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1. Seeking Signs of Life on Mars: the Importance of Sedimentary Suites as Part of a Mars Sample Return Campaign

Author

Mangold, N, McLennan, S. M, Czaja, A. D, Ori, G. G, Tosca, N. J, Altieri, F, Amelin, Y, Ammannito, E, Anand, M, Beaty, D. W, Benning, L. G, Bishop, J. L, Borg, L. E, Boucher, D, Brucato, J. R, Busemann, H, Campbell, K. A, Carrier, B. L, Debaille, V, Des Marais, D. J, Dixon, M, Ehlmann, B. L, Farmer, J. D, Fernandez-Remolar, D. C, Fogarty, J, Glavin, D. P, Goreva, Y. S, Grady, M. M, Hallis, L. J, Harrington, A. D, Hausrath, E. M, Herd, C. D. K, Horgan, B, Humayun, M, Kleine, T, Kleinhenz, J, Mackelprang, R, Mayhew, L. E, McCubbin, F. M, McCoy, J. T, McSween, H. Y, Moser, D. E, Moynier, F, Mustard, J. F, Niles, P. B, Raulin, F, Rettberg, P, Rucker, M. A, Schmitz, N, Sefton-Nash, E, Sephton, M. A, Shaheen, R, Shuster, D. L, Siljeström, S, Smith, C. L, Spry, J. A, Steele, A, Swindle, T. D, ten Kate, I. L, Usui, T, Van Kranendonk, M. J, Wadhwa, M, Weiss, B. P, Werner, S. C, Westall, F, Wheeler, R. M, Zipfel, J, and Zorzano, M. P

Subjects
Space Sciences (General)
Abstract

Seeking the signs of life on Mars is often considered the "first among equal" objectives for any potential Mars Sample Return (MSR) campaign. Among the geological settings considered to have the greatest potential for recording evidence of ancient life or its pre-biotic chemistry on Mars are lacustrine (and marine, if ever present) sedimentary depositional environments. This potential, and the possibility of returning samples that could meaningfully address this objective, have been greatly enhanced by investigations of an ancient redox stratified lake system in Gale crater by the Curiosity rover.

Published
2018

2. Seeking Signs of Life on Mars: A Strategy for Selecting and Analyzing Returned Samples from Hydrothermal Deposits

Author

Campbell, K. A, Farmer, J. D, Van Kranendonk, M. J, Fernandez-Remolar, D. C, Czaja, A. D, Altieri, F, Amelin, Y, Ammannito, E, Anand, M, Beaty, D. W, Benning, L. G, Bishop, J. L, Borg, L. E, Boucher, D, Brucato, J. R, Busemann, J. R, Carrier, B. L, Debaille, V, Des Marais, D. J, Dixon, M, Ehlmann, B. L, Fogarty, James T, Glavin, D. P, Goreva, Y. S, Grady, M. M, Hallis, L. J, Harrington, A. D, Hausrath, E. M, Herd, C. D. K, Horgan, B, Humayun, M, Kleine, T, Kleinhenz, J, Mangold, N, Mackelprang, R, Mayhew, L. E, McCubbin, F. M, Mccoy, Teresa R, McLennan, S. M, McSween, H. Y, Moser, D. E, Moynier, F, Mustard, J. F, Niles, P. B, Ori, G. G, Raulin, F, Rettberg, P, Rucker, Michelle A, Schmitz, N, Sefton-Nash, E, Sephton, M. A, Shaheen, R, Shuster, D. L, Siljestrom, S, Smith, C. L, Spry, J. A, Steele, A, Swindle, T. D, ten Kate, I. L, Tosca, N. J, Usui, T, Wadhwa, M, Weiss, B. P, Werner, S. C, Westall, F, Wheeler, R. M, Zipfel, J, and Zorzano, M. P

Subjects
Space Sciences (General)
Abstract

Highly promising locales for biosignature prospecting on Mars are ancient hydrothermal deposits, formed by the interaction of surface water with heat from volcanism or impacts. On Earth, they occur throughout the geological record (to at least approx. 3.5 Ga), preserving robust mineralogical, textural and compositional evidence of thermophilic microbial activity. Hydrothermal systems were likely present early in Mars' history, including at two of the three finalist candidate landing sites for M2020, Columbia Hills and NE Syrtis Major. Hydrothermal environments on Earth's surface are varied, constituting subaerial hot spring aprons, mounds and fumaroles; shallow to deep-sea hydrothermal vents (black and white smokers); and vent mounds and hot-spring discharges in lacustrine and fluvial settings. Biological information can be preserved by rapid, spring-sourced mineral precipitation, but also could be altered or destroyed by postdepositional events. Thus, field observations need to be followed by detailed laboratory analysis to verify potential biosignatures. See Attachment

Published
2018

3. Volatile Analysis by Pyrolysis of Regolith (Vapor) for Planetary Resource Prospecting

Author

Glavin, D. P, Malespin, C. A, Ten Kate, I. L, Mcadam, A, Getty, S. A, Mumm, E, Franz, H. B, Southard, A. E, Bleacher, J. E, and Mahaffy, P. R

Subjects
Lunar And Planetary Science And Exploration, Exobiology
Abstract

Measuring the chemical composition of planetary bodies and their atmospheres is key to understanding the formation of the Solar System and the evolution of the planets and their moons. In situ volatile measurements enable a ground-truth assessment of the distribution and abundance of resources such as water-ice and oxygen, important for a sustained human presence on the Moon and beyond. The Volatile Analysis by Pyrolysis of Regolith (VAPoR) instrument is a compact pyrolysis mass spectrometer designed to detect volatiles released from solid samples that are heated to elevated temperatures and is one technique that should be considered for resource prospecting on the Moon, Mars, and asteroids.

Published
2016

4. Martian Atmospheric Methane Plumes from Meteor Shower Infall: A Hypothesis

Author

Fries, M, Christou, A, Archer, D, Conrad, P, Cooke, W, Eigenbrode, J, ten Kate, I. L, Matney, M, Niles, P, and Sykes, M

Subjects
Lunar And Planetary Science And Exploration
Abstract

Methane plumes in the martian atmosphere have been detected using Earth-based spectroscopy, the Planetary Fourier Spectrometer on the ESA Mars Express mission, and the NASA Mars Science Laboratory. The methane's origin remains a mystery, with proposed sources including volcanism, exogenous sources like impacts and interplanetary dust, aqueous alteration of olivine in the presence of carbonaceous material, release from ancient deposits of methane clathrates, and/or biological activity. To date, none of these phenomena have been found to reliably correlate with the detection of methane plumes. An additional source exists, however: meteor showers could generate martian methane via UV pyrolysis of carbon-rich infall material. We find a correlation between the dates of Mars/cometary orbit encounters and detections of methane on Mars. We hypothesize that cometary debris falls onto Mars during these interactions, depositing freshly disaggregated meteor shower material in a regional concentration. The material generates methane via UV photolysis, resulting in a localized "plume" of short-lived methane.

Published
2016

5. Martian Methane From a Cometary Source: A Hypothesis

Author

Fries, M, Christou, A, Archer, D, Conrad, P, Cooke, W, Eigenbrode, J, ten Kate, I. L, Matney, M, Niles, P, Sykes, M, Steele, A, and Treiman, A

Subjects
Lunar And Planetary Science And Exploration
Abstract

In recent years, methane in the martian atmosphere has been detected by Earth-based spectroscopy, the Planetary Fourier Spectrometer on the ESA Mars Express mission, and the NASA Mars Science Laboratory. The methane's origin remains a mystery, with proposed sources including volcanism, exogenous sources like impacts and interplanetary dust, aqueous alteration of olivine in the presence of carbonaceous material, release from ancient deposits of methane clathrates, and/or biological activity. An additional potential source exists: meteor showers from the emission of large comet dust particles could generate martian methane via UV pyrolysis of carbon-rich infall material. We find a correlation between the dates of Mars/cometary orbit encounters and detections of methane on Mars. We hypothesize that cometary debris falls onto Mars during these interactions, generating methane via UV photolysis.

Published
2016

7. Enrichment of the HR 8799 planets by minor bodies and dust

Author

Frantseva, K., Mueller, M., Pokorný, P., Van Der Tak, F. F.S., Ten Kate, I. L., Frantseva, K., Mueller, M., Pokorný, P., Van Der Tak, F. F.S., and Ten Kate, I. L.

Abstract

Context. In the Solar System, minor bodies and dust deliver various materials to planetary surfaces. Several exoplanetary systems are known to host inner and outer belts, analogues of the main asteroid belt and the Kuiper belt, respectively. Aims. We study the possibility that exominor bodies and exodust deliver volatiles and refractories to the exoplanets in the well-characterised system HR 8799. Methods. We performed N-body simulations to study the impact rates of minor bodies in the system HR 8799. The model consists of the host star, four giant planets (HR 8799 e, d, c, and b), 650 000 test particles representing the inner belt, and 1 450 000 test particles representing the outer belt. Moreover we modelled dust populations that originate from both belts. Results. Within a million years, the two belts evolve towards the expected dynamical structure (also derived in other works), where mean-motion resonances with the planets carve the analogues of Kirkwood gaps. We find that, after this point, the planets suffer impacts by objects from the inner and outer belt at rates that are essentially constant with time, while dust populations do not contribute significantly to the delivery process. We convert the impact rates to volatile and refractory delivery rates using our best estimates of the total mass contained in the belts and their volatile and refractory content. Over their lifetime, the four giant planets receive between 10-4 and 10-3 M⊕ of material from both belts. Conclusions. The total amount of delivered volatiles and refractories, 5 × 10-3 M⊕ , is small compared to the total mass of the planets, 11 × 103 M⊕ . However, if the planets were formed to be volatile-rich, their exogenous enrichment in refractory material may well be significant and observable, for example with JWST-MIRI. If terrestrial planets exist within the snow line of the system, volatile delivery would be an important astrobiological mechanism and may be observable as atmospheric trace gas

Published
2020

10. Precision Subsampling System for Mars Surface Missions

Author

Mahaffy, P. R, Paulsen, G, Mellerowicz, B, ten Kate, I. L, Conrad, P, Corrigan, C. M, and Li, X

Subjects
Lunar And Planetary Science And Exploration
Abstract

The ability to analyze heterogeneous rock samples at fine spatial scales would represent a powerful addition to our planetary in situ analytical toolbox. This is particularly true for Mars, where the signatures of past environments and, potentially, habitability are preserved in chemical and morphological variations across sedimentary layers and among mineral pr.ases in a given rock specimen. On Earth, microbial life often associates with surfaces at the interface of chemical nutrients, and ultimately retains sub-millimeter to millimeter-scale layer confinement in fossilization. On Mars, and possibly other bodies, trace chemical markers (elemental, organic/molecular, isotopic, chiral, etc.) and fine-scale morphological markers (e.g., micro-fossils) may he too subtle, degraded, or ambiguous to be detected, using miniaturized instrumentation, without some concentration or isolation. This is because (i) instrument sensitivity may not be high enough to detect trace markers in bulk averages; and (ii) instrument s~lectiviry may not be sufficient to distinguish such markers from interfering/counteracting signals from the bulk. Moreover from a fundamental chemostratigraphic perspective there would be a great benefit to assessing specific chemical and stable isotopic gradients, over millimeter-to-centimeter scales and beyond, with higher precision than currently possible in situ. We have developed a precision subsampling system (PSS) that addresses this need while remaining relatively flexible to a variety of instruments that may take advantage of the capability on future missions. The PSS is relevant to a number of possible lander/rover missions, especially Mars Sample Return. Our specific PSS prototype is undergoing testing under Mars ambient conditions, on a variety of natural analog rocks and rock drill cores, using a set of complementary flight-compatible measurement techniques. The system is available for testing with other contact instruments that may benefit from precision sampling.

Published
2012

11. delta C-13 Analysis of Mars Analog Carbonates Using Evolved Gas Cavity - Ringdown Spectrometry on the 2010 Arctic Mars Analog Svalbard Expedition (AMASE)

Author

Stern, J. C, McAdam, A. C, ten Kate, I. L, Mahaffy, P. R, Steele, A, and Amundson, H. E. F

Subjects
Lunar And Planetary Science And Exploration
Abstract

The 2010 Arctic Mars Analog Svalbard Expedition (AMASE) investigated two distinct geologic settings on Svalbard, using instrumentation and techniques in development for future Mars missions, such as the Mars Science Laboratory (MSL), ExoMars, and Mars Sample Return (MSR). The Sample Analysis at Mars (SAM) instrument suite, which will fly on MSL, was developed at Goddard Space Flight Center (GSFC), together with several partners. SAM consists of a quadrupole mass spectrometer (QMS), a gas chromatograph CGC), and a tunable laser spectrometer (TLS), which all analyze gases created by evolved gas analysis (EGA). The two sites studied represent "biotic" and "abiotic" analogs; the "biotic" site being the Knorringfjell fossil methane seep, and the "abiotic" site being the basaltic Sigurdfjell vent complex. The data presented here represent experiments to measure the carbon isotopic composition of carbonates from these two analogs using evolved gas analysis coupled with a commercial cavity ringdown CO2 isotopic analyzer (Picarro) as a proxy for the TLS on SAM.

Published
2011

12. Field Characterization of the Mineralogy and Organic Chemistry of Carbonates from the 2010 Arctic Mars Analog Svalbard Expedition by Evolved Gas Analysis

Author

McAdam, A. C, Ten Kate, I. L, Stern, J. C, Mahaffy, P. R, Blake, D. F, Morris, R. V, Steele, A, and Amundson, H. E. F

Subjects
Geophysics
Abstract

The 2010 Arctic Mars Analog Svalbard Expedition (AMASE) investigated two geologic settings using methodologies and techniques being developed or considered for future Mars missions, such as the Mars Science Laboratory (MSL), ExoMars, and Mars Sample Return. The Sample Analysis at Mars (SAM) [1] instrument suite, which will be on MSL, consists of a quadrupole mass spectrometer (QMS), a gas chromatograph (GC), and a tunable laser mass spectrometer (TLS); all will be applied to analyze gases created by pyrolysis of samples. During AMASE, a Hiden Evolved Gas Analysis-Mass Spectrometer (EGA-MS) system represented the EGA-MS capability of SAM. Another MSL instrument, CheMin, will use x-ray diffraction (XRD) and x-ray fluorescence (XRF) to perform quantitative mineralogical characterization of samples [e.g., 2]. Field-portable versions of CheMin were used during AMASE. AMASE 2010 focused on two sites that represented biotic and abiotic analogs. The abiotic site was the basaltic Sigurdfjell vent complex, which contains Mars-analog carbonate cements including carbonate globules which are excellent analogs for the globules in the ALH84001 martian meteorite [e.g., 3, 4]. The biotic site was the Knorringfjell fossil methane seep, which featured carbonates precipitated in a methane-supported chemosynthetic community [5]. This contribution focuses on EGA-MS analyses of samples from each site, with mineralogy comparisons to CheMin team results. The results give insight into organic content and organic-mineral associations, as well as some constraints on the minerals present.

Published
2011

13. VAPoR - Volatile Analysis by Pyrolysis of Regolith - an Instrument for In Situ Detection of Water, Noble Gases, and Organics on the Moon

Author

ten Kate, I. L, Cardiff, E. H, Feng, S. H, Holmes, V, Malespin, C, Stern, J. G, Swindle, T. D, and Glavin, D. P

Subjects
Lunar And Planetary Science And Exploration
Abstract

We present the Volatile Analysis by Pyrolysis of Regolith (VAPoR) instrument design and demonstrate the validity of an in situ pyrolysis mass spectrometer for evolved gas analyses of lunar and planetary regolith samples. In situ evolved gas analyses of the lunar regolith have not yet been carried out and no atmospheric or evolved gas measurements have been made at the lunar poles. VAPoR is designed to do both kinds of measurements, is currently under development at NASA's Goddard Space Flight Center, and will be able to heat powdered regolith samples or rock drill fines up to 1400 C in vacuo. To validate the instrument concept, evolved gas species released from different planetary analogs were determined as a function of temperature using a laboratory breadboard. Evolved gas measurements of an Apollo 16 regolith sample and a fragment of the carbonaceous meteorite Murchison were made by VAPoR and our results compared with existing data. The results imply that in situ evolved gas measurements of the lunar regolith at the polar regions by VAPoR will be a very powerful tool for identifying water and other volatile signatures of lunar or exogenous origin as potential resources for future human exploration.

Published
2010
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14. Mauna Kea, Hawaii as an Analogue Site for Future Planetary Resource Exploration: Results from the 2010 ILSO-ISRU Field-Testing Campaign

Author

ten Kate, I. L, Armstrong, R, Bernhardt, B, Blummers, M, Boucher, D, Caillibot, E, Captain, J, Deleuterio, G, Farmer, J. D, Glavin, D. P, Hamilton, J. C, Klingelhoefer, G, Morris, R. V, Nunez, J. I, Quinn, J. W, Sanders, G. B, Sellar, R. G, Sigurdson, L, Taylor, R, and Zacny, K

Subjects
Lunar And Planetary Science And Exploration
Abstract

Within the framework of the International Lunar Surface Operation - In-Situ Resource Utilization Analogue Test held on January 27 - February 11, 2010 on the Mauna Kea volcano in Hawaii, a number of scientific instrument teams collaborated to characterize the field site and test instrument capabilities outside laboratory environments. In this paper, we provide a geological setting for this new field-test site, a description of the instruments that were tested during the 2010 ILSO-ISRU field campaign, and a short discussion for each instrument about the validity and use of the results obtained during the test. These results will form a catalogue that may serve as reference for future test campaigns. In this paper we provide a description and regional geological setting for a new field analogue test site for lunar resource exploration, and discuss results obtained from the 2010 ILSO-ISRU field campaign as a reference for future field-testing at this site. The following instruments were tested: a multispectral microscopic imager, MMI, a Mossbauer spectrometer, an evolved gas analyzer, VAPoR, and an oxygen and volatile extractor called RESOLVE. Preliminary results show that the sediments change from dry, organic-poor, poorly-sorted volcaniclastic sand on the surface, containing basalt, iron oxides and clays, to more water- and organic-rich, fine grained, well-sorted volcaniclastic sand, primarily consisting of iron oxides and depleted of basalt and clays. Furthermore, drilling experiments showed a very close correlation between drilling on the Moon and drilling at the test site. The ILSO-ISRU test site was an ideal location for testing strategies for in situ resource exploration at the lunar or martian surface.

Published
2010

15. The potential science and engineering value of samples delivered to Earth by Mars sample return

Author

Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., Zorzano, M. P., Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), The Open University [Milton Keynes] (OU), School of Earth Sciences [Bristol], University of Bristol [Bristol], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Australian National University (ANU), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Planetary and Space Sciences [Milton Keynes] (PSS), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU)-Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Génotoxicologie et cycle cellulaire (GCC), Institut Curie [Paris]-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Planetary and Space Sciences Research Institute [Milton Keynes] (PSSRI), Centre for Earth, Planetary, Space and Astronomical Research [Milton Keynes] (CEPSAR), Université libre de Bruxelles (ULB), NASA Ames Research Center (ARC), Laboratoire d'étude de la pollution atmospherique, Institut National de la Recherche Agronomique (INRA), California Institute of Technology (CALTECH), ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), NASA Goddard Space Flight Center (GSFC), University of Glasgow, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), McDonnell Center for Space Sciences, Washington University in St Louis, Department of Geological Sciences [Providence], Brown University, Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, International Research School of Planetary Sciences [Pescara] (IRSPS), Università degli studi 'G. d'Annunzio' Chieti-Pescara [Chieti-Pescara] (Ud'A), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), DLR Institute of Aerospace Medicine, Deutsches Zentrum für Luft- und Raumfahrt [Köln] (DLR), Max Planck Institute for Nuclear Physics (MPIK), Max-Planck-Gesellschaft, SP Technical Research Institute of Sweden, Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science [Washington], Geological Survey of Western Australia, 100 Plain Street, East Perth, WA 6004, Australia, Department of Geology, The Field Museum, Massachusetts Institute of Technology (MIT), Centre de géochimie de la surface (CGS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Conception, Ingénierie et Développement de l'Aliment et du Médicament (CIDAM), Université d'Auvergne - Clermont-Ferrand I (UdA), Université Libre de Bruxelles [Bruxelles] (ULB), Division of Geological and Planetary Sciences [Pasadena], Department of Earth, Ocean and Atmospheric Science [Tallahassee] (EOAS), Florida State University [Tallahassee] (FSU), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), RISE Research Institutes of Sweden, Centre National de la Recherche Scientifique (CNRS)-Université Louis Pasteur - Strasbourg I-Institut national des sciences de l'Univers (INSU - CNRS), Department of Earth, Ocean and Atmospheric Science [Tallahassee] (FSU | EOAS), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Washington University in Saint Louis (WUSTL), Carnegie Institution for Science, Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), International Mars Exploration Working Group, Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), California Institute of Technology (CALTECH)-NASA, Agence Spatiale Européenne = European Space Agency (ESA), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Laboratoire de Physico-Chimie de l'Atmosphère (LPCA), and Université du Littoral Côte d'Opale (ULCO)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Value (ethics), Engineering, GeneralLiterature_INTRODUCTORYANDSURVEY, Science and engineering, Mars, sample return, 010502 geochemistry & geophysics, Exploration of Mars, 01 natural sciences, Strahlenbiologie, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 0103 physical sciences, Géographie physique, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Martian, Mars sample return, business.industry, Environmental resource management, Mars Exploration Program, Sciences de l'espace, Geophysics, IMOST, [SDU]Sciences of the Universe [physics], Space and Planetary Science, [SDU.OTHER]Sciences of the Universe [physics]/Other, business
Abstract

Executive summary provided in lieu of abstract., SCOPUS: no.j, info:eu-repo/semantics/published

Published
2019
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16. The potential science and engineering value of samples delivered to Earth by Mars sample return: International MSR Objectives and Samples Team (iMOST)

Author

Beaty, D. W., Grady, M. M., McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., Hausrath, E. M., Herd, C. D.K., Horgan, B., Humayun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Schmitz, N., ten Kate, I. L., and Petrology

Subjects
Geophysics, Space and Planetary Science
Abstract

Return of samples from the surface of Mars has been a goal of the international Mars science community for many years. Affirmation by NASA and ESA of the importance of Mars exploration led the agencies to establish the international MSR Objectives and Samples Team (iMOST). The purpose of the team is to re-evaluate and update the sample-related science and engineering objectives of a Mars Sample Return (MSR) campaign. The iMOST team has also undertaken to define the measurements and the types of samples that can best address the objectives. Seven objectives have been defined for MSR, traceable through two decades of previously published international priorities. The first two objectives are further divided into sub-objectives. Within the main part of the report, the importance to science and/or engineering of each objective is described, critical measurements that would address the objectives are specified, and the kinds of samples that would be most likely to carry key information are identified. These seven objectives provide a framework for demonstrating how the first set of returned Martian samples would impact future Martian science and exploration. They also have implications for how analogous investigations might be conducted for samples returned by future missions from other solar system bodies, especially those that may harbor biologically relevant or sensitive material, such as Ocean Worlds (Europa, Enceladus, Titan) and others. Summary of Objectives and Sub-Objectives for MSR Identified by iMOST: Objective 1 Interpret the primary geologic processes and history that formed the Martian geologic record, with an emphasis on the role of water. Intent To investigate the geologic environment(s) represented at the Mars 2020 landing site, provide definitive geologic context for collected samples, and detail any characteristics that might relate to past biologic processesThis objective is divided into five sub-objectives that would apply at different landing sites. 1.1 Characterize the essential stratigraphic, sedimentologic, and facies variations of a sequence of Martian sedimentary rocks. Intent To understand the preserved Martian sedimentary record. Samples A suite of sedimentary rocks that span the range of variation. Importance Basic inputs into the history of water, climate change, and the possibility of life 1.2 Understand an ancient Martian hydrothermal system through study of its mineralization products and morphological expression. Intent To evaluate at least one potentially life-bearing “habitable” environment Samples A suite of rocks formed and/or altered by hydrothermal fluids. Importance Identification of a potentially habitable geochemical environment with high preservation potential. 1.3 Understand the rocks and minerals representative of a deep subsurface groundwater environment. Intent To evaluate definitively the role of water in the subsurface. Samples Suites of rocks/veins representing water/rock interaction in the subsurface. Importance May constitute the longest-lived habitable environments and a key to the hydrologic cycle. 1.4 Understand water/rock/atmosphere interactions at the Martian surface and how they have changed with time. Intent To constrain time-variable factors necessary to preserve records of microbial life. Samples Regolith, paleosols, and evaporites. Importance Subaerial near-surface processes could support and preserve microbial life. 1.5 Determine the petrogenesis of Martian igneous rocks in time and space. Intent To provide definitive characterization of igneous rocks on Mars. Samples Diverse suites of ancient igneous rocks. Importance Thermochemical record of the planet and nature of the interior. Objective 2 Assess and interpret the potential biological history of Mars, including assaying returned samples for the evidence of life. Intent To investigate the nature and extent of Martian habitability, the conditions and processes that supported or challenged life, how different environments might have influenced the preservation of biosignatures and created nonbiological “mimics,” and to look for biosignatures of past or present life.This objective has three sub-objectives: 2.1 Assess and characterize carbon, including possible organic and pre-biotic chemistry. Samples All samples collected as part of Objective 1. Importance Any biologic molecular scaffolding on Mars would likely be carbon-based. 2.2 Assay for the presence of biosignatures of past life at sites that hosted habitable environments and could have preserved any biosignatures. Samples All samples collected as part of Objective 1. Importance Provides the means of discovering ancient life. 2.3 Assess the possibility that any life forms detected are alive, or were recently alive. Samples All samples collected as part of Objective 1. Importance Planetary protection, and arguably the most important scientific discovery possible. Objective 3 Quantitatively determine the evolutionary timeline of Mars. Intent To provide a radioisotope-based time scale for major events, including magmatic, tectonic, fluvial, and impact events, and the formation of major sedimentary deposits and geomorphological features. Samples Ancient igneous rocks that bound critical stratigraphic intervals or correlate with crater-dated surfaces. Importance Quantification of Martian geologic history. Objective 4 Constrain the inventory of Martian volatiles as a function of geologic time and determine the ways in which these volatiles have interacted with Mars as a geologic system. Intent To recognize and quantify the major roles that volatiles (in the atmosphere and in the hydrosphere) play in Martian geologic and possibly biologic evolution. Samples Current atmospheric gas, ancient atmospheric gas trapped in older rocks, and minerals that equilibrated with the ancient atmosphere. Importance Key to understanding climate and environmental evolution. Objective 5 Reconstruct the processes that have affected the origin and modification of the interior, including the crust, mantle, core and the evolution of the Martian dynamo. Intent To quantify processes that have shaped the planet's crust and underlying structure, including planetary differentiation, core segregation and state of the magnetic dynamo, and cratering. Samples Igneous, potentially magnetized rocks (both igneous and sedimentary) and impact-generated samples. Importance Elucidate fundamental processes for comparative planetology. Objective 6 Understand and quantify the potential Martian environmental hazards to future human exploration and the terrestrial biosphere. Intent To define and mitigate an array of health risks related to the Martian environment associated with the potential future human exploration of Mars. Samples Fine-grained dust and regolith samples. Importance Key input to planetary protection planning and astronaut health. Objective 7 Evaluate the type and distribution of in-situ resources to support potential future Mars exploration. Intent To quantify the potential for obtaining Martian resources, including use of Martian materials as a source of water for human consumption, fuel production, building fabrication, and agriculture. Samples Regolith. Importance Production of simulants that will facilitate long-term human presence on Mars. Summary of iMOST Findings: Several specific findings were identified during the iMOST study. While they are not explicit recommendations, we suggest that they should serve as guidelines for future decision making regarding planning of potential future MSR missions. The samples to be collected by the Mars 2020 (M-2020) rover will be of sufficient size and quality to address and solve a wide variety of scientific questions. Samples, by definition, are a statistical representation of a larger entity. Our ability to interpret the source geologic units and processes by studying sample sub sets is highly dependent on the quality of the sample context. In the case of the M-2020 samples, the context is expected to be excellent, and at multiple scales. (A) Regional and planetary context will be established by the on-going work of the multi-agency fleet of Mars orbiters. (B) Local context will be established at field area- to outcrop- to hand sample- to hand lens scale using the instruments carried by M-2020. A significant fraction of the value of the MSR sample collection would come from its organization into sample suites, which are small groupings of samples designed to represent key aspects of geologic or geochemical variation. If the Mars 2020 rover acquires a scientifically well-chosen set of samples, with sufficient geological diversity, and if those samples were returned to Earth, then major progress can be expected on all seven of the objectives proposed in this study, regardless of the final choice of landing site. The specifics of which parts of Objective 1 could be achieved would be different at each of the final three candidate landing sites, but some combination of critically important progress could be made at any of them. An aspect of the search for evidence of life is that we do not know in advance how evidence for Martian life would be preserved in the geologic record. In order for the returned samples to be most useful for both understanding geologic processes (Objective 1) and the search for life (Objective 2), the sample collection should contain BOTH typical and unusual samples from the rock units explored. This consideration should be incorporated into sample selection and the design of the suites. The retrieval missions of a MSR campaign should (1) minimize stray magnetic fields to which the samples would be exposed and carry a magnetic witness plate to record exposure, (2) collect and return atmospheric gas sample(s), and (3) collect additional dust and/or regolith sample mass if possible.

Published
2019

17. The potential science and engineering value of samples delivered to Earth by Mars sample return: International MSR Objectives and Samples Team (iMOST)

Author

Petrology, Beaty, D. W., Grady, M. M., McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., Hausrath, E. M., Herd, C. D.K., Horgan, B., Humayun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Schmitz, N., ten Kate, I. L., Petrology, Beaty, D. W., Grady, M. M., McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., Hausrath, E. M., Herd, C. D.K., Horgan, B., Humayun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Schmitz, N., and ten Kate, I. L.

Published
2019

18. The Potential Science and Engineering Value of Samples Delivered to Earth by Mars Sample Return - Final Report (white paper)

Author

International MSR Objectives and Samples Team, iMOST, Beaty, D. W., Grady, M. M., McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., Hausrath, E. M., Herd, C. D. K., Horgan, B., Humayun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, Petra, Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Shuster, D. L., Siljeström, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., Zorzano, M. P., co-chair: Beaty, D. W., co-chair: Grady, M. M., co-chair: McSween, H. Y., co-chair: Sefton-Nash, E., documentarian: Carrier, B.L., and plus 66 co-authors, .

Subjects
Strahlenbiologie, Mars sample return, iMOST
Abstract

Executive Summary: Return of samples from the surface of Mars has been a goal of the international Mars science community for many years. Affirmation by NASA and ESA of the importance of Mars exploration led the agencies to establish the international MSR Objectives and Samples Team (iMOST). The purpose of the team is to re-evaluate and update the sample-related science and engineering objectives of a Mars Sample Return (MSR) campaign. The iMOST team has also undertaken to define the measurements and the types of samples that can best address the objectives. Seven objectives have been defined for MSR, traceable through two decades of previously published international priorities. The first two objectives are further divided into sub-objectives. Within the main part of the report, the importance to science and/or engineering of each objective is described, critical measurements that would address the objectives are specified, and the kinds of samples that would be most likely to carry key information are identified. These seven objectives provide a framework for demonstrating how the first set of returned martian samples would impact future martian science and exploration. They also have implications for how analogous investigations might be conducted for samples returned by future missions from other solar system bodies, especially those that may harbor biologically relevant or sensitive material, such as Ocean Worlds (Europa, Enceladus, Titan) and others.

Published
2018

19. Designing remote operations strategies to optimize science mission goals: Lessons learned from the Moon Mars Analog Mission Activities Mauna Kea 2012 field test

Author

Yingst, R. A., Russell, P., Ten Kate, I. L., Noble, S., Graff, T., Graham, L. D., Eppler, D., Petrology, and Petrology

Subjects
Engineering, Traverse, Apollo Valley geologic map, business.industry, Aerospace Engineering, Mars Exploration Program, Plan (drawing), Field (computer science), Concept of operations, Test (assessment), Data flow diagram, Science operations, MER, Systems engineering, Instrumentation (computer programming), Aerospace engineering, business
Abstract

The Moon Mars Analog Mission Activities Mauna Kea 2012 (MMAMA 2012) field campaign aimed to assess how effectively an integrated science and engineering rover team operating on a 24-h planning cycle facilitates high-fidelity science products. The science driver of this field campaign was to determine the origin of a glacially-derived deposit: was the deposit the result of (1) glacial outwash from meltwater; or (2) the result of an ice dam breach at the head of the valley? Lessons learned from MMAMA 2012 science operations include: (1) current rover science operations scenarios tested in this environment provide adequate data to yield accurate derivative products such as geologic maps; (2) instrumentation should be selected based on both engineering and science goals; and chosen during, rather than after, mission definition; and (3) paralleling the tactical and strategic science processes provides significant efficiencies that impact science return. The MER-model concept of operations utilized, in which rover operators were sufficiently facile with science intent to alter traverse and sampling plans during plan execution, increased science efficiency, gave the Science Backroom time to develop mature hypotheses and science rationales, and partially alleviated the problem of data flow being greater than the processing speed of the scientists.

Published
2015
Full Text
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22. Laboratory spectroscopy and astronomical significance of the fully-benzenoid PAH triphenylene and its cation

Author

Kofman, V., Sarre, P. J., Hibbins, R. E., ten Kate, I. L., Linnartz, H., Kofman, V., Sarre, P. J., Hibbins, R. E., ten Kate, I. L., and Linnartz, H.

Abstract

Triphenylene (C18H12) is a highly symmetric polycyclic aromatic hydrocarbon (PAH) molecule with a ‘fully-benzenoid’ electronic structure. This confers a high chemical stability compared with PAHs of similar size. Although numerous infrared and UV-vis experimental spectroscopic and theoretical studies of a wide range PAHs in an astrophysical context have been conducted, triphenylene and its radical cation have received almost no attention. There exists a huge body of spectroscopic evidence for neutral and ionised PAHs in astrophysical sources, obtained principally through detection of infrared emission features that are characteristic of PAHs as a chemical class. However, it has so far not proved possible to identify spectroscopically a single isolated PAH in space, although PAHs including triphenylene have been detected mass spectrometrically in meteorites. In this work we focus on recording laboratory electronic spectra of neutral and ionised triphenylene between 220 and 780 nm, trapped in H2O ice and solid argon at 12 K. The studies are motivated by the potential for spectroscopic astronomical detection of electronic absorption spectra of PAHs in ice mantles on interstellar grains as discussed by Linnartz (2014), and were performed also in a cold Ar matrix to provide guidance as to whether triphenylene (particularly in its singly positively ionised form) could be a viable candidate for any of the unidentified diffuse interstellar absorption bands. Based on the argon-matrix experimental results, comparison is made with previously unpublished astronomical spectra near 400 nm which contain broad interstellar absorption features consistent with the predictions from the laboratory matrix spectra, thus providing motivation for the recording of gas-phase electronic spectra of the internally cold triphenylene cation.

Published
2017

24. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars

Author

Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Miller, Kristen, Summons, Roger E, Freissinet, C., Glavin, D. P., Mahaffy, P. R., Eigenbrode, J. L., Brunner, A. E., Buch, A., Szopa, C., Archer, P. D., Franz, H. B., Atreya, S. K., Brinckerhoff, W. B., Cabane, M., Coll, P., Conrad, P. G., Des Marais, D. J., Dworkin, J. P., Fairén, A. G., François, P., Grotzinger, J. P., Kashyap, S., ten Kate, I. L., Leshin, L. A., Malespin, C. A., Martin, M. G., Martin-Torres, F. J., McAdam, A. C., Ming, D. W., Navarro-González, R., Pavlov, A. A., Prats, B. D., Squyres, S. W., Steele, A., Stern, J. C., Sumner, D. Y., Sutter, B., Zorzano, M.-P., Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Miller, Kristen, Summons, Roger E, Freissinet, C., Glavin, D. P., Mahaffy, P. R., Eigenbrode, J. L., Brunner, A. E., Buch, A., Szopa, C., Archer, P. D., Franz, H. B., Atreya, S. K., Brinckerhoff, W. B., Cabane, M., Coll, P., Conrad, P. G., Des Marais, D. J., Dworkin, J. P., Fairén, A. G., François, P., Grotzinger, J. P., Kashyap, S., ten Kate, I. L., Leshin, L. A., Malespin, C. A., Martin, M. G., Martin-Torres, F. J., McAdam, A. C., Ming, D. W., Navarro-González, R., Pavlov, A. A., Prats, B. D., Squyres, S. W., Steele, A., Stern, J. C., Sumner, D. Y., Sutter, B., and Zorzano, M.-P.

Abstract

The 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.

Published
2017

25. Boundary conditions for the formation of the Moon

Author

Reuver, Maarten, de Meijer, R. J., ten Kate, I. L., van Westrenen, W., Petrology, Earth Sciences, Geology and Geochemistry, and Petrology

Subjects
Angular momentum, Work (thermodynamics), 010504 meteorology & atmospheric sciences, 010502 geochemistry & geophysics, angular momentum, 01 natural sciences, Physics::Geophysics, Total angular momentum quantum number, Boundary value problem, rotation frequency, 0105 earth and related environmental sciences, Giant impact hypothesis, Computer Science::Information Retrieval, Earth–Moon system, Geology, Geophysics, Moment of inertia, Computational physics, oblateness, Moon formation, Magnetic field of the Moon, Roche limit, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract

Recent measurements of the chemical and isotopic composition of lunar samples indicate that the Moon's bulk composition shows great similarities with the composition of the silicate Earth. Moon formation models that attempt to explain these similarities make a wide variety of assumptions about the properties of the Earth prior to the formation of the Moon (the proto-Earth), and about the necessity and properties of an impactor colliding with the proto-Earth. This paper investigates the effects of the proto-Earth's mass, oblateness and internal core-mantle differentiation on its moment of inertia. The ratio of angular momentum and moment of inertia determines the stability of the proto-Earth and the binding energy, i.e. the energy needed to make the transition from an initial state in which the system is a rotating single body with a certain angular momentum to a final state with two bodies (Earth and Moon) with the same total angular momentum, redistributed between Earth and Moon. For the initial state two scenarios are being investigated: a homogeneous (undifferentiated) proto-Earth and a proto-Earth differentiated in a central metallic and an outer silicate shell; for both scenarios a range of oblateness values is investigated. Calculations indicate that a differentiated proto-Earth would become unstable at an angular momentum L that exceeds the total angular momentum of the present-day Earth–Moon system (L0) by factors of 2.5–2.9, with the precise maximum dependent on the proto-Earth's oblateness. Further limitations are imposed by the Roche limit and the logical condition that the separated Earth–Moon system should be formed outside the proto-Earth. This further limits the L values of the Earth–Moon system to a maximum of about L/L0 = 1.5, at a minimum oblateness (a/c ratio) of 1.2. These calculations provide boundary conditions for the main classes of Moon-forming models. Our results show that at the high values of L used in recent giant impact models (1.8 < L/L0 < 3.1), the proposed proto-Earths are unstable before (Cuk & Stewart, 2012) or immediately after (Canup, 2012) the impact, even at a high oblateness (the most favourable condition for stability). We conclude that the recent attempts to improve the classic giant impact hypothesis by studying systems with very high values of L are not supported by the boundary condition calculations in this work. In contrast, this work indicates that the nuclear explosion model for Moon formation (De Meijer et al., 2013) fulfills the boundary conditions and requires approximately one order of magnitude less energy than originally estimated. Hence in our view the nuclear explosion model is presently the model that best explains the formation of the Moon from predominantly terrestrial silicate material.

Published
2016
Full Text
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26. Organic compounds of th Pueblito de Allende meteorite

Author

Visser, R., ten Kate, I. L (Thesis Advisor), King, H, Visser, R., ten Kate, I. L (Thesis Advisor), and King, H

Abstract

The CV3 Pueblito de Allende meteorite is used to test new in situ methods to identify organic compounds. These methods can potentially be a good alternative to avoid the difficult extraction methods, reducing the risk of losing organic molecules and contaminating the samples with terrestrial organics. The distribution, formation, and characteristics of the organic compounds of the Pueblito de Allende meteorite are studied by Electron MicroProbe (EMP), Raman spectroscopy and Surface Enhanced Raman Spectroscopy (SERS) and nuclear magnetic resonance (NMR). Elemental maps, spot analysis and Raman measurements show the heterogeneous distribution of organic compounds in the matrix and chondrules. The G- and D-bands are used to reveal the differences between the thermally stressed organics of Allende and the relative unaltered organics of other CV3 chondrites. The SERS method, where synthesized silver nanoparticles are added to the surface of minerals have an enhancement effect (~106) on organics, is used to show that this method works when the organics are added to the minerals in thin film. This study shows that the enhancements effects on the intensities of the organics are dramatically reduced when the silver colloids are used to determine the organic compounds imbedded in the matrix. The G- and D-band are enhanced slightly (101-102), but no other organic compounds could be detected. The addition of chloride ions used to stabilize the silver particles decreases the enhancements effects even more.

Published
2016

28. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars

Author

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

Abstract

The 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 70ppbw) 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.

Published
2015

30. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars

Author

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

Published
2015

31. Martian fluvial conglomerates at gale crater

Author

Williams, R. M. E., Grotzinger, J. P., Dietrich, W. E., Gupta, S., Sumner, D. Y., Wiens, R. C., Mangold, N., Malin, M. C., Edgett, K. S., Maurice, S., Forni, O., Gasnault, O., Ollila, A., Newsom, H. E., Dromart, G., Palucis, M. C., Yingst, R. A., Anderson, R. B., Herkenhoff, K. E., Le Mouelic, S., Goetz, W., Madsen, M. B., Koefoed, A., Jensen, J. K., Bridges, J. C., Schwenzer, S. P., Lewis, K. W., Stack, K. M., Rubin, D., Kah, L. C., Bell, J. F., Farmer, J. D., Sullivan, R., Van Beek, T., Blaney, D. L., Pariser, O., Deen, R. G., Kemppinen, O., Bridges, N., Johnson, J. R., Minitti, M., Cremers, D., Edgar, L., Godber, A., Wadhwa, M., Wellington, D., McEwan, I., Newman, C., Richardson, M., Charpentier, A., Peret, L., King, P., Blank, J., Weigle, G., Schmidt, M., Li, S., Milliken, R., Robertson, K., Sun, V., Baker, M., Edwards, C., Ehlmann, B., Farley, K., Griffes, J., Miller, H., Newcombe, M., Pilorget, C., Rice, M., Siebach, K., Stolper, E., Brunet, C., Hipkin, V., Leveille, R., Marchand, G., Sobron Sanchez, P., Favot, L., Cody, G., Steele, A., Fluckiger, L., Lees, D., Nefian, A., Martin, M., Gailhanou, M., Westall, F., Israel, G., Agard, C., Baroukh, J., Donny, C., Gaboriaud, A., Guillemot, P., Lafaille, V., Lorigny, E., Paillet, A., Perez, R., Saccoccio, M., Yana, C., Aparicio, C. A., Caride Rodriguez, J., Carrasco Blazquez, I., Gomez Gomez, F., Elvira, J. G., Hettrich, S., Lepinette Malvitte, A., Marin Jimenez, M., Frias, J. M., Soler, J. M., Torres, F. J. M., Molina Jurado, A., Sotomayor, L. M., Munoz Caro, G., Navarro Lopez, S., Gonzalez, V. P., Garcia, J. P., Rodriguez Manfredi, J. A., Planello, J. J. R., Alejandra Sans Fuentes, S., Sebastian Martinez, E., Torres Redondo, J., O'Callaghan, R. U., Zorzano Mier, M.-P., Chipera, S., Lacour, J.-L., Mauchien, P., Sirven, J.-B., Manning, H., Fairen, A., Hayes, A., Joseph, J., Squyres, S., Thomas, P., Dupont, A., Lundberg, A., Melikechi, N., Mezzacappa, A., DeMarines, J., Grinspoon, D., Reitz, G., Prats, B., Atlaskin, E., Genzer, M., Harri, A.-M., Haukka, H., Kahanpaa, H., Kauhanen, J., Paton, M., Polkko, J., Schmidt, W., Siili, T., Fabre, C., Wray, J., Wilhelm, M. B., Poitrasson, F., Patel, K., Gorevan, S., Indyk, S., Paulsen, G., Bish, D., Schieber, J., Gondet, B., Langevin, Y., Geffroy, C., Baratoux, D., Berger, G., Cros, A., Uston, C. d., Lasue, J., Lee, Q.-M., Meslin, P.-Y., Pallier, E., Parot, Y., Pinet, P., Schroder, S., Toplis, M., Lewin, E., Brunner, W., Heydari, E., Achilles, C., Oehler, D., Sutter, B., Cabane, M., Coscia, D., Szopa, C., Robert, F., Sautter, V., Nachon, M., Buch, A., Stalport, F., Coll, P., Francois, P., Raulin, F., Teinturier, S., Cameron, J., Clegg, S., Cousin, A., DeLapp, D., Dingler, R., Jackson, R. S., Johnstone, S., Lanza, N., Little, C., Nelson, T., Williams, R. B., Jones, A., Kirkland, L., Treiman, A., Baker, B., Cantor, B., Caplinger, M., Davis, S., Duston, B., Fay, D., Hardgrove, C., Harker, D., Herrera, P., Jensen, E., Kennedy, M. R., Krezoski, G., Krysak, D., Lipkaman, L., McCartney, E., McNair, S., Nixon, B., Posiolova, L., Ravine, M., Salamon, A., Saper, L., Stoiber, K., Supulver, K., Van Beek, J., Zimdar, R., French, K. L., Iagnemma, K., Miller, K., Summons, R., Goesmann, F., Hviid, S., Johnson, M., Lefavor, M., Lyness, E., Breves, E., Dyar, M. D., Fassett, C., Blake, D. F., Bristow, T., DesMarais, D., Edwards, L., Haberle, R., Hoehler, T., Hollingsworth, J., Kahre, M., Keely, L., McKay, C., Bleacher, L., Brinckerhoff, W., Choi, D., Conrad, P., Dworkin, J. P., Eigenbrode, J., Floyd, M., Freissinet, C., Garvin, J., Glavin, D., Harpold, D., Mahaffy, P., Martin, D. K., McAdam, A., Pavlov, A., Raaen, E., Smith, M. D., Stern, J., Tan, F., Trainer, M., Meyer, M., Posner, A., Voytek, M., Anderson, R. C., Aubrey, A., Beegle, L. W., Behar, A., Brinza, D., Calef, F., Christensen, L., Crisp, J. A., DeFlores, L., Feldman, J., Feldman, S., Flesch, G., Hurowitz, J., Jun, I., Keymeulen, D., Maki, J., Mischna, M., Morookian, J. M., Parker, T., Pavri, B., Schoppers, M., Sengstacken, A., Simmonds, J. J., Spanovich, N., de la Torre Juarez, M., Vasavada, A. R., Webster, C. R., Yen, A., Archer, P. D., Cucinotta, F., Jones, J. H., Ming, D., Morris, R. V., Niles, P., Rampe, E., Nolan, T., Fisk, M., Radziemski, L., Barraclough, B., Bender, S., Berman, D., Dobrea, E. N., Tokar, R., Vaniman, D., Leshin, L., Cleghorn, T., Huntress, W., Manhes, G., Hudgins, J., Olson, T., Stewart, N., Sarrazin, P., Grant, J., Vicenzi, E., Wilson, S. A., Bullock, M., Ehresmann, B., Hamilton, V., Hassler, D., Peterson, J., Rafkin, S., Zeitlin, C., Fedosov, F., Golovin, D., Karpushkina, N., Kozyrev, A., Litvak, M., Malakhov, A., Mitrofanov, I., Mokrousov, M., Nikiforov, S., Prokhorov, V., Sanin, A., Tretyakov, V., Varenikov, A., Vostrukhin, A., Kuzmin, R., Clark, B., Wolff, M., McLennan, S., Botta, O., Drake, D., Bean, K., Lemmon, M., Lee, E. M., Sucharski, R., Hernandez, M. A. d. P., Blanco Avalos, J. J., Ramos, M., Kim, M.-H., Malespin, C., Plante, I., Muller, J.-P., Gonzalez, R. N., Ewing, R., Boynton, W., Downs, R., Fitzgibbon, M., Harshman, K., Morrison, S., Kortmann, O., Williams, A., Lugmair, G., Wilson, M. A., Jakosky, B., Zunic, T. B., Frydenvang, J., Kinch, K., Stipp, S. L. S., Boyd, N., Campbell, J. L., Gellert, R., Perrett, G., Pradler, I., VanBommel, S., Jacob, S., Owen, T., Rowland, S., Savijarvi, H., Boehm, E., Bottcher, S., Burmeister, S., Guo, J., Kohler, J., Garcia, C. M., Mellin, R. M., Schweingruber, R. W., McConnochie, T., Benna, M., Franz, H., Bower, H., Brunner, A., Blau, H., Boucher, T., Carmosino, M., Atreya, S., Elliott, H., Halleaux, D., Renno, N., Wong, M., Pepin, R., Elliott, B., Spray, J., Thompson, L., Gordon, S., Williams, J., Vasconcelos, P., Bentz, J., Nealson, K., Popa, R., Moersch, J., Tate, C., Day, M., Kocurek, G., Hallet, B., Sletten, R., Francis, R., McCullough, E., Cloutis, E., ten Kate, I. L., Arvidson, R., Fraeman, A., Scholes, D., Slavney, S., Stein, T., Ward, J., Berger, J., Moores, J. E., NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, GeoRessources, and Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
MSL Mars Gale Crater Fluvial Activity, Martian, Multidisciplinary, 010504 meteorology & atmospheric sciences, Outcrop, Curiosity rover, Geochemistry, Mars, Sediment, Fluvial, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Mars Exploration Program, 01 natural sciences, Abrasion (geology), martian fluvial conglomerates, 13. Climate action, Rocknest, 0103 physical sciences, MSL, Sedimentary rock, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

Going to Mars The Mars Science Laboratory spacecraft containing the Curiosity rover, was launched from Earth in November 2011 and arrived at Gale crater on Mars in August 2012. Zeitlin et al. (p. 1080 ) report measurements of the energetic particle radiation environment inside the spacecraft during its cruise to Mars, confirming the hazard likely to be posed by this radiation to astronauts on a future potential trip to Mars. Williams et al. (p. 1068 , see the Perspective by Jerolmack ) report the detection of sedimentary conglomerates (pebbles mixed with sand and turned to rock) at Gale crater. The rounding of the rocks suggests abrasion of the pebbles as they were transported by flowing water several kilometers or more from their source.

Published
2013
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32. Abundance and isotopic composition of gases in the martian atmosphere from the Curiosity rover

Author

Mahaffy, P. R., Webster, C. R., Atreya, S. K., Franz, H., Wong, M., Conrad, P. G., Harpold, D., Jones, J. J., Leshin, L. A., Manning, H., Owen, T., Pepin, R. O., Squyres, S., Trainer, M., Kemppinen, O., Bridges, N., Johnson, J. R., Minitti, M., Cremers, D., Bell, J. F., Edgar, L., Farmer, J., Godber, A., Wadhwa, M., Wellington, D., McEwan, I., Newman, C., Richardson, M., Charpentier, A., Peret, L., King, P., Blank, J., Weigle, G., Schmidt, M., Li, S., Milliken, R., Robertson, K., Sun, V., Baker, M., Edwards, C., Ehlmann, B., Farley, K., Griffes, J., Grotzinger, J., Miller, H., Newcombe, M., Pilorget, C., Rice, M., Siebach, K., Stack, K., Stolper, E., Brunet, C., Hipkin, V., Leveille, R., Marchand, G., Sanchez, P. S., Favot, L., Cody, G., Steele, A., Fluckiger, L., Lees, D., Nefian, A., Martin, M., Gailhanou, M., Westall, F., Israel, G., Agard, C., Baroukh, J., Donny, C., Gaboriaud, A., Guillemot, P., Lafaille, V., Lorigny, E., Paillet, A., Perez, R., Saccoccio, M., Yana, C., Armiens-Aparicio, C., Rodriguez, J. C., Blazquez, I. C., Gomez, F. G., Gomez-Elvira, J., Hettrich, S., Malvitte, A. L., Jimenez, M. M., Martinez-Frias, J., Martin-Soler, J., Martin-Torres, F. J., Jurado, A. M., Mora-Sotomayor, L., Caro, G. M., Lopez, S. N., Peinado-Gonzalez, V., Pla-Garcia, J., Manfredi, J. A. R., Romeral-Planello, J. J., Fuentes, S. A. S., Martinez, E. S., Redondo, J. T., Urqui-O'Callaghan, R., Mier, M.-P. Z., Chipera, S., Lacour, J.-L., Mauchien, P., Sirven, J.-B., Fairen, A., Hayes, A., Joseph, J., Sullivan, R., Thomas, P., Dupont, A., Lundberg, A., Melikechi, N., Mezzacappa, A., DeMarines, J., Grinspoon, D., Reitz, G., Prats, B., Atlaskin, E., Genzer, M., Harri, A.-M., Haukka, H., Kahanpaa, H., Kauhanen, J., Paton, M., Polkko, J., Schmidt, W., Siili, T., Fabre, C., Wray, J., Wilhelm, M. B., Poitrasson, F., Patel, K., Gorevan, S., Indyk, S., Paulsen, G., Gupta, S., Bish, D., Schieber, J., Gondet, B., Langevin, Y., Geffroy, C., Baratoux, D., Berger, G., Cros, A., d'Uston, C., Forni, O., Gasnault, O., Lasue, J., Lee, Q.-M., Maurice, S., Meslin, P.-Y., Pallier, E., Parot, Y., Pinet, P., Schroder, S., Toplis, M., Lewin, E., Brunner, W., Heydari, E., Achilles, C., Oehler, D., Sutter, B., Cabane, M., Coscia, D., Szopa, C., Dromart, G., Robert, F., Sautter, V., Le Mouelic, S., Mangold, N., Nachon, M., Buch, A., Stalport, F., Coll, P., Francois, P., Raulin, F., Teinturier, S., Cameron, J., Clegg, S., Cousin, A., DeLapp, D., Dingler, R., Jackson, R. S., Johnstone, S., Lanza, N., Little, C., Nelson, T., Wiens, R. C., Williams, R. B., Jones, A., Kirkland, L., Treiman, A., Baker, B., Cantor, B., Caplinger, M., Davis, S., Duston, B., Edgett, K., Fay, D., Hardgrove, C., Harker, D., Herrera, P., Jensen, E., Kennedy, M. R., Krezoski, G., Krysak, D., Lipkaman, L., Malin, M., McCartney, E., McNair, S., Nixon, B., Posiolova, L., Ravine, M., Salamon, A., Saper, L., Stoiber, K., Supulver, K., Van Beek, J., Van Beek, T., Zimdar, R., French, K. L., Iagnemma, K., Miller, K., Summons, R., Goesmann, F., Goetz, W., Hviid, S., Johnson, M., Lefavor, M., Lyness, E., Breves, E., Dyar, M. D., Fassett, C., Blake, D. F., Bristow, T., DesMarais, D., Edwards, L., Haberle, R., Hoehler, T., Hollingsworth, J., Kahre, M., Keely, L., McKay, C., Bleacher, L., Brinckerhoff, W., Choi, D., Dworkin, J. P., Eigenbrode, J., Floyd, M., Freissinet, C., Garvin, J., Glavin, D., Martin, D. K., McAdam, A., Pavlov, A., Raaen, E., Smith, M. D., Stern, J., Tan, F., Meyer, M., Posner, A., Voytek, M., Anderson, R. C., Aubrey, A., Beegle, L. W., Behar, A., Blaney, D., Brinza, D., Calef, F., Christensen, L., Crisp, J. A., DeFlores, L., Feldman, J., Feldman, S., Flesch, G., Hurowitz, J., Jun, I., Keymeulen, D., Maki, J., Mischna, M., Morookian, J. M., Parker, T., Pavri, B., Schoppers, M., Sengstacken, A., Simmonds, J. J., Spanovich, N., Juarez, M. d. l. T., Vasavada, A. R., Yen, A., Archer, P. D., Cucinotta, F., Ming, D., Morris, R. V., Niles, P., Rampe, E., Nolan, T., Fisk, M., Radziemski, L., Barraclough, B., Bender, S., Berman, D., Dobrea, E. N., Tokar, R., Vaniman, D., Williams, R. M. E., Yingst, A., Lewis, K., Cleghorn, T., Huntress, W., Manhes, G., Hudgins, J., Olson, T., Stewart, N., Sarrazin, P., Grant, J., Vicenzi, E., Wilson, S. A., Bullock, M., Ehresmann, B., Hamilton, V., Hassler, D., Peterson, J., Rafkin, S., Zeitlin, C., Fedosov, F., Golovin, D., Karpushkina, N., Kozyrev, A., Litvak, M., Malakhov, A., Mitrofanov, I., Mokrousov, M., Nikiforov, S., Prokhorov, V., Sanin, A., Tretyakov, V., Varenikov, A., Vostrukhin, A., Kuzmin, R., Clark, B., Wolff, M., McLennan, S., Botta, O., Drake, D., Bean, K., Lemmon, M., Schwenzer, S. P., Anderson, R. B., Herkenhoff, K., Lee, E. M., Sucharski, R., Hernandez, M. A. d. P., Avalos, J. J. B., Ramos, M., Kim, M.-H., Malespin, C., Plante, I., Muller, J.-P., Navarro-Gonzalez, R., Ewing, R., Boynton, W., Downs, R., Fitzgibbon, M., Harshman, K., Morrison, S., Dietrich, W., Kortmann, O., Palucis, M., Sumner, D. Y., Williams, A., Lugmair, G., Wilson, M. A., Rubin, D., Jakosky, B., Balic-Zunic, T., Frydenvang, J., Jensen, J. K., Kinch, K., Koefoed, A., Madsen, M. B., Stipp, S. L. S., Boyd, N., Campbell, J. L., Gellert, R., Perrett, G., Pradler, I., VanBommel, S., Jacob, S., Rowland, S., Savijarvi, H., Boehm, E., Bottcher, S., Burmeister, S., Guo, J., Kohler, J., Garcia, C. M., Mueller-Mellin, R., Wimmer-Schweingruber, R., Bridges, J. C., McConnochie, T., Benna, M., Bower, H., Brunner, A., Blau, H., Boucher, T., Carmosino, M., Elliott, H., Halleaux, D., Renno, N., Elliott, B., Spray, J., Thompson, L., Gordon, S., Newsom, H., Ollila, A., Williams, J., Vasconcelos, P., Bentz, J., Nealson, K., Popa, R., Kah, L. C., Moersch, J., Tate, C., Day, M., Kocurek, G., Hallet, B., Sletten, R., Francis, R., McCullough, E., Cloutis, E., ten Kate, I. L., Arvidson, R., Fraeman, A., Scholes, D., Slavney, S., Stein, T., Ward, J., Berger, J., Moores, J. E., GeoRessources, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), MSL Science Team, NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, and Petrology

Subjects
010504 meteorology & atmospheric sciences, Curiosity rover, chemistry.chemical_element, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Mars, MSL Mars Atmosphere Isotopis Composition, martian atmosphere, 01 natural sciences, Astrobiology, Isotopic signature, chemistry.chemical_compound, 0103 physical sciences, MSL, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Martian, Multidisciplinary, δ13C, Atmosphere of Mars, Nitrogen, chemistry, 13. Climate action, Sample Analysis at Mars, Carbon dioxide, Environmental science, Carbon monoxide
Abstract

Mars' Atmosphere from Curiosity The Sample Analysis at Mars (SAM) instrument on the Curiosity rover that landed on Mars in August last year is designed to study the chemical and isotopic composition of the martian atmosphere. Mahaffy et al. (p. 263 ) present volume-mixing ratios of Mars' five major atmospheric constituents (CO 2 , Ar, N 2 , O 2 , and CO) and isotope measurements of 40 Ar/ 36 Ar and C and O in CO 2 , based on data from one of SAM's instruments, obtained between 31 August and 21 November 2012. Webster et al. (p. 260 ) used data from another of SAM's instruments obtained around the same period to determine isotope ratios of H, C, and O in atmospheric CO 2 and H 2 O. Agreement between the isotopic ratios measured by SAM with those of martian meteorites, measured in laboratories on Earth, confirms the origin of these meteorites and implies that the current atmospheric reservoirs of CO 2 and H 2 O were largely established after the period of early atmospheric loss some 4 billion years ago.

Published
2013
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33. Curiosity at Gale Crater, Mars: Characterization and analysis of the rocknest sand shadow

Author

Blake, D. F., Morris, R. V., Kocurek, G., Morrison, S. M., Downs, R. T., Bish, D., Ming, D. W., Edgett, K. S., Rubin, D., Goetz, W., Madsen, M. B., Sullivan, R., Gellert, R., Campbell, I., Treiman, A. H., McLennan, S. M., Yen, A. S., Grotzinger, J., Vaniman, D. T., Chipera, S. J., Achilles, C. N., Rampe, E. B., Sumner, D., Meslin, P.- Y., Maurice, S., Forni, O., Gasnault, O., Fisk, M., Schmidt, M., Mahaffy, P., Leshin, L. A., Glavin, D., Steele, A., Freissinet, C., Navarro-Gonzalez, R., Yingst, R. A., Kah, L. C., Bridges, N., Lewis, K. W., Bristow, T. F., Farmer, J. D., Crisp, J. A., Stolper, E. M., Des Marais, D. J., Sarrazin, P., Agard, C., Alves Verdasca, J. A., Anderson, R., Archer, D., Armiens-Aparicio, C., Arvidson, R., Atlaskin, E., Atreya, S., Aubrey, A., Baker, B., Baker, M., Balic-Zunic, T., Baratoux, D., Baroukh, J., Barraclough, B., Bean, K., Beegle, L., Behar, A., Bell, J., Bender, S., Benna, M., Bentz, J., Berger, G., Berger, J., Berman, D., Blanco Avalos, J. J., Blaney, D., Blank, J., Blau, H., Bleacher, L., Boehm, E., Botta, O., Bottcher, S., Boucher, T., Bower, H., Boyd, N., Boynton, B., Breves, E., Bridges, J., Brinckerhoff, W., Brinza, D., Brunet, C., Brunner, A., Brunner, W., Buch, A., Bullock, M., Burmeister, S., Cabane, M., Calef, F., Cameron, J., Cantor, B., Caplinger, M., Rodriguez, J. C., Carmosino, M., Blazquez, I. C., Charpentier, A., Choi, D., Clark, B., Clegg, S., Cleghorn, T., Cloutis, E., Cody, G., Coll, P., Conrad, P., Coscia, D., Cousin, A., Cremers, D., Cros, A., Cucinotta, F., d'Uston, C., Davis, S., Day, M., Juarez, M. d. l. T., DeFlores, L., DeLapp, D., DeMarines, J., Dietrich, W., Dingler, R., Donny, C., Drake, D., Dromart, G., Dupont, A., Duston, B., Dworkin, J., Dyar, M. D., Edgar, L., Edwards, C., Edwards, L., Ehlmann, B., Ehresmann, B., Eigenbrode, J., Elliott, B., Elliott, H., Ewing, R., Fabre, C., Fairen, A., Farley, K., Fassett, C., Favot, L., Fay, D., Fedosov, F., Feldman, J., Feldman, S., Fitzgibbon, M., Flesch, G., Floyd, M., Fluckiger, L., Fraeman, A., Francis, R., Francois, P., Franz, H., French, K. L., Frydenvang, J., Gaboriaud, A., Gailhanou, M., Garvin, J., Geffroy, C., Genzer, M., Godber, A., Goesmann, F., Golovin, D., Gomez, F. G., Gomez-Elvira, J., Gondet, B., Gordon, S., Gorevan, S., Grant, J., Griffes, J., Grinspoon, D., Guillemot, P., Guo, J., Gupta, S., Guzewich, S., Haberle, R., Halleaux, D., Hallet, B., Hamilton, V., Hardgrove, C., Harker, D., Harpold, D., Harri, A.-M., Harshman, K., Hassler, D., Haukka, H., Hayes, A., Herkenhoff, K., Herrera, P., Hettrich, S., Heydari, E., Hipkin, V., Hoehler, T., Hollingsworth, J., Hudgins, J., Huntress, W., Hurowitz, J., Hviid, S., Iagnemma, K., Indyk, S., Israel, G., Jackson, R., Jacob, S., Jakosky, B., Jensen, E., Jensen, J. K., Johnson, J., Johnson, M., Johnstone, S., Jones, A., Jones, J., Joseph, J., Jun, I., Kahanpaa, H., Kahre, M., Karpushkina, N., Kasprzak, W., Kauhanen, J., Keely, L., Kemppinen, O., Keymeulen, D., Kim, M.-H., Kinch, K., King, P., Kirkland, L., Koefoed, A., Kohler, J., Kortmann, O., Kozyrev, A., Krezoski, J., Krysak, D., Kuzmin, R., Lacour, J. L., Lafaille, V., Langevin, Y., Lanza, N., Lasue, J., Le Mouelic, S., Lee, E. M., Lee, Q.-M., Lees, D., Lefavor, M., Lemmon, M., Lepinette Malvitte, A., Leveille, R., Lewin-Carpintier, E., Li, S., Lipkaman, L., Little, C., Litvak, M., Lorigny, E., Lugmair, G., Lundberg, A., Lyness, E., Maki, J., Malakhov, A., Malespin, C., Malin, M., Mangold, N., Manning, H., Marchand, G., Marin Jimenez, M., Martin Garcia, C., Martin, D., Martin, M., Martinez-Frias, J., Martin-Soler, J., Martin-Torres, F. J., Mauchien, P., McAdam, A., McCartney, E., McConnochie, T., McCullough, E., McEwan, I., McKay, C., McNair, S., Melikechi, N., Meyer, M., Mezzacappa, A., Miller, H., Miller, K., Milliken, R., Minitti, M., Mischna, M., Mitrofanov, I., Moersch, J., Mokrousov, M., Molina Jurado, A., Moores, J., Mora-Sotomayor, L., Morookian, J. M., Mueller-Mellin, R., Muller, J.-P., Munoz Caro, G., Nachon, M., Navarro Lopez, S., Nealson, K., Nefian, A., Nelson, T., Newcombe, M., Newman, C., Newsom, H., Nikiforov, S., Niles, P., Nixon, B., Dobrea, E. N., Nolan, T., Oehler, D., Ollila, A., Olson, T., Owen, T., Pablo, H., Paillet, A., Pallier, E., Palucis, M., Parker, T., Parot, Y., Patel, K., Paton, M., Paulsen, G., Pavlov, A., Pavri, B., Peinado-Gonzalez, V., Pepin, R., Peret, L., Perez, R., Perrett, G., Peterson, J., Pilorget, C., Pinet, P., Pla-Garcia, J., Plante, I., Poitrasson, F., Polkko, J., Popa, R., Posiolova, L., Pradler, I., Prats, B., Prokhorov, V., Purdy, S. W., Raaen, E., Radziemski, L., Rafkin, S., Ramos, M., Raulin, F., Ravine, M., Reitz, G., Renno, N., Rice, M., Richardson, M., Robert, F., Rodriguez Manfredi, J. A., Romeral-Planello, J. J., Rowland, S., Saccoccio, M., Salamon, A., Sandoval, J., Sanin, A., Sans Fuentes, S. A., Saper, L., Sautter, V., Savijarvi, H., Schieber, J., Schmidt, W., Scholes, D., Schoppers, M., Schroder, S., Sebastian Martinez, E., Sengstacken, A., Shterts, R., Siebach, K., Siili, T., Simmonds, J., Sirven, J.-B., Slavney, S., Sletten, R., Smith, M., Sobron Sanchez, P., Spanovich, N., Spray, J., Squyres, S., Stack, K., Stalport, F., Stein, T., Stern, J., Stewart, N., Stipp, S. L. S., Stoiber, K., Sucharski, B., Summons, R., Sun, V., Supulver, K., Sutter, B., Szopa, C., Tate, C., Teinturier, S., ten Kate, I. L., Thomas, P., Thompson, L., Tokar, R., Toplis, M., Torres Redondo, J., Trainer, M., Tretyakov, V., Urqui-O'Callaghan, R., Van Beek, J., Van Beek, T., VanBommel, S., Varenikov, A., Vasavada, A., Vasconcelos, P., Vicenzi, E., Vostrukhin, A., Voytek, M., Wadhwa, M., Ward, J., Webster, C., Weigle, E., Wellington, D., Westall, F., Wiens, R. C., Wilhelm, M. B., Williams, A., Williams, J., Williams, R., Williams, R. B., Wilson, M., Wimmer-Schweingruber, R., Wolff, M., Wong, M., Wray, J., Wu, M., Yana, C., Zeitlin, C., Zimdar, R., Zorzano Mier, M.-P., GeoRessources, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), NASA Ames Research Center (ARC), NASA Johnson Space Center (JSC), NASA, Department of Geological Sciences [Austin], Jackson School of Geosciences (JSG), University of Texas at Austin [Austin]-University of Texas at Austin [Austin], Department of Geology [Tucson], University of Arizona, Department of Geological Sciences [Bloomington], Indiana University [Bloomington], Indiana University System-Indiana University System, Malin Space Science Systems (MSSS), NASA Goddard Space Flight Center (GSFC), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, and Petrology

Subjects
Basalt, Meridiani Planum, Multidisciplinary, 010504 meteorology & atmospheric sciences, Curiosity rover, Geochemistry, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Mars Exploration Program, Exploration of Mars, 01 natural sciences, Astrobiology, Impact crater, 13. Climate action, MSL Mars Gale Crater Rocknest, Rocknest, 0103 physical sciences, Sample Analysis at Mars, Aeolian processes, MSL, Rocknest aeolian deposit, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

The Rocknest aeolian deposit is similar to aeolian features analyzed by the Mars Exploration Rovers (MERs) Spirit and Opportunity. The fraction of sand

Published
2013
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34. The Petrochemistry of Jake_M: A Martian Mugearite

Author

Stolper, E. M., Baker, M. B., Newcombe, M. E., Schmidt, M. E., Treiman, A. H., Cousin, A., Dyar, M. D., Fisk, M. R., Gellert, R., King, P. L., Leshin, L., Maurice, S., McLennan, S. M., Minitti, M. E., Perrett, G., Rowland, S., Sautter, V., Wiens, R. C., Kemppinen, O., Bridges, N., Johnson, J. R., Cremers, D., Bell, J. F., Edgar, L., Farmer, J., Godber, A., Wadhwa, M., Wellington, D., McEwan, I., Newman, C., Richardson, M., Charpentier, A., Peret, L., Blank, J., Weigle, G., Li, S., Milliken, R., Robertson, K., Sun, V., Edwards, C., Ehlmann, B., Farley, K., Griffes, J., Grotzinger, J., Miller, H., Pilorget, C., Rice, M., Siebach, K., Stack, K., Brunet, C., Hipkin, V., Leveille, R., Marchand, G., Sanchez, P. S., Favot, L., Cody, G., Steele, A., Fluckiger, L., Lees, D., Nefian, A., Martin, M., Gailhanou, M., Westall, F., Israel, G., Agard, C., Baroukh, J., Donny, C., Gaboriaud, A., Guillemot, P., Lafaille, V., Lorigny, E., Paillet, A., Perez, R., Saccoccio, M., Yana, C., Armiens-Aparicio, C., Rodriguez, J. C., Blazquez, I. C., Gomez, F. G., Gomez-Elvira, J., Hettrich, S., Malvitte, A. L., Jimenez, M. M., Martinez-Frias, J., Martin-Soler, J., Martin-Torres, F. J., Jurado, A. M., Mora-Sotomayor, L., Caro, G. M., Lopez, S. N., Peinado-Gonzalez, V., Pla-Garcia, J., Manfredi, J. A. R., Romeral-Planello, J. J., Fuentes, S. A. S., Martinez, E. S., Redondo, J. T., Urqui-O'Callaghan, R., Mier, M.-P. Z., Chipera, S., Lacour, J.-L., Mauchien, P., Sirven, J.-B., Manning, H., Fairen, A., Hayes, A., Joseph, J., Squyres, S., Sullivan, R., Thomas, P., Dupont, A., Lundberg, A., Melikechi, N., Mezzacappa, A., DeMarines, J., Grinspoon, D., Reitz, G., Prats, B., Atlaskin, E., Genzer, M., Harri, A.-M., Haukka, H., Kahanpaa, H., Kauhanen, J., Paton, M., Polkko, J., Schmidt, W., Siili, T., Fabre, C., Wray, J., Wilhelm, M. B., Poitrasson, F., Patel, K., Gorevan, S., Indyk, S., Paulsen, G., Gupta, S., Bish, D., Schieber, J., Gondet, B., Langevin, Y., Geffroy, C., Baratoux, D., Berger, G., Cros, A., d'Uston, C., Forni, O., Gasnault, O., Lasue, J., Lee, Q.-M., Meslin, P.-Y., Pallier, E., Parot, Y., Pinet, P., Schroder, S., Toplis, M., Lewin, E., Brunner, W., Heydari, E., Achilles, C., Oehler, D., Sutter, B., Cabane, M., Coscia, D., Szopa, C., Teinturier, S., Dromart, G., Robert, F., Le Mouelic, S., Mangold, N., Nachon, M., Buch, A., Stalport, F., Coll, P., Francois, P., Raulin, F., Cameron, J., Clegg, S., DeLapp, D., Dingler, R., Jackson, R. S., Johnstone, S., Lanza, N., Little, C., Nelson, T., Williams, R. B., Kirkland, L., Baker, B., Cantor, B., Caplinger, M., Davis, S., Duston, B., Edgett, K., Fay, D., Hardgrove, C., Harker, D., Herrera, P., Jensen, E., Kennedy, M. R., Krezoski, G., Krysak, D., Lipkaman, L., Malin, M., McCartney, E., McNair, S., Nixon, B., Posiolova, L., Ravine, M., Salamon, A., Saper, L., Stoiber, K., Supulver, K., Van Beek, J., Van Beek, T., Zimdar, R., French, K. L., Iagnemma, K., Miller, K., Summons, R., Goesmann, F., Goetz, W., Hviid, S., Johnson, M., Lefavor, M., Lyness, E., Breves, E., Fassett, C., Blake, D. F., Bristow, T., DesMarais, D., Edwards, L., Haberle, R., Hoehler, T., Hollingsworth, J., Kahre, M., Keely, L., McKay, C., Bleacher, L., Brinckerhoff, W., Choi, D., Conrad, P., Dworkin, J. P., Eigenbrode, J., Floyd, M., Freissinet, C., Garvin, J., Glavin, D., Harpold, D., Mahaffy, P., Martin, D. K., McAdam, A., Pavlov, A., Raaen, E., Smith, M. D., Stern, J., Tan, F., Trainer, M., Meyer, M., Posner, A., Voytek, M., Anderson, R. C., Aubrey, A., Beegle, L. W., Behar, A., Blaney, D., Brinza, D., Calef, F., Christensen, L., Crisp, J., DeFlores, L., Feldman, J., Feldman, S., Flesch, G., Hurowitz, J., Jun, I., Keymeulen, D., Maki, J., Mischna, M., Morookian, J. M., Parker, T., Pavri, B., Schoppers, M., Sengstacken, A., Simmonds, J. J., Spanovich, N., Juarez, M. d. l. T., Vasavada, A., Webster, C. R., Yen, A., Archer, P. D., Cucinotta, F., Jones, J. H., Ming, D., Morris, R. V., Niles, P., Rampe, E., Nolan, T., Radziemski, L., Barraclough, B., Bender, S., Berman, D., Dobrea, E. N., Tokar, R., Vaniman, D., Williams, R. M. E., Yingst, A., Lewis, K., Cleghorn, T., Huntress, W., Manhes, G., Hudgins, J., Olson, T., Stewart, N., Sarrazin, P., Grant, J., Vicenzi, E., Wilson, S. A., Bullock, M., Ehresmann, B., Hamilton, V., Hassler, D., Peterson, J., Rafkin, S., Zeitlin, C., Fedosov, F., Golovin, D., Karpushkina, N., Kozyrev, A., Litvak, M., Malakhov, A., Mitrofanov, I., Mokrousov, M., Nikiforov, S., Prokhorov, V., Sanin, A., Tretyakov, V., Varenikov, A., Vostrukhin, A., Kuzmin, R., Clark, B., Wolff, M., Botta, O., Drake, D., Bean, K., Lemmon, M., Schwenzer, S. P., Anderson, R. B., Herkenhoff, K., Lee, E. M., Sucharski, R., Hernandez, M. A. d. P., Avalos, J. J. B., Ramos, M., Jones, A., Kim, M.-H., Malespin, C., Plante, I., Muller, J.-P., Navarro-Gonzalez, R., Ewing, R., Boynton, W., Downs, R., Fitzgibbon, M., Harshman, K., Morrison, S., Dietrich, W., Kortmann, O., Palucis, M., Sumner, D. Y., Williams, A., Lugmair, G., Wilson, M. A., Rubin, D., Jakosky, B., Balic-Zunic, T., Frydenvang, J., Jensen, J. K., Kinch, K., Koefoed, A., Madsen, M. B., Stipp, S. L. S., Boyd, N., Campbell, J. L., Pradler, I., VanBommel, S., Jacob, S., Owen, T., Savijarvi, H., Boehm, E., Bottcher, S., Burmeister, S., Guo, J., Kohler, J., Garcia, C. M., Mueller-Mellin, R., Wimmer-Schweingruber, R., Bridges, J. C., McConnochie, T., Benna, M., Franz, H., Bower, H., Brunner, A., Blau, H., Boucher, T., Carmosino, M., Atreya, S., Elliott, H., Halleaux, D., Renno, N., Wong, M., Pepin, R., Elliott, B., Spray, J., Thompson, L., Gordon, S., Newsom, H., Ollila, A., Williams, J., Vasconcelos, P., Bentz, J., Nealson, K., Popa, R., Kah, L. C., Moersch, J., Tate, C., Day, M., Kocurek, G., Hallet, B., Sletten, R., Francis, R., McCullough, E., Cloutis, E., ten Kate, I. L., Arvidson, R., Fraeman, A., Scholes, D., Slavney, S., Stein, T., Ward, J., Berger, J., Moores, J. E., GeoRessources, Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS), California Institute of Technology (CALTECH), Department of Earth Sciences [St. Catharines], Brock University [Canada], Lunar and Planetary Institute [Houston] (LPI), Los Alamos National Laboratory (LANL), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Mount Holyoke College, Oregon State University (OSU), University of Guelph, Research School of Earth Sciences [Canberra] (RSES), Australian National University (ANU), Rensselaer Polytechnic Institute (RPI), State University of New York (SUNY), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), University of Hawaii, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS), MSL Science Team, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Curiosity rover, Geochemistry, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, 010502 geochemistry & geophysics, 01 natural sciences, Jake_M: a martian mugearite, chemistry.chemical_compound, Nepheline, MSL, Chemical composition, 0105 earth and related environmental sciences, Martian, Phonolite, Multidisciplinary, Fractional crystallization (geology), petrochemistry, Igneous rock, Planetary science, MSL Mars Petrochemistry, chemistry, 13. Climate action, Petrochemistry, Geology, [SDU.STU.MI]Sciences of the Universe [physics]/Earth Sciences/Mineralogy
Abstract

International audience; "Jake_M," the first rock analyzed by the Alpha Particle X-ray Spectrometer instrument on the Curiosity rover, differs substantially in chemical composition from other known martian igneous rocks: It is alkaline (>15% normative nepheline) and relatively fractionated. Jake_M is compositionally similar to terrestrial mugearites, a rock type typically found at ocean islands and continental rifts. By analogy with these comparable terrestrial rocks, Jake_M could have been produced by extensive fractional crystallization of a primary alkaline or transitional magma at elevated pressure, with or without elevated water contents. The discovery of Jake_M suggests that alkaline magmas may be more abundant on Mars than on Earth and that Curiosity could encounter even more fractionated alkaline rocks (for example, phonolites and trachytes).

Published
2013
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35. Volatile, Isotope, and Organic Analysis of Martian Fines with the Mars Curiosity Rover

Author

Leshin, L. A., Mahaffy, P. R., Webster, C. R., Cabane, M., Coll, P., Conrad, P. G., Archer, P. D., Atreya, S. K., Brunner, A. E., Buch, A., Eigenbrode, J. L., Flesch, G. J., Franz, H. B., Freissinet, C., Glavin, D. P., McAdam, A. C., Miller, K. E., Ming, D. W., Morris, R. V., Navarro-Gonzalez, R., Niles, P. B., Owen, T., Pepin, R. O., Squyres, S., Steele, A., Stern, J. C., Summons, R. E., Sumner, D. Y., Sutter, B., Szopa, C., Teinturier, S., Trainer, M. G., Wray, J. J., Grotzinger, J. P., Kemppinen, O., Bridges, N., Johnson, J. R., Minitti, M., Cremers, D., Bell, J. F., Edgar, L., Farmer, J., Godber, A., Wadhwa, M., Wellington, D., McEwan, I., Newman, C., Richardson, M., Charpentier, A., Peret, L., King, P., Blank, J., Weigle, G., Schmidt, M., Li, S., Milliken, R., Robertson, K., Sun, V., Baker, M., Edwards, C., Ehlmann, B., Farley, K., Griffes, J., Miller, H., Newcombe, M., Pilorget, C., Rice, M., Siebach, K., Stack, K., Stolper, E., Brunet, C., Hipkin, V., Leveille, R., Marchand, G., Sanchez, P. S., Favot, L., Cody, G., Fluckiger, L., Lees, D., Nefian, A., Martin, M., Gailhanou, M., Westall, F., Israel, G., Agard, C., Baroukh, J., Donny, C., Gaboriaud, A., Guillemot, P., Lafaille, V., Lorigny, E., Paillet, A., Perez, R., Saccoccio, M., Yana, C., Armiens-Aparicio, C., Rodriguez, J. C., Blazquez, I. C., Gomez, F. G., Gomez-Elvira, J., Hettrich, S., Malvitte, A. L., Jimenez, M. M., Martinez-Frias, J., Martin-Soler, J., Martin-Torres, F. J., Jurado, A. M., Mora-Sotomayor, L., Caro, G. M., Lopez, S. N., Peinado-Gonzalez, V., Pla-Garcia, J., Manfredi, J. A. R., Romeral-Planello, J. J., Fuentes, S. A. S., Martinez, E. S., Redondo, J. T., Urqui-O'Callaghan, R., Mier, M.-P. Z., Chipera, S., Lacour, J.-L., Mauchien, P., Sirven, J.-B., Manning, H., Fairen, A., Hayes, A., Joseph, J., Sullivan, R., Thomas, P., Dupont, A., Lundberg, A., Melikechi, N., Mezzacappa, A., DeMarines, J., Grinspoon, D., Reitz, G., Prats, B., Atlaskin, E., Genzer, M., Harri, A.-M., Haukka, H., Kahanpaa, H., Kauhanen, J., Paton, M., Polkko, J., Schmidt, W., Siili, T., Fabre, C., Wilhelm, M. B., Poitrasson, F., Patel, K., Gorevan, S., Indyk, S., Paulsen, G., Gupta, S., Bish, D., Schieber, J., Gondet, B., Langevin, Y., Geffroy, C., Baratoux, D., Berger, G., Cros, A., d'Uston, C., Forni, O., Gasnault, O., Lasue, J., Lee, Q.-M., Maurice, S., Meslin, P.-Y., Pallier, E., Parot, Y., Pinet, P., Schroder, S., Toplis, M., Lewin, E., Brunner, W., Heydari, E., Achilles, C., Oehler, D., Coscia, D., Dromart, G., Robert, F., Sautter, V., Le Mouelic, S., Mangold, N., Nachon, M., Stalport, F., Francois, P., Raulin, F., Cameron, J., Clegg, S., Cousin, A., DeLapp, D., Dingler, R., Jackson, R. S., Johnstone, S., Lanza, N., Little, C., Nelson, T., Wiens, R. C., Williams, R. B., Jones, A., Kirkland, L., Treiman, A., Baker, B., Cantor, B., Caplinger, M., Davis, S., Duston, B., Edgett, K., Fay, D., Hardgrove, C., Harker, D., Herrera, P., Jensen, E., Kennedy, M. R., Krezoski, G., Krysak, D., Lipkaman, L., Malin, M., McCartney, E., McNair, S., Nixon, B., Posiolova, L., Ravine, M., Salamon, A., Saper, L., Stoiber, K., Supulver, K., Van Beek, J., Van Beek, T., Zimdar, R., French, K. L., Iagnemma, K., Goesmann, F., Goetz, W., Hviid, S., Johnson, M., Lefavor, M., Lyness, E., Breves, E., Dyar, M. D., Fassett, C., Blake, D. F., Bristow, T., DesMarais, D., Edwards, L., Haberle, R., Hoehler, T., Hollingsworth, J., Kahre, M., Keely, L., McKay, C., Bleacher, L., Brinckerhoff, W., Choi, D., Dworkin, J. P., Floyd, M., Garvin, J., Harpold, D., Martin, D. K., Pavlov, A., Raaen, E., Smith, M. D., Tan, F., Meyer, M., Posner, A., Voytek, M., Anderson, R. C., Aubrey, A., Beegle, L. W., Behar, A., Blaney, D., Brinza, D., Calef, F., Christensen, L., Crisp, J. A., DeFlores, L., Feldman, J., Feldman, S., Hurowitz, J., Jun, I., Keymeulen, D., Maki, J., Mischna, M., Morookian, J. M., Parker, T., Pavri, B., Schoppers, M., Sengstacken, A., Simmonds, J. J., Spanovich, N., Juarez, M. d. l. T., Vasavada, A. R., Yen, A., Cucinotta, F., Jones, J. H., Rampe, E., Nolan, T., Fisk, M., Radziemski, L., Barraclough, B., Bender, S., Berman, D., Dobrea, E. N., Tokar, R., Vaniman, D., Williams, R. M. E., Yingst, A., Lewis, K., Cleghorn, T., Huntress, W., Manhes, G., Hudgins, J., Olson, T., Stewart, N., Sarrazin, P., Grant, J., Vicenzi, E., Wilson, S. A., Bullock, M., Ehresmann, B., Hamilton, V., Hassler, D., Peterson, J., Rafkin, S., Zeitlin, C., Fedosov, F., Golovin, D., Karpushkina, N., Kozyrev, A., Litvak, M., Malakhov, A., Mitrofanov, I., Mokrousov, M., Nikiforov, S., Prokhorov, V., Sanin, A., Tretyakov, V., Varenikov, A., Vostrukhin, A., Kuzmin, R., Clark, B., Wolff, M., McLennan, S., Botta, O., Drake, D., Bean, K., Lemmon, M., Schwenzer, S. P., Anderson, R. B., Herkenhoff, K., Lee, E. M., Sucharski, R., Hernandez, M. A. d. P., Avalos, J. J. B., Ramos, M., Kim, M.-H., Malespin, C., Plante, I., Muller, J.-P., Ewing, R., Boynton, W., Downs, R., Fitzgibbon, M., Harshman, K., Morrison, S., Dietrich, W., Kortmann, O., Palucis, M., Williams, A., Lugmair, G., Wilson, M. A., Rubin, D., Jakosky, B., Balic-Zunic, T., Frydenvang, J., Jensen, J. K., Kinch, K., Koefoed, A., Madsen, M. B., Stipp, S. L. S., Boyd, N., Campbell, J. L., Gellert, R., Perrett, G., Pradler, I., VanBommel, S., Jacob, S., Rowland, S., Savijarvi, H., Boehm, E., Bottcher, S., Burmeister, S., Guo, J., Kohler, J., Garcia, C. M., Mueller-Mellin, R., Wimmer-Schweingruber, R., Bridges, J. C., McConnochie, T., Benna, M., Bower, H., Blau, H., Boucher, T., Carmosino, M., Elliott, H., Halleaux, D., Renno, N., Wong, M., Elliott, B., Spray, J., Thompson, L., Gordon, S., Newsom, H., Ollila, A., Williams, J., Vasconcelos, P., Bentz, J., Nealson, K., Popa, R., Kah, L. C., Moersch, J., Tate, C., Day, M., Kocurek, G., Hallet, B., Sletten, R., Francis, R., McCullough, E., Cloutis, E., ten Kate, I. L., Arvidson, R., Fraeman, A., Scholes, D., Slavney, S., Stein, T., Ward, J., Berger, J., Moores, J. E., Department of Earth and Environmental Sciences [Troy, NY], Rensselaer Polytechnic Institute (RPI), NASA Goddard Space Flight Center (GSFC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Department of Astronomy [College Park], University of Maryland [College Park], University of Maryland System-University of Maryland System, Laboratoire de Génie des Procédés et Matériaux - EA 4038 (LGPM), CentraleSupélec, Center for Research and Exploration in Space Science and Technology [GSFC] (CRESST), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Laboratorio de Química de Plasmas y Estudios Planetarios [Mexico], Instituto de Ciencias Nucleares [Mexico], Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM)-Universidad Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), School of Physics and Astronomy [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Cornell University [New York], Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science, University of California [Davis] (UC Davis), University of California (UC), Jacobs Technology ESCG, Institut Pierre-Simon-Laplace (IPSL), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), School of Earth and Atmospheric Sciences [Atlanta], Georgia Institute of Technology [Atlanta], Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, California Institute of Technology (CALTECH)-NASA, Universidad Nacional Autónoma de México (UNAM)-Universidad Nacional Autónoma de México (UNAM), Carnegie Institution for Science [Washington], University of California, École normale supérieure - Paris (ENS Paris), IMPEC - LATMOS, Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of Minnesota [Twin Cities], Cornell University, and École normale supérieure - Paris (ENS Paris)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National d'Études Spatiales [Toulouse] (CNES)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)

Subjects
Martian, Multidisciplinary, 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Thermal decomposition, Curiosity rover, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], chemistry.chemical_element, Mars, organic analysis, Mars Exploration Program, 01 natural sciences, Astrobiology, chemistry.chemical_compound, chemistry, 13. Climate action, Isotopes of carbon, Rocknest, 0103 physical sciences, Sample Analysis at Mars, Carbonate, MSL Mars Volatiles Isotopes Organics Soil Gale Crater, 010303 astronomy & astrophysics, Carbon, 0105 earth and related environmental sciences
Abstract

Samples from the Rocknest aeolian deposit were heated to ~835°C under helium flow and evolved gases analyzed by Curiosity’s Sample Analysis at Mars instrument suite. H 2 O, SO 2 , CO 2 , and O 2 were the major gases released. Water abundance (1.5 to 3 weight percent) and release temperature suggest that H 2 O is bound within an amorphous component of the sample. Decomposition of fine-grained Fe or Mg carbonate is the likely source of much of the evolved CO 2 . Evolved O 2 is coincident with the release of Cl, suggesting that oxygen is produced from thermal decomposition of an oxychloride compound. Elevated δD values are consistent with recent atmospheric exchange. Carbon isotopes indicate multiple carbon sources in the fines. Several simple organic compounds were detected, but they are not definitively martian in origin.

Published
2013
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36. A Possible Sink for Methane on Mars

Author

Nørnberg, P., Jensen, S. J. K., Skibsted, J., Jakobsen, H. J., ten Kate, I. L., Gunnlaugsson, H. P., Merrison, J. P., Finster, K., Bak, E., Iversen, J. J., Kondrup, J. C., Nørnberg, P., Jensen, S. J. K., Skibsted, J., Jakobsen, H. J., ten Kate, I. L., Gunnlaugsson, H. P., Merrison, J. P., Finster, K., Bak, E., Iversen, J. J., and Kondrup, J. C.

Abstract

Mechanical simulated wind activation of mineral surfaces act as a trap for Methane through formation of covalent Si-C bonds stable up to temperatures above 250 C. This mechanism is proposed as a Methane sink on Mars.

Published
2014

37. A Possible Sink for Methane on Mars

Author

Petrology, NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Nørnberg, P., Jensen, S. J. K., Skibsted, J., Jakobsen, H. J., ten Kate, I. L., Gunnlaugsson, H. P., Merrison, J. P., Finster, K., Bak, E., Iversen, J. J., Kondrup, J. C., Petrology, NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Nørnberg, P., Jensen, S. J. K., Skibsted, J., Jakobsen, H. J., ten Kate, I. L., Gunnlaugsson, H. P., Merrison, J. P., Finster, K., Bak, E., Iversen, J. J., and Kondrup, J. C.

Published
2014

40. The potential science and engineering value of samples delivered to Earth by Mars sample return

Author

Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., Zorzano, M. P., Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., and Zorzano, M. P.

41. The potential science and engineering value of samples delivered to Earth by Mars sample return

Author

Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., Zorzano, M. P., Beaty, D. W., Grady, Monica, McSween, H. Y., Sefton-Nash, E., Carrier, B. L., Altieri, F., Amelin, Y., Ammannito, E., Anand, M., Benning, L. G., Bishop, J. L., Borg, L. E., Boucher, D., Brucato, J. R., Busemann, H., Campbell, K. A., Czaja, A. D., Debaille, V., Des Marais, D. J., Dixon, M., Ehlmann, B. L., Farmer, J. D., Fernandez-Remolar, D. C., Filiberto, J., Fogarty, J., Glavin, D. P., Goreva, Y. S., Hallis, L. J., Harrington, A. D., M. Hausrath, E., Herd, C. D. K., Horgan, B., Humanyun, M., Kleine, T., Kleinhenz, J., Mackelprang, R., Mangold, N., Mayhew, L. E., McCoy, J. T., McCubbin, F. M., McLennan, S. M., Moser, D. E., Moynier, F., Mustard, J. F., Niles, P. B., Ori, G. G., Raulin, F., Rettberg, P., Rucker, M. A., Schmitz, N., Schwenzer, S. P., Sephton, M. A., Shaheen, R., Sharp, Z. D., Schuster, D. L., Siljestrom, S., Smith, C. L., Spry, J. A., Steele, A., Swindle, T. D., ten Kate, I. L., Tosca, N. J., Usui, T., Van Kranendonk, M. J., Wadhwa, M., Weiss, B. P., Werner, S. C., Westall, F., Wheeler, R. M., Zipfel, J., and Zorzano, M. P.

42. EPJ Web of Conferences

Author

Markovich, D. M., Kuibin, P. A., Vorobyev, M. A., Valore, L., Colalillo, R., Guarino, F., Wrońska, Aleksandra, Magiera, Andrzej, Przygoda, Witold, Mogilevtsev, D., Deustua, S., Eastwood, K., ten Kate, I. L., Bobrikov, I., Chudoba, V., Derenovskaya, O., Friesen, A., Verkheev, A., Bondar, A., Eidelman, S., Poli, E., Laqua, H., Oosterbeek, J., Bondarenko, S., Burov, V., Malakhov, A., Cerullo, G., Ogilvie, J., Kärtner, F., Khalil, M., Li, R., Yang, A., Wang, W. Y., Ng, S. C. C., Chan, A. H., Oh, C. H., Phua, K. K., Spiering, C., Pattison, B., Itow, Y., Sako, T., Menjo, H., De Vincenzi, M., Capone, A., Morselli, A., Lhenry-Yvon, I., Biteau, J., Deligny, O., Ghia, P., Serot, O., Chebboubi, A., Achasov, N. N., Ignatov, F. V., Krokovny, P. P., Dančová, P., Novosad, J., Forti, A., Betev, L., Litmaath, M., Smirnova, O., Hristov, P., Fähnle, O., Vasdekis, A., Riccobene, G., Biagi, S., Distefano, C., Piattelli, P., Rehtanz, C., Voropai, N., Denig, A., Redmer, C.-F., Jenke, T., Degenkolb, S., Geltenbort, P., Jentschel, M., Nesvizhevsky, V. V., Rebreyend, D., Roccia, S., Soldner, T., Stutz, A., Zimmer, O., Arakelyan, S., Evlyukhin, A., Kalachev, A., Naumov, A., Fomin, V., Placidi, L., Melikhov, D., Volobuev, I., de Angelis, G., Corradi, L., Nadykto, A., Uvarova, L., Zelensky, A., Pivkin, P., Lima, P., Aleksic, N., Egiazarian, K., and Jiang, X.

Published
2019

43. Organic molecules in the Sheepbed Mudstone, Gale Crater, Mars.

Author

Freissinet C, Glavin DP, Mahaffy PR, Miller KE, Eigenbrode JL, Summons RE, Brunner AE, Buch A, Szopa C, Archer PD, Franz HB, Atreya SK, Brinckerhoff WB, Cabane M, Coll P, Conrad PG, Des Marais DJ, Dworkin JP, Fairén AG, François P, Grotzinger JP, Kashyap S, Ten Kate IL, Leshin LA, Malespin CA, Martin MG, Martin-Torres FJ, McAdam AC, Ming DW, Navarro-González R, Pavlov AA, Prats BD, Squyres SW, Steele A, Stern JC, Sumner DY, Sutter B, and Zorzano MP

Abstract

The 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 C 2 to C 4 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., Key Points: First in situ evidence of nonterrestrial organics in Martian surface sediments Chlorinated hydrocarbons identified in the Sheepbed mudstone by SAM Organics preserved in sample exposed to ionizing radiation and oxidative condition.

Published
2015
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