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Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars

By Caroline Freissinet, D. P. Glavin, Paul R. Mahaffy, K. E. Miller, J. L. Eigenbrode, R. E. Summons, A. E. Brunner, A. Buch, Cyril Szopa, P. D. Archer, H. B. Franz, S. K. Atreya, W. B. Brinckerhoff, Michel Cabane, Patrice Coll, P. G. Conrad, D. J. Des Marais, J. P. Dworkin, A. G. Fairén, P. François, J. P. Grotzinger, S. Kashyap, I. L. Ten Kate, L. A. Leshin, C. A. Malespin, M. G. Martin, F. J. Martin-Torres, A. C. Mcadam, D. W. Ming, R. Navarro-González, A. A. Pavlov, B. D. Prats, S. W. Squyres, A. Steele, J. C. Stern, D. Y. Sumner, B. Sutter and M.-P. Zorzano

Abstract

International audienceThe Sample Analysis at Mars (SAM) instrument on board the Mars Science Laboratory Curiosity rover is designed to conduct inorganic and organic chemical analyses of the atmosphere and the surface regolith and rocks to help evaluate the past and present habitability potential of Mars at Gale Crater. Central to this task is the development of an inventory of any organic molecules present to elucidate processes associated with their origin, diagenesis, concentration, and long-term preservation. This will guide the future search for biosignatures. Here we report the definitive identification of chlorobenzene (150–300 parts per billion by weight (ppbw)) and C2 to C4 dichloroalkanes (up to 70 ppbw) with the SAM gas chromatograph mass spectrometer (GCMS) and detection of chlorobenzene in the direct evolved gas analysis (EGA) mode, in multiple portions of the fines from the Cumberland drill hole in the Sheepbed mudstone at Yellowknife Bay. When combined with GCMS and EGA data from multiple scooped and drilled samples, blank runs, and supporting laboratory analog studies, the elevated levels of chlorobenzene and the dichloroalkanes cannot be solely explained by instrument background sources known to be present in SAM. We conclude that these chlorinated hydrocarbons are the reaction products of Martian chlorine and organic carbon derived from Martian sources (e.g., igneous, hydrothermal, atmospheric, or biological) or exogenous sources such as meteorites, comets, or interplanetary dust particles

Topics: Surface materials and properties, Volcanism, Composition, Erosion and weathering, Mars, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ SDU.ASTR.SR ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR]
Publisher: Wiley-Blackwell
Year: 2015
DOI identifier: 10.1002/2014JE004737
OAI identifier: oai:HAL:insu-01218165v1
Provided by: Hal-Diderot

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