan Digital
Sky Survey data.
---------------------------------------------------------
Title: Planck 2013 results. XXVIII. The Planck Catalogue of Compact
Sources
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Argüeso,
F.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela,
F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.;
Bartlett, J. G.; Battaner, E.; Beelen, A.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Bridges, M.; Bucher, M.; Burigana,
C.; Butler, R. C.; Cardoso, J. -F.; Carvalho, P.; Catalano, A.;
Challinor, A.; Chamballu, A.; Chen, X.; Chiang, H. C.; Chiang,
L. -Y.; Christensen, P. R.; Church, S.; Clemens, M.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill,
B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis,
R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.;
Delouis, J. -M.; Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dole,
H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.;
Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis, M.;
Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton,
S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison,
D. L.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.;
Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leahy, J. P.; Leonardi, R.; León-Tavares, J.; Leroy,
C.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese,
S.; Matthai, F.; Mazzotta, P.; McGehee, P.; Meinhold, P. R.;
Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.;
Natoli, P.; Negrello, M.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.;
Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne,
S.; Oxborrow, C. A.; Paci, F.; Pagano, L.; Pajot, F.; Paladini,
R.; Paoletti, D.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson,
T. J.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.;
Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri,
M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard,
E. P. S.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Stompor,
R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.;
Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.;
Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Walter,
B.; Wandelt, B. D.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...571A..28P Altcode: 2013arXiv1303.5088P
The Planck Catalogue of Compact Sources (PCCS) is the catalogue
of sources detected in the first 15 months of Planck operations,
the “nominal” mission. It consists of nine single-frequency
catalogues of compact sources, both Galactic and extragalactic,
detected over the entire sky. The PCCS covers the frequency range
30-857 GHz with higher sensitivity (it is 90% complete at 180 mJy in
the best channel) and better angular resolution (from 32.88' to 4.33')
than previous all-sky surveys in this frequency band. By construction
its reliability is >80% and more than 65% of the sources have been
detected in at least two contiguous Planck channels. In this paper we
present the construction and validation of the PCCS, its contents and
its statistical characterization.
---------------------------------------------------------
Title: Planck 2013 results. XXVII. Doppler boosting of the CMB:
Eppur si muove
Authors: Planck Collaboration; Aghanim, N.; Armitage-Caplan, C.;
Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Benabed, K.;
Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.;
Bobin, J.; Bock, J. J.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Bridges, M.; Burigana, C.; Butler, R. C.; Cardoso, J. -F.; Catalano,
A.; Challinor, A.; Chamballu, A.; Chiang, H. C.; Chiang, L. -Y.;
Christensen, P. R.; Clements, D. L.; Colombo, L. P. L.; Couchot,
F.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies,
R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.;
Delabrouille, J.; Diego, J. M.; Donzelli, S.; Doré, O.; Dupac, X.;
Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni,
O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard,
M.; Giardino, G.; González-Nuevo, J.; Górski, K. M.; Gratton, S.;
Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison,
D. L.; Helou, G.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hovest, W.; Huffenberger, K. M.; Jones, W. C.; Juvela, M.;
Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Knoche, J.; Knox, L.;
Kunz, M.; Kurki-Suonio, H.; Lähteenmäki, A.; Lamarre, J. -M.;
Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leonardi, R.; Lewis,
A.; Liguori, M.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego,
M.; Lubin, P. M.; Macías-Pérez, J. F.; Mandolesi, N.; Maris, M.;
Marshall, D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.;
Massardi, M.; Matarrese, S.; Mazzotta, P.; Meinhold, P. R.; Melchiorri,
A.; Mendes, L.; Migliaccio, M.; Mitra, S.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Naselsky, P.; Nati,
F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.;
Novikov, I.; Osborne, S.; Oxborrow, C. A.; Pagano, L.; Pajot, F.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perrotta,
F.; Piacentini, F.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Pratt, G. W.;
Prézeau, G.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Reinecke,
M.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Rubiño-Martín, J. A.; Rusholme, B.; Santos, D.; Savini, G.; Scott,
D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Sunyaev,
R.; Sureau, F.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Tucci, M.; Türler, M.; Valenziano, L.; Valiviita, J.; Van Tent,
B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
White, M.; Yvon, D.; Zacchei, A.; Zibin, J. P.; Zonca, A.
2014A&A...571A..27P Altcode: 2013arXiv1303.5087P
Our velocity relative to the rest frame of the cosmic microwave
background (CMB) generates a dipole temperature anisotropy on the
sky which has been well measured for more than 30 years, and has
an accepted amplitude of v/c = 1.23 × 10<SUP>-3</SUP>, or v =
369. In addition to this signal generated by Doppler boosting of
the CMB monopole, our motion also modulates and aberrates the CMB
temperature fluctuations (as well as every other source of radiation at
cosmological distances). This is an order 10<SUP>-3</SUP> effect applied
to fluctuations which are already one part in roughly 10<SUP>5</SUP>,
so it is quite small. Nevertheless, it becomes detectable with the
all-sky coverage, high angular resolution, and low noise levels of
the Planck satellite. Here we report a first measurement of this
velocity signature using the aberration and modulation effects on
the CMB temperature anisotropies, finding a component in the known
dipole direction, (l,b) = (264°,48°), of 384 km s<SUP>-1</SUP> ±
78 km s<SUP>-1</SUP> (stat.) ± 115 km s<SUP>-1</SUP> (syst.). This
is a significant confirmation of the expected velocity. <P />"And yet
it moves", the phrase popularly attributed to Galileo Galilei after
being forced to recant his view that the Earth goes around the Sun.
---------------------------------------------------------
Title: Planck 2013 results. I. Overview of products and scientific
results
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Alves, M. I. R.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.;
Atrio-Barandela, F.; Aumont, J.; Aussel, H.; Baccigalupi, C.; Banday,
A. J.; Barreiro, R. B.; Barrena, R.; Bartelmann, M.; Bartlett, J. G.;
Bartolo, N.; Basak, S.; Battaner, E.; Battye, R.; Benabed, K.; Benoît,
A.; Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bertincourt,
B.; Bethermin, M.; Bielewicz, P.; Bikmaev, I.; Blanchard, A.; Bobin,
J.; Bock, J. J.; Böhringer, H.; Bonaldi, A.; Bonavera, L.; Bond,
J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bourdin, H.;
Bowyer, J. W.; Bridges, M.; Brown, M. L.; Bucher, M.; Burenin, R.;
Burigana, C.; Butler, R. C.; Calabrese, E.; Cappellini, B.; Cardoso,
J. -F.; Carr, R.; Carvalho, P.; Casale, M.; Castex, G.; Catalano, A.;
Challinor, A.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, H. C.;
Chiang, L. -Y.; Chon, G.; Christensen, P. R.; Churazov, E.; Church, S.;
Clemens, M.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Combet,
C.; Comis, B.; Couchot, F.; Coulais, A.; Crill, B. P.; Cruz, M.; Curto,
A.; Cuttaia, F.; Da Silva, A.; Dahle, H.; Danese, L.; Davies, R. D.;
Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Déchelette,
T.; Delabrouille, J.; Delouis, J. -M.; Démoclès, J.; Désert,
F. -X.; Dick, J.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.;
Donzelli, S.; Doré, O.; Douspis, M.; Ducout, A.; Dunkley, J.; Dupac,
X.; Efstathiou, G.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.;
Fabre, O.; Falgarone, E.; Falvella, M. C.; Fantaye, Y.; Fergusson,
J.; Filliard, C.; Finelli, F.; Flores-Cacho, I.; Foley, S.; Forni, O.;
Fosalba, P.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Freschi, M.;
Fromenteau, S.; Frommert, M.; Gaier, T. C.; Galeotta, S.; Gallegos,
J.; Galli, S.; Gandolfo, B.; Ganga, K.; Gauthier, C.; Génova-Santos,
R. T.; Ghosh, T.; Giard, M.; Giardino, G.; Gilfanov, M.; Girard,
D.; Giraud-Héraud, Y.; Gjerløw, E.; González-Nuevo, J.; Górski,
K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Gudmundsson, J. E.;
Haissinski, J.; Hamann, J.; Hansen, F. K.; Hansen, M.; Hanson, D.;
Harrison, D. L.; Heavens, A.; Helou, G.; Hempel, A.; Henrot-Versillé,
S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon,
E.; Ho, S.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hou, Z.; Hovest,
W.; Huey, G.; Huffenberger, K. M.; Hurier, G.; Ilić, S.; Jaffe,
A. H.; Jaffe, T. R.; Jasche, J.; Jewell, J.; Jones, W. C.; Juvela, M.;
Kalberla, P.; Kangaslahti, P.; Keihänen, E.; Kerp, J.; Keskitalo,
R.; Khamitov, I.; Kiiveri, K.; Kim, J.; Kisner, T. S.; Kneissl,
R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lacasa, F.;
Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Langer, M.; Lasenby,
A.; Lattanzi, M.; Laureijs, R. J.; Lavabre, A.; Lawrence, C. R.; Le
Jeune, M.; Leach, S.; Leahy, J. P.; Leonardi, R.; León-Tavares, J.;
Leroy, C.; Lesgourgues, J.; Lewis, A.; Li, C.; Liddle, A.; Liguori,
M.; Lilje, P. B.; Linden-Vørnle, M.; Lindholm, V.; López-Caniego,
M.; Lowe, S.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish, C. J.;
Maffei, B.; Maggio, G.; Maino, D.; Mandolesi, N.; Mangilli, A.;
Marcos-Caballero, A.; Marinucci, D.; Maris, M.; Marleau, F.; Marshall,
D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Matsumura, T.; Matthai, F.; Maurin, L.; Mazzotta, P.;
McDonald, A.; McEwen, J. D.; McGehee, P.; Mei, S.; Meinhold, P. R.;
Melchiorri, A.; Melin, J. -B.; Mendes, L.; Menegoni, E.; Mennella,
A.; Migliaccio, M.; Mikkelsen, K.; Millea, M.; Miniscalco, R.; Mitra,
S.; Miville-Deschênes, M. -A.; Molinari, D.; Moneti, A.; Montier, L.;
Morgante, G.; Morisset, N.; Mortlock, D.; Moss, A.; Munshi, D.; Murphy,
J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Negrello, M.; Nesvadba,
N. P. H.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; North, C.;
Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Orieux, F.;
Osborne, S.; O'Sullivan, C.; Oxborrow, C. A.; Paci, F.; Pagano, L.;
Pajot, F.; Paladini, R.; Pandolfi, S.; Paoletti, D.; Partridge, B.;
Pasian, F.; Patanchon, G.; Paykari, P.; Pearson, D.; Pearson, T. J.;
Peel, M.; Peiris, H. V.; Perdereau, O.; Perotto, L.; Perrotta, F.;
Pettorino, V.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Platania, P.; Pogosyan, D.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Pullen, A. R.; Rachen, J. P.;
Racine, B.; Rahlin, A.; Räth, C.; Reach, W. T.; Rebolo, R.; Reinecke,
M.; Remazeilles, M.; Renault, C.; Renzi, A.; Riazuelo, A.; Ricciardi,
S.; Riller, T.; Ringeval, C.; Ristorcelli, I.; Robbers, G.; Rocha,
G.; Roman, M.; Rosset, C.; Rossetti, M.; Roudier, G.; Rowan-Robinson,
M.; Rubiño-Martín, J. A.; Ruiz-Granados, B.; Rusholme, B.; Salerno,
E.; Sandri, M.; Sanselme, L.; Santos, D.; Savelainen, M.; Savini, G.;
Schaefer, B. M.; Schiavon, F.; Scott, D.; Seiffert, M. D.; Serra, P.;
Shellard, E. P. S.; Smith, K.; Smoot, G. F.; Souradeep, T.; Spencer,
L. D.; Starck, J. -L.; Stolyarov, V.; Stompor, R.; Sudiwala, R.;
Sunyaev, R.; Sureau, F.; Sutter, P.; Sutton, D.; Suur-Uski, A. -S.;
Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Taylor, D.; Terenzi,
L.; Texier, D.; Toffolatti, L.; Tomasi, M.; Torre, J. -P.; Tristram,
M.; Tucci, M.; Tuovinen, J.; Türler, M.; Tuttlebee, M.; Umana, G.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Vibert, L.;
Viel, M.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt,
B. D.; Watson, C.; Watson, R.; Wehus, I. K.; Welikala, N.; Weller, J.;
White, M.; White, S. D. M.; Wilkinson, A.; Winkel, B.; Xia, J. -Q.;
Yvon, D.; Zacchei, A.; Zibin, J. P.; Zonca, A.
2014A&A...571A...1P Altcode: 2013arXiv1303.5062P
The European Space Agency's Planck satellite, dedicated to studying the
early Universe and its subsequent evolution, was launched 14 May 2009
and has been scanning the microwave and submillimetre sky continuously
since 12 August 2009. In March 2013, ESA and the Planck Collaboration
released the initial cosmology products based on the first 15.5 months
of Planck data, along with a set of scientific and technical papers
and a web-based explanatory supplement. This paper gives an overview
of the mission and its performance, the processing, analysis, and
characteristics of the data, the scientific results, and the science
data products and papers in the release. The science products include
maps of the cosmic microwave background (CMB) and diffuse extragalactic
foregrounds, a catalogue of compact Galactic and extragalactic
sources, and a list of sources detected through the Sunyaev-Zeldovich
effect. The likelihood code used to assess cosmological models against
the Planck data and a lensing likelihood are described. Scientific
results include robust support for the standard six-parameter ΛCDM
model of cosmology and improved measurements of its parameters,
including a highly significant deviation from scale invariance of
the primordial power spectrum. The Planck values for these parameters
and others derived from them are significantly different from those
previously determined. Several large-scale anomalies in the temperature
distribution of the CMB, first detected by WMAP, are confirmed with
higher confidence. Planck sets new limits on the number and mass of
neutrinos, and has measured gravitational lensing of CMB anisotropies at
greater than 25σ. Planck finds no evidence for non-Gaussianity in the
CMB. Planck's results agree well with results from the measurements of
baryon acoustic oscillations. Planck finds a lower Hubble constant than
found in some more local measures. Some tension is also present between
the amplitude of matter fluctuations (σ<SUB>8</SUB>) derived from CMB
data and that derived from Sunyaev-Zeldovich data. The Planck and WMAP
power spectra are offset from each other by an average level of about 2%
around the first acoustic peak. Analysis of Planck polarization data
is not yet mature, therefore polarization results are not released,
although the robust detection of E-mode polarization around CMB hot
and cold spots is shown graphically.
---------------------------------------------------------
Title: LoCuSS: hydrostatic mass measurements of the high-L<SUB>X</SUB>
cluster sample - cross-calibration of Chandra and XMM-Newton
Authors: Martino, Rossella; Mazzotta, Pasquale; Bourdin, Hervé;
Smith, Graham P.; Bartalucci, Iacopo; Marrone, Daniel P.; Finoguenov,
Alexis; Okabe, Nobuhiro
2014MNRAS.443.2342M Altcode: 2014arXiv1406.6831M
We present a consistent analysis of Chandra and XMM-Newton observations
of an approximately mass-selected sample of 50 galaxy clusters at 0.15
< z < 0.3 - the `LoCuSS high-L<SUB>X</SUB> sample'. We apply
the same analysis methods to data from both satellites, including
newly developed analytic background models that predict the spatial
variation of the Chandra and XMM-Newton backgrounds to <2 and <5
per cent precision, respectively. To verify the cross-calibration of
Chandra- and XMM-Newton-based cluster mass measurements, we derive
the mass profiles of the 21 clusters that have been observed with both
satellites, extracting surface brightness and temperature profiles from
identical regions of the respective data sets. We obtain consistent
results for the gas and total hydrostatic cluster masses: the average
ratio of Chandra- to XMM-Newton-based measurements of M<SUB>gas</SUB>
and M<SUB>X</SUB> at r<SUB>500</SUB> are 0.99 ± 0.02 and 1.02 ± 0.05,
respectively, with an intrinsic scatter of ∼3 per cent for gas masses
and ∼8 per cent for hydrostatic masses. Comparison of our hydrostatic
mass measurements at r<SUB>500</SUB> with the latest Local Cluster
Substructure Survey (LoCuSS) weak-lensing results indicate that the
data are consistent with non-thermal pressure support at this radius
of ∼7 per cent. We also investigate the scaling relation between our
hydrostatic cluster masses and published integrated Compton parameter
Y<SUB>sph</SUB> measurements from the Sunyaev-Zel'dovich Array. We
measure a scatter in mass at fixed Y<SUB>sph</SUB> of ∼16 per cent at
Δ = 500, which is consistent with theoretical predictions of ∼10-15
per cent scatter.
---------------------------------------------------------
Title: Temperature Structure of the Intracluster Medium from
Smoothed-particle Hydrodynamics and Adaptive-mesh Refinement
Simulations
Authors: Rasia, Elena; Lau, Erwin T.; Borgani, Stefano; Nagai, Daisuke;
Dolag, Klaus; Avestruz, Camille; Granato, Gian Luigi; Mazzotta,
Pasquale; Murante, Giuseppe; Nelson, Kaylea; Ragone-Figueroa, Cinthia
2014ApJ...791...96R Altcode: 2014arXiv1406.4410R
Analyses of cosmological hydrodynamic simulations of galaxy clusters
suggest that X-ray masses can be underestimated by 10%-30%. The largest
bias originates from both violation of hydrostatic equilibrium (HE)
and an additional temperature bias caused by inhomogeneities in the
X-ray-emitting intracluster medium (ICM). To elucidate this large
dispersion among theoretical predictions, we evaluate the degree
of temperature structures in cluster sets simulated either with
smoothed-particle hydrodynamics (SPH) or adaptive-mesh refinement (AMR)
codes. We find that the SPH simulations produce larger temperature
variations connected to the persistence of both substructures
and their stripped cold gas. This difference is more evident in
nonradiative simulations, whereas it is reduced in the presence of
radiative cooling. We also find that the temperature variation in
radiative cluster simulations is generally in agreement with that
observed in the central regions of clusters. Around R <SUB>500</SUB>
the temperature inhomogeneities of the SPH simulations can generate
twice the typical HE mass bias of the AMR sample. We emphasize that
a detailed understanding of the physical processes responsible for
the complex thermal structure in ICM requires improved resolution and
high-sensitivity observations in order to extend the analysis to higher
temperature systems and larger cluster-centric radii.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Anomalous microwave emission in
Galactic clouds (Planck+, 2014)
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alves,
M. I. R.; Arnaud, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.;
Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoit-Levy,
A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bonaldi,
A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Burigana,
C.; Cardoso, J. -F.; Casassus, S.; Catalano, A.; Chamballu, A.; Chen,
X.; Chiang, H. C.; Chiang, L. -Y.; Christensen, P. R.; Clements,
D. L.; Colombi, S.; Colombo, L. P. L.; Couchot, F.; Crill, B. P.;
Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis,
P.; De Rosa, A.; de Zotti, G.; Delabrouille, J.; Desert, F. -X.;
Dickinson, C.; Diego, J. M.; Donzelli, S.; Dore, O.; Dupac, X.;
Ensslin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Franceschi,
E.; Galeotta, S.; Ganga, K.; Genova-Santos, R. T.; Ghosh, T.; Giard,
M.; Gonzalez-Nuevo, J.; Gorski, K. M.; Gregorio, A.; Gruppuso, A.;
Hansen, F. K.; Harrison, D. L.; Helou, G.; Hernandez-Monteagudo, C.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Hornstrup, A.; Jaffe,
A. H.; Jaffe, T. R.; Jones, W. C.; Keihaenen, E.; Keskitalo, R.;
Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Laehteenmaeki,
A.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.; Leonardi, R.;
Liguori, M.; Lilje, P. B.; Linden-Vornle, M.; Lopez-Caniego, M.;
Macias-Perez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Marshall,
D. J.; Martin, P. G.; Martinez-Gonzalez, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Migliaccio, M.; Miville-Deschenes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Naselsky, P.;
Nati, F.; Natoli, P.; Norgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini,
R.; Paoletti, D.; Patanchon, G.; Pearson, T. J.; Peel, M.; Perdereau,
O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.;
Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.;
Rebolo, R.; Reich, W.; Reinecke, M.; Remazeilles, M.; Renault, C.;
Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Roudier, G.; Rubino-Martin, J. A.; Rusholme, B.; Sandri, M.; Savini,
G.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.;
Tibbs, C. T.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Verstraete,
L.; Vielva, P.; Villa, F.; Wandelt, B. D.; Watson, R.; Wilkinson,
A.; Ysard, N.; Yvon, D.; Zacchei, A.; Zonca, A.
2014yCat..35650103P Altcode: 2014yCat..35659103P
Anomalous microwave emission (AME) is believed to be due to electric
dipole radiation from small spinning dust grains. The aim of this
paper is a statistical study of the basic properties of AME regions
and the environment in which they emit. We used WMAP and Planck maps,
combined with ancillary radio and IR data, to construct a sample of 98
candidate AME sources, assembling SEDs for each source using aperture
photometry on 1°-smoothed maps from 0.408GHz up to 3000GHz. <P />Each
spectrum is fitted with a simple model of free-free, synchrotron
(where necessary), cosmic microwave background (CMB), thermal dust,
and spinning dust components. We find that 42 of the 98 sources have
significant (>5σ) excess emission at frequencies between 20 and
60GHz. An analysis of the potential contribution of optically thick
free-free emission from ultra-compact HII regions, using IR colour
criteria, reduces the significant AME sample to 27 regions. The spectrum
of the AME is consistent with model spectra of spinning dust. Peak
frequencies are in the range 20-35GHz except for the California nebula
(NGC1499), which appears to have a high spinning dust peak frequency of
(50+/-17)GHz. The AME regions tend to be more spatially extended than
regions with little or no AME. The AME intensity is strongly correlated
with the sub-millimetre/IR flux densities and comparable to previous AME
detections in the literature. AME emissivity, defined as the ratio of
AME to dust optical depth, varies by an order of magnitude for the AME
regions. The AME regions tend to be associated with cooler dust in the
range 14-20K and an average emissivity index, β<SUB>d</SUB>, of +1.8,
while the non-AME regions are typically warmer, at 20-27K. In agreement
with previous studies, the AME emissivity appears to decrease with
increasing column density. This supports the idea of AME originating
from small grains that are known to be depleted in dense regions,
probably due to coagulation onto larger grains. We also find a
correlation between the AME emissivity (and to a lesser degree the
spinning dust peak frequency) and the intensity of the interstellar
radiation field, G<SUB>0</SUB>. Modelling of this trend suggests
that both radiative and collisional excitation are important for the
spinning dust emission. The most significant AME regions tend to have
relatively less ionized gas (free-free emission), although this could
be a selection effect. The infrared excess, a measure of the heating of
dust associated with HII regions, is typically >4 for AME sources,
indicating that the dust is not primarily heated by hot OB stars. The
AME regions are associated with known dark nebulae and have higher
12μm/25μm ratios. The emerging picture is that the bulk of the AME is
coming from the polycyclic aromatic hydrocarbons and small dust grains
from the colder neutral interstellar medium phase. <P />(1 data file).
---------------------------------------------------------
Title: Planck intermediate results. XVI. Profile likelihoods for
cosmological parameters
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro,
R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bonaldi, A.;
Bond, J. R.; Bouchet, F. R.; Burigana, C.; Cardoso, J. -F.; Catalano,
A.; Chamballu, A.; Chiang, H. C.; Christensen, P. R.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Couchot, F.; Cuttaia, F.; Danese, L.;
Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli,
S.; Doré, O.; Douspis, M.; Dupac, X.; Enßlin, T. A.; Eriksen, H. K.;
Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.;
Galli, S.; Ganga, K.; Giard, M.; Giraud-Héraud, Y.; González-Nuevo,
J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.;
Harrison, D. L.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe, A. H.;
Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo,
R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.;
Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.;
Lasenby, A.; Lawrence, C. R.; Leonardi, R.; Liddle, A.; Liguori, M.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris,
M.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.;
Migliaccio, M.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.;
Montier, L.; Morgante, G.; Munshi, D.; Murphy, J. A.; Naselsky, P.;
Nati, F.; Natoli, P.; Noviello, F.; Novikov, D.; Novikov, I.; Oxborrow,
C. A.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Pettorino, V.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski∗, S.; Pointecouteau,
E.; Polenta, G.; Popa, L.; Pratt, G. W.; Puget, J. -L.; Rachen, J. P.;
Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Roudier, G.;
Rouillé d'Orfeuil, B.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri,
M.; Savelainen, M.; Savini, G.; Spencer, L. D.; Spinelli, M.; Starck,
J. -L.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.;
Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Tucci, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent,
B.; Vielva, P.; Villa, F.; Wade, L. A.; Wandelt, B. D.; White, M.;
Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...566A..54P Altcode: 2013arXiv1311.1657P
We explore the 2013 Planck likelihood function with a high-precision
multi-dimensional minimizer (Minuit). This allows a refinement of
the ΛCDM best-fit solution with respect to previously-released
results, and the construction of frequentist confidence intervals
using profile likelihoods. The agreement with the cosmological
results from the Bayesian framework is excellent, demonstrating the
robustness of the Planck results to the statistical methodology. We
investigate the inclusion of neutrino masses, where more significant
differences may appear due to the non-Gaussian nature of the posterior
mass distribution. By applying the Feldman-Cousins prescription,
we again obtain results very similar to those of the Bayesian
methodology. However, the profile-likelihood analysis of the cosmic
microwave background (CMB) combination (Planck+WP+highL) reveals a
minimum well within the unphysical negative-mass region. We show that
inclusion of the Planck CMB-lensing information regularizes this issue,
and provide a robust frequentist upper limit ∑ m<SUB>ν</SUB> ≤
0.26 eV (95% confidence) from the CMB+lensing+BAO data combination.
---------------------------------------------------------
Title: Chandra ACIS-I particle background: an analytical model
Authors: Bartalucci, I.; Mazzotta, P.; Bourdin, H.; Vikhlinin, A.
2014A&A...566A..25B Altcode: 2014arXiv1404.3587B
<BR /> Aims: Imaging and spectroscopy of X-ray extended sources
require a proper characterisation of a spatially unresolved background
signal. This background includes sky and instrumental components,
each of which are characterised by its proper spatial and spectral
behaviour. While the X-ray sky background has been extensively studied
in previous work, here we analyse and model the instrumental background
of the ACIS-I detector on board the Chandra X-ray observatory in very
faint mode. <BR /> Methods: Caused by interaction of highly energetic
particles with the detector, the ACIS-I instrumental background
is spectrally characterised by the superimposition of several
fluorescence emission lines onto a continuum. To isolate its flux from
any sky component, we fitted an analytical model of the continuum to
observations performed in very faint mode with the detector in the
stowed position shielded from the sky, and gathered over the eight-year
period starting in 2001. The remaining emission lines were fitted
to blank-sky observations of the same period. We found 11 emission
lines. Analysing the spatial variation of the amplitude, energy and
width of these lines has further allowed us to infer that three lines
of these are presumably due to an energy correction artefact produced
in the frame store. <BR /> Results: We provide an analytical model
that predicts the instrumental background with a precision of 2% in
the continuum and 5% in the lines. We use this model to measure the
flux of the unresolved cosmic X-ray background in the Chandra deep
field south. We obtain a flux of 10.2<SUP>+0.5</SUP><SUB>-0.4</SUB> ×
10<SUP>-13</SUP> erg cm<SUP>-2</SUP> deg<SUP>-2</SUP> s<SUP>-1</SUP>
for the [1-2] keV band and (3.8 ± 0.2) × 10<SUP>-12</SUP> erg
cm<SUP>-2</SUP> deg<SUP>-2</SUP> s<SUP>-1</SUP> for the [2-8] keV band.
---------------------------------------------------------
Title: Planck intermediate results. XVII. Emission of dust in the
diffuse interstellar medium from the far-infrared to microwave
frequencies
Authors: Planck Collaboration; Abergel, A.; Ade, P. A. R.; Aghanim,
N.; Alves, M. I. R.; Aniano, G.; Arnaud, M.; Ashdown, M.; Aumont,
J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J. -P.;
Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bonaldi, A.; Bond, J. R.;
Bouchet, F. R.; Boulanger, F.; Burigana, C.; Cardoso, J. -F.; Catalano,
A.; Chamballu, A.; Chiang, H. C.; Christensen, P. R.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Couchot, F.; Crill, B. P.; Cuttaia, F.;
Danese, L.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.;
Delabrouille, J.; Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dole,
H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.; Efstathiou, G.;
Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Finelli, F.; Forni,
O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Ghosh, T.;
Giard, M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.;
Gregorio, A.; Gruppuso, A.; Guillet, V.; Hansen, F. K.; Harrison,
D.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Jaffe,
A. H.; Jaffe, T. R.; Joncas, G.; Jones, A.; Jones, W. C.; Juvela,
M.; Kalberla, P.; Keihänen, E.; Kerp, J.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.;
Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.; Linden-Vørnle,
M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio,
M.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.;
Nati, F.; Natoli, P.; Noviello, F.; Novikov, D.; Novikov, I.; Oxborrow,
C. A.; Pagano, L.; Pajot, F.; Paoletti, D.; Pasian, F.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli,
E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta,
G.; Ponthieu, N.; Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.;
Rosset, C.; Roudier, G.; Rusholme, B.; Sandri, M.; Savini, G.; Spencer,
L. D.; Starck, J. -L.; Sureau, F.; Sutton, D.; Suur-Uski, A. -S.;
Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Tristram, M.; Tucci, M.; Umana, G.; Valenziano, L.; Valiviita,
J.; Van Tent, B.; Verstraete, L.; Vielva, P.; Villa, F.; Wade, L. A.;
Wandelt, B. D.; Winkel, B.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...566A..55P Altcode: 2013arXiv1312.5446P
The dust-Hi correlation is used to characterize the emission properties
of dust in the diffuse interstellar medium (ISM) from far infrared
wavelengths to microwave frequencies. The field of this investigation
encompasses the part of the southern sky best suited to study the
cosmic infrared and microwave backgrounds. We cross-correlate sky maps
from Planck, the Wilkinson Microwave Anisotropy Probe (WMAP), and the
diffuse infrared background experiment (DIRBE), at 17 frequencies from
23 to 3000 GHz, with the Parkes survey of the 21 cm line emission of
neutral atomic hydrogen, over a contiguous area of 7500 deg<SUP>2</SUP>
centred on the southern Galactic pole. We present a general methodology
to study the dust-Hi correlation over the sky, including simulations
to quantify uncertainties. Our analysis yields four specific
results. (1) We map the temperature, submillimetre emissivity, and
opacity of the dust per H-atom. The dust temperature is observed to
be anti-correlated with the dust emissivity and opacity. We interpret
this result as evidence of dust evolution within the diffuse ISM. The
mean dust opacity is measured to be (7.1 ± 0.6) × 10<SUP>-27</SUP>
cm<SUP>2</SUP> H<SUP>-1</SUP> × (ν/ 353 GHz)<SUP>1.53 ± 0.03</SUP>
for 100 ≤ ν ≤ 353 GHz. This is a reference value to estimate
hydrogen column densities from dust emission at submillimetre and
millimetre wavelengths. (2) We map the spectral index β<SUB>mm</SUB>
of dust emission at millimetre wavelengths (defined here as ν ≤
353 GHz), and find it to be remarkably constant at β<SUB>mm</SUB>
= 1.51 ± 0.13. We compare it with the far infrared spectral index
β<SUB>FIR</SUB> derived from greybody fits at higher frequencies,
and find a systematic difference, β<SUB>mm</SUB> - β<SUB>FIR</SUB>
= - 0.15, which suggests that the dust spectral energy distribution
(SED) flattens at ν ≤ 353 GHz. (3) We present spectral fits of
the microwave emission correlated with Hi from 23 to 353 GHz, which
separate dust and anomalous microwave emission (AME). We show that the
flattening of the dust SED can be accounted for with an additional
component with a blackbody spectrum. This additional component,
which accounts for (26 ± 6)% of the dust emission at 100 GHz, could
represent magnetic dipole emission. Alternatively, it could account
for an increasing contribution of carbon dust, or a flattening of the
emissivity of amorphous silicates, at millimetre wavelengths. These
interpretations make different predictions for the dust polarization
SED. (4) We analyse the residuals of the dust-Hi correlation. We
identify a Galactic contribution to these residuals, which we model
with variations of the dust emissivity on angular scales smaller than
that of our correlation analysis. This model of the residuals is used
to quantify uncertainties of the CIB power spectrum in a companion
Planck paper. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org/10.1051/0004-6361/201323270/olm">http://www.aanda.org</A>
---------------------------------------------------------
Title: Discovery of large-scale diffuse radio emission and of a new
galaxy cluster in the surroundings of MACS J0520.7-1328
Authors: Macario, G.; Intema, H. T.; Ferrari, C.; Bourdin,
H.; Giacintucci, S.; Venturi, T.; Mazzotta, P.; Bartalucci, I.;
Johnston-Hollitt, M.; Cassano, R.; Dallacasa, D.; Pratt, G. W.; Kale,
R.; Brown, S.
2014A&A...565A..13M Altcode: 2014arXiv1402.4436M
We report the discovery of large-scale diffuse radio emission south-east
of the galaxy cluster <ASTROBJ>MACS J0520.7-1328</ASTROBJ>, detected
through high-sensitivity Giant Metrewave Radio Telescope 323 MHz
observations. This emission is dominated by an elongated diffuse
radio source and surrounded by other features of lower surface
brightness. Patches of these faint sources are marginally detected
in a 1.4 GHz image obtained through a re-analysis of archival
NVSS data. Interestingly, the elongated radio source coincides
with a previously unclassified extended X-ray source. We perform a
multi-wavelength analysis based on archival infrared, optical, and X-ray
Chandra data. We find that this source is a low-temperature (~3.6 keV)
cluster of galaxies, with indications of a disturbed dynamical state,
located at a redshift that is consistent with the one of the main
galaxy cluster <ASTROBJ>MACS J0520.7-132</ASTROBJ> (z = 0.336). We
suggest that the diffuse radio emission is associated to non-thermal
components in the intracluster and intergalactic medium in and around
the newly detected cluster. We are planning deeper multi-wavelength
and multi-frequency radio observations to accurately investigate the
dynamical scenario of the two clusters and to address the nature of
the complex radio emission more precisely.
---------------------------------------------------------
Title: Planck intermediate results. XV. A study of anomalous microwave
emission in Galactic clouds
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alves,
M. I. R.; Arnaud, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.;
Benoit-Lévy, A.; Bernard, J. -P.; Bersanelli, M.; Bielewicz,
P.; Bobin, J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Boulanger, F.; Burigana, C.; Cardoso, J. -F.; Casassus,
S.; Catalano, A.; Chamballu, A.; Chen, X.; Chiang, H. C.; Chiang,
L. -Y.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Colombo,
L. P. L.; Couchot, F.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies,
R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.;
Delabrouille, J.; Désert, F. -X.; Dickinson; , C.; Diego, J. M.;
Donzelli, S.; Doré, O.; Dupac, X.; Enßlin, T. A.; Eriksen, H. K.;
Finelli, F.; Forni, O.; Franceschi, E.; Galeotta, S.; Ganga, K.;
Génova-Santos, R. T.; Ghosh, T.; Giard, M.; González-Nuevo, J.;
Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison,
D. L.; Helou, G.; Hernández-Monteagudo, C.; Hildebrandt, S. R.;
Hivon, E.; Hobson, M.; Hornstrup, A.; Jaffe, A. H.; Jaffe, T. R.;
Jones, W. C.; Keihänen, E.; Keskitalo, R.; Kneissl, R.; Knoche,
J.; Kunz, M.; Kurki-Suonio, H.; Lähteenmäki, A.; Lamarre, J. -M.;
Lasenby, A.; Lawrence, C. R.; Leonardi, R.; Liguori, M.; Lilje,
P. B.; Linden-Vørnle, M.; López-Caniego, M.; Macías-Pérez, J. F.;
Maffei, B.; Maino, D.; Mandolesi, N.; Marshall, D. J.; Martin, P. G.;
Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella,
A.; Migliaccio, M.; Miville-Deschênes, M. -A.; Moneti, A.; Montier,
L.; Morgante, G.; Mortlock, D.; Munshi, D.; Naselsky, P.; Nati, F.;
Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.;
Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Patanchon, G.; Pearson, T. J.; Peel, M.; Perdereau,
O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.;
Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.;
Rebolo, R.; Reich, W.; Reinecke, M.; Remazeilles, M.; Renault, C.;
Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Roudier, G.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini,
G.; Scott, D.; Spencer, L. D.; Stolyarov, V.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.;
Tibbs, C. T.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.;
Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Verstraete,
L.; Vielva, P.; Villa, F.; Wandelt, B. D.; Watson, R.; Wilkinson,
A.; Ysard, N.; Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...565A.103P Altcode: 2013arXiv1309.1357P
Anomalous microwave emission (AME) is believed to be due to electric
dipole radiation from small spinning dust grains. The aim of this paper
is a statistical study of the basic properties of AME regions and the
environment in which they emit. We used WMAP and Planck maps, combined
with ancillary radio and IR data, to construct a sample of 98 candidate
AME sources, assembling SEDs for each source using aperture photometry
on 1°-smoothed maps from 0.408 GHz up to 3000 GHz. Each spectrum is
fitted with a simple model of free-free, synchrotron (where necessary),
cosmic microwave background (CMB), thermal dust, and spinning dust
components. We find that 42 of the 98 sources have significant
(>5σ) excess emission at frequencies between 20 and 60 GHz. An
analysis of the potential contribution of optically thick free-free
emission from ultra-compact H ii regions, using IR colour criteria,
reduces the significant AME sample to 27 regions. The spectrum of the
AME is consistent with model spectra of spinning dust. Peak frequencies
are in the range 20-35 GHz except for the California nebula (NGC 1499),
which appears to have a high spinning dust peak frequency of (50 ± 17)
GHz. The AME regions tend to be more spatially extended than regions
with little or no AME. The AME intensity is strongly correlated with
the sub-millimetre/IR flux densities and comparable to previous AME
detections in the literature. AME emissivity, defined as the ratio of
AME to dust optical depth, varies by an order of magnitude for the
AME regions. The AME regions tend to be associated with cooler dust
in the range 14-20 K and an average emissivity index, β<SUB>d</SUB>,
of +1.8, while the non-AME regions are typically warmer, at 20-27
K. In agreement with previous studies, the AME emissivity appears to
decrease with increasing column density. This supports the idea of AME
originating from small grains that are known to be depleted in dense
regions, probably due to coagulation onto larger grains. We also find
a correlation between the AME emissivity (and to a lesser degree the
spinning dust peak frequency) and the intensity of the interstellar
radiation field, G<SUB>0</SUB>. Modelling of this trend suggests
that both radiative and collisional excitation are important for the
spinning dust emission. The most significant AME regions tend to have
relatively less ionized gas (free-free emission), although this could
be a selection effect. The infrared excess, a measure of the heating of
dust associated with H ii regions, is typically >4 for AME sources,
indicating that the dust is not primarily heated by hot OB stars. The
AME regions are associated with known dark nebulae and have higher 12
μm/25 μm ratios. The emerging picture is that the bulk of the AME
is coming from the polycyclic aromatic hydrocarbons and small dust
grains from the colder neutral interstellar medium phase.
---------------------------------------------------------
Title: Planck intermediate results. XIV. Dust emission at millimetre
wavelengths in the Galactic plane
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alves,
M. I. R.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont,
J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Bartlett,
J. G.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.; Bernard, J. -P.;
Bersanelli, M.; Bielewicz, P.; Bobin, J.; Bonaldi, A.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bucher, M.; Burigana,
C.; Butler, R. C.; Cardoso, J. -F.; Catalano, A.; Chamballu, A.;
Chiang, H. C.; Chiang, L. -Y.; Christensen, P. R.; Clements, D. L.;
Colombi, S.; Colombo, L. P. L.; Couchot, F.; Crill, B. P.; Curto, A.;
Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis,
P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Dickinson, C.;
Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac,
X.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Finelli, F.;
Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.;
Ghosh, T.; Giard, M.; Giardino, G.; González-Nuevo, J.; Górski,
K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D. L.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon,
E.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Jaffe, A. H.; Jones,
W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.;
Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leonardi, R.; Levrier, F.; Liguori, M.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall, D. J.; Martin,
P. G.; Martínez-González, E.; Masi, S.; Matarrese, S.; Mazzotta,
P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Migliaccio, M.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati,
F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.;
Novikov, I.; Oxborrow, C. A.; Pagano, L.; Pajot, F.; Paladini, R.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Peel, M.; Perdereau, O.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon,
D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.;
Popa, L.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.;
Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault,
C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset,
C.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.;
Scott, D.; Spencer, L. D.; Starck, J. -L.; Stolyarov, V.; Sureau,
F.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.;
Tucci, M.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Verstraete,
L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
Yvon, D.; Zacchei, A.; Zonca, A.
2014A&A...564A..45P Altcode: 2013arXiv1307.6815P
We use Planck HFI data combined with ancillary radio data to study the
emissivity index of the interstellar dust emission in the frequency
range 100-353 GHz, or 3-0.8 mm, in the Galactic plane. We analyse the
region l = 20°-44° and |b| ≤ 4° where the free-free emission can
be estimated from radio recombination line data. We fit the spectra
at each sky pixel with a modified blackbody model and two opacity
spectral indices, β<SUB>mm</SUB> and β<SUB>FIR</SUB>, below and
above 353 GHz, respectively. We find that β<SUB>mm</SUB> is smaller
than β<SUB>FIR</SUB>, and we detect a correlation between this
low frequency power-law index and the dust optical depth at 353 GHz,
τ<SUB>353</SUB>. The opacity spectral index β<SUB>mm</SUB> increases
from about 1.54 in the more diffuse regions of the Galactic disk, |b|
= 3°-4° and τ<SUB>353</SUB> ~ 5 × 10<SUP>-5</SUP>, to about 1.66
in the densest regions with an optical depth of more than one order of
magnitude higher. We associate this correlation with an evolution of
the dust emissivity related to the fraction of molecular gas along the
line of sight. This translates into β<SUB>mm</SUB> ~ 1.54 for a medium
that is mostly atomic and β<SUB>mm</SUB> ~ 1.66 when the medium is
dominated by molecular gas. We find that both the two-level system model
and magnetic dipole emission by ferromagnetic particles can explain
the results. These results improve our understanding of the physics
of interstellar dust and lead towards a complete model of the dust
spectrum of the Milky Way from far-infrared to millimetre wavelengths.
---------------------------------------------------------
Title: New Detections of Radio Minihalos in Cool Cores of Galaxy
Clusters
Authors: Giacintucci, Simona; Markevitch, Maxim; Venturi, Tiziana;
Clarke, Tracy E.; Cassano, Rossella; Mazzotta, Pasquale
2014ApJ...781....9G Altcode: 2013arXiv1311.5248G
Cool cores of some galaxy clusters exhibit faint radio
"minihalos." Their origin is unclear, and their study has been limited
by their small number. We undertook a systematic search for minihalos
in a large sample of X-ray luminous clusters with high-quality radio
data. In this article, we report four new minihalos (A 478, ZwCl 3146,
RXJ 1532.9+3021, and A 2204) and five candidates found in the reanalyzed
archival Very Large Array observations. The radio luminosities of
our minihalos and candidates are in the range of 10<SUP>23-25</SUP>
W Hz<SUP>-1</SUP> at 1.4 GHz, which is consistent with these types of
radio sources. Their sizes (40-160 kpc in radius) are somewhat smaller
than those of previously known minihalos. We combine our new detections
with previously known minihalos, obtaining a total sample of 21 objects,
and briefly compare the cluster radio properties to the average X-ray
temperature and the total masses estimated from Planck. We find that
nearly all clusters hosting minihalos are hot and massive. Beyond that,
there is no clear correlation between the minihalo radio power and
cluster temperature or mass (in contrast with the giant radio halos
found in cluster mergers, whose radio luminosity correlates with the
cluster mass). Chandra X-ray images indicate gas sloshing in the cool
cores of most of our clusters, with minihalos contained within the
sloshing regions in many of them. This supports the hypothesis that
radio-emitting electrons are reaccelerated by sloshing. Advection of
relativistic electrons by the sloshing gas may also play a role in
the formation of the less extended minihalos.
---------------------------------------------------------
Title: Recent Results from the Local Cluster Substructure Survey
Authors: Smith, G.; Okabe, N.; Scott, K.; Mulroy, S.; May, P.; Martino,
R.; Babul, A.; Egami, E.; Finoguenov, A.; Haines, C.; Marrone,
D.; Mazzotta, P.; Richard, J.; Takada, M.; Umetsu, K.; Ziparo, F.;
McCarthy, I.; Le Brun, A.; Bahé, Y.
2014egcc.confE...7S Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Planck intermediate results. XIII. Constraints on peculiar
velocities
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday,
A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoit-Lévy, A.;
Bernard, J. -P.; Bersanelli, M.; Bielewicz, P.; Bikmaev, I.; Bobin,
J.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Burigana, C.; Butler, R. C.; Cabella, P.; Cardoso, J. -F.;
Catalano, A.; Chamballu, A.; Chiang, L. -Y.; Chon, G.; Christensen,
P. R.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Crill, B. P.;
Cuttaia, F.; Da Silva, A.; Dahle, H.; Davies, R. D.; Davis, R. J.;
de Bernardis, P.; de Gasperis, G.; de Zotti, G.; Delabrouille,
J.; Démoclès, J.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli,
S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Enßlin, T. A.;
Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Frommert, M.;
Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; Giardino,
G.; Gonzáalez-Nuevo, J.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.;
Harrison, D.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt,
S. R.; Hivon, E.; Holmes, W. A.; Hovest, W.; Huffenberger, K. M.;
Hurier, G.; Jaffe, T. R.; Jaffe, A. H.; Jasche, J.; Jones, W. C.;
Juvela, M.; Keihánen, E.; Keskitalo, R.; Khamitov, I.; Kisner, T. S.;
Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.;
Leonardi, R.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Macías-Pérez, J. F.; Maino, D.; Mak, D. S. Y.; Mandolesi, N.; Maris,
M.; Marleau, F.; Martínez-González, E.; Masi, S.; Matarrese, S.;
Mazzotta, P.; Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella,
A.; Migliaccio, M.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.;
Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.;
Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.;
Osborne, S.; Pagano, L.; Paoletti, D.; Perdereau, O.; Perrotta, F.;
Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski,
S.; Pointecouteau, E.; Polenta, G.; Popa, L.; Poutanen, T.; Pratt,
G. W.; Prunet, S.; Puget, J. -L.; Puisieux, S.; Rachen, J. P.; Rebolo,
R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Roman,
M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.;
Scott, D.; Spencer, L.; Sunyaev, R.; Sutton, D.; Suur-Uski, A. -S.;
Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Tristram, M.; Tucci, M.; Valenziano, L.; Valiviita, J.; Van Tent,
B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Welikala, N.;
Yvon, D.; Zacchei, A.; Zibin, J. P.; Zonca, A.
2014A&A...561A..97P Altcode: 2013arXiv1303.5090T; 2013arXiv1303.5090P
Using Planck data combined with the Meta Catalogue of X-ray detected
Clusters of galaxies (MCXC), we address the study of peculiar motions
by searching for evidence of the kinetic Sunyaev-Zeldovich effect
(kSZ). By implementing various filters designed to extract the kSZ
generated at the positions of the clusters, we obtain consistent
constraints on the radial peculiar velocity average, root mean square
(rms), and local bulk flow amplitude at different depths. For the whole
cluster sample of average redshift 0.18, the measured average radial
peculiar velocity with respect to the cosmic microwave background (CMB)
radiation at that redshift, i.e., the kSZ monopole, amounts to 72 ±
60 km s<SUP>-1</SUP>. This constitutes less than 1% of the relative
Hubble velocity of the cluster sample with respect to our local CMB
frame. While the linear ΛCDM prediction for the typical cluster radial
velocity rms at z = 0.15 is close to 230 km s<SUP>-1</SUP>, the upper
limit imposed by Planck data on the cluster subsample corresponds to
800 km s<SUP>-1</SUP> at 95% confidence level, i.e., about three times
higher. Planck data also set strong constraints on the local bulk
flow in volumes centred on the Local Group. There is no detection
of bulk flow as measured in any comoving sphere extending to the
maximum redshift covered by the cluster sample. A blind search for bulk
flows in this sample has an upper limit of 254 km s<SUP>-1</SUP> (95%
confidence level) dominated by CMB confusion and instrumental noise,
indicating that the Universe is largely homogeneous on Gpc scales. In
this context, in conjunction with supernova observations, Planck is able
to rule out a large class of inhomogeneous void models as alternatives
to dark energy or modified gravity. The Planck constraints on peculiar
velocities and bulk flows are thus consistent with the ΛCDM scenario.
---------------------------------------------------------
Title: Erratum: Planck intermediate results (Corrigendum). V. Pressure
profiles of galaxy clusters from the Sunyaev-Zeldovich effect
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.;
Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner,
E.; Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia,
R.; Bikmaev, I.; Bobin, J.; Böhringer, H.; Bonaldi, A.; Bond, J. R.;
Borgani, S.; Borrill, J.; Bouchet, F. R.; Bourdin, H.; Brown, M. L.;
Burenin, R.; Burigana, C.; Cabella, P.; Cardoso, J. -F.; Carvalho,
P.; Castex, G.; Catalano, A.; Cayón, L.; Chamballu, A.; Chiang,
L. -Y.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements,
D. L.; Colafrancesco, S.; Colombi, S.; Colombo, L. P. L.; Comis,
B.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Da Silva, A.; Dahle, H.;
Danese, L.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Zotti,
G.; Delabrouille, J.; Démoclès, J.; Désert, F. -X.; Diego, J. M.;
Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.;
Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli,
F.; Flores-Cacho, I.; Forni, O.; Fosalba, P.; Frailis, M.; Franceschi,
E.; Frommert, M.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.;
Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Hempel,
A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hurier, G.;
Jaffe, T. R.; Jaffe, A. H.; Jagemann, T.; Jones, W. C.; Juvela, M.;
Keihänen, E.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.;
Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.;
Leonardi, R.; Liddle, A.; Lilje, P. B.; López-Caniego, M.; Luzzi, G.;
Macías-Pérez, J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Marleau,
F.; Marshall, D. J.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Mazzotta, P.; Mei, S.; Melchiorri, A.; Melin, J. -B.;
Mendes, L.; Mennella, A.; Mitra, S.; Miville-Deschênes, M. -A.;
Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.;
Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen,
H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot, F.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Piffaretti,
R.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.;
Popa, L.; Poutanen, T.; Pratt, G. W.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Roman, M.; Rosset, C.; Rossetti, M.; Rubiño-Martín, J. A.;
Rusholme, B.; Sandri, M.; Savini, G.; Scott, D.; Smoot, G. F.;
Starck, J. -L.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.;
Tomasi, M.; Tristram, M.; Tuovinen, J.; Valenziano, L.; Van Tent, B.;
Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt,
B. D.; Welikala, N.; White, S. D. M.; White, M.; Yvon, D.; Zacchei,
A.; Zonca, A.
2013A&A...558C...2P Altcode:
No abstract at ADS
---------------------------------------------------------
Title: On the Discrepancy between Theoretical and X-Ray
Concentration-Mass Relations for Galaxy Clusters
Authors: Rasia, E.; Borgani, S.; Ettori, S.; Mazzotta, P.; Meneghetti,
M.
2013ApJ...776...39R Altcode: 2013arXiv1301.7476R
In the past 15 years, the concentration-mass relation has been
investigated diffusely in theoretical studies. On the other hand, only
recently has this relation been derived from X-ray observations. When
that happened, the results caused a certain level of concern: the X-ray
normalizations and slopes were found significantly dissimilar from
those predicted by theory. We analyzed 52 galaxy clusters and groups,
simulated with different descriptions of the physical processes that
affect the baryonic component, with the purpose of determining whether
these discrepancies are real or induced by biases in the computation
of the concentration parameter or in the determination of the selection
function of the cluster sample for which the analysis is carried out. In
particular, we investigate how the simulated concentration-mass relation
depends (1) on the radial range used to derive the concentration; (2)
on the presence of baryons in the simulations, and on the effect of
star formation and feedback from supernovae and active galactic nuclei
(AGNs). Finally, we evaluate (3) how the results differ when adopting an
X-ray approach for the analysis and (4) how the selection function based
on X-ray luminosity can impact the results. All effects studied go in
the direction of alleviating the discrepancy between observations and
simulations, although with different significance: while the choice of
the radial range to fit the profiles and the inclusion of the baryonic
component play only a minor role, the X-ray approach to reconstruct
the mass profiles and the selection of the cluster sample have a strong
impact on the resulting concentration-mass relation. Extending the fit
to the most central regions or reducing the fitting radius from the
virial boundary to the typical X-ray external radius causes an increase
of the normalization in radiative simulations by 5%-10%. In the second
case, we measure a slope that is up to twice steeper than that derived
by using the typical theoretical radial range. Radiative simulations
including only supernova feedback produce 30% higher concentrations
than the dark matter case. Such a difference is largely reduced when
including the effect of AGN feedback. The concentration-mass relation
derived from the X-ray synthetic catalog is significantly steeper due
to the combination of several different effects, such as environment,
dynamical state and dynamical history of the clusters, bias in mass
and temperature measurements, and their dependence on the radius and
on the mass of the system. Finally, selecting clusters according to
their X-ray luminosity produces a net increase in both normalization
and slope of the relation, since at fixed mass, the most luminous
clusters are also the most concentrated.
---------------------------------------------------------
Title: Is the Sunyaev-Zeldovich effect responsible for the observed
steepening in the spectrum of the Coma radio halo?
Authors: Brunetti, G.; Rudnick, L.; Cassano, R.; Mazzotta, P.; Donnert,
J.; Dolag, K.
2013A&A...558A..52B Altcode: 2013arXiv1309.1820B
<BR /> Aims: The radio halo in the Coma cluster is unique in that its
spectrum has been measured over almost two decades in frequency. The
current radio data show a steepening of the spectrum at higher
frequencies, which has implications for models of the radio halo
origin. There is an on-going debate on the possibility that the observed
steepening of the spectrum and the apparent shrinking of the halo-size
at higher frequencies is not intrinsic to the emitted radiation, but is
instead caused by the Sunyaev-Zeldovich (SZ) effect. <BR /> Methods:
Recently, the Planck satellite obtained unprecedented measurements
of the SZ signal and its spatial distribution in the Coma cluster,
allowing a conclusive testing of this hypothesis. Using the Planck
results, we calculated the modification of the radio halo spectrum by
the SZ effect in three different ways. With the first two methods we
measured the SZ-decrement by adopting self-consistently the aperture
radii used for flux measurements of the radio halo at the different
frequencies. First we adopted the global compilation of data-points
from Thierbach et al. (2003, A&A, 397, 53) and a reference aperture
radius consistent with those used by various authors. Second we used
the available brightness profiles of the halo at different frequencies
to derive the spectrum of the halo within two fixed apertures,
corresponding to the size of the halo measured at 2.675 and at 4.85
GHz, and derived the SZ-decrement using these apertures. As a third
method we used the quasi-linear correlation between the y-signal
and the radio-halo brightness at 330 MHz discovered by the Planck
collaboration to derive the modification of the synchrotron spectrum
by the SZ-decrement in a way that is almost independent of the adopted
aperture radius. <BR /> Results: We found that the spectral modification
induced by the SZ-decrement is negligible and results in values 4-5
times smaller than those necessary to explain the observed steepening
at higher frequencies. We also show that, if a spectral steepening is
absent from the emitted spectrum, future deep observations at 5 GHz
with single dishes are expected to measure a halo flux in a 40 arcmin
aperture-radius that would be ~7-8 times higher than currently seen,
thus providing a complementary test to our findings. <BR /> Conclusions:
We conclude that according to the current radio data the emitted
synchrotron spectrum of the radio halo steepens at higher frequencies,
implying a break or cut-off in the spectrum of the emitting electrons
at energies of a few GeV.
---------------------------------------------------------
Title: Planck intermediate results. XI. The gas content of dark
matter halos: the Sunyaev-Zeldovich-stellar mass relation for locally
brightest galaxies
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Balbi,
A.; Banday, A. J.; Barreiro, R. B.; Barrena, R.; Bartlett, J. G.;
Battaner, E.; Benabed, K.; Bernard, J. -P.; Bersanelli, M.; Bikmaev,
I.; Bock, J. J.; Böhringer, H.; Bonaldi, A.; Bond, J. R.; Borrill,
J.; Bouchet, F. R.; Bourdin, H.; Burenin, R.; Burigana, C.; Butler,
R. C.; Cabella, P.; Chamballu, A.; Chary, R. -R.; Chiang, L. -Y.;
Chon, G.; Christensen, P. R.; Clements, D. L.; Colafrancesco, S.;
Colombi, S.; Colombo, L. P. L.; Comis, B.; Coulais, A.; Crill, B. P.;
Cuttaia, F.; Da Silva, A.; Dahle, H.; Davis, R. J.; de Bernardis,
P.; de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.;
Démoclès, J.; Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.;
Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Finelli, F.;
Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi, E.; Frommert,
M.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gregorio,
A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.; Hurier, G.;
Jaffe, T. R.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen,
E.; Keskitalo, R.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche,
J.; Kunz, M.; Kurki-Suonio, H.; Lähteenmäki, A.; Lamarre, J. -M.;
Lasenby, A.; Lawrence, C. R.; Le Jeune, M.; Leonardi, R.; Lilje,
P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Luzzi, G.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.;
Maino, D.; Mandolesi, N.; Maris, M.; Marleau, F.; Marshall, D. J.;
Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Mazzotta, P.; Mei, S.; Melchiorri, A.; Melin, J. -B.; Mendes, L.;
Mennella, A.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.;
Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.;
Naselsky, P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.; Pajot,
F.; Paoletti, D.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Piffaretti, R.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Ristorcelli, I.; Rocha, G.; Roman,
M.; Rosset, C.; Rossetti, M.; Rubiño-Martín, J. A.; Rusholme, B.;
Sandri, M.; Savini, G.; Scott, D.; Spencer, L.; Starck, J. -L.;
Stolyarov, V.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.;
Tomasi, M.; Tristram, M.; Valenziano, L.; Van Tent, B.; Vielva,
P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Wang,
W.; Welikala, N.; Weller, J.; White, S. D. M.; White, M.; Yvon, D.;
Zacchei, A.; Zonca, A.
2013A&A...557A..52P Altcode: 2012arXiv1212.4131P; 2013A&A...557A..52.
We present the scaling relation between Sunyaev-Zeldovich (SZ)
signal and stellar mass for almost 260,000 locally brightest galaxies
(LBGs) selected from the Sloan Digital Sky Survey (SDSS). These are
predominantly the central galaxies of their dark matter halos. We
calibrate the stellar-to-halo mass conversion using realistic
mock catalogues based on the Millennium Simulation. Applying a
multi-frequency matched filter to the Planck data for each LBG, and
averaging the results in bins of stellar mass, we measure the mean SZ
signal down to M<SUB>∗</SUB> ~ 2 × 10<SUP>11</SUP> M<SUB>⊙</SUB>,
with a clear indication of signal at even lower stellar mass. We derive
the scaling relation between SZ signal and halo mass by assigning halo
properties from our mock catalogues to the real LBGs and simulating
the Planck observation process. This relation shows no evidence for
deviation from a power law over a halo mass range extending from rich
clusters down to M<SUB>500</SUB> ~ 2 × 10<SUP>13</SUP> M<SUB>⊙</SUB>,
and there is a clear indication of signal down to M<SUB>500</SUB> ~
4 × 10<SUP>12</SUP> M<SUB>⊙</SUB>. Planck's SZdetections in such
low-mass halos imply that about a quarter of all baryons have now
been seen in the form of hot halo gas, and that this gas must be less
concentrated than the dark matter in such halos in order to remain
consistent with X-ray observations. At the high-mass end, the measured
SZ signal is 20% lower than found from observations of X-ray clusters,
a difference consistent with the magnitude of Malmquist bias effects
that were previously estimated for the X-ray sample.
---------------------------------------------------------
Title: Planck intermediate results. XII: Diffuse Galactic components
in the Gould Belt system
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alves,
M. I. R.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont,
J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.;
Bartlett, J. G.; Battaner, E.; Bedini, L.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bonaldi, A.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Boulanger, F.; Burigana, C.; Butler,
R. C.; Cabella, P.; Cardoso, J. -F.; Chen, X.; Chiang, L. -Y.;
Christensen, P. R.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.;
Coulais, A.; Cuttaia, F.; Davies, R. D.; Davis, R. J.; de Bernardis,
P.; de Gasperis, G.; de Zotti, G.; Delabrouille, J.; Dickinson, C.;
Diego, J. M.; Dobler, G.; Dole, H.; Donzelli, S.; Doré, O.; Douspis,
M.; Dupac, X.; Enßlin, T. A.; Finelli, F.; Forni, O.; Frailis, M.;
Franceschi, E.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Ghosh,
T.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison,
D.; Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson,
M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.;
Jaffe, T. R.; Jaffe, A. H.; Juvela, M.; Keihänen, E.; Keskitalo, R.;
Kisner, T. S.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.;
Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.;
Leach, S.; Leonardi, R.; Lilje, P. B.; Linden-Vørnle, M.; Lubin,
P. M.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.;
Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez-González, E.;
Masi, S.; Massardi, M.; Matarrese, S.; Mazzotta, P.; Melchiorri,
A.; Mennella, A.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.;
Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.;
Naselsky, P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Oxborrow, C. A.; Pajot,
F.; Paladini, R.; Paoletti, D.; Peel, M.; Perotto, L.; Perrotta, F.;
Piacentini, F.; Piat, M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski,
S.; Pointecouteau, E.; Polenta, G.; Popa, L.; Poutanen, T.; Pratt,
G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo,
R.; Reinecke, M.; Renault, C.; Ricciardi, S.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Rubiño-Martín, J. A.; Rusholme, B.; Salerno, E.;
Sandri, M.; Savini, G.; Scott, D.; Spencer, L.; Stolyarov, V.;
Sudiwala, R.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Terenzi, L.; Tibbs, C. T.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Valenziano, L.; Van Tent, B.; Varis, J.; Vielva, P.; Villa,
F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Ysard, N.; Yvon, D.;
Zacchei, A.; Zonca, A.
2013A&A...557A..53P Altcode: 2013arXiv1301.5839P; 2013A&A...557A..53.
We perform an analysis of the diffuse low-frequency Galactic components
in the southern part of the Gould Belt system (130° ≤ l ≤ 230° and
-50° ≤ b ≤ -10°). Strong ultra-violet flux coming from the Gould
Belt super-association is responsible for bright diffuse foregrounds
that we observe from our position inside the system and that can help
us improve our knowledge of the Galactic emission. Free-free emission
and anomalous microwave emission (AME) are the dominant components at
low frequencies (ν < 40 GHz), while synchrotron emission is very
smooth and faint. We separated diffuse free-free emission and AME from
synchrotron emission and thermal dust emission by using Planck data,
complemented by ancillary data, using the correlated component analysis
(CCA) component-separation method and we compared our results with the
results of cross-correlation of foreground templates with the frequency
maps. We estimated the electron temperature T<SUB>e</SUB> from Hα and
free-free emission using two methods (temperature-temperature plot
and cross-correlation) and obtained T<SUB>e</SUB> ranging from 3100
to 5200K for an effective fraction of absorbing dust along the line
of sight of 30% (f<SUB>d</SUB> = 0.3). We estimated the frequency
spectrum of the diffuse AME and recovered a peak frequency (in flux
density units) of 25.5 ± 1.5 GHz. We verified the reliability of this
result with realistic simulations that include biases in the spectral
model for the AME and in the free-free template. By combining physical
models for vibrational and rotational dust emission and adding the
constraints from the thermal dust spectrum from Planck and IRAS,
we are able to present a good description of the AME frequency
spectrum for plausible values of the local density and radiation
field. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org">http://www.aanda.org</A>
---------------------------------------------------------
Title: Hot X-Ray Coronae around Massive Spiral Galaxies: A Unique
Probe of Structure Formation Models
Authors: Bogdán, Ákos; Forman, William R.; Vogelsberger, Mark;
Bourdin, Hervé; Sijacki, Debora; Mazzotta, Pasquale; Kraft, Ralph P.;
Jones, Christine; Gilfanov, Marat; Churazov, Eugene; David, Laurence P.
2013ApJ...772...97B Altcode: 2012arXiv1212.0541B
Luminous X-ray gas coronae in the dark matter halos of massive spiral
galaxies are a fundamental prediction of structure formation models,
yet only a few such coronae have been detected so far. In this paper,
we study the hot X-ray coronae beyond the optical disks of two "normal"
massive spirals, NGC 1961 and NGC 6753. Based on XMM-Newton X-ray
observations, hot gaseous emission is detected to ~60 kpc—well
beyond their optical radii. The hot gas has a best-fit temperature
of kT ~ 0.6 keV and an abundance of ~0.1 Solar, and exhibits a
fairly uniform distribution, suggesting that the quasi-static gas
resides in hydrostatic equilibrium in the potential well of the
galaxies. The bolometric luminosity of the gas in the (0.05-0.15)r
<SUB>200</SUB> region (r <SUB>200</SUB> is the virial radius) is ~6
× 10<SUP>40</SUP> erg s<SUP>-1</SUP> for both galaxies. The baryon
mass fractions of NGC 1961 and NGC 6753 are f <SUB>b, NGC 1961</SUB>
~ 0.11 and f <SUB>b, NGC 6753</SUB> ~ 0.09, which values fall short of
the cosmic baryon fraction. The hot coronae around NGC 1961 and NGC 6753
offer an excellent basis to probe structure formation simulations. To
this end, the observations are confronted with the moving mesh code
AREPO and the smoothed particle hydrodynamics code GADGET. Although
neither model gives a perfect description, the observed luminosities,
gas masses, and abundances favor the AREPO code. Moreover, the shape
and the normalization of the observed density profiles are better
reproduced by AREPO within ~0.5r <SUB>200</SUB>. However, neither
model incorporates efficient feedback from supermassive black holes or
supernovae, which could alter the simulated properties of the X-ray
coronae. With the further advance of numerical models, the present
observations will be essential in constraining the feedback effects
in structure formation simulations.
---------------------------------------------------------
Title: X-Ray Analysis of Simulated Clusters
Authors: Rasia, E.; Borgani, S.; Dolag, K.; Ettori, S.; Mazzotta,
P.; Meneghetti, M.
2013tcec.confE...5R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: The Hot and Energetic Universe: The evolution of galaxy groups
and clusters
Authors: Pointecouteau, E.; Reiprich, T. H.; Adami, C.; Arnaud, M.;
Biffi, V.; Borgani, S.; Borm, K.; Bourdin, H.; Brueggen, M.; Bulbul,
E.; Clerc, N.; Croston, J. H.; Dolag, K.; Ettori, S.; Finoguenov, A.;
Kaastra, J.; Lovisari, L.; Maughan, B.; Mazzotta, P.; Pacaud, F.;
de Plaa, J.; Pratt, G. W.; Ramos-Ceja, M.; Rasia, E.; Sanders, J.;
Zhang, Y. -Y.; Allen, S.; Boehringer, H.; Brunetti, G.; Elbaz, D.;
Fassbender, R.; Hoekstra, H.; Hildebrandt, H.; Lamer, G.; Marrone, D.;
Mohr, J.; Molendi, S.; Nevalainen, J.; Ohashi, T.; Ota, N.; Pierre,
M.; Romer, K.; Schindler, S.; Schrabback, T.; Schwope, A.; Smith,
R.; Springel, V.; von der Linden, A.
2013arXiv1306.2319P Altcode:
Major astrophysical questions related to the formation and evolution
of structures, and more specifically of galaxy groups and clusters,
will still be open in the coming decade and beyond: what is the
interplay of galaxy, supermassive black hole, and intergalactic gas
evolution in the most massive objects in the Universe - galaxy groups
and clusters? What are the processes driving the evolution of chemical
enrichment of the hot diffuse gas in large-scale structures? How and
when did the first galaxy groups in the Universe, massive enough to
bind more than 10^7 K gas, form? Focussing on the period when groups and
clusters assembled (0.5<z<2.5), we show that, due to the continuum
and line emission of this hot intergalactic gas at X-ray wavelengths,
Athena+, combining high sensitivity with excellent spectral and spatial
resolution, will deliver breakthrough observations in view of the
aforementioned issues. Indeed, the physical and chemical properties
of the hot intra-cluster gas, and their evolution across time, are a
key to understand the co-evolution of galaxy and supermassive black
hole within their environments.
---------------------------------------------------------
Title: The Hot and Energetic Universe: A White Paper presenting the
science theme motivating the Athena+ mission
Authors: Nandra, Kirpal; Barret, Didier; Barcons, Xavier; Fabian,
Andy; den Herder, Jan-Willem; Piro, Luigi; Watson, Mike; Adami,
Christophe; Aird, James; Afonso, Jose Manuel; Alexander, Dave;
Argiroffi, Costanza; Amati, Lorenzo; Arnaud, Monique; Atteia, Jean-Luc;
Audard, Marc; Badenes, Carles; Ballet, Jean; Ballo, Lucia; Bamba,
Aya; Bhardwaj, Anil; Stefano Battistelli, Elia; Becker, Werner;
De Becker, Michaël; Behar, Ehud; Bianchi, Stefano; Biffi, Veronica;
Bîrzan, Laura; Bocchino, Fabrizio; Bogdanov, Slavko; Boirin, Laurence;
Boller, Thomas; Borgani, Stefano; Borm, Katharina; Bouché, Nicolas;
Bourdin, Hervé; Bower, Richard; Braito, Valentina; Branchini, Enzo;
Branduardi-Raymont, Graziella; Bregman, Joel; Brenneman, Laura;
Brightman, Murray; Brüggen, Marcus; Buchner, Johannes; Bulbul,
Esra; Brusa, Marcella; Bursa, Michal; Caccianiga, Alessandro;
Cackett, Ed; Campana, Sergio; Cappelluti, Nico; Cappi, Massimo;
Carrera, Francisco; Ceballos, Maite; Christensen, Finn; Chu, You-Hua;
Churazov, Eugene; Clerc, Nicolas; Corbel, Stephane; Corral, Amalia;
Comastri, Andrea; Costantini, Elisa; Croston, Judith; Dadina, Mauro;
D'Ai, Antonino; Decourchelle, Anne; Della Ceca, Roberto; Dennerl,
Konrad; Dolag, Klaus; Done, Chris; Dovciak, Michal; Drake, Jeremy;
Eckert, Dominique; Edge, Alastair; Ettori, Stefano; Ezoe, Yuichiro;
Feigelson, Eric; Fender, Rob; Feruglio, Chiara; Finoguenov, Alexis;
Fiore, Fabrizio; Galeazzi, Massimiliano; Gallagher, Sarah; Gandhi,
Poshak; Gaspari, Massimo; Gastaldello, Fabio; Georgakakis, Antonis;
Georgantopoulos, Ioannis; Gilfanov, Marat; Gitti, Myriam; Gladstone,
Randy; Goosmann, Rene; Gosset, Eric; Grosso, Nicolas; Guedel, Manuel;
Guerrero, Martin; Haberl, Frank; Hardcastle, Martin; Heinz, Sebastian;
Alonso Herrero, Almudena; Hervé, Anthony; Holmstrom, Mats; Iwasawa,
Kazushi; Jonker, Peter; Kaastra, Jelle; Kara, Erin; Karas, Vladimir;
Kastner, Joel; King, Andrew; Kosenko, Daria; Koutroumpa, Dimita; Kraft,
Ralph; Kreykenbohm, Ingo; Lallement, Rosine; Lanzuisi, Giorgio; Lee,
J.; Lemoine-Goumard, Marianne; Lobban, Andrew; Lodato, Giuseppe;
Lovisari, Lorenzo; Lotti, Simone; McCharthy, Ian; McNamara, Brian;
Maggio, Antonio; Maiolino, Roberto; De Marco, Barbara; de Martino,
Domitilla; Mateos, Silvia; Matt, Giorgio; Maughan, Ben; Mazzotta,
Pasquale; Mendez, Mariano; Merloni, Andrea; Micela, Giuseppina; Miceli,
Marco; Mignani, Robert; Miller, Jon; Miniutti, Giovanni; Molendi,
Silvano; Montez, Rodolfo; Moretti, Alberto; Motch, Christian; Nazé,
Yaël; Nevalainen, Jukka; Nicastro, Fabrizio; Nulsen, Paul; Ohashi,
Takaya; O'Brien, Paul; Osborne, Julian; Oskinova, Lida; Pacaud,
Florian; Paerels, Frederik; Page, Mat; Papadakis, Iossif; Pareschi,
Giovanni; Petre, Robert; Petrucci, Pierre-Olivier; Piconcelli, Enrico;
Pillitteri, Ignazio; Pinto, C.; de Plaa, Jelle; Pointecouteau, Etienne;
Ponman, Trevor; Ponti, Gabriele; Porquet, Delphine; Pounds, Ken; Pratt,
Gabriel; Predehl, Peter; Proga, Daniel; Psaltis, Dimitrios; Rafferty,
David; Ramos-Ceja, Miriam; Ranalli, Piero; Rasia, Elena; Rau, Arne;
Rauw, Gregor; Rea, Nanda; Read, Andy; Reeves, James; Reiprich, Thomas;
Renaud, Matthieu; Reynolds, Chris; Risaliti, Guido; Rodriguez, Jerome;
Rodriguez Hidalgo, Paola; Roncarelli, Mauro; Rosario, David; Rossetti,
Mariachiara; Rozanska, Agata; Rovilos, Emmanouil; Salvaterra, Ruben;
Salvato, Mara; Di Salvo, Tiziana; Sanders, Jeremy; Sanz-Forcada, Jorge;
Schawinski, Kevin; Schaye, Joop; Schwope, Axel; Sciortino, Salvatore;
Severgnini, Paola; Shankar, Francesco; Sijacki, Debora; Sim, Stuart;
Schmid, Christian; Smith, Randall; Steiner, Andrew; Stelzer, Beate;
Stewart, Gordon; Strohmayer, Tod; Strüder, Lothar; Sun, Ming; Takei,
Yoh; Tatischeff, V.; Tiengo, Andreas; Tombesi, Francesco; Trinchieri,
Ginevra; Tsuru, T. G.; Ud-Doula, Asif; Ursino, Eugenio; Valencic,
Lynne; Vanzella, Eros; Vaughan, Simon; Vignali, Cristian; Vink,
Jacco; Vito, Fabio; Volonteri, Marta; Wang, Daniel; Webb, Natalie;
Willingale, Richard; Wilms, Joern; Wise, Michael; Worrall, Diana;
Young, Andrew; Zampieri, Luca; In't Zand, Jean; Zane, Silvia; Zezas,
Andreas; Zhang, Yuying; Zhuravleva, Irina
2013arXiv1306.2307N Altcode:
This White Paper, submitted to the recent ESA call for science
themes to define its future large missions, advocates the need for a
transformational leap in our understanding of two key questions in
astrophysics: 1) How does ordinary matter assemble into the large
scale structures that we see today? 2) How do black holes grow and
shape the Universe? Hot gas in clusters, groups and the intergalactic
medium dominates the baryonic content of the local Universe. To
understand the astrophysical processes responsible for the formation
and assembly of these large structures, it is necessary to measure
their physical properties and evolution. This requires spatially
resolved X-ray spectroscopy with a factor 10 increase in both telescope
throughput and spatial resolving power compared to currently planned
facilities. Feedback from supermassive black holes is an essential
ingredient in this process and in most galaxy evolution models, but
it is not well understood. X-ray observations can uniquely reveal
the mechanisms launching winds close to black holes and determine the
coupling of the energy and matter flows on larger scales. Due to the
effects of feedback, a complete understanding of galaxy evolution
requires knowledge of the obscured growth of supermassive black
holes through cosmic time, out to the redshifts where the first
galaxies form. X-ray emission is the most reliable way to reveal
accreting black holes, but deep survey speed must improve by a factor
~100 over current facilities to perform a full census into the early
Universe. The Advanced Telescope for High Energy Astrophysics (Athena+)
mission provides the necessary performance (e.g. angular resolution,
spectral resolution, survey grasp) to address these questions and
revolutionize our understanding of the Hot and Energetic Universe. These
capabilities will also provide a powerful observatory to be used in
all areas of astrophysics.
---------------------------------------------------------
Title: Planck intermediate results. IX. Detection of the Galactic
haze with Planck
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Balbi,
A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.;
Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bonaldi,
A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Burigana, C.; Cabella,
P.; Cardoso, J. -F.; Catalano, A.; Cayón, L.; Chary, R. -R.; Chiang,
L. -Y.; Christensen, P. R.; Clements, D. L.; Colombo, L. P. L.;
Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.; D'Arcangelo,
O.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de
Zotti, G.; Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dobler, G.;
Dole, H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.;
Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni,
O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard,
M.; Giardino, G.; González-Nuevo, J.; Górski, K. M.; Gratton, S.;
Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Helou, G.;
Henrot-Versillé, S.; Hernández-Monteagudo, C.; Hildebrandt, S. R.;
Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.;
Huffenberger, K. M.; Jaffe, T. R.; Jagemann, T.; Jewell, J.; Jones,
W. C.; Juvela, M.; Keihänen, E.; Knoche, J.; Knox, L.; Kunz, M.;
Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.;
Lasenby, A.; Lawrence, C. R.; Leach, S.; Leonardi, R.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall,
D. J.; Martin, P. G.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri,
A.; Mendes, L.; Mennella, A.; Mitra, S.; Moneti, A.; Montier, L.;
Morgante, G.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Natoli, P.;
Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.;
Osborne, S.; Pajot, F.; Paladini, R.; Paoletti, D.; Partridge, B.;
Pearson, T. J.; Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Pietrobon, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.;
Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.;
Rosset, C.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini,
G.; Schaefer, B. M.; Scott, D.; Smoot, G. F.; Spencer, L.; Stivoli,
F.; Sudiwala, R.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Türler,
M.; Umana, G.; Valenziano, L.; Van Tent, B.; Vielva, P.; Villa,
F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; White, M.; Yvon, D.;
Zacchei, A.; Zonca, A.
2013A&A...554A.139P Altcode: 2012arXiv1208.5483P
Using precise full-sky observations from Planck, and applying several
methods of component separation, we identify and characterise the
emission from the Galactic "haze" at microwave wavelengths. The
haze is a distinct component of diffuse Galactic emission, roughly
centered on the Galactic centre, and extends to | b | ~ 35-50° in
Galactic latitude and | l | ~ 15-20° in longitude. By combining the
Planck data with observations from the Wilkinson Microwave Anisotropy
Probe, we were able to determine the spectrum of this emission to high
accuracy, unhindered by the strong systematic biases present in previous
analyses. The derived spectrum is consistent with power-law emission
with a spectral index of -2.56 ± 0.05, thus excluding free-free
emission as the source and instead favouring hard-spectrum synchrotron
radiation from an electron population with a spectrum (number density
per energy) dN/dE ∝ E<SUP>-2.1</SUP>. At Galactic latitudes | b | <
30°, the microwave haze morphology is consistent with that of the Fermi
gamma-ray "haze" or "bubbles", while at b ~ -50° we have identified an
edge in the microwave haze that is spatially coincident with the edge
in the gamma-ray bubbles. Taken together, this indicates that we have
a multi-wavelength view of a distinct component of our Galaxy. Given
both the very hard spectrum and the extended nature of the emission,
it is highly unlikely that the haze electrons result from supernova
shocks in the Galactic disk. Instead, a new astrophysical mechanism
for cosmic-ray acceleration in the inner Galaxy is implied.
---------------------------------------------------------
Title: Planck intermediate results. X. Physics of the hot gas in
the Coma cluster
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Balbi,
A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.;
Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bikmaev, I.;
Böhringer, H.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Bourdin, H.; Brown, M. L.; Brown, S. D.; Burenin, R.; Burigana, C.;
Cabella, P.; Cardoso, J. -F.; Carvalho, P.; Catalano, A.; Cayón, L.;
Chiang, L. -Y.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements,
D. L.; Colafrancesco, S.; Colombo, L. P. L.; Coulais, A.; Crill,
B. P.; Cuttaia, F.; Da Silva, A.; Dahle, H.; Danese, L.; Davis,
R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Démoclès, J.; Désert, F. -X.; Dickinson,
C.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.;
Dörl, U.; Douspis, M.; Dupac, X.; Enßlin, T. A.; Eriksen, H. K.;
Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi, E.;
Frommert, M.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard,
M.; Gilfanov, M.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.;
Gruppuso, A.; Hansen, F. K.; Harrison, D.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson,
M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger, K. M.;
Hurier, G.; Jaffe, T. R.; Jagemann, T.; Jones, W. C.; Juvela, M.;
Keihänen, E.; Khamitov, I.; Kneissl, R.; Knoche, J.; Knox, L.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre,
J. -M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.; Leonardi, R.;
Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi, N.; Maris,
M.; Marleau, F.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Matthai, F.; Mazzotta, P.; Mei, S.; Melchiorri, A.;
Melin, J. -B.; Mendes, L.; Mennella, A.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Munshi, D.; Murphy,
J. A.; Naselsky, P.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot, F.; Paoletti, D.;
Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli,
E.; Piffaretti, R.; Plaszczynski, S.; Pointecouteau, E.; Polenta,
G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.;
Roman, M.; Rosset, C.; Rossetti, M.; Rubiño-Martín, J. A.; Rudnick,
L.; Rusholme, B.; Sandri, M.; Savini, G.; Schaefer, B. M.; Scott,
D.; Smoot, G. F.; Stivoli, F.; Sudiwala, R.; Sunyaev, R.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tuovinen, J.; Türler,
M.; Umana, G.; Valenziano, L.; Van Tent, B.; Varis, J.; Vielva, P.;
Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Welikala, N.;
White, S. D. M.; Yvon, D.; Zacchei, A.; Zaroubi, S.; Zonca, A.
2013A&A...554A.140P Altcode: 2012arXiv1208.3611P
We present an analysis of Planck satellite data on the Coma
cluster observed via the Sunyaev-Zeldovich effect. Thanks to its
great sensitivity, Planck is able, for the first time, to detect
SZ emission up to r ≈ 3 × R<SUB>500</SUB>. We test previously
proposed spherically symmetric models for the pressure distribution
in clusters against the azimuthally averaged data. In particular,
we find that the Arnaud et al. (2010, A&A, 517, A92) "universal"
pressure profile does not fit Coma, and that their pressure profile
for merging systems provides a reasonable fit to the data only at r
< R<SUB>500</SUB>; by r = 2 × R<SUB>500</SUB> it underestimates
the observed y profile by a factor of ≃2. This may indicate that at
these larger radii either: i) the cluster SZ emission is contaminated
by unresolved SZ sources along the line of sight; or ii) the pressure
profile of Coma is higher at r > R<SUB>500</SUB> than the mean
pressure profile predicted by the simulations used to constrain the
models. The Planck image shows significant local steepening of the
y profile in two regions about half a degree to the west and to the
south-east of the cluster centre. These features are consistent with
the presence of shock fronts at these radii, and indeed the western
feature was previously noticed in the ROSAT PSPC mosaic as well as
in the radio. Using Plancky profiles extracted from corresponding
sectors we find pressure jumps of 4.9<SUB>-0.2</SUB><SUP>+0.4</SUP>
and 5.0<SUB>-0.1</SUB><SUP>+1.3</SUP> in the west and south-east,
respectively. Assuming Rankine-Hugoniot pressure jump conditions,
we deduce that the shock waves should propagate with Mach number
M<SUB>w</SUB> = 2.03<SUB>-0.04</SUB><SUP>+0.09</SUP> and M<SUB>se</SUB>
= 2.05<SUB>-0.02</SUB><SUP>+0.25</SUP> in the west and south-east,
respectively. Finally, we find that the y and radio-synchrotron
signals are quasi-linearly correlated on Mpc scales, with small
intrinsic scatter. This implies either that the energy density of
cosmic-ray electrons is relatively constant throughout the cluster,
or that the magnetic fields fall off much more slowly with radius than
previously thought.
---------------------------------------------------------
Title: The pre-launch Planck Sky Model: a model of sky emission at
submillimetre to centimetre wavelengths
Authors: Delabrouille, J.; Betoule, M.; Melin, J. -B.;
Miville-Deschênes, M. -A.; Gonzalez-Nuevo, J.; Le Jeune, M.; Castex,
G.; de Zotti, G.; Basak, S.; Ashdown, M.; Aumont, J.; Baccigalupi,
C.; Banday, A. J.; Bernard, J. -P.; Bouchet, F. R.; Clements, D. L.;
da Silva, A.; Dickinson, C.; Dodu, F.; Dolag, K.; Elsner, F.; Fauvet,
L.; Faÿ, G.; Giardino, G.; Leach, S.; Lesgourgues, J.; Liguori, M.;
Macías-Pérez, J. F.; Massardi, M.; Matarrese, S.; Mazzotta, P.;
Montier, L.; Mottet, S.; Paladini, R.; Partridge, B.; Piffaretti,
R.; Prezeau, G.; Prunet, S.; Ricciardi, S.; Roman, M.; Schaefer, B.;
Toffolatti, L.
2013A&A...553A..96D Altcode: 2012arXiv1207.3675D
We present the Planck Sky Model (PSM), a parametric model for generating
all-sky, few arcminute resolution maps of sky emission at submillimetre
to centimetre wavelengths, in both intensity and polarisation. Several
options are implemented to model the cosmic microwave background,
Galactic diffuse emission (synchrotron, free-free, thermal and spinning
dust, CO lines), Galactic H ii regions, extragalactic radio sources,
dusty galaxies, and thermal and kinetic Sunyaev-Zeldovich signals from
clusters of galaxies. Each component is simulated by means of educated
interpolations/extrapolations of data sets available at the time of
the launch of the Planck mission, complemented by state-of-the-art
models of the emission. Distinctive features of the simulations
are spatially varying spectral properties of synchrotron and dust;
different spectral parameters for each point source; modelling of
the clustering properties of extragalactic sources and of the power
spectrum of fluctuations in the cosmic infrared background. The PSM
enables the production of random realisations of the sky emission,
constrained to match observational data within their uncertainties. It
is implemented in a software package that is regularly updated with
incoming information from observations. The model is expected to serve
as a useful tool for optimising planned microwave and sub-millimetre
surveys and testing data processing and analysis pipelines. It is,
in particular, used to develop and validate data analysis pipelines
within the Planck collaboration. A version of the software that can
be used for simulating the observations for a variety of experiments
is made available on a dedicated website.
---------------------------------------------------------
Title: X-Ray c-M Relation: Theory & Observations
Authors: Rasia, E.; Mazzotta, P.; Borgani, S.; Ettori, S.; Meneghetti,
M.
2013sncl.confE..15R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Lensing Analysis of Simulated Galaxy Clusters
Authors: Meneghetti, M.; Rasia, E.; Giocoli, C.; Vega, J.; Ettori,
S.; Mazzotta, P.; Borgani, S.; Killedar, M.; Carrasco, M.; Coe, D.;
Merten, J.; Melchior, P.
2013sncl.confE..51M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Planck Results on the Coma Cluster
Authors: Mazzotta, P.
2013sncl.confE..97M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Observations of Radio Minihalos in Sloshing Cool Cores
Authors: Giacintucci, S.; Markevitch, M.; Clarke, T.; Venturi, T.;
Brunetti, G.; Cassano, R.; Mazzotta, P.; ZuHone, J.; Kale, R.
2013sncl.confE..38G Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Planck intermediate results. III. The relation between galaxy
cluster mass and Sunyaev-Zeldovich signal
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi,
C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.;
Battaner, E.; Battye, R.; Benabed, K.; Bernard, J. -P.; Bersanelli,
M.; Bhatia, R.; Bikmaev, I.; Böhringer, H.; Bonaldi, A.; Bond, J. R.;
Borgani, S.; Borrill, J.; Bouchet, F. R.; Bourdin, H.; Brown, M. L.;
Bucher, M.; Burenin, R.; Burigana, C.; Butler, R. C.; Cabella, P.;
Cardoso, J. -F.; Carvalho, P.; Chamballu, A.; Chiang, L. -Y.; Chon,
G.; Clements, D. L.; Colafrancesco, S.; Coulais, A.; Cuttaia, F.;
Da Silva, A.; Dahle, H.; Davis, R. J.; de Bernardis, P.; de Gasperis,
G.; Delabrouille, J.; Démoclès, J.; Désert, F. -X.; Diego, J. M.;
Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac,
X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.;
Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi, E.; Frommert,
M.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.;
Gruppuso, A.; Hansen, F. K.; Harrison, D.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.;
Huffenberger, K. M.; Hurier, G.; Jagemann, T.; Juvela, M.; Keihänen,
E.; Khamitov, I.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.;
Le Jeune, M.; Leach, S.; Leonardi, R.; Liddle, A.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Luzzi, G.; Macías-Pérez,
J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Marleau, F.; Marshall,
D. J.; Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.;
Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Melin, J. -B.; Mendes,
L.; Mitra, S.; Miville-Deschênes, M. -A.; Montier, L.; Morgante,
G.; Munshi, D.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.;
Osborne, S.; Pajot, F.; Paoletti, D.; Partridge, B.; Pearson, T. J.;
Perdereau, O.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.;
Piffaretti, R.; Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu,
N.; Popa, L.; Poutanen, T.; Pratt, G. W.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.;
Ricciardi, S.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rossetti, M.;
Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Scott,
D.; Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Sudiwala, R.; Sunyaev,
R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Valenziano,
L.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wandelt, B. D.;
Weller, J.; White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2013A&A...550A.129P Altcode: 2012arXiv1204.2743P; 2013A&A...550A.129A
We examine the relation between the galaxy cluster mass M and
Sunyaev-Zeldovich (SZ) effect signal D<SUB>A</SUB><SUP>2</SUP>
Y<SUB>500</SUB> for a sample of 19 objects for which weak lensing (WL)
mass measurements obtained from Subaru Telescope data are available in
the literature. Hydrostatic X-ray masses are derived from XMM-Newton
archive data, and the SZ effect signal is measured from Planck all-sky
survey data. We find an M<SUB>WL</SUB> - D<SUB>A</SUB><SUP>2</SUP>
Y<SUB>500</SUB> relation that is consistent in slope and normalisation
with previous determinations using weak lensing masses; however,
there is a normalisation offset with respect to previous measures
based on hydrostatic X-ray mass-proxy relations. We verify
that our SZ effect measurements are in excellent agreement with
previous determinations from Planck data. For the present sample,
the hydrostatic X-ray masses at R<SUB>500</SUB> are on average ~ 20
percent larger than the corresponding weak lensing masses, which is
contrary to expectations. We show that the mass discrepancy is driven
by a difference in mass concentration as measured by the two methods
and, for the present sample, that the mass discrepancy and difference
in mass concentration are especially large for disturbed systems. The
mass discrepancy is also linked to the offset in centres used by the
X-ray and weak lensing analyses, which again is most important in
disturbed systems. We outline several approaches that are needed to
help achieve convergence in cluster mass measurement with X-ray and
weak lensing observations. <P />Appendices are available in electronic
form at <A href="http://www.aanda.org">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck intermediate results. II. Comparison of
Sunyaev-Zeldovich measurements from Planck and from the Arcminute
Microkelvin Imager for 11 galaxy clusters
Authors: Planck Collaboration; AMI Collaboration; Ade, P. A. R.;
Aghanim, N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.;
Balbi, A.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Battye, R.;
Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.;
Bikmaev, I.; Böhringer, H.; Bonaldi, A.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Bourdin, H.; Brown, M. L.; Bucher, M.; Burenin, R.;
Burigana, C.; Butler, R. C.; Cabella, P.; Carvalho, P.; Catalano, A.;
Cayón, L.; Chamballu, A.; Chary, R. -R.; Chiang, L. -Y.; Chon, G.;
Clements, D. L.; Colafrancesco, S.; Colombi, S.; Coulais, A.; Crill,
B. P.; Cuttaia, F.; Da Silva, A.; Dahle, H.; Davies, R. D.; Davis,
R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Démoclès, J.; Dickinson, C.; Diego, J. M.;
Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac, X.;
Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Feroz, F.; Finelli,
F.; Flores-Cacho, I.; Forni, O.; Fosalba, P.; Frailis, M.; Franceschi,
E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski,
K. M.; Grainge, K. J. B.; Gregorio, A.; Gruppuso, A.; Hansen,
F. K.; Harrison, D.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Huffenberger, K. M.; Hurier, G.; Hurley-Walker, N.; Jagemann,
T.; Juvela, M.; Keihänen, E.; Khamitov, I.; Kneissl, R.; Knoche, J.;
Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby,
A.; Lawrence, C. R.; Le Jeune, M.; Leach, S.; Leonardi, R.; Liddle,
A.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Luzzi,
G.; Macías-Pérez, J. F.; MacTavish, C. J.; Maino, D.; Mandolesi,
N.; Maris, M.; Marleau, F.; Marshall, D. J.; Martínez-González,
E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta,
P.; Meinhold, P. R.; Melchiorri, A.; Melin, J. -B.; Mendes, L.;
Mennella, A.; Mitra, S.; Miville-Deschênes, M. -A.; Montier, L.;
Morgante, G.; Munshi, D.; Naselsky, P.; Natoli, P.; Nørgaard-Nielsen,
H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Olamaie, M.; Osborne,
S.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon, G.; Pearson,
T. J.; Perdereau, O.; Perrott, Y. C.; Perrotta, F.; Piacentini, F.;
Pierpaoli, E.; Platania, P.; Pointecouteau, E.; Polenta, G.; Popa, L.;
Poutanen, T.; Pratt, G. W.; Puget, J. -L.; Rachen, J. P.; Rebolo, R.;
Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Ristorcelli,
I.; Rocha, G.; Rodríguez-Gonzálvez, C.; Rosset, C.; Rossetti, M.;
Rubiño-Martín, J. A.; Rumsey, C.; Rusholme, B.; Sandri, M.; Saunders,
R. D. E.; Savini, G.; Schammel, M. P.; Scott, D.; Shimwell, T. W.;
Smoot, G. F.; Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Sudiwala,
R.; Sunyaev, R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.;
Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Valenziano, L.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio,
N.; Wade, L. A.; Wandelt, B. D.; Yvon, D.; Zacchei, A.; Zonca, A.
2013A&A...550A.128P Altcode: 2012arXiv1204.1318P; 2013A&A...550A.128A
A comparison is presented of Sunyaev-Zeldovich measurements for
11 galaxy clusters as obtained by Planck and by the ground-based
interferometer, the Arcminute Microkelvin Imager. Assuming a universal
spherically-symmetric Generalised Navarro, Frenk and White (GNFW)
model for the cluster gas pressure profile, we jointly constrain the
integrated Compton-Y parameter (Y<SUB>500</SUB>) and the scale radius
(θ<SUB>500</SUB>) of each cluster. Our resulting constraints in
the Y<SUB>500</SUB> - θ<SUB>500</SUB> 2D parameter space derived
from the two instruments overlap significantly for eight of the
clusters, although, overall, there is a tendency for AMI to find the
Sunyaev-Zeldovich signal to be smaller in angular size and fainter
than Planck. Significant discrepancies exist for the three remaining
clusters in the sample, namely A1413, A1914, and the newly-discovered
Planck cluster PLCKESZ G139.59+24.18. The robustness of the analysis
of both the Planck and AMI data is demonstrated through the use of
detailed simulations, which also discount confusion from residual
point (radio) sources and from diffuse astrophysical foregrounds
as possible explanations for the discrepancies found. For a subset
of our cluster sample, we have investigated the dependence of our
results on the assumed pressure profile by repeating the analysis
adopting the best-fitting GNFW profile shape which best matches X-ray
observations. Adopting the best-fitting profile shape from the X-ray
data does not, in general, resolve the discrepancies found in this
subset of five clusters. Though based on a small sample, our results
suggest that the adopted GNFW model may not be sufficiently flexible
to describe clusters universally.
---------------------------------------------------------
Title: Planck intermediate results. IV. The XMM-Newton validation
programme for new Planck galaxy clusters
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.;
Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bikmaev, I.; Böhringer, H.;
Bonaldi, A.; Bond, J. R.; Borgani, S.; Borrill, J.; Bouchet, F. R.;
Brown, M. L.; Burigana, C.; Butler, R. C.; Cabella, P.; Carvalho,
P.; Catalano, A.; Cayón, L.; Chamballu, A.; Chary, R. -R.; Chiang,
L. -Y.; Chon, G.; Christensen, P. R.; Clements, D. L.; Colafrancesco,
S.; Colombi, S.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Da Silva, A.;
Dahle, H.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Zotti,
G.; Delabrouille, J.; Démoclès, J.; Désert, F. -X.; Diego, J. M.;
Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac,
X.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Flores-Cacho, I.;
Forni, O.; Frailis, M.; Franceschi, E.; Frommert, M.; Galeotta, S.;
Ganga, K.; Génova-Santos, R. T.; Giraud-Héraud, Y.; González-Nuevo,
J.; González-Riestra, R.; Górski, K. M.; Gregorio, A.; Gruppuso,
A.; Hansen, F. K.; Harrison, D.; Hempel, A.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huffenberger,
K. M.; Hurier, G.; Jaffe, A. H.; Jagemann, T.; Jones, W. C.; Juvela,
M.; Kneissl, R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio,
H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.;
Le Jeune, M.; Leach, S.; Leonardi, R.; Liddle, A.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Luzzi, G.; Macías-Pérez,
J. F.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Marleau, F.;
Marshall, D. J.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Mazzotta, P.; Mei, S.; Meinhold, P. R.; Melchiorri, A.;
Melin, J. -B.; Mendes, L.; Mennella, A.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Morgante, G.; Mortlock, D.; Munshi, D.; Naselsky,
P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.;
Osborne, S.; Pajot, F.; Paoletti, D.; Perdereau, O.; Perrotta, F.;
Piacentini, F.; Piat, M.; Pierpaoli, E.; Piffaretti, R.; Plaszczynski,
S.; Platania, P.; Pointecouteau, E.; Polenta, G.; Popa, L.; Poutanen,
T.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Rocha, G.; Rosset, C.; Rossetti, M.;
Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Scott,
D.; Smoot, G. F.; Stanford, A.; Stivoli, F.; Sudiwala, R.; Sunyaev,
R.; Sutton, D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Valenziano,
L.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Welikala, N.; Weller, J.; White, S. D. M.; Yvon, D.;
Zacchei, A.; Zonca, A.
2013A&A...550A.130P Altcode: 2012arXiv1205.3376P; 2013A&A...550A.130A
We present the final results from the XMM-Newton validation follow-up of
new Planck galaxy cluster candidates. We observed 15 new candidates,
detected with signal-to-noise ratios between 4.0 and 6.1 in the
15.5-month nominal Planck survey. The candidates were selected using
ancillary data flags derived from the ROSAT All Sky Survey (RASS)
and Digitized Sky Survey all-sky maps, with the aim of pushing into
the low SZ flux, high-z regime and testing RASS flags as indicators
of candidate reliability. Fourteen new clusters were detected by
XMM-Newton, ten single clusters and two double systems. Redshifts from
X-ray spectroscopy lie in the range 0.2 to 0.9, with six clusters
at z > 0.5. Estimated masses (M<SUB>500</SUB>) range from 2.5 ×
10<SUP>14</SUP> to 8 × 10<SUP>14</SUP> M<SUB>⊙</SUB>. We discuss
our results in the context of the full XMM-Newton validation programme,
in which 51 new clusters have been detected. This includes four double
and two triple systems, some of which are chance projections on the
sky of clusters at different redshifts. We find thatassociation with
a source from the RASS-Bright Source Catalogue is a robust indicator
of the reliability of a candidate, whereas association with a source
from the RASS-Faint Source Catalogue does not guarantee that the SZ
candidate is a bona fide cluster. Nevertheless, most Planck clusters
appear in RASS maps, with a significance greater than 2σ being
a good indication that the candidate is a real cluster. Candidate
validation from association with SDSS galaxy overdensity at z >
0.5 is also discussed. The full sample gives a Planck sensitivity
threshold of Y<SUB>500</SUB> ~ 4 × 10<SUP>-4</SUP> arcmin<SUP>2</SUP>,
with indication for Malmquist bias in the Y<SUB>X</SUB>-Y<SUB>500</SUB>
relation below this threshold. The corresponding mass threshold depends
on redshift. Systems with M<SUB>500</SUB> > 5 × 10<SUP>14</SUP>
M<SUB>⊙</SUB> at z > 0.5 are easily detectable with Planck. The
newly-detected clusters follow the Y<SUB>X</SUB>-Y<SUB>500</SUB>
relation derived from X-ray selected samples. Compared to X-ray selected
clusters, the new SZ clusters have a lower X-ray luminosity on average
for their mass. There is no indication of departure from standard
self-similar evolution in the X-ray versus SZ scaling properties. In
particular, there is no significant evolution of the Y<SUB>X</SUB> /
Y<SUB>500</SUB> ratio.
---------------------------------------------------------
Title: Planck intermediate results. VII. Statistical properties of
infrared and radio extragalactic sources from the Planck Early Release
Compact Source Catalogue at frequencies between 100 and 857 GHz
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.;
Argüeso, F.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont,
J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.;
Battaner, E.; Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli,
M.; Bethermin, M.; Bhatia, R.; Bonaldi, A.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Burigana, C.; Cabella, P.; Cardoso, J. -F.; Catalano,
A.; Cayón, L.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, L. -Y.;
Christensen, P. R.; Clements, D. L.; Colafrancesco, S.; Colombi, S.;
Colombo, L. P. L.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese,
L.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Zotti, G.;
Delabrouille, J.; Dickinson, C.; Diego, J. M.; Dole, H.; Donzelli, S.;
Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin,
T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Fosalba, P.; Frailis,
M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gregorio,
A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon,
E.; Hobson, M.; Holmes, W. A.; Jaffe, T. R.; Jaffe, A. H.; Jagemann,
T.; Jones, W. C.; Juvela, M.; Keihänen, E.; Kisner, T. S.; Kneissl,
R.; Knoche, J.; Knox, L.; Kunz, M.; Kurinsky, N.; Kurki-Suonio,
H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.;
Lawrence, C. R.; Leonardi, R.; Lilje, P. B.; López-Caniego, M.;
Macías-Pérez, J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Marshall,
D. J.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese,
S.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Mitra,
S.; Miville-Deschènes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati,
F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; Osborne, S.; Pajot, F.; Paladini, R.; Paoletti, D.;
Partridge, B.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Plaszczynski,
S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen,
T.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach,
W. T.; Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi, S.; Riller,
T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rowan-Robinson, M.;
Rubiño-Martín, J. A.; Rusholme, B.; Sajina, A.; Sandri, M.; Savini,
G.; Scott, D.; Smoot, G. F.; Starck, J. -L.; Sudiwala, R.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.;
Tomasi, M.; Tristram, M.; Tucci, M.; Türler, M.; Valenziano, L.; Van
Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt,
B. D.; White, M.; Yvon, D.; Zacchei, A.; Zonca, A.
2013A&A...550A.133P Altcode: 2012arXiv1207.4706P; 2013A&A...550A.133A
We make use of the Planck all-sky survey to derive number counts and
spectral indices of extragalactic sources - infrared and radio sources -
from the Planck Early Release Compact Source Catalogue (ERCSC) at 100
to 857 GHz (3 mm to 350 μm). Three zones (deep, medium and shallow)
of approximately homogeneous coverage are used to permit a clean and
controlled correction for incompleteness, which was explicitly not done
for the ERCSC, as it was aimed at providing lists of sources to be
followed up. Our sample, prior to the 80% completeness cut, contains
between 217 sources at 100 GHz and 1058 sources at 857 GHz over about
12 800 to 16 550 deg<SUP>2</SUP> (31 to 40% of the sky). After the
80% completeness cut, between 122 and 452 and sources remain, with
flux densities above 0.3 and 1.9 Jy at 100 and 857 GHz. The sample so
defined can be used for statistical analysis. Using the multi-frequency
coverage of the Planck High Frequency Instrument, all the sources
have been classified as either dust-dominated (infrared galaxies) or
synchrotron-dominated (radio galaxies) on the basis of their spectral
energy distributions (SED). Our sample is thus complete, flux-limited
and color-selected to differentiate between the two populations. We
find an approximately equal number of synchrotron and dusty sources
between 217 and 353 GHz; at 353 GHz or higher (or 217 GHz and lower)
frequencies, the number is dominated by dusty (synchrotron) sources,
as expected. For most of the sources, the spectral indices are also
derived. We provide for the first time counts of bright sources from 353
to 857 GHz and the contributions from dusty and synchrotron sources at
all HFI frequencies in the key spectral range where these spectra are
crossing. The observed counts are in the Euclidean regime. The number
counts are compared to previously published data (from earlier Planck
results, Herschel, BLAST, SCUBA, LABOCA, SPT, and ACT) and models taking
into account both radio or infrared galaxies, and covering a large range
of flux densities. We derive the multi-frequency Euclidean level - the
plateau in the normalised differential counts at high flux-density -
and compare it to WMAP, Spitzer and IRAS results. The submillimetre
number counts are not well reproduced by current evolution models
of dusty galaxies, whereas the millimetre part appears reasonably
well fitted by the most recent model for synchrotron-dominated
sources. Finally we provide estimates of the local luminosity density
of dusty galaxies, providing the first such measurements at 545
and 857 GHz. <P />Appendices are available in electronic form at <A
href="http://www.aanda.org">http://www.aanda.org</A>Corresponding
author: herve.dole@ias.u-psud.fr
---------------------------------------------------------
Title: Planck intermediate results. VI. The dynamical structure of
PLCKG214.6+37.0, a Planck discovered triple system of galaxy clusters
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.;
Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner,
E.; Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.;
Bhatia, R.; Bikmaev, I.; Böhringer, H.; Bonaldi, A.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Bourdin, H.; Burenin, R.; Burigana,
C.; Cabella, P.; Cardoso, J. -F.; Castex, G.; Catalano, A.; Cayón,
L.; Chamballu, A.; Chiang, L. -Y.; Chon, G.; Christensen, P. R.;
Clements, D. L.; Colafrancesco, S.; Colombi, S.; Colombo, L. P. L.;
Comis, B.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Da Silva, A.;
Dahle, H.; Danese, L.; Davis, R. J.; de Bernardis, P.; de Gasperis,
G.; de Zotti, G.; Delabrouille, J.; Démoclès, J.; Diego, J. M.;
Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.;
Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.;
Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi, E.; Frommert, M.;
Galeotta, S.; Ganga, K.; Génova-Santos, R. T.; Giard, M.; Gilfanov,
M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gregorio,
A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Heinämäki, P.; Hempel,
A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hurier, G.;
Jaffe, T. R.; Jaffe, A. H.; Jagemann, T.; Jones, W. C.; Juvela, M.;
Keihänen, E.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.;
Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.;
Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.; Leonardi,
R.; Lilje, P. B.; López-Caniego, M.; Luzzi, G.; Macías-Pérez,
J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Marleau, F.; Marshall,
D. J.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese,
S.; Mazzotta, P.; Mei, S.; Melchiorri, A.; Melin, J. -B.; Mendes,
L.; Mennella, A.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.;
Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, J. A.;
Naselsky, P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot, F.; Paoletti, D.;
Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.;
Piacentini, F.; Piat, M.; Pierpaoli, E.; Piffaretti, R.; Plaszczynski,
S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen,
T.; Pratt, G. W.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rebolo,
R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller,
T.; Ristorcelli, I.; Rocha, G.; Roman, M.; Rosset, C.; Rossetti, M.;
Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Scott,
D.; Smoot, G. F.; Starck, J. -L.; Sudiwala, R.; Sunyaev, R.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tuovinen, J.; Valenziano,
L.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Welikala, N.; Yvon, D.; Zacchei, A.; Zaroubi, S.;
Zonca, A.
2013A&A...550A.132P Altcode: 2012arXiv1207.4009P; 2013A&A...550A.132A
The survey of galaxy clusters performed by Planck through the
Sunyaev-Zeldovich effect has already discovered many interesting
objects, thanks to its full sky coverage. One of the SZ candidates
detected inthe early months of the mission near to the signal-to-noise
threshold, PLCKG214.6+37.0, was later revealed by XMM-Newton to
be a triple system of galaxy clusters. We present the results
from a deep XMM-Newton re-observation of PLCKG214.6+37.0, part
of a multi-wavelength programme to investigate Planck discovered
superclusters. The characterisation of the physical properties of the
three components has allowed us to build a template model to extract
the total SZ signal of this system with Planck data. We have partly
reconciled the discrepancy between the expected SZ signal derived from
X-rays and the observed one, which are now consistent within 1.2σ. We
measured the redshift of the three components with the iron lines in
the X-ray spectrum, and confirm that the three clumps are likely part
of the same supercluster structure. The analysis of the dynamical
state of the three components, as well as the absence of detectable
excess X-ray emission, suggests that we are witnessing the formation
of a massive cluster at an early phase of interaction.
---------------------------------------------------------
Title: Shock Heating of the Merging Galaxy Cluster A521
Authors: Bourdin, H.; Mazzotta, P.; Markevitch, M.; Giacintucci, S.;
Brunetti, G.
2013ApJ...764...82B Altcode: 2013arXiv1302.0696B
A521 is an interacting galaxy cluster located at z = 0.247, hosting a
low-frequency radio halo connected to an eastern radio relic. Previous
Chandra observations hinted at the presence of an X-ray brightness edge
at the position of the relic, which may be a shock front. We analyze a
deep observation of A521 recently performed with XMM-Newton in order to
probe the cluster structure up to the outermost regions covered by the
radio emission. The cluster atmosphere exhibits various brightness and
temperature anisotropies. In particular, two cluster cores appear to
be separated by two cold fronts. We find two shock fronts, one that was
suggested by Chandra and that is propagating to the east, and another to
the southwestern cluster outskirt. The two main interacting clusters
appear to be separated by a shock-heated region, which exhibits a
spatial correlation with the radio halo. The outer edge of the radio
relic coincides spatially with a shock front, suggesting that this
shock is responsible for the generation of cosmic-ray electrons in the
relic. The propagation direction and Mach number of the shock front
derived from the gas density jump, M = 2.4 ± 0.2, are consistent with
expectations from the radio spectral index, under the assumption of
Fermi I acceleration mechanism.
---------------------------------------------------------
Title: Planck intermediate results. V. Pressure profiles of galaxy
clusters from the Sunyaev-Zeldovich effect
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.;
Balbi, A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner,
E.; Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia,
R.; Bikmaev, I.; Bobin, J.; Böhringer, H.; Bonaldi, A.; Bond, J. R.;
Borgani, S.; Borrill, J.; Bouchet, F. R.; Bourdin, H.; Brown, M. L.;
Burenin, R.; Burigana, C.; Cabella, P.; Cardoso, J. -F.; Carvalho,
P.; Castex, G.; Catalano, A.; Cayón, L.; Chamballu, A.; Chiang,
L. -Y.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements,
D. L.; Colafrancesco, S.; Colombi, S.; Colombo, L. P. L.; Comis,
B.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Da Silva, A.; Dahle, H.;
Danese, L.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Zotti,
G.; Delabrouille, J.; Démoclès, J.; Désert, F. -X.; Diego, J. M.;
Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.;
Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli,
F.; Flores-Cacho, I.; Forni, O.; Fosalba, P.; Frailis, M.; Franceschi,
E.; Frommert, M.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.;
Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Hempel,
A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hurier, G.;
Jaffe, T. R.; Jaffe, A. H.; Jagemann, T.; Jones, W. C.; Juvela, M.;
Keihänen, E.; Khamitov, I.; Kisner, T. S.; Kneissl, R.; Knoche, J.;
Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.;
Leonardi, R.; Liddle, A.; Lilje, P. B.; López-Caniego, M.; Luzzi, G.;
Macías-Pérez, J. F.; Maino, D.; Mandolesi, N.; Maris, M.; Marleau,
F.; Marshall, D. J.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Mazzotta, P.; Mei, S.; Melchiorri, A.; Melin, J. -B.;
Mendes, L.; Mennella, A.; Mitra, S.; Miville-Deschênes, M. -A.;
Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.;
Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Nørgaard-Nielsen,
H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot, F.;
Paoletti, D.; Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Piffaretti,
R.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.;
Popa, L.; Poutanen, T.; Pratt, G. W.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Roman, M.; Rosset, C.; Rossetti, M.; Rubiño-Martín, J. A.;
Rusholme, B.; Sandri, M.; Savini, G.; Scott, D.; Smoot, G. F.;
Starck, J. -L.; Sudiwala, R.; Sunyaev, R.; Sutton, D.; Suur-Uski,
A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.;
Tomasi, M.; Tristram, M.; Tuovinen, J.; Valenziano, L.; Van Tent, B.;
Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt,
B. D.; Welikala, N.; White, S. D. M.; White, M.; Yvon, D.; Zacchei,
A.; Zonca, A.
2013A&A...550A.131P Altcode: 2013A&A...550A.131A; 2012arXiv1207.4061P
Taking advantage of the all-sky coverage and broadfrequency range
of the Planck satellite, we study the Sunyaev-Zeldovich (SZ) and
pressure profiles of 62 nearby massive clusters detected at high
significance in the 14-month nominal survey. Careful reconstruction of
the SZ signal indicates that most clusters are individually detected
at least out to R<SUB>500</SUB>. By stacking the radial profiles,
we have statistically detected the radial SZ signal out to 3 ×
R<SUB>500</SUB>, i.e., at a density contrast of about 50-100, though
the dispersion about the mean profile dominates the statistical
errors across the whole radial range. Our measurement is fully
consistent with previous Planck results on integrated SZ fluxes,
further strengthening the agreement between SZ and X-ray measurements
inside R<SUB>500</SUB>. Correcting for the effects of the Planck
beam, we have calculated the corresponding pressure profiles. This
new constraint from SZ measurements is consistent with the X-ray
constraints from XMM-Newton in the region in which the profiles overlap
(i.e., [0.1-1] R<SUB>500</SUB>), and is in fairly good agreement with
theoretical predictions within the expected dispersion. At larger
radii the average pressure profile is slightly flatter than most
predictions from numerical simulations. Combining the SZ and X-ray
observed profiles into a joint fit to a generalised pressure profile
gives best-fit parameters [P<SUB>0</SUB>,c<SUB>500</SUB>,γ,α,β ]
= [6.41,1.81,0.31,1.33,4.13 ] . Using a reasonable hypothesis for
the gas temperature in the cluster outskirts we reconstruct from
our stacked pressure profile the gas mass fraction profile out to 3
R<SUB>500</SUB>. Within the temperature driven uncertainties, our Planck
constraints are compatible with the cosmic baryon fraction and expected
gas fraction in halos. <P />Appendices are available in electronic
form at <A href="http://www.aanda.org">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck intermediate results. VIII. Filaments between
interacting clusters
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.;
Balbi, A.; Banday, A. J.; Barreiro, R. B.; Battaner, J. G. Bartlett E.;
Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.;
Bikmaev, I.; Böhringer, H.; Bonaldi, A.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Bourdin, H.; Burenin, R.; Burigana, C.; Cabella, P.;
Cardoso, J. -F.; Castex, G.; Catalano, A.; Cayón, L.; Chamballu, A.;
Chary, R. -R.; Chiang, L. -Y.; Chon, G.; Christensen, P. R.; Clements,
D. L.; Colafrancesco, S.; Colombo, L. P. L.; Comis, B.; Coulais, A.;
Crill, B. P.; Cuttaia, F.; Danese, L.; Davis, R. J.; de Bernardis,
P.; de Gasperis, G.; de Zotti, G.; Delabrouille, J.; Démoclès, J.;
Désert, F. -X.; Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.;
Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin,
T. A.; Eriksen, H. K.; Finelli, F.; Flores-Cacho, I.; Forni, O.;
Frailis, M.; Franceschi, E.; Frommert, M.; Ganga, K.; Génova-Santos,
T.; Giard, M.; Gilfanov, M.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison,
D.; Hempel, A.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hovest, W.; Hurier, G.; Jaffe, T. R.; Jaffe, A. H.; Jagemann,
T.; Jones, W. C.; Juvela, M.; Khamitov, I.; Kisner, T. S.; Kneissl,
R.; Knoche, J.; Knox, L.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.;
Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.; Le Jeune, M.; Leonardi,
R.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Luzzi, G.; Macías-Pérez, J. F.; Maffei, B.; Maino, D.; Mandolesi,
N.; Maris, M.; Marleau, F.; Marshall, D. J.; Martínez-González, E.;
Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Mei,
S.; Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella, A.; Mitra,
S.; Miville-Deschènes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.;
Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.;
Osborne, S.; Pajot, F.; Paoletti, D.; Pasian, F.; Patanchon, G.;
Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.;
Pierpaoli, E.; Piffaretti, R.; Plaszczynski, S.; Pointecouteau, E.;
Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.;
Remazeilles, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli,
I.; Rocha, G.; Roman, M.; Rosset, C.; Rossetti, M.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Savini, G.; Schaefer, B. M.; Scott,
D.; Smoot, G. F.; Starck, J. -L.; Sudiwala, R.; Sunyaev, R.; Sutton,
D.; Suur-Uski, A. -S.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Valenziano,
L.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Welikala, N.; White, S. D. M.; Yvon, D.; Zacchei,
A.; Zonca, A.
2013A&A...550A.134P Altcode: 2013A&A...550A.134A; 2012arXiv1208.5911P
Context. About half of the baryons of the Universe are expected to
be in the form of filaments of hot and low-density intergalactic
medium. Most of these baryons remain undetected even by the most
advanced X-ray observatories, which are limited in sensitivity to
the diffuse low-density medium. <BR /> Aims: The Planck satellite
has provided hundreds of detections of the hot gas in clusters of
galaxies via the thermal Sunyaev-Zel'dovich (tSZ) effect and is an
ideal instrument for studying extended low-density media through
the tSZ effect. In this paper we use the Planck data to search for
signatures of a fraction of these missing baryons between pairs of
galaxy clusters. <BR /> Methods: Cluster pairs are good candidates for
searching for the hotter and denser phase of the intergalactic medium
(which is more easily observed through the SZ effect). Using an X-ray
catalogue of clusters and the Planck data, we selected physical pairs of
clusters as candidates. Using the Planck data, we constructed a local
map of the tSZ effect centred on each pair of galaxy clusters. ROSAT
data were used to construct X-ray maps of these pairs. After modelling
and subtracting the tSZ effect and X-ray emission for each cluster in
the pair, we studied the residuals on both the SZ and X-ray maps. <BR
/> Results: For the merging cluster pair A399-A401 we observe a
significant tSZ effect signal in the intercluster region beyond the
virial radii of the clusters. A joint X-ray SZ analysis allows us to
constrain the temperature and density of this intercluster medium. We
obtain a temperature of kT = 7.1 ± 0.9 keV (consistent with previous
estimates) and a baryon density of (3.7 ± 0.2) × 10<SUP>-4</SUP>
cm<SUP>-3</SUP>. <BR /> Conclusions: The Planck satellite mission has
provided the first SZ detection of the hot and diffuse intercluster gas.
---------------------------------------------------------
Title: Testing Galaxy Formation Models: Characterizing Extended Hot
X-ray Coronae Around Massive Spiral Galaxies
Authors: Bogdan, Akos; Forman, W. R.; Bourdin, H.; Crain, R. A.;
Sijacki, D.; Vogelsberger, M.; Kraft, R. P.; Jones, C.; David, L. P.;
Churazov, E.; Gilfanov, M.; Mazzotta, P.
2013AAS...22131306B Altcode:
The presence of hot gaseous coronae in the dark matter halos of massive
galaxies is a basic prediction of galaxy formation models. Theoretical
models predict copious X-ray emission at large radii around massive
spiral galaxies. We have studied two galaxies, NGC1961 and NGC6753,
that are optically luminous and massive, with moderate star formation
rates, and that can be probed to sufficiently large radii. For these
two galaxies we detect emission with sufficient counts to measure
X-ray gas temperatures and gas abundances. Hence, for the first time,
we are able to characterize the properties - X-ray luminosity, gas
temperature, elemental abundance, gas density, and gas mass - of hot
coronae in normal spiral galaxies.
---------------------------------------------------------
Title: Observational Evidences of a Clear Connection Between Radio
Mini-Halos and Core Gas Sloshing in Clusters of Galaxies
Authors: Mazzotta, Pasquale
2013cfgc.confE...8M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: A comparison of algorithms for the construction of SZ cluster
catalogues
Authors: Melin, J. -B.; Aghanim, N.; Bartelmann, M.; Bartlett, J. G.;
Betoule, M.; Bobin, J.; Carvalho, P.; Chon, G.; Delabrouille, J.;
Diego, J. M.; Harrison, D. L.; Herranz, D.; Hobson, M.; Kneissl, R.;
Lasenby, A. N.; Le Jeune, M.; Lopez-Caniego, M.; Mazzotta, P.; Rocha,
G. M.; Schaefer, B. M.; Starck, J. -L.; Waizmann, J. C.; Yvon, D.
2012A&A...548A..51M Altcode: 2012arXiv1210.1416M
We evaluate the construction methodology of an all-sky catalogue
of galaxy clusters detected through the Sunyaev-Zel'dovich (SZ)
effect. We perform an extensive comparison of twelve algorithms applied
to the same detailed simulations of the millimeter and submillimeter
sky based on a Planck-like case. We present the results of this "SZ
Challenge" in terms of catalogue completeness, purity, astrometric
and photometric reconstruction. Our results provide a comparison of
a representative sample of SZ detection algorithms and highlight
important issues in their application. In our study case, we show
that the exact expected number of clusters remains uncertain (about
a thousand cluster candidates at |b| > 20 deg with 90% purity) and
that it depends on the SZ model and on the detailed sky simulations,
and on algorithmic implementation of the detection methods. We also
estimate the astrometric precision of the cluster candidates which
is found of the order of ~2 arcmin on average, and the photometric
uncertainty of about 30%, depending on flux.
---------------------------------------------------------
Title: ORIGIN: metal creation and evolution from the cosmic dawn
Authors: den Herder, Jan-Willem; Piro, Luigi; Ohashi, Takaya;
Kouveliotou, Chryssa; Hartmann, Dieter H.; Kaastra, Jelle S.; Amati,
L.; Andersen, M. I.; Arnaud, M.; Attéia, J. -L.; Bandler, S.;
Barbera, M.; Barcons, X.; Barthelmy, S.; Basa, S.; Basso, S.; Boer,
M.; Branchini, E.; Branduardi-Raymont, G.; Borgani, S.; Boyarsky, A.;
Brunetti, G.; Budtz-Jorgensen, C.; Burrows, D.; Butler, N.; Campana,
S.; Caroli, E.; Ceballos, M.; Christensen, F.; Churazov, E.; Comastri,
A.; Colasanti, L.; Cole, R.; Content, R.; Corsi, A.; Costantini, E.;
Conconi, P.; Cusumano, G.; de Plaa, J.; De Rosa, A.; Del Santo, M.;
Di Cosimo, S.; De Pasquale, M.; Doriese, R.; Ettori, S.; Evans, P.;
Ezoe, Y.; Ferrari, L.; Finger, H.; Figueroa-Feliciano, T.; Friedrich,
P.; Fujimoto, R.; Furuzawa, A.; Fynbo, J.; Gatti, F.; Galeazzi, M.;
Gehrels, N.; Gendre, B.; Ghirlanda, G.; Ghisellini, G.; Gilfanov, M.;
Giommi, P.; Girardi, M.; Grindlay, J.; Cocchi, M.; Godet, O.; Guedel,
M.; Haardt, F.; den Hartog, R.; Hepburn, I.; Hermsen, W.; Hjorth, J.;
Hoekstra, H.; Holland, A.; Hornstrup, A.; van der Horst, A.; Hoshino,
A.; in't Zand, J.; Irwin, K.; Ishisaki, Y.; Jonker, P.; Kitayama, T.;
Kawahara, H.; Kawai, N.; Kelley, R.; Kilbourne, C.; de Korte, P.;
Kusenko, A.; Kuvvetli, I.; Labanti, M.; Macculi, C.; Maiolino, R.;
Hesse, M. Mas; Matsushita, K.; Mazzotta, P.; McCammon, D.; Méndez,
M.; Mignani, R.; Mineo, T.; Mitsuda, K.; Mushotzky, R.; Molendi, S.;
Moscardini, L.; Natalucci, L.; Nicastro, F.; O'Brien, P.; Osborne,
J.; Paerels, F.; Page, M.; Paltani, S.; Pedersen, K.; Perinati, E.;
Ponman, T.; Pointecouteau, E.; Predehl, P.; Porter, S.; Rasmussen, A.;
Rauw, G.; Röttgering, H.; Roncarelli, M.; Rosati, P.; Quadrini, E.;
Ruchayskiy, O.; Salvaterra, R.; Sasaki, S.; Sato, K.; Savaglio, S.;
Schaye, J.; Sciortino, S.; Shaposhnikov, M.; Sharples, R.; Shinozaki,
K.; Spiga, D.; Sunyaev, R.; Suto, Y.; Takei, Y.; Tanvir, N.; Tashiro,
M.; Tamura, T.; Tawara, Y.; Troja, E.; Tsujimoto, M.; Tsuru, T.;
Ubertini, P.; Ullom, J.; Ursino, E.; Verbunt, F.; van de Voort, F.;
Viel, M.; Wachter, S.; Watson, D.; Weisskopf, M.; Werner, N.; White,
N.; Willingale, R.; Wijers, R.; Yamasaki, N.; Yoshikawa, K.; Zane, S.
2012ExA....34..519D Altcode: 2011ExA...tmp...50D; 2011arXiv1104.2048D; 2011ExA...tmp...20D;
2011ExA...tmp...30D
ORIGIN is a proposal for the M3 mission call of ESA aimed at the study
of metal creation from the epoch of cosmic dawn. Using high-spectral
resolution in the soft X-ray band, ORIGIN will be able to identify
the physical conditions of all abundant elements between C and Ni to
red-shifts of z = 10, and beyond. The mission will answer questions
such as: When were the first metals created? How does the cosmic metal
content evolve? Where do most of the metals reside in the Universe? What
is the role of metals in structure formation and evolution? To reach
out to the early Universe ORIGIN will use Gamma-Ray Bursts (GRBs) to
study their local environments in their host galaxies. This requires
the capability to slew the satellite in less than a minute to the
GRB location. By studying the chemical composition and properties
of clusters of galaxies we can extend the range of exploration to
lower redshifts ( z ∼0.2). For this task we need a high-resolution
spectral imaging instrument with a large field of view. Using the
same instrument, we can also study the so far only partially detected
baryons in the Warm-Hot Intergalactic Medium (WHIM). The less dense
part of the WHIM will be studied using absorption lines at low redshift
in the spectra for GRBs. The ORIGIN mission includes a Transient Event
Detector (coded mask with a sensitivity of 0.4 photon/cm<SUP>2</SUP>/s
in 10 s in the 5-150 keV band) to identify and localize 2000 GRBs over
a five year mission, of which ∼65 GRBs have a redshift >7. The
Cryogenic Imaging Spectrometer, with a spectral resolution of 2.5 eV,
a field of view of 30 arcmin and large effective area below 1 keV
has the sensitivity to study clusters up to a significant fraction
of the virial radius and to map the denser parts of the WHIM (factor
30 higher than achievable with current instruments). The payload is
complemented by a Burst InfraRed Telescope to enable onboard red-shift
determination of GRBs (hence securing proper follow up of high-z bursts)
and also probes the mildly ionized state of the gas. Fast repointing is
achieved by a dedicated Controlled Momentum Gyro and a low background
is achieved by the selected low Earth orbit.
---------------------------------------------------------
Title: X-ray concentration-mass relation: theory and observations
Authors: Rasia, Elena; Meneghetti, Massimo; Mazzotta; Ettori, Stefano;
Borgani, Stefano
2012hcxa.confE..53R Altcode:
The concentration-mass relation represents a valuable tool to constrain
cosmological parameters such as matter density and sigma_8. In the
last few years, X-ray data led to the conclusion that the observed
relation has higher normalization and slope than those predicted
by dark matter only simulations. In this work, we explore whether
this disagreement is real or artificially due to an unfair comparison
between the two approaches. To this purpose, we consider ~50 clusters
simulated by progressively increasing the simulation complexity:
(i) dark-matter only, (ii) non-radiative hydrodynamics, (iii) adding
cooling, star-formation and feedback by Supernovae, (iv) adding
feedback by AGN. We produced X-ray synthetic catalogues to derive the
concentration-mass relation following an observational approach. We find
that even if cooling has the effect of steepening the concentration-
mass relation with respect to the DM-only simulations, the introduction
of AGN makes this difference small. A larger variation is expected when
reducing the radial range over which density profiles are fitted to a
NFW profile. In particular if the external radius is about half R500
the slope can double its value. Therefore, observations, suffering from
background contamination, are more inclined to detect a steeper c-M
relations. Finally, we analyze the effect of X-ray selection function
using an X-ray synthetic catalogue. We conclude by indicating the best
strategy to follow to conduct a fair theory-observation comparison
and to lead an observational campaign.
---------------------------------------------------------
Title: PSM: Planck Sky Model
Authors: Ashdown, Mark; Aumont, Jonathan; Baccigalupi, Carlo; Banday,
Anthony; Basak, Soumen; Bernard, Jean-Philippe; Betoule, Marc; Bouchet,
François; Castex, Guillaume; Clements, Dave; Da Silva, Antonio;
De Zotti, Gianfranco; Delabrouille, Jacques; Dickinson, Clive; Dodu,
Fabrice; Dolag, Klaus; Elsner, Franz; Fauvet, Lauranne; Faÿ, Gilles;
Giardino, Giovanna; Gonzalez-Nuevo, Joaquin; le Jeune, Maude; Leach,
Samuel; Lesgourgues, Julien; Liguori, Michele; Macias, Juan; Massardi,
Marcella; Matarrese, Sabino; Mazzotta, Pasquale; Melin, Jean-Baptiste;
Miville-Deschênes, Marc-Antoine; Montier, Ludovic; Mottet, Sylvain;
Paladini, Roberta; Partridge, Bruce; Piffaretti, Rocco; Prézeau,
Gary; Prunet, Simon; Ricciardi, Sara; Roman, Matthieu; Schaefer,
Bjorn; Toffolatti, Luigi
2012ascl.soft08005A Altcode:
The Planck Sky Model (PSM) is a global representation of the
multi-component sky at frequencies ranging from a few GHz to a few
THz. It summarizes in a synthetic way as much of our present knowledge
as possible of the GHz sky. PSM is a complete and versatile set of
programs and data that can be used for the simulation or the prediction
of sky emission in the frequency range of typical CMB experiments, and
in particular of the Planck sky mission. It was originally developed
as part of the activities of Planck component separation Working Group
(or "Working Group 2" - WG2), and of the ADAMIS team at APC. <P />PSM
gives users the opportunity to investigate the model in some depth:
look at its parameters, visualize its predictions for all individual
components in various formats, simulate sky emission compatible with
a given parameter set, and observe the modeled sky with a synthetic
instrument. In particular, it makes possible the simulation of sky
emission maps as could be plausibly observed by Planck or other CMB
experiments that can be used as inputs for the development and testing
of data processing and analysis techniques.
---------------------------------------------------------
Title: LoCuSS: The Sunyaev-Zel'dovich Effect and Weak-lensing Mass
Scaling Relation
Authors: Marrone, Daniel P.; Smith, Graham P.; Okabe, Nobuhiro;
Bonamente, Massimiliano; Carlstrom, John E.; Culverhouse, Thomas L.;
Gralla, Megan; Greer, Christopher H.; Hasler, Nicole; Hawkins, David;
Hennessy, Ryan; Joy, Marshall; Lamb, James W.; Leitch, Erik M.;
Martino, Rossella; Mazzotta, Pasquale; Miller, Amber; Mroczkowski,
Tony; Muchovej, Stephen; Plagge, Thomas; Pryke, Clem; Sanderson,
Alastair J. R.; Takada, Masahiro; Woody, David; Zhang, Yuying
2012ApJ...754..119M Altcode: 2011arXiv1107.5115M
We present the first weak-lensing-based scaling relation between galaxy
cluster mass, M <SUB>WL</SUB>, and integrated Compton parameter Y
<SUB>sph</SUB>. Observations of 18 galaxy clusters at z ~= 0.2 were
obtained with the Subaru 8.2 m telescope and the Sunyaev-Zel'dovich
Array. The M <SUB>WL</SUB>-Y <SUB>sph</SUB> scaling relations,
measured at Δ = 500, 1000, and 2500 ρ<SUB> c </SUB>, are consistent
in slope and normalization with previous results derived under the
assumption of hydrostatic equilibrium (HSE). We find an intrinsic
scatter in M <SUB>WL</SUB> at fixed Y <SUB>sph</SUB> of 20%, larger
than both previous measurements of M <SUB>HSE</SUB>-Y <SUB>sph</SUB>
scatter as well as the scatter in true mass at fixed Y <SUB>sph</SUB>
found in simulations. Moreover, the scatter in our lensing-based
scaling relations is morphology dependent, with 30%-40% larger M
<SUB>WL</SUB> for undisturbed compared to disturbed clusters at
the same Y <SUB>sph</SUB> at r <SUB> 500</SUB>. Further examination
suggests that the segregation may be explained by the inability of
our spherical lens models to faithfully describe the three-dimensional
structure of the clusters, in particular, the structure along the line
of sight. We find that the ellipticity of the brightest cluster galaxy,
a proxy for halo orientation, correlates well with the offset in mass
from the mean scaling relation, which supports this picture. This
provides empirical evidence that line-of-sight projection effects are
an important systematic uncertainty in lensing-based scaling relations.
---------------------------------------------------------
Title: Planck intermediate results. I. Further validation of new
Planck clusters with XMM-Newton
Authors: Planck Collaboration; Aghanim, N.; Arnaud, M.; Ashdown, M.;
Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday,
A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed,
K.; Bernard, J. -P.; Bersanelli, M.; Böhringer, H.; Bonaldi, A.;
Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bourdin, H.; Brown, M. L.;
Burigana, C.; Butler, R. C.; Cabella, P.; Cardoso, J. -F.; Carvalho,
P.; Catalano, A.; Cayón, L.; Chamballu, A.; Chary, R. -R.; Chiang,
L. -Y.; Chon, G.; Christensen, P. R.; Clements, D. L.; Colafrancesco,
S.; Colombi, S.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Da Silva, A.;
Dahle, H.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Zotti,
G.; Delabrouille, J.; Démoclès, J.; Désert, F. -X.; Diego, J. M.;
Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac,
X.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Flores-Cacho, I.;
Forni, O.; Fosalba, P.; Frailis, M.; Fromenteau, S.; Galeotta, S.;
Ganga, K.; Génova-Santos, R. T.; Giard, M.; González-Nuevo, J.;
González-Riestra, R.; Górski, K. M.; Gregorio, A.; Gruppuso, A.;
Hansen, F. K.; Harrison, D.; Hempel, A.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hornstrup, A.; Huffenberger,
K. M.; Hurier, G.; Jagemann, T.; Jasche, J.; Juvela, M.; Keihänen,
E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Knox, L.;
Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.;
Lasenby, A.; Lawrence, C. R.; Leach, S.; Leonardi, R.; Liddle, A.;
Lilje, P. B.; López-Caniego, M.; Luzzi, G.; Macías-Pérez, J. F.;
Maino, D.; Mandolesi, N.; Mann, R.; Marleau, F.; Marshall, D. J.;
Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Melin,
J. -B.; Mendes, L.; Mennella, A.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Naselsky,
P.; Natoli, P.; Nørgaard-Nielsen, H. U.; Noviello, F.; Osborne, S.;
Pasian, F.; Patanchon, G.; Perdereau, O.; Perrotta, F.; Piacentini,
F.; Pierpaoli, E.; Plaszczynski, S.; Platania, P.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Pratt, G. W.;
Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Rossetti, M.; Rubiño-Martín, J. A.; Rusholme, B.;
Sandri, M.; Savini, G.; Schaefer, B. M.; Scott, D.; Smoot, G. F.;
Starck, J. -L.; Stivoli, F.; Sunyaev, R.; Sutton, D.; Sygnet, J. -F.;
Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram,
M.; Valenziano, L.; Van Tent, B.; Vielva, P.; Villa, F.; Vittorio,
N.; Wandelt, B. D.; Weller, J.; White, S. D. M.; Yvon, D.; Zacchei,
A.; Zonca, A.
2012A&A...543A.102P Altcode: 2011arXiv1112.5595T; 2011arXiv1112.5595P
We present further results from the ongoing XMM-Newton validation
follow-up of Planck cluster candidates, detailing X-ray observations of
eleven candidates detected at a signal-to-noise ratio of 4.5 < S/N
< 5.3 in the same 10-month survey maps used in the construction of
the Early SZ sample. The sample was selected in order to test internal
SZ quality flags, and the pertinence of these flags is discussed
in light of the validation results. Ten of the candidates are found
to be bona fide clusters lying below the RASS flux limit. Redshift
estimates are available for all confirmed systems via X-ray Fe-line
spectroscopy. They lie in the redshift range 0.19 < z < 0.94,
demonstrating Planck’s capability to detect clusters up to high z. The
X-ray properties of the new clusters appear to be similar to previous
new detections by Planck at lower z and higher SZ flux: the majority
are X-ray underluminous for their mass, estimated using Y<SUB>X</SUB>
as mass proxy, and many have a disturbed morphology. We find tentative
indication for Malmquist bias in the Y<SUB>SZ</SUB>-Y<SUB>X</SUB>
relation, with a turnover at Y<SUB>SZ</SUB> ~ 4 × 10<SUP>-4</SUP>
arcmin<SUP>2</SUP>. We present additional new optical redshift
determinations with ENO and ESO telescopes of candidates previously
confirmed with XMM-Newton. The X-ray and optical redshifts for a
total of 20 clusters are found to be in excellent agreement. We also
show that useful lower limits can be put on cluster redshifts using
X-ray data only via the use of the Y<SUB>X</SUB> vs. Y<SUB>SZ</SUB>
and X-ray flux F<SUB>X</SUB> vs. Y<SUB>SZ</SUB> relations.
---------------------------------------------------------
Title: Lensing and x-ray mass estimates of clusters (simulations)
Authors: Rasia, E.; Meneghetti, M.; Martino, R.; Borgani, S.; Bonafede,
A.; Dolag, K.; Ettori, S.; Fabjan, D.; Giocoli, C.; Mazzotta, P.;
Merten, J.; Radovich, M.; Tornatore, L.
2012NJPh...14e5018R Altcode: 2012arXiv1201.1569R
We present a comparison between weak-lensing and x-ray mass estimates
of a sample of numerically simulated clusters. The sample consists of
the 20 most massive objects at redshift z = 0.25 and M<SUB>vir</SUB>
> 5 × 10<SUP>14</SUP>M<SUB>⊙</SUB> h<SUP>-1</SUP>. They
were found in a cosmological simulation of volume 1 h<SUP>-3</SUP>
Gpc<SUP>3</SUP>, evolved in the framework of a WMAP-7 normalized
cosmology. Each cluster has been resimulated at higher resolution and
with more complex gas physics. We processed it through Skylens and
X-MAS to generate optical and x-ray mock observations along three
orthogonal projections. The final sample consists of 60 cluster
realizations. The optical simulations include lensing effects on
background sources. Standard observational tools and methods of analysis
are used to recover the mass profiles of each cluster projection from
the mock catalogue. The resulting mass profiles from lensing and x-ray
are individually compared to the input mass distributions. Given the
size of our sample, we could also investigate the dependence of the
results on cluster morphology, environment, temperature inhomogeneity
and mass. We confirm previous results showing that lensing masses
obtained from the fit of the cluster tangential shear profiles with
Navarro-Frenk-White functionals are biased low by ∼5-10% with a
large scatter (∼10-25%). We show that scatter could be reduced
by optimally selecting clusters either having regular morphology or
living in substructure-poor environment. The x-ray masses are biased
low by a large amount (∼25-35%), evidencing the presence of both
non-thermal sources of pressure in the intra-cluster medium (ICM)
and temperature inhomogeneity, but they show a significantly lower
scatter than weak-lensing-derived masses. The x-ray mass bias grows
from the inner to the outer regions of the clusters. We find that both
biases are weakly correlated with the third-order power ratio, while a
stronger correlation exists with the centroid shift. Finally, the x-ray
bias is strongly connected with temperature inhomogeneities. Comparison
with a previous analysis of simulations leads to the conclusion that
the values of x-ray mass bias from simulations are still uncertain,
showing dependences on the ICM physical treatment and, possibly,
on the hydrodynamical scheme adopted.
---------------------------------------------------------
Title: Planck Intermediate Paper: Physics Of The Hot Gas In The
Coma Cluster
Authors: Mazzotta, Pasquale; Planck Collaboration
2012AAS...22050705M Altcode:
We present the data analysis of the Coma Cluster observed via
Sunyaev-Zeldovich effect with the Planck satellite. <P />Being a low
redshift massive hot clusters, its angular size is so extended that
Planck can resolve it spatially. Thanks to its great sensitivity,
Planck is capable, for the first time, to detect SZ emission up
to r 3-4 t R500. This allow us to study the pressure distribution
of the Intracluster Medium to the outermost cluster regions, not
yet achieved by any other instrument. We test the validity of some
pressure models proposed to described the pressure distribution
in clusters. In particular we find that the Arnuad et al. pressure
profile for merging systems provides a good fit of the data only at
r<R500: at larger radii it seems to underestimate the observed
profile up to 20%. This may either indicate that at these larger radii
i) the cluster profile is contaminated by unresolved SZ sources along
the line of sight ii) the pressure profile of Coma is higher than the
mean pressure profile predicted by simulations. Very interestingly the
Planck image shows two abrupt variations of the y signal located at
approx 33 arcmin to the west and to the south east with respect to the
cluster center. Using Planck y profiles extracted from corresponding
sectors we verified that both abrupt variations are compatible with
the presence of discontinuities of in the underlying density profile
and we find pressure jumps of 4.5 and 4.9 in the west and south east,
respectively. <P />Finally, we find that the y and radio-synchrotron
signals are quasi-linearly correlated on Mpc-scales with very small
intrinsic scatter. This implies either that the energy density of
cosmic-ray electrons is relatively constant throughout the cluster,
or that the magnetic fields fall off much slower with radius than
previously thought.
---------------------------------------------------------
Title: NIKA: A High-Resolution Millimetre Camera for the IRAM 30m
Telescope
Authors: Desert, F. Xavier; Mazzotta, P.; NIKA, C.
2012AAS...22013204D Altcode:
A consortium of European laboratories lead by Alain Benoit
(CNRS-Institut Néel, Grenoble) is building a new continuum dual-band
camera for the IRAM 30m telescope. It will map the sky simultaneously
at 150 and 230 GHz (2 and 1.3 mm), with an angular resolution of 15 and
10 arcseconds and a field-of-view of 6.5 arcminutes in diameter. It
is based on new Kinetic Inductance Detector arrays (1000 pixels at
2 mm, 3000 at 1.3 mm) cooled to 100 mK. It will provide in 2015 a
high-resolution ground-based follow-up of the numerous clusters of
galaxies detected with the SZ effect by the Planck satellite and ACT
at the same frequency (150 GHz). A prototype camera is already being
tested that provides a sensitivity for the y compton parameter of
about 1E-5 (1 sigma, 1 hour, 1 beam).
---------------------------------------------------------
Title: VizieR Online Data Catalog: Planck early results. VIII. ESZ
sample. (Planck+, 2011)
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Baker, M.; Balbi,
A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.;
Benabed, K.; Bennett, K.; Benoit, A.; Bernard, J. -P.; Bersanelli,
M.; Bhatia, R.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Bradshaw, T.; Bremer, M.; Bucher, M.; Burigana, C.;
Butler, R. C.; Cabella, P.; Cantalupo, C. M.; Cappellini, B.; Cardoso,
J. -F.; Carr, R.; Casale, M.; Catalano, A.; Cayon, L.; Challinor, A.;
Chamballu, A.; Charra, J.; Chary, R. -R.; Chiang, L. -Y.; Chiang,
C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.;
Coulais, A.; Crill, B. P.; Crone, G.; Crook, M.; Cuttaia, F.; Danese,
L.; D'Arcangelo, O.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de
Bruin, J.; de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille,
J.; Delouis, J. -M.; Desert, F. -X.; Dick, J.; Dickinson, C.; Dolag,
K.; Dole, H.; Donzelli, S.; Dore, O.; Doerl, U.; Douspis, M.; Dupac,
X.; Efstathiou, G.; Ensslin, T. A.; Eriksen, H. K.; Finelli, F.; Foley,
S.; Forni, O.; Fosalba, P.; Frailis, M.; Franceschi, E.; Freschi, M.;
Gaier, T. C.; Galeotta, S.; Gallegos, J.; Gandolfo, B.; Ganga, K.;
Giard, M.; Giardino, G.; Gienger, G.; Giraud-Heraud, Y.; Gonzalez,
J.; Gonzalez-Nuevo, J.; Gorski, K. M.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Guyot, G.; Haissinski, J.; Hansen, F. K.; Harrison, D.;
Helou, G.; Henrot-Versille, S.; Hernandez-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.;
Jagemann, T.; Jones, W. C.; Juillet, J. J.; Juvela, M.; Kangaslahti,
P.; Keihaenen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knox,
L.; Krassenburg, M.; Kurki-Suonio, H.; Lagache, G.; Laehteenmaeki,
A.; Lamarre, J. -M.; Lange, A. E.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leach, S.; Leahy, J. P.; Leonardi, R.; Leroy, C.;
Lilje, P. B.; Linden-Vornle, M.; Lopez-Caniego, M.; Lowe, S.; Lubin,
P. M.; Macias-Perez, J. F.; Maciaszek, T.; Mactavish, C. J.; Maffei,
B.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Martinez-Gonzalez,
E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.;
McDonald, A.; McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Melin,
J. -B.; Mendes, L.; Mennella, A.; Mevi, C.; Miniscalco, R.; Mitra,
S.; Miville-Deschenes, M. -A.; Moneti, A.; Montier, L.; Morgante, G.;
Morisset, N.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.;
Natoli, P.; Netterfield, C. B.; Norgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Ortiz, I.; Osborne,
S.; Osuna, P.; Oxborrow, C. A.; Pajot, F.; Paladini, R.; Partridge,
B.; Pasian, F.; Passvogel, T.; Patanchon, G.; Pearson, D.; Pearson,
T. J.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Plaszczynski, S.; Platania, P.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Prezeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Reix, J. -M.; Renault, C.; Ricciardi, S.; Riller,
T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rowan-Robinson,
M.; Rubino-Martin, J. A.; Rusholme, B.; Salerno, E.; Sandri, M.;
Santos, D.; Savini, G.; Schaefer, B. M.; Scott, D.; Seiffert, M. D.;
Shellard, P.; Simonetto, A.; Smoot, G. F.; Sozzi, C.; Starck, J. -L.;
Sternberg, J.; Stivoli, F.; Stolyarov, V.; Stompor, R.; Stringhetti,
L.; Sudiwala, R.; Sunyaev, R.; Sygnet, J. -F.; Tapiador, D.; Tauber,
J. A.; Tavagnacco, D.; Taylor, D.; Terenzi, L.; Texier, D.; Toffolatti,
L.; Tomasi, M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Tuerler,
M.; Tuttlebee, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Varis,
J.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Watson, C.; White, S. D. M.; White, M.; Wilkinson,
A.; Yvon, D.; Zacchei, A.; Zonca, A.
2012yCat..35360008P Altcode: 2012yCat..35369008P
We present the first all-sky sample of galaxy clusters detected
blindly by the Planck satellite through the Sunyaev-Zeldovich (SZ)
effect from its six highest frequencies. This early SZ (ESZ) sample
is comprised of 189 candidates, which have a high signal-to-noise
ratio ranging from 6 to 29. Its high reliability (purity above 95%)
is further ensured by an extensive validation process based on Planck
internal quality assessments and by external cross-identification
and follow-up observations. Planck provides the first measured SZ
signal for about 80% of the 169 previously-known ESZ clusters. Planck
furthermore releases 30 new cluster candidates, amongst which 20 meet
the ESZ signal-to-noise selection criterion. At the submission date,
twelve of the 20 ESZ candidates were confirmed as new clusters, with
eleven confirmed using XMM-Newton snapshot observations, most of them
with disturbed morphologies and low luminosities. The ESZ clusters
are mostly at moderate redshifts (86% with z below 0.3) and span more
than a decade in mass, up to the rarest and most massive clusters with
masses above 1x10<SUP>15</SUP>M<SUB>⊙</SUB>. <P />(1 data file).
---------------------------------------------------------
Title: Unveiling the Most Massive Clusters at z>0.5 with Planck
and XMM-Newton
Authors: Mazzotta, Pasquale
2012adap.prop..131M Altcode:
With this proposal, we request support for an approved XMM-Newton
AO-11 (PI M. Arnaud, Co-I of this proposal) Large Programs that aim
to study the physical properties of a sample of 33 massive (M_500>5
10e14 solar mass) clusters of galaxies blindly detected by Planck and
confirmed to-day to be in the redshift range 0.5<z<1. Using for
the first time a statistically significant sample in this high-mass,
high-redshift regime, we will study the fundamental scalings between
YSZ, YX, and M500, and the pressure and entropy profiles. To reach
this purpose we requested the observation of 25 systems that, to date,
did not have sufficient X-ray exposure or no X-ray data at all. The
XMM Newton Observing Time Allocation Committee awarded us to observe
all the proposed targets for a total exposure time of 595 ks. Based
on other work carried out as part of Planck catalog validation,
we know that all the clusters in the sample are hot (kT >5keV),
high mass objects with complex morphologies and density profiles far
shallower than those of X-ray-selected cluster samples in the same
mass range. Our study will help addressing fundamental questions
in the field like the structure formation in the Universe and the
physics of the intracluster medium. In particular, we will be able
to constraining, for the first time, the SZ-X-ray-Optical scaling
relations of a unique and statistically significant sample of cluster
of galaxies in the high mass high z (0.5<z<1) regime. Beside
being an important probe of the physics of the gas gravitational
collapse, we will also precisely quantify how new SZ-selected clusters
differ from X-ray selected clusters so that we can better assess the
implication on the use of the clusters of galaxies as tools for precise
cosmology studies. Furthermore, it will be of large legacy value for the
cosmological exploitation of the full Planck cluster sample that will
be made available to the scientific community in the next few years.
---------------------------------------------------------
Title: Planck early results. VIII. The all-sky early Sunyaev-Zeldovich
cluster sample
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.;
Barreiro, R. B.; Bartelmann, M.; Bartlett, J. G.; Battaner, E.;
Battye, R.; Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli,
M.; Bhatia, R.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Brown, M. L.; Bucher, M.; Burigana, C.; Cabella, P.;
Cantalupo, C. M.; Cardoso, J. -F.; Carvalho, P.; Catalano, A.; Cayón,
L.; Challinor, A.; Chamballu, A.; Chary, R. -R.; Chiang, L. -Y.;
Chiang, C.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements,
D. L.; Colafrancesco, S.; Colombi, S.; Couchot, F.; Coulais, A.;
Crill, B. P.; Cuttaia, F.; da Silva, A.; Dahle, H.; Danese, L.; Davis,
R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti, G.;
Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Dickinson, C.;
Diego, J. M.; Dolag, K.; Dole, H.; Donzelli, S.; Doré, O.; Dörl,
U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Eisenhardt, P.; Enßlin,
T. A.; Feroz, F.; Finelli, F.; Flores-Cacho, I.; Forni, O.; Fosalba,
P.; Frailis, M.; Franceschi, E.; Fromenteau, S.; Galeotta, S.; Ganga,
K.; Génova-Santos, R. T.; Giard, M.; Giardino, G.; Giraud-Héraud,
Y.; González-Nuevo, J.; González-Riestra, R.; Górski, K. M.;
Grainge, K. J. B.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Harrison,
D.; Heinämäki, P.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Hurier, G.;
Hurley-Walker, N.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen,
E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knox, L.; Kurki-Suonio,
H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Le Jeune, M.; Leach, S.; Leonardi, R.; Li, C.; Liddle,
A.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.;
Mandolesi, N.; Mann, R.; Maris, M.; Marleau, F.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Mei, S.;
Meinhold, P. R.; Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella,
A.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.;
Noviello, F.; Novikov, D.; Novikov, I.; Olamaie, M.; Osborne, S.;
Pajot, F.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.;
Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.;
Piffaretti, R.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.;
Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.;
Rosset, C.; Rubiño-Martín, J. A.; Rusholme, B.; Saar, E.; Sandri,
M.; Santos, D.; Saunders, R. D. E.; Savini, G.; Schaefer, B. M.;
Scott, D.; Seiffert, M. D.; Shellard, P.; Smoot, G. F.; Stanford, A.;
Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Stompor, R.; Sudiwala, R.;
Sunyaev, R.; Sutton, D.; Sygnet, J. -F.; Taburet, N.; Tauber, J. A.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Torre, J. -P.; Tristram,
M.; Tuovinen, J.; Valenziano, L.; Vibert, L.; Vielva, P.; Villa,
F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Weller, J.; White,
S. D. M.; White, M.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A...8P Altcode: 2011arXiv1101.2024P; 2011A&A...536A...8A
We present the first all-sky sample of galaxy clusters detected blindly
by the Planck satellite through the Sunyaev-Zeldovich (SZ) effect from
its six highest frequencies. This early SZ (ESZ) sample is comprised
of 189 candidates, which have a high signal-to-noise ratio ranging
from 6 to 29. Its high reliability (purity above 95%) is further
ensured by an extensive validation process based on Planck internal
quality assessments and by external cross-identification and follow-up
observations. Planck provides the first measured SZ signal for about 80%
of the 169 previously-known ESZ clusters. Planck furthermore releases 30
new cluster candidates, amongst which 20 meet the ESZ signal-to-noise
selection criterion. At the submission date, twelve of the 20 ESZ
candidates were confirmed as new clusters, with eleven confirmed
using XMM-Newton snapshot observations, most of them with disturbed
morphologies and low luminosities. The ESZ clusters are mostly at
moderate redshifts (86% with z below 0.3) and span more than a decade in
mass, up to the rarest and most massive clusters with masses above 1 ×
10<SUP>15</SUP> M<SUB>⊙</SUB>. <P />Corresponding author: M. Douspis,
e-mail: marian.douspis@ias.u-psud.frAppendix is available in electronic
form at <A href="http://www.aanda.org">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck early results. XII. Cluster Sunyaev-Zeldovich optical
scaling relations
Authors: Planck Collaboration; Aghanim, N.; Arnaud, M.; Ashdown, M.;
Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.;
Bartelmann, M.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.; Bonaldi,
A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Brown, M. L.; Bucher,
M.; Burigana, C.; Cabella, P.; Cardoso, J. -F.; Catalano, A.; Cayón,
L.; Challinor, A.; Chamballu, A.; Chiang, L. -Y.; Chiang, C.; Chon,
G.; Christensen, P. R.; Churazov, E.; Clements, D. L.; Colafrancesco,
S.; Colombi, S.; Couchot, F.; Coulais, A.; Crill, B. P.; Cuttaia, F.;
da Silva, A.; Dahle, H.; Danese, L.; Davis, R. J.; de Bernardis, P.;
de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis,
J. -M.; Désert, F. -X.; Diego, J. M.; Dolag, K.; Donzelli, S.; Doré,
O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi,
E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Harrison,
D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest,
W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.; Jones,
W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre,
J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.;
Leonardi, R.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.;
Mandolesi, N.; Mann, R.; Maris, M.; Marleau, F.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Mei, S.;
Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella, A.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Pajot, F.; Pasian, F.;
Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini,
F.; Piat, M.; Pierpaoli, E.; Piffaretti, R.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Poutanen, T.; Pratt,
G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.; Rebolo, R.; Reinecke,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.;
Savini, G.; Schaefer, B. M.; Scott, D.; Seiffert, M. D.; Shellard, P.;
Smoot, G. F.; Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Sudiwala, R.;
Sunyaev, R.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Valenziano,
L.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wandelt, B. D.;
White, S. D. M.; White, M.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..12P Altcode: 2011A&A...536A..12A; 2011arXiv1101.2027P
We present the Sunyaev-Zeldovich (SZ) signal-to-richness scaling
relation (Y<SUB>500</SUB> - N<SUB>200</SUB>) for the MaxBCG cluster
catalogue. Employing a multi-frequency matched filter on the Planck
sky maps, we measure the SZ signal for each cluster by adapting the
filter according to weak-lensing calibrated mass-richness relations
(N<SUB>200</SUB> - M<SUB>500</SUB>). We bin our individual measurements
and detect the SZ signal down to the lowest richness systems
(N<SUB>200</SUB> = 10) with high significance, achieving a detection
of the SZ signal in systems with mass as low as M<SUB>500</SUB> ≈
5 × 10<SUP>13</SUP> M<SUB>⊙</SUB>. The observed Y<SUB>500</SUB> -
N<SUB>200</SUB> relation is well modeled by a power law over the full
richness range. It has a lower normalisation at given N<SUB>200</SUB>
than predicted based on X-ray models and published mass-richness
relations. An X-ray subsample, however, does conform to the predicted
scaling, and model predictions do reproduce the relation between
our measured bin-average SZ signal and measured bin-average X-ray
luminosities. At fixed richness, we find an intrinsic dispersion in the
Y<SUB>500</SUB> - N<SUB>200</SUB> relation of 60% rising to of order
100% at low richness. Thanks to its all-sky coverage, Planck provides
observations for more than 13000 MaxBCG clusters and an unprecedented
SZ/optical data set, extending the list of known cluster scaling laws
to include SZ-optical properties. The data set offers essential clues
for models of galaxy formation. Moreover, the lower normalisation of
the SZ-mass relation implied by the observed SZ-richness scaling has
important consequences for cluster physics and cosmological studies
with SZ clusters. <P />Corresponding author: J. G. Bartlett, e-mail:
bartlett@apc.univ-paris7.fr
---------------------------------------------------------
Title: Planck early results. I. The Planck mission
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Baker, M.; Balbi, A.; Banday,
A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.;
Bennett, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.;
Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Bradshaw, T.; Bremer, M.; Bucher, M.; Burigana, C.; Butler, R. C.;
Cabella, P.; Cantalupo, C. M.; Cappellini, B.; Cardoso, J. -F.; Carr,
R.; Casale, M.; Catalano, A.; Cayón, L.; Challinor, A.; Chamballu,
A.; Charra, J.; Chary, R. -R.; Chiang, L. -Y.; Chiang, C.; Christensen,
P. R.; Clements, D. L.; Colombi, S.; Couchot, F.; Coulais, A.; Crill,
B. P.; Crone, G.; Crook, M.; Cuttaia, F.; Danese, L.; D'Arcangelo,
O.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Bruin, J.; de
Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis,
J. -M.; Désert, F. -X.; Dick, J.; Dickinson, C.; Dolag, K.; Dole,
H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.;
Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Foley,
S.; Forni, O.; Fosalba, P.; Frailis, M.; Franceschi, E.; Freschi, M.;
Gaier, T. C.; Galeotta, S.; Gallegos, J.; Gandolfo, B.; Ganga, K.;
Giard, M.; Giardino, G.; Gienger, G.; Giraud-Héraud, Y.; González,
J.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Guyot, G.; Haissinski, J.; Hansen, F. K.; Harrison,
D.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hornstrup, A.; Hovest, W.; Hoyland, R. J.; Huffenberger,
K. M.; Jaffe, A. H.; Jagemann, T.; Jones, W. C.; Juillet, J. J.;
Juvela, M.; Kangaslahti, P.; Keihänen, E.; Keskitalo, R.; Kisner,
T. S.; Kneissl, R.; Knox, L.; Krassenburg, M.; Kurki-Suonio, H.;
Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.; Lange, A. E.;
Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leahy,
J. P.; Leonardi, R.; Leroy, C.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lowe, S.; Lubin, P. M.; Macías-Pérez, J. F.;
Maciaszek, T.; MacTavish, C. J.; Maffei, B.; Maino, D.; Mandolesi, N.;
Mann, R.; Maris, M.; Martínez-González, E.; Masi, S.; Massardi, M.;
Matarrese, S.; Matthai, F.; Mazzotta, P.; McDonald, A.; McGehee, P.;
Meinhold, P. R.; Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella,
A.; Mevi, C.; Miniscalco, R.; Mitra, S.; Miville-Deschênes, M. -A.;
Moneti, A.; Montier, L.; Morgante, G.; Morisset, N.; Mortlock, D.;
Munshi, D.; Murphy, A.; Naselsky, P.; Natoli, P.; Netterfield, C. B.;
Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.;
O'Dwyer, I. J.; Ortiz, I.; Osborne, S.; Osuna, P.; Oxborrow, C. A.;
Pajot, F.; Paladini, R.; Partridge, B.; Pasian, F.; Passvogel, T.;
Patanchon, G.; Pearson, D.; Pearson, T. J.; Perdereau, O.; Perotto, L.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Plaszczynski,
S.; Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa,
L.; Poutanen, T.; Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen,
J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Reix, J. -M.; Renault,
C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.; Salerno,
E.; Sandri, M.; Santos, D.; Savini, G.; Schaefer, B. M.; Scott, D.;
Seiffert, M. D.; Shellard, P.; Simonetto, A.; Smoot, G. F.; Sozzi, C.;
Starck, J. -L.; Sternberg, J.; Stivoli, F.; Stolyarov, V.; Stompor,
R.; Stringhetti, L.; Sudiwala, R.; Sunyaev, R.; Sygnet, J. -F.;
Tapiador, D.; Tauber, J. A.; Tavagnacco, D.; Taylor, D.; Terenzi, L.;
Texier, D.; Toffolatti, L.; Tomasi, M.; Torre, J. -P.; Tristram, M.;
Tuovinen, J.; Türler, M.; Tuttlebee, M.; Umana, G.; Valenziano, L.;
Valiviita, J.; Varis, J.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio,
N.; Wade, L. A.; Wandelt, B. D.; Watson, C.; White, S. D. M.; White,
M.; Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A...1P Altcode: 2011A&A...536A...1A; 2011arXiv1101.2022P
The European Space Agency's Planck satellite was launched on 14 May
2009, and has been surveying the sky stably and continuously since
13 August 2009. Its performance is well in line with expectations,
and it will continue to gather scientific data until the end of its
cryogenic lifetime. We give an overview of the history of Planck in
its first year of operations, and describe some of the key performance
aspects of the satellite. This paper is part of a package submitted
in conjunction with Planck's Early Release Compact Source Catalogue,
the first data product based on Planck to be released publicly. The
package describes the scientific performance of the Planck payload,
and presents results on a variety of astrophysical topics related to
the sources included in the Catalogue, as well as selected topics on
diffuse emission. <P />Corresponding author: J. A. Tauber, e-mail:
jtauber@rssd.esa.int
---------------------------------------------------------
Title: Planck early results. XIII. Statistical properties of
extragalactic radio sources in the Planck Early Release Compact
Source Catalogue
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Argüeso,
F.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.;
Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed,
K.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bonaldi, A.; Bonavera,
L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bucher, M.; Burigana, C.;
Cabella, P.; Cappellini, B.; Cardoso, J. -F.; Catalano, A.; Cayón, L.;
Challinor, A.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, L. -Y.;
Christensen, P. R.; Clements, D. L.; Colafrancesco, S.; Colombi, S.;
Couchot, F.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies, R. D.;
Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Dickinson, C.;
Dole, H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.;
Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni,
O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.;
Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.;
Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison,
D.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger,
K. M.; Jaffe, A. H.; Juvela, M.; Keihänen, E.; Keskitalo, R.;
Kisner, T. S.; Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.;
Lähteenmäki, A.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.;
Leach, S.; Leahy, J. P.; Leonardi, R.; Lilje, P. B.; Linden-Vørnle,
M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Magliocchetti, M.; Maino, D.; Mandolesi, N.; Mann, R.; Maris,
M.; Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Miville-Deschênes, M. -A.; Moneti, A.; Montier,
L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Pajot,
F.; Paladini, R.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson,
T. J.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.;
Polenta, G.; Ponthieu, N.; Poutanen, T.; Prézeau, G.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Rebolo, R.; Reinecke, M.; Ricciardi, S.;
Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rowan-Robinson,
M.; Rubiño-Martín, J. A.; Rusholme, B.; Sajina, A.; Sandri, M.;
Scott, D.; Seiffert, M. D.; Serjeant, S.; Shellard, P.; Smoot, G. F.;
Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Stompor, R.; Sudiwala, R.;
Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Türler, M.; Umana, G.;
Valenziano, L.; Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade,
L. A.; Wandelt, B. D.; Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..13P Altcode: 2011arXiv1101.2044P; 2011A&A...536A..13A
The data reported in Planck's Early Release Compact Source Catalogue
(ERCSC) are exploited to measure the number counts (dN/dS) of
extragalactic radio sources at 30, 44, 70, 100, 143 and 217 GHz. Due to
the full-sky nature of the catalogue, this measurement extends to the
rarest and brightest sources in the sky. At lower frequencies (30, 44,
and 70 GHz) our counts are in very good agreement with estimates based
on WMAP data, being somewhat deeper at 30 and 70 GHz, and somewhat
shallower at 44 GHz. Planck's source counts at 143 and 217 GHz join
smoothly with the fainter ones provided by the SPT and ACT surveys over
small fractions of the sky. An analysis of source spectra, exploiting
Planck's uniquely broad spectral coverage, finds clear evidence of a
steepening of the mean spectral index above about 70 GHz. This implies
that, at these frequencies, the contamination of the CMB power spectrum
by radio sources below the detection limit is significantly lower than
previously estimated. <P />Corresponding author: J. González-Nuevo,
e-mail: gnuevo@sissa.it
---------------------------------------------------------
Title: Planck early results. XIV. ERCSC validation and extreme
radio sources
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Angelakis,
E.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.;
Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed,
K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bonaldi,
A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bucher, M.;
Burigana, C.; Cabella, P.; Cappellini, B.; Cardoso, J. -F.; Catalano,
A.; Cayón, L.; Challinor, A.; Chamballu, A.; Chary, R. -R.; Chen,
X.; Chiang, L. -Y.; Christensen, P. R.; Clements, D. L.; Colombi,
S.; Couchot, F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.;
Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de
Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert,
F. -X.; Dickinson, C.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis,
M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Finelli, F.; Forni,
O.; Frailis, M.; Franceschi, E.; Fuhrmann, L.; Galeotta, S.; Ganga,
K.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Harrison,
D.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger,
K. M.; Huynh, M.; Jaffe, A. H.; Juvela, M.; Keihänen, E.; Keskitalo,
R.; Kisner, T. S.; Kneissl, R.; Knox, L.; Krichbaum, T. P.;
Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.;
Lasenby, A.; Laureijs, R. J.; Lavonen, N.; Lawrence, C. R.; Leach,
S.; Leahy, J. P.; Leonardi, R.; León-Tavares, J.; Linden-Vørnle,
M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Marleau, F.;
Martínez-González, E.; Masi, S.; Massardi, M.; Matarrese, S.;
Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Mingaliev, M.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy,
A.; Naselsky, P.; Natoli, P.; Nestoras, I.; Netterfield, C. B.;
Nieppola, E.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.;
Novikov, I.; Osborne, S.; Pajot, F.; Paladini, R.; Partridge, B.;
Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto, L.;
Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Plaszczynski,
S.; Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.;
Poutanen, T.; Prézeau, G.; Procopio, P.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Renault, C.;
Ricciardi, S.; Riller, T.; Riquelme, D.; Ristorcelli, I.; Rocha, G.;
Rosset, C.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.;
Sajina, A.; Sandri, M.; Savolainen, P.; Scott, D.; Seiffert, M. D.;
Sievers, A.; Smoot, G. F.; Sotnikova, Y.; Starck, J. -L.; Stivoli,
F.; Stolyarov, V.; Sudiwala, R.; Sygnet, J. -F.; Tammi, J.; Tauber,
J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tornikoski, M.; Torre,
J. -P.; Tristram, M.; Tuovinen, J.; Türler, M.; Turunen, M.; Umana,
G.; Ungerechts, H.; Valenziano, L.; Varis, J.; Vielva, P.; Villa,
F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Wilkinson, A.; Yvon,
D.; Zacchei, A.; Zensus, J. A.; Zonca, A.
2011A&A...536A..14P Altcode: 2011arXiv1101.1721P; 2011A&A...536A..14A
Planck's all-sky surveys at 30-857 GHz provide an unprecedented
opportunity to follow the radio spectra of a large sample of
extragalactic sources to frequencies 2-20 times higher than allowed
by past, large-area, ground-based surveys. We combine the results
of the Planck Early Release Compact Source Catalog (ERCSC) with
quasi-simultaneous ground-based observations as well as archival
data at frequencies below or overlapping Planck frequency bands,
to validate the astrometry and photometry of the ERCSC radio sources
and study the spectral features shown in this new frequency window
opened by Planck. The ERCSC source positions and flux density scales
are found to be consistent with the ground-based observations. We
present and discuss the spectral energy distributions of a sample of
"extreme" radio sources, to illustrate the richness of the ERCSC for
the study of extragalactic radio sources. Variability is found to play
a role in the unusual spectral features of some of these sources. <P
/>Corresponding author: B. Partridge, e-mail: bpartrid@haverford.edu
---------------------------------------------------------
Title: Planck early results. XI. Calibration of the local galaxy
cluster Sunyaev-Zeldovich scaling relations
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday,
A. J.; Barreiro, R. B.; Bartelmann, M.; Bartlett, J. G.; Battaner,
E.; Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.;
Bhatia, R.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Bourdin, H.; Brown, M. L.; Bucher, M.; Burigana, C.;
Cabella, P.; Cardoso, J. -F.; Catalano, A.; Cayón, L.; Challinor,
A.; Chamballu, A.; Chiang, L. -Y.; Chiang, C.; Chon, G.; Christensen,
P. R.; Churazov, E.; Clements, D. L.; Colafrancesco, S.; Colombi,
S.; Couchot, F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; da Silva,
A.; Dahle, H.; Danese, L.; de Bernardis, P.; de Gasperis, G.;
de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.;
Désert, F. -X.; Diego, J. M.; Dolag, K.; Donzelli, S.; Doré, O.;
Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi,
E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Harrison,
D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest,
W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.; Jones, W. C.;
Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.;
Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lanoux, J.;
Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leonardi,
R.; Liddle, A.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego,
M.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei,
B.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Marleau, F.;
Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.;
Mazzotta, P.; Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella,
A.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot, F.; Pasian, F.;
Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini,
F.; Piat, M.; Pierpaoli, E.; Piffaretti, R.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Poutanen, T.; Pratt,
G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.; Rachen, J. P.;
Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi, S.; Riller, T.;
Ristorcelli, I.; Rocha, G.; Rosset, C.; Rubiño-Martín, J. A.;
Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Schaefer, B. M.;
Scott, D.; Seiffert, M. D.; Shellard, P.; Smoot, G. F.; Starck, J. -L.;
Stivoli, F.; Stolyarov, V.; Sudiwala, R.; Sunyaev, R.; Sygnet, J. -F.;
Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Torre, J. -P.;
Tristram, M.; Tuovinen, J.; Valenziano, L.; Vibert, L.; Vielva, P.;
Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; White, S. D. M.;
White, M.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..11P Altcode: 2011arXiv1101.2026P; 2011A&A...536A..11A
We present precise Sunyaev-Zeldovich (SZ) effect measurements
in the direction of 62 nearby galaxy clusters (z < 0.5)
detected at high signal-to-noise in the first Planck all-sky data
set. The sample spans approximately a decade in total mass, 2 ×
10<SUP>14</SUP> M<SUB>⊙</SUB> < M<SUB>500</SUB> < 2 ×
10<SUP>15</SUP> M<SUB>⊙</SUB>, where M<SUB>500</SUB> is the mass
corresponding to a total density contrast of 500. Combining these
high quality Planck measurements with deep XMM-Newton X-ray data,
we investigate the relations between D<SUB>A</SUB><SUP>2</SUP>
Y<SUB>500</SUB>, the integrated Compton parameter due to the SZ
effect, and the X-ray-derived gas mass M<SUB>g,500</SUB>, temperature
T<SUB>X</SUB>, luminosity L<SUB>X,500</SUB>, SZ signal analogue
Y<SUB>X,500</SUB> = M<SUB>g,500</SUB> × T<SUB>X</SUB>, and total mass
M<SUB>500</SUB>. After correction for the effect of selection bias on
the scaling relations, we find results that are in excellent agreement
with both X-ray predictions and recently-published ground-based data
derived from smaller samples. The present data yield an exceptionally
robust, high-quality local reference, and illustrate Planck's unique
capabilities for all-sky statistical studies of galaxy clusters. <P
/>Corresponding author: G. W. Pratt, e-mail: gabriel.pratt@cea.fr
---------------------------------------------------------
Title: Planck early results. XXIV. Dust in the diffuse interstellar
medium and the Galactic halo
Authors: Planck Collaboration; Abergel, A.; Ade, P. A. R.; Aghanim,
N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi,
A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner,
E.; Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.;
Bhatia, R.; Blagrave, K.; Bock, J. J.; Bonaldi, A.; Bond, J. R.;
Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bucher, M.; Burigana,
C.; Cabella, P.; Cantalupo, C. M.; Cardoso, J. -F.; Catalano, A.;
Cayón, L.; Challinor, A.; Chamballu, A.; Chiang, L. -Y.; Chiang,
C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.;
Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies, R. D.;
Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Dickinson, C.;
Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou,
G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis,
M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino,
G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton,
S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Helou,
G.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger,
K. M.; Jaffe, A. H.; Joncas, G.; Jones, A.; Jones, W. C.; Juvela,
M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knox,
L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.;
Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leonardi, R.; Leroy,
C.; Linden-Vørnle, M.; Lockman, F. J.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Maino,
D.; Mandolesi, N.; Mann, R.; Maris, M.; Marshall, D. J.; Martin,
P.; Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.;
Mazzotta, P.; McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Miville-Deschênes, M. -A.; Moneti, A.; Montier,
L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.;
Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne,
S.; Pajot, F.; Paladini, R.; Pasian, F.; Patanchon, G.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pinheiro
Gonçalves, D.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Poutanen, T.; Prézeau, G.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Reach, W. T.; Reinecke, M.; Renault, C.; Ricciardi, S.;
Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rowan-Robinson,
M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.;
Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, P.; Smoot, G. F.;
Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Stompor, R.; Sudiwala, R.;
Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Umana, G.; Valenziano,
L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..24P Altcode: 2011A&A...536A..24A; 2011arXiv1101.2036P
This paper presents the first results from a comparison of Planck dust
maps at 353, 545 and 857GHz, along with IRAS data at 3000 (100 μm)
and 5000GHz (60 μm), with Green Bank Telescope 21-cm observations of
Hi in 14 fields covering more than 800 deg<SUP>2</SUP> at high Galactic
latitude. The main goal of this study is to estimate the far-infrared
to sub-millimeter (submm) emissivity of dust in the diffuse local
interstellar medium (ISM) and in the intermediate-velocity (IVC)
and high-velocity clouds (HVC) of the Galactic halo. Galactic dust
emission for fields with average Hi column density lower than 2
× 10<SUP>20</SUP> cm<SUP>-2</SUP> is well correlated with 21-cm
emission because in such diffuse areas the hydrogen is predominantly
in the neutral atomic phase. The residual emission in these fields,
once the Hi-correlated emission is removed, is consistent with the
expected statistical properties of the cosmic infrared background
fluctuations. The brighter fields in our sample, with an average Hi
column density greater than 2 × 10<SUP>20</SUP> cm<SUP>-2</SUP>,
show significant excess dust emission compared to the Hi column
density. Regions of excess lie in organized structures that suggest
the presence of hydrogen in molecular form, though they are not always
correlated with CO emission. In the higher Hi column density fields
the excess emission at 857 GHz is about 40% of that coming from the
Hi, but over all the high latitude fields surveyed the molecular mass
faction is about 10%. Dust emission from IVCs is detected with high
significance by this correlation analysis. Its spectral properties
are consistent with, compared to the local ISM values, significantly
hotter dust (T ~ 20K), lower submm dust opacity normalized per H-atom,
and a relative abundance of very small grains to large grains about four
times higher. These results are compatible with expectations for clouds
that are part of the Galactic fountain in which there is dust shattering
and fragmentation. Correlated dust emission in HVCs is not detected;
the average of the 99.9% confidence upper limits to the emissivity
is 0.15 times the local ISM value at 857 and 3000GHz, in accordance
with gas phase evidence for lower metallicity and depletion in these
clouds. Unexpected anti-correlated variations of the dust temperature
and emission cross-section per H atom are identified in the local
ISM and IVCs, a trend that continues into molecular environments. This
suggests that dust growth through aggregation, seen in molecular clouds,
is active much earlier in the cloud condensation and star formation
processes. <P />Corresponding author: M.-A. Miville-Deschênes, e-mail:
mamd@ias.u-psud.fr
---------------------------------------------------------
Title: Planck early results. XXIII. The first all-sky survey of
Galactic cold clumps
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday,
A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.;
Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.;
Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger,
F.; Bucher, M.; Burigana, C.; Cabella, P.; Cantalupo, C. M.; Cardoso,
J. -F.; Catalano, A.; Cayón, L.; Challinor, A.; Chamballu, A.; Chary,
R. -R.; Chiang, L. -Y.; Christensen, P. R.; Clements, D. L.; Colombi,
S.; Couchot, F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese,
L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Gasperis,
G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.;
Désert, F. -X.; Dickinson, C.; Dobashi, K.; Donzelli, S.; Doré, O.;
Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Falgarone, E.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.;
Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Héraud,
Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Hansen, F. K.; Harrison, D.; Helou, G.; Henrot-Versillé,
S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.;
Joncas, G.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.;
Kisner, T. S.; Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.;
Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach,
S.; Leonardi, R.; Leroy, C.; Linden-Vørnle, M.; López-Caniego,
M.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei,
B.; Mandolesi, N.; Mann, R.; Maris, M.; Marshall, D. J.; Martin, P.;
Martínez-González, E.; Marton, G.; Masi, S.; Matarrese, S.; Matthai,
F.; Mazzotta, P.; McGehee, P.; Melchiorri, A.; Mendes, L.; Mennella,
A.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.;
Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.;
Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot, F.;
Paladini, R.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Pelkonen,
V. -M.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini,
F.; Piat, M.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Poutanen, T.; Prézeau, G.; Prunet, S.; Puget, J. -L.;
Reach, W. T.; Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi, S.;
Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rowan-Robinson,
M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos, D.;
Savini, G.; Scott, D.; Seiffert, M. D.; Smoot, G. F.; Starck, J. -L.;
Stivoli, F.; Stolyarov, V.; Sudiwala, R.; Sygnet, J. -F.; Tauber,
J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Torre, J. -P.; Toth,
V.; Tristram, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Vielva,
P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Ysard, N.;
Yvon, D.; Zacchei, A.; Zahorecz, S.; Zonca, A.
2011A&A...536A..23P Altcode: 2011A&A...536A..23A; 2011arXiv1101.2035P
We present the statistical properties of the Cold Clump Catalogue of
Planck Objects (C3PO), the first all-sky catalogue of cold objects, in
terms of their spatial distribution, dust temperature, distance, mass,
and morphology. We have combined Planck and IRAS data to extract 10342
cold sources that stand out against a warmer environment. The sources
are distributed over the whole sky, including in the Galactic plane,
despite the confusion, and up to high latitudes (>30°). We find a
strong spatial correlation of these sources with ancillary data tracing
Galactic molecular structures and infrared dark clouds where the latter
have been catalogued. These cold clumps are not isolated but clustered
in groups. Dust temperature and emissivity spectral index values are
derived from their spectral energy distributions using both Planck and
IRAS data. The temperatures range from 7K to 19K, with a distribution
peaking around 13K. The data are inconsistent with a constant value
of the associated spectral index β over the whole temperature range:
β varies from 1.4 to 2.8, with a mean value around 2.1. Distances
are obtained for approximately one third of the objects. Most of the
detections lie within 2kpc of the Sun, but more distant sources are
also detected, out to 7kpc. The mass estimates inferred from dust
emission range from 0.4 M<SUB>⊙</SUB> to 2.4 × 10<SUP>5</SUP>
M<SUB>⊙</SUB>. Their physical properties show that these cold
sources trace a broad range of objects, from low-mass dense cores to
giant molecular clouds, hence the "cold clump" terminology. This first
statistical analysis of the C3PO reveals at least two colder populations
of special interest with temperatures in the range 7 to 12K: cores that
mostly lie close to the Sun; and massive cold clumps located in the
inner Galaxy. We also describe the statistics of the early cold core
(ECC) sample that is a subset of the C3PO, containing only the 915 most
reliable detections. The ECC is delivered as a part of the Planck Early
Release Compact Source Catalogue (ERCSC). <P />Corresponding author:
L. Montier, e-mail: Ludovic.Montier@irap.omp.eu
---------------------------------------------------------
Title: Planck early results. XXI. Properties of the interstellar
medium in the Galactic plane
Authors: Planck Collaboration; Abergel, A.; Ade, P. A. R.; Aghanim,
N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi,
A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.;
Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia,
R.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet,
F. R.; Boulanger, F.; Bucher, M.; Burigana, C.; Cabella, P.; Cardoso,
J. -F.; Catalano, A.; Cayón, L.; Challinor, A.; Chamballu, A.;
Chiang, L. -Y.; Chiang, C.; Christensen, P. R.; Colombi, S.; Couchot,
F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Dame, T. M.; Danese,
L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Gasperis,
G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.;
Désert, F. -X.; Dickinson, C.; Donzelli, S.; Doré, O.; Dörl, U.;
Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Finelli, F.;
Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Grenier, I. A.; Gruppuso,
A.; Hansen, F. K.; Harrison, D.; Henrot-Versillé, S.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest,
W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, T. R.; Jaffe, A. H.;
Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.;
Leach, S.; Leonardi, R.; Leroy, C.; Lilje, P. B.; Linden-Vørnle, M.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish,
C. J.; Maffei, B.; Mandolesi, N.; Mann, R.; Maris, M.; Marshall,
D. J.; Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.;
Mazzotta, P.; McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Mendes,
L.; Mennella, A.; Miville-Deschênes, M. -A.; Moneti, A.; Montier,
L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot, F.; Paladini, R.;
Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta,
F.; Piacentini, F.; Piat, M.; Plaszczynski, S.; Pointecouteau, E.;
Polenta, G.; Ponthieu, N.; Poutanen, T.; Prézeau, G.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reich, W.;
Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.;
Rosset, C.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri, M.; Santos,
D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, P.; Smoot, G. F.;
Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Stompor, R.; Sudiwala, R.;
Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.;
Torre, J. -P.; Tristram, M.; Tuovinen, J.; Umana, G.; Valenziano, L.;
Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt,
B. D.; Wilkinson, A.; Ysard, N.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..21P Altcode: 2011arXiv1101.2032P; 2011A&A...536A..21A
Planck has observed the entire sky from 30 GHz to 857GHz. The observed
foreground emission contains contributions from different phases of
the interstellar medium (ISM). We have separated the observed Galactic
emission into the different gaseous components (atomic, molecular and
ionised) in each of a number of Galactocentric rings. This technique
provides the necessary information to study dust properties (emissivity,
temperature, etc.), as well as other emission mechanisms as a function
of Galactic radius. Templates are created for various Galactocentric
radii using velocity information from atomic (neutral hydrogen)
and molecular (<SUP>12</SUP>CO) observations. The ionised template
is assumed to be traced by free-free emission as observed by WMAP,
while 408 MHz emission is used to trace the synchrotron component. Gas
emission not traced by the above templates, namely "dark gas", as
evidenced using Planck data, is included as an additional template, the
first time such a component has been used in this way. These templates
are then correlated with each of the Planck frequency bands, as well
as with higher frequency data from IRAS and DIRBE along with radio
data at 1.4 GHz. The emission per column density of the gas templates
allows us to create distinct spectral energy distributions (SEDs) per
Galactocentric ring and in each of the gaseous tracers from 1.4 GHz to
25 THz (12μm). The resulting SEDs allow us to explore the contribution
of various emission mechanisms to the Planck signal. Apart from the
thermal dust and free-free emission, we have probed the Galaxy for
anomalous (e.g., spinning) dust as well as synchrotron emission. We
find the dust opacity in the solar neighbourhood, τ/N<SUB>H</SUB>
= 0.92 ± 0.05 × 10<SUP>-25</SUP> cm<SUP>2</SUP> at 250 μm, with
no significant variation with Galactic radius, even though the dust
temperature is seen to vary from over 25 K to under 14 K. Furthermore,
we show that anomalous dust emission is present in the atomic,
molecular and dark gas phases throughout the Galactic disk. Anomalous
emission is not clearly detected in the ionised phase, as free-free
emission is seen to dominate. The derived dust propeties associated
with the dark gas phase are derived but do not allow us to reveal the
nature of this phase. For all environments, the anomalous emission
is consistent with rotation from polycyclic aromatic hydrocarbons
(PAHs) and, according to our simple model, accounts for (25 ± 5)%
(statistical) of the total emission at 30 GHz. <P />Corresponding
author: D. J. Marshall, e-mail: douglas.marshall@irap.omp.eu
---------------------------------------------------------
Title: Planck early results. XXV. Thermal dust in nearby molecular
clouds
Authors: Planck Collaboration; Abergel, A.; Ade, P. A. R.; Aghanim,
N.; Arnaud, M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi,
A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.;
Benabed, K.; Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.;
Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Boulanger, F.; Bucher, M.; Burigana, C.; Cabella, P.; Cardoso, J. -F.;
Catalano, A.; Cayón, L.; Challinor, A.; Chamballu, A.; Chiang, L. -Y.;
Chiang, C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot,
F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies, R. D.;
Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Dickinson,
C.; Dobashi, K.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.;
Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli,
F.; Forni, O.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Guillet,
V.; Hansen, F. K.; Harrison, D.; Henrot-Versillé, S.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest,
W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.; Jones, A.;
Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.;
Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leonardi,
R.; Leroy, C.; Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.;
Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Mandolesi, N.;
Mann, R.; Maris, M.; Marshall, D. J.; Martin, P.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee, P.;
Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; Osborne, S.; Pajot, F.; Paladini, R.; Pasian, F.;
Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini,
F.; Piat, M.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Poutanen, T.; Prézeau, G.; Prunet, S.; Puget, J. -L.;
Reach, W. T.; Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi, S.;
Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.;
Seiffert, M. D.; Shellard, P.; Smoot, G. F.; Starck, J. -L.; Stivoli,
F.; Stolyarov, V.; Sudiwala, R.; Sygnet, J. -F.; Tauber, J. A.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Torre, J. -P.; Tristram,
M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Verstraete, L.; Vielva,
P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Yvon, D.;
Zacchei, A.; Zonca, A.
2011A&A...536A..25P Altcode: 2011A&A...536A..25A; 2011arXiv1101.2037P
Planck allows unbiased mapping of Galactic sub-millimetre and millimetre
emission from the most diffuse regions to the densest parts of molecular
clouds. We present an early analysis of the Taurus molecular complex,
on line-of-sight-averaged data and without component separation. The
emission spectrum measured by Planck and IRAS can be fitted pixel by
pixel using a single modified blackbody. Some systematic residuals
are detected at 353 GHz and 143 GHz, with amplitudes around -7%
and +13%, respectively, indicating that the measured spectra are
likely more complex than a simple modified blackbody. Significant
positive residuals are also detected in the molecular regions and in
the 217 GHz and 100 GHz bands, mainly caused by the contribution of
the J = 2 → 1 and J = 1 → 0 <SUP>12</SUP>CO and <SUP>13</SUP>CO
emission lines. We derive maps of the dust temperature T, the dust
spectral emissivity index β, and the dust optical depth at 250 μm
τ<SUB>250</SUB>. The temperature map illustrates the cooling of the
dust particles in thermal equilibrium with the incident radiation
field, from 16 - 17 K in the diffuse regions to 13 - 14 K in the dense
parts. The distribution of spectral indices is centred at 1.78, with a
standard deviation of 0.08 and a systematic error of 0.07. We detect a
significant T - β anti-correlation. The dust optical depth map reveals
the spatial distribution of the column density of the molecular complex
from the densest molecular regions to the faint diffuse regions. We use
near-infrared extinction and Hi data at 21-cm to perform a quantitative
analysis of the spatial variations of the measured dust optical
depth at 250 μm per hydrogen atom τ<SUB>250</SUB>/N<SUB>H</SUB>. We
report an increase of τ<SUB>250</SUB>/N<SUB>H</SUB> by a factor of
about 2 between the atomic phase and the molecular phase, which has a
strong impact on the equilibrium temperature of the dust particles. <P
/>Corresponding author: A. Abergel, e-mail: alain.abergel@ias.u-psud.fr
---------------------------------------------------------
Title: Planck early results. XXVI. Detection with Planck and
confirmation by XMM-Newton of PLCK G266.6-27.3, an exceptionally
X-ray luminous and massive galaxy cluster at z ~ 1
Authors: Planck Collaboration; Aghanim, N.; Arnaud, M.; Ashdown, M.;
Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday,
A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.;
Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Böhringer,
H.; Bonaldi, A.; Bond, J. R.; Borgani, S.; Borrill, J.; Bouchet,
F. R.; Brown, M. L.; Burigana, C.; Cabella, P.; Cantalupo, C. M.;
Cappellini, B.; Carvalho, P.; Catalano, A.; Cayón, L.; Chiang, L. -Y.;
Chiang, C.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements,
D. L.; Colafrancesco, S.; Colombi, S.; Crill, B. P.; Cuttaia, F.; da
Silva, A.; Dahle, H.; Danese, L.; 'Arcangelo, O. D.; Davis, R. J.;
de Bernardis, P.; de Gasperis, G.; de Zotti, G.; Delabrouille, J.;
Delouis, J. -M.; Démoclès, J.; Désert, F. -X.; Dickinson, C.;
Diego, J. M.; Dole, H.; Donzelli, S.; Doré, O.; Douspis, M.; Dupac,
X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.;
Flores-Cacho, I.; Forni, O.; Fosalba, P.; Frailis, M.; Franceschi,
E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; González-Nuevo, J.; González-Riestra, R.; Górski, K. M.;
Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Heinämäki,
P.; Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson,
M.; Hurier, G.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen, E.;
Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Lawrence, C. R.;
Le Jeune, M.; Leach, S.; Leonardi, R.; Leroy, C.; Liddle, A.; Lilje,
P. B.; López-Caniego, M.; Luzzi, G.; Macías-Pérez, J. F.; Maino,
D.; Mandolesi, N.; Marleau, F.; Martínez-González, E.; Masi, S.;
Matarrese, S.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Melin,
J. -B.; Mendes, L.; Mennella, A.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Naselsky, P.;
Natoli, P.; Nevalainen, J.; Nørgaard-Nielsen, H. U.; Noviello, F.;
Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Paladini, R.;
Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto,
L.; Perrotta, F.; Piacentini, F.; Pierpaoli, E.; Piffaretti, R.;
Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Popa, L.;
Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi,
S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rubiño-Martín, J. A.;
Saar, E.; Sandri, M.; Savini, G.; Schaefer, B. M.; Scott, D.; Smoot,
G. F.; Starck, J. -L.; Sutton, D.; Sygnet, J. -F.; Tauber, J. A.;
Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Türler, M.;
Valenziano, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Weller, J.; White, S. D. M.; White, M.; Yvon, D.;
Zacchei, A.; Zonca, A.
2011A&A...536A..26P Altcode: 2011A&A...536A..26A; 2011arXiv1106.1376P
We present first results on PLCKG266.6-27.3, a galaxy cluster
candidate detected at a signal-to-noise ratio of 5 in the Planck
All Sky survey. An XMM-Newton validation observation has allowed
us to confirm that the candidate isa bona fide galaxy cluster. With
these X-ray data we measure an accurate redshift, z = 0.94 ± 0.02,
and estimate the cluster mass to be M<SUB>500</SUB> = (7.8 ± 0.8)
× 10<SUP>14</SUP> M<SUB>⊙</SUB>. PLCKG266.6-27.3 is an exceptional
system: its luminosity of L<SUB>X</SUB> [0.5-2.0 keV] = (1.4 ± 0.05)
× 10<SUP>45</SUP> erg s<SUP>-1</SUP> equals that of the two most
luminous known clusters in the z > 0.5 universe, and it is one of
the most massive clusters at z ~ 1. Moreover, unlike the majority
of high-redshift clusters, PLCKG266.6-27.3 appears to be highly
relaxed. This observation confirms Planck's capability of detecting
high-redshift, high-mass clusters, and opens the way to the systematic
study of population evolution in the exponential tail of the mass
function. <P />Corresponding author: M. Arnaud, monique.arnaud@cea.fr
---------------------------------------------------------
Title: Planck early results. II. The thermal performance of Planck
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Baker, M.; Balbi, A.;
Banday, A. J.; Barreiro, R. B.; Battaner, E.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bhandari, P.; Bhatia, R.;
Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borders, J.; Borrill, J.;
Bouchet, F. R.; Bowman, B.; Bradshaw, T.; Bréelle, E.; Bucher, M.;
Burigana, C.; Butler, R. C.; Cabella, P.; Camus, P.; Cantalupo, C. M.;
Cappellini, B.; Cardoso, J. -F.; Catalano, A.; Cayón, L.; Challinor,
A.; Chamballu, A.; Chambelland, J. P.; Charra, J.; Charra, M.; Chiang,
L. -Y.; Chiang, C.; Christensen, P. R.; Clements, D. L.; Collaudin,
B.; Colombi, S.; Couchot, F.; Coulais, A.; Crill, B. P.; Crook, M.;
Cuttaia, F.; Damasio, C.; Danese, L.; Davies, R. D.; Davis, R. J.;
de Bernardis, P.; de Gasperis, G.; de Rosa, A.; Delabrouille, J.;
Delouis, J. -M.; Désert, F. -X.; Dolag, K.; Donzelli, S.; Doré, O.;
Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Eriksen, H. K.; Filliard, C.; Finelli, F.; Foley, S.; Forni, O.;
Fosalba, P.; Fourmond, J. -J.; Frailis, M.; Franceschi, E.; Galeotta,
S.; Ganga, K.; Gavila, E.; Giard, M.; Giardino, G.; Giraud-Héraud,
Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Guyot, G.; Harrison, D.; Helou, G.; Henrot-Versillé,
S.; Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon,
E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Hoyland,
R. J.; Huffenberger, K. M.; Israelsson, U.; Jaffe, A. H.; Jones, W. C.;
Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.;
Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lami, P.;
Lasenby, A.; Laureijs, R. J.; Lavabre, A.; Lawrence, C. R.; Leach,
S.; Lee, R.; Leonardi, R.; Leroy, C.; Lilje, P. B.; López-Caniego,
M.; Lubin, P. M.; Macías-Pérez, J. F.; Maciaszek, T.; MacTavish,
C. J.; Maffei, B.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.;
Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.;
Mazzotta, P.; McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Melot,
F.; Mendes, L.; Mennella, A.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Mora, J.; Morgante, G.; Morisset, N.; Mortlock,
D.; Munshi, D.; Murphy, A.; Naselsky, P.; Nash, A.; Natoli, P.;
Netterfield, C. B.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne,
S.; Pajot, F.; Pasian, F.; Patanchon, G.; Pearson, D.; Perdereau, O.;
Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Plaszczynski,
S.; Platania, P.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.;
Poutanen, T.; Prézeau, G.; Prina, M.; Prunet, S.; Puget, J. -L.;
Rachen, J. P.; Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi, S.;
Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Schaefer,
B. M.; Scott, D.; Seiffert, M. D.; Shellard, P.; Smoot, G. F.; Starck,
J. -L.; Stassi, P.; Stivoli, F.; Stolyarov, V.; Stompor, R.; Sudiwala,
R.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.;
Tomasi, M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Valenziano,
L.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Watson, C.; White, S. D. M.; Wilkinson, A.; Wilson,
P.; Yvon, D.; Zacchei, A.; Zhang, B.; Zonca, A.
2011A&A...536A...2P Altcode: 2011arXiv1101.2023P; 2011A&A...536A...2A
The performance of the Planck instruments in space is enabled by their
low operating temperatures, 20 K for LFI and 0.1 K for HFI, achieved
through a combination of passive radiative cooling and three active
mechanical coolers. The scientific requirement for very broad frequency
coverage led to two detector technologies with widely different
temperature and cooling needs. Active coolers could satisfy these needs;
a helium cryostat, as used by previous cryogenic space missions (IRAS,
COBE, ISO, Spitzer, AKARI), could not. Radiative cooling is provided
by three V-groove radiators and a large telescope baffle. The active
coolers are a hydrogen sorption cooler (<20 K), a <SUP>4</SUP>He
Joule-Thomson cooler (4.7 K), and a <SUP>3</SUP>He-<SUP>4</SUP>He
dilution cooler (1.4 K and 0.1 K). The flight system was at ambient
temperature at launch and cooled in space to operating conditions. The
HFI bolometer plate reached 93 mK on 3 July 2009, 50 days after
launch. The solar panel always faces the Sun, shadowing the rest of
Planck, andoperates at a mean temperature of 384 K. At the other end
of the spacecraft, the telescope baffle operates at 42.3 K and the
telescope primary mirror operates at 35.9 K. The temperatures of key
parts of the instruments are stabilized by both active and passive
methods. Temperature fluctuations are driven by changes in the distance
from the Sun, sorption cooler cycling and fluctuations in gas-liquid
flow, and fluctuations in cosmic ray flux on the dilution and bolometer
plates. These fluctuations do not compromise the science data.
---------------------------------------------------------
Title: Planck early results. XIX. All-sky temperature and dust
optical depth from Planck and IRAS. Constraints on the "dark gas"
in our Galaxy
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday,
A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.;
Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.;
Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.;
Bucher, M.; Burigana, C.; Cabella, P.; Cardoso, J. -F.; Catalano, A.;
Cayón, L.; Challinor, A.; Chamballu, A.; Chiang, L. -Y.; Chiang,
C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.;
Coulais, A.; Crill, B. P.; Cuttaia, F.; Dame, T. M.; Danese, L.;
Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de
Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert,
F. -X.; Dickinson, C.; Dobashi, K.; Donzelli, S.; Doré, O.; Dörl,
U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen,
H. K.; Falgarone, E.; Finelli, F.; Forni, O.; Fosalba, P.; Frailis,
M.; Franceschi, E.; Fukui, Y.; Galeotta, S.; Ganga, K.; Giard, M.;
Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.;
Gratton, S.; Gregorio, A.; Grenier, I. A.; Gruppuso, A.; Hansen,
F. K.; Harrison, D.; Helou, G.; Henrot-Versillé, S.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest,
W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.; Jones, W. C.;
Juvela, M.; Kawamura, A.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.;
Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leonardi, R.;
Leroy, C.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.;
Mandolesi, N.; Mann, R.; Maris, M.; Martin, P.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee,
P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.;
Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante, G.;
Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; O'Dwyer, I. J.; Onishi, T.; Osborne, S.; Pajot, F.;
Paladini, R.; Paradis, D.; Pasian, F.; Patanchon, G.; Perdereau, O.;
Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Poutanen, T.; Prézeau,
G.; Prunet, S.; Puget, J. -L.; Reach, W. T.; Reinecke, M.; Renault,
C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset,
C.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri,
M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, P.;
Smoot, G. F.; Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Stompor, R.;
Sudiwala, R.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Umana,
G.; Valenziano, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Wilkinson, A.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..19P Altcode: 2011A&A...536A..19A; 2011arXiv1101.2029P
An all sky map of the apparent temperature and optical depth of
thermal dust emission is constructed using the Planck-HFI (350μm
to 2 mm) andIRAS(100μm) data. The optical depth maps are correlated
with tracers of the atomic (Hi) and molecular gas traced by CO. The
correlation with the column density of observed gas is linear in
the lowest column density regions at high Galactic latitudes. At
high N<SUB>H</SUB>, the correlation is consistent with that of the
lowest N<SUB>H</SUB>, for a given choice of the CO-to-H<SUB>2</SUB>
conversion factor. In the intermediate N<SUB>H</SUB> range, a departure
from linearity is observed, with the dust optical depth in excess
of the correlation. This excess emission is attributed to thermal
emission by dust associated with a dark gas phase, undetected in the
available Hi and CO surveys. The 2D spatial distribution of the dark
gas in the solar neighbourhood (|b<SUB>II</SUB>| > 10°) is shown
to extend around known molecular regions traced by CO. The average
dust emissivity in the Hi phase in the solar neighbourhood is found to
be τ<SUB>D</SUB>/N<SUB>H</SUB><SUP>tot</SUP> = 5.2×10<SUP>-26</SUP>
cm<SUP>2</SUP> at 857 GHz. It follows roughly a power law distribution
with a spectral index β = 1.8 all the way down to 3 mm, although
the SED flattens slightly in the millimetre. Taking into account the
spectral shape of the dust optical depth, the emissivity is consistent
with previous values derived fromFIRAS measurements at high latitudes
within 10%. The threshold for the existence of the dark gas is
found at N<SUB>H</SUB><SUP>tot</SUP> = (8.0±0.58)×10<SUP>20</SUP>
H cm<SUP>-2</SUP> (A<SUB>V</SUB> = 0.4mag). Assuming the same high
frequency emissivity for the dust in the atomic and the molecular phases
leads to an average X<SUB>CO</SUB> = (2.54 ± 0.13) × 10<SUP>20</SUP>
H<SUB>2</SUB> cm<SUP>-2</SUP>/(K km s<SUP>-1</SUP>). The mass of dark
gas is found to be 28% of the atomic gas and 118% of the CO emitting
gas in the solar neighbourhood. The Galactic latitude distribution
shows that its mass fraction is relatively constant down to a few
degrees from the Galactic plane. A possible explanation for the dark
gas lies in a dark molecular phase, where H<SUB>2</SUB> survives
photodissociation but CO does not. The observed transition for the
onsetof this phase in the solar neighbourhood (A<SUB>V</SUB> = 0.4mag)
appears consistent with recent theoretical predictions. It is also
possible that up to half of the dark gas could be in atomic form, due
to optical depth effects in the Hi measurements. <P />Corresponding
author: J.-P. Bernard, e-mail: Jean-Philippe.Bernard@cesr.fr
---------------------------------------------------------
Title: Planck early results. XX. New light on anomalous microwave
emission from spinning dust grains
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday,
A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.;
Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.;
Bonaldi, A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger,
F.; Bucher, M.; Burigana, C.; Cabella, P.; Cappellini, B.; Cardoso,
J. -F.; Casassus, S.; Catalano, A.; Cayón, L.; Challinor, A.;
Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, L. -Y.; Chiang,
C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot,
F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies,
R. D.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Dickinson, C.;
Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou,
G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Frailis,
M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Hansen,
F. K.; Harrison, D.; Helou, G.; Henrot-Versillé, S.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest,
W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, T. R.; Jaffe,
A. H.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.;
Kisner, T. S.; Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs,
R. J.; Lawrence, C. R.; Leach, S.; Leonardi, R.; Lilje, P. B.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.; Mandolesi, N.;
Mann, R.; Maris, M.; Marshall, D. J.; Martínez-González, E.;
Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee, P.;
Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Pajot, F.; Paladini,
R.; Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Peel,
M.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Poutanen, T.; Prézeau, G.; Procopio, P.; Prunet, S.;
Puget, J. -L.; Reach, W. T.; Rebolo, R.; Reich, W.; Reinecke, M.;
Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.;
Rosset, C.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme,
B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.;
Shellard, P.; Smoot, G. F.; Starck, J. -L.; Stivoli, F.; Stolyarov,
V.; Stompor, R.; Sudiwala, R.; Sygnet, J. -F.; Tauber, J. A.; Terenzi,
L.; Toffolatti, L.; Tomasi, M.; Torre, J. -P.; Tristram, M.; Tuovinen,
J.; Umana, G.; Valenziano, L.; Varis, J.; Verstraete, L.; Vielva,
P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Watson,
R.; Wilkinson, A.; Ysard, N.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..20P Altcode: 2011arXiv1101.2031P; 2011A&A...536A..20A
Anomalous microwave emission (AME) has been observed by numerous
experiments in the frequency range ~10-60 GHz. Using Planck maps and
multi-frequency ancillary data, we have constructed spectra for two
known AME regions: the Perseus and ρ Ophiuchi molecular clouds. The
spectra are well fitted by a combination of free-free radiation, cosmic
microwave background, thermal dust, and electric dipole radiation from
small spinning dust grains. The spinning dust spectra are the most
precisely measured to date, and show the high frequency side clearly
for the first time. The spectra have a peak in the range 20-40 GHz and
are detected at high significances of 17.1σ for Perseus and 8.4σ for
ρ Ophiuchi. In Perseus, spinning dust in the dense molecular gas can
account for most of the AME; the low density atomic gas appears to
play a minor role. In ρ Ophiuchi, the ~30 GHz peak is dominated by
dense molecular gas, but there is an indication of an extended tail
at frequencies 50-100 GHz, which can be accounted for by irradiated
low density atomic gas. The dust parameters are consistent with those
derived from other measurements. We have also searched the Planck map
at 28.5 GHz for candidate AME regions, by subtracting a simple model
of the synchrotron, free-free, and thermal dust. We present spectra
for two of the candidates; S140 and S235 are bright Hii regions that
show evidence for AME, and are well fitted by spinning dust models. <P
/>Corresponding author: C. Dickinson, Clive.Dickinson@manchester.ac.uk
---------------------------------------------------------
Title: Planck early results. XV. Spectral energy distributions and
radio continuum spectra of northern extragalactic radio sources
Authors: Planck Collaboration; Aatrokoski, J.; Ade, P. A. R.;
Aghanim, N.; Aller, H. D.; Aller, M. F.; Angelakis, E.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.;
Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Berdyugin, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.;
Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.;
Bucher, M.; Burigana, C.; Burrows, D. N.; Cabella, P.; Capalbi, M.;
Cappellini, B.; Cardoso, J. -F.; Catalano, A.; Cavazzuti, E.; Cayón,
L.; Challinor, A.; Chamballu, A.; Chary, R. -R.; Chiang, L. -Y.;
Christensen, P. R.; Clements, D. L.; Colafrancesco, S.; Colombi, S.;
Couchot, F.; Coulais, A.; Cutini, S.; Cuttaia, F.; Danese, L.; Davies,
R. D.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa,
A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Dickinson, C.;
Dole, H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.;
Efstathiou, G.; Enßlin, T. A.; Finelli, F.; Forni, O.; Frailis, M.;
Franceschi, E.; Fuhrmann, L.; Galeotta, S.; Ganga, K.; Gargano, F.;
Gasparrini, D.; Gehrels, N.; Giard, M.; Giardino, G.; Giglietto, N.;
Giommi, P.; Giordano, F.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Harrison,
D.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger,
K. M.; Jaffe, A. H.; Juvela, M.; Keihänen, E.; Keskitalo, R.;
King, O.; Kisner, T. S.; Kneissl, R.; Knox, L.; Krichbaum, T. P.;
Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J. -M.;
Lasenby, A.; Laureijs, R. J.; Lavonen, N.; Lawrence, C. R.; Leach,
S.; Leonardi, R.; León-Tavares, J.; Linden-Vørnle, M.; Lindfors, E.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei, B.;
Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Martínez-González, E.;
Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Max-Moerbeck, W.;
Mazziotta, M. N.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella,
A.; Michelson, P. F.; Mingaliev, M.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Monte, C.; Montier, L.; Morgante, G.; Mortlock,
D.; Munshi, D.; Murphy, A.; Naselsky, P.; Natoli, P.; Nestoras, I.;
Netterfield, C. B.; Nieppola, E.; Nilsson, K.; Nørgaard-Nielsen,
H. U.; Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.;
Osborne, S.; Pajot, F.; Partridge, B.; Pasian, F.; Patanchon, G.;
Pavlidou, V.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perri, M.;
Perrotta, F.; Piacentini, F.; Piat, M.; Plaszczynski, S.; Platania, P.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Poutanen, T.; Prézeau,
G.; Procopio, P.; Prunet, S.; Puget, J. -L.; Rachen, J. P.; Rainò,
S.; Reach, W. T.; Readhead, A.; Rebolo, R.; Reeves, R.; Reinecke, M.;
Reinthal, R.; Renault, C.; Ricciardi, S.; Richards, J.; Riller, T.;
Riquelme, D.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rowan-Robinson,
M.; Rubiño-Martín, J. A.; Rusholme, B.; Saarinen, J.; Sandri, M.;
Savolainen, P.; Scott, D.; Seiffert, M. D.; Sievers, A.; Sillanpää,
A.; Smoot, G. F.; Sotnikova, Y.; Starck, J. -L.; Stevenson, M.;
Stivoli, F.; Stolyarov, V.; Sudiwala, R.; Sygnet, J. -F.; Takalo, L.;
Tammi, J.; Tauber, J. A.; Terenzi, L.; Thompson, D. J.; Toffolatti,
L.; Tomasi, M.; Tornikoski, M.; Torre, J. -P.; Tosti, G.; Tramacere,
A.; Tristram, M.; Tuovinen, J.; Türler, M.; Turunen, M.; Umana, G.;
Ungerechts, H.; Valenziano, L.; Valtaoja, E.; Varis, J.; Verrecchia,
F.; Vielva, P.; Villa, F.; Vittorio, N.; Wandelt, B. D.; Wu, J.;
Yvon, D.; Zacchei, A.; Zensus, J. A.; Zhou, X.; Zonca, A.
2011A&A...536A..15P Altcode: 2011A&A...536A..15A; 2011arXiv1101.2047P
Spectral energy distributions (SEDs) and radio continuum spectra are
presented for a northern sample of 104 extragalactic radio sources,
based on the Planck Early Release Compact Source Catalogue (ERCSC)
and simultaneous multifrequency data. The nine Planck frequencies, from
30 to 857 GHz, are complemented by a set of simultaneous observations
ranging from radio to gamma-rays. This is the first extensive frequency
coverage in the radio and millimetre domains for an essentially
complete sample of extragalactic radio sources, and it shows how the
individual shocks, each in their own phase of development, shape the
radio spectra as they move in the relativistic jet. The SEDs presented
in this paper were fitted with second and third degree polynomials to
estimate the frequencies of the synchrotron and inverse Compton (IC)
peaks, and the spectral indices of low and high frequency radio data,
including the Planck ERCSC data, were calculated. SED modelling methods
are discussed, with an emphasis on proper, physical modelling of the
synchrotron bump using multiple components. Planck ERCSC data also
suggest that the original accelerated electron energy spectrum could
be much harder than commonly thought, with power-law indexaround 1.5
instead of the canonical 2.5. The implications of this are discussed
for the acceleration mechanisms effective in blazar shocks. Furthermore
in many cases the Planck data indicate that gamma-ray emission must
originate in the same shocks that produce the radio emission. <P
/>Tables 1 and 4, Figs. 18-121 are available in electronic form at
<A href="http://www.aanda.org">http://www.aanda.org</A>
---------------------------------------------------------
Title: Planck early results. XVI. The Planck view of nearby galaxies
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.;
Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.; Bonaldi,
A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bucher, M.; Burigana,
C.; Cabella, P.; Cardoso, J. -F.; Catalano, A.; Cayón, L.; Challinor,
A.; Chamballu, A.; Chary, R. -R.; Chiang, L. -Y.; Christensen, P. R.;
Clements, D. L.; Colombi, S.; Couchot, F.; Coulais, A.; Crill, B. P.;
Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis,
P.; de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.;
Delouis, J. -M.; Désert, F. -X.; Dickinson, C.; Dole, H.; Donzelli,
S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.;
Enßlin, T. A.; Finelli, F.; Forni, O.; Frailis, M.; Franceschi, E.;
Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud-Héraud,
Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Hansen, F. K.; Harrison, D.; Helou, G.; Henrot-Versillé,
S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.;
Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki,
A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.;
Leach, S.; Leonardi, R.; Linden-Vørnle, M.; López-Caniego, M.; Lubin,
P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Madden, S.; Maffei, B.;
Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Melchiorri,
A.; Mendes, L.; Mennella, A.; Miville-Deschênes, M. -A.; Moneti,
A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi, D.; Murphy,
A.; Naselsky, P.; Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen,
H. U.; Noviello, F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot,
F.; Partridge, B.; Pasian, F.; Patanchon, G.; Peel, M.; Perdereau, O.;
Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Poutanen, T.; Prézeau,
G.; Prunet, S.; Puget, J. -L.; Reach, W. T.; Rebolo, R.; Reinecke,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme,
B.; Sandri, M.; Savini, G.; Scott, D.; Seiffert, M. D.; Shellard, P.;
Smoot, G. F.; Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Sudiwala, R.;
Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Türler, M.; Umana,
G.; Valenziano, L.; Varis, J.; Vielva, P.; Villa, F.; Vittorio, N.;
Wade, L. A.; Wandelt, B. D.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..16P Altcode: 2011arXiv1101.2045P; 2011A&A...536A..16A
The all-sky coverage of the Planck Early Release Compact Source
Catalogue (ERCSC) provides an unsurpassed survey of galaxies at
submillimetre (submm) wavelengths, representing a major improvement in
the numbers of galaxies detected, as well as the range of far-IR/submm
wavelengths over which they have been observed. We here present the
first results on the properties of nearby galaxies using these data. We
match the ERCSC catalogue to IRAS-detected galaxies in the Imperial
IRAS Faint Source Redshift Catalogue (IIFSCz), so that we can measure
the spectral energy distributions (SEDs) of these objects from 60 to
850μm. This produces a list of 1717 galaxies with reliable associations
between Planck and IRAS, from which we select a subset of 468 for
SED studies, namely those with strong detections in the three highest
frequency Planck bands and no evidence of cirrus contamination. The SEDs
are fitted using parametric dust models to determine the range of dust
temperatures and emissivities. We find evidence for colder dust than
has previously been found in external galaxies, with T < 20K. Such
cold temperatures are found using both the standard single temperature
dust model with variable emissivity β, or a two dust temperature model
with β fixed at 2. We also compare our results to studies of distant
submm galaxies (SMGs) which have been claimed to contain cooler dust
than their local counterparts. We find that including our sample of
468 galaxies significantly reduces the distinction between the two
populations. Fits to SEDs of selected objects using more sophisticated
templates derived from radiative transfer models confirm the presence of
the colder dust found through parametric fitting. We thus conclude that
cold (T < 20K) dust is a significant and largely unexplored component
of many nearby galaxies. <P />Corresponding author: D. L. Clements,
e-mail: d.clements@imperial.ac.uk
---------------------------------------------------------
Title: Planck early results. X. Statistical analysis of
Sunyaev-Zeldovich scaling relations for X-ray galaxy clusters
Authors: Planck Collaboration; Aghanim, N.; Arnaud, M.; Ashdown, M.;
Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.;
Bartelmann, M.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.; Bonaldi,
A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Brown, M. L.; Bucher, M.;
Burigana, C.; Cabella, P.; Cardoso, J. -F.; Catalano, A.; Cayón, L.;
Challinor, A.; Chamballu, A.; Chary, R. -R.; Chiang, L. -Y.; Chiang,
C.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements, D. L.;
Colafrancesco, S.; Colombi, S.; Couchot, F.; Coulais, A.; Crill, B. P.;
Cuttaia, F.; da Silva, A.; Dahle, H.; Danese, L.; de Bernardis, P.;
de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis,
J. -M.; Désert, F. -X.; Diego, J. M.; Dolag, K.; Donzelli, S.; Doré,
O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi,
E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Harrison,
D.; Henrot-Versillé, S.; Hernández-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest,
W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.; Jones, W. C.;
Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.;
Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby,
A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leonardi, R.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; MacTavish, C. J.; Maffei, B.; Maino, D.; Mandolesi, N.; Mann,
R.; Maris, M.; Marleau, F.; Martínez-González, E.; Masi, S.;
Matarrese, S.; Matthai, F.; Mazzotta, P.; Melchiorri, A.; Melin,
J. -B.; Mendes, L.; Mennella, A.; Mitra, S.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi,
D.; Murphy, A.; Naselsky, P.; Natoli, P.; Netterfield, C. B.;
Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.;
Osborne, S.; Pajot, F.; Pasian, F.; Patanchon, G.; Perdereau, O.;
Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.;
Piffaretti, R.; Plaszczynski, S.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.;
Puget, J. -L.; Rebolo, R.; Reinecke, M.; Renault, C.; Ricciardi, S.;
Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rubiño-Martín,
J. A.; Rusholme, B.; Sandri, M.; Santos, D.; Schaefer, B. M.; Scott,
D.; Seiffert, M. D.; Smoot, G. F.; Starck, J. -L.; Stivoli, F.;
Stolyarov, V.; Sunyaev, R.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.;
Toffolatti, L.; Tomasi, M.; Tristram, M.; Tuovinen, J.; Valenziano,
L.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wandelt, B. D.;
White, S. D. M.; White, M.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..10P Altcode: 2011arXiv1101.2043P; 2011A&A...536A..10A
All-sky data from the Planck survey and the Meta-Catalogue of X-ray
detected Clusters of galaxies (MCXC) are combined to investigate
the relationship between the thermal Sunyaev-Zeldovich (SZ) signal
and X-ray luminosity. The sample comprises ~1600 X-ray clusters with
redshifts up to ~1 and spans a wide range in X-ray luminosity. The SZ
signal is extracted for each object individually, and the statistical
significance of the measurement is maximised by averaging the SZ
signal in bins of X-ray luminosity, total mass, or redshift. The
SZ signal is detected at very high significance over more than
two decades in X-ray luminosity (10<SUP>43</SUP>erg s<SUP>-1</SUP>
≲ L<SUB>500</SUB>E(z)<SUP>-7/3</SUP> ≲ 2 × 10<SUP>45</SUP>erg
s<SUP>-1</SUP>). The relation between intrinsic SZ signal and X-ray
luminosity is investigated and the measured SZ signal is compared to
values predicted from X-ray data. Planck measurements and X-ray based
predictions are found to be in excellent agreement over the whole
explored luminosity range. No significant deviation from standard
evolution of the scaling relations is detected. For the first time
the intrinsic scatter in the scaling relation between SZ signal and
X-ray luminosity is measured and found to be consistent with the one
in the luminosity - mass relation from X-ray studies. There is no
evidence of any deficit in SZ signal strength in Planck data relative
to expectations from the X-ray properties of clusters, underlining
the robustness and consistency of our overall view of intra-cluster
medium properties. <P />Corresponding author: R. Piffaretti, e-mail:
rocco.piffaretti@cea.fr
---------------------------------------------------------
Title: Planck early results. VII. The Early Release Compact Source
Catalogue
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.;
Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bonaldi, A.; Bonavera,
L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Bucher, M.; Burigana,
C.; Butler, R. C.; Cabella, P.; Cantalupo, C. M.; Cappellini, B.;
Cardoso, J. -F.; Carvalho, P.; Catalano, A.; Cayón, L.; Challinor,
A.; Chamballu, A.; Chary, R. -R.; Chen, X.; Chiang, L. -Y.; Chiang, C.;
Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.; Coulais,
A.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davis, R. J.; de Bernardis,
P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis, J. -M.;
Désert, F. -X.; Dickinson, C.; Diego, J. M.; Dolag, K.; Dole, H.;
Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou,
G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni, O.; Fosalba,
P.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton, S.;
Gregorio, A.; Gruppuso, A.; Haissinski, J.; Hansen, F. K.; Harrison,
D.; Helou, G.; Henrot-Versillé, S.; Hernández-Monteagudo, C.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.;
Hornstrup, A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Huynh,
M.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo,
R.; Kisner, T. S.; Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache,
G.; Lähteenmäki, A.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leach, S.; Leahy, J. P.; Leonardi, R.; León-Tavares,
J.; Leroy, C.; Lilje, P. B.; Linden-Vørnle, M.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Maffei, B.;
Maggio, G.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Marleau,
F.; Marshall, D. J.; Martínez-González, E.; Masi, S.; Massardi,
M.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee, P.; Meinhold,
P. R.; Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella, A.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov,
D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Pajot, F.; Paladini, R.;
Partridge, B.; Pasian, F.; Patanchon, G.; Pearson, T. J.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Piffaretti,
R.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.; Polenta, G.;
Ponthieu, N.; Poutanen, T.; Pratt, G. W.; Prézeau, G.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.; Reinecke,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme,
B.; Sajina, A.; Sandri, M.; Santos, D.; Savini, G.; Schaefer, B. M.;
Scott, D.; Seiffert, M. D.; Shellard, P.; Smoot, G. F.; Starck, J. -L.;
Stivoli, F.; Stolyarov, V.; Sudiwala, R.; Sunyaev, R.; Sygnet, J. -F.;
Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi,
M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Türler, M.; Umana,
G.; Valenziano, L.; Valiviita, J.; Varis, J.; Vielva, P.; Villa, F.;
Vittorio, N.; Wade, L. A.; Wandelt, B. D.; White, S. D. M.; Wilkinson,
A.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A...7P Altcode: 2011A&A...536A...7A; 2011arXiv1101.2041P
A brief description of the methodology of construction, contents and
usage of the Planck Early Release Compact Source Catalogue (ERCSC),
including the Early Cold Cores (ECC) and the Early Sunyaev-Zeldovich
(ESZ) cluster catalogue is provided. The catalogue is based on data
that consist of mapping the entire sky once and 60% of the sky a
second time by Planck, thereby comprising the first high sensitivity
radio/submillimetre observations of the entire sky. Four source
detection algorithms were run as part of the ERCSC pipeline. A
Monte-Carlo algorithm based on the injection and extraction
of artificial sources into the Planck maps was implemented to
select reliable sources among all extracted candidates such that
the cumulative reliability of the catalogue is ≥90%. There is
no requirement on completeness for the ERCSC. As a result of the
Monte-Carlo assessment of reliability of sources from the different
techniques, an implementation of the PowellSnakes source extraction
technique was used at the five frequencies between 30 and 143GHz while
the SExtractor technique was used between 217 and 857GHz. The 10σ
photometric flux density limit of the catalogue at |b| > 30° is
0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of
the nine frequencies between 30 and 857GHz. Sources which are up to a
factor of ~2 fainter than this limit, and which are present in "clean"
regions of the Galaxy where the sky background due to emission from
the interstellar medium is low, are included in the ERCSC if they meet
the high reliability criterion. The Planck ERCSC sources have known
associations to stars with dust shells, stellar cores, radio galaxies,
blazars, infrared luminous galaxies and Galactic interstellar medium
features. A significant fraction of unclassified sources are also
present in the catalogs. In addition, two early release catalogs that
contain 915 cold molecular cloud core candidates and 189 SZ cluster
candidates that have been generated using multifrequency algorithms are
presented. The entire source list, with more than 15000 unique sources,
is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA,
ALMA and other ground-based observing facilities. <P />Corresponding
author: R.-R. Chary, e-mail: rchary@caltech.edu
---------------------------------------------------------
Title: Planck early results. XVII. Origin of the submillimetre excess
dust emission in the Magellanic Clouds
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.;
Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.; Bonaldi,
A.; Bond, J. R.; Borrill, J.; Bot, C.; Bouchet, F. R.; Boulanger, F.;
Bucher, M.; Burigana, C.; Cabella, P.; Cardoso, J. -F.; Catalano, A.;
Cayón, L.; Challinor, A.; Chamballu, A.; Chiang, L. -Y.; Chiang,
C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.;
Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies, R. D.;
Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.; de Zotti,
G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.; Dickinson,
C.; Dobashi, K.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.;
Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Finelli, F.; Forni, O.;
Frailis, M.; Franceschi, E.; Fukui, Y.; Galeotta, S.; Ganga, K.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
Górski, K. M.; Gratton, S.; Gregorio, A.; Gruppuso, A.; Harrison,
D.; Helou, G.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt,
S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland,
R. J.; Huffenberger, K. M.; Jaffe, A. H.; Jones, W. C.; Juvela, M.;
Kawamura, A.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.;
Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre,
J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.;
Leonardi, R.; Leroy, C.; Linden-Vørnle, M.; López-Caniego, M.;
Lubin, P. M.; Macías-Pérez, J. F.; MacTavish, C. J.; Madden, S.;
Maffei, B.; Mandolesi, N.; Mann, R.; Maris, M.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; Meinhold,
P. R.; Melchiorri, A.; Mendes, L.; Mennella, A.; Miville-Deschênes,
M. -A.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Munshi,
D.; Murphy, A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield,
C. B.; Nørgaard-Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov,
I.; Onishi, T.; Osborne, S.; Pajot, F.; Paladini, R.; Paradis, D.;
Pasian, F.; Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta,
F.; Piacentini, F.; Piat, M.; Plaszczynski, S.; Pointecouteau, E.;
Polenta, G.; Ponthieu, N.; Poutanen, T.; Prézeau, G.; Prunet, S.;
Puget, J. -L.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Renault, C.;
Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Rosset, C.;
Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme, B.; Sandri,
M.; Savini, G.; Scott, D.; Seiffert, M. D.; Smoot, G. F.; Starck,
J. -L.; Stivoli, F.; Stolyarov, V.; Sudiwala, R.; Sygnet, J. -F.;
Tauber, J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Torre, J. -P.;
Tristram, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Varis, J.;
Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.;
Wilkinson, A.; Ysard, N.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..17P Altcode: 2011A&A...536A..17A; 2011arXiv1101.2046P
The integrated spectral energy distributions (SED) of the Large
Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) appear
significantly flatter than expected from dust models based on their
far-infrared and radio emission. The still unexplained origin of this
millimetre excess is investigated here using the Planck data. The
integrated SED of the two galaxies before subtraction of the foreground
(Milky Way) and background (CMB fluctuations) emission are in good
agreement with previous determinations, confirming the presence of the
millimetre excess. In the context of this preliminary analysis we do not
propose a full multi-component fitting of the data, but instead subtract
contributions unrelated to the galaxies and to dust emission. The
background CMB contribution is subtracted using an internal linear
combination (ILC) method performed locally around the galaxies. The
foreground emission from the Milky Way is subtracted as a Galactic Hi
template, and the dust emissivity is derived in a region surrounding the
two galaxies and dominated by Milky Way emission. After subtraction, the
remaining emission of both galaxies correlates closely with the atomic
and molecular gas emission of the LMC and SMC. The millimetre excess
in the LMC can be explained by CMB fluctuations, but a significant
excess is still present in the SMC SED. The Planck and IRAS-IRIS
data at 100 μm are combined to produce thermal dust temperature and
optical depth maps of the two galaxies. The LMC temperature map shows
the presence of a warm inner arm already found with the Spitzer data,
but which also shows the existence of a previously unidentified cold
outer arm. Several cold regions are found along this arm, some of
which are associated with known molecular clouds. The dust optical
depth maps are used to constrain the thermal dust emissivity power-law
index (β). The average spectral index is found to be consistent with
β = 1.5 and β = 1.2 below 500μm for the LMC and SMC respectively,
significantly flatter than the values observed in the Milky Way. Also,
there is evidence in the SMC of a further flattening of the SED in the
sub-mm, unlike for the LMC where the SED remains consistent with β =
1.5. The spatial distribution of the millimetre dustexcess in the SMC
follows the gas and thermal dust distribution. Different models are
explored in order to fit the dust emission in the SMC. It is concluded
that the millimetre excess is unlikely to be caused by very cold dust
emission and that it could be due to a combination of spinning dust
emission and thermal dust emission by more amorphous dust grains than
those present in our Galaxy. <P />Corresponding author: J.-P. Bernard,
e-mail: jean-philippe.bernard@cesr.fr
---------------------------------------------------------
Title: Planck early results. XVIII. The power spectrum of cosmic
infrared background anisotropies
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday,
A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.;
Benoît, A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Blagrave,
K.; Bock, J. J.; Bonaldi, A.; Bonavera, L.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Bucher, M.; Burigana, C.; Cabella, P.; Cardoso, J. -F.;
Catalano, A.; Cayón, L.; Challinor, A.; Chamballu, A.; Chiang, L. -Y.;
Chiang, C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot,
F.; Coulais, A.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies,
R. D.; Davis, R. J.; de Bernardis, P.; de Gasperis, G.; de Rosa, A.;
de Zotti, G.; Delabrouille, J.; Delouis, J. -M.; Désert, F. -X.;
Dole, H.; Donzelli, S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.;
Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Finelli, F.; Forni,
O.; Fosalba, P.; Frailis, M.; Franceschi, E.; Galeotta, S.; Ganga,
K.; Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo,
J.; Górski, K. M.; Grain, J.; Gratton, S.; Gregorio, A.; Gruppuso,
A.; Hansen, F. K.; Harrison, D.; Helou, G.; Henrot-Versillé, S.;
Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes,
W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.;
Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.;
Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.;
Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leonardi,
R.; Leroy, C.; Lilje, P. B.; Linden-Vørnle, M.; Lockman, F. J.;
López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; MacTavish,
C. J.; Maffei, B.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.;
Martin, P.; Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai,
F.; Mazzotta, P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.; Natoli, P.;
Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Novikov, D.; Novikov,
I.; O'Dwyer, I. J.; Oliver, S.; Osborne, S.; Pajot, F.; Pasian, F.;
Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini,
F.; Piat, M.; Pinheiro Gonçalves, D.; Plaszczynski, S.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Poutanen, T.; Prézeau, G.; Prunet, S.;
Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Reinecke, M.; Remazeilles,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusholme,
B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Seiffert, M. D.;
Shellard, P.; Smoot, G. F.; Starck, J. -L.; Stivoli, F.; Stolyarov,
V.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sygnet, J. -F.; Tauber,
J. A.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Torre, J. -P.;
Tristram, M.; Tuovinen, J.; Umana, G.; Valenziano, L.; Vielva, P.;
Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; White, M.;
Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..18P Altcode: 2011arXiv1101.2028P; 2011A&A...536A..18A
Using Planck maps of six regions of low Galactic dust emission with
a total area of about 140 deg<SUP>2</SUP>, we determine the angular
power spectra of cosmic infrared background (CIB) anisotropies from
multipole ℓ = 200 to ℓ = 2000 at 217, 353, 545 and 857 GHz. We use
21-cm observations of Hi as a tracer of thermal dust emission to reduce
the already low level of Galactic dust emission and use the 143 GHz
Planck maps in these fields to clean out cosmic microwave background
anisotropies. Both of these cleaning processes are necessary to avoid
significant contamination of the CIB signal. We measure correlated CIB
structure across frequencies. As expected, the correlation decreases
with increasing frequency separation, because the contribution
of high-redshift galaxies to CIB anisotropies increases with
wavelengths. We find no significant difference between the frequency
spectrum of the CIB anisotropies and the CIB mean, with ΔI / I = 15%
from 217 to 857 GHz. In terms of clustering properties, the Planck
data alone rule out the linear scale- and redshift-independent bias
model. Non-linear corrections are significant. Consequently, we develop
an alternative model that couples a dusty galaxy, parametric evolution
model with a simple halo-model approach. It provides an excellent fit
to the measured anisotropy angular power spectra and suggests that a
different halo occupation distribution is required at each frequency,
which is consistent with our expectation that each frequency is
dominated by contributions from different redshifts. In our best-fit
model, half of the anisotropy power at ℓ = 2000 comes from redshifts z
< 0.8 at 857 GHz and z < 1.5 at 545 GHz, while about 90% come from
redshifts z > 2 at 353 and 217 GHz, respectively. <P />Corresponding
author: G. Lagache, e-mail: guilaine.lagache@ias.u-psud.fr
---------------------------------------------------------
Title: Planck early results. XXII. The submillimetre properties of
a sample of Galactic cold clumps
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud, M.;
Ashdown, M.; Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.;
Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.; Bonaldi,
A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bucher,
M.; Burigana, C.; Cabella, P.; Cantalupo, C. M.; Cardoso, J. -F.;
Catalano, A.; Cayón, L.; Challinor, A.; Chamballu, A.; Chiang, L. -Y.;
Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.; Coulais,
A.; Crill, B. P.; Cuttaia, F.; Danese, L.; Davies, R. D.; de Bernardis,
P.; de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.;
Delouis, J. -M.; Désert, F. -X.; Dickinson, C.; Doi, Y.; Donzelli,
S.; Doré, O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.;
Enßlin, T. A.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis, M.;
Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.;
Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gratton,
S.; Gregorio, A.; Gruppuso, A.; Hansen, F. K.; Harrison, D.; Helou,
G.; Henrot-Versillé, S.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger,
K. M.; Ikeda, N.; Jaffe, A. H.; Jones, W. C.; Juvela, M.; Keihänen,
E.; Keskitalo, R.; Kisner, T. S.; Kitamura, Y.; Kneissl, R.; Knox,
L.; Kurki-Suonio, H.; Lagache, G.; Lamarre, J. -M.; Lasenby, A.;
Laureijs, R. J.; Lawrence, C. R.; Leach, S.; Leonardi, R.; Leroy, C.;
Linden-Vørnle, M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez,
J. F.; MacTavish, C. J.; Maffei, B.; Malinen, J.; Mandolesi, N.; Mann,
R.; Maris, M.; Marshall, D. J.; Martin, P.; Martínez-González,
E.; Masi, S.; Matarrese, S.; Matthai, F.; Mazzotta, P.; McGehee,
P.; Melchiorri, A.; Mendes, L.; Mennella, A.; Meny, C.; Mitra,
S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.; Morgante,
G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.; Nati, F.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Pagani, L.; Pajot, F.;
Paladini, R.; Pasian, F.; Patanchon, G.; Pelkonen, V. -M.; Perdereau,
O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat, M.; Plaszczynski,
S.; Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Poutanen, T.;
Prézeau, G.; Prunet, S.; Puget, J. -L.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli,
I.; Rocha, G.; Rosset, C.; Rowan-Robinson, M.; Rubiño-Martín, J. A.;
Rusholme, B.; Sandri, M.; Santos, D.; Savini, G.; Scott, D.; Seiffert,
M. D.; Smoot, G. F.; Starck, J. -L.; Stivoli, F.; Stolyarov, V.;
Sudiwala, R.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti,
L.; Tomasi, M.; Torre, J. -P.; Toth, V.; Tristram, M.; Tuovinen, J.;
Umana, G.; Valenziano, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade,
L. A.; Wandelt, B. D.; Ysard, N.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A..22P Altcode: 2011arXiv1101.2034P; 2011A&A...536A..22A
We perform a detailed investigation of sources from the Cold Cores
Catalogue of Planck Objects (C3PO). Our goal is to probe the reliability
of the detections, validate the separation between warm and cold
dust emission components, provide the first glimpse at the nature,
internal morphology and physical characterictics of the Planck-detected
sources. We focus on a sub-sample of ten sources from the C3PO list,
selected to sample different environments, from high latitude cirrus to
nearby (150pc) and remote (2kpc) molecular complexes. We present Planck
surface brightness maps and derive the dust temperature, emissivity
spectral index, and column densities of the fields. With the help
of higher resolution Herschel and AKARI continuum observations and
molecular line data, we investigate the morphology of the sources and
the properties of the substructures at scales below the Planck beam
size. The cold clumps detected by Planck are found to be located on
large-scale filamentary (or cometary) structures that extend up to
20pc in the remote sources. The thickness of these filaments ranges
between 0.3 and 3pc, for column densities N<SUB>H<SUB>2</SUB></SUB> ~
0.1 to 1.6 × 10<SUP>22</SUP> cm<SUP>-2</SUP>, and with linear mass
density covering a broad range, between 15 and 400 M<SUB>⊙</SUB>
pc<SUP>-1</SUP>. The dust temperatures are low (between 10 and 15K) and
the Planck cold clumps correspond to local minima of the line-of-sight
averaged dust temperature in these fields. These low temperatures are
confirmed when AKARI and Herschel data are added to the spectral energy
distributions. Herschel data reveal a wealth of substructure within
the Planck cold clumps. In all cases (except two sources harbouring
young stellar objects), the substructures are found to be colder,
with temperatures as low as 7K. Molecular line observations provide
gas column densities which are consistent with those inferred from
the dust. The linewidths are all supra-thermal, providing large
virial linear mass densities in the range 10 to 300 M<SUB>⊙</SUB>
pc<SUP>-1</SUP>, comparable within factors of a few, to the gas linear
mass densities. The analysis of this small set of cold clumps already
probes a broad variety of structures in the C3PO sample, probably
associated with different evolutionary stages, from cold and starless
clumps, to young protostellar objects still embedded in their cold
surrounding cloud. Because of the all-sky coverage and its sensitivity,
Planck is able to detect and locate the coldest spots in massive
elongated structures that may be the long-searched for progenitors of
stellar clusters. <P />Appendix A is available in electronic form at
<A href="http://www.aanda.org">http://www.aanda.org</A>Corresponding
author: I. Ristorcelli, e-mail: isabelle.ristorcelli@irap.omp.eu
---------------------------------------------------------
Title: Planck early results. IX. XMM-Newton follow-up for validation
of Planck cluster candidates
Authors: Planck Collaboration; Aghanim, N.; Arnaud, M.; Ashdown, M.;
Aumont, J.; Baccigalupi, C.; Balbi, A.; Banday, A. J.; Barreiro, R. B.;
Bartelmann, M.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît,
A.; Bernard, J. -P.; Bersanelli, M.; Bhatia, R.; Bock, J. J.; Bonaldi,
A.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Brown, M. L.; Bucher, M.;
Burigana, C.; Cabella, P.; Cantalupo, C. M.; Cardoso, J. -F.; Carvalho,
P.; Catalano, A.; Cayón, L.; Challinor, A.; Chamballu, A.; Chiang,
L. -Y.; Chon, G.; Christensen, P. R.; Churazov, E.; Clements, D. L.;
Colafrancesco, S.; Colombi, S.; Couchot, F.; Coulais, A.; Crill, B. P.;
Cuttaia, F.; da Silva, A.; Dahle, H.; Danese, L.; de Bernardis, P.;
de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Delouis,
J. -M.; Désert, F. -X.; Diego, J. M.; Dolag, K.; Donzelli, S.; Doré,
O.; Dörl, U.; Douspis, M.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.;
Finelli, F.; Flores-Cacho, I.; Forni, O.; Frailis, M.; Franceschi,
E.; Fromenteau, S.; Galeotta, S.; Ganga, K.; Génova-Santos, R. T.;
Giard, M.; Giardino, G.; Giraud-Héraud, Y.; González-Nuevo, J.;
González-Riestra, R.; Górski, K. M.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Harrison, D.; Heinämäki, P.; Henrot-Versillé, S.;
Hernández-Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.;
Hobson, M.; Holmes, W. A.; Hovest, W.; Hoyland, R. J.; Huffenberger,
K. M.; Hurier, G.; Jaffe, A. H.; Juvela, M.; Keihänen, E.; Keskitalo,
R.; Kisner, T. S.; Kneissl, R.; Knox, L.; Kurki-Suonio, H.; Lagache,
G.; Lamarre, J. -M.; Lasenby, A.; Laureijs, R. J.; Lawrence, C. R.;
Le Jeune, M.; Leach, S.; Leonardi, R.; Liddle, A.; Linden-Vørnle,
M.; López-Caniego, M.; Lubin, P. M.; Macías-Pérez, J. F.; Maffei,
B.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Marleau, F.;
Martínez-González, E.; Masi, S.; Matarrese, S.; Matthai, F.;
Mazzotta, P.; Melchiorri, A.; Melin, J. -B.; Mendes, L.; Mennella,
A.; Mitra, S.; Miville-Deschênes, M. -A.; Moneti, A.; Montier, L.;
Morgante, G.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.;
Natoli, P.; Netterfield, C. B.; Nørgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; Osborne, S.; Pajot, F.; Pasian, F.;
Patanchon, G.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini,
F.; Piat, M.; Pierpaoli, E.; Piffaretti, R.; Plaszczynski, S.;
Pointecouteau, E.; Polenta, G.; Ponthieu, N.; Poutanen, T.; Pratt,
G. W.; Prézeau, G.; Prunet, S.; Puget, J. -L.; Rebolo, R.; Reinecke,
M.; Renault, C.; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha,
G.; Rosset, C.; Rubiño-Martín, J. A.; Rusholme, B.; Saar, E.;
Sandri, M.; Santos, D.; Schaefer, B. M.; Scott, D.; Seiffert, M. D.;
Smoot, G. F.; Starck, J. -L.; Stivoli, F.; Stolyarov, V.; Sunyaev,
R.; Sygnet, J. -F.; Tauber, J. A.; Terenzi, L.; Toffolatti, L.;
Tomasi, M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Valenziano,
L.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wandelt, B. D.;
White, S. D. M.; Yvon, D.; Zacchei, A.; Zonca, A.
2011A&A...536A...9P Altcode: 2011A&A...536A...9A; 2011arXiv1101.2025P
We present the XMM-Newton follow-up for confirmation of Planck cluster
candidates. Twenty-five candidates have been observed to date using
snapshot (~10ks) exposures, ten as part of a pilot programme to
sample a low range of signal-to-noise ratios (4 < S/N < 6),
and a further 15 in a programme to observe a sample of S/N > 5
candidates. The sensitivity and spatial resolution of XMM-Newton allows
unambiguous discrimination between clusters and false candidates. The
4 false candidates have S/N ≤ 4.1. A total of 21 candidates are
confirmed as extended X-ray sources. Seventeen are single clusters,
the majority of which are found to have highly irregular and disturbed
morphologies (about ~70%). The remaining four sources are multiple
systems, including the unexpected discovery of a supercluster at z =
0.45. For 20 sources we are able to derive a redshift estimate from
the X-ray Fe K line (albeit of variable quality). The new clusters
span the redshift range 0.09 ≲ z ≲ 0.54, with a median redshift
of z ~ 0.37. A first determination is made of their X-ray properties
including the characteristic size, which is used to improve the
estimate of the SZ Compton parameter, Y<SUB>500</SUB>. The follow-up
validation programme has helped to optimise the Planck candidate
selection process. It has also provided a preview of the X-ray
properties of these newly-discovered clusters, allowing comparison
with their SZ properties, and to the X-ray and SZ properties of
known clusters observed in the Planck survey. Our results suggest
that Planck may have started to reveal a non-negligible population
of massive dynamically perturbed objects that is under-represented in
X-ray surveys. However, despite their particular properties, these new
clusters appear to follow the Y<SUB>500</SUB>-Y<SUB>X</SUB> relation
established for X-ray selected objects, where Y<SUB>X</SUB> is the
product of the gas mass and temperature. <P />Corresponding author:
E. Pointecouteau, e-mail: etienne.pointecouteau@irap.omp.eu
---------------------------------------------------------
Title: Subaru Weak-lensing Study of A2163: Bimodal Mass Structure
Authors: Okabe, N.; Bourdin, H.; Mazzotta, P.; Maurogordato, S.
2011ApJ...741..116O Altcode: 2011arXiv1107.0004O
We present a weak-lensing analysis of the merging cluster A2163 using
Subaru/Suprime-Cam and CFHT/Mega-Cam data and discuss the dynamics of
this cluster merger, based on complementary weak-lensing, X-ray, and
optical spectroscopic data sets. From two-dimensional multi-component
weak-lensing analysis, we reveal that the cluster mass distribution is
well described by three main components including the two-component
main cluster A2163-A with mass ratio 1:8, and its cluster satellite
A2163-B. The bimodal mass distribution in A2163-A is similar to the
galaxy density distribution, but appears as spatially segregated
from the brightest X-ray emitting gas region. We discuss the possible
origins of this gas-dark-matter offset and suggest the gas core of the
A2163-A subcluster has been stripped away by ram pressure from its dark
matter component. The survival of this gas core from the tidal forces
exerted by the main cluster lets us infer a subcluster accretion with
a non-zero impact parameter. Dominated by the most massive component
of A2163-A, the mass distribution of A2163 is well described by a
universal Navarro-Frenk-White profile as shown by a one-dimensional
tangential shear analysis, while the singular-isothermal sphere
profile is strongly ruled out. Comparing this cluster mass profile with
profiles derived assuming intracluster medium hydrostatic equilibrium
(H.E.) in two opposite regions of the cluster atmosphere has allowed
us to confirm the prediction of a departure from H.E. in the eastern
cluster side, presumably due to shock heating. Yielding a cluster mass
estimate of M <SUB>500</SUB> = 11.18<SUP>+1.64</SUP> <SUB> - 1.46</SUB>
× 10<SUP>14</SUP> h <SUP>-1</SUP> M <SUB>⊙</SUB>, our mass profile
confirms the exceptionally high mass of A2163, consistent with previous
analyses relying on the cluster dynamical analysis and Y <SUB>X</SUB>
mass proxy. <P />This work is based in part on data collected at
Subaru Telescope and obtained from the SMOKA, which is operated by
the Astronomy Data Center, National Astronomical Observatory of Japan.
---------------------------------------------------------
Title: Discovery of the correspondence between intra-cluster
radio emission and a high pressure region detected through the
Sunyaev-Zel'dovich effect
Authors: Ferrari, C.; Intema, H. T.; Orrù, E.; Govoni, F.; Murgia,
M.; Mason, B.; Bourdin, H.; Asad, K. M.; Mazzotta, P.; Wise, M. W.;
Mroczkowski, T.; Croston, J. H.
2011A&A...534L..12F Altcode: 2011arXiv1107.5945F
We analyzed new 237 MHz and 614 MHz GMRT data of the most X-ray luminous
galaxy cluster, RX J1347-1145. Our radio results are compared with
the MUSTANG 90 GHz Sunyaev-Zel'dovich effect map and with re-processed
Chandra and XMM-Newton archival data of this cluster. We point out for
the first time in an unambiguous way the correspondence between a radio
excess in a diffuse intra-cluster radio source and a hot region detected
through both Sunyaev-Zel'dovich effect and X-ray observations. Our
result indicates that electron re-acceleration in the excess emission
of the radio mini-halo at the center of RX J1347-1145 is most likely
related to a shock front propagating into the intra-cluster medium.
---------------------------------------------------------
Title: a Detailed Chandra/hst Study of the First z approx 1 Cluster
Blindly Discovered in the Planck all Sky Survey
Authors: Mazzotta, Pasquale
2011hst..prop12757M Altcode:
PLCKG266.6-27.3 is the first Planck blindly discovered cluster of
galaxies at z=1. Consistent with expectations for high z Planck-detected
clusters, a 10ks XMM observation confirms that it is an exceptional
system: with its L500=15 10^44 ergs^-1, T500=11.6pm1.4keV, and
M500=7.8pm1.0 10^14 M it is the most luminous cluster known at z
> 0.5 and one of the most {if not the most} massive cluster at
redshift z>1. Furthermore, unlike other high redshift clusters,
PLCKG266.6-27.3 is likely to be a relaxed system so potentially ideal
to make accurate hydrostatic mass measurements. We propose a joint
Chandra-HST observation of PLCKG266.6-27.3 to confirm the relaxed
dynamical status and, for the first time, to compare weak lensing and
hydrostatic measurements in a z=1 cluster.
---------------------------------------------------------
Title: a Detailed Chandra/hst Study of the First z approx 1 Cluster
Blindly Discovered in the Planck all Sky Survey
Authors: Mazzotta, Pasquale
2011cxo..prop.3451M Altcode:
PLCKG266.6-27.3 is the first Planck blindly discovered cluster of
galaxies at z=1. Consistent with expectations for high z Planck-detected
clusters, a 10ks XMM observation confirms that it is an exceptional
system: with its L500=15 10^44 ergs^-1, T500=11.6pm1.4keV, and
M500=7.8pm1.0 10^14 M it is the most luminous cluster known at z
> 0.5 and one of the most (if not the most) massive cluster at
redshift z>1. Furthermore, unlike other high redshift clusters,
PLCKG266.6-27.3 is likely to be a relaxed system so potentially ideal
to make accurate hydrostatic mass measurements. We propose a joint
Chandra-HST observation of PLCKG266.6-27.3 to confirm the relaxed
dynamical status and, for the first time, to compare weak lensing and
hydrostatic measurements in a z=1 cluster.
---------------------------------------------------------
Title: Chandra Archival Study of Planck Clusters
Authors: Mazzotta, Pasquale
2011cxo..prop.4242M Altcode:
This archive proposal is linked to the X-ray Visionary Project number
13800087, The Chandra-Planck Cluster Legacy, whose primary scientific
goals is to characterize the massive clusters in the local (z <
0.5) Universe found through the Planck SZ analysis. To be completed,
the project requires Chandra observations for all the 189 clusters in
the Planck ESZ sample. With this archive proposal we request funding
to perform the analysis of the 109 Cluster already available into
the archive.
---------------------------------------------------------
Title: A Combined Low-radio Frequency/X-ray Study of Galaxy
Groups. I. Giant Metrewave Radio Telescope Observations at 235 MHz
AND 610 MHz
Authors: Giacintucci, Simona; O'Sullivan, Ewan; Vrtilek, Jan; David,
Laurence P.; Raychaudhury, Somak; Venturi, Tiziana; Athreya, Ramana M.;
Clarke, Tracy E.; Murgia, Matteo; Mazzotta, Pasquale; Gitti, Myriam;
Ponman, Trevor; Ishwara-Chandra, C. H.; Jones, Christine; Forman,
William R.
2011ApJ...732...95G Altcode: 2011arXiv1103.1364G
We present new Giant Metrewave Radio Telescope observations at 235
MHz and 610 MHz of 18 X-ray bright galaxy groups. These observations
are part of an extended project, presented here and in future papers,
which combines low-frequency radio and X-ray data to investigate
the interaction between central active galactic nuclei (AGNs) and
the intra-group medium (IGM). The radio images show a very diverse
population of group-central radio sources, varying widely in size,
power, morphology, and spectral index. Comparison of the radio images
with Chandra and XMM-Newton X-ray images shows that groups with
significant substructure in the X-ray band and marginal radio emission
at gsim1 GHz host low-frequency radio structures that correlate with
substructures in IGM. Radio-filled X-ray cavities, the most evident form
of AGN/IGM interaction in our sample, are found in half of the systems
and are typically associated with small, low-, or mid-power double radio
sources. Two systems, NGC5044 and NGC4636, possess multiple cavities,
which are isotropically distributed around the group center, possibly
due to group weather. In other systems the radio/X-ray correlations
are less evident. However, the AGN/IGM interaction can manifest itself
through the effects of the high-pressure medium on the morphology,
spectral properties, and evolution of the radio-emitting plasma. In
particular, the IGM can confine fading radio lobes in old/dying
radio galaxies and prevent them from dissipating quickly. Evidence
for radio emission produced by former outbursts that co-exist with
current activity is found in six groups of the sample.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Massive galaxy clusters lensing
analyse (Richard+, 2010)
Authors: Richard, J.; Smith, G. P.; Kneib, J. -P.; Ellis, R. S.;
Sanderson, A. J. R.; Pei, L.; Targett, T. A.; Sand, D. J.; Swinbank,
A. M.; Dannerbauer, H.; Mazzotta, P.; Limousin, M.; Egami, E.; Jullo,
E.; Hamilton-Morris, V.; Moran, S. M.
2011yCat..74040325R Altcode:
High-resolution imaging data taken with the Advanced Camera for Surveys
(ACS) or Wide Field Planetary Camera 2 (WFPC2) instrument on HST
are available for each selected cluster in one or two bands, either
through our dedicated LoCuSS programme (GO-DD 11312, PI: G.P. Smith)
or from the archive. <P />J- and KS-band data were obtained between
2003 March and 2007 April on the following near-infrared instruments:
Wide Infrared Camera (WIRC) on the Palomar-200-inch telescope, Infrared
Side Port Imager (ISPI) on the CTIO Blanco 4-m telescope and Florida
Infrared Imaging Multi-Object Spectrograph (FLAMINGOS) on the Kitt Peak
(KPNO) 4-m telescope. <P />We used the LRIS on the Keck-I telescope
to perform long-slit and multislit observations of the clusters. The
spectroscopic data used in the current paper are the outcome of six
different observing runs between 2004 and 2008. <P />(1 data file).
---------------------------------------------------------
Title: The stellar and hot gas content of low-mass galaxy clusters
Authors: Balogh, Michael L.; Mazzotta, Pasquale; Bower, Richard G.;
Eke, Vince; Bourdin, Hervé; Lu, Ting; Theuns, Tom
2011MNRAS.412..947B Altcode: 2010arXiv1011.0602B; 2010MNRAS.tmp.1842B
We analyse the stellar and hot gas content of 18 nearby, low-mass
galaxy clusters, detected in redshift space and selected to have a
dynamical mass 3 × 10<SUP>14</SUP> < M/M<SUB>⊙</SUB> < 6 ×
10<SUP>14</SUP> (h= 0.7), as measured from the 2dF Galaxy Redshift
Survey. We combine X-ray measurements from both Chandra and XMM with
ground-based near-infrared observations from CTIO, Anglo-Australian
Telescope and Canada-France-Hawaii Telescope to compare the mass in hot
gas and stars to the dynamical mass and state of the clusters. Only 13
of the clusters are detected in X-ray emission, and for these systems we
find that a range of 7-20 per cent of their baryonic mass, and <3 per
cent of their dynamical mass, is detected in starlight, similar to what
is observed in more massive clusters. In contrast, the five undetected
clusters are underluminous in X-ray emission, by up to a factor of
10, given their stellar mass. Although the velocity distribution of
cluster members in these systems is indistinguishable from a Gaussian,
all show subtle signs of being unrelaxed: either they lack a central,
dominant galaxy, or the bright galaxy distribution is less concentrated
and/or more elongated than the rest of the sample. Thus we conclude that
low-mass clusters and groups selected from the velocity distribution of
their galaxies exhibit a dichotomy in their hot gas properties. Either
they are detected in X-ray, in which case they generally lie on the
usual scaling relations, or they are completely undetected in X-ray
emission. The non-detections may be partly related to the apparently
young dynamical state of the clusters, but it remains a distinct
possibility that some of these systems are exceptionally devoid of
hot emitting gas as the result of its expulsion or rarefaction.
---------------------------------------------------------
Title: Scaling Relation in Two Situations of Extreme Mergers
Authors: Rasia, E.; Mazzotta, P.; Evrard, A.; Markevitch, M.; Dolag,
K.; Meneghetti, M.
2011ApJ...729...45R Altcode: 2010arXiv1012.4027R
Clusters of galaxies are known to be dynamically active systems, yet
X-ray studies of the low-redshift population exhibit tight scaling
laws. In this work, we extend previous studies of this apparent paradox
using numerical simulations of two extreme merger cases, one is a high
Mach number (above 2.5) satellite merger similar to the "bullet cluster"
and the other is a merger of nearly equal-mass progenitors. Creating
X-ray images densely sampled in time, we construct T <SUB>X</SUB>,
M <SUB>gas</SUB>, and Y <SUB>X</SUB> measures within R <SUB>500</SUB>
and compare to the calibrations of Kravtsov et al. We find that these
extreme merger cases respect the scaling relations, for both intrinsic
measures and for measures derived from appropriately masked, synthetic
Chandra X-ray images. The masking procedure plays a critical role in
the X-ray temperature calculation, while it is irrelevant in the X-ray
gas mass derivation. Miscentering up to 100 kpc does not influence the
result. The observationally determined radius R <SUB>500</SUB> might
conduce to systematic shifts in M <SUB>gas</SUB> and Y <SUB>X</SUB>,
which increases the total mass scatter.
---------------------------------------------------------
Title: A2163: Merger events in the hottest Abell galaxy
cluster. II. Subcluster accretion with galaxy-gas separation
Authors: Bourdin, H.; Arnaud, M.; Mazzotta, P.; Pratt, G. W.;
Sauvageot, J. -L.; Martino, R.; Maurogordato, S.; Cappi, A.; Ferrari,
C.; Benoist, C.
2011A&A...527A..21B Altcode: 2010arXiv1011.3154B
Located at z = 0.203, A2163 is a rich galaxy cluster with an
intra-cluster medium (ICM) that exhibits extraordinary properties,
including an exceptionally high X-ray luminosity, average temperature,
and a powerful and extended radio halo. The irregular and complex
morphology of its gas and galaxy structure suggests that this cluster
has recently undergone major merger events that involve two or more
cluster components. In this paper, we study the gas structure and
dynamics by means of spectral-imaging analysis of X-ray data obtained
from XMM-Newton and Chandra observations. From the evidence of a cold
front, we infer the westward motion of a cool core across the E-W
elongated atmosphere of the main cluster A2163-A. Located close to a
galaxy over-density, this gas "bullet" appears to have been spatially
separated from its galaxy (and presumably dark matter component) as a
result of high-velocity accretion. From gas brightness and temperature
profile analysis performed in two opposite regions of the main cluster,
we show that the ICM has been adiabatically compressed behind the
crossing "bullet" possibly because of shock heating, leading to a
strong departure of the ICM from hydrostatic equilibrium in this
region. Assuming that the mass estimated from the Y<SUB>X</SUB>
proxy best indicates the overall mass of the system and that the
western cluster sector is in approximate hydrostatic equilibrium
before subcluster accretion, we infer a merger scenario between two
subunits of mass ratio 1:4, leading to a present total system mass of
M<SUB>500</SUB> ≃ 1.9 × 10<SUP>15</SUP> M<SUB>⊙</SUB>. Additional
analysis of the spatially-separated northern subcluster A2163-B does
not show any evidence of strong interaction with the main cluster
A2163-A, leading us to infer that the physical distance separating the
northern subcluster and the main component is longer than the projected
separation of these components. The exceptional properties of A2163
present various similarities with those of 1E0657-56, the so-called
"bullet-cluster". These similarities are likely to be related to a
comparable merger scenario.
---------------------------------------------------------
Title: Overview of the Planck Cluster SZ Results
Authors: Mazzotta, Pasquale
2011gcca.progE...6M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Study of the M shock wave propagation in RXJ1314.4-2515
Authors: Mazzotta, P.; Bourdin, H.; Giacintucci, S.; Markevitch, M.;
Venturi, T.
2011MmSAI..82..495M Altcode:
We present the analysis of XMM-Newton observations of the merging
cluster of galaxies RXJ1314.4-2515. The cluster is known to host a small
radio halo at its center and two Mpc-size relics in the outskirts,
one to the east and one to the west. The XMM-Newton observation
reveals the presence of a shock underlying the western relic. The
outer border of the relic is remarkably coincident with the shock
front. This provides important support to the shock (re)acceleration
models as likely mechanisms behind the formation of the radio relics
in clusters. Very interestingly the shock, which seems to propagate
with a Mach number of 2.5, also shows an M-like shape with the nose
of the front slightly tilted inward which is likely produced by the
material infalling along the filament.
---------------------------------------------------------
Title: VizieR Online Data Catalog: Planck Early Release Compact
Source Catalogue (Planck, 2011)
Authors: Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Arnaud,
M.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Baker, M.; Balbi,
A.; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.;
Benabed, K.; Bennett, K.; Benoit, A.; Bernard, J. -P.; Bersanelli,
M.; Bhatia, R.; Bock, J. J.; Bonaldi, A.; Bond, J. R.; Borrill, J.;
Bouchet, F. R.; Bradshaw, T.; Bremer, M.; Bucher, M.; Burigana, C.;
Butler, R. C.; Cabella, P.; Cantalupo, C. M.; Cappellini, B.; Cardoso,
J. -F.; Carr, R.; Casale, M.; Catalano, A.; Cayon, L.; Challinor, A.;
Chamballu, A.; Charra, J.; Chary, R. -R.; Chiang, L. -Y.; Chiang,
C.; Christensen, P. R.; Clements, D. L.; Colombi, S.; Couchot, F.;
Coulais, A.; Crill, B. P.; Crone, G.; Crook, M.; Cuttaia, F.; Danese,
L.; D'Arcangelo, O.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de
Bruin, J.; de Gasperis, G.; de Rosa, A.; de Zotti, G.; Delabrouille,
J.; Delouis, J. -M.; Desert, F. -X.; Dick, J.; Dickinson, C.; Dolag,
K.; Dole, H.; Donzelli, S.; Dore, O.; Doerl, U.; Douspis, M.; Dupac,
X.; Efstathiou, G.; Ensslin, T. A.; Eriksen, H. K.; Finelli, F.; Foley,
S.; Forni, O.; Fosalba, P.; Frailis, M.; Franceschi, E.; Freschi, M.;
Gaier, T. C.; Galeotta, S.; Gallegos, J.; Gandolfo, B.; Ganga, K.;
Giard, M.; Giardino, G.; Gienger, G.; Giraud-Heraud, Y.; Gonzalez,
J.; Gonzalez-Nuevo, J.; Gorski, K. M.; Gratton, S.; Gregorio, A.;
Gruppuso, A.; Guyot, G.; Haissinski, J.; Hansen, F. K.; Harrison, D.;
Helou, G.; Henrot-Versille, S.; Hernandez-Monteagudo, C.; Herranz, D.;
Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup,
A.; Hovest, W.; Hoyland, R. J.; Huffenberger, K. M.; Jaffe, A. H.;
Jagemann, T.; Jones, W. C.; Juillet, J. J.; Juvela, M.; Kangaslahti,
P.; Keihaenen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knox,
L.; Krassenburg, M.; Kurki-Suonio, H.; Lagache, G.; Laehteenmaeki,
A.; Lamarre, J. -M.; Lange, A. E.; Lasenby, A.; Laureijs, R. J.;
Lawrence, C. R.; Leach, S.; Leahy, J. P.; Leonardi, R.; Leroy, C.;
Lilje, P. B.; Linden-Vornle, M.; Lopez-Caniego, M.; Lowe, S.; Lubin,
P. M.; Macias-Perez, J. F.; Maciaszek, T.; MacTavish, C. J.; Maffei,
B.; Maino, D.; Mandolesi, N.; Mann, R.; Maris, M.; Martinez-Gonzalez,
E.; Masi, S.; Massardi, M.; Matarrese, S.; Matthai, F.; Mazzotta, P.;
McDonald, A.; McGehee, P.; Meinhold, P. R.; Melchiorri, A.; Melin,
J. -B.; Mendes, L.; Mennella, A.; Mevi, C.; Miniscalco, R.; Mitra,
S.; Miville-Deschenes, M. -A.; Moneti, A.; Montier, L.; Morgante, G.;
sMorisset, N.; Mortlock, D.; Munshi, D.; Murphy, A.; Naselsky, P.;
Natoli, P.; Netterfield, C. B.; Norgaard-Nielsen, H. U.; Noviello,
F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Ortiz, I.; Osborne,
S.; Osuna, P.; Oxborrow, C. A.; Pajot, F.; Paladini, R.; Partridge,
B.; Pasian, F.; Passvogel, T.; Patanchon, G.; Pearson, D.; Pearson,
T. J.; Perdereau, O.; Perotto, L.; Perrotta, F.; Piacentini, F.; Piat,
M.; Pierpaoli, E.; Plaszczynski, S.; Platania, P.; Pointecouteau,
E.; Polenta, G.; Ponthieu, N.; Popa, L.; Poutanen, T.; Prezeau, G.;
Prunet, S.; Puget, J. -L.; Rachen, J. P.; Reach, W. T.; Rebolo, R.;
Reinecke, M.; Reix, J. -M.; Renault, C.; Ricciardi, S.; Riller,
T.; Ristorcelli, I.; Rocha, G.; Rosset, C.; Rowan-Robinson,
M.; Rubino-Martin, J. A.; Rusholme, B.; Salerno, E.; Sandri, M.;
Santos, D.; Savini, G.; Schaefer, B. M.; Scott, D.; Seiffert, M. D.;
Shellard, P.; Simonetto, A.; Smoot, G. F.; Sozzi, C.; Starck, J. -L.;
Sternberg, J.; Stivoli, F.; Stolyarov, V.; Stompor, R.; Stringhetti,
L.; Sudiwala, R.; Sunyaev, R.; Sygnet, J. -F.; Tapiador, D.; Tauber,
J. A.; Tavagnacco, D.; Taylor, D.; Terenzi, L.; Texier, D.; Toffolatti,
L.; Tomasi, M.; Torre, J. -P.; Tristram, M.; Tuovinen, J.; Tuerler,
M.; Tuttlebee, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Varis,
J.; Vibert, L.; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.;
Wandelt, B. D.; Watson, C.; White, S. D. M.; White, M.; Wilkinson,
A.; Yvon, D.; Zacchei, A.; Zonca, A.
2011yCat.8088....0P Altcode:
Planck is a European Space Agency (ESA) mission, with significant
contributions from the U.S. National Aeronautics and Space Agency
(NASA). It is the third generation of space-based cosmic microwave
background experiments, after the Cosmic Background Explorer (COBE) and
the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on
14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following
a cruise to the Earth-Sun L2 Lagrange point, cooling and in orbit
checkout, Planck initiated the First Light Survey on 13 August
2009. Since then, Planck has been continuously measuring the intensity
of the sky over a range of frequencies from 30 to 857GHz (wavelengths
of 1cm to 350μm) with spatial resolutions ranging from about 33'
to 5' respectively. The Low Frequency Instrument (LFI) on Planck
provides temperature and polarization information using radiometers
which operate between 30 and 70GHz. The High Frequency Instrument
(HFI) uses pairs of polarization-sensitive bolometers at each of four
frequencies between 100 and 353GHz but does not measure polarization
information in the two upper HFI bands at 545 and 857GHz. The lowest
frequencies overlap with WMAP, and the highest frequencies extend far
into the submillimeter in order to improve separation between Galactic
foregrounds and the cosmic microwave background (CMB). By extending
to wavelengths longer than those at which the Infrared Astronomical
Satellite (IRAS) operated, Planck is providing an unprecedented window
into dust emission at far-infrared and submillimeter wavelengths. <P
/>The Planck Early Release Compact Source Catalogue (ERCSC) is a list
of all high reliability sources, both Galactic and extragalactic,
derived from the first sky coverage. The data that went into this
early release comprise all observations undertaken between 13 August
2009 and 6 June 2010, corresponding to Planck operational days
91-389. Since the Planck scan strategy results in the entire sky
being observed every 6 months, the data considered in this release
correspond to more than the first sky coverage. The source lists have
reliability goals of >90% across the entire sky and >95% at high
Galactic latitude. The goals on photometric accuracy are 30% while the
positional accuracy goal translates to a positional root mean square
(RMS) uncertainty that is less than 1/5 of the beam full width at half
maximum (FWHM). <P />Detailed explanations about the mission and the
catalogs included here can be found in the "Explanatory supplement"
(file "ercsc4_3.pdf"). Skymaps of the sources can be found in the
"skymaps" subdirectory; postage stamps of the sources in the ECC (Early
Cold Cores) catalog and in the different filters are located in the
"stamps" subdirectory. <P />The "Byte-by-byte Description" below contain
column names standardized according to the conventions used at CDS;
the original column names, as defined in the FITS files, are listed,
enclosed within parentheses, at the end of the explanations. <P />(16
data files).
---------------------------------------------------------
Title: Planck pre-launch status: The Planck mission
Authors: Tauber, J. A.; Mandolesi, N.; Puget, J. -L.; Banos, T.;
Bersanelli, M.; Bouchet, F. R.; Butler, R. C.; Charra, J.; Crone, G.;
Dodsworth, J.; Efstathiou, G.; Gispert, R.; Guyot, G.; Gregorio, A.;
Juillet, J. J.; Lamarre, J. -M.; Laureijs, R. J.; Lawrence, C. R.;
Nørgaard-Nielsen, H. U.; Passvogel, T.; Reix, J. M.; Texier, D.;
Vibert, L.; Zacchei, A.; Ade, P. A. R.; Aghanim, N.; Aja, B.; Alippi,
E.; Aloy, L.; Armand, P.; Arnaud, M.; Arondel, A.; Arreola-Villanueva,
A.; Artal, E.; Artina, E.; Arts, A.; Ashdown, M.; Aumont, J.; Azzaro,
M.; Bacchetta, A.; Baccigalupi, C.; Baker, M.; Balasini, M.; Balbi, A.;
Banday, A. J.; Barbier, G.; Barreiro, R. B.; Bartelmann, M.; Battaglia,
P.; Battaner, E.; Benabed, K.; Beney, J. -L.; Beneyton, R.; Bennett,
K.; Benoit, A.; Bernard, J. -P.; Bhandari, P.; Bhatia, R.; Biggi,
M.; Biggins, R.; Billig, G.; Blanc, Y.; Blavot, H.; Bock, J. J.;
Bonaldi, A.; Bond, R.; Bonis, J.; Borders, J.; Borrill, J.; Boschini,
L.; Boulanger, F.; Bouvier, J.; Bouzit, M.; Bowman, R.; Bréelle, E.;
Bradshaw, T.; Braghin, M.; Bremer, M.; Brienza, D.; Broszkiewicz, D.;
Burigana, C.; Burkhalter, M.; Cabella, P.; Cafferty, T.; Cairola, M.;
Caminade, S.; Camus, P.; Cantalupo, C. M.; Cappellini, B.; Cardoso,
J. -F.; Carr, R.; Catalano, A.; Cayón, L.; Cesa, M.; Chaigneau, M.;
Challinor, A.; Chamballu, A.; Chambelland, J. P.; Charra, M.; Chiang,
L. -Y.; Chlewicki, G.; Christensen, P. R.; Church, S.; Ciancietta,
E.; Cibrario, M.; Cizeron, R.; Clements, D.; Collaudin, B.; Colley,
J. -M.; Colombi, S.; Colombo, A.; Colombo, F.; Corre, O.; Couchot, F.;
Cougrand, B.; Coulais, A.; Couzin, P.; Crane, B.; Crill, B.; Crook,
M.; Crumb, D.; Cuttaia, F.; Dörl, U.; da Silva, P.; Daddato, R.;
Damasio, C.; Danese, L.; D'Aquino, G.; D'Arcangelo, O.; Dassas, K.;
Davies, R. D.; Davies, W.; Davis, R. J.; de Bernardis, P.; de Chambure,
D.; de Gasperis, G.; de La Fuente, M. L.; de Paco, P.; de Rosa, A.;
de Troia, G.; de Zotti, G.; Dehamme, M.; Delabrouille, J.; Delouis,
J. -M.; Désert, F. -X.; di Girolamo, G.; Dickinson, C.; Doelling,
E.; Dolag, K.; Domken, I.; Douspis, M.; Doyle, D.; Du, S.; Dubruel,
D.; Dufour, C.; Dumesnil, C.; Dupac, X.; Duret, P.; Eder, C.; Elfving,
A.; Enßlin, T. A.; Eng, P.; English, K.; Eriksen, H. K.; Estaria, P.;
Falvella, M. C.; Ferrari, F.; Finelli, F.; Fishman, A.; Fogliani, S.;
Foley, S.; Fonseca, A.; Forma, G.; Forni, O.; Fosalba, P.; Fourmond,
J. -J.; Frailis, M.; Franceschet, C.; Franceschi, E.; François, S.;
Frerking, M.; Gómez-Reñasco, M. F.; Górski, K. M.; Gaier, T. C.;
Galeotta, S.; Ganga, K.; García Lázaro, J.; Garnica, A.; Gaspard, M.;
Gavila, E.; Giard, M.; Giardino, G.; Gienger, G.; Giraud-Heraud, Y.;
Glorian, J. -M.; Griffin, M.; Gruppuso, A.; Guglielmi, L.; Guichon,
D.; Guillaume, B.; Guillouet, P.; Haissinski, J.; Hansen, F. K.;
Hardy, J.; Harrison, D.; Hazell, A.; Hechler, M.; Heckenauer, V.;
Heinzer, D.; Hell, R.; Henrot-Versillé, S.; Hernández-Monteagudo,
C.; Herranz, D.; Herreros, J. M.; Hervier, V.; Heske, A.; Heurtel,
A.; Hildebrandt, S. R.; Hills, R.; Hivon, E.; Hobson, M.; Hollert,
D.; Holmes, W.; Hornstrup, A.; Hovest, W.; Hoyland, R. J.; Huey, G.;
Huffenberger, K. M.; Hughes, N.; Israelsson, U.; Jackson, B.; Jaffe,
A.; Jaffe, T. R.; Jagemann, T.; Jessen, N. C.; Jewell, J.; Jones, W.;
Juvela, M.; Kaplan, J.; Karlman, P.; Keck, F.; Keihänen, E.; King,
M.; Kisner, T. S.; Kletzkine, P.; Kneissl, R.; Knoche, J.; Knox,
L.; Koch, T.; Krassenburg, M.; Kurki-Suonio, H.; Lähteenmäki, A.;
Lagache, G.; Lagorio, E.; Lami, P.; Lande, J.; Lange, A.; Langlet,
F.; Lapini, R.; Lapolla, M.; Lasenby, A.; Le Jeune, M.; Leahy, J. P.;
Lefebvre, M.; Legrand, F.; Le Meur, G.; Leonardi, R.; Leriche, B.;
Leroy, C.; Leutenegger, P.; Levin, S. M.; Lilje, P. B.; Lindensmith,
C.; Linden-Vørnle, M.; Loc, A.; Longval, Y.; Lubin, P. M.; Luchik,
T.; Luthold, I.; Macias-Perez, J. F.; Maciaszek, T.; MacTavish, C.;
Madden, S.; Maffei, B.; Magneville, C.; Maino, D.; Mambretti, A.;
Mansoux, B.; Marchioro, D.; Maris, M.; Marliani, F.; Marrucho, J. -C.;
Martí-Canales, J.; Martínez-González, E.; Martín-Polegre, A.;
Martin, P.; Marty, C.; Marty, W.; Masi, S.; Massardi, M.; Matarrese,
S.; Matthai, F.; Mazzotta, P.; McDonald, A.; McGrath, P.; Mediavilla,
A.; Meinhold, P. R.; Mélin, J. -B.; Melot, F.; Mendes, L.; Mennella,
A.; Mervier, C.; Meslier, L.; Miccolis, M.; Miville-Deschenes, M. -A.;
Moneti, A.; Montet, D.; Montier, L.; Mora, J.; Morgante, G.; Morigi,
G.; Morinaud, G.; Morisset, N.; Mortlock, D.; Mottet, S.; Mulder, J.;
Munshi, D.; Murphy, A.; Murphy, P.; Musi, P.; Narbonne, J.; Naselsky,
P.; Nash, A.; Nati, F.; Natoli, P.; Netterfield, B.; Newell, J.;
Nexon, M.; Nicolas, C.; Nielsen, P. H.; Ninane, N.; Noviello, F.;
Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Oldeman, P.; Olivier, P.;
Ouchet, L.; Oxborrow, C. A.; Pérez-Cuevas, L.; Pagan, L.; Paine,
C.; Pajot, F.; Paladini, R.; Pancher, F.; Panh, J.; Parks, G.;
Parnaudeau, P.; Partridge, B.; Parvin, B.; Pascual, J. P.; Pasian,
F.; Pearson, D. P.; Pearson, T.; Pecora, M.; Perdereau, O.; Perotto,
L.; Perrotta, F.; Piacentini, F.; Piat, M.; Pierpaoli, E.; Piersanti,
O.; Plaige, E.; Plaszczynski, S.; Platania, P.; Pointecouteau, E.;
Polenta, G.; Ponthieu, N.; Popa, L.; Poulleau, G.; Poutanen, T.;
Prézeau, G.; Pradell, L.; Prina, M.; Prunet, S.; Rachen, J. P.;
Rambaud, D.; Rame, F.; Rasmussen, I.; Rautakoski, J.; Reach, W. T.;
Rebolo, R.; Reinecke, M.; Reiter, J.; Renault, C.; Ricciardi, S.;
Rideau, P.; Riller, T.; Ristorcelli, I.; Riti, J. B.; Rocha, G.;
Roche, Y.; Pons, R.; Rohlfs, R.; Romero, D.; Roose, S.; Rosset, C.;
Rouberol, S.; Rowan-Robinson, M.; Rubiño-Martín, J. A.; Rusconi, P.;
Rusholme, B.; Salama, M.; Salerno, E.; Sandri, M.; Santos, D.; Sanz,
J. L.; Sauter, L.; Sauvage, F.; Savini, G.; Schmelzel, M.; Schnorhk,
A.; Schwarz, W.; Scott, D.; Seiffert, M. D.; Shellard, P.; Shih, C.;
Sias, M.; Silk, J. I.; Silvestri, R.; Sippel, R.; Smoot, G. F.; Starck,
J. -L.; Stassi, P.; Sternberg, J.; Stivoli, F.; Stolyarov, V.; Stompor,
R.; Stringhetti, L.; Strommen, D.; Stute, T.; Sudiwala, R.; Sugimura,
R.; Sunyaev, R.; Sygnet, J. -F.; Türler, M.; Taddei, E.; Tallon,
J.; Tamiatto, C.; Taurigna, M.; Taylor, D.; Terenzi, L.; Thuerey,
S.; Tillis, J.; Tofani, G.; Toffolatti, L.; Tommasi, E.; Tomasi,
M.; Tonazzini, E.; Torre, J. -P.; Tosti, S.; Touze, F.; Tristram,
M.; Tuovinen, J.; Tuttlebee, M.; Umana, G.; Valenziano, L.; Vallée,
D.; van der Vlis, M.; van Leeuwen, F.; Vanel, J. -C.; van-Tent, B.;
Varis, J.; Vassallo, E.; Vescovi, C.; Vezzu, F.; Vibert, D.; Vielva,
P.; Vierra, J.; Villa, F.; Vittorio, N.; Vuerli, C.; Wade, L. A.;
Walker, A. R.; Wandelt, B. D.; Watson, C.; Werner, D.; White, M.;
White, S. D. M.; Wilkinson, A.; Wilson, P.; Woodcraft, A.; Yoffo, B.;
Yun, M.; Yurchenko, V.; Yvon, D.; Zhang, B.; Zimmermann, O.; Zonca,
A.; Zorita, D.
2010A&A...520A...1T Altcode:
The European Space Agency's Planck satellite, launched on 14 May
2009, is the third-generation space experiment in the field of cosmic
microwave background (CMB) research. It will image the anisotropies of
the CMB over the whole sky, with unprecedented sensitivity ({{Δ T}over
T} 2 × 10<SUP>-6</SUP>) and angular resolution ( 5 arcmin). Planck
will provide a major source of information relevant to many fundamental
cosmological problems and will test current theories of the early
evolution of the Universe and the origin of structure. It will also
address a wide range of areas of astrophysical research related to the
Milky Way as well as external galaxies and clusters of galaxies. The
ability of Planck to measure polarization across a wide frequency range
(30-350 GHz), with high precision and accuracy, and over the whole
sky, will provide unique insight, not only into specific cosmological
questions, but also into the properties of the interstellar medium. This
paper is part of a series which describes the technical capabilities of
the Planck scientific payload. It is based on the knowledge gathered
during the on-ground calibration campaigns of the major subsystems,
principally its telescope and its two scientific instruments, and
of tests at fully integrated satellite level. It represents the best
estimate before launch of the technical performance that the satellite
and its payload will achieve in flight. In this paper, we summarise the
main elements of the payload performance, which is described in detail
in the accompanying papers. In addition, we describe the satellite
performance elements which are most relevant for science, and provide
an overview of the plans for scientific operations and data analysis.
---------------------------------------------------------
Title: Weighing simulated galaxy clusters using lensing and X-ray
Authors: Meneghetti, M.; Rasia, E.; Merten, J.; Bellagamba, F.;
Ettori, S.; Mazzotta, P.; Dolag, K.; Marri, S.
2010A&A...514A..93M Altcode: 2009arXiv0912.1343M
Context. Among the methods employed to measure the mass of galaxy
clusters, the techniques based on lensing and X-ray analyses are
perhaps the most widely used; however, the comparison between these
mass estimates is often difficult and, in several clusters, the
results apparently inconsistent. <BR /> Aims: We aim at investigating
potential biases in lensing and X-ray methods to measure the cluster
mass profiles. <BR /> Methods: We performed realistic simulations of
lensing and X-ray observations that were subsequently analyzed using
observational techniques. The resulting mass estimates were compared
with the input models. Three clusters obtained from state-of-the-art
hydrodynamical simulations, each of which projected along three
independent lines-of-sight, were used for this analysis. <BR />
Results: We find that strong lensing models can be trusted over
a limited region around the cluster core. Extrapolating the strong
lensing mass models to outside the Einstein ring can lead to significant
biases in the mass estimates, if the BCG is not modeled properly, for
example. Weak-lensing mass measurements can be strongly affected by
substructures, depending on the method implemented to convert the shear
into a mass estimate. Using nonparametric methods which combine weak
and strong lensing data, the projected masses within R<SUB>200</SUB>
can be constrained with a precision of ~10%. Deprojection of lensing
masses increases the scatter around the true masses by more than a
factor of two because of cluster triaxiality. X-ray mass measurements
have much smaller scatter (about a factor of two less than the lensing
masses), but they are generally biased toward low values between 5
and 10%. This bias is entirely ascribable to bulk motions in the gas
of our simulated clusters. Using the lensing and the X-ray masses as
proxies for the true and the hydrostatic equilibrium masses of the
simulated clusters and by averaging over the cluster sample, we are
able to measure the lack of hydrostatic equilibrium in the systems we
have investigated. <BR /> Conclusions: Although the comparison between
lensing and X-ray masses may be difficult in individual systems due to
triaxiality and substructures, using a large number of clusters with
both lensing and X-ray observations may lead to important information
about their gas physics and allow use of lensing masses to calibrate
the X-ray scaling relations.
---------------------------------------------------------
Title: LoCuSS: first results from strong-lensing analysis of 20
massive galaxy clusters at z = 0.2
Authors: Richard, Johan; Smith, Graham P.; Kneib, Jean-Paul; Ellis,
Richard S.; Sanderson, A. J. R.; Pei, L.; Targett, T. A.; Sand, D. J.;
Swinbank, A. M.; Dannerbauer, H.; Mazzotta, P.; Limousin, M.; Egami,
E.; Jullo, E.; Hamilton-Morris, V.; Moran, S. M.
2010MNRAS.404..325R Altcode: 2010MNRAS.tmp..313R; 2009arXiv0911.3302R
We present a statistical analysis of a sample of 20 strong
lensing clusters drawn from the Local Cluster Substructure Survey,
based on high-resolution Hubble Space Telescope imaging of the
cluster cores and follow-up spectroscopic observations using the
Keck-I telescope. We use detailed parametrized models of the mass
distribution in the cluster cores, to measure the total cluster mass
and fraction of that mass associated with substructures within R <=
250kpc. These measurements are compared with the distribution of
baryons in the cores, as traced by the old stellar populations and
the X-ray emitting intracluster medium. Our main results include:
(i) the distribution of Einstein radii is lognormal, with a peak
and 1σ width of <log<SUB>10</SUB>θ<SUB>E</SUB>(z = 2)> =
1.16 +/- 0.28; (ii) we detect an X-ray/lensing mass discrepancy of
<M<SUB>SL</SUB>/M<SUB>X</SUB>> = 1.3 at 3σ significance -
clusters with larger substructure fractions displaying greater mass
discrepancies, and thus greater departures from hydrostatic equilibrium
and (iii) cluster substructure fraction is also correlated with the
slope of the gas density profile on small scales, implying a connection
between cluster-cluster mergers and gas cooling. Overall our results are
consistent with the view that cluster-cluster mergers play a prominent
role in shaping the properties of cluster cores, in particular causing
departures from hydrostatic equilibrium, and possibly disturbing cool
cores. Our results do not support recent claims that large Einstein
radius clusters present a challenge to the cold dark matter paradigm.
---------------------------------------------------------
Title: LoCuSS: A Comparison of Cluster Mass Measurements from
XMM-Newton and Subaru—Testing Deviation from Hydrostatic Equilibrium
and Non-thermal Pressure Support
Authors: Zhang, Yu-Ying; Okabe, Nobuhiro; Finoguenov, Alexis; Smith,
Graham P.; Piffaretti, Rocco; Valdarnini, Riccardo; Babul, Arif;
Evrard, August E.; Mazzotta, Pasquale; Sanderson, Alastair J. R.;
Marrone, Daniel P.
2010ApJ...711.1033Z Altcode: 2010arXiv1001.0780Z
We compare X-ray hydrostatic and weak-lensing mass estimates for a
sample of 12 clusters that have been observed with both XMM-Newton and
Subaru. At an over-density of Δ = 500, we obtain 1 - M <SUP>X</SUP>/M
<SUP>WL</SUP> = 0.01 ± 0.07 for the whole sample. We also divided the
sample into undisturbed and disturbed sub-samples based on quantitative
X-ray morphologies using asymmetry and fluctuation parameters, obtaining
1 - M <SUP>X</SUP>/M <SUP>WL</SUP> = 0.09 ± 0.06 and -0.06 ± 0.12
for the undisturbed and disturbed clusters, respectively. In addition
to non-thermal pressure support, there may be a competing effect
associated with adiabatic compression and/or shock heating which leads
to overestimate of X-ray hydrostatic masses for disturbed clusters,
for example, in the famous merging cluster A1914. Despite the modest
statistical significance of the mass discrepancy, on average, in the
undisturbed clusters, we detect a clear trend of improving agreement
between M <SUP>X</SUP> and M <SUP>WL</SUP> as a function of increasing
over-density, M^X/M^WL=(0.908 ± 0.004)+(0.187 ± 0.010) \cdot log_{10}
(Δ /500). We also examine the gas mass fractions, f <SUB>gas</SUB> =
M <SUP>gas</SUP>/M <SUP>WL</SUP>, finding that they are an increasing
function of cluster radius, with no dependence on dynamical state,
in agreement with predictions from numerical simulations. Overall,
our results demonstrate that XMM-Newton and Subaru are a powerful
combination for calibrating systematic uncertainties in cluster mass
measurements. <P />This work is based on observations made with the
XMM-Newton, an ESA science mission with instruments and contributions
directly funded by ESA member states and the USA (NASA), and data
collected at Subaru Telescope and obtained from the SMOKA, which is
operated by the Astronomy Data Center, National Astronomical Observatory
of Japan.
---------------------------------------------------------
Title: Testing the radio halo-cluster merger scenario. The case of
RXC J2003.5-2323
Authors: Giacintucci, S.; Venturi, T.; Brunetti, G.; Dallacasa, D.;
Mazzotta, P.; Cassano, R.; Bardelli, S.; Zucca, E.
2009A&A...505...45G Altcode: 2009arXiv0905.3479G
Aims: We present a combined radio, X-ray, and optical study of
the galaxy cluster RXC J2003.5-2323. The cluster hosts one of the
largest, most powerful, and distant giant radio halos known to date,
suggesting that it may be undergoing a strong merger. The aim of
our multiwavelength study is to investigate the radio-halo cluster
merger scenario. <BR />Methods: We studied the radio properties of
the giant radio halo in RXC J2003.5-2323 by means of new radio data
obtained at 1.4 GHz with the Very Large Array, and at 240 MHz with
the Giant Metrewave Radio Telescope, in combination with previously
published GMRT data at 610 MHz. The dynamical state of the cluster was
investigated by means of X-ray Chandra observations and optical ESO-NTT
observations. <BR />Results: Our study confirms that RXC J2003.5-2323
is an unrelaxed cluster. The unusual filamentary and clumpy morphology
of the radio halo could be due to a combination of the filamentary
structure of the magnetic field and turbulence in the inital stage of
a cluster merger.
---------------------------------------------------------
Title: Energy injection in AWM4: a cool corona, a strong radio source,
and missing X-ray cavities
Authors: Giacintucci, Simona; O'Sullivan, E.; Vrtilek, J.; David,
L.; Raychaudhury, S.; Mazzotta, P.; Venturi, T.
2009cfdd.confE.108G Altcode:
We will present the results of the combined X-ray/radio analysis
of the group/poor cluster of galaxies AWM4, using a new 80 ksec
Chandra observation and low frequency GMRT radio data, taken as part
of a larger project of an in-depth study of the AGN feedback in the
group environment. Previous XMM-Newton observations showed AWM4 to
be isothermal, with its powerful central radio galaxy the most likely
source of heating. However, with only small lobes detected at 1.4GHz
and with no indications of cavities or shocks associated with the
AGN, the question of the coupling between jets and intra-group gas
remained unresolved. Deep, low frequency GMRT radio observations have
revealed the full extent of the radio jets and lobes and allowed us to
determine their age, orientation, energy and physical parameters. Our
new Chandra data reveals the small-scale galactic corona fueling the
AGN and explains why this long, energetic outburst has not quenched
cooling in the core. While some weak X-ray features associated with
the jets and lobes are detected, we do not detect the clear cavities
seen in many other similar systems, bringing us back to the question of
the nature of the interaction between the jets and the IGM. We discuss
possible interpretations, including entrainment or mixing of thermal gas
into the jets and lobes, contributions from non-thermal emission, and
dynamical motions of the BCG within the group. AWM4 provides a strong
example of the benefits of a combined X-ray/multi-band radio approach
to the study of AGN feedback, and emphasizes the power of Chandra's
superb spatial resolution to search for the small-scale features which
are key to our understanding of the mechanisms of this process.
---------------------------------------------------------
Title: EDGE: Explorer of diffuse emission and gamma-ray burst
explosions
Authors: Piro, L.; den Herder, J. W.; Ohashi, T.; Amati, L.; Atteia,
J. L.; Barthelmy, S.; Barbera, M.; Barret, D.; Basso, S.; Boer, M.;
Borgani, S.; Boyarskiy, O.; Branchini, E.; Branduardi-Raymont, G.;
Briggs, M.; Brunetti, G.; Budtz-Jorgensen, C.; Burrows, D.; Campana,
S.; Caroli, E.; Chincarini, G.; Christensen, F.; Cocchi, M.; Comastri,
A.; Corsi, A.; Cotroneo, V.; Conconi, P.; Colasanti, L.; Cusumano,
G.; de Rosa, A.; Del Santo, M.; Ettori, S.; Ezoe, Y.; Ferrari,
L.; Feroci, M.; Finger, M.; Fishman, G.; Fujimoto, R.; Galeazzi,
M.; Galli, A.; Gatti, F.; Gehrels, N.; Gendre, B.; Ghirlanda, G.;
Ghisellini, G.; Giommi, P.; Girardi, M.; Guzzo, L.; Haardt, F.;
Hepburn, I.; Hermsen, W.; Hoevers, H.; Holland, A.; in't Zand, J.;
Ishisaki, Y.; Kawahara, H.; Kawai, N.; Kaastra, J.; Kippen, M.; de
Korte, P. A. J.; Kouveliotou, C.; Kusenko, A.; Labanti, C.; Lieu,
R.; Macculi, C.; Makishima, K.; Matt, G.; Mazzotta, P.; McCammon,
D.; Méndez, M.; Mineo, T.; Mitchell, S.; Mitsuda, K.; Molendi, S.;
Moscardini, L.; Mushotzky, R.; Natalucci, L.; Nicastro, F.; O'Brien,
P.; Osborne, J.; Paerels, F.; Page, M.; Paltani, S.; Pareschi, G.;
Perinati, E.; Perola, C.; Ponman, T.; Rasmussen, A.; Roncarelli, M.;
Rosati, P.; Ruchayskiy, O.; Quadrini, E.; Sakurai, I.; Salvaterra,
R.; Sasaki, S.; Sato, G.; Schaye, J.; Schmitt, J.; Sciortino, S.;
Shaposhnikov, M.; Shinozaki, K.; Spiga, D.; Suto, Y.; Tagliaferri,
G.; Takahashi, T.; Takei, Y.; Tawara, Y.; Tozzi, P.; Tsunemi, H.;
Tsuru, T.; Ubertini, P.; Ursino, E.; Viel, M.; Vink, J.; White, N.;
Willingale, R.; Wijers, R.; Yoshikawa, K.; Yamasaki, N.
2009ExA....23...67P Altcode: 2008ExA...tmp....9P
How structures of various scales formed and evolved from the early
Universe up to present time is a fundamental question of astrophysical
cosmology. EDGE (Piro et al., 2007) will trace the cosmic history of the
baryons from the early generations of massive stars by Gamma-Ray Burst
(GRB) explosions, through the period of galaxy cluster formation,
down to the very low redshift Universe, when between a third and
one half of the baryons are expected to reside in cosmic filaments
undergoing gravitational collapse by dark matter (the so-called warm
hot intragalactic medium). In addition EDGE, with its unprecedented
capabilities, will provide key results in many important fields. These
scientific goals are feasible with a medium class mission using existing
technology combined with innovative instrumental and observational
capabilities by: (a) observing with fast reaction Gamma-Ray Bursts with
a high spectral resolution. This enables the study of their star-forming
and host galaxy environments and the use of GRBs as back lights of large
scale cosmological structures; (b) observing and surveying extended
sources (galaxy clusters, WHIM) with high sensitivity using two wide
field of view X-ray telescopes (one with a high angular resolution
and the other with a high spectral resolution). The mission concept
includes four main instruments: a Wide-field Spectrometer (0.1-2.2 eV)
with excellent energy resolution (3 eV at 0.6 keV), a Wide-Field Imager
(0.3-6 keV) with high angular resolution (HPD = 15”) constant over
the full 1.4 degree field of view, and a Wide Field Monitor (8-200 keV)
with a FOV of ¼ of the sky, which will trigger the fast repointing to
the GRB. Extension of its energy response up to 1 MeV will be achieved
with a GRB detector with no imaging capability. This mission is proposed
to ESA as part of the Cosmic Vision call. We will outline the science
drivers and describe in more detail the payload of this mission.
---------------------------------------------------------
Title: Relics and Halos at intermediate redshift: testing the
merging paradigm
Authors: Mazzotta, Pasquale
2008xmm..prop...44M Altcode:
In A0-6 we proposed to observe the galaxy cluster RXCJ1314.4-2515 which
was approved in priority A. Unfortunately the observation is affected
by strong flares for 69% of the time. We propose to re-observe it to
compensate for the time loss. RXCJ1314.4-2515 was selected from an
extensive radio observational campaign aimed to search for radio halos
and relics in galaxy clusters in the redshift range 0.2div0.4 at 610
MHz. RXCJ1314.4-2515 is exceptional as it is the unique case known to
date of a cluster hosting both a radio halo and a double relic. The
detailed study of the dynamics of this cluster will help us to test
the merging paradigm and the physical properties of the ICM related
to the relics and halo formation.
---------------------------------------------------------
Title: A Giant Metrewave Radio Telescope Multifrequency Radio Study
of the Isothermal Core of the Poor Galaxy Cluster AWM 4
Authors: Giacintucci, Simona; Vrtilek, Jan M.; Murgia, Matteo;
Raychaudhury, Somak; O'Sullivan, Ewan J.; Venturi, Tiziana; David,
Laurence P.; Mazzotta, Pasquale; Clarke, Tracy E.; Athreya, Ramana M.
2008ApJ...682..186G Altcode: 2008arXiv0804.1906G
We present a detailed radio morphological study and spectral analysis
of the wide-angle tail radio source 4C +24.36 associated with the
dominant galaxy in the relaxed galaxy cluster AWM 4. Our study is
based on new high-sensitivity GMRT observations at 235, 327, and 610
MHz and on literature and archival data at other frequencies. We find
that the source major axis is likely oriented at a small angle with
respect to the plane of the sky. The wide-angle tail morphology can
be reasonably explained by adopting a simple hydrodynamical model in
which both ram pressure (driven by the motion of the host galaxy) and
buoyancy forces contribute to bend the radio structure. The spectral
index progressively steepens along the source major axis from α ~ 0.3
in the region close to the radio nucleus to beyond 1.5 in the lobes. The
results of the analysis of the spectral index image allow us to derive
an estimate of the radiative age of the source of ~160 Myr. The cluster
X-ray-emitting gas has a relaxed morphology and short cooling time,
but its temperature profile is isothermal out to at least 160 kpc from
the center. Therefore, we seek evidence of energy ejection from the
central AGN to prevent catastrophic cooling. We find that the energy
injected by 4C +24.36 in the form of synchrotron luminosity during its
lifetime is far less than the energy required to maintain the high gas
temperature in the core. We also find that it is not possible for the
central source to eject the requisite energy in the intracluster gas
in terms of the enthalpy of buoyant bubbles of relativistic fluid,
without creating discernible large cavities in the existing X-ray
XMM-Newton observations.
---------------------------------------------------------
Title: Do Radio Core-Halos and Cold Fronts in Non-Major-Merging
Clusters Originate from the Same Gas Sloshing?
Authors: Mazzotta, Pasquale; Giacintucci, Simona
2008ApJ...675L...9M Altcode: 2008arXiv0801.1905M
We show an interesting correlation between the surface brightness
and temperature structure of the relaxed clusters RX J1720.1+2638
and MS 1455.0+2232, hosting a pair of cold fronts, and their central
core-halo radio source. We discuss the possibility that the origin
of this diffuse radio emission may be strictly connected with the gas
sloshing mechanism suggested to explain the formation of cold fronts
in non-major-merging clusters. We show that the radiative lifetime of
the relativistic electrons is much shorter than the timescale on which
they can be transported from the central galaxy up to the radius of
the outermost cold front. This strongly indicates that the observed
diffuse radio emission is likely produced by electrons reaccelerated
via some kind of turbulence generated within the cluster volume limited
by the cold fronts during the gas sloshing.
---------------------------------------------------------
Title: Temperature structure of the intergalactic medium within
seven nearby and bright clusters of galaxies observed with XMM-Newton
Authors: Bourdin, H.; Mazzotta, P.
2008A&A...479..307B Altcode: 2008arXiv0802.1866B
Aims:Using a newly developed algorithm, we map, to the highest
angular resolution allowed by the data, the temperature structure
of the intra-cluster medium (ICM) within a nearly complete X-ray
flux limited sample of galaxy clusters in the redshift range between
{z}=0.045 and {z}=0.096. Our sample contains seven bright clusters
of galaxies observed with XMM-Newton: Abell 399, Abell 401, Abell
478, Abell 1795, Abell 2029, Abell 2065, Abell 2256. <BR />Methods:
We use a multi-scale spectral mapping algorithm especially designed
to map spectroscopic observables from X-ray extended emission of the
ICM. By means of a wavelet analysis, this algorithm couples spatially
resolved spectroscopy with a structure detection approach. Derived
from a former algorithm using Haar wavelets, our algorithm is now
implemented with B-spline wavelets in order to perform a more regular
analysis of the signal. Compared to other adaptive algorithms, our
method has the advantage of analysing spatially the gas temperature
structure itself, instead of being primarily driven by the geometry
of gas brightness. <BR />Results: For the four clusters in our
sample that are major mergers, we find a rather complex thermal
structure with strong thermal variations consistent with their
dynamics. For two of them, A2065 and A2256, we perform a 3-d analysis
of cold front-like features evidenced from the gas temperature and
brightness maps. Furthermore, we detect a significant non-radial
thermal structure outside the cool core region of the other 3 more
“regular” clusters, with relative amplitudes of about about 10%
and typical sizes ranging between 2 and 3 arcmin. We investigate
possible implications of this thermal structure on the mass estimates,
by extracting the surface brightness and temperature profiles from
complementary sectors in the “regular” clusters A1795 and A2029,
corresponding to hottest and coldest regions in the maps. For A2029,
the temperature and surface brightness gradients seem to compensate
each other, leading to a consistent mass profile. For A1795, however,
the temperature structure leads to a significant mass discrepancy in
the innermost cluster region. The third “regular” cluster, A478,
is located in a particular sky region characterised by strong variations
of neutral hydrogen column density, Nh, even on angular scales smaller
than the cluster itself. For this cluster, we derive a spectroscopic
Nh map and investigate the origin of Nh structure by discussing its
correlation with galactic emission of dust in the infrared.
---------------------------------------------------------
Title: X-MAS2: Study Systematics on the ICM Metallicity Measurements
Authors: Rasia, E.; Mazzotta, P.; Bourdin, H.; Borgani, S.; Tornatore,
L.; Ettori, S.; Dolag, K.; Moscardini, L.
2008ApJ...674..728R Altcode: 2007arXiv0707.2614R
X-ray measurements of the intracluster medium metallicity are
becoming more and more frequent due to the availability of powerful
X-ray telescopes with excellent spatial and spectral resolutions. The
information that can be extracted from measurements of the α-elements,
such as oxygen, magnesium, and silicon, with respect to the iron
abundance is extremely important to a better understanding of stellar
formation and its evolutionary history. In this paper we investigate
possible source of bias or systematic effects connected to the plasma
physics when recovering metal abundances from X-ray spectra. To do
this, we analyze six simulated galaxy clusters processed through the
new version of our X-Ray Map Simulator (X-MAS), which allows us to
create mock XMM-Newton EPIC MOS1 and MOS2 observations. By comparing the
spectroscopic results inferred from the X-ray spectra to the expected
values directly obtained from the original simulation, we find that
(1) the iron is recovered with high accuracy for both hot (T >
3 keV) and cold (T < 2 keV) systems; at intermediate temperatures,
however, we find a systematic overestimate, which depends inversely on
the number counts; (2) oxygen is well recovered in cold clusters, while
in hot systems the X-ray measurement may overestimate the true value
by a up to a factor of 2-3; (3) being a weak line, the measurement of
magnesium is always difficult; despite this, for cold systems (i.e.,
with T < 2 keV) we do not find any systematic behavior, while for
very hot systems (i.e., with T > 5 keV) the spectroscopic measurement
may strongly overestimate the true value by up to a factor of 4; and
(4) silicon is well recovered for all the clusters in our sample. We
investigate in detail the nature of the systematic effects and biases
found in performing XSPEC simulations. We conclude that they are
mainly connected with the multitemperature nature of the projected
observed spectra and to the intrinsic limitation of the XMM-Newton
EPIC spectral resolution, which does not always allow disentangling
the emission lines produced by different elements.
---------------------------------------------------------
Title: Radio morphology and spectral analysis of cD galaxies in rich
and poor galaxy clusters
Authors: Giacintucci, S.; Venturi, T.; Murgia, M.; Dallacasa, D.;
Athreya, R.; Bardelli, S.; Mazzotta, P.; Saikia, D. J.
2007A&A...476...99G Altcode: 2007arXiv0708.4330G
Aims:We present a radio morphological study and spectral analysis of
a sample of 13 cD galaxies in rich and poor clusters of galaxies. <BR
/>Methods: Our study is based on new high sensitivity Giant Metrewave
Radio Telescope (GMRT) observations at 1.28 GHz, 610 MHz and 235 MHz,
and on archival data. From a statistical sample of cluster cD galaxies
we selected those sources with little information available in the
literature and promising for the detection of aged radio emission. As
well as the high sensitivity images for all 13 radio galaxies,
we present also a detailed spectral analysis for 7 of them. <BR
/>Results: We found a variety of morphologies and linear sizes, as
typical for radio galaxies in the radio power range sampled here (low
to intermediate power radio galaxies). The spectral analysis shows
that 10/13 radio galaxies have a steep radio spectrum, with spectral
index α ≥ 1. In general, the radiative ages and growth velocities
are consistent with previous findings that the evolution of radio
galaxies at cluster centres is affected by the dense external medium
(i.e. low growth velocities and old ages). We suggest that the dominant
galaxies in A 2622 and MKW 03s are dying radio sources, which at present
are not fed by nuclear activity. On the other hand, the spectacular
source at the centre of A 2372 might be a very interesting example of
a restarted radio galaxy. For this source we estimated a life cycle
of the order of 10<SUP>6</SUP> yr.
---------------------------------------------------------
Title: The importance of merging activity for the kinetic polarization
of the Sunyaev-Zel'dovich signal from galaxy clusters
Authors: Maturi, M.; Moscardini, L.; Mazzotta, P.; Dolag, K.;
Tormen, G.
2007A&A...475...71M Altcode: 2007arXiv0706.0830M
Context: The polarization sensitivity of upcoming millimetric
observatories will open new possibilities for studying the properties
of galaxy clusters and for using them as powerful cosmological
probes. For this reason it is necessary to investigate in detail
the characteristics of the polarization signals produced by their
highly ionized intra-cluster medium (ICM). This work is focused on
the polarization effect induced by the ICM bulk motion, the so-called
kpSZ signal, which has an amplitude proportional to the optical depth
and to the square of the tangential velocity. <BR />Aims: We study
how this polarization signal is affected by the internal dynamics of
galaxy clusters and its dependence on the physical modelling adopted
to describe the baryonic component. <BR />Methods: This is done by
producing realistic kpSZ maps starting from the outputs of two different
sets of high-resolution hydrodynamical N-body simulations. The first
set (17 objects) follows only non-radiative hydrodynamics, while for
each of 9 objects of the second set we implement four different kinds
of physical processes. <BR />Results: Our results shows that the kpSZ
signal is a very sensitive probe of the dynamical status of galaxy
clusters. We find that major merger events can amplify the signal up
to one order of magnitude with respect to relaxed clusters, reaching
amplitudes up to about 100 nK. This result implies that the internal ICM
dynamics must be taken into account when evaluating this signal because
simplicistic models, based on spherical rigid bodies, may provide wrong
estimates. In particular, the selection of sufficient relaxed clusters
seems to be fundamental to obtain a robust measurement of the intrinsic
quadrupole of the cosmic microwave background through polarization. We
find that the dependence on the physical modelling of the baryonic
component is relevant only in the very inner regions of clusters.
---------------------------------------------------------
Title: Relics and Halos at intermediate redshift: testing the
merging paradigm
Authors: Mazzotta, Pasquale
2007xmm..prop...36M Altcode:
In A0-6 we proposed to observe the galaxy cluster RXCJ1314.4-2515 which
was approved in priority A. Unfortunately the observation is affected
by strong flares for 69% of the time. We propose to re-observe it to
compensate for the time loss. RXCJ1314.4-2515 was selected from an
extensive radio observational campaign aimed to search for radio halos
and relics in galaxy clusters in the redshift range 0.2div0.4 at 610
MHz. RXCJ1314.4-2515 is exceptional as it is the unique case known to
date of a cluster hosting both a radio halo and a double relic. The
detailed study of the dynamics of this cluster will help us to test
the merging paradigm and the physical properties of the ICM related
to the relics and halo formation.
---------------------------------------------------------
Title: A Chandra Archival Study of the Temperature and Metal Abundance
Profiles in Hot Galaxy Clusters at 0.1 <~ z <~ 0.3
Authors: Baldi, A.; Ettori, S.; Mazzotta, P.; Tozzi, P.; Borgani, S.
2007ApJ...666..835B Altcode: 2007arXiv0705.3865B
We present an analysis of the temperature and metallicity profiles
of 12 galaxy clusters in the redshift range 0.1-0.3 selected from
the Chandra archive with at least ~20,000 net ACIS counts and
kT>6 keV. We divide the sample between seven cooling-core (CC)
and five non-cooling-core (NCC) clusters according to their central
cooling time. We find that single power laws can properly describe
both the temperature and metallicity profiles at radii larger than
0.1r<SUB>180</SUB> in both CC and NCC systems, with NCC objects showing
steeper profiles outward. A significant deviation is present only in the
inner 0.1r<SUB>180</SUB>. We perform a comparison of our sample with the
De Grandi & Molendi BeppoSAX sample of local CC and NCC clusters,
finding a complete agreement in the CC cluster profile and a marginally
higher value (at ~1 σ) in the inner regions of the NCC clusters. The
slope of the power law describing kT(r) within 0.1r<SUB>180</SUB>
correlates strongly with the ratio between the cooling time and the
age of the universe at the cluster redshift, with a slope >0 and
τ<SUB>c</SUB>/τ<SUB>age</SUB><~0.6 in CC systems.
---------------------------------------------------------
Title: The Local Cluster Substructure Survey (LoCuSS): Exploring
K-band Light as a Probe of Cluster Mass and Substructure
Authors: Egami, Eiichi; Marshall, Phil; Mazzotta, Pasquale; Evrard,
August; Carlstrom, John; Smith, Graham P.; Kneib, Jean-Paul;
Finoguenov, Alexis; Futamase, Toshifumi; Taylor, James
2007noao.prop..451E Altcode:
LoCuSS is a systematic multi-wavelength survey of 100 X-ray
luminous galaxy clusters at z~eq0.2. A key goal is to construct
robust cluster mass-observable scaling relations for cosmological and
astrophysical applications. For example the mass-temperature and mass-
SZE relations are pivotal to cluster-based dark energy measurements. We
are using gravitational lensing to measure cluster mass and thus to
test explicitly assumptions about how baryons trace the total cluster
mass. Here, we propose to obtain NIR imaging of LoCuSS clusters to probe
their evolved stellar populations. These data will allow a detailed
investigation of how the the integrated cluster K-band luminosity and
substructure within K-band light maps correlate with the total cluster
mass and substructure obtained from lensing. In addition to exploring
the mass-L_K scaling relation for possible cosmological application,
we will calibrate NIR data as an inexpensive probe of cluster mass and
substructure to aide the interpretation of ongoing and future surveys
for high-redshift clusters.
---------------------------------------------------------
Title: A Joint Spitzer/Lensing Survey - Exploring the Connection
Between Hierarchical Assembly and Starburst Activity in Galaxy
Clusters at z=0.2
Authors: Smith, Graham; Babul, Arif; Carlstrom, John; Egami, Eiichi;
Ellis, Richard; Evrard, Gus; Finoguenov, Alexis; Futamase, Toshifumi;
Kneib, Jean-Paul; Marshall, Phil; Mazzotta, Pasquale; Ponman, Trevor;
Takada, Masahiro; Taylor, James
2007sptz.prop40872S Altcode:
We propose to conduct a wide-field Spitzer/MIPS 24um survey of 32
X-ray luminous galaxy clusters at z~0.2. These 32 are drawn from
the 100 clusters under intense multi-wavelength study as part of
the Local Cluster Substructure Survey (LoCuSS). All 32 have high
quality wide-field weak lensing data from Subaru, supplemented by HST
imaging of the cluster cores. Our primary science goal is to achieve
a definitive survey of starburst activity in local clusters and to
correlate the amount of obscured activity with dynamical state of the
clusters. The combination of the proposed 25'x25' MIPS 24um maps and
our detailed lensing-based mass maps will be uniquely powerful for
that purpose. The superb sensitivity of MIPS will allow us to detect
LIRGs in the virialised region of each cluster in just ~1.2 hours
per cluster; the structural analysis of the lensing mass maps will
diagnose the amount and location of recent hierarchical infall into the
clusters. We will therefore be able to quantify precisely the amount
of obscured star formation in local clusters and to delineate how that
activity relates to hierarchical assembly. Our results will therefore
have a major impact on efforts to understand whether infalling spiral
galaxies transform into S0 galaxies by gradual fading or via an intense
starburst phase. For this huge statistical survey (several orders of
magnitude larger than the state of the art), we request a modest 36
hours of observing time.
---------------------------------------------------------
Title: The Local Cluster Substructure Survey (LoCuSS): Exploring
K-band light as a probe of cluster mass and substructure
Authors: Egami, Eiichi; Marshall, Phil; Mazzotta, Pasquale; Evrard,
August; Carlstrom, John; Smith, Graham P.; Kneib, Jean-Paul;
Finoguenov, Alexis; Futamase, Toshifumi; Taylor, James
2007noao.prop..428E Altcode:
LoCuSS is a systematic multi-wavelength survey of 100 X-ray
luminous galaxy clusters at z~eq0.2. A key goal is to construct
robust cluster mass-observable scaling relations for cosmological and
astrophysical applications. For example the mass-temperature and mass-
SZE relations are pivotal to cluster-based dark energy measurements. We
are using gravitational lensing to measure cluster mass and thus to
test explicitly assumptions about how baryons trace the total cluster
mass. Here, we propose to obtain NIR imaging of LoCuSS clusters to probe
their evolved stellar populations. These data will allow a detailed
investigation of how the the integrated cluster K-band luminosity and
substructure within K-band light maps correlate with the total cluster
mass and substructure obtained from lensing. In addition to exploring
the mass-L_K scaling relation for possible cosmological application,
we will calibrate NIR data as an inexpensive probe of cluster mass and
substructure to aide the interpretation of ongoing and future surveys
for high-redshift clusters.
---------------------------------------------------------
Title: High Sensitivity Low Frequency Radio Observations of cD
Galaxies
Authors: Giacintucci, S.; Venturi, T.; Bardelli, S.; Dallacasa, D.;
Mazzotta, P.; Saikia, D. J.
2007hvcg.conf..130G Altcode: 2006astro.ph.12530G
We present the GMRT 235 MHz images of three radio galaxies and 610 MHz
images of two sources belonging to a complete sample of cD galaxies in
rich and poor galaxy clusters. The analysis of the spectral properties
confirms the presence of aged radio emission in two of the presented
sources.
---------------------------------------------------------
Title: Observing Metallicity in Simulated Clusters with X-MAS2
Authors: Rasia, E.; Mazzotta, P.; Bourdin, H.; Ettori, S.; Borgani,
S.; Dolag, K.; Moscardini, L.; Sauvageot, J. L.; Tornatore, L.
2007hvcg.conf..365R Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Relics and Halos at intermediate redshift: testing the
merging paradigm
Authors: Mazzotta, Pasquale
2006xmm..prop...57M Altcode:
Within the framework of an extensive radio observational campaign aimed
to search for radio halos and relics in galaxy clusters in the redshift
range 0.2-0.4 at 610 MHz, we propose to observe one cluster of our
sample which is exceptional in the radio band and therefore extremely
promising for testing the merging paradigm. RXCJ1314.4-2515 is the
unique case known to date of galaxy cluster hosting both a radio halo
and a double relic. Our goal is to reconstruct the detailed dynamics
of this cluster and to test the physical properties of the ICM related
to the relics and halo formation.
---------------------------------------------------------
Title: Systematics in the X-ray cluster mass estimators
Authors: Rasia, E.; Ettori, S.; Moscardini, L.; Mazzotta, P.; Borgani,
S.; Dolag, K.; Tormen, G.; Cheng, L. M.; Diaferio, A.
2006MNRAS.369.2013R Altcode: 2006astro.ph..2434R; 2006MNRAS.tmp..610R
We examine the systematics affecting the X-ray mass estimators
applied to a set of five galaxy clusters resolved at high resolution
in hydrodynamic simulations, including cooling, star formation and
feedback processes. These simulated objects are processed through the
X-ray Map Simulator, X-MAS, to provide Chandra-like long exposures
that are analysed to reconstruct the gas temperature, density and mass
profiles used as input. These clusters have different dynamic state:
we consider a hot cluster with temperature T = 11.4keV, a perturbed
cluster with T = 3.9keV, a merging object with T = 3.6keV, and two
relaxed systems with T = 3.3keV and T = 2.7keV, respectively. These
systems are located at z = 0.175 so that their emission fits within
the Chandra ACIS-S3 chip between 0.6 and 1.2 R<SUB>500</SUB>. <P
/>We find that the mass profile obtained via a direct application
of the hydrostatic equilibrium (HE) equation is dependent upon the
measured temperature profile. An irregular radial distribution of the
temperature values, with associated large errors, induces a significant
scatter on the reconstructed mass measurements. At R<SUB>2500</SUB>,
the actual mass is recovered within 1σ, although we notice this
estimator shows high statistical errors due to high level of Chandra
background. Instead, the poorness of the β-model in describing the gas
density profile makes the evaluated masses to be underestimated by ~40
per cent with respect to the true mass, both with an isothermal and a
polytropic temperature profile. We also test ways to recover the mass
by adopting an analytic mass model, such as those proposed by Nvarro,
Frenk & White and Rasia, Tormen & Moscardini, and fitting the
temperature profile expected from the HE equation to the observed
one. We conclude that the methods of the HE equation and those of
the analytic fits provide a more robust mass estimation than the ones
based on the β-model. In the present work, the main limitation for
a precise mass reconstruction is to ascribe to the relatively high
level of the background chosen to reproduce the Chandra one. After
artificially reducing the total background by a factor of 100, we
find that the estimated mass significantly underestimates the true
mass profiles. This is manly due (i) to the neglected contribution of
the gas bulk motions to the total energy budget and (ii) to the bias
towards lower values of the X-ray temperature measurements because of
the complex thermal structure of the emitting plasma.
---------------------------------------------------------
Title: ESTREMO/WFXRT: Extreme phySics in the TRansient and Evolving
COsmos
Authors: Piro, Luigi; Amati, Lorenzo; Barbera, Marco; Borgani,
Stefano; Bazzano, Angela; Branchini, Enzo; Brunetti, G.; Campana,
Sergio; Caroli, Ezio; Cocchi, Massimo; Colafrancesco, Sergio;
Colasanti, Luca; Corsi, Alessandra; Costa, Enrico; Cusumano,
Giancarlo; Del Santo, Melania; Den Herder, Jan-Willem; De Rosa,
Alessandra; Di Cocco, Guido; Ettori, Stefano; Feroci, Marco; Fiore,
Fabrizio; Fusco-Femiano, Roberto; Galeazzi, Massimiliano; Galli,
Alessandra; Gatti, Flavio; Gendre, Bruce; Guzzo, Luigi; Hermsen, Wim;
in't Zand, Jean; Kaastra, Jelle; La Rosa, Giovanni; Labanti, Claudio;
Marisaldi, Mario; Mazzotta, Pasquale; Mineo, Teresa; Molendi, Silvano;
Moscardini, Lauro; Natalucci, Lorenzo; Nicastro, Fabrizio; Pareschi,
Giovanni; Pian, Elena; Quadrini, E.; Roncarelli, Mauro; Shaye, Jaap;
Tagliaferri, Gianpiero; Tozzi, Paolo; Ubertini, Pietro; Ursino,
Eugenio; Viel, Matteo
2006SPIE.6266E..0KP Altcode: 2006SPIE.6266E..16P
We present a mission designed to address two main themes of the
ESA Cosmic Vision Programme: the Evolution of the Universe and its
Violent phenomena. ESTREMO/WFXRT is based on innovative instrumental
and observational approaches, out of the mainstream of observatories
of progressively increasing area, i.e.: Observing with fast reaction
transient sources, like GRB, at their brightest levels, thus allowing
high resolution spectroscopy. Observing and surveying through a
X-ray telescope with a wide field of view and with high sensitivity
extended sources, like cluster and Warm Hot Intragalactic Medium
(WHIM). ESTREMO/WFXRT will rely on two cosmological probes: GRB and
large scale X-ray structures. This will allow measurements of the dark
energy, of the missing baryon mass in the local universe, thought
to be mostly residing in outskirts of clusters and in hot filaments
(WHIM) accreting onto dark matter structures, the detection of first
objects in the dark Universe, the history of metal formation. The
key asset of ESTREMO/WFXRT with regard to the study of Violent
Universe is the capability to observe the most extreme objects of
the Universe during their bursting phases. The large flux achieved
in this phase allows unprecedented measurements with high resolution
spectroscopy. The mission is based on a wide field X-ray/hard X-ray
monitor, covering >1/4 of the sky, to localize transients; fast
(min) autonomous follow-up with X-ray telescope (2000 cm<SUP>2</SUP>)
equipped with high resolution spectroscopy transition edge (TES)
microcalorimeters (2eV resolution below 2 keV) and with a wide field
(1°) for imaging with 10" resolution (CCD) extended faint structures
and for cluster surveys. A low background is achieved by a 600 km
equatorial orbit. The performances of the mission on GRB and their
use as cosmological beacons are presented and discussed.
---------------------------------------------------------
Title: Evidence of gas heating by the central AGN in MKW 3s
Authors: Giacintucci, S.; Mazzotta, P.; Brunetti, G.; Venturi, T.;
Bardelli, S.
2006AN....327..573G Altcode:
We present the results of radio observations of the galaxy cluster
MKW 3s carried out at 1.28 GHz and 610 MHz with the Giant Metrewave
Radio Telescope (GMRT). The Chandra observations of MKW 3s revealed
that this cluster is characterized by a complex X-ray structure hosting
both a X-ray filament and a X-ray cavity. The temperature structure of
the cluster core is even more complex, with the presence of extended
regions of gas heated above the radially averaged gas temperature at any
radius. The magnetic field derived from the radio observations is ∼ 2
μG and provides radiative ages of the order of ∼ 2 × 10<SUP>8</SUP>
yrs. Thanks to this estimate of the magnetic field strength and the
comparison between the radio structure and the Chandra data, we found
clear evidence for a close connection between the radio activity of
the central AGN and the heated gas regions in this cluster.
---------------------------------------------------------
Title: Bias on Estimates of X-ray Cluster Mass
Authors: Rasia, E.; Ettori, S.; Moscardini, L.; Mazzotta, P.; Borgani,
S.; Dolag, K.; Tormen, G.; Cheng, L. M.; Diaferio, A.
2006EAS....20..295R Altcode:
We examine the systematics affecting the X-ray mass estimators applied
to Chandra-like long exposures images of five simulated clusters.
---------------------------------------------------------
Title: X-ray Properties of a Mass-Selected Group Catalog
Authors: Mazzotta, P.; Bower, R.; Balogh, M.; Ponman, T.; Theuns,
T.; Edge, A.; Eke, V.; Bohringer, H.; Collins, C.; Colless, M.
2006cosp...36..647M Altcode: 2006cosp.meet..647M
The observed X-ray luminosities of groups are inconsistent with a model
in which the intragroup medium is shock-heated during the collapse It
is thought that a combination of pre-heating gas cooling and energy
injection removes low entropy gas reducing the system s X-ray luminosity
However the extent of this process is uncertain because the previous
selection of group catalogs has been based on X-ray emission We have
constructed a complete mass-selected catalog of 18 groups from the
2dFGRS that we proposed for observation with Chandra and XMM-Newton
To date twelve these groups have been observed and here we present
some preliminary results
---------------------------------------------------------
Title: Temperature structure of the intra-cluster medium within
relaxed clusters of galaxies
Authors: Bourdin, H.; Mazzotta, P.
2006EAS....20..267B Altcode:
Using a wavelet algorithm, we have mapped the temperature structure of
the three relaxed clusters of galaxies Abell 478, Abell 1795 and Abell
2029. The findings of significant non-radial thermal structures outside
the core region of two of these clusters question the validity limits
of the elliptical symmetry hypothesis required for deriving cluster
mass profiles from gas brightness and temperature profiles measurements.
---------------------------------------------------------
Title: Temperature structure of the intra-cluster medium within
a sample of nearby and bright clusters of galaxies observed with
XMM-Newton.
Authors: Bourdin, H.; Mazzotta, P.
2005sf2a.conf..705B Altcode:
Using a wavelet algorithm especially designed for that purpose, we
have mapped, to the highest angular resolution allowed by the data,
the temperature structure of the intra-cluster medium within eight
bright and extended clusters of galaxies observed with XMM-Newton: A399,
A401, A478, A1795, A2029, A2065, A2256, A2255. This set is an almost
complete X-ray flux limited cluster sample, which includes merging and
relaxed clusters. Being major mergers, we find that 5 out of 8 cluster
show a rather complex thermal structure consistent with their merger
dynamics. More surprisingly significant non-radial thermal structures
are also observed outside the core region of two of the remaining
“relaxed" clusters. These findings question the validity limits of
the elliptical symmetry hypothesis required for deriving cluster mass
profiles from gas brightness and temperature profiles measurements.
---------------------------------------------------------
Title: An Archival Study of the Metal Distribution and X-ray Scaling
Relations in Galaxy Clusters at 0.1< z <0.7
Authors: Mazzotta, Pasquale
2005cxo..prop.4058M Altcode:
This proposal aims at exploiting the archived observations of galaxy
clusters in the redshift range 0.1<z<0.7, in order to address
a number of open issues: 1) tracing the evolution of the metal
abundances in the ICM and its dependence upon the gas temperature;
2) establishing the evolution of the cluster scaling relations; 3)
studying the implications of the cluster metal budget through realistic
X-ray observations of the products of N-body simulations obtained via
our software "X-ray MAp Simulator". With this proposal we intend to
analyze in a systematic and robust way a final sample of 115 clusters
(out of which 63 in the proposed sample) to achieve the strongest
constraints reachable nowadays on the thermodynamical and chemical
history of the Intra Cluster Medium.
---------------------------------------------------------
Title: A full-sky prediction of the Sunyaev-Zeldovich effect from
diffuse hot gas in the local universe and the upper limit from the
WMAP data
Authors: Hansen, F. K.; Branchini, E.; Mazzotta, P.; Cabella, P.;
Dolag, K.
2005MNRAS.361..753H Altcode: 2005astro.ph..2227H; 2005MNRAS.tmp..601H
We use the Point Source Catalogue Redshift Survey galaxy redshift
catalogue combined with constrained simulations based on the IRAS 1.2-Jy
galaxy density field to estimate the contribution of hot gas in the
local universe to the Sunyaev-Zeldovich (SZ) effect on a large scale. We
produce a full-sky HEALPIX map predicting the SZ effect from clusters
as well as diffuse hot gas within 80h<SUP>-1</SUP>Mpc. Performing
cross-correlation tests between this map and the WMAP data in pixel,
harmonic and wavelet space we can put an upper limit on the effect. We
conclude that the SZ effect from diffuse gas in the local universe
cannot be detected in current cosmic microwave background (CMB) data
and is not a large-scale contaminating factor (l < 60) in studies
of CMB angular anisotropies. We derive an upper limit for the mean
temperature decrement of ΔT < 0.33μK at the 2σ confidence level
for the 61-GHz frequency channel. However, for future high-sensitivity
experiments observing at a wider range of frequencies, the predicted
large-scale SZ effect could be of importance.
---------------------------------------------------------
Title: Tracing the warm-hot intergalactic medium in the local Universe
Authors: Viel, M.; Branchini, E.; Cen, R.; Ostriker, J. P.; Matarrese,
S.; Mazzotta, P.; Tully, B.
2005MNRAS.360.1110V Altcode: 2004astro.ph.12566V; 2005MNRAS.tmp..478V
We present a simple method for tracing the spatial distribution and
predicting the physical properties of the Warm-Hot Intergalactic Medium
(WHIM), from the map of galaxy light in the Local Universe. Under
the assumption that biasing is local and monotonic we map the ~2
h<SUP>-1</SUP> Mpc smoothed density field of galaxy light into the
mass-density field, from which we infer the spatial distribution of
the WHIM in the Local Supercluster. Taking into account the scatter
in the WHIM density-temperature and density-metallicity relation,
extracted from the z= 0 outputs of high-resolution and large-box-size
hydrodynamical cosmological simulations, we are able to quantify the
probability of detecting WHIM signatures in the form of absorption
features in the X-ray spectra, along arbitrary directions in the
sky. To illustrate the usefulness of this semi-analytical method we
focus on the WHIM properties in the Virgo cluster region.
---------------------------------------------------------
Title: A Hubble Space Telescope lensing survey of X-ray luminous
galaxy clusters - IV. Mass, structure and thermodynamics of cluster
cores at z= 0.2
Authors: Smith, Graham P.; Kneib, Jean-Paul; Smail, Ian; Mazzotta,
Pasquale; Ebeling, Harald; Czoske, Oliver
2005MNRAS.359..417S Altcode: 2005MNRAS.tmp..313S; 2004astro.ph..3588S
We present a comprehensive space-based study of 10 X-ray luminous galaxy
clusters (L<SUB>X</SUB>>= 8 × 10<SUP>44</SUP> erg s<SUP>-1</SUP>,
0.1-2.4 keV) at z= 0.2. Hubble Space Telescope (HST) observations
reveal numerous gravitationally lensed arcs for which we present four
new spectroscopic redshifts, bringing the total to 13 confirmed arcs
in this cluster sample. The confirmed arcs reside in just half of
the clusters; we thus obtain a firm lower limit on the fraction of
clusters with a central projected mass density exceeding the critical
density required for strong lensing of 50 per cent. We combine the
multiple-image systems with the weakly sheared background galaxies
to model the total mass distribution in the cluster cores (R<=
500 kpc). These models are complemented by high-resolution X-ray data
from Chandra and used to develop quantitative criteria to classify
the clusters as relaxed or unrelaxed. Formally, (30 +/- 20) per cent
of the clusters form a relatively homogeneous subsample of relaxed
clusters; the remaining (70 +/- 20) per cent are unrelaxed and are a
much more diverse population. Most of the clusters therefore appear
to be experiencing a cluster-cluster merger or relaxing after such an
event. We also study the normalization and scatter of scaling relations
between the cluster mass, the X-ray luminosity and the temperature. The
scatter in these relations is dominated by the unrelaxed clusters and
is typically σ~= 0.4. Most notably, we detect two to three times more
scatter in the mass-temperature relation than theoretical simulations
and models predict. The observed scatter is also asymmetric - the
unrelaxed clusters are systematically 40 per cent hotter than the
relaxed clusters at 2.5σ significance. This structural segregation
should be a major concern for experiments designed to constrain
cosmological parameters using galaxy clusters. Overall our results are
consistent with a scenario of cluster-cluster merger-induced boosts
to cluster X-ray luminosities and temperatures.
---------------------------------------------------------
Title: Predictions for high-frequency radio surveys of extragalactic
sources
Authors: de Zotti, G.; Ricci, R.; Mesa, D.; Silva, L.; Mazzotta, P.;
Toffolatti, L.; González-Nuevo, J.
2005A&A...431..893D Altcode: 2004astro.ph.10709D
We present detailed predictions of the contributions of the various
source populations to the counts at frequencies of tens of GHz. New
evolutionary models are worked out for flat-spectrum radio quasars,
BL Lac objects, and steep-spectrum sources. Source populations
characterized by spectra peaking at high radio frequencies, such as
extreme GPS sources, ADAF/ADIOS sources and early phases of γ-ray burst
afterglows are also dealt with. The counts of different populations
of star-forming galaxies (normal spirals, starbursts, high-z galaxies
detected by SCUBA and MAMBO surveys, interpreted as proto-spheroidal
galaxies) are estimated taking into account both synchrotron and
free-free emission, and dust re-radiation. Our analysis is completed
by updated counts of Sunyaev-Zeldovich effects in clusters of galaxies
and by a preliminary estimate of galactic-scale Sunyaev-Zeldovich
signals associated to proto-galactic plasma.
---------------------------------------------------------
Title: Mismatch between X-Ray and Emission-weighted Temperatures in
Galaxy Clusters: Cosmological Implications
Authors: Rasia, E.; Mazzotta, P.; Borgani, S.; Moscardini, L.; Dolag,
K.; Tormen, G.; Diaferio, A.; Murante, G.
2005ApJ...618L...1R Altcode: 2004astro.ph..9650R
The thermal properties of hydrodynamical simulations of galaxy
clusters are usually compared to observations by relying on
the emission-weighted temperature T<SUB>ew</SUB> instead of on
the spectroscopic X-ray temperature T<SUB>spec</SUB>, which is
obtained by actual observational data. In a recent paper, Mazzotta
et al. show that if the intracluster medium is thermally complex,
T<SUB>ew</SUB> fails at reproducing T<SUB>spec</SUB>. They propose
a new formula, the spectroscopic-like temperature, T<SUB>sl</SUB>,
which approximates T<SUB>spec</SUB> better than a few percent. By
analyzing a set of hydrodynamical simulations of galaxy clusters, we
find that T<SUB>sl</SUB> is lower than T<SUB>ew</SUB> by 20%-30%. As a
consequence, the normalization of the M-T<SUB>sl</SUB> relation from the
simulations is larger than the observed one by about 50%. If masses in
simulated clusters are estimated by following the same assumptions of
hydrostatic equilibrium and β-model gas density profile, as is often
done for observed clusters, then the M-T relation decreases by about 40%
and significantly reduces its scatter. On the basis of this result, we
conclude that using the observed M-T relation to infer the amplitude of
the power spectrum from the X-ray temperature function could bias low
σ<SUB>8</SUB> by 10%-20%. This may alleviate the tension between the
value of σ<SUB>8</SUB> inferred from the cluster number density and
those from the cosmic microwave background and large-scale structure.
---------------------------------------------------------
Title: Spectroscopic-Like Temperature of Clusters of Galaxies and
Cosmological Implications
Authors: Mazzotta, P.; Rasia, E.; Borgani, S.; Moscardini, L.; Dolag,
K.; Tormen, G.
2004astro.ph.12536M Altcode:
The thermal properties of hydrodynamical simulations of galaxy
clusters are usually compared to observations by relying on the
emission-weighted temperature T_ew, instead of on the spectroscopic
X-ray temperature T_spec, which is obtained by actual observational
data. Here we show that, if the intra-cluster medium is thermally
complex, T_ew fails at reproducing T_spec. We propose a new formula,
the spectroscopic-like temperature, T_sl, which approximates T_spec
better than a few per cent. By analyzing a set of hydrodynamical
simulations of galaxy clusters, we also find that T_sl is lower than
T_ew by 20-30 per cent. As a consequence, the normalization of the
M-T relation from the simulations is larger than the observed one by
about 50 per cent. If masses in simulated clusters are estimated by
following the same assumptions of hydrostatic equilibrium and beta-model
gas density profile, as often done for observed clusters, then the M-T
relation decreases by about 40 per cent, and significantly reduces its
scatter. Based on this result, we conclude that using the observed M-T
relation to infer the amplitude of the power spectrum from the X--ray
temperature function could bias low sigma_8 by 10-20 per cent. This
may alleviate the tension between the value of sigma_8 inferred from
the cluster number density and those from cosmic microwave background
and large scale structure.
---------------------------------------------------------
Title: Heated Intracluster Gas and Radio Connections: The Singular
Case of MKW 3S
Authors: Mazzotta, Pasquale; Brunetti, Gianfranco; Giacintucci,
Simona; Venturi, Tiziana; Bardelli, Sandro
2004JKAS...37..381M Altcode: 2004astro.ph.11708M
Similarly to other cluster of galaxies previously classified as cooling
flow systems, the Chandra observation of MKW3s reveals that this object
has a complex X-ray structure hosting both a X-ray cavity and a X-ray
filament. Unlike the other clusters, however, the temperature map of
the core of MKW3s shows the presence of extended regions of gas heated
above the radially averaged gas temperature at any radius. As the
cluster does not show evidences for ongoing major mergers Mazzotta et
al. suggest a connection between the heated gas and the activity of the
central AGN. Nevertheless, due to the lack of high quality radio maps,
this interpretation was controversial. In this paper we present the
results of two new radio observations of MKW3s at 1.28GHz and 604MHz
obtained at the GMRT. Together with the Chandra observation and a
separate VLA observation at 327MHz from Young, we show unequivocal
evidences for a close connection between the heated gas region and
the AGN activity and we briefly summarize possible implications.
---------------------------------------------------------
Title: Quenching cluster cooling flows with recurrent hot plasma
bubbles
Authors: Dalla Vecchia, Claudio; Bower, Richard G.; Theuns, Tom;
Balogh, Michael L.; Mazzotta, Pasquale; Frenk, Carlos S.
2004MNRAS.355..995D Altcode: 2004MNRAS.tmp..507D; 2004astro.ph..2441V; 2004astro.ph..2441D
The observed cooling rate of hot gas in clusters is much lower than
that inferred from the gas density profiles. This suggests that the
gas is being heated by some source. We use an adaptive-mesh refinement
code (FLASH) to simulate the effect of multiple, randomly positioned,
injections of thermal energy within 50 kpc of the centre of an initially
isothermal cluster with mass M<SUB>200</SUB>= 3 × 10<SUP>14</SUP>
M<SUB>solar</SUB> and kT= 3.1 keV. We have performed eight simulations
with spherical bubbles of energy generated every 10<SUP>8</SUP> yr, over
a total of 1.5Gyr. Each bubble is created by injecting thermal energy
steadily for 10<SUP>7</SUP> yr; the total energy of each bubble lies in
the range (0.1-3)×10<SUP>60</SUP>erg, depending on the simulation. We
find that 2 × 10<SUP>60</SUP>erg per bubble (corresponding to an
average power of 6.3 × 10<SUP>44</SUP>ergs<SUP>-1</SUP>) effectively
balances energy loss in the cluster and prevents the accumulation of gas
below kT= 1 keV from exceeding the observational limits. This injection
rate is comparable to the radiated luminosity of the cluster, and the
required energy and periodic time-scale of events are consistent with
observations of bubbles produced by central active galactic nuclei in
clusters. The effectiveness of this process depends primarily on the
total amount of injected energy and the initial location of the bubbles,
but is relatively insensitive to the exact duty cycle of events.
---------------------------------------------------------
Title: Comparing the temperatures of galaxy clusters from
hydrodynamical N-body simulations to Chandra and XMM-Newton
observations
Authors: Mazzotta, P.; Rasia, E.; Moscardini, L.; Tormen, G.
2004MNRAS.354...10M Altcode: 2004astro.ph..4425M; 2004MNRAS.tmp..320M
Theoretical studies of the physical processes guiding the formation
and evolution of galaxies and galaxy clusters in the X-ray region
are mainly based on the results of numerical hydrodynamical N-body
simulations, which in turn are often directly compared with X-ray
observations. Although trivial in principle, these comparisons are
not always simple. We demonstrate that the projected spectroscopic
temperature of thermally complex clusters obtained from X-ray
observations is always lower than the emission-weighed temperature,
which is widely used in the analysis of numerical simulations. We
show that this temperature bias is mainly related to the fact that
the emission-weighted temperature does not reflect the actual spectral
properties of the observed source. This has important implications for
the study of thermal structures in clusters, especially when strong
temperature gradients, such as shock fronts, are present. Because of
this bias, in real observations shock fronts appear much weaker than
what is predicted by emission-weighted temperature maps, and may not
even be detected. This may explain why, although numerical simulations
predict that shock fronts are a quite common feature in clusters
of galaxies, to date there are very few observations of objects in
which they are clearly seen. To fix this problem we propose a new
formula, the spectroscopic-like temperature function, and show that,
for temperatures higher than 3 keV, it approximates the spectroscopic
temperature to better than a few per cent, making simulations more
directly comparable to observations.
---------------------------------------------------------
Title: X-ray Properties of a Mass-Selected Group Catalog
Authors: Mazzotta, Pasquale
2004cxo..prop.1783M Altcode:
The observed X-ray luminosities of groups are inconsistent with
pure shock-heated gas model. It is thought that a combination of
pre-heating, gas cooling and energy injection act to remove low
entropy gas. However, the extent of these processes is uncertain
because the previous selection of group catalogs have been based on
X-ray emission. We have constructed a complete, mass-selected catalog
of 18 groups from the 2dFGRS. X-ray observations of this sample would
for the first time provide accurate determinations of the entropy in
a mass-selected sample. This project was highly ranked by last year
Chandra and XMM tacs. In return twelve groups have been accepted for
observation. Here we propose the observation of the remaining 6 groups
to complete the sample.
---------------------------------------------------------
Title: Comparing the temperatures of galaxy clusters from hydro-N-body
simulations to Chandra and XMM-Newton observations
Authors: Mazzotta, P.; Rasia, E.; Moscardini, L.; Tormen, G.
2004astro.ph..9618M Altcode:
Theoretical studies of the physical processes in clusters of galaxies
are mainly based on the results of numerical simulations, which in turn
are often directly compared to X-ray observations. Although trivial
in principle, these comparisons are not always simple. We show that
the projected spectroscopic temperature of clusters obtained from X-ray
observations is always lower than the emission-weighed temperature. This
bias is related to the fact that the emission-weighted temperature does
not reflect the actual spectral properties of the observed source. This
has implications for the study of thermal structures in clusters,
especially when strong temperature gradients, like shock fronts, are
present. In real observations shock fronts appear much weaker than
what is predicted by emission-weighted temperature maps. We propose a
new formula, the spectroscopic-like temperature function that better
approximates the spectroscopic temperature, making simulations more
directly comparable to observations
---------------------------------------------------------
Title: The faint X-ray source population near 3C 295
Authors: D'Elia, V.; Fiore, F.; Elvis, M.; Cappi, M.; Mathur, S.;
Mazzotta, P.; Falco, E.; Cocchia, F.
2004A&A...422...11D Altcode: 2004astro.ph..3401D
We present a statistical analysis of the Chandra observation of the
source field around the 3C 295 galaxy cluster (z=0.46) to search for
clustering of X-ray sources. We applied three different methods of
analysis, all suggesting a strong clustering in the field on scales
of a few arcmin. In particular 1) the log N-log S computed separately
for the four ACIS-I chips reveals that there is a significant (3.2
σ in the 0.5-2 keV, 3.3 σ in the 2-10 keV and 4.0 σ in the 0.5-10
keV band) excess of sources to the North-North East and a void to
the South of the central cluster; 2) the two point, two-dimensional
Kolmogorov-Smirnov (KS) test, shows the probability that the sources
are uniformly distributed is only a few percent; 3) a strong spatial
correlation emerges from the study of the angular correlation function
of the field: the angular correlation function (ACF) shows a clear
signal on scales of 0.5/5 arcmin, correlation angle in the 0.5-7 keV
band θ<SUB>0</SUB>=8.5<SUP>+6.5</SUP><SUB>-4.5</SUB>, 90% confidence
limit (assuming a power law ACF with slope γ=1.8). This correlation
angle is 2 times higher than that of a sample of 8 ACIS-I field at the
2.5 σ confidence level. The above scales translate to 0.2/2 Mpc at
the cluster redshift, higher than the typical cluster core radius, and
more similar to the size of a “filament” of the large scale structure.
---------------------------------------------------------
Title: Simulating Chandra observations of galaxy clusters
Authors: Rasia, E.; Gardini, A.; Mazzotta, P.; Tormen, G.; de Grandi,
S.; Moscardini, L.
2004ogci.conf..313R Altcode: 2004IAUCo.195..313R
The direct comparison of observations to numerical hydro-N-body
simulations, although simple in principle, is not always trivial
because of possible artificial effects produced by the instrument
response and by instrumental and sky background. To overcome this
problem we build the software package X-MAS (X-ray MAp Simulator)
devoted to simulate X-ray observations of galaxy clusters obtained
from hydro-N-body simulations.
---------------------------------------------------------
Title: The faint X-ray source population near 3C 295
Authors: D'Elia, V.; Fiore, F.; Elvis, M.; Cappi, M.; Mathur, S.;
Mazzotta, P.; Falco, E.; Cocchia, F.
2004ogci.conf...39D Altcode: 2004IAUCo.195...39D
We present a statistical analysis of the Chandra observation of the
source field around the 3C 295 galaxy cluster (z=0.46). Three different
methods of analysis, namely a chip by chip LogN-LogS, a two-dimentional
Kolmogorov-Smirnov (KS) test, and the angular correlation function
(ACF) show a strong overdensity of sources in the North-East of the
field, that may indicate a filament of the large scale structure of
the universe towards 3C 295.
---------------------------------------------------------
Title: X-ray sources overdensity around the 3C 295 galaxy cluster
Authors: D'Elia, V.; Fiore, F.; Elvis, M.; Cappi, M.; Mathur, S.;
Mazzotta, P.; Falco, E.
2004NuPhS.132...54D Altcode: 2003astro.ph.10744D
We present a statistical analysis of the Chandra observation of the
source field around the 3C 295 galaxy cluster (z=0.46). The logN-logS
of this field is in good agreement with that computed for the Chandra
Deep Field South in this work and in previous ones. Nevertheless,
the logN-logS computed separately for the four ACIS-I chips reveals
that there is a significant excess of sources to the North-North East
and a void to the South of the central cluster. Such an asymmetric
distribution is confirmed by the two-dimensional Kolmogorov-Smirnov
test, which excludes (P~3%) a uniform distribution. In addition,
a strong spatial correlation emerges from the study of the angular
correlation function of the field: the angular correlation function
is above that expected for X-ray sources on a few arcmin scales. In
synthesis, the present analysis may indicate a filament of the large
scale structure of the Universe toward 3C 295. This kind of study may
open-up a new way to map (with high efficiency) high-density peaks of
large scale structures at high redshift.
---------------------------------------------------------
Title: The Faint X-ray Source Population Near the 3C 295 cluster
Authors: D'Elia, V.; Fiore, F.; Elvis, M.; Cappi, M.; Mathur, S.;
Mazzotta, P.; Falco, E.; Cocchia, F.
2004astro.ph..6080D Altcode:
We present a statistical analysis of the Chandra observation of the
source field around the 3C 295 galaxy cluster (z=0.46). Three different
methods of analysis, namely a chip by chip logN-logS, a two dimentional
Kolmogorov-Smirnov (KS) test, and the angular correlation function
(ACF) show a strong overdensity of sources in the North-East of the
field, that may indicate a filament of the large scale structure of
the Universe toward 3C 295.
---------------------------------------------------------
Title: Simulating Chandra observations of galaxy clusters
Authors: Gardini, A.; Rasia, E.; Mazzotta, P.; Tormen, G.; De Grandi,
S.; Moscardini, L.
2004MNRAS.351..505G Altcode: 2003astro.ph.10844G
Although trivial in principle, direct comparison of galaxy clusters
X-ray observations to numerical hydro-N-body simulations is not
always simple, because of many possible artefacts introduced by
the instrument response, sky background and instrumental noise. To
address these problems, we constructed the software package X-MAS
(X-ray Map Simulator), a tool devoted to simulate X-ray observations
of galaxy clusters obtained from hydro-N-body simulations. One of
the main features of X-MAS is the ability to generate event files
following the same standards used for real observations. This implies
that its simulated observations can be analysed in the same way as
- and with the same tools of - real observations. In this paper we
present how the X-MAS package works, and discuss its application to
the simulation of Chandra ACIS-S3 observations. Using the results of
high-resolution hydro-N-body simulations, we generate fake Chandra
observations of a number of simulated clusters. We then compare some
of the main physical properties of the input data to those derived
from the simulated observations after performing a standard imaging
and spectral analysis. We find that, because of the sky background,
the lower surface brightness spatial substructures, which can be
easily identified in the simulations, are no longer detected in the
simulated observations. We also show that, when a cluster has a complex
(i.e. not isothermal) thermal structure along the line of sight, then
the projected spectroscopic temperature obtained from the observation
is significantly lower than the emission-weighed value inferred directly
from hydrodynamical simulation. This implies that much attention should
be paid in the theoretical interpretation of observed temperatures.
---------------------------------------------------------
Title: Massive Galaxy Clusters - New Insights from Hubble and Chandra
Authors: Smith, G. P.; Kneib, J. -P.; Smail, I.; Mazzotta, P.; Ebeling,
H.; Czoske, O.
2003AAS...203.3001S Altcode: 2003BAAS...35.1252S
Massive galaxy clusters contain vast quantities of luminous and
non-luminous material, including dark matter, X-ray emitting plasma
and stars. The high projected matter densities reached in these deep
(and rare) potential wells render them powerful gravitational lenses,
causing the appearance of more distant galaxies to be magnified and
distorted. The superb image quality of Hubble Space Telescope (HST)
observations offers uniquely precise constraints on the distribution of
matter in these spectacular systems. I will present new results from a
systematic survey of ten X-ray luminous clusters at z=0.2. Our sensitive
high-resolution HST imaging of the cluster cores is essential to detect
and measure reliably the lensing signal in this objectively selected
cluster sample. I use a sophisticated ray-tracing code to interpret
this signal, and thus to measure the mass and structure of the cluster
cores. Analysis of archival Chandra observations of the same clusters
complements the lensing analysis and allows us to relate the details
of the total cluster matter distribution to the thermodynamics of the
intra-cluster medium. In summary, we find that 70% of X-ray luminuos
clusters at z=0.2 are dynamically immature and have likely experienced
infall from the field in the previous 2-3Gyr. The normalization of the
mass-temperature relation for the immature clusters is 30% hotter than
for the mature clusters. I will briefly discuss the implications of
these results for large-scale structure, including the normalization
of the matter power spectrum and the evolution of massive clusters.
---------------------------------------------------------
Title: Kinetic Sunyaev-Zel'dovich Effect and Cosmic Microwave
Background Polarization from Subsonic Bulk Motions of Dense Gas
Clouds in Galaxy Cluster Cores
Authors: Diego, J. M.; Mazzotta, P.; Silk, J.
2003ApJ...597L...1D Altcode: 2003astro.ph..9181D
Recent Chandra observations have revealed the presence of cold fronts
in many clusters of galaxies. The cold fronts are believed to be
produced by the bulk motions of massive, dense, cold gas clouds with
respect to the hotter, more rarefied ambient gas at velocities that
can be as high as the speed of sound. This phenomenon may produce a
significant contamination of both the kinetic Sunyaev-Zel'dovich (SZ)
effect and the cosmic microwave background (CMB) polarization pattern
observed in the direction of a cluster. We estimate the contributions
to the kinetic SZ effect and to the CMB polarization toward galaxy
clusters produced by the bulk motions of the gas in the inner parts of
galaxy clusters. The observed cold fronts probe the absolute velocities
of the gas motion, while the induced polarization and the kinetic SZ
effect probe the transverse and the radial components, respectively. We
show that these signals may be easily detected with sensitive future
experiments, opening an exciting new window for studies of galaxy
cluster internal dynamics and eventually facilitating reconstruction
of the intrinsic cluster polarization of the CMB and the associated
measure of the local CMB quadrupole.
---------------------------------------------------------
Title: X-Ray Sources Overdensity Around 3C 295
Authors: D'Elia, V.; Fiore, F.; Elvis, M.; Cappi, M.; Mathur, S.;
Mazzotta, P.; Falco, E.
2003astro.ph.10506D Altcode:
We present a statistical analysis of the Chandra observation of
the source field around the 3C 295 galaxy cluster ($z=0.46$). Three
different methods of analysis, namely a chip by chip logN-logS, a two
dimentional Kolmogorov-Smirnov (KS) test, and the angular correlation
function (ACF) show a strong overdensity of sources in the North-East
of the field, that may indicate a filament of the large scale structure
of the Universe toward 3C 295.
---------------------------------------------------------
Title: A Chandra Study of the Complex Structure in the Core of
2A 0335+096
Authors: Mazzotta, P.; Edge, A. C.; Markevitch, M.
2003ApJ...596..190M Altcode: 2003astro.ph..3314M
We present a Chandra observation of the central (r<200 kpc) region of
the cluster of galaxies 2A 0335+096, rich in interesting phenomena. On
large scales (r>40 kpc), the X-ray surface brightness is symmetric
and slightly elliptical. The cluster has a cool, dense core; the
radial temperature gradient varies with position angle. The radial
metallicity profile shows a pronounced central drop and an off-center
peak. Similarly to many clusters with dense cores, 2A 0335+096 hosts a
cold front at r~40 kpc south of the center. The gas pressure across
the front is discontinuous by a factor A<SUB>P</SUB>=1.6+/-0.3,
indicating that the cool core is moving with respect to the ambient
gas with a Mach number M~0.75+/-0.2. The central dense region inside
the cold front shows an unusual X-ray morphology, which consists of
a number of X-ray blobs and/or filaments on scales >~3 kpc, along
with two prominent X-ray cavities. The X-ray blobs are not correlated
with either the optical line emission (Hα+[N II]), member galaxies,
or radio emission. The deprojected temperature of the dense blobs is
consistent with that of the less dense ambient gas, so these gas phases
do not appear to be in thermal pressure equilibrium. An interesting
possibility is a significant, unseen nonthermal pressure component in
the interblob gas, possibly arising from the activity of the central
active galactic nucleus (AGN). We discuss two models for the origin
of the gas blobs-hydrodynamic instabilities caused by the observed
motion of the gas core and “bubbling” of the core caused by multiple
outbursts of the central AGN.
---------------------------------------------------------
Title: Detecting X-ray filaments in the low-redshift Universe with
XEUS and Constellation-X
Authors: Viel, M.; Branchini, E.; Cen, R.; Matarrese, S.; Mazzotta,
P.; Ostriker, J. P.
2003MNRAS.341..792V Altcode: 2002astro.ph.10497V
We propose a possible way to detect baryons at low redshifts from
the analysis of X-ray absorption spectra of bright AGN pairs. A simple
semi-analytical model to simulate the spectra is presented. We model the
diffuse warm-hot intergalactic medium (WHIM) component, responsible for
the X-ray absorption, using inputs from high-resolution hydrodynamical
simulations and analytical prescriptions. We show that the number
of OVII absorbers per unit redshift with column density larger than
10<SUP>13.5</SUP> cm<SUP>-2</SUP>- corresponding to an equivalent
width of ~1 km s<SUP>-1</SUP>- that will possibly be detectable by
XEUS, is >~30 per unit redshift. Constellation-X will detect ~6
OVII absorptions per unit redshift with an equivalent width of 10
km s<SUP>-1</SUP>. Our results show that, in a ΛCDM universe, the
characteristic size of these absorbers at z~ 0.1 is ~1 h<SUP>-1</SUP>
Mpc. The filamentary structure of WHIM can be probed by finding
coincident absorption lines in the spectra of background AGN pairs. We
estimate that at least 20 AGN pairs at separation <~20 arcmin are
needed to detect this filamentary structure at the 3σ level. Assuming
observations of distant sources using XEUS for exposure times of 500
ks, we find that the minimum source flux to probe the filamentary
structure is ~2 × 10<SUP>-12</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>
in the 0.1-2.4 keV energy band. Thus, most pairs of these extragalactic
X-ray bright sources have already been identified in the ROSAT All-Sky
Survey. Re-observation of these objects by future missions could be
a powerful way to search for baryons in the low-redshift Universe.
---------------------------------------------------------
Title: Chandra Temperature Map of A754 and Constraints on Thermal
Conduction
Authors: Markevitch, M.; Mazzotta, P.; Vikhlinin, A.; Burke, D.;
Butt, Y.; David, L.; Donnelly, H.; Forman, W. R.; Harris, D.; Kim,
D. -W.; Virani, S.; Vrtilek, J.
2003ApJ...586L..19M Altcode: 2003astro.ph..1367M
We use Chandra data to derive a detailed gas temperature map of
the nearby, hot, merging galaxy cluster A754. Combined with the
X-ray and optical images, the map reveals a more complex merger
geometry than previously thought, possibly involving more than two
subclusters or a cool gas cloud sloshing independently from its former
host subcluster. In the cluster central region, we detect spatial
variations of the gas temperature on all linear scales, from 100 kpc
(the map resolution) and up, which likely remain from a merger shock
passage. These variations are used to derive an upper limit on effective
thermal conductivity on a 100 kpc scale, which is at least an order of
magnitude lower than the Spitzer value. This constraint pertains to the
bulk of the intracluster gas, as compared to the previously reported
estimates for cold fronts (which are rather peculiar sites). If the
conductivity in a tangled magnetic field is at the recently predicted
higher values (i.e., about 1/5 Spitzer), the observed suppression
can be achieved, for example, if the intracluster gas consists of
magnetically isolated domains.
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Title: XMM-Newton Proposal 02017516
Authors: Mazzotta, Pasquale
2003xmm..prop...94M Altcode:
The observed X-ray luminosities of groups are inconsistent with
a model in which the intragroup medium is shock-heated during the
collapse. It is thought that a combination of pre-heating, gas cooling
and energy injection removes low entropy gas, reducing the system's
X-ray luminosity. However, the extent of this process is uncertain
because the previous selection of group catalogs has been based on
X-ray emission. We have constructed a complete, mass-selected catalog
of groups from the 2dFGRS. X-ray observations of this sample would
for the first time provide accurate determinations of the entropy in
a mass-selected sample. These observations are of key importance for
understanding the thermal history of the intragroup medium and the
interplay between X-ray cooling and galaxy formation.
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Title: Study of a Cold Front in a Massive Cooling Flow Cluster of
Galaxies with Strong Lensing
Authors: Mazzotta, Pasquale
2002cxo..prop.1311M Altcode: 2002chan.prop.1282M; 2002cxo..prop.1282M
Using the data contained in the Chandra archive we discovered a cold
front in the atmosphere of the cluster of galaxies MS1455.0+2232. The
importance of this finding is related to the fact that: i) it represents
the biggest edge observed so far; ii) it lies in one of the most
massive cooling flow clusters known; iii) the optical image of the
cluster hosts a lensed arc inside the cold front sector. Moreover the
X-ray and the lensig estimates show a discrepancy of a factor 1.8. It
has been argued that cold fronts may both influence the development
of cooling flows as well as to induce a mass bias that could explain
point iii) above. We propose a deep Chandra follow-up of MS1455.0+2232
that will shade light on the above issues.
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Title: Chandra Observation of a 300 Kiloparsec Hydrodynamic
Instability in the Intergalactic Medium of the Merging Cluster of
Galaxies A3667
Authors: Mazzotta, Pasquale; Fusco-Femiano, Roberto; Vikhlinin, Alexey
2002ApJ...569L..31M Altcode: 2002astro.ph..1423M
We present results from the combination of two Chandra pointings of
the central region of the cluster of galaxies A3667. From the data
analysis of the first pointing, Vikhlinin, Markevitch, and Murray
reported the discovery of a prominent cold front that is interpreted
as the boundary of a cool gas cloud moving through the hotter ambient
gas. They discussed the role of the magnetic fields in maintaining the
apparent dynamical stability of the cold front over a wide sector at the
forward edge of the moving cloud and in suppressing transport processes
across the front. In this Letter, we identify two new features in the
X-ray image of A3667: (1) a 300 kpc arclike filamentary X-ray excess
extending from the cold gas cloud border into the hotter ambient gas and
(2) a similar arclike filamentary X-ray depression that develops inside
the gas cloud. Both features are located beyond the sector identified
by the cold front and are oriented in a direction perpendicular to the
direction of motion. The temperature map suggests that the temperature
of the filamentary excess is consistent with that inside the gas cloud,
while the temperature of the depression is consistent with that of the
ambient gas. We suggest that the observed features represent the first
evidence for the development of a large-scale hydrodynamic instability
in the cluster atmosphere resulting from a major merger. This result
confirms previous claims for the presence of a moving cold gas cloud
in the hotter ambient gas. Moreover, it shows that, although the gas
mixing is suppressed at the leading edge of the subcluster as a result
its magnetic structure, strong turbulent mixing occurs at larger angles
toward the direction of motion. We show that this mixing process may
favor the deposition of a nonnegligible quantity of thermal energy
right in the cluster center, affecting the development of the central
cooling flow.
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Title: Evidence for a Heated Gas Bubble inside the “Cooling Flow”
Region of MKW 3s
Authors: Mazzotta, P.; Kaastra, J. S.; Paerels, F. B.; Ferrigno, C.;
Colafrancesco, S.; Mewe, R.; Forman, W. R.
2002ApJ...567L..37M Altcode: 2001astro.ph..7557M
We report on the deep Chandra observation of the central r=200
kpc region of the cluster of galaxies MKW 3s, which was previously
identified as a moderate cooling flow cluster. The Chandra image
reveals two striking features-a 100 kpc long and 21 kpc wide filament,
extending from the center to the southwest, and a nearly circular, 50
kpc diameter depression 90 kpc south of the X-ray peak. The temperature
map shows that the filamentary structure is colder while the surface
brightness depression is hotter than the average cluster temperature
at any radius. The hot and the cold regions indicate that both cooling
and heating processes are taking place in the center of MKW 3s. We
argue that the surface brightness depression is produced by a heated,
low-density gas bubble along the line of sight. We suggest that the
heated bubble is produced by short-lived nuclear outbursts from the
central galaxy.
---------------------------------------------------------
Title: Development of Hydrodynamic Instability in the Intergalactic
Medium of the Merging Cluster of Galaxies A3667
Authors: Mazzotta, Pasquale; Vikhlinin, Alexey; Fusco-Femiano, Roberto;
Markevich, Maxim
2002astro.ph..2324M Altcode:
A3667, a spectacular merger cluster, was observed by Chandra twice. In
this paper we review the main results of the analysis of these
observations. In particular we show evidence for the presence in the
cluster of a 300 kpc Kelvin-Helmholtz hydrodynamic instability. We
discuss the development of such instability and the structure of the
intracluster magnetic filed in light of a self-consistent cluster
dynamical model.
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Title: Chandra Observations of Cold Fronts in Clusters of Galaxies
Authors: Mazzotta, P.; Markevitch, M.; Vikhlinin, A.; Forman, W. R.
2002ASPC..257..173M Altcode: 2002hzcm.conf..173M; 2001astro.ph..9420M
High-resolution Chandra images of several clusters of galaxies
reveal sharp, edge-like discontinuities in their gas density. The
gas temperature is higher in front of the edge where the density is
low, corresponding to approximately continuous pressure across the
edge. This new phenomenon was called “cold fronts”, to contrast it
to shock fronts that should look similar in X-ray images but where the
temperature should jump in the opposite direction. The first cold fronts
were discovered in merging clusters, where they appear to delineate
the boundaries of dense cool subcluster remnants moving through and
being stripped by the surrounding shock-heated gas. Later, Chandra
revealed cold fronts in the central regions of several apparently
relaxed clusters. To explain the gas bulk motion in these clusters,
we propose either a peculiar cluster formation history that resulted
in an oscillating core, or gas sloshing (without the involvement of
the underlying dark matter peak) caused by past subcluster infall or
central AGN activity. We review these observations and discuss their
implications for the X-ray cluster mass estimates.
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Title: Nonhydrostatic Gas in the Core of the Relaxed Galaxy Cluster
A1795
Authors: Markevitch, M.; Vikhlinin, A.; Mazzotta, P.
2001ApJ...562L.153M Altcode: 2001astro.ph..8520M
Chandra data on A1795 reveal a mild edge-shaped discontinuity in the
gas density and temperature in the southern sector of the cluster at
r=60 h<SUP>-1</SUP> kpc. The gas inside the edge is 1.3-1.5 times
denser and cooler than outside, while the pressure is continuous,
indicating that this is a “cold front,” the surface of contact between
two moving gases. The continuity of the pressure indicates that the
current relative velocity of the gases is near zero, making the edge
appear to be in hydrostatic equilibrium. However, a total mass profile,
derived from the data in this sector under the equilibrium assumption,
exhibits an unphysical jump by a factor of 2, with the mass inside
the edge being lower. We propose that the cooler gas is “sloshing”
in the cluster gravitational potential well and is now near the
point of maximum displacement, where it has zero velocity but nonzero
centripetal acceleration. The distribution of this nonhydrostatic gas
should reflect the reduced gravity force in the accelerating reference
frame, resulting in the apparent mass discontinuity. Assuming that the
gas outside the edge is hydrostatic, the acceleration of the moving gas
can be estimated from the mass jump, a~800 h km s<SUP>-1</SUP> (10<SUP>
8</SUP> yr)<SUP>-1</SUP>. The gravitational potential energy of this
gas that is available for dissipation is about half of its current
thermal energy. The length of the cool filament extending from the cD
galaxy (Fabian et al.) may give the amplitude of the gas sloshing,
30-40 h<SUP>-1</SUP> kpc. Such gas bulk motion might be caused by a
disturbance of the central gravitational potential by past subcluster
infall.
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Title: 1WGA J1226.9+3332: A High-Redshift Cluster Discovered by
Chandra
Authors: Cagnoni, I.; Elvis, M.; Kim, D. -W.; Mazzotta, P.; Huang,
J. -S.; Celotti, A.
2001ApJ...560...86C Altcode: 2001astro.ph..6066C
We report the detection of 1WGA J1226.9+3332 as an arcminute-scale
extended X-ray source with the Chandra X-Ray Observatory. The
Chandra observation and R- and K-band imaging strongly support
the identification of 1WGA 1226.9+3332 as a high-redshift
cluster of galaxies, most probably at z=0.85+/-0.15, with an
inferred temperature kT=10<SUP>+4</SUP><SUB>-3</SUB> keV, and
an unabsorbed luminosity (in a r=120<SUP>”</SUP> aperture)
of 1.3<SUP>+0.16</SUP><SUB>-0.14</SUB>×10<SUP>45</SUP> ergs
s<SUP>-1</SUP> (0.5-10 keV). This indication of redshift is also
supported by the K- and R-band imaging and is in agreement with the
spectroscopic redshift of 0.89 found by Ebeling and coworkers. The
surface brightness profile is consistent with a β model with
β=0.770+/-0.025, r<SUB>c</SUB>=18.1"+/-0.9" (corresponding to 101+/-5
kpc at z=0.89), and S(0)=1.02+/-0.08 counts arcsec<SUP>-2</SUP>. 1WGA
J1226.9+3332 was selected as an extreme X-ray-loud source with
F<SUB>X</SUB>/F<SUB>V</SUB>>60 this selection method, thanks to the
large area sampled, seems to be a highly efficient method for finding
luminous, high-z clusters of galaxies.
---------------------------------------------------------
Title: RXJ1720.1+2638: a Nearly Relaxed Cluster with a Fast Moving
Core?
Authors: Mazzotta, Pasquale
2001cxo..prop.1000M Altcode: 2001cxo..prop..992M; 2001chan.prop..992M
Observed with previous X-ray missions, RXJ1720.1+2638 looks like the
prototype of a "relaxed cluster of galaxies". The cluster appears
azimuthally symmetric and the X-ray brightness peak coincides with
the cluster central galaxy. Thanks to its unprecedented spatial
resolution, the Chandra observation of this cluster shows a far more
complex structure. In particular it shows two X-ray features, on the
opposite sides of the X-ray peak, that strongly indicate motion of the
cluster core. Because of the low exposure of the previous observation
several issues relative to the cluster formation and evolution are
answered. We propose a 52ks ASCI-I observation to study the details
of the dual structure in the gravitational potential of this cluster.
---------------------------------------------------------
Title: Chandra Observation of MS 1455.0+2232: cold fronts in a
massive cooling flow cluster?
Authors: Mazzotta, P.; Markevitch, M.; Forman, W. R.; Jones, C.;
Vikhlinin, A.; VanSpeybroeck, L.
2001astro.ph..8476M Altcode:
We present the Chandra observation of the cluster of galaxies MS
1455.0+2232. From previous ASCA and ROSAT observations, this cluster
was identified as a “relaxed” cluster that hosts one of the most
massive cooling flows detected. With higher angular resolution, the
Chandra X-ray image shows the presence of two surface brightness edges
on opposite sides of the X-ray peak: the first at 190 kpc to the north
and the second at 450 kpc to the south. Even though the low exposure of
this observation limits our ability to constrain the temperature jump
across both edges, we show that the northern edge is likely to be a
“cold front” similar to others observed recently by Chandra in the
clusters A2142, A3667, RX J1720.1+2638, and A2256. The observed cold
front is most likely produced by the motion, from south to north,
of a group-size dark matter halo. The most natural explanation for
the presence of this observed moving subclump is that MS 1455.0+2232
is a merger cluster in the very last stage before it becomes fully
relaxed. This scenario, however, appears to be unlikely as the cluster
shows no further sign of ongoing merger. Moreover, it is not clear if
a massive cooling flow could have survived this kind of merger. We
propose an alternative scenario in which, as for RX J1720.1+2638,
MS 1455.0+2232 is the result of the hierarchical collapse of two
co-located density perturbations, the first a group-scale perturbation
collapse followed by a second cluster-scale perturbation collapse
that surrounded, but did not destroy, the first. We suggest that a
cooling flow may have begun inside the already collapsed group-scale
perturbation and may have been later amplified by the gas compression
induced by the infall of the overlying main cluster mass.
---------------------------------------------------------
Title: Chandra Observation of RX J1720.1+2638: a Nearly Relaxed
Cluster with a Fast-moving Core?
Authors: Mazzotta, P.; Markevitch, M.; Vikhlinin, A.; Forman, W. R.;
David, L. P.; van Speybroeck, L.
2001ApJ...555..205M Altcode: 2001astro.ph..2291M
We have analyzed the Chandra observation of the distant (z=0.164)
galaxy cluster RX J1720.1+2638, in which we find sharp features in
the X-ray surface brightness on opposite sides of the X-ray peak:
an edge at about 250h<SUP>-1</SUP><SUB>50</SUB> kpc to the southeast
and a plateau at about 130h<SUP>-1</SUP><SUB>50</SUB> kpc to the
northwest. The surface brightness edge and the plateau can be modeled
as a gas density discontinuity (jump) and a slope change (break). The
temperature profiles suggest that the jump and the break are the
boundaries of a central, group-size (d~380h<SUP>-1</SUP><SUB>50</SUB>
kpc), dense, cold (T~4 keV) gas cloud, embedded in a diffuse hot
(T~10 keV) intracluster medium. The density jump and the temperature
change across the discontinuity are similar to the “cold fronts”
discovered by Chandra in A2142 and A3667 and suggest subsonic motion
of this central gas cloud with respect to the cluster itself. The most
natural explanation is that we are observing a merger in the very last
stage before the cluster becomes fully relaxed. However, the data are
also consistent with an alternative scenario in which RX J1720.1+2638
is the result of the collapse of two co-located density perturbations,
the first a group-scale perturbation collapse followed by a second
cluster-scale perturbation collapse that surrounded, but did not
destroy, the first one. We also show that, because of the core motion,
the total mass inside the cluster core, derived under the assumption of
hydrostatic equilibrium, may underestimate the true cluster mass. If
widespread, such motion may partially explain the discrepancy between
X-ray and the strong-lensing mass determinations found in some clusters.
---------------------------------------------------------
Title: Temperature and total mass profiles of the A3571 cluster
of galaxies
Authors: Nevalainen, J.; Kaastra, J.; Parmar, A. N.; Markevitch, M.;
Oosterbroek, T.; Colafrancesco, S.; Mazzotta, P.
2001A&A...369..459N Altcode: 2001astro.ph..1412N
We present BeppoSAX results of a spatially resolved spectral
analysis of A3571, a relaxed nearby cluster of galaxies. In the
central 2' (130 h<SUB>50</SUB><SUP>-1</SUP> kpc) radius the metal
abundance is 0.49 +/- 0.08 solar and the absorption (1.13 +/- 0.28)
10<SUP>21</SUP> atom cm<SUP>-2</SUP>, whereas elsewhere within an 8'
(520 h<SUB>50</SUB><SUP>-1</SUP> kpc) radius the abundance is 0.32
+/- 0.05 solar and the absorption consistent with the galactic value
of 4.4 10<SUP>20</SUP> atom cm<SUP>-2</SUP>. The significant central
metal abundance enhancement is consistent with the supernova enrichment
scenario. The excess absorption may be attributed to the cooling flow,
whose mass flow rate is 80 +/- 40 M<SUB>sun</SUB> yr<SUP>-1</SUP>
from our spectral fit. The BeppoSAX and ASCA radial temperature
profiles agree over the entire overlapping radial range r < 25' =
1.6 h<SUB>50</SUB><SUP>-1</SUP> Mpc. The combined BeppoSAX and ASCA
temperature profile exhibits a constant value out to a radius of ~ 10'
(650 h<SUB>50</SUB><SUP>-1</SUP> kpc) and a significant decrease (T ~
r<SUP>-0.55</SUP>, corresponding to gamma =1.28) at larger radii. These
temperature data are used to derive the total mass profile. The best
fit NFW dark matter density model results in a temperature profile
that is not convectively stable, but the model is acceptable within
the uncertainties of the data. The temperature profile is acceptably
modeled with a “core” model for the dark matter density, consisting
of a core radius with a constant slope at larger radii. With this model
the total mass and formal 90% confidence errors within the virial radius
r<SUB>178</SUB> (2.5 h<SUB>50</SUB><SUP>-1</SUP> Mpc) are 9.1[+3.6,-1.5]
10<SUP>14</SUP> h<SUB>50</SUB><SUP>-1</SUP> M<SUB>sun</SUB>, by a
factor of 1.4 smaller than the isothermal value. The gas mass fraction
increases with radius, reaching f<SUB>gas</SUB>(r<SUB>178</SUB>) =
0.26[+-0.05,-0.10] x h<SUB>50</SUB><SUP>-3/2</SUP>. Assuming that
the measured gas mass fraction is the lower limit to the primordial
baryonic fraction gives Omega <SUB>m</SUB> < 0.4 at 90% confidence.
---------------------------------------------------------
Title: Chandra Study of an Overdensity of X-Ray Sources around Two
Distant (Z~0.5) Clusters
Authors: Cappi, M.; Mazzotta, P.; Elvis, M.; Burke, D. J.; Comastri,
A.; Fiore, F.; Forman, W.; Fruscione, A.; Green, P.; Harris, D.;
Hooper, E. J.; Jones, C.; Kaastra, J. S.; Kellogg, E.; Murray,
S.; McNamara, B.; Nicastro, F.; Ponman, T. J.; Schlegel, E. M.;
Siemiginowska, A.; Tananbaum, H.; Vikhlinin, A.; Virani, S.; Wilkes, B.
2001ApJ...548..624C Altcode: 2000astro.ph..9199C
We present results from a Chandra X-Ray Observatory study of the
field X-ray source populations in four different observations:
two high-redshift (z~0.5) clusters of galaxies 3C 295 and
RX J003033.2+261819; and two noncluster fields with similar
exposure time. Surprisingly, the 0.5-2 keV source surface
densities (~900-1200 sources deg<SUP>-2</SUP> at a flux limit of
1.5×10<SUP>-15</SUP> ergs cm<SUP>-2</SUP> s<SUP>-1</SUP>) measured in
an ~8<SUP>'</SUP>×8<SUP>'</SUP> area surrounding each cluster exceed
by a factor of ~2 the value expected on the basis of the ROSAT and
Chandra logN-logS, with a significance of ~2 σ each, or ~3.5 σ when
the two fields are combined (i.e., a probability to be a statistical
fluctuation of <1% and <0.04%, respectively). The same analysis
performed on the noncluster fields and on the outer chips of the cluster
fields does not show evidence of such an excess. In both cluster fields,
the summed 0.5-10 keV spectrum of the detected objects is well fitted
by a power law with Γ~1.7 similar to active galactic nuclei (AGNs)
and shows no sign of intrinsic absorption. The few (~10 of 35) optical
identifications available to date confirm that most of them are, as
expected, AGNs, but the number of redshifts available is too small to
allow conclusions on their nature. We discuss possible interpretations
of the overdensity in terms of a statistical variation of cosmic
background sources; a concentration of AGNs and/or powerful starburst
galaxies associated with the clusters; and gravitational lensing of
background QSOs by the galaxy clusters. All explanations, however,
are difficult to reconcile with the large number of excess sources
detected. Deeper X-ray observations and more redshifts measurements
are clearly required to settle the issue.
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Title: Clusters of galaxies among ROSAT blank field sources
Authors: Cagnoni, I.; Elvis, M.; Kim, D. -W.; Mazzotta, P.; Huang,
J. -S.; Celotti, A.
2001cghr.confE..27C Altcode: 2001astro.ph..5430C
We present here an efficient method for selecting high luminosity and
massive high redshift clusters of galaxies, crucially important tools in
cosmology. By selecting bright and extremely X-ray loud (high F(X)/F(V))
sources, we were able to identify 2 high redshift (z=0.45 and z=0.89)
clusters so far and we have evidence for at least one more candidate
at 0.4<z<1.1 out of a total of 16 selected sources.
---------------------------------------------------------
Title: Chandra study of a concentration of X-ray sources around two
distant (z ~ 0.5) clusters
Authors: Cappi, M.; Mazzotta, P.; Burke, D. J.; Comastri, A.;
David, L.; Elvis, M.; Fiore, F.; Forman, W.; Fruscione, A.; Green,
P.; Harris, D.; Hooper, E.; Jones, C.; Kaastra, J. S.; Kellogg, E.;
Murray, S.; McNamara, B.; Nicastro, F.; Ponman, T. J.; Schlegel, E. M.;
Siemiginowska, A.; Tananbaum, H.; Vikhlinin, A.; Virani, S.; Wilkes, B.
2001MmSAI..72..207C Altcode:
We present preliminary results from a Chandra X-ray Observatory
study of the field X-ray source populations in 3 different fields:
two include the two medium-redshift (z~0.5) clusters of galaxies 3C
295 and RXJ003033.2+261819, and the third is a non-cluster field with
similar exposure time. Surprisingly, the 0.5 - 2 keV source surface
densities (~900 - 1200 sources deg<SUP>-2</SUP> at a flux limit of
1.5×10<SUP>-15</SUP> erg cm<SUP>-2</SUP> s<SUP>-1</SUP>) measured in
an ~8'×8' area surrounding each cluster exceed by a factor of ~2 the
value expected on the basis of the ROSAT logN-logS, with a significance
of ~2σ each. The same analysis performed on the non-cluster field and
on the outer chips of the cluster fields does not show evidence of such
an excess. In both cluster fields, the summed 0.5 - 10 keV spectrum
of the detected objects is well fitted by a power-law with Γ ~ 1.7
similar to AGNs and shows no sign of intrinsic absorption. The few
(~20%) optical identifications available to date confirm that most
of them are, as expected, AGNs but the number of redshifts available
is too small to allow conclusions. If associated with the clusters
(as supported by their apparent concentrations around the clusters),
their X-ray luminosities (~10<SUP>42-43</SUP> erg s<SUP>-1</SUP> on
average) are typical of Seyfert-like galaxies. Optical classification
of more sources are clearly required to settle the issue.
---------------------------------------------------------
Title: Temperature Structure of Four Merging Clusters Obtained
with Chandra
Authors: Markevitch, M.; Vikhlinin, A.; Mazzotta, P.; VanSpeybroeck, L.
2000astro.ph.12215M Altcode:
We present preliminary Chandra results on z=0.2 clusters A665, A2163
and A2218, and a z=0.05 cluster A754. For A754, A665 and A2163, we have
derived first high-resolution projected gas temperature maps. All three
show strong spatial temperature variations in the inner r<0.5-1
Mpc regions, indicating ongoing mergers. The maps reveal a probable
shock in front of a moving cluster core in A665, a rather complicated
temperature distribution in the center of A2163, and possibly a merger
of three subclusters in A754. At greater off-center distances, radial
profiles for A2163 and A2218 show a temperature decline, in agreement
with earlier ASCA results.
---------------------------------------------------------
Title: Chandra Observation of RXJ1720.1+2638: Study of a Cluster
Core Moving in its Own Environment
Authors: Mazzotta, P.; van Speybroeck, L.; David, L. P.; Forman,
W. R.; Markevitch, M.; Vikhlinin, A.
2000HEAD....5.4404M Altcode: 2000BAAS...32.1651M
We have analyzed the Chandra observation of the distant (z=0.164) galaxy
cluster RXJ1720.1+2638 in which we find a sharp edge and plateau in
the X-ray surface brightness at about 250 h<SUB>50</SUB><SUP>-1</SUP>
kpc and 130 h<SUB>50</SUB><SUP>-1</SUP> kpc from the X-ray peak
respectively. These features are consistent with a density discontinuity
and a density break, on angular scales <= 10<SUP>”</SUP>. The
temperature profiles suggest that the edge and the break are the
boundaries of a central, group-size (d≈ 380h<SUB>50</SUB><SUP>-1</SUP>
kpc), dense, cold thermally isolated (T≈ 4 keV) gas cloud, embedded
in a more diffuse hot (T≈ 10 keV) ambient intracluster. The density
jump and the temperature change across the discontinuity are similar
to the edge discovered by Chandra in A2142 and A3667, and suggest a
subsonic motion of this central gas cloud with respect to the cluster
itself. As for A2142 and A3667, the most natural explanation for
this cluster is that we are observing a merger cluster. However the
cluster appears to be relaxed just outside the two density features,
thus we suggest that the merger is in the very last stage before
the cluster become fully relaxed. We show that the gas inside the
central cloud is not in hydrostatic equilibrium and, thus, the X-ray
cluster mass determination on scales smaller than gas cloud size may
be substantially influenced. The dimension of the moving cloud is
comparable to the cluster core and to the Einstein ring. If, as we
suspect, RXJ1720.1+2638 is not a “special” cluster and the core-size
gas cloud motion phenomenon is present in many other clusters, then
it may partially explain the discrepancy between X-ray and the strong
lensing mass determination found in some systems. P.M. is supported
by ESA fellowship.
---------------------------------------------------------
Title: Chandra Observation of Abell 2142: Survival of Dense Subcluster
Cores in a Merger
Authors: Markevitch, M.; Ponman, T. J.; Nulsen, P. E. J.; Bautz, M. W.;
Burke, D. J.; David, L. P.; Davis, D.; Donnelly, R. H.; Forman, W. R.;
Jones, C.; Kaastra, J.; Kellogg, E.; Kim, D. -W.; Kolodziejczak, J.;
Mazzotta, P.; Pagliaro, A.; Patel, S.; Van Speybroeck, L.; Vikhlinin,
A.; Vrtilek, J.; Wise, M.; Zhao, P.
2000ApJ...541..542M Altcode: 2000astro.ph..1269M
We use Chandra data to map the gas temperature in the central region
of the merging cluster A2142. The cluster is markedly nonisothermal;
it appears that the central cooling flow has been disturbed but
not destroyed by a merger. The X-ray image exhibits two sharp,
bow-shaped, shocklike surface brightness edges or gas density
discontinuities. However, temperature and pressure profiles across
these edges indicate that these are not shock fronts. The pressure is
reasonably continuous across these edges, while the entropy jumps in
the opposite sense to that in a shock (i.e., the denser side of the
edge has lower temperature, and hence lower entropy). Most plausibly,
these edges delineate the dense subcluster cores that have survived
a merger and ram pressure stripping by the surrounding shock-heated gas.
---------------------------------------------------------
Title: An X-ray and optical study of the cluster A33
Authors: Colafrancesco, S.; Mullis, C. R.; Wolter, A.; Gioia, I. M.;
Maccacaro, T.; Antonelli, A.; Fiore, F.; Kaastra, J.; Mewe, R.;
Rephaeli, Y.; Fusco-Femiano, R.; Antonuccio-Delogu, V.; Matteucci,
F.; Mazzotta, P.
2000A&AS..144..187C Altcode: 2000astro.ph..2224C
We report the first detailed X-ray and optical observations of the
medium-distant cluster A33 obtained with the Beppo-SAX satellite and
with the UH 2.2 m and Keck II telescopes at Mauna Kea. The information
deduced from X-ray and optical imaging and spectroscopic data allowed us
to identify the X-ray source 1SAXJ0027.2-1930 as the X-ray counterpart
of the A33 cluster. The faint, F_{2-10 keV} ~ 2.4 10<SUP>-13</SUP>
erg s<SUP>-1</SUP> cm<SUP>-2</SUP>, X-ray source 1SAXJ0027.2-1930, ~
2 arcmin away from the optical position of the cluster as given in the
Abell catalogue, is identified with the central region of A33. Based
on six cluster galaxy redshifts, we determine the redshift of A33,
z=0.2409; this is lower than the value derived by \cite[Leir &
Van Den Bergh (1977)]{lei77}. The source X-ray luminosity, L_{2-10
keV} = 7.7 10<SUP>43</SUP> erg s<SUP>-1</SUP> cm<SUP>-2</SUP>,
and intracluster gas temperature, T = 2.9 keV, make this cluster
interesting for cosmological studies of the cluster L_X-T relation at
intermediate redshifts. Two other X-ray sources in the A33 field are
identified. An AGN at z=0.2274, and an M-type star, whose emissions
are blended to form an extended X-ray emission ~ 4 arcmin north of
the A33 cluster. A third possibly point-like X-ray source detected ~
3 arcmin north-west of A33 lies close to a spiral galaxy at z=0.2863
and to an elliptical galaxy at the same redshift as the cluster.
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Title: Chandra X-Ray Detection of the Radio Hot Spots of 3C 295
Authors: Harris, D. E.; Nulsen, P. E. J.; Ponman, T. J.; Bautz,
M.; Cameron, R. A.; David, L. P.; Donnelly, R. H.; Forman, W. R.;
Grego, L.; Hardcastle, M. J.; Henry, J. P.; Jones, C.; Leahy, J. P.;
Markevitch, M.; Martel, A. R.; McNamara, B. R.; Mazzotta, P.; Tucker,
W.; Virani, S. N.; Vrtilek, J.
2000ApJ...530L..81H Altcode: 1999astro.ph.11381H
An observation of the radio galaxy 3C 295 during the calibration phase
of the Chandra X-Ray Observatory reveals X-ray emission from the core of
the galaxy, from each of the two prominent radio hot spots, and from the
previously known cluster gas. We discuss the possible emission processes
for the hot spots and argue that a synchrotron self-Compton (SSC)
model is preferred for most or all of the observed X-ray emission. SSC
models with near-equipartition fields thus explain the X-ray emission
from the hot spots in the two highest surface brightness FR II radio
galaxies, Cygnus A and 3C 295. This lends weight to the assumption of
equipartition and suggests that relativistic protons do not dominate
the particle energy density.
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Title: Chandra X-ray Detection of the Radio Hotspots of 3C 295
Authors: Harris, D. E.; Cameron, R. A.; David, L. P.; Donnelly, R. H.;
Forman, W. R.; Grego, L.; Jones, C.; Markevitch, M.; McNamara, B. R.;
Mazzotta, P.; Nulsen, P.; Ponman, T. J.; Tucker, W.; Virani, S. N.;
Vrtilek, J.; Leahy, J. P.; Martel, A. R.; Bautz, M.; Hardcastle, M.;
Henry, P.
1999AAS...195.2004H Altcode: 1999BAAS...31.1403H
An observation of 3C 295 during the calibration phase reveals X-ray
emission from the previously known cluster gas, the core of the
galaxy, and from each of the two prominent radio hotspots. We discuss
the possible emission processes for the hotspots and argue that a
synchrotron self-Compton model is preferred for part or all of the
observed X-ray emission.
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Title: The Planck Surveyor mission: astrophysical prospects
Authors: de Zotti, Gianfranco; Toffolatti, Luigi; Argüeso, Francisco;
Davies, Rodney D.; Mazzotta, Pasquale; Partridge, R. Bruce; Smoot,
George F.; Vittorio, Nicola
1999AIPC..476..204D Altcode: 1999astro.ph..2103D; 1999tkc..conf..204D
Although the Planck Surveyor mission is optimized to map the cosmic
microwave background anisotropies, it will also provide extremely
valuable information on astrophysical phenomena. We review our present
understanding of Galactic and extragalactic foregrounds relevant to
the mission and discuss on one side, Planck's impact on the study of
their properties and, on the other side, to what extent foreground
contamination may affect Planck's ability to accurately determine
cosmological parameters. Planck's multifrequency surveys will be unique
in their coverage of large areas of the sky (actually, of the full sky);
this will extend by two or more orders of magnitude the flux density
interval over which mm/sub-mm counts of extragalactic sources can be
determined by instruments already available (like SCUBA) or planned for
the next decade (like the LSA-MMA or the space mission FIRST), which
go much deeper but over very limited areas. Planck will thus provide
essential complementary information on the epoch-dependent luminosity
functions. Bright radio sources will be studied over a poorly explored
frequency range where spectral signatures, essential to understand the
physical processes that are going on, show up. The Sunyaev-Zeldovich
effect, with its extremely rich information content, will be observed
in the direction of a large number of rich clusters of Galaxies. Thanks
again to its all sky coverage, Planck will provide unique information
on the structure and on the emission properties of the interstellar
medium in the Galaxy. At the same time, the foregrounds are unlikely
to substantially limit Planck's ability to measure the cosmological
signals. Even measurements of polarization of the primordial Cosmic
Microwave background fluctuations appear to be feasible.
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Title: X-ray spectra from hot thin plasmas: first results from a new,
updated plasma code
Authors: Mazzotta, P.; Mazzitelli, P.; Colafrancesco, S.; Vittorio, N.
1999NuPhS..69..585M Altcode:
We present in this paper new and updated calculations of the ionization
equilibrium for all the elements from He to Ni. Moreover, we discuss
some preliminary results on the application of such calculations to
a new spectral code for the X-ray continuum and line emission from
hot plasmas.
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Title: Evolution of distant X-ray clusters of galaxies: the BeppoSAX
data
Authors: Colafrancesco, S.; Antonelli, A.; Mazzotta, P.; Vittorio, N.
1999NuPhS..69..573C Altcode:
We present the results of the Beppo-SAX observations of two distant
z~0.3 galaxy clusters: A348 and A33. We outline the main results of
the data analysis and discuss the cosmological relevance of these new
data for the evolution of the Inter Galactic Medium (IGM) in distant
clusters of galaxies.
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Title: A New Ionization Balance for Optically Thin Plasmas: the
Implication for the Calculated X Ray Spectrum.
Authors: Mazzotta, P.; Mazzitelli, G.
1998tx19.confE.525M Altcode:
The next coming X ray mission will allow us to measure the
emission of the astrophysical X-ray sources with high energy
resolution. Nevertheless to determine the relevant physical parameters
describing the plasmas we need to compare observed data with a t This
year we developed a new ionization balance code. This code as been
already included in the spectral code SPEX. In this paper we show how
the result of the standard analysis of AXAF or XMM spectra could be
affected by the use of different ionization b
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Title: Ionization balance for optically thin plasmas: Rate
coefficients for all atoms and ions of the elements H to NI
Authors: Mazzotta, P.; Mazzitelli, G.; Colafrancesco, S.; Vittorio, N.
1998A&AS..133..403M Altcode: 1998astro.ph..6391M
We present in this paper new and updated calculations of the ionization
equilibrium for all the elements from H to Ni. We collected for these
elements all the data available in the literature for the ionization
and radiative plus dielectronic recombination rates. In particular,
the dielectronic rates have been fitted with a single formula and
the related coefficients are tabulated. Our results are compared with
previous works. Tables 1 and 2 are available only in electronic form
at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
or via http://cdsweb.u-strasbg.fr/Abstract.html
---------------------------------------------------------
Title: VizieR Online Data Catalog: Ionization balance for optically
thin plasmas (Mazzotta+ 1998)
Authors: Mazzotta, P.; Mazzitelli, G.; Colafrancesco, S.; Vittorio, N.
1998yCat..41330403M Altcode:
Fitting coefficients for dielectronic recombination rates of formula
(7) of the paper are detailed in two tables. (2 data files).
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Title: The T - L Correlation for Distant Galaxy Clusters
Authors: Colafrancesco, S.; Mazzotta, P.; Vittorio, N.
1998lsst.conf..159C Altcode:
In this paper we discuss the constrains that high-quality observations
of clusters at $z \sim 0.3$ can pose on the evolution of their intra
cluster (IC) gas and on the overall cosmological parameters.
---------------------------------------------------------
Title: Ionization Balance for Optically Thin Plasmas: Rate
Coefficients for all Atoms and Ions of the Elements H to Ni and
implication for the calculated X-ray spectrum
Authors: Mazzotta, Pasquale; Mazzitelli, Giuseppe
1998sxmm.confE..33M Altcode:
No abstract at ADS
---------------------------------------------------------
Title: Is the Cluster Temperature Function a Reliable Test for
Ω<SUB>0</SUB>?
Authors: Colafrancesco, Sergio; Mazzotta, Pasquale; Vittorio, Nicola
1997ApJ...488..566C Altcode: 1997astro.ph..5167C
We discuss the evolution of the cluster temperature function (TF)
in different scenarios for structure formation. We use the commonly
adopted procedure of fitting the model parameters to the local TF
data to find the best-fit values and, most of all, the associated
statistical errors. These errors yield an uncertainty in the prediction
of the TF evolution. We conclude that, at the moment, observations
of cluster temperatures at z <~ 0.5 could provide only a weak test
for Ω<SUB>0</SUB>.
---------------------------------------------------------
Title: Intracluster Comptonization of the Cosmic Microwave Background:
Mean Spectral Distortion and Cluster Number Counts
Authors: Colafrancesco, S.; Mazzotta, P.; Rephaeli, Y.; Vittorio, N.
1997ApJ...479....1C Altcode: 1997astro.ph..3121C
The mean sky-averaged Comptonization parameter, ȳ, describing the
scattering of the cosmic microwave background (CMB) by hot gas in
clusters of galaxies, is calculated in an array of flat and open
cosmological and dark matter models. The models are globally normalized
to fit cluster X-ray data, and intracluster gas is assumed to have
evolved in a manner consistent with current observations. We predict
values of ȳ lower than the COBE/FIRAS upper limit. The corresponding
values of the overall optical thickness to Compton scattering are
<~10<SUP>-4</SUP> for relevant parameter values. Of more practical
importance are number counts of clusters across which a net flux
(with respect to the CMB) higher than some limiting value can be
detected. Such number counts are specifically predicted for the
COBRAS/SAMBA and BOOMERANG missions.
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Title: Evolution of clusters of galaxies.
Authors: Colafrancesco, S.; Vittorio, N.; Mazzotta, P.
1997mba..conf..395C Altcode: 1997mba..proc..395C
In this paper the authors discuss theoretical predictions for the local
abundance of galaxy clusters and their evolution. They also discuss
the constraints set by two different databases: the X-ray luminosity
function and the temperature function.
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Title: Intracluster comptonization of the CMB in CDM cosmologies.
Authors: Vittorio, N.; Colafrancesco, S.; Mazzotta, P.; Rephaeli, Y.
1997mba..conf..401V Altcode: 1997mba..proc..401V
The authors present calculations of the mean sky-averaged Comptonization
parameter describing the scattering of the CMB by hot gas in clusters
of galaxies, in an array of flat and open CDM cosmologies. The models
are globally normalized to fit cluster X-ray data, and the intracluster
gas is assumed to have evolved in a manner consistent with current
observations. The authors also discuss the rms temperature fluctuations
induced by a population of evolving clusters. Finally, they predict
the number counts of clusters across which a net flux (with respect to
the CMB) higher than some limiting value can be detected. Such number
counts are specifically predicted for the COBRAS/SAMBA mission.
---------------------------------------------------------
Title: Cosmic Microwave Background Anisotropy Induced by Gas in
Clusters of Galaxies
Authors: Colafrancesco, S.; Mazzotta, P.; Rephaeli, Y.; Vittorio, N.
1994ApJ...433..454C Altcode:
The spectral change induced by Compton scattering of the cosmic
microwave background radiation off hot electron gas in clusters of
galaxies is an important component of the anisotropy on arcminute
scales. The level and spatial characteristics of this anisotropy are
explored in detail in the context of flat cold (taking 0.8 and 1 for the
index of the density fluctuation power spectrum) and mixed dark matter
models. Properties of intracluster gas and its evolution are directly
modeled based on X-ray measurements, with an implied decrease in the gas
mass fraction with increasing redshift. Our calculations yield levels
of rms temperature anisotropy, ({DELTA}T/T)_rms_, ~a few 10^-6^ for
a wide range of angular scales and in the context of realistic models
for the intracluster gas evolution and spatial distribution. This is
the minimum level of anisotropy expected on sub-degree angular scales
if the universe underwent a phase of late reheating.
