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      A Mineralogical Context for the Organic Matter in the Paris Meteorite Determined by A Multi-Technique Analysis

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          Abstract

          This study is a multi-technique investigation of the Paris carbonaceous chondrite directly applied on two selected 500 × 500 µm² areas of a millimetric fragment, without any chemical extraction. By mapping the partial hydration of the amorphous silicate phase dominating the meteorite sample matrix, infrared spectroscopy gave an interesting glimpse into the way the fluid may have circulated into the sample and partially altered it. The TOF-SIMS in-situ analysis allowed the studying and mapping of the wide diversity of chemical moieties composing the meteorite organic content. The results of the combined techniques show that at the micron scale, the organic matter was always spatially associated with the fine-grained and partially-hydrated amorphous silicates and to the presence of iron in different chemical states. These systematic associations, illustrated in previous studies of other carbonaceous chondrites, were further supported by the identification by TOF-SIMS of cyanide and/or cyanate salts that could be direct remnants of precursor ices that accreted with dust during the parent body formation, and by the detection of different metal-containing large organic ions. Finally, the results obtained emphasized the importance of studying the specific interactions taking place between organic and mineral phases in the chondrite matrix, in order to investigate their role in the evolution story of primitive organic matter in meteorite parent bodies.

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          Most cited references103

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          Organic compounds in carbonaceous meteorites.

          The carbonaceous chondrite meteorites are fragments of asteroids that have remained relatively unprocessed since the formation of the solar system 4.6 billion years ago. These carbon-rich objects contain a variety of extraterrestrial organic molecules that constitute a record of chemical evolution prior to the origin of life. Compound classes include aliphatic hydrocarbons, aromatic hydrocarbons, amino acids, carboxylic acids, sulfonic acids, phosphonic acids, alcohols, aldehydes, ketones, sugars, amines, amides, nitrogen heterocycles, sulfur heterocycles and a relatively abundant high molecular weight macromolecular material. Structural and stable isotopic characteristics suggest that a number of environments may have contributed to the organic inventory, including interstellar space, the solar nebula and the asteroidal meteorite parent body. This review covers work published between 1950 and the present day and cites 193 references.
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            High molecular diversity of extraterrestrial organic matter in Murchison meteorite revealed 40 years after its fall.

            Numerous descriptions of organic molecules present in the Murchison meteorite have improved our understanding of the early interstellar chemistry that operated at or just before the birth of our solar system. However, all molecular analyses were so far targeted toward selected classes of compounds with a particular emphasis on biologically active components in the context of prebiotic chemistry. Here we demonstrate that a nontargeted ultrahigh-resolution molecular analysis of the solvent-accessible organic fraction of Murchison extracted under mild conditions allows one to extend its indigenous chemical diversity to tens of thousands of different molecular compositions and likely millions of diverse structures. This molecular complexity, which provides hints on heteroatoms chronological assembly, suggests that the extraterrestrial chemodiversity is high compared to terrestrial relevant biological- and biogeochemical-driven chemical space.
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              Carbonaceous meteorites contain a wide range of extraterrestrial nucleobases.

              All terrestrial organisms depend on nucleic acids (RNA and DNA), which use pyrimidine and purine nucleobases to encode genetic information. Carbon-rich meteorites may have been important sources of organic compounds required for the emergence of life on the early Earth; however, the origin and formation of nucleobases in meteorites has been debated for over 50 y. So far, the few nucleobases reported in meteorites are biologically common and lacked the structural diversity typical of other indigenous meteoritic organics. Here, we investigated the abundance and distribution of nucleobases and nucleobase analogs in formic acid extracts of 12 different meteorites by liquid chromatography-mass spectrometry. The Murchison and Lonewolf Nunataks 94102 meteorites contained a diverse suite of nucleobases, which included three unusual and terrestrially rare nucleobase analogs: purine, 2,6-diaminopurine, and 6,8-diaminopurine. In a parallel experiment, we found an identical suite of nucleobases and nucleobase analogs generated in reactions of ammonium cyanide. Additionally, these nucleobase analogs were not detected above our parts-per-billion detection limits in any of the procedural blanks, control samples, a terrestrial soil sample, and an Antarctic ice sample. Our results demonstrate that the purines detected in meteorites are consistent with products of ammonium cyanide chemistry, which provides a plausible mechanism for their synthesis in the asteroid parent bodies, and strongly supports an extraterrestrial origin. The discovery of new nucleobase analogs in meteorites also expands the prebiotic molecular inventory available for constructing the first genetic molecules.
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                Author and article information

                Journal
                Life (Basel)
                Life (Basel)
                life
                Life
                MDPI
                2075-1729
                30 May 2019
                June 2019
                : 9
                : 2
                : 44
                Affiliations
                [1 ]Institut de Physique Nucléaire d’Orsay, UMR 8608, CNRS/IN2P3, Université Paris-Sud, Université Paris-Saclay, F-91406 Orsay, France; ribaud@ 123456ipno.in2p3.fr (I.R.); dellaneg@ 123456ipno.in2p3.fr (S.D.-N.)
                [2 ]Lebanese Atomic Energy Commission, NCSR, Beirut 11-8281, Lebanon; bnsouli@ 123456cnrs.edu.lb (B.N.); mroumie@ 123456cnrs.edu.lb (M.R.)
                [3 ]Institut d’Astrophysique Spatiale, UMR 8617, CNRS/Université Paris-Sud, Université Paris-Saclay, bâtiment 121, Université Paris-Sud, 91405 Orsay CEDEX, France; rosario.brunetto@ 123456ias.u-psud.fr (R.B.); zelia.dionnet@ 123456u-psud.fr (Z.D.); ldh@ 123456ias.u-psud.fr (L.L.S.d.)
                [4 ]Synchrotron Soleil, L’Orme des Merisiers, BP48, Saint Aubin, 91192 Gif sur Yvette CEDEX, France; ferenc.borondics@ 123456synchrotron-soleil.fr
                [5 ]Centre de Recherche et de Restauration des musées de France, UMR 171, Palais du Louvre, 75001 Paris, France; thomas.calligaro@ 123456culture.gouv.fr
                [6 ]PSL Research University, Institut de Recherche Chimie Paris, Chimie ParisTech, CNRS UMR 8247, 75005 Paris, France
                [7 ]Università degli Studi di Napoli Parthenope, Dip. di Scienze e Tecnologie, CDN IC4, I-80143 Naples, Italy
                [8 ]Université Aix-Marseille, Laboratoire de Physique des Interactions Ioniques et Moléculaires (PIIM), UMR CNRS 7345, F-13397 Marseille, France
                Author notes
                [* ]Correspondence: manale.noun@ 123456cnrs.edu.lb (M.N.); donia.baklouti@ 123456ias.u-psud.fr (D.B.); Tel.: +961-1-45-08-11 (M.N.); +33-1-69-85-87-88 (D.B.)
                Author information
                https://orcid.org/0000-0003-0840-0132
                https://orcid.org/0000-0002-2754-7829
                https://orcid.org/0000-0001-9975-4301
                https://orcid.org/0000-0002-9190-0842
                Article
                life-09-00044
                10.3390/life9020044
                6617381
                31151218
                0036a6f2-be60-4957-b721-63284053ba46
                © 2019 by the authors.

                Licensee MDPI, Basel, Switzerland. This article is an open access article distributed under the terms and conditions of the Creative Commons Attribution (CC BY) license ( http://creativecommons.org/licenses/by/4.0/).

                History
                : 30 March 2019
                : 25 May 2019
                Categories
                Article

                paris chondrite,tof-sims imaging,micro-infrared reflectance spectroscopy,visible reflectance spectroscopy,micro-raman,micro-pixe,chemical composition,organic species,aqueous alteration

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