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  • 11
    Publication Date: 1991-10-04
    Description: Insects and other invertebrates use glutamate as a neurotransmitter in the central nervous system and at the neuromuscular junction. A complementary DNA from Drosophila melanogaster, designated DGluR-II, has been isolated that encodes a distant homolog of the cloned mammalian ionotropic glutamate receptor family and is expressed in somatic muscle tissue of Drosophila embryos. Electrophysiological recordings made in Xenopus oocytes that express DGluR-II revealed depolarizing responses to L-glutamate and L-aspartate but low sensitivity to quisqualate, alpha-amino-3-hydroxy-5-methyl-4-isoxazolepropionate (AMPA), and kainate. The DGluR-II protein may represent a distinct glutamate receptor subtype, which shares its structural design with other members of the ionotropic glutamate receptor family.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Schuster, C M -- Ultsch, A -- Schloss, P -- Cox, J A -- Schmitt, B -- Betz, H -- New York, N.Y. -- Science. 1991 Oct 4;254(5028):112-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Zentrum fur Molekulare Biologie, Universitat Heidelberg, Federal Republic of Germany.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/1681587" target="_blank"〉PubMed〈/a〉
    Keywords: Amino Acid Sequence ; Animals ; Base Sequence ; Cloning, Molecular ; DNA/genetics ; Drosophila melanogaster/*genetics/physiology ; Gene Expression ; Glutamates/pharmacology ; Glutamic Acid ; Molecular Sequence Data ; Muscles/*physiology ; Oligonucleotides/chemistry ; Receptors, Glutamate ; Receptors, Neurotransmitter/*genetics/physiology ; Sequence Alignment
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  • 12
    Publication Date: 2005-02-19
    Description: The Observatoire pour la Mineralogie, l'Eau, les Glaces, et l'Activite (OMEGA) visible-infrared imaging spectrometer extensively observed regions of Mars with latitudes above 70 degrees N in late 2004 (heliocentric longitude from Ls 93 degrees to Ls 127 degrees ). The extent of water ice at the surface and the size of ice grains were monitored as a function of time. Bright, small-grained frost, which initially covered a large fraction of the polar cap, waned in favor of large-grained ice. In outlying regions, dominated by large-grained ice, the albedo increased over the period. Evaluating the dust content was model dependent. However, contamination of ice by dust was low.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Langevin, Y -- Poulet, F -- Bibring, J-P -- Schmitt, B -- Doute, S -- Gondet, B -- New York, N.Y. -- Science. 2005 Mar 11;307(5715):1581-4. Epub 2005 Feb 17.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institut d'Astrophysique Spatiale, CNRS-Universite Paris Sud, 91405 Orsay, France. yves.langevin@ias.u-psud.fr〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15718426" target="_blank"〉PubMed〈/a〉
    Keywords: Carbon Dioxide ; Extraterrestrial Environment ; *Ice ; *Mars ; Seasons ; Spacecraft ; Spectroscopy, Near-Infrared ; Spectrum Analysis ; Water
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  • 13
    Publication Date: 2004-04-10
    Description: Plastic deformation in coarse-grained metals is governed by dislocation-mediated processes. These processes lead to the accumulation of a residual dislocation network, producing inhomogeneous strain and an irreversible broadening of the Bragg peaks in x-ray diffraction. We show that during plastic deformation of electrodeposited nanocrystalline nickel, the peak broadening is reversible upon unloading; hence, the deformation process does not build up a residual dislocation network. The results were obtained during in situ peak profile analysis using the Swiss Light Source. This in situ technique, based on well-known peak profile analysis methods, can be used to address the relationship between microstructure and mechanical properties in nanostructured materials.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Budrovic, Zeljka -- Van Swygenhoven, Helena -- Derlet, Peter M -- Van Petegem, Steven -- Schmitt, Bernd -- New York, N.Y. -- Science. 2004 Apr 9;304(5668):273-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Paul Scherrer Institute, CH-5232 Villigen PSI, Switzerland.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/15073373" target="_blank"〉PubMed〈/a〉
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  • 14
    Publication Date: 2006-04-22
    Description: Global mineralogical mapping of Mars by the Observatoire pour la Mineralogie, l'Eau, les Glaces et l'Activite (OMEGA) instrument on the European Space Agency's Mars Express spacecraft provides new information on Mars' geological and climatic history. Phyllosilicates formed by aqueous alteration very early in the planet's history (the "phyllocian" era) are found in the oldest terrains; sulfates were formed in a second era (the "theiikian" era) in an acidic environment. Beginning about 3.5 billion years ago, the last era (the "siderikian") is dominated by the formation of anhydrous ferric oxides in a slow superficial weathering, without liquid water playing a major role across the planet.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Bibring, Jean-Pierre -- Langevin, Yves -- Mustard, John F -- Poulet, Francois -- Arvidson, Raymond -- Gendrin, Aline -- Gondet, Brigitte -- Mangold, Nicolas -- Pinet, P -- Forget, F -- Berthe, Michel -- Gomez, Cecile -- Jouglet, Denis -- Soufflot, Alain -- Vincendon, Mathieu -- Combes, Michel -- Drossart, Pierre -- Encrenaz, Therese -- Fouchet, Thierry -- Merchiorri, Riccardo -- Belluci, Giancarlo -- Altieri, Francesca -- Formisano, Vittorio -- Capaccioni, Fabricio -- Cerroni, Pricilla -- Coradini, Angioletta -- Fonti, Sergio -- Korablev, Oleg -- Kottsov, Volodia -- Ignatiev, Nikolai -- Moroz, Vassili -- Titov, Dimitri -- Zasova, Ludmilla -- Loiseau, Damien -- Pinet, Patrick -- Doute, Sylvain -- Schmitt, Bernard -- Sotin, Christophe -- Hauber, Ernst -- Hoffmann, Harald -- Jaumann, Ralf -- Keller, Uwe -- Arvidson, Ray -- Duxbury, Tom -- Forget, Francois -- Neukum, G -- New York, N.Y. -- Science. 2006 Apr 21;312(5772):400-4.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Institut d'Astrophysique Spatiale (IAS), Batiment 121, 91405 Orsay Campus, France.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/16627738" target="_blank"〉PubMed〈/a〉
    Keywords: Aluminum Silicates ; Atmosphere ; Carbon Dioxide ; Extraterrestrial Environment ; Ferric Compounds ; *Mars ; *Minerals ; Silicates ; Sulfates ; Time ; *Water
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  • 15
    Publication Date: 1993-08-06
    Description: Observations of the 1.4- to 2.4-micrometer spectrum of Pluto reveal absorptions of carbon monoxide and nitrogen ices and confirm the presence of solid methane. Frozen nitrogen is more abundant than the other two ices by a factor of about 50; gaseous nitrogen must therefore be the major atmospheric constituent. The absence of carbon dioxide absorptions is one of several differences between the spectra of Pluto and Triton in this region. Both worlds carry information about the composition of the solar nebula and the processes by which icy planetesimals formed.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Owen, T C -- Roush, T L -- Cruikshank, D P -- Elliot, J L -- Young, L A -- de Bergh, C -- Schmitt, B -- Geballe, T R -- Brown, R H -- Bartholomew, M J -- New York, N.Y. -- Science. 1993 Aug 6;261(5122):745-8.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17757212" target="_blank"〉PubMed〈/a〉
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  • 16
    Publication Date: 1993-08-06
    Description: The near-infrared spectrum of Triton reveals ices of nitrogen, methane, carbon monoxide, and carbon dioxide, of which nitrogen is the dominant component. Carbon dioxide ice may be spatially segregated from the other more volatile ices, covering about 10 percent of Triton's surface. The absence of ices of other hydrocarbons and nitriles challenges existing models of methane and nitrogen photochemistry on Triton.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Cruikshank, D P -- Roush, T L -- Owen, T C -- Geballe, T R -- de Bergh, C -- Schmitt, B -- Brown, R H -- Bartholomew, M J -- New York, N.Y. -- Science. 1993 Aug 6;261(5122):742-5.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17757211" target="_blank"〉PubMed〈/a〉
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  • 17
    Publication Date: 2011-10-29
    Description: The Visible, InfraRed, and Thermal Imaging Spectrometer (VIRTIS) on Rosetta obtained hyperspectral images, spectral reflectance maps, and temperature maps of the asteroid 21 Lutetia. No absorption features, of either silicates or hydrated minerals, have been detected across the observed area in the spectral range from 0.4 to 3.5 micrometers. The surface temperature reaches a maximum value of 245 kelvin and correlates well with topographic features. The thermal inertia is in the range from 20 to 30 joules meter(-2) kelvin(-1) second(-0.5), comparable to a lunarlike powdery regolith. Spectral signatures of surface alteration, resulting from space weathering, seem to be missing. Lutetia is likely a remnant of the primordial planetesimal population, unaltered by differentiation processes and composed of chondritic materials of enstatitic or carbonaceous origin, dominated by iron-poor minerals that have not suffered aqueous alteration.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Coradini, A -- Capaccioni, F -- Erard, S -- Arnold, G -- De Sanctis, M C -- Filacchione, G -- Tosi, F -- Barucci, M A -- Capria, M T -- Ammannito, E -- Grassi, D -- Piccioni, G -- Giuppi, S -- Bellucci, G -- Benkhoff, J -- Bibring, J P -- Blanco, A -- Blecka, M -- Bockelee-Morvan, D -- Carraro, F -- Carlson, R -- Carsenty, U -- Cerroni, P -- Colangeli, L -- Combes, M -- Combi, M -- Crovisier, J -- Drossart, P -- Encrenaz, E T -- Federico, C -- Fink, U -- Fonti, S -- Giacomini, L -- Ip, W H -- Jaumann, R -- Kuehrt, E -- Langevin, Y -- Magni, G -- McCord, T -- Mennella, V -- Mottola, S -- Neukum, G -- Orofino, V -- Palumbo, P -- Schade, U -- Schmitt, B -- Taylor, F -- Tiphene, D -- Tozzi, G -- New York, N.Y. -- Science. 2011 Oct 28;334(6055):492-4. doi: 10.1126/science.1204062.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Istituto di Fisica dello Spazio Interplanetario, Istituto Nazionale di Astrofisica (INAF), 00133 Rome, Italy.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/22034430" target="_blank"〉PubMed〈/a〉
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  • 18
    Publication Date: 2015-01-24
    Description: The VIRTIS (Visible, Infrared and Thermal Imaging Spectrometer) instrument on board the Rosetta spacecraft has provided evidence of carbon-bearing compounds on the nucleus of the comet 67P/Churyumov-Gerasimenko. The very low reflectance of the nucleus (normal albedo of 0.060 +/- 0.003 at 0.55 micrometers), the spectral slopes in visible and infrared ranges (5 to 25 and 1.5 to 5% kA(-1)), and the broad absorption feature in the 2.9-to-3.6-micrometer range present across the entire illuminated surface are compatible with opaque minerals associated with nonvolatile organic macromolecular materials: a complex mixture of various types of carbon-hydrogen and/or oxygen-hydrogen chemical groups, with little contribution of nitrogen-hydrogen groups. In active areas, the changes in spectral slope and absorption feature width may suggest small amounts of water-ice. However, no ice-rich patches are observed, indicating a generally dehydrated nature for the surface currently illuminated by the Sun.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Capaccioni, F -- Coradini, A -- Filacchione, G -- Erard, S -- Arnold, G -- Drossart, P -- De Sanctis, M C -- Bockelee-Morvan, D -- Capria, M T -- Tosi, F -- Leyrat, C -- Schmitt, B -- Quirico, E -- Cerroni, P -- Mennella, V -- Raponi, A -- Ciarniello, M -- McCord, T -- Moroz, L -- Palomba, E -- Ammannito, E -- Barucci, M A -- Bellucci, G -- Benkhoff, J -- Bibring, J P -- Blanco, A -- Blecka, M -- Carlson, R -- Carsenty, U -- Colangeli, L -- Combes, M -- Combi, M -- Crovisier, J -- Encrenaz, T -- Federico, C -- Fink, U -- Fonti, S -- Ip, W H -- Irwin, P -- Jaumann, R -- Kuehrt, E -- Langevin, Y -- Magni, G -- Mottola, S -- Orofino, V -- Palumbo, P -- Piccioni, G -- Schade, U -- Taylor, F -- Tiphene, D -- Tozzi, G P -- Beck, P -- Biver, N -- Bonal, L -- Combe, J-Ph -- Despan, D -- Flamini, E -- Fornasier, S -- Frigeri, A -- Grassi, D -- Gudipati, M -- Longobardo, A -- Markus, K -- Merlin, F -- Orosei, R -- Rinaldi, G -- Stephan, K -- Cartacci, M -- Cicchetti, A -- Giuppi, S -- Hello, Y -- Henry, F -- Jacquinod, S -- Noschese, R -- Peter, G -- Politi, R -- Reess, J M -- Semery, A -- New York, N.Y. -- Science. 2015 Jan 23;347(6220):aaa0628. doi: 10.1126/science.aaa0628.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy. fabrizio.capaccioni@iaps.inaf.it. ; Istituto di Astrofisica e Planetologia Spaziali, Istituto Nazionale di Astrofisica (INAF), Rome, Italy. ; Laboratoire d'Etudes Spatiales et d'Instrumentation en Astrophysique, Observatoire de Paris/CNRS/Universite Pierre et Marie Curie[acute accent over last letter in "Universite"]/Universite Paris-Diderot, Meudon, France. ; Institute for Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Berlin, Germany. ; Universite Grenoble Alpes, CNRS, Institut de Planetologie et d'Astrophysique de Grenoble, Grenoble, France. ; Osservatorio di Capodimonte, INAF, Napoli, Italy. ; Bear Fight Institute, Winthrop, WA 98862, USA. ; University of California, Los Angeles, Los Angeles, CA 90095, USA. ; European Space Agency (ESA), European Space Research and Technology Centre (ESTEC), Noordwijk, Netherlands. ; Institut d'Astrophysique Spatial, CNRS, Orsay, France. ; Dipartimento di Matematica e Fisica "Ennio De Giorgi," Universita del Salento, Italy. ; Space Research Centre, Polish Academy of Sciences, Warsaw, Poland. ; NASA Jet Propulsion Laboratory, Pasadena, CA 91109, USA. ; Space Physics Research Laboratory, The University of Michigan, Ann Arbor, MI 48109, USA. ; Universita di Perugia, Perugia, Italy. ; Lunar Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA. ; National Central University, Taipei, Taiwan. ; Departement of Physics, Oxford University, Oxford, UK. ; Institute for Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR), Berlin, Germany. Free University of Berlin, Institute of Geosciences, Malteserstrasse 74-100, Building Haus A, 12249 Berlin, Germany. ; Universita "Parthenope," Napoli, Italy. ; Helmholtz-Zentrum Berlin fur Materialien und Energie, Berlin, Germany. ; Osservatorio Astrofisico di Arcetri, INAF, Firenze, Italy. ; Agenzia Spaziale Italiana, Rome, Italy. ; NASA Jet Propulsion Laboratory, Pasadena, CA 91109, USA. Institute for Physical Science and Technology, University of Maryland, College Park, MD 20742, USA. ; Istituto di Radioastronomia, INAF, Bologna, Italy. ; Institut fur Optische Sensorsysteme, DLR, Berlin, Germany.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/25613895" target="_blank"〉PubMed〈/a〉
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  • 19
    Publication Date: 2016-03-19
    Description: The New Horizons mission has provided resolved measurements of Pluto's moons Styx, Nix, Kerberos, and Hydra. All four are small, with equivalent spherical diameters of ~40 kilometers for Nix and Hydra and ~10 kilometers for Styx and Kerberos. They are also highly elongated, with maximum to minimum axis ratios of ~2. All four moons have high albedos (~50 to 90%) suggestive of a water-ice surface composition. Crater densities on Nix and Hydra imply surface ages of at least 4 billion years. The small moons rotate much faster than synchronous, with rotational poles clustered nearly orthogonal to the common pole directions of Pluto and Charon. These results reinforce the hypothesis that the small moons formed in the aftermath of a collision that produced the Pluto-Charon binary.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Weaver, H A -- Buie, M W -- Buratti, B J -- Grundy, W M -- Lauer, T R -- Olkin, C B -- Parker, A H -- Porter, S B -- Showalter, M R -- Spencer, J R -- Stern, S A -- Verbiscer, A J -- McKinnon, W B -- Moore, J M -- Robbins, S J -- Schenk, P -- Singer, K N -- Barnouin, O S -- Cheng, A F -- Ernst, C M -- Lisse, C M -- Jennings, D E -- Lunsford, A W -- Reuter, D C -- Hamilton, D P -- Kaufmann, D E -- Ennico, K -- Young, L A -- Beyer, R A -- Binzel, R P -- Bray, V J -- Chaikin, A L -- Cook, J C -- Cruikshank, D P -- Dalle Ore, C M -- Earle, A M -- Gladstone, G R -- Howett, C J A -- Linscott, I R -- Nimmo, F -- Parker, J Wm -- Philippe, S -- Protopapa, S -- Reitsema, H J -- Schmitt, B -- Stryk, T -- Summers, M E -- Tsang, C C C -- Throop, H H B -- White, O L -- Zangari, A M -- New York, N.Y. -- Science. 2016 Mar 18;351(6279):aae0030. doi: 10.1126/science.aae0030.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. hal.weaver@jhuapl.edu. ; Southwest Research Institute, Boulder, CO 80302, USA. ; NASA Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. ; Lowell Observatory, Flagstaff, AZ 86001, USA. ; National Optical Astronomy Observatory, Tucson, AZ 26732, USA. ; SETI Institute, Mountain View, CA 94043, USA. ; Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA. ; Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA. ; Space Science Division, NASA Ames Research Center, Moffett Field, CA 94035, USA. ; Lunar and Planetary Institute, Houston, TX 77058, USA. ; Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. ; Department of Astronomy, University of Maryland, College Park, MD 20742, USA. ; SETI Institute, Mountain View, CA 94043, USA. Space Science Division, NASA Ames Research Center, Moffett Field, CA 94035, USA. ; Massachusetts Institute of Technology, Cambridge, MA 02139, USA. ; University of Arizona, Tucson, AZ 85721, USA. ; Independent science writer, Arlington, VT, USA. ; Southwest Research Institute, San Antonio, TX 78238, USA. ; Stanford University, Stanford, CA 94305, USA. ; University of California, Santa Cruz, CA 95064, USA. ; Universite Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. ; Roane State Community College, Oak Ridge, TN 37830, USA. ; George Mason University, Fairfax, VA 22030, USA. ; Planetary Science Institute, Tucson, AZ 85719, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26989256" target="_blank"〉PubMed〈/a〉
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  • 20
    Publication Date: 2016-03-19
    Description: The New Horizons spacecraft mapped colors and infrared spectra across the encounter hemispheres of Pluto and Charon. The volatile methane, carbon monoxide, and nitrogen ices that dominate Pluto's surface have complicated spatial distributions resulting from sublimation, condensation, and glacial flow acting over seasonal and geological time scales. Pluto's water ice "bedrock" was also mapped, with isolated outcrops occurring in a variety of settings. Pluto's surface exhibits complex regional color diversity associated with its distinct provinces. Charon's color pattern is simpler, dominated by neutral low latitudes and a reddish northern polar region. Charon's near-infrared spectra reveal highly localized areas with strong ammonia absorption tied to small craters with relatively fresh-appearing impact ejecta.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Grundy, W M -- Binzel, R P -- Buratti, B J -- Cook, J C -- Cruikshank, D P -- Dalle Ore, C M -- Earle, A M -- Ennico, K -- Howett, C J A -- Lunsford, A W -- Olkin, C B -- Parker, A H -- Philippe, S -- Protopapa, S -- Quirico, E -- Reuter, D C -- Schmitt, B -- Singer, K N -- Verbiscer, A J -- Beyer, R A -- Buie, M W -- Cheng, A F -- Jennings, D E -- Linscott, I R -- Parker, J Wm -- Schenk, P M -- Spencer, J R -- Stansberry, J A -- Stern, S A -- Throop, H B -- Tsang, C C C -- Weaver, H A -- Weigle, G E 2nd -- Young, L A -- New Horizons Science Team -- New York, N.Y. -- Science. 2016 Mar 18;351(6279):aad9189. doi: 10.1126/science.aad9189.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Lowell Observatory, Flagstaff, AZ 86001, USA. w.grundy@lowell.edu. ; Massachusetts Institute of Technology, Cambridge, MA 02139, USA. ; NASA Jet Propulsion Laboratory, La Canada Flintridge, CA 91011, USA. ; Southwest Research Institute, Boulder, CO 80302, USA. ; NASA Ames Research Center, Space Science Division, Moffett Field, CA 94035, USA. ; NASA Ames Research Center, Space Science Division, Moffett Field, CA 94035, USA. Carl Sagan Center, SETI Institute, Mountain View, CA 94043, USA. ; NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA. ; Universite Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France. ; Department of Astronomy, University of Maryland, College Park, MD 20742, USA. ; Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA. ; Johns Hopkins University Applied Physics Laboratory, Laurel, MD 20723, USA. ; Stanford University, Stanford, CA 94305, USA. ; Lunar and Planetary Institute, Houston, TX 77058, USA. ; Space Telescope Science Institute, Baltimore, MD, USA. ; Planetary Science Institute, Mumbai, India. ; Southwest Research Institute, San Antonio, TX 28510, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/26989260" target="_blank"〉PubMed〈/a〉
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