Author name code: deming ADS astronomy entries on 2022-09-14 author:"Deming, L. Drake" ------------------------------------------------------------------------ Title: Terrestrial Planet Optical Phase Curves. I. Direct Measurements of the Earth Authors: De Cock, Roderick; Livengood, Timothy A.; Stam, Daphne M.; Lisse, Carey M.; Hewagama, Tilak; Deming, L. Drake Bibcode: 2022AJ....163....5D Altcode: NASA's EPOXI mission used the Deep Impact spacecraft to observe the disk-integrated Earth as an analog to terrestial exoplanets' appearance. The mission took five 24 hr observations in 2008-2009 at various phase angles (57.°7-86.°4) and ranges (0.11-0.34 au), of which three equatorial (E1, E4, E5) and two polar (P1, North and P2, South). The visible data taken by the HRIV instrument ranges from 0.3 to 1.0 μm, taken trough seven spectral filters that have spectral widths of about 100 nm, and which are centered about 100 nm apart, from 350 to 950 nm. The disk-integrated, 24 hr averaged signal is used in a phase angle analysis. A Lambertian-reflecting, spherical planet model is used to estimate geometric albedo for every observation and wavelength. The geometric albedos range from 0.143 (E1, 950 nm) to 0.353 (P2, 350 nm) and show wavelength dependence. The equatorial observations have similar values, while the polar observations have higher values due to the ice in view. Therefore, equatorial observations can be predicted for other phase angles, but (Earth-like) polar views (with ice) would be underestimated. Title: Characterizing Terrestrial Exoplanets Authors: Meadows, V. S.; Lustig-Yaeger, J.; Lincowski, A.; Arney, G. N.; Robinson, T. D.; Schwieterman, E. W.; Deming, L. D.; Tovar, G. Bibcode: 2017LPICo2042.4114M Altcode: We will provide an overview of the measurements, techniques, and upcoming missions required to characterize terrestrial planet environments and evolution, and search for signs of habitability and life. Title: Illusion and reality in the atmospheres of exoplanets Authors: Deming, L. Drake; Seager, Sara Bibcode: 2017JGRE..122...53D Altcode: The atmospheres of exoplanets reveal all their properties beyond mass, radius, and orbit. Based on bulk densities, we know that exoplanets larger than 1.5 Earth radii must have gaseous envelopes and, hence, atmospheres. We discuss contemporary techniques for characterization of exoplanetary atmospheres. The measurements are difficult, because—even in current favorable cases—the signals can be as small as 0.001% of the host star's flux. Consequently, some early results have been illusory and not confirmed by subsequent investigations. Prominent illusions to date include polarized scattered light, temperature inversions, and the existence of carbon planets. The field moves from the first tentative and often incorrect conclusions, converging to the reality of exoplanetary atmospheres. That reality is revealed using transits for close-in exoplanets and direct imaging for young or massive exoplanets in distant orbits. Several atomic and molecular constituents have now been robustly detected in exoplanets as small as Neptune. In our current observations, the effects of clouds and haze appear ubiquitous. Topics at the current frontier include the measurement of heavy element abundances in giant planets, detection of carbon-based molecules, measurement of atmospheric temperature profiles, definition of heat circulation efficiencies for tidally locked planets, and the push to detect and characterize the atmospheres of super-Earths. Future observatories for this quest include the James Webb Space Telescope and the new generation of extremely large telescopes on the ground. On a more distant horizon, NASA's study concepts for the Habitable Exoplanet Imaging Mission (HabEx) and the Large UV/Optical/Infrared Surveyor (LUVOIR) missions could extend the study of exoplanetary atmospheres to true twins of Earth. Title: A Uniform and Improved Analysis of Spitzer's Exoplanet Eclipse Data Authors: Deming, L. Bibcode: 2015adap.prop..122D Altcode: Thermal emission measurements of exoplanets - dominated by data from the Spitzer Space Telescope - are our only window into the temperature structure of exoplanetary atmospheres. Our current understanding of the temperatures and molecular abundances in giant exoplanets is built on the foundation of Spitzer's eclipse measurements. Exoplanet eclipses are an order of magnitude smaller than the instrument signatures in Spitzer data. Corrections for Spitzer's instrumental signatures depend on data analyses techniques that have evolved considerably since the first eclipse detections a decade ago. However, several of the key conclusions from Spitzer's eclipses have recently been questioned based on new analyses. Resolving those questions requires improved data analysis techniques. Fortunately, we have recently developed a new and powerful data analysis method that can significantly strengthen and improve the Spitzer analyses. Nearly simultaneously, powerful Bayesian temperature and abundance retrieval techniques have emerged, that can robustly define the range of temperature structure and molecular mixing ratios that are consistent with the Spitzer data. Those retrievals are especially valuable when applied to a group of planets that have been measured using uniformly consistent analysis techniques. We propose to re-analyze all of Spitzer's secondary eclipse data using a uniform and improved method. Our results will address the temperature structure and abundances in hot Jupiter to hot Neptune atmospheres, and will define and focus the future questions to be answered via spectroscopy from JWST. Title: A Statistical Characterization of the Atmospheres of Kepler's Small Planets Authors: Deming, L. Bibcode: 2014adap.prop...46D Altcode: We propose a two year program to characterize the atmospheres of super-Earths, mini-Neptunes, and Neptunes in the Kepler data, using a novel statistical method. The Kepler mission is the most productive exoplanet mission ever launched, and our program mines the Kepler data to extract the maximum amount of information concerning the atmospheres of Kepler's planets. We group the planets by similar physical characteristics, then we apply a piecewise-linear transformation to their orbital phases near transit and secondary eclipse. We thereby scale, bin and average all of the planets in each physical grouping, greatly increasing the signal to noise. We will detect reflected light (and/or thermal emission) for groups of planets at secondary eclipse, as well as refractive shoulders on their average transit curve just before ingress and just after egress. The combination of refracted and reflected light provides a powerful probe of the atmospheric scale height and cloud cover on each group of planets. We demonstrate our method on a group of small planets (sub-Saturns) observed at secondary eclipse using Kepler's short cadence data. Our two-year program will utilize both the short- and long cadence data for many more planets. We will validate our eclipse analyses by applying our method to the average secondary eclipse for a group of well-observed Kepler hot Jupiters. Our refraction analysis will use a new numerical code that we will validate by reproducing the amplitude of refraction during the transit of Venus (archival data from the TRACE mission). We also analyze control groups of planets wherein no signal is reasonably expected, to prove the reality of the signals we detect. Title: NIMBUS: the Near-infrared Multi-Band Ultraprecise Spectroimager for SOFIA Authors: McElwain, Michael W.; Mandell, Avi; Woodgate, Bruce; Spiegel, David S.; Madhusudhan, Nikku; Amatucci, Edward; Blake, Cullen; Budinoff, Jason; Burgasser, Adam; Burrows, Adam; Clampin, Mark; Conroy, Charlie; Deming, L. Drake; Dunham, Edward; Foltz, Roger; Gong, Qian; Knutson, Heather; Muench, Theodore; Murray-Clay, Ruth; Peabody, Hume; Rauscher, Bernard; Rinehart, Stephen; Villanueva, Geronimo Bibcode: 2012SPIE.8446E..7BM Altcode: 2012arXiv1208.0832M We present a new and innovative near-infrared multi-band ultraprecise spectroimager (NIMBUS) for SOFIA. This design is capable of characterizing a large sample of extrasolar planet atmospheres by measuring elemental and molecular abundances during primary transit and occultation. This wide-field spectroimager would also provide new insights into Trans-Neptunian Objects (TNO), Solar System occultations, brown dwarf atmospheres, carbon chemistry in globular clusters, chemical gradients in nearby galaxies, and galaxy photometric redshifts. NIMBUS would be the premier ultraprecise spectroimager by taking advantage of the SOFIA observatory and state of the art infrared technologies. This optical design splits the beam into eight separate spectral bandpasses, centered around key molecular bands from 1 to 4μm. Each spectral channel has a wide field of view for simultaneous observations of a reference star that can decorrelate time-variable atmospheric and optical assembly effects, allowing the instrument to achieve ultraprecise calibration for imaging and photometry for a wide variety of astrophysical sources. NIMBUS produces the same data products as a low-resolution integral field spectrograph over a large spectral bandpass, but this design obviates many of the problems that preclude high-precision measurements with traditional slit and integral field spectrographs. This instrument concept is currently not funded for development. Title: Properties of an Earth-Like Planet Orbiting a Sun-Like Star: Earth Observed by the EPOXI Mission Authors: Livengood, Timothy A.; Deming, L. Drake; A'Hearn, Michael F.; Charbonneau, David; Hewagama, Tilak; Lisse, Carey M.; McFadden, Lucy A.; Meadows, Victoria S.; Robinson, Tyler D.; Seager, Sara; Wellnitz, Dennis D. Bibcode: 2011AsBio..11..907L Altcode: No abstract at ADS Title: A NIR spectrum of a hot Jupiter from the ground: Preliminary results Authors: Mandell, Avi M.; Deming, L. Drake; Blake, Geoffrey A.; Knutson, Heather A.; Mumma, Michael J.; Villanueva, Geronimo L.; Salyk, Colette Bibcode: 2011IAUS..276..158M Altcode: High resolution NIR spectroscopy offers an excellent complement to the expanding dataset of transit and secondary eclipse observations of exo-planets with Spitzer that have provided the bulk of our understanding of the atmospheres and internal structure of these objects. High-resolution data can quantify the vertical temperature structure by isolating specific spectral lines formed at various depths. The presence of an opaque absorbing layer can also be inferred - and its pressure level determined quantitatively - via its effect on spectral line intensities.

We have analyzed data for a single secondary eclipse of the bright transiting exo-planet host star HD189733 at L-band wavelengths (3-4 μm) using the NIRSPEC instrument on Keck-II. We utilize a sophisticated first-order telluric absorption modeling technique that, combined with a calibration star, has already been proven to remove the effects of varying atmospheric transmittance and allow us to reach unprecedented S/N. We are conducting validation of the final data reduction products and developing high-resolution atmospheric models for comparison, but we have already been able to rule out emission from methane as reported by Swain et al. (2010). We present preliminary results and discuss future plans for analysis and observations. Title: Alien Earth: Glint observations of a remote planet Authors: Barry, Richard K.; Deming, L. Drake Bibcode: 2011IAUS..276..471B Altcode: We give a preliminary report on a multi-wavelength study of specular reflections from the oceans and clouds of Earth. We use space-borne observations from a distance sufficient to ensure that light rays reflected from all parts of Earth are closely parallel, as they will be when studying exoplanets. We find that the glint properties of Earth in this far-field vantage point are surprising - in the sense that some of the brightest reflections are not from conventional ocean-glints, but appear to arise from cirrus cloud crystals. The Earth observations discussed here were acquired with the High Resolution Instrument (HRI) - a 0.3 m f/35 telescope on the Deep Impact (DI) spacecraft during the Extrasolar Planet Observation and Characterization (EPOCh) investigation. Title: Views from EPOXI: Colors in Our Solar System as an Analog for Extrasolar Planets Authors: Crow, Carolyn A.; McFadden, L. A.; Robinson, T.; Meadows, V. S.; Livengood, T. A.; Hewagama, T.; Barry, R. K.; Deming, L. D.; Lisse, C. M.; Wellnitz, Dennis Bibcode: 2011ApJ...729..130C Altcode: The first visible-light studies of Earth-sized extrasolar planets will employ photometry or low-resolution spectroscopy. This work uses EPOCh medium-band filter photometry between 350 and 950 nm obtained with the Deep Impact (DI) High Resolution Instrument (HRI) of Earth, the Moon, and Mars in addition to previous full-disk observations of the other six solar system planets and Titan to analyze the limitations of using photometric colors to characterize extrasolar planets. We determined that the HRI 350, 550, and 850 nm filters are optimal for distinguishing Earth from the other planets and separating planets to first order based on their atmospheric and surface properties. Detailed conclusions that can be drawn about exoplanet atmospheres simply from a color-color plot are limited due to potentially competing physical processes in the atmosphere. The presence of a Rayleigh scattering atmosphere can be detected by an increase in the 350-550 nm brightness ratio, but the absence of Rayleigh scattering cannot be confirmed due to the existence of atmospheric and surface absorbing species in the UV. Methane and ammonia are the only species responsible for strong absorption in the 850 nm filter in our solar system. The combination of physical processes present on extrasolar planets may differ from those we see locally. Nevertheless, a generation of telescopes capable of collecting such photometric observations can serve a critical role in first-order characterization and constraining the population of Earth-like extrasolar planets. Title: Views from EPOXI: Colors in our Solar System as an Analog for Extrasolar Planets Authors: Crow, Carolyn; McFadden, L. A.; Robinson, T.; Meadows, V.; Livengood, T. A.; Hewagama, T.; Barry, R. K.; Deming, L. D.; Lisse, C. M. Bibcode: 2010DPS....42.5206C Altcode: 2010BAAS...42Q1071C The first visible light studies of Earth-sized extrasolar planets will employ photometry or low-resolution spectroscopy. We analyzed the limitations of using photometric colors to characterize extrasolar planets using EPOCh medium-band filter photometry between 350 and 950 nm obtained with the Deep Impact (DI) High Resolution Instrument (HRI) of the Earth, Moon, and Mars in addition to previous full-disk observations of the other six solar system planets and Titan. We determined the HRI 350, 550, and 850 nm filters are optimal for distinguishing Earth from the other planets and separating planets to first order based on their atmospheric and surface properties. As in this study, detailed conclusions that can be drawn about exoplanet atmospheres simply from a color-color plot are limited due to potentially competing physical processes in the atmosphere. For example, the presence of a Rayleigh scattering atmosphere can be detected by an increase between 350 to 550 nm, but the absence or Rayleigh scattering cannot be confirmed due to the existence of atmospheric and surface absorbing species in the UV. We also observed that methane and ammonia are the only species responsible for absorption in the 850 nm filter in our Solar System. The combination of physical processes present on extrasolar planets may differ from those we see locally. Nevertheless, a generation of telescopes capable of collecting such photometric observations can serve a critical role in first order characterization and constraining the population of Earth-like extrasolar planets. Title: Detection of the Secondary Eclipse of Exoplanet HAT-P-11b Authors: Barry, R. K.; Bakos, G.; Harrington, J.; Madhusudhan, N.; Noyes, R.; Seager, S.; Deming, L. D. Bibcode: 2010epsc.conf..342B Altcode: No abstract at ADS Title: Development and utilization of a point spread function for the Extrasolar Planet Observation and Characterization/Deep Impact Extended Investigation (EPOXI) Mission Authors: Barry, R. K.; Lindler, D.; Deming, L. D.; A'Hearn, M. F.; Ballard, S.; Carcich, B.; Charbonneau, D.; Christiansen, J.; Hewagama, T.; McFadden, L.; Wellnitz, D. Bibcode: 2010SPIE.7731E..3DB Altcode: 2010SPIE.7731E.107B The Extrasolar Planet Observation Characterization and the Deep Impact Extended Investigation missions (EPOXI) are currently observing the transits of exoplanets, a comet nucleus at short range, and Earth using the High Resolution Instrument (HRI) - a 0.3 m f/35 telescope - on the Deep Impact flyby spacecraft. The HRI is in a permanently defocused state with the instrument point of focus about 0.6 cm before the focal plane due to the use of a reference flat mirror that became a powered optic due to thermal warping during ground thermal-vacuum testing. Consequently, the point spread function (PSF) covers approximately nine pixels FWHM and is characterized by a patch with three-fold symmetry due to the three-point support structures of the primary and secondary mirrors. The PSF is also strongly color dependent varying in shape and size with change in filtration and target color. While defocus is highly desirable for exoplanet transit observations to limit sensitivity to intra-pixel variation, it is suboptimal for observations of spatially resolved targets. Consequently, all images used in our analysis of such objects were deconvolved with an instrument PSF. The instrument PSF is also being used to optimize transit analysis. We discuss development and usage of an instrument PSF for these observations. Title: Earth as an Extrasolar Planet: Comparing Polar and Equatorial Views Authors: Shields, A. L.; Meadows, V. S.; Robinson, T. D.; Deming, L. D.; A'Hearn, M. F.; Charbonneau, D.; Hewagama, T.; Lisse, C.; Livengood, T.; McFadden, L.; Seager, S.; Welnitz, D. D.; Epoxi Earthling Team Bibcode: 2010LPICo1538.5408S Altcode: We present data-model comparisons for EPOXI observations of the distant Earth's equator and poles modelled with the NAI's VPL 3D Earth Model. These are being used to determine the detectability of habitability for different planetary inclinations. Title: A Time-Dependent Radiative Model for the Atmosphere of the Eccentric Exoplanets Authors: Iro, N.; Deming, L. D. Bibcode: 2010ApJ...712..218I Altcode: We present a time-dependent radiative model for the atmosphere of extrasolar planets that takes into account the eccentricity of their orbit. In addition to the modulation of stellar irradiation by the varying planet-star distance, the pseudo-synchronous rotation of the planets may play a significant role. We include both of these time-dependent effects when modeling the planetary thermal structure. We investigate the thermal structure and spectral characteristics for time-dependent stellar heating for two highly eccentric planets. Finally, we discuss observational aspects for those planets suitable for Spitzer measurements and investigate the role of the rotation rate. Title: Transiting Exoplanet Survey Satellite (TESS) Authors: Ricker, George R.; Latham, D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.; Villasenor, J. N.; Winn, J. N.; Worden, S. P. Bibcode: 2010AAS...21545006R Altcode: 2010BAAS...42..459R TESS is a low-cost SMEX-class satellite mission. In a two-year all-sky survey, TESS will observe more than 2,000,000 nearby stars, searching for temporary drops in brightness caused by planetary transits.

TESS is expected to identify more than 1000 transiting exoplanet candidates, including a sample of about 100 Super Earths---small rock-and-ice planets in the range 1 to 10 Earth masses---orbiting F, G, K, and M dwarfs. TESS's "wide-shallow” survey complements the "narrow-deep” CoRoT and Kepler surveys. TESS-discovered transiting systems will be nearby (< 50 pc), and typically 10-20 x brighter than those discovered by CoRoT and Kepler. Thus, the resulting TESS Transit Catalog will comprise all of the best transiting systems for follow-up observations. TESS will identify Super Earths orbiting IR-bright stars, within reach of JWST spectroscopic searches for planetary water and carbon dioxide.

TESS is a collaborative effort led by researchers at the Massachusetts Institute of Technology, the Harvard-Smithsonian Center for Astrophysics, and the NASA Ames Research Center. Additional TESS scientific partners include Las Cumbres Observatory Global Telescope, Lowell Observatory, the NASA Goddard Space Flight Center, the Infrared Processing and Analysis Center at the California Institute of Technology, the Geneva Observatory (Switzerland), the Tokyo Institute of Technology (Japan), and Institut Supérieur de l'Aéronautique et de l'Espace (France).

TESS was funded by NASA for a Phase A study from May 2008 - June 2009, but was not selected for flight. Additional funding leading to a flight opportunity is being sought. Support has also been provided by the Kavli Foundation, Google, and the Smithsonian Institution. TESS could launch as early as 2013-2014. Title: Estimates of the Population of Exoplanets Discoverable by the Transiting Exoplanet Survey Satellite (TESS) Authors: Seager, Sara; Winn, J. N.; Ricker, G. R.; Latham, D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Schingler, R. H.; Torres, G.; Udry, S.; Villasenor, J. N.; Worden, S. P. Bibcode: 2010AAS...21545004S Altcode: 2010BAAS...42R.458S In a two year survey, the Transiting Exoplanet Survey Satellite (TESS) will search the entire sky for planets orbiting nearby, bright stars. In this paper, we calculate the number of transiting planets that TESS will detect, as a function of the properties of the planet and the properties of the host star. The ingredients in this calculation are divided into five groups:

The properties of the planet: its radius r and orbital distance a.

The properties of the star: its luminosity L, mass M, radius R, and number density n in our Galactic neighborhood.

The TESS instrumental parameters: its effective area, bandpass, and limiting photometric precision.

The TESS survey parameters: the characteristics of the input catalog (2.5 million V < 13.5 dwarfs over the whole sky), observing duty cycle (observing a given star 10.3% of the time), and duration of observations for a given star (72 days).

The abundance of planets around stars, which may depend on r, a, and L

The calculation is performed for a three-dimensional grid of planet/star/orbit combinations, in which the three parameters are the planet radius r, the stellar luminosity L, and the orbital distance a. For the range of instrument and population parameters and assumptions considered, we estimate that TESS will detect 1600-2700 planets in total, of which 100-300 should be small planets: SuperEarths or Earths.

Support for this work has been provided by NASA, the Kavli Foundation, Google, and the Smithsonian Institution. Title: Monte Carlo Simulations of Transit Light Curves for the Transiting Exoplanet Survey Satellite (TESS) Authors: Jernigan, J. G.; Villasenor, J. N.; Ricker, G. R.; Latham, D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.; Winn, J. N.; Worden, S. P. Bibcode: 2010AAS...21545003J Altcode: 2010BAAS...42..458J During the Phase A for TESS, simulations of planetary transits were performed to confirm the instrument's ability to detect transits. The simulations cover the full TESS discovery space in the planet period-transit duration plane. Examples included a 36-day period planet, two previously known systems (HAT-P-11 and CoRoT 7B), and one Earth and one SuperEarth. In addition, a broad matrix of planetary periods and transit depths were also simulated. We present simulated light curves of transiting planets that are typical of those that TESS will detect. Each light curve is computed via a Monte Carlo algorithm. The timing of the optical emission includes the parameters of orbital motion for the planet-star system. All simulations include estimates of the noise from the following effects: spacecraft pointing jitter, vignetting, optical PSF wings, background effects, CCD gain and bias instability, sky background, and intrinsic stellar variability. The stellar variability includes a scaled, full temporal power spectrum of the Sun. Typical light curves of planet-star systems are simulated for a 72 day duration with a 10 minute time resolution of each TESS sample. These simulated light curves are analyzed to determine estimates of the S/N for detection for each simulated system. Support for this work has been provided by NASA, the Kavli Foundation, Google, and the Smithsonian Institution. Title: High-Precision Imaging Photometers for the Transient Exoplanet Survey Satellite Authors: Kraft Vanderspek, Roland; Ricker, G. R.; Latham, D. W.; Ennico, K.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Schingler, R. H.; Seager, S.; Szentgyorgyi, A.; Torres, G.; Udry, S.; Villasenor, J. N.; Winn, J. N.; Worden, S. P. Bibcode: 2010AAS...21545007K Altcode: 2010BAAS...42..459K The Transient Exoplanet Survey Satellite (TESS) is designed to search for transiting exoplanet systems around all stars with V < 12. The TESS payload consists of a bank of six identical, wide-field, high-precision imaging photometers. When deployed on the highly-stable TESS satellite platform, these photometers can perform <200 ppm photometry for V=8 stars (∼100 ppm for V=6 stars) in a 10-minute observation. We describe the components of the TESS imaging photometers: the custom, wide-field optics; the large-area CCD arrays; and the low-power, high precision CCD electronics. Support for TESS has been provided by NASA, the Kavli Foundation, Google, and the Smithsonian Institution. Title: Data Network for the TESS Mission Authors: Martel, Francois; Villasenor, J. N.; Ricker, G. R.; Latham, D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Sasselov, D. D.; Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.; Winn, J. N.; Worden, S. P. Bibcode: 2010AAS...21545002M Altcode: 2010BAAS...42..458M The Transiting Exoplanet Survey Satellite (TESS) is designed for an all-sky photometric survey of bright stars, extending&nbspover the entire celestial sphere.&nbspTESS will catalog planetary transits of nearby stars that can be followed-up with ground observatories. The satellite cameras will perform measurements of 2,500,000 stars with brightness ranging from V=4.5 to V=13.5 within two years, and download typically 4.7 G Bytes of data per day.&nbspWe describe the TESS operation plan and the communication and ground system designed to download and process the TESS data. The dedicated ground system uses a network of S-band ground stations spaced around the equator which allows three communications passes per orbit, at data rates of 3.5 Mbit/sec, for up to 45 data downloads per day. Satellite operations and data download are controlled remotely through the internet by the TESS Mission Operation Center at NASA Ames Research Center, which transfers the TESS observation data for processing and distribution to the Science Operation Center managed by &nbspMIT and Harvard-SAO in Cambridge. Support for this work has been provided by NASA, the Kavli Foundation, Google, and the Smithsonian Institution. Title: Transiting Exoplanet Survey Satellite (TESS) Community Observer Program including the Science Enhancement Option Box (SEO Box) - 12 TB On-board Flash Memory for Serendipitous Science Authors: Schingler, Robert; Villasenor, J. N.; Ricker, G. R.; Latham, D. W.; Vanderspek, R. K.; Ennico, K. A.; Lewis, B. S.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Seager, S.; Torres, G.; Udry, S.; Winn, J. N.; Worden, S. P. Bibcode: 2010AAS...21545001S Altcode: 2010BAAS...42Q.458S The Transiting Exoplanet Survey Satellite (TESS) will perform an all-sky survey in a low-inclination, low-Earth orbit. TESS's 144 GB of raw data collected each orbit will be stacked, cleaned, cut, compressed and downloaded. The Community Observer Program is a Science Enhancement Option (SEO) that takes advantage of the low-radiation environment, technology advances in flash memory, and the vast amount of astronomical data collected by TESS. The Community Observer Program requires the addition of a 12 TB "SEO Box” inside the TESS Bus. The hardware can be built using low-cost Commercial Off-The-Shelf (COTS) components and fits within TESS's margins while accommodating GSFC gold rules.

The SEO Box collects and stores a duplicate of the TESS camera data at a "raw” stage ( 4.3 GB/orbit, after stacking and cleaning) and makes them available for on-board processing. The sheer amount of onboard storage provided by the SEO Box allows the stacking and storing of several months of data, allowing the investigator to probe deeper in time prior to a given event. Additionally, with computation power and data in standard formats, investigators can utilize data-mining techniques to investigate serendipitous phenomenon, including pulsating stars, eclipsing binaries, supernovae or other transient phenomena.

The Community Observer Program enables ad-hoc teams of citizen scientists to propose, test, refine and rank algorithms for on-board analysis to support serendipitous science. Combining "best practices” of online collaboration, with careful moderation and community management, enables this `crowd sourced’ participatory exploration with a minimal risk and impact on the core TESS Team. This system provides a powerful and independent tool opening a wide range of opportunity for science enhancement and secondary science.

Support for this work has been provided by NASA, the Kavli Foundation, Google, and the Smithsonian Institution. Title: Our Solar System at Low Spectral Resolution: A Starting Point for Characterizing Colors of Other Systems Authors: Crow, Carolyn A.; McFadden, L. A.; Livengood, T. A.; Hewagama, T.; Barry, R.; Deming, L. D. Bibcode: 2009DPS....41.0808C Altcode: One of the next frontiers in extrasolar planet exploration is color characterization. We have analyzed images of the Earth and Moon acquired during the EPOXI mission with the High Resolution Instrument (HRI) and seven color filters, and compiled disk-integrated spectra for a range of Solar System planets from previous studies. These data form a basis for characterizing exoplanetary systems in the future. The images used for this study were taken on January 16, 2005 and May 29, 2008 by the Deep Impact spacecraft's HRI at distances of 1.64x106 km and 0.33 AU, phase angles of 97.6° and 75.1°, resolutions of 3.3 and 99.0 km/pix, respectively. We derived disk-integrated spectra of the Earth and far side of the Moon in addition to regionally integrated spectra of the Sahara Desert, African savanna, northern and southern hemispheres of the lunar far side, and various regions of the lunar near side. Ground based low-resolution spectra of lunar near side regions from McCord et al. 1972 were compared with our data for verification. We also convolved disk-integrated spectra of Jupiter, Saturn, Uranus, Neptune, and Titan (Karkoschka 1994, 1998) with the HRI filter transmission curves to compare the low-resolution spectral features of gaseous planets with those of terrestrial bodies. The resulting spectra of the Moon and Earth are similar to what is expected for rocky bodies with and without an atmosphere, and the spectra of the Sahara and savanna are also what is expected of dry desert and vegetated regions. We observe that the low-resolution spectral signatures of the Giant Planets, the Moon and Earth are unique. A solar system like our own would have these characteristic spectral features at low resolution and visible wavelengths. Title: Transiting Exoplanet Survey Satellite (TESS) Authors: Ricker, George R.; Latham, D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.; Villasenor, J. S.; Winn, J. N.; Worden, S. P. Bibcode: 2009AAS...21430605R Altcode: The Transiting Exoplanet Survey Satellite (TESS) is a low cost, SMEX-class planet finder. In a two year all-sky survey, TESS will observe more than two million bright, nearby stars, searching for temporary drops in brightness that are caused by planetary transits. Such transits not only provide the means of identifying the planet, but also provide knowledge of the planet's diameter, mass density, surface gravity, temperature, and other key properties. TESS is expected to detect more than 1000 transiting exoplanet candidates. These detections will include a sample of 100 Super Earths -- small rock-and-ice planets with masses in the range 1 to 10 Earth masses -- orbiting nearby stars with spectral types spanning a broad range, including F, G, K, and M dwarfs. No ground-based survey can achieve this feat. TESS's "wide-shallow" survey complements the "narrow-deep" Corot and Kepler mission surveys. The resulting TESS Transit Catalog of the nearest and brightest stars in the sky will constitute a unique scientific legacy for followup observations. TESS will identify Super Earths orbiting IR-bright stars, ideal for JWST searches for planetary water and carbon dioxide.

The TESS mission is a collaborative effort led by researchers at the Massachusetts Institute of Technology, the Harvard-Smithsonian Center for Astrophysics, and the NASA Ames Research Center. Additional TESS partners include ATK Space Systems, the Las Cumbres Observatory Global Telescope Network, Lowell Observatory, the NASA Goddard Space Flight Center, the Infrared Processing and Analysis Center at the California Institute of Technology, the University of California (Berkeley and Santa Cruz), the SETI Institute, Espace Incorporated, the Geneva Observatory (Switzerland), the Tokyo Institute of Technology (Japan), and Institut Supérieur de l'Aéronautique et de l'Espace (France).

TESS is currently completing a NASA-funded Phase A study, and is proposed for launch in December 2012. Title: Exoplanet HAT-P-11b Secondary Transit Observations Authors: Barry, Richard; Deming, Drake; Bakos, Gaspar; Deming, L. Drake; Harrington, Joseph; Madhusudhan, Nikku; Noyes, Robert; Seager, Sarah Bibcode: 2009sptz.prop60063B Altcode: We propose to conduct secondary eclipse observations of exoplanet HAT-P-11b, recently discovered by proposal Co-Investigator G. Bakos and his colleagues. HAT-P-11b is the smallest transiting extrasolar planet yet found and one of only two known exo-Neptunes. We will observe the system at 3.6 microns for a period of 22 hours centered on the anticipated secondary eclipse time, to detect the eclipse and determine its phase. Once the secondary eclipse is located, we will make a more focused series of observations in both the 3.6 and 4.5 micron bands to fully characterize it. HAT-P-11b has a period of 4.8878 days, radius of 0.422 RJ, mass of 0.081 MJ and semi-major axis 0.053 AU. Measurements of the secondary eclipse will clarify two key issues; 1) the planetary brightness temperature and the nature of its atmosphere, and 2) the eccentricity of its orbit, with implications for its dynamical evolution. A precise determination of the orbit phase for the secondary eclipse will also be of great utility for Kepler observations of this system at visible wavelengths. Title: The Transiting Exoplanet Survey Satellite (TESS) Authors: Ricker, George R.; Latham, D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.; Villasenor, J. S.; Winn, J. N.; Worden, S. P. Bibcode: 2009AAS...21340301R Altcode: 2009BAAS...41..193R The Transiting Exoplanet Survey Satellite (TESS) is a low cost, SMEX-class planet finder. In a two year all-sky survey, TESS will observe more than two million bright, nearby stars, searching for temporary drops in brightness that are caused by planetary transits, which occur when a planet's orbit carries it directly in front of its parent star. Such transits not only provide the means of identifying the planet, but also provide knowledge of the planet's diameter, mass density, surface gravity, temperature, and other key properties.

TESS is expected to catalog more than 1000 transiting exoplanet candidates--20 times as many as are presently known, including a sample of 'super Earths'. The TESS "wide-shallow" survey will be complementary to the "narrow-deep" ones of the Corot and Kepler missions: its sky coverage will exceed that of Corot by 1000 times, and that of Kepler by 400 times. Because the TESS all-sky survey will systematically examine every interesting bright star likely to harbor an exoplanet, the resulting TESS Transit Catalog will constitute a unique scientific legacy. High resolution, follow-up ground-based optical and space-based IR spectroscopy of exoplanets demands bright targets. Thus, TESS should identify those new exoplanets that are ideal for study with the world's largest ground-based telescopes, as well as with NASA's upcoming James Webb Space Telescope.

The TESS mission is a collaborative effort led by researchers at MIT, the Harvard-Smithsonian Center for Astrophysics, and the NASA Ames Research Center. Additional TESS partners include the NASA Goddard Space Flight Center, the Harvard Origins of Life Initiative, Lowell Observatory, Caltech's IPAC, the SETI Institute, Geneva Observatory in Switzerland, Tokyo Institute of Technology, SUPAERO in France, ATK Space, Espace Inc, and the Las Cumbres Observatory Global Telescope Network. TESS has been accepted for Phase A study by NASA, and is proposed for launch in late 2012. Title: The Fourier Kelvin Stellar Interferometer (FKSI): A Probe-class Infrared Space Mission for the Spectroscopic Characterization of Exoplanets, Exozodi Levels, Debris Disks, and High Angular Resolution Astrophysics Authors: Barry, Richard K.; Danchi, W. C.; Deming, L. D.; Lawsen, P.; Traub, W.; Unwin, S. Bibcode: 2009AAS...21333601B Altcode: 2009BAAS...41..397B The Fourier-Kelvin Stellar Interferometer (FKSI) mission is a two-telescope infrared space interferometer with a 12.5 meter baseline on a boom, operating in the spectral range 3 to 8 (or 10) microns, and passively cooled to about 60 K. The main goals for the mission are the measurement and characterization of the exozodiacal emission around nearby stars, debris disks, and the atmospheres of known exoplanets, and the search for Super Earths around nearby stars. We discuss progress on this mission in the context of the upcoming Decadal Survey, in particular how FKSI is ideally suited to be an Exoplanet Probe mission in terms of crucial observations which should be done before a flagship mission can be undertaken, as well as technical readiness, cost, and risk. Title: Chromospheric Lines as Diagnostics of Stellar Oscillations Authors: Paulson, Diane B.; Pesnell, W. Dean; Deming, L. Drake; Snow, Martin; Metcalfe, Travis S.; Woods, Tom; Hesman, Brigette Bibcode: 2008psa..conf..311P Altcode: Gravitational waves in the chromosphere, theorized as early as 1963 [10], are thoroughly explored in the more recent papers by [7, 8]. Theory predicts that the convective overshoot in the upper photosphere and low chromosphere will readily excite gravity waves. [9] note that these waves are not easily detected because of the long periods, short wavelengths required and slanted propagation angles of the waves themselves (causing small velocity shifts and short duration on individual detector pixels). Recently, [9] find evidence for gravity waves manifested in the f 700Å chromospheric line with frequencies <1 mHz. Title: Solar Magnetograms at 12 μm Using the Celeste Spectrograph Authors: Moran, Thomas G.; Jennings, Donald E.; Deming, L. Drake; McCabe, George H.; Sada, Pedro V.; Boyle, Robert J. Bibcode: 2007SoPh..241..213M Altcode: We present the first solar vector magnetogram constructed from measurements of infra-red Mg I 12.32-μm line spectra. Observations were made at the McMath-Pierce Telescope using the Celeste spectrometer/polarimeter. Zeeman-split Stokes line spectra were fitted with Seares profiles to obtain the magnetic field parameters. Maps of absolute field strength, line-of-sight angle, and azimuth are presented. Analysis shows that the variation in field strength within a spatial resolution element, 2 arcseconds, is greatest in the sunspot penumbra and that this is most likely caused by vertical field strength gradients, rather than horizontal image smearing. Widths of the Zeeman-split σ components, assuming a formation layer thickness of 200 km, indicate that vertical field strength gradients can be as large as 6.5 G/km in a penumbra. Title: The Fourier-Kelvin Stellar Interferometer: a low-complexity low-cost space mission for high-resolution astronomy and direct exoplanet detection Authors: Barry, R. K.; Danchi, W. C.; Deming, L. D.; Richardson, L. J.; Kuchner, M. J.; Seager, S.; Frey, B. J.; Martino, A. J.; Lee, K. A.; Zuray, M.; Rajagopal, J.; Hyde, T. T.; Millan-Gabete, R.; Monnier, J. D.; Allen, R. J.; Traub, W. A. Bibcode: 2006SPIE.6265E..1LB Altcode: 2006SPIE.6265E..46B The Fourier-Kelvin Stellar Interferometer (FKSI) is a mission concept for a spacecraft-borne nulling interferometer for high-resolution astronomy and the direct detection of exoplanets and assay of their environments and atmospheres. FKSI is a high angular resolution system operating in the near to mid-infrared spectral region and is a scientific and technological pathfinder to the Darwin and Terrestrial Planet Finder (TPF) missions. The instrument is configured with an optical system consisting, depending on configuration, of two 0.5 - 1.0 m telescopes on a 12.5 - 20 m boom feeding a symmetric, dual Mach- Zehnder beam combiner. We report on progress on our nulling testbed including the design of an optical pathlength null-tracking control system and development of a testing regime for hollow-core fiber waveguides proposed for use in wavefront cleanup. We also report results of integrated simulation studies of the planet detection performance of FKSI and results from an in-depth control system and residual optical pathlength jitter analysis. Title: The Fourier-Kelvin Stellar Interferometer: an achievable, space-borne interferometer for the direct detection and study of extrasolar giant planets Authors: Barry, R. K.; Danchi, W. C.; Deming, L. D.; Richardson, L. J.; Kuchner, M. J.; Chambers, V. J.; Frey, B. J.; Martino, A. J.; Rajagopal, J.; Allen, R. J.; Harrington, J. A.; Hyde, T. T.; Johnson, V. S.; Linfield, R.; Millan-Gabet, R.; Monnier, J. D.; Mundy, L. G.; Noecker, C.; Seager, S.; Traub, W. A. Bibcode: 2006dies.conf..221B Altcode: 2006IAUCo.200..221B The Fourier-Kelvin Stellar Interferometer (FKSI) is a mission concept for a spacecraft-borne imaging and nulling interferometer for the near to mid-infrared spectral region. FKSI is a scientific and technological pathfinder to the Darwin and Terrestrial Planet Finder (TPF) missions and will be a high angular resolution system complementary to the James Webb Space Telescope (JWST). There are four key scientific issues the FKSI mission is designed to address. These are: 1.) characterization of the atmospheres of the known extra-solar giant planets, 2.) assay of the morphology of debris disks to look for resonant structures characteristic of the presence of extrasolar planets, 3.) study of circumstellar material around a variety of stellar types to better understand their evolutionary state, and in the case of young stellar systems, their planet forming potential, and 4.) measurement of detailed structures inside active galactic nuclei. We report results of simulation studies of the imaging capabilities of the FKSI, current progress on our nulling testbed, results from control system and residual jitter analysis, and selection of hollow waveguide fibers for wavefront cleanup. Title: HD209458b Transit Spectroscopy Authors: Harrington, J.; Deming, L. D.; Matthews, K.; Richardson, L. J.; Rojo, P.; Steyert, D.; Wiedemann, G.; Zeehandelaar, D. Bibcode: 2002DPS....34.3005H Altcode: 2002BAAS...34Q.893H We search for the spectral signature of H2O, CH4, and CO on the extrasolar planet HD 209458b using transit spectroscopy. The planet will modulate the stellar spectrum during transit. The extinction altitude of tangent rays of a given wavelength depends on the abundance and distribution of molecular species that absorb at that wavelength. The depth of the occultation at a given wavelength depends on the cross-sectional area of the planet, which is determined by the extinction altitude. For deep lines of H2O, CH4, and CO, the effect is about 0.07%, due to the ~750 km scale height. Our S/N calculations show that well-calibrated, ground-based spectra, integrated over time and wavelength, can measure or place useful limits on the atmospheric abundances of H2O, CH4, and CO. Carbon forms predominantly CH4 below 1400 K and CO if hotter. Since the effective temperature is around 1400 K, detecting CH4 and/or CO would provide a tight constraint on atmospheric temperatures. Observations began in August 2001 at Palomar and we have 12 additional nights granted in 2002 at Keck, VLT, and IRTF. The expected modulation of the stellar spectrum is model-dependent: high-altitude hazes, photochemical effects, and different thermal profiles would substantially modify the effect for the same planetary elemental abundances. Since the effect is subtle compared to the noise in the data, we correlate model spectra against thousands of observed spectra and average the correlations to test whether the data support a given model. We are developing a radiative-transfer model to predict the spectrum of a given planetary model, and we are measuring H2O, CH4, and CO in the laboratory at 1300 K, with pressure-broadening by H2, to make our model spectra realistic at these elevated temperatures (crucial for detecting H2O). Analysis of the 2001 data and acquisition of 2002 data are in progress. We solicit participation by those who wish to test their planetary models. Title: Simple Models of SL-9 Impact Plumes Authors: Harrington, J.; Deming, L. D. Bibcode: 1996DPS....28.2249H Altcode: 1996BAAS...28.1150H The impacts of the larger fragments of Comet Shomaker-Levy 9 on Jupiter left debris patterns of consistent appearance, likely caused by the landing of the observed impact plumes. Realistic fluid simulations of impact plume evolution may take months to years for even single computer runs. To provide guidance for these models and to elucidate the most basic aspects of the plumes, debris patterns, and their ultimate effect on the atmosphere, we have developed simple models that reproduce many of the key features. These Monte-Carlo models divide the plume into discrete mass elements, assign to them a velocity distribution based on numerical impact models, and follow their ballistic trajectories until they hit the planet. If particles go no higher than the observed ~ 3,000 km plume heights, they cannot reach the observed crescent pattern located ~ 10,000 km from the impact sites unless they slide horizontally after ballistic flight. By introducing parameterized sliding or higher trajectories, we can reproduce most of the observed impact features, including the central streak, the crescent, and the ephemeral ring located ~ 30,000 km from the impact sites. We also keep track of the amounts of energy and momentum delivered to the atmosphere as a function of time and location, for use in atmospheric models (D. Deming and J. Harrington, this meeting). Title: The Bounce of SL-9 Impact Ejecta Plumes on Re-Entry Authors: Deming, L. D.; Harrington, J. Bibcode: 1996DPS....28.2250D Altcode: 1996BAAS...28.1151D We have generated synthetic light curves of the re-entry of SL-9 ejecta plumes into Jupiter's atmosphere and have modeled the periodic oscillation of the observed R plume light curves (P. D. Nicholson et al. 1995, Geophys. Res. Lett. 22, 1613--1616) as a hydrodynamic bounce. Our model is separated into plume and atmospheric components. The plume portion of the model is a ballistic Monte Carlo calculation (Harrington and Deming, this meeting). In this paper we describe the atmospheric portion of the model. The infalling plume is divided over a spatial grid (in latitude/longitude). The plume is layered, and joined to a 1-D Lagrangian radiative-hydrodynamic model of the atmosphere, at each grid point. The radiative-hydrodynamic code solves the momentum, energy, and radiative transfer equations for both the infalling plume layers and the underlying atmosphere using an explicit finite difference scheme. It currently uses gray opacities for both the plume and the atmosphere, and the calculations indicate that a much greater opacity is needed for the plume than for the atmosphere. We compute the emergent infrared intensity at each grid point, and integrate spatially to yield a synthetic light curve. These curves exhibit many features in common with observed light curves, including a rapid rise to maximum light followed by a gradual decline due to radiative damping. Oscillatory behavior (the ``bounce'') is a persistent feature of the light curves, and is caused by the elastic nature of the plume impact. In addition to synthetic light curves, the model also calculates temperature profiles for the jovian atmosphere as heated by the plume infall. Title: Location of Hydrocarbon Emission Near Jupiter's South Pole Authors: Livengood, T. A.; Buhl, D.; Deming, L. D.; Espenak, F.; Kostiuk, T.; Reuter, D.; Fast, K. E. Bibcode: 1993DPS....25.0902L Altcode: 1993BAAS...25.1051L No abstract at ADS Title: Photometric observations of visual binaries and inferences concerning mixing in red giants Authors: Deming, Leo Drake Bibcode: 1976PhDT.......168D Altcode: No abstract at ADS Title: Photometric Observations of Visual Binaries and Inferences Concerning Mixing in Red Giants. Authors: Deming, L. D. Bibcode: 1976PhDT.........2D Altcode: The DDO and uvby beta methods photometry were used to study a sample of visual binaries. Inferences were made concerning the amount and kind of mixing which occurs in population I red giants before and during the stage of core helium burning. The binaries consist of G and K giants in association with main sequence stars of nearly solar type. The DDO photometry of the giant components of the binaries yields absolute magnitudes which are in generally good accord with the absolute magnitudes derived for the secondary components from uvby beta photometry. The spectral types indicated by DDO photometry are in generally good agreement with spectral types given by visual classification. However there exists a small group of stars for which DDO photometry gives widely discrepant spectral types and absolute magnitudes. These stars can often be noticed to have peculiar spectra at the time of visual classification; they may be spectroscopic binaries but this is not certain. Title: a Comparison of Spectrographic and DDO Photoelectric Luminosities and Composition Indices Authors: Yoss, Kenneth M.; Deming, L. Drake Bibcode: 1975mpth.conf..359Y Altcode: 1975mpth.proc..359Y No abstract at ADS