Isotopic characterisation of kerogen-like material in the Murchison carbonaceous chondrite |
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| Affiliation: | 1. Institute of Geophysics, University of California, Los Angeles, CA 90024, U.S.A.;2. Extraterrestrial Research Division, NASA Ames Research Center, Moffett Field, CA 94035, U.S.A.;2. NASA Astrobiology Institute, Virtual Planetary Laboratory, Seattle, WA 98195, USA;4. University of Washington, Department of Earth & Space Sciences and Astrobiology Program, Seattle, WA 98195-1310, USA;1. Université Grenoble Alpes, CNRS, Institut de Planétologie et Astrophysique de Grenoble (IPAG), UMR 5274, Grenoble F-38041, France;2. Univ Lyon, ENSL, Univ Lyon 1, CNRS, LGL-TPE, F-69007 Lyon, France;1. Institut de Planétologie et d’Astrophysique de Grenoble (IPAG), Université Grenoble Alpes/CNRS-INSU, UMR 5274, Grenoble F-38041, France;2. LRGP, CNRS, Université de Lorraine, 1 rue Grandville, 54000 Nancy, France;3. CNRS/INSU, LATMOS-IPSL, Guyancourt F-78280, France;4. Unité Matériaux et Transformations, UMET, UMR-CNRS 8207, Université de Lille, France;5. Muséum National d''Histoire Naturelle, Sorbonne Université, CNRS UMR 7590, IRD, Institut de Minéralogie, de Physique des Matériaux et de Cosmochimie, Paris, France;6. ICS, CNRS, Université de Strasbourg, BP 296 R8, 670008 Strasbourg, France;1. Freie Universität Berlin, Institut für Geologische Wissenschaften, Berlin, Germany;2. Swedish Museum of Natural History, Stockholm, Sweden;3. Institut für Planetologie, University of Münster, Münster, Germany;1. Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, 55128 Mainz, Germany;2. Department of Earth and Planetary Science, The University of Tokyo, 7-3-1 Hongo, Tokyo 113-0033, Japan;3. Université de Lorraine, CRPG, UMR 7358, Vandoeuvre les Nancy F-54501, France;4. CNRS, CRPG UMR 7358, Vandoeuvre les Nancy, F-54501, France;5. Atmosphere and Ocean Research Institute, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8564, Japan |
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| Abstract: | Isotopic data for C, H and N in acid-resistant residues from carbonaceous chondrites show substantial variability during stepwise pyrolysis and/or combustion. After subtraction of contributions due apparently to inorganic C grains, of probably circumstellar origin, considerable isotopic variability remains, attributable to the kerogen-like organic fraction. That variability may be interpreted in terms of three or four distinct components, based on C, H and N isotopes. The relative proportions of those components vary significantly from sample to sample. The different isotopic components are tentatively identified in terms of specific chemical/structural moieties within the kerogen-like material. This combination of chemical, structural and isotopic information suggests a complex history for meteoritic organic matter. At least three components within the organic population as a whole still carry a signature of apparently interstellar Denrichment. Part, at least, of the interstellar carrier consisted of reactive entities, not solely polymers. |
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