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  • 1
    Publication Date: 2015-02-12
    Description: Using the Mars Exploration Rover Opportunity , we have compiled one of the first field geologic maps on Mars while traversing the Noachian terrain along the rim of the 22-km diameter Endeavour crater (Lat -2° 16’ 33”, Long -5° 10’ 51”). In situ mapping of the petrographic, elemental, structural, and stratigraphic characteristics of outcrops and rocks distinguishes four mappable bedrock lithologic units. Three of these rock units pre-date the surrounding Burns formation sulfate-rich sandstones and one, the Matijevic formation, represents conditions on early Mars pre-dating the formation of Endeavour crater. The stratigraphy assembled from these observations includes several geologic unconformities. The differences in lithologic units across these unconformities record changes in the character and intensity of the Martian aqueous environment over geologic time. Water circulated through fractures in the oldest rocks over periods long enough that texturally and elementally significant alteration occurred in fracture walls. These oldest pre-Endeavour rocks and their network of mineralized and altered fractures were preserved by burial beneath impact ejecta and were subsequently exhumed and exposed. The alteration along joints in the oldest rocks, and the mineralized veins and concentrations of trace metals in overlying lithologic units is direct evidence that copious volumes of mineralized and/or hydrothermal fluids circulated through the early Martian crust. The wide range in intensity of structural and chemical modification from outcrop to outcrop along the crater rim shows that the ejecta of large (〉8 km in diameter) impact craters is complex. These results imply that geologic complexity is to be anticipated in other areas of Mars where cratering has been a fundamental process in the local and regional geology and mineralogy.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 2
    Publication Date: 2015-02-10
    Description: CRISM hyperspectral (1.0-2.65 µm) along-track oversampled observations (ATOs) covering Victoria, Santa Maria, Endeavour, and Ada craters were processed to 6 m/pixel and used in combination with Opportunity observations to detect and map hydrated Mg and Ca-sulfate minerals in the Burns formation. The strongest spectral absorption features were found to be associated with outcrops that are relatively young and fresh (Ada) or preferentially scoured of dust, soil, and coatings by prevailing winds. At Victoria and Santa Maria the scoured areas are on the southeastern rims and walls, opposite to the sides where wind-blown sands extend out of the craters. At Endeavour the deepest absorptions are in Botany Bay, a subdued and buried rim segment that exhibits high thermal inertias, extensive outcrops, and is interpreted to be a region of enhanced wind scour extending up and out of the crater. Ada, Victoria, and Santa Maria outcrops expose the upper portion of the preserved Burns formation and show spectral evidence for the presence of kieserite. In contrast, gypsum is pervasive spectrally in the Botany Bay exposures. Gypsum, a relatively insoluble evaporative mineral, is interpreted to have formed close to the contact with the Noachian crust as rising ground waters brought brines close to and onto the surface, either as a direct precipitate or during later diagenesis. The presence of kieserite at the top of the section is hypothesized to reflect precipitation from evaporatively concentrated brines or dehydration of polyhydrated sulfates, in both scenarios as the aqueous environment evolved to very arid conditions.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 3
    Publication Date: 2006-12-16
    Description: The Stardust spacecraft collected thousands of particles from comet 81P/Wild 2 and returned them to Earth for laboratory study. The preliminary examination of these samples shows that the nonvolatile portion of the comet is an unequilibrated assortment of materials that have both presolar and solar system origin. The comet contains an abundance of silicate grains that are much larger than predictions of interstellar grain models, and many of these are high-temperature minerals that appear to have formed in the inner regions of the solar nebula. Their presence in a comet proves that the formation of the solar system included mixing on the grandest scales.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Brownlee, Don -- Tsou, Peter -- Aleon, Jerome -- Alexander, Conel M O'd -- Araki, Tohru -- Bajt, Sasa -- Baratta, Giuseppe A -- Bastien, Ron -- Bland, Phil -- Bleuet, Pierre -- Borg, Janet -- Bradley, John P -- Brearley, Adrian -- Brenker, F -- Brennan, Sean -- Bridges, John C -- Browning, Nigel D -- Brucato, John R -- Bullock, E -- Burchell, Mark J -- Busemann, Henner -- Butterworth, Anna -- Chaussidon, Marc -- Cheuvront, Allan -- Chi, Miaofang -- Cintala, Mark J -- Clark, B C -- Clemett, Simon J -- Cody, George -- Colangeli, Luigi -- Cooper, George -- Cordier, Patrick -- Daghlian, C -- Dai, Zurong -- D'Hendecourt, Louis -- Djouadi, Zahia -- Dominguez, Gerardo -- Duxbury, Tom -- Dworkin, Jason P -- Ebel, Denton S -- Economou, Thanasis E -- Fakra, Sirine -- Fairey, Sam A J -- Fallon, Stewart -- Ferrini, Gianluca -- Ferroir, T -- Fleckenstein, Holger -- Floss, Christine -- Flynn, George -- Franchi, Ian A -- Fries, Marc -- Gainsforth, Z -- Gallien, J-P -- Genge, Matt -- Gilles, Mary K -- Gillet, Philipe -- Gilmour, Jamie -- Glavin, Daniel P -- Gounelle, Matthieu -- Grady, Monica M -- Graham, Giles A -- Grant, P G -- Green, Simon F -- Grossemy, Faustine -- Grossman, Lawrence -- Grossman, Jeffrey N -- Guan, Yunbin -- Hagiya, Kenji -- Harvey, Ralph -- Heck, Philipp -- Herzog, Gregory F -- Hoppe, Peter -- Horz, Friedrich -- Huth, Joachim -- Hutcheon, Ian D -- Ignatyev, Konstantin -- Ishii, Hope -- Ito, Motoo -- Jacob, Damien -- Jacobsen, Chris -- Jacobsen, Stein -- Jones, Steven -- Joswiak, David -- Jurewicz, Amy -- Kearsley, Anton T -- Keller, Lindsay P -- Khodja, H -- Kilcoyne, A L David -- Kissel, Jochen -- Krot, Alexander -- Langenhorst, Falko -- Lanzirotti, Antonio -- Le, Loan -- Leshin, Laurie A -- Leitner, J -- Lemelle, L -- Leroux, Hugues -- Liu, Ming-Chang -- Luening, K -- Lyon, Ian -- Macpherson, Glen -- Marcus, Matthew A -- Marhas, Kuljeet -- Marty, Bernard -- Matrajt, Graciela -- McKeegan, Kevin -- Meibom, Anders -- Mennella, Vito -- Messenger, Keiko -- Messenger, Scott -- Mikouchi, Takashi -- Mostefaoui, Smail -- Nakamura, Tomoki -- Nakano, T -- Newville, M -- Nittler, Larry R -- Ohnishi, Ichiro -- Ohsumi, Kazumasa -- Okudaira, Kyoko -- Papanastassiou, Dimitri A -- Palma, Russ -- Palumbo, Maria E -- Pepin, Robert O -- Perkins, David -- Perronnet, Murielle -- Pianetta, P -- Rao, William -- Rietmeijer, Frans J M -- Robert, Francois -- Rost, D -- Rotundi, Alessandra -- Ryan, Robert -- Sandford, Scott A -- Schwandt, Craig S -- See, Thomas H -- Schlutter, Dennis -- Sheffield-Parker, J -- Simionovici, Alexandre -- Simon, Steven -- Sitnitsky, I -- Snead, Christopher J -- Spencer, Maegan K -- Stadermann, Frank J -- Steele, Andrew -- Stephan, Thomas -- Stroud, Rhonda -- Susini, Jean -- Sutton, S R -- Suzuki, Y -- Taheri, Mitra -- Taylor, Susan -- Teslich, Nick -- Tomeoka, Kazu -- Tomioka, Naotaka -- Toppani, Alice -- Trigo-Rodriguez, Josep M -- Troadec, David -- Tsuchiyama, Akira -- Tuzzolino, Anthony J -- Tyliszczak, Tolek -- Uesugi, K -- Velbel, Michael -- Vellenga, Joe -- Vicenzi, E -- Vincze, L -- Warren, Jack -- Weber, Iris -- Weisberg, Mike -- Westphal, Andrew J -- Wirick, Sue -- Wooden, Diane -- Wopenka, Brigitte -- Wozniakiewicz, Penelope -- Wright, Ian -- Yabuta, Hikaru -- Yano, Hajime -- Young, Edward D -- Zare, Richard N -- Zega, Thomas -- Ziegler, Karen -- Zimmerman, Laurent -- Zinner, Ernst -- Zolensky, Michael -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1711-6.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, University of Washington, Seattle, WA 98195, USA. brownlee@astro.washington.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170289" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 4
    Publication Date: 2006-12-16
    Description: We measured the elemental compositions of material from 23 particles in aerogel and from residue in seven craters in aluminum foil that was collected during passage of the Stardust spacecraft through the coma of comet 81P/Wild 2. These particles are chemically heterogeneous at the largest size scale analyzed ( approximately 180 ng). The mean elemental composition of this Wild 2 material is consistent with the CI meteorite composition, which is thought to represent the bulk composition of the solar system, for the elements Mg, Si, Mn, Fe, and Ni to 35%, and for Ca and Ti to 60%. The elements Cu, Zn, and Ga appear enriched in this Wild 2 material, which suggests that the CI meteorites may not represent the solar system composition for these moderately volatile minor elements.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Flynn, George J -- Bleuet, Pierre -- Borg, Janet -- Bradley, John P -- Brenker, Frank E -- Brennan, Sean -- Bridges, John -- Brownlee, Don E -- Bullock, Emma S -- Burghammer, Manfred -- Clark, Benton C -- Dai, Zu Rong -- Daghlian, Charles P -- Djouadi, Zahia -- Fakra, Sirine -- Ferroir, Tristan -- Floss, Christine -- Franchi, Ian A -- Gainsforth, Zack -- Gallien, Jean-Paul -- Gillet, Philippe -- Grant, Patrick G -- Graham, Giles A -- Green, Simon F -- Grossemy, Faustine -- Heck, Philipp R -- Herzog, Gregory F -- Hoppe, Peter -- Horz, Friedrich -- Huth, Joachim -- Ignatyev, Konstantin -- Ishii, Hope A -- Janssens, Koen -- Joswiak, David -- Kearsley, Anton T -- Khodja, Hicham -- Lanzirotti, Antonio -- Leitner, Jan -- Lemelle, Laurence -- Leroux, Hugues -- Luening, Katharina -- Macpherson, Glenn J -- Marhas, Kuljeet K -- Marcus, Matthew A -- Matrajt, Graciela -- Nakamura, Tomoki -- Nakamura-Messenger, Keiko -- Nakano, Tsukasa -- Newville, Matthew -- Papanastassiou, Dimitri A -- Pianetta, Piero -- Rao, William -- Riekel, Christian -- Rietmeijer, Frans J M -- Rost, Detlef -- Schwandt, Craig S -- See, Thomas H -- Sheffield-Parker, Julie -- Simionovici, Alexandre -- Sitnitsky, Ilona -- Snead, Christopher J -- Stadermann, Frank J -- Stephan, Thomas -- Stroud, Rhonda M -- Susini, Jean -- Suzuki, Yoshio -- Sutton, Stephen R -- Taylor, Susan -- Teslich, Nick -- Troadec, D -- Tsou, Peter -- Tsuchiyama, Akira -- Uesugi, Kentaro -- Vekemans, Bart -- Vicenzi, Edward P -- Vincze, Laszlo -- Westphal, Andrew J -- Wozniakiewicz, Penelope -- Zinner, Ernst -- Zolensky, Michael E -- New York, N.Y. -- Science. 2006 Dec 15;314(5806):1731-5.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Physics, State University of New York at Plattsburgh, 101 Broad Street, Plattsburgh, NY 12901, USA. george.flynn@plattsburgh.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17170294" target="_blank"〉PubMed〈/a〉
    Print ISSN: 0036-8075
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  • 5
    Publication Date: 2007-05-05
    Description: Home Plate is a layered plateau in Gusev crater on Mars. It is composed of clastic rocks of moderately altered alkali basalt composition, enriched in some highly volatile elements. A coarsegrained lower unit lies under a finer-grained upper unit. Textural observations indicate that the lower strata were emplaced in an explosive event, and geochemical considerations favor an explosive volcanic origin over an impact origin. The lower unit likely represents accumulation of pyroclastic materials, whereas the upper unit may represent eolian reworking of the same pyroclastic materials.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Squyres, S W -- Aharonson, O -- Clark, B C -- Cohen, B A -- Crumpler, L -- de Souza, P A -- Farrand, W H -- Gellert, R -- Grant, J -- Grotzinger, J P -- Haldemann, A F C -- Johnson, J R -- Klingelhofer, G -- Lewis, K W -- Li, R -- McCoy, T -- McEwen, A S -- McSween, H Y -- Ming, D W -- Moore, J M -- Morris, R V -- Parker, T J -- Rice, J W Jr -- Ruff, S -- Schmidt, M -- Schroder, C -- Soderblom, L A -- Yen, A -- New York, N.Y. -- Science. 2007 May 4;316(5825):738-42.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA.〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/17478719" target="_blank"〉PubMed〈/a〉
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  • 6
    Publication Date: 2008-05-24
    Description: Mineral deposits on the martian surface can elucidate ancient environmental conditions on the planet. Opaline silica deposits (as much as 91 weight percent SiO2) have been found in association with volcanic materials by the Mars rover Spirit. The deposits are present both as light-toned soils and as bedrock. We interpret these materials to have formed under hydrothermal conditions and therefore to be strong indicators of a former aqueous environment. This discovery is important for understanding the past habitability of Mars because hydrothermal environments on Earth support thriving microbial ecosystems.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Squyres, S W -- Arvidson, R E -- Ruff, S -- Gellert, R -- Morris, R V -- Ming, D W -- Crumpler, L -- Farmer, J D -- Marais, D J Des -- Yen, A -- McLennan, S M -- Calvin, W -- Bell, J F 3rd -- Clark, B C -- Wang, A -- McCoy, T J -- Schmidt, M E -- de Souza, P A Jr -- New York, N.Y. -- Science. 2008 May 23;320(5879):1063-7. doi: 10.1126/science.1155429.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA. squyres@astro.cornell.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/18497295" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Hot Temperature ; Hydrogen-Ion Concentration ; *Mars ; *Silicon Dioxide ; Spacecraft ; *Water
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  • 7
    Publication Date: 2009-07-04
    Description: The Wet Chemistry Laboratory on the Phoenix Mars Lander performed aqueous chemical analyses of martian soil from the polygon-patterned northern plains of the Vastitas Borealis. The solutions contained approximately 10 mM of dissolved salts with 0.4 to 0.6% perchlorate (ClO4) by mass leached from each sample. The remaining anions included small concentrations of chloride, bicarbonate, and possibly sulfate. Cations were dominated by Mg2+ and Na+, with small contributions from K+ and Ca2+. A moderately alkaline pH of 7.7 +/- 0.5 was measured, consistent with a carbonate-buffered solution. Samples analyzed from the surface and the excavated boundary of the approximately 5-centimeter-deep ice table showed no significant difference in soluble chemistry.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Hecht, M H -- Kounaves, S P -- Quinn, R C -- West, S J -- Young, S M M -- Ming, D W -- Catling, D C -- Clark, B C -- Boynton, W V -- Hoffman, J -- Deflores, L P -- Gospodinova, K -- Kapit, J -- Smith, P H -- New York, N.Y. -- Science. 2009 Jul 3;325(5936):64-7. doi: 10.1126/science.1172466.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA. michael.h.hecht@jpl.nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19574385" target="_blank"〉PubMed〈/a〉
    Keywords: *Anions ; *Cations ; Chemical Phenomena ; Extraterrestrial Environment ; Hydrogen-Ion Concentration ; *Mars ; Oxidation-Reduction ; *Perchlorates ; Solubility ; Spacecraft ; Temperature ; Water
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  • 8
    Publication Date: 2009-05-23
    Description: The Mars rover Opportunity has explored Victoria crater, an approximately 750-meter eroded impact crater formed in sulfate-rich sedimentary rocks. Impact-related stratigraphy is preserved in the crater walls, and meteoritic debris is present near the crater rim. The size of hematite-rich concretions decreases up-section, documenting variation in the intensity of groundwater processes. Layering in the crater walls preserves evidence of ancient wind-blown dunes. Compositional variations with depth mimic those approximately 6 kilometers to the north and demonstrate that water-induced alteration at Meridiani Planum was regional in scope.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Squyres, S W -- Knoll, A H -- Arvidson, R E -- Ashley, J W -- Bell, J F 3rd -- Calvin, W M -- Christensen, P R -- Clark, B C -- Cohen, B A -- de Souza, P A Jr -- Edgar, L -- Farrand, W H -- Fleischer, I -- Gellert, R -- Golombek, M P -- Grant, J -- Grotzinger, J -- Hayes, A -- Herkenhoff, K E -- Johnson, J R -- Jolliff, B -- Klingelhofer, G -- Knudson, A -- Li, R -- McCoy, T J -- McLennan, S M -- Ming, D W -- Mittlefehldt, D W -- Morris, R V -- Rice, J W Jr -- Schroder, C -- Sullivan, R J -- Yen, A -- Yingst, R A -- New York, N.Y. -- Science. 2009 May 22;324(5930):1058-61. doi: 10.1126/science.1170355.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Department of Astronomy, Space Sciences Building, Cornell University, Ithaca, NY 14853, USA. squyres@astro.cornell.edu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/19461001" target="_blank"〉PubMed〈/a〉
    Keywords: Extraterrestrial Environment ; Ferric Compounds ; *Mars ; Spacecraft ; Water
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  • 9
    Publication Date: 2010-06-05
    Description: Decades of speculation about a warmer, wetter Mars climate in the planet's first billion years postulate a denser CO2-rich atmosphere than at present. Such an atmosphere should have led to the formation of outcrops rich in carbonate minerals, for which evidence has been sparse. Using the Mars Exploration Rover Spirit, we have now identified outcrops rich in magnesium-iron carbonate (16 to 34 weight percent) in the Columbia Hills of Gusev crater. Its composition approximates the average composition of the carbonate globules in martian meteorite ALH 84001. The Gusev carbonate probably precipitated from carbonate-bearing solutions under hydrothermal conditions at near-neutral pH in association with volcanic activity during the Noachian era.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Morris, Richard V -- Ruff, Steven W -- Gellert, Ralf -- Ming, Douglas W -- Arvidson, Raymond E -- Clark, Benton C -- Golden, D C -- Siebach, Kirsten -- Klingelhofer, Gostar -- Schroder, Christian -- Fleischer, Iris -- Yen, Albert S -- Squyres, Steven W -- New York, N.Y. -- Science. 2010 Jul 23;329(5990):421-4. doi: 10.1126/science.1189667. Epub 2010 Jun 3.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉NASA Johnson Space Center, Houston, TX 77058, USA. richard.v.morris@nasa.gov〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/20522738" target="_blank"〉PubMed〈/a〉
    Keywords: Atmosphere ; Carbon Dioxide ; *Carbonates/chemistry ; Climate ; Extraterrestrial Environment ; Ferrous Compounds ; Magnesium ; *Mars ; Meteoroids ; Spacecraft ; Temperature ; *Water
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  • 10
    Publication Date: 2013-09-28
    Description: The ChemCam instrument, which provides insight into martian soil chemistry at the submillimeter scale, identified two principal soil types along the Curiosity rover traverse: a fine-grained mafic type and a locally derived, coarse-grained felsic type. The mafic soil component is representative of widespread martian soils and is similar in composition to the martian dust. It possesses a ubiquitous hydrogen signature in ChemCam spectra, corresponding to the hydration of the amorphous phases found in the soil by the CheMin instrument. This hydration likely accounts for an important fraction of the global hydration of the surface seen by previous orbital measurements. ChemCam analyses did not reveal any significant exchange of water vapor between the regolith and the atmosphere. These observations provide constraints on the nature of the amorphous phases and their hydration.〈br /〉〈span class="detail_caption"〉Notes: 〈/span〉Meslin, P-Y -- Gasnault, O -- Forni, O -- Schroder, S -- Cousin, A -- Berger, G -- Clegg, S M -- Lasue, J -- Maurice, S -- Sautter, V -- Le Mouelic, S -- Wiens, R C -- Fabre, C -- Goetz, W -- Bish, D -- Mangold, N -- Ehlmann, B -- Lanza, N -- Harri, A-M -- Anderson, R -- Rampe, E -- McConnochie, T H -- Pinet, P -- Blaney, D -- Leveille, R -- Archer, D -- Barraclough, B -- Bender, S -- Blake, D -- Blank, J G -- Bridges, N -- Clark, B C -- DeFlores, L -- Delapp, D -- Dromart, G -- Dyar, M D -- Fisk, M -- Gondet, B -- Grotzinger, J -- Herkenhoff, K -- Johnson, J -- Lacour, J-L -- Langevin, Y -- Leshin, L -- Lewin, E -- Madsen, M B -- Melikechi, N -- Mezzacappa, A -- Mischna, M A -- Moores, J E -- Newsom, H -- Ollila, A -- Perez, R -- Renno, N -- Sirven, J-B -- Tokar, R -- de la Torre, M -- d'Uston, L -- Vaniman, D -- Yingst, A -- MSL Science Team -- New York, N.Y. -- Science. 2013 Sep 27;341(6153):1238670. doi: 10.1126/science.1238670.〈br /〉〈span class="detail_caption"〉Author address: 〈/span〉Universite de Toulouse, UPS-OMP, IRAP, 31028 Toulouse, France. pmeslin@irap.omp.eu〈br /〉〈span class="detail_caption"〉Record origin:〈/span〉 〈a href="http://www.ncbi.nlm.nih.gov/pubmed/24072924" target="_blank"〉PubMed〈/a〉
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