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2. The SuperCam Instrument Suite on the NASA Mars 2020 Rover: Body Unit and Combined System Tests

Author

Roger C. Wiens, Sylvestre Maurice, Scott H. Robinson, Anthony E. Nelson, Philippe Cais, Pernelle Bernardi, Raymond T. Newell, Sam Clegg, Shiv K. Sharma, Steven Storms, Jonathan Deming, Darrel Beckman, Ann M. Ollila, Olivier Gasnault, Ryan B. Anderson, Yves André, S. Michael Angel, Gorka Arana, Elizabeth Auden, Pierre Beck, Joseph Becker, Karim Benzerara, Sylvain Bernard, Olivier Beyssac, Louis Borges, Bruno Bousquet, Kerry Boyd, Michael Caffrey, Jeffrey Carlson, Kepa Castro, Jorden Celis, Baptiste Chide, Kevin Clark, Edward Cloutis, Elizabeth C. Cordoba, Agnes Cousin, Magdalena Dale, Lauren Deflores, Dorothea Delapp, Muriel Deleuze, Matthew Dirmyer, Christophe Donny, Gilles Dromart, M. George Duran, Miles Egan, Joan Ervin, Cecile Fabre, Amaury Fau, Woodward Fischer, Olivier Forni, Thierry Fouchet, Reuben Fresquez, Jens Frydenvang, Denine Gasway, Ivair Gontijo, John Grotzinger, Xavier Jacob, Sophie Jacquinod, Jeffrey R. Johnson, Roberta A. Klisiewicz, James Lake, Nina Lanza, Javier Laserna, Jeremie Lasue, Stéphane Le Mouélic, Carey Legett, Richard Leveille, Eric Lewin, Guillermo Lopez-Reyes, Ralph Lorenz, Eric Lorigny, Steven P. Love, Briana Lucero, Juan Manuel Madariaga, Morten Madsen, Soren Madsen, Nicolas Mangold, Jose Antonio Manrique, J. P. Martinez, Jesus Martinez-Frias, Kevin P. McCabe, Timothy H. McConnochie, Justin M. McGlown, Scott M. McLennan, Noureddine Melikechi, Pierre-Yves Meslin, John M. Michel, David Mimoun, Anupam Misra, Gilles Montagnac, Franck Montmessin, Valerie Mousset, Naomi Murdoch, Horton Newsom, Logan A. Ott, Zachary R. Ousnamer, Laurent Pares, Yann Parot, Rafal Pawluczyk, C. Glen Peterson, Paolo Pilleri, Patrick Pinet, Gabriel Pont, Francois Poulet, Cheryl Provost, Benjamin Quertier, Heather Quinn, William Rapin, Jean-Michel Reess, Amy H. Regan, Adriana L. Reyes-Newell, Philip J. Romano, Clement Royer, Fernando Rull, Benigno Sandoval, Joseph H. Sarrao, Violaine Sautter, Marcel J. Schoppers, Susanne Schröder, Daniel Seitz, Terra Shepherd, Pablo Sobron, Bruno Dubois, Vishnu Sridhar, Michael J. Toplis, Imanol Torre-Fdez, Ian A. Trettel, Mark Underwood, Andres Valdez, Jacob Valdez, Dawn Venhaus, and Peter Willis

Published
2020
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3. Askival:An altered feldspathic cumulate sample in Gale crater

Author

Donald Lewis Bowden, John C. Bridges, Agnes Cousin, William Rapin, Julia Semprich, Olivier Gasnault, Olivier Forni, Patrick Gasda, Debarati Das, Valerie Payré, Violaine Sautter, Candice C. Bedford, Roger C. Wiens, Patrick Pinet, Jens Frydenvang, School of Physics and Astronomy [Leicester], University of Leicester, 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), School of Environment, Earth and Ecosystem Sciences, The Open University, Milton Keynes, UK, Los Alamos National Laboratory (LANL), Department of Earth and Planetary Sciences [Montréal] (EPS), McGill University = Université McGill [Montréal, Canada], Department of Earth and Environmental Sciences [Iowa City], University of Iowa [Iowa City], Muséum national d'Histoire naturelle (MNHN), Lunar and Planetary Institute [Houston] (LPI), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, GLOBE Institute, and University of Copenhagen

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Geophysics, Space and Planetary Science
Abstract

Askival is a light-toned, coarsely crystalline float rock, which was identified near the base of Vera Rubin Ridge in Gale crater. We have studied Askival, principally with the ChemCam instrument but also using APXS compositional data and MAHLI images. Askival and an earlier identified sample, Bindi, represent two rare examples of feldspathic cumulate float rocks in Gale crater with >65% relict plagioclase. Bindi appears unaltered whereas Askival shows textural and compositional signatures of silicification, along with alkali remobilization and hydration. Askival likely experienced multiple stages of alteration, occurring first through acidic hydrolysis of metal cations, followed by deposition of silica and possible phyllosilicates at low T and neutral-alkaline pH. Through laser-induced breakdown spectroscopy compositional analyses and normative calculations, we suggest that an assemblage of Fe-Mg silicates including amphibole and pyroxene, Fe phases, and possibly Mg-rich phyllosilicate are present. Thermodynamic modeling of the more pristine Bindi composition predicts that amphibole and feldspar are stable within an upper crustal setting. This is consistent with the presence of amphibole in the parent igneous rocks of Askival and suggests that the paucity of amphiboles in other known Martian samples reflects the lack of representative samples of the Martian crust rather than their absence on Mars.

Published
2023

4. Alkali magmatism on Mars: an unexpected diversity

Author

Valerie Payre and Violaine Sautter

Subjects
Earth science, Magmatism, General Earth and Planetary Sciences, Mars Exploration Program, Geology, General Environmental Science, Diversity (business)
Published
2022

6. Understanding the Chemistry of the Rocks at Jezero crater, Mars, through the Combined Use of SuperCam Spectroscopic and Optical Techniques

Author

Juan Manuel Madariaga, Roger Wiens, Gorka Arana, Violaine Sautter, Karim Benzerara, Arya Udry, Olivier Beyssac, Lucia Mandon, Olivier Gasnault, Jeffrey Johnson, Ann Ollila, Kepa Castro, Agnes Cousin, Sylvestre Maurice, Samuel Clegg, Ryan Anderson, Tanja Bosak, Pierre Beck, Thierry Fouchet, Svetlana Shkolyar, Edward Cloutis, Cathy Quantin-Nataf, Imanol Torre Fernandez, Clément Royer, Chip Legett, and Paolo Pilleri

Published
2021

7. Martian meteorites reflectance and implications for rover missions

Author

Pierre Beck, C. Quantin-Nataf, Violaine Sautter, M. Martinot, Lu Pan, Erwin Dehouck, Antoine Pommerol, Romain Cerubini, Lucia Mandon, Zurine Yoldi, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Universität Bern [Bern] (UNIBE), Physikalisches Institut [Bern], Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), and Universität Bern [Bern]

Subjects
spectroscopy, 010504 meteorology & atmospheric sciences, Imaging spectrometer, Mineralogy, FOS: Physical sciences, Mars, 01 natural sciences, Spectral line, meteorites, Physics - Geophysics, 0103 physical sciences, surface, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Martian, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Spectrometer, 520 Astronomy, Hyperspectral imaging, Astronomy and Astrophysics, Mars Exploration Program, 620 Engineering, Geophysics (physics.geo-ph), Imaging spectroscopy, Meteorite, Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract

International audience; During this decade, two rovers will characterize in situ the mineralogy of rocks on Mars, using for the first time near-infrared reflectance spectrometers: SuperCam onboard the Mars 2020 rover and MicrOmega onboard the ExoMars rover, although this technique is predominantly used in orbit for mineralogical investigations. Until successful completion of sample-return missions from Mars, Martian meteorites are currently the only samples of the red planet available for study in terrestrial laboratories and comparison with in situ data. However, the current spectral database available for these samples does not represent their diversity and consists primarily of spectra acquired on finely crushed samples, albeit grain size is known to greatly affect spectral features. Here, we measured the reflected light of a broad Martian meteorite suite as a means to catalogue and characterize their spectra between 0.4 and 3 μm. These measurements are achieved using a point spectrometer acquiring data comparable to SuperCam, and an imaging spectrometer producing hyperspectral cubes, similarly to MicrOmega. Our results indicate that point spectrometry is sufficient to discriminate the different Martian meteorites families, to identify their primary petrology based on band parameters, and to detect their low content in alteration minerals. However, significant spectral mixing occurs in the point measurements, even at spot sizes down to a few millimeters, and high-resolution imaging spectroscopy is needed to correctly identify the various mineral phases in the meteorites. Additional bidirectional spectral measurements on a consolidated and powdered shergottite confirm their non-Lambertian behavior, with backward and suspected forward scattering peaks. With changing observation geometry, the main absorption strengths show variations up to ~10–15%. The variation of reflectance levels is reduced for the rock surface compared to the powder. All the spectra presented are provided in the supplementary data for further comparison with in situ and orbital measurements.

Published
2021

8. The SuperCam Instrument Suite on the Mars 2020 Rover: Science Objectives and Mast-Unit Description

Author

I. Torre-Fdez, V. Gharakanian, E. Cordoba, Jérôme Parisot, R. Perez, Amaury Fau, Peter Willis, Ruth A. Anderson, Pablo Sobron, K. W. Wong, A. Debus, Julien Mekki, Noureddine Melikechi, K. Mathieu, S. Gauffre, M. Toplis, Jesús Martínez-Frías, Alexandre Cadu, Francois Poulet, B. Quertier, Horton E. Newsom, H. Seran, C. Quantin-Nataf, W. D’anna, Jens Frydenvang, Frédéric Chapron, Pierre Beck, Jean-François Mariscal, B. Chide, Y. André, Y. Michel, G. Orttner, N. Toulemont, A. Dufour, Briana Lucero, Olivier Gilard, Marion Bonafous, D. Pheav, Q.-M. Lee, D. Standarovsky, Franck Montmessin, R. Gonzalez, S. Le Mouélic, Cedric Virmontois, L. Roucayrol, I. Gontijo, M. Deleuze, L. Parès, L. Oudda, Y. Micheau, F. Manni, Bruno Dubois, Bruno Bousquet, G. de los Santos, D. M. Delapp, Guillermo Lopez-Reyes, L. Picot, Clément Royer, E. Clave, Richard Leveille, Erwin Dehouck, Gaetan Lacombe, J. Javier Laserna, Olivier Beyssac, P. Romano, Y. Daydou, Scott M. McLennan, John Michel, V. Sridhar, Driss Kouach, Gabriel Pont, M. Dupieux, Michel Gauthier, Jean-Michel Reess, J. Moros, J.-C. Dameury, T. Fouchet, Ann Ollila, Sophie Jacquinod, P. Y. Meslin, M. Egan, Juan Manuel Madariaga, Karim Benzerara, G. Hervet, Gilles Montagnac, Woodward W. Fischer, Olivier Gasnault, T. Nelson, Stanley M. Angel, Lauren DeFlores, Violaine Sautter, Marco Veneranda, C. Leyrat, Olivier Humeau, Y. Morizet, Jose Antonio Manrique, M. Sodki, P. Pilleri, C. Velasco, Naomi Murdoch, M. J. Schoppers, S. A. Storms, Sylvestre Maurice, Benigno Sandoval, Cedric Pilorget, N. Striebig, S. Robinson, V. Mousset, David Mimoun, Morten Madsen, M. Heim, A. Doressoundiram, Christophe Montaron, Eric Lewin, Patrick Pinet, C. Donny, Susanne Schröder, Agnès Cousin, Sadok Abbaki, John P. Grotzinger, Claude Collin, Xavier Jacob, Jeffrey R. Johnson, Cécile Fabre, K. McCabe, C. Legett, J. P. Berthias, Shiv K. Sharma, Timothy H. McConnochie, A. Sournac, Ralph D. Lorenz, M. Viso, Yann Parot, N. Mangold, W. Rapin, Jérémie Lasue, Gorka Arana, Joan Ervin, E. Le Comte, N. Nguyen Tuong, P. Cais, Olivier Forni, D. Rambaud, T. Battault, D. Venhaus, Anupam K. Misra, K. Clark, M. Tatat, Laurent Lapauw, P. Bernardi, Roger C. Wiens, Samuel M. Clegg, Nina Lanza, Sylvain Bernard, Soren N. Madsen, Kepa Castro, M. Boutillier, Raymond Newell, D. Granena, Y. Hello, Fernando Rull, M. Ruellan, R. Mathon, Edward A. Cloutis, Gilles Dromart, L. Le Deit, Rafik Hassen-Khodja, 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), Los Alamos National Laboratory (LANL), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Universidad de Valladolid [Valladolid] (UVa), Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), US Geological Survey [Flagstaff], United States Geological Survey [Reston] (USGS), University of South Carolina [Columbia], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), University of Winnipeg, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), 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, University of Hawai‘i [Mānoa] (UHM), 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), California Institute of Technology (CALTECH), University of Copenhagen = Københavns Universitet (UCPH), Institut de mécanique des fluides de Toulouse (IMFT), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), PLANETO - LATMOS, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universidad de Málaga [Málaga] = University of Málaga [Málaga], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), McGill University = Université McGill [Montréal, Canada], Institut des Sciences de la Terre (ISTerre), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Gustave Eiffel-Université Grenoble Alpes (UGA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Maryland [College Park], University of Maryland System, Stony Brook University [SUNY] (SBU), State University of New York (SUNY), University of Massachusetts [Lowell] (UMass Lowell), University of Massachusetts System (UMASS), Laboratoire de Planétologie et Géodynamique - Angers (LPG-ANGERS), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), The University of New Mexico [Albuquerque], Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), In­sti­tut für Op­ti­sche Sen­sor­sys­te­me, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), SETI Institute, 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), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Bordeaux (UB), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), 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), 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), University of Copenhagen = Københavns Universitet (KU), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-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)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), and Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées

Subjects
Rocks, 010504 meteorology & atmospheric sciences, Computer science, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Mars, Context (language use), Perseverance, Imaging on Mars, Mars 2020 Perseverance rover, 01 natural sciences, SuperCam Instrument, Unit (housing), Mast (sailing), Jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, imaging on Mars, Microphone on Mars, 0103 physical sciences, Calibration, Rover, [PHYS.COND]Physics [physics]/Condensed Matter [cond-mat], infrared spectroscopy, Raman, 010303 astronomy & astrophysics, Infrared spectroscopy, 0105 earth and related environmental sciences, [SPI.ACOU]Engineering Sciences [physics]/Acoustics [physics.class-ph], M2020, LIBS, Payload, Suite, Mars2020, Astronomy and Astrophysics, Laser-Induced Breakdown Spectroscopy, Mars Exploration Program, microphone on Mars, Planetary science, SuperCam, Space and Planetary Science, Raman spectroscopy, Systems engineering, [PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], Mars 2020 PERSEVERANCE rover
Abstract

On the NASA 2020 rover mission to Jezero crater, the remote determination of the texture, mineralogy and chemistry of rocks is essential to quickly and thoroughly characterize an area and to optimize the selection of samples for return to Earth. As part of the Perseverance payload, SuperCam is a suite of five techniques that provide critical and complementary observations via Laser-Induced Breakdown Spectroscopy (LIBS), Time-Resolved Raman and Luminescence (TRR/L), visible and near-infrared spectroscopy (VISIR), high-resolution color imaging (RMI), and acoustic recording (MIC). SuperCam operates at remote distances, primarily 2-7 m, while providing data at sub-mm to mm scales. We report on SuperCam's science objectives in the context of the Mars 2020 mission goals and ways the different techniques can address these questions. The instrument is made up of three separate subsystems: the Mast Unit is designed and built in France; the Body Unit is provided by the United States; the calibration target holder is contributed by Spain, and the targets themselves by the entire science team. This publication focuses on the design, development, and tests of the Mast Unit; companion papers describe the other units. The goal of this work is to provide an understanding of the technical choices made, the constraints that were imposed, and ultimately the validated performance of the flight model as it leaves Earth, and it will serve as the foundation for Mars operations and future processing of the data. In France was provided by the Centre National d'Etudes Spatiales (CNES). Human resources were provided in part by the Centre National de la Recherche Scientifique (CNRS) and universities. Funding was provided in the US by NASA's Mars Exploration Program. Some funding of data analyses at Los Alamos National Laboratory (LANL) was provided by laboratory-directed research and development funds.

Published
2021

9. Critical knowledge gaps in the Martian geological record: A rationale for regional-scale in situ exploration by rotorcraft mid-air deployment

Author

Valerie Payre, Bethany L. Ehlmann, N. Mangold, Robert Lillis, J. Bapst, Sylvestre Maurice, Violaine Sautter, A. A. Fraeman, William Rapin, Benoit Langlais, Jessica Flahaut, Anna Mittelholz, Arya Udry, David Baratoux, James Tuttle Keane, Gilles Dromart, C. Quantin-Nataf, and Briony Horgan

Subjects
Martian, Scale (ratio), Software deployment, Earth science, Geologic record, Geology
Published
2021

10. The SuperCam Instrument Suite on the NASA Mars 2020 Rover: Body Unit and Combined System Tests

Author

Francois Poulet, Nina Lanza, John Michel, Kerry Boyd, Valerie Mousset, Fernando Rull, Anupam K. Misra, Horton E. Newsom, Magdalena Dale, Richard Leveille, Sylvain Bernard, Karim Benzerara, Logan Ott, Timothy H. McConnochie, M. George Duran, Jonathan Deming, C. Glen Peterson, Jorden Celis, Juan Manuel Madariaga, Anthony Nelson, Elizabeth C. Auden, Violaine Sautter, Paolo Pilleri, Naomi Murdoch, Susanne Schröder, Joseph H. Sarrao, Miles Egan, Bruno Dubois, Ann Ollila, Roberta A. Klisiewicz, M. Deleuze, K. McCabe, Ryan B. Anderson, Kevin Clark, Noureddine Melikechi, Jens Frydenvang, Matthew R. Dirmyer, A. Regan, Pierre Beck, Olivier Forni, A. Reyes-Newell, David Mimoun, Lauren DeFlores, Stéphane Le Mouélic, Nicolas Mangold, Eric Lorigny, Denine Gasway, John P. Grotzinger, M. Caffrey, Shiv K. Sharma, J. Javier Laserna, Olivier Gasnault, Steven P. Love, Eric Lewin, Sophie Jacquinod, Jeffrey R. Johnson, Dorothea Delapp, Soren N. Madsen, James Lake, Kepa Castro, Joan Ervin, Olivier Beyssac, C. Donny, Yann Parot, J. P. Martinez, Pierre-Yves Meslin, Gabriel Pont, Jean-Michel Reess, L. Parès, P. Bernardi, D. Venhaus, Guillermo Lopez-Reyes, Benjamin Quertier, Gorka Arana, Morten Madsen, Ivair Gontijo, Ralph D. Lorenz, Philip J. Romano, Ian A. Trettel, S. Michael Angel, Gilles Montagnac, Joseph Becker, Vishnu Sridhar, Rafal Pawluczyk, Jérémie Lasue, P. Cais, William Rapin, Jose Antonio Manrique, Xavier Jacob, Clement Royer, Jacob Valdez, I. Torre-Fdez, Amaury Fau, Peter Willis, Louis Borges, Cheryl Provost, Elizabeth C. Cordoba, M. L. Underwood, Justin McGlown, Daniel Seitz, S. A. Storms, Briana Lucero, Heather Quinn, Thierry Fouchet, Raymond Newell, Cécile Fabre, B. Chide, Y. André, Jeffrey Carlson, Roger C. Wiens, Scott M. McLennan, Woodward W. Fischer, Benigno Sandoval, S. Robinson, Patrick Pinet, Samuel M. Clegg, Agnes Cousin, Sylvestre Maurice, Edward A. Cloutis, Gilles Dromart, Franck Montmessin, C. Legett, Andres Valdez, Bruno Bousquet, Reuben Fresquez, Terra Shepherd, Zachary R. Ousnamer, Pablo Sobron, M. Toplis, Marcel J. Schoppers, Jesús Martínez-Frías, D. T. Beckman, 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), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Hawai‘i [Mānoa] (UHM), Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Centre National d'Études Spatiales [Toulouse] (CNES), University of South Carolina [Columbia], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), University of Winnipeg, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), 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), California Institute of Technology (CALTECH), University of Copenhagen = Københavns Universitet (UCPH), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de mécanique des fluides de Toulouse (IMFT), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Universidad de Valladolid [Valladolid] (UVa), Universidad de Málaga [Málaga] = University of Málaga [Málaga], McGill University = Université McGill [Montréal, Canada], Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Maryland [College Park], University of Maryland System, State University of New York (SUNY), University of Massachusetts [Lowell] (UMass Lowell), University of Massachusetts System (UMASS), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), The University of New Mexico [Albuquerque], Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), FiberTech Optica (FTO), In­sti­tut für Op­ti­sche Sen­sor­sys­te­me, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), SETI Institute, Observatoire Midi-Pyrénées (OMP), 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 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), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Bordeaux (UB), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), 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), University of Copenhagen = Københavns Universitet (KU), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire de Planétologie et Géodynamique - Angers (LPG-ANGERS), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), 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), Institut Supérieur de l'Aéronautique et de l'Espace - ISAE-SUPAERO (FRANCE), and Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Mars, 01 natural sciences, 7. Clean energy, Article, law.invention, Telescope, symbols.namesake, Jezero crater, Optics, ChemCam instrument, law, Microphone on Mars, 0103 physical sciences, SuperCam, planetary exploration, luminescence, Traitement du signal et de l'image, Perseverance rover, Spectroscopy, 010303 astronomy & astrophysics, Infrared spectroscopy, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, laboratory curiosity rover, remote Raman system, LIBS, Spectrometer, business.industry, Detector, Astronomy and Astrophysics, Mars Exploration Program, Gale crater, Laser, induced breakdown spectroscopy, Wavelength, in-situ, mission, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Raman spectroscopy, symbols, business
Abstract

The SuperCam instrument suite provides the Mars 2020 rover, Perseverance, with a number of versatile remote-sensing techniques that can be used at long distance as well as within the robotic-arm workspace. These include laser-induced breakdown spectroscopy (LIBS), remote time-resolved Raman and luminescence spectroscopies, and visible and infrared (VISIR; separately referred to as VIS and IR) reflectance spectroscopy. A remote micro-imager (RMI) provides high-resolution color context imaging, and a microphone can be used as a stand-alone tool for environmental studies or to determine physical properties of rocks and soils from shock waves of laser-produced plasmas. SuperCam is built in three parts: The mast unit (MU), consisting of the laser, telescope, RMI, IR spectrometer, and associated electronics, is described in a companion paper. The on-board calibration targets are described in another companion paper. Here we describe SuperCam's body unit (BU) and testing of the integrated instrument. The BU, mounted inside the rover body, receives light from the MU via a 5.8 m optical fiber. The light is split into three wavelength bands by a demultiplexer, and is routed via fiber bundles to three optical spectrometers, two of which (UV and violet; 245-340 and 385-465 nm) are crossed Czerny-Turner reflection spectrometers, nearly identical to their counterparts on ChemCam. The third is a high-efficiency transmission spectrometer containing an optical intensifier capable of gating exposures to 100 ns or longer, with variable delay times relative to the laser pulse. This spectrometer covers 535-853 nm ( 105 - 7070 cm − 1 Raman shift relative to the 532 nm green laser beam) with 12 cm − 1 full-width at half-maximum peak resolution in the Raman fingerprint region. The BU electronics boards interface with the rover and control the instrument, returning data to the rover. Thermal systems maintain a warm temperature during cruise to Mars to avoid contamination on the optics, and cool the detectors during operations on Mars. Results obtained with the integrated instrument demonstrate its capabilities for LIBS, for which a library of 332 standards was developed. Examples of Raman and VISIR spectroscopy are shown, demonstrating clear mineral identification with both techniques. Luminescence spectra demonstrate the utility of having both spectral and temporal dimensions. Finally, RMI and microphone tests on the rover demonstrate the capabilities of these subsystems as well., Proyecto MINECO Retos de la Sociedad. Ref. ESP2017-87690-C3-1-R

Published
2021

11. Tardi-magmatic precipitation of Cl-bearing Fe/Mg clay minerals on Mars

Author

Roger H. Hewins, Laurent Remusat, Brigitte Zanda, Sylvain Bernard, Corentin Le Guillou, Philippe Schmitt-Kopplin, Jean-Christophe Viennet, Violaine Sautter, Olivier Beyssac, Sylvain Courrech du Pont, Albert Jambon, and Brian Grégoire

Subjects
Bearing (mechanical), Chemistry, law, Geochemistry, Mars Exploration Program, Precipitation, Clay minerals, law.invention
Published
2021

12. Marble quarries in Delos Island (Greece): a geological characterization

Author

Tommy Vettor, Violaine Sautter, Laurent Jolivet, Jean-Charles Moretti, Sylvain Pont, Institut de recherche sur l'architecture antique (IRAA), and Université Lumière - Lyon 2 (UL2)-Aix Marseille Université (AMU)-Université de Pau et des Pays de l'Adour (UPPA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SHS.ARCHI]Humanities and Social Sciences/Architecture, space management, [SHS.ARCHEO]Humanities and Social Sciences/Archaeology and Prehistory, Geology, [SHS.ART]Humanities and Social Sciences/Art and art history, [SHS.HIST]Humanities and Social Sciences/History, [SHS.CLASS]Humanities and Social Sciences/Classical studies
Abstract

International audience; Traces of extraction in Delian marble quarries attest their exploitation during Antiquity. A preliminary non-destructive provenance study confirmed the presence of indigenous marble in Delos constructions. In contrast, Delos marble quarries have not been geochemically described so far. Therefore, a detailed (1/5000 scale) geological mapping and cross-sections were performed in the four Delian marble quarries in order to better determine their dimension and to estimate the volume of extracted marble. The surface of the quarries was revised into up to six times larger areas, increasing the extracted volume estimations. Quarries were sampled and studied with mineralo-petrographic (optical and electronic microscopy, X-Ray Diffraction) and isotopic (δ 13 C and δ 18 O) characterization. Three categories were observed, i.e. , a coarse whitish to bluish marble, a fine yellowish dolomitic marble and marble with giant white and blue calcite crystals. The Maximum Grain Size associated with oxygen and carbon isotopic ratios showed a good potential to distinguish Delian marbles from most of the main Mediterranean marbles used during Antiquity. However, geochemical elemental analyses such as trace elements analysis could supplement Delian marble characterization which will benefit future provenance studies.; Des traces d’extraction dans les carrières de marbre de Délos attestent de leur exploitation durant l’Antiquité. Une première étude géochimique non destructive a permis d’identifier du marbre dans les constructions de Délos. Toutefois les carrières n’avaient jamais fait l’objet d’une étude géochimique détaillée jusque-là. Par conséquent, une carte géologique détaillée (échelle 1/5000) ainsi que des coupes géologiques ont été réalisées dans les quatre carrières de marbre afin de mieux cerner la dimension des carrières et les volumes de marbre qui en ont été extraits. La surface des carrières a été largement revue à la hausse, atteignant jusqu’à six fois la surface de la précédente cartographie des carrières, ce qui augmente donc considérablement le volume théorique de marbre extrait à Délos. Les carrières ont été échantillonnées et étudiées par une caractérisation minéralo-pétrographique (microscopie optique et électronique, diffraction de rayons X) et isotopique (δ 13 C et δ 18 O). Trois catégories ont été observées, à savoir un marbre grossier blanchâtre à bleuté, un marbre dolomitique jaunâtre fin et un marbre à cristaux géants de calcite blanche et bleue. La taille maximale des grains associée aux rapports isotopiques de l’oxygène et du carbone ont montré un bon potentiel pour distinguer les marbres déliens de la plupart des principaux marbres Méditerranéens utilisés durant l’Antiquité. Cependant, des analyses géochimiques élémentaires comme l’analyse des éléments traces dans la calcite/dolomite pourraient apporter des éléments discriminants dans la caractérisation des marbres autochtones, ce qui profitera à de futures études de provenance des marbres.

Published
2022

13. Tardi-magmatic precipitation of Martian Fe/Mg-rich clay minerals via igneous differentiation

Author

Jean-Christophe Viennet, C. Le Guillou, Brigitte Zanda, Violaine Sautter, Olivier Beyssac, Sylvain Courrech du Pont, P. Schmitt-Kopplin, R. H. Hewins, Sylvain Bernard, Laurent Remusat, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Unité Matériaux et Transformations - UMR 8207 (UMET), Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Centrale Lille Institut (CLIL)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), German Research Center for Environmental Health - Helmholtz Center München (GmbH), French National Research Agency (ANR) Region Ile-de-FranceI-07-593/RCentre National de la Recherche Scientifique (CNRS) Centre National de la Recherche Scientifique (CNRS) UPMC-Paris 6 French National Research Agency (ANR)ANR07-BLAN-0124-01Chevreul Institute European Union (EU) Region Hauts-de-France, Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Centrale Lille Institut (CLIL), Centrale Lille-Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Université de Lille, CNRS, INRA, ENSCL, Institut de minéralogie, de physique des matériaux et de cosmochimie [IMPMC], and Unité Matériaux et Transformations - UMR 8207 [UMET]

Subjects
010504 meteorology & atmospheric sciences, Geochemistry, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, [PHYS.PHYS.PHYS-GEO-PH]Physics [physics]/Physics [physics]/Geophysics [physics.geo-ph], 01 natural sciences, Petrography, Geochemistry and Petrology, 0103 physical sciences, Environmental Chemistry, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Basalt, Martian, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], magmatic precipitation, clay minerals, Noachian, Geology, Mars Exploration Program, [CHIM.MATE]Chemical Sciences/Material chemistry, Meteorite, [SDU]Sciences of the Universe [physics], [PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], Igneous differentiation, Clay minerals, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Mars is seen as a basalt covered world that has been extensively altered through hydrothermal or near surface water-rock interactions. As a result, all the Fe/Mg-rich clay minerals detected from orbit so far have been interpreted as secondary, i.e. as products of aqueous alteration of pre-existing silicates by (sub)surface water. Based on the fine scale petrographic study of the evolved mesostasis of the Nakhla meteorite, we report here the presence of primary Fe/Mg-rich clay minerals that directly precipitated from a water-rich fluid exsolved from the Cl-rich parental melt of nakhlites during igneous differentiation. Such a tardi-magmatic precipitation of clay minerals requires much lower amounts of water compared to production via aqueous alteration. Although primary Fe/Mg-rich clay minerals are minor phases in Nakhla, the contribution of such a process to Martian clay formation may have been quite significant during the Noachian given that Noachian magmas were richer in H 2 O. In any case, the present discovery justifies a re-evaluation of the exact origin of the clay minerals detected on Mars so far, with potential consequences for our vision of the early magmatic and climatic histories of Mars.

Published
2020

14. Caleta el Cobre 022 Martian meteorite: Increasing nakhlite diversity

Author

Bertrand Devouard, Vinciane Debaille, R. Martinez, Violaine Sautter, P. G. Beck, Jérôme Gattacceca, Colin Maden, Arya Udry, Lydie Bonal, Henner Busemann, L. Krämer Ruggiu, Matthias M. M. Meier, Geneviève Hublet, Pierre Rochette, Jean-Pierre Lorand, Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Institut National de la Recherche Agronomique (INRA), Aix Marseille Université (AMU), Université libre de Bruxelles (ULB), University of Hawai‘i [Mānoa] (UHM), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble [2020-....] (OSUG [2020-....]), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes [2020-....] (UGA [2020-....])-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes [2020-....] (UGA [2020-....]), Minéralogie, Pétrologie (MP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN), Planetary and Space Sciences Research Institute [Milton Keynes] (PSSRI), Centre for Earth, Planetary, Space and Astronomical Research [Milton Keynes] (CEPSAR), The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), University of Nevada [Las Vegas] (WGU Nevada), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes - Faculté d'Économie de Grenoble (UGA UFR FEG), Université Grenoble Alpes (UGA), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Laboratoire Géochimie, Traçage Isotopique, Minéral et élémentaire - G-Time (Bruxelles, Belgium), Belgian Federal Science Policy OfficeInstitut National des Sciences de l'Univers (INSU-France)Swiss National Science Foundation (SNSF)European Commission, ANR-16-CE31-0012,MARS-PRIME,Environnement Primitif de Mars(2016), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Collège de France (CdF (institution))-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Analytical, Environmental & Geo-Chemistry, and Chemistry

Subjects
Geochemistry, [SDU.STU.PE]Sciences of the Universe [physics]/Earth Sciences/Petrography, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Pyroxene, engineering.material, 010502 geochemistry & geophysics, 01 natural sciences, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Nakhlite, [SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, 0103 physical sciences, Plagioclase, 14. Life underwater, Géologie, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Olivine, Géochimie, Iddingsite, Geophysics, Augite, Meteorite, 13. Climate action, Space and Planetary Science, engineering, Phenocryst, Geology
Abstract

Caleta el Cobre (CeC) 022 is a Martian meteorite of the nakhlite group, showing an unbrecciated cumulate texture, composed mainly of clinopyroxene and olivine. Augite shows irregular core zoning, euhedral rims, and thin overgrowths enriched in Fe relative to the core. Low-Ca pyroxene is found adjacent to olivine. Phenocrysts of Fe-Ti oxides are titanomagnetite with exsolutions of ilmenite/ulvöspinel. Intercumulus material consists of both coarse plagioclase and fine-grained mesostasis, comprising K-feldspars, pyroxene, apatite, ilmenite, Fe-Ti oxides, and silica. CeC 022 shows a high proportion of Martian aqueous alteration products (iddingsite) in olivine (45.1 vol% of olivine) and mesostasis. This meteorite is the youngest nakhlite with a distinct Sm/Nd crystallization age of 1.215 ± 0.067 Ga. Its ejection age of 11.8 ± 1.8 Ma is similar to other nakhlites. CeC 022 reveals contrasted cooling rates with similarities with faster cooled nakhlites, such as Northwest Africa (NWA) 817, NWA 5790, or Miller Range 03346 nakhlites: augite irregular cores, Fe-rich overgrowths, fine-grained K-feldspars, quenched oxides, and high rare earth element content. CeC 022 also shares similarities with slower cooled nakhlites, including Nakhla and NWA 10153: pyroxene modal abundance, pyroxenes crystal size distribution, average pyroxene size, phenocryst mineral compositions, unzoned olivine, and abundant coarse plagioclase. Moreover, CeC 022 is the most magnetic nakhlite and represents an analog source lithology for the strong magnetization of the Martian crust. With its particular features, CeC 022 must originate from a previously unsampled sill or flow in the same volcanic system as the other nakhlites, increasing Martian sample diversity and our knowledge of nakhlites., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2020

15. Diagenetic silica enrichment and late-stage groundwater activity in Gale crater, Mars

Author

Violaine Sautter, N. Mangold, Horton E. Newsom, Insoo Jun, Fred Calef, Candice Bedford, P. Edwards, William Rapin, R. Gellert, Kenneth S. Edgett, David T. Vaniman, Lucy M. Thompson, P. Y. Meslin, J. A. Watkins, Martin R. Fisk, Ryan B. Anderson, John Bridges, Melissa S. Rice, John P. Grotzinger, Jeffrey R. Johnson, Ralph E. Milliken, Nina Lanza, Patrick J. Gasda, Kjartan M. Kinch, Dawn Y. Sumner, B. C. Clark, Nathaniel Stein, David F. Blake, Morten Madsen, Sanjeev Gupta, Agnès Cousin, Ashwin R. Vasavada, Joel A. Hurowitz, I. G. Mitrofanov, Sylvestre Maurice, Jens Frydenvang, Roger C. Wiens, Samuel M. Clegg, Valerie Payre, Abigail A. Fraeman, Susanne P. Schwenzer, and J. Van Beek

Subjects
geography, geography.geographical_feature_category, 010504 meteorology & atmospheric sciences, Earth science, Bedrock, Geochemistry, Mars Exploration Program, Structural basin, 01 natural sciences, Deposition (geology), Diagenesis, Geophysics, 13. Climate action, 0103 physical sciences, General Earth and Planetary Sciences, Aeolian processes, Sedimentary rock, 010303 astronomy & astrophysics, Geology, Groundwater, 0105 earth and related environmental sciences
Abstract

Diagenetic silica enrichment in fracture-associated halos that crosscut lacustrine and unconformably overlying aeolian sedimentary bedrock is observed on the lower north slope of Aeolis Mons in Gale crater, Mars. The diagenetic silica enrichment is colocated with detrital silica enrichment observed in the lacustrine bedrock yet extends into a considerably younger, unconformably draping aeolian sandstone, implying that diagenetic silica enrichment postdates the detrital silica enrichment. A causal connection between the detrital and diagenetic silica enrichment implies that water was present in the subsurface of Gale crater long after deposition of the lacustrine sediments and that it mobilized detrital amorphous silica and precipitated it along fractures in the overlying bedrock. Although absolute timing is uncertain, the observed diagenesis likely represents some of the most recent groundwater activity in Gale crater and suggests that the timescale of potential habitability extended considerably beyond the time that the lacustrine sediments of Aeolis Mons were deposited.

Published
2017

16. Alkali trace elements in Gale crater, Mars, with ChemCam: Calibration update and geological implications

Author

Ann Ollila, Jérémie Lasue, Marion Nachon, Roger C. Wiens, Samuel M. Clegg, Olivier Forni, Olivier Gasnault, N. Mangold, Nina Lanza, Agnes Cousin, L. Le Deit, Violaine Sautter, P. Y. Meslin, Sylvestre Maurice, Valerie Payre, Cécile Fabre, and W. Rapin

Subjects
010504 meteorology & atmospheric sciences, Calibration (statistics), Gale crater, Mineralogy, Weathering, Mars Exploration Program, Alkali metal, 01 natural sciences, Trace (semiology), Geophysics, Space and Planetary Science, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Igneous differentiation, Laser-induced breakdown spectroscopy, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Published
2017

17. Copper enrichments in the Kimberley formation in Gale crater, Mars: Evidence for a Cu deposit at the source

Author

Walter Goetz, Marion Nachon, Jérémie Lasue, Laetitia Le Deit, William Rapin, Agnès Cousin, Pierre-Yves Meslin, B. C. Clark, Olivier Gasnault, Cécile Fabre, Nina Lanza, Olivier Forni, Sylvestre Maurice, Roger C. Wiens, Violaine Sautter, Nicolas Mangold, Valerie Payre, Rice University [Houston], 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), Muséum national d'Histoire naturelle (MNHN), Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Los Alamos National Laboratory (LANL), Institut de Radioprotection et de Sûreté Nucléaire (IRSN), Space Science Institute [Boulder] (SSI), 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), 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), and ANR-16-CE31-0012,MARS-PRIME,Environnement Primitif de Mars(2016)

Subjects
010504 meteorology & atmospheric sciences, Fracture (mineralogy), Geochemistry, chemistry.chemical_element, 01 natural sciences, Porphyry copper deposit, Hydrothermal alteration, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Impact crater, Kimberley, 0103 physical sciences, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, geography, geography.geographical_feature_category, Bedrock, Astronomy and Astrophysics, Mars Exploration Program, Gale crater, Copper, Igneous rock, chemistry, Copper deposit, 13. Climate action, Space and Planetary Science, ChemCam, Sedimentary rock, Geology
Abstract

International audience; Copper quantification with laser induced breakdown spectroscopy (LIBS) using a univariate calibration model enables the ChemCam instrument onboard the Curiosity rover to measure unusually elevated Cu concentrations in potassic sandstones and Mn-oxide-bearing fracture fills in the Kimberley region of Gale crater, Mars. Mostly, the copper phases occurring in sedimentary bedrock are associated with detrital silicates, including feldspars, pyroxenes and K-phyllosilicates, likely coming from a potassic igneous source near the northern crater rim, while those present in the fractures are likely adsorbed on the surface of manganese oxides. These two different mineralogical associations imply at least two distinct processes: Cu enrichment in bedrock at the source, likely during crystallization of the igneous silicates, and adsorption of Cu on Mn-oxides precipitated from groundwater that encountered oxidizing conditions within fractures in the bedrock. The potassic sediments enriched in copper may be evidence of a porphyry copper deposit or an impact-induced hydrothermal deposit in the source region.

Published
2019

18. Martian Eolian Dust Probed by ChemCam

Author

María Paz Zorzano, Erwin Dehouck, Gilles Berger, William Rapin, S. Le Mouélic, Olivier Gasnault, Jeffrey R. Johnson, P.-Y. Meslin, Horton E. Newsom, Olivier Forni, Javier Martin-Torres, Ann Ollila, Jérémie Lasue, N. Mangold, Nina Lanza, Claude d’Uston, Ruth A. Anderson, Agnes Cousin, Violaine Sautter, Morten Madsen, Cécile Fabre, Noureddine Melikechi, B. C. Clark, Diana L. Blaney, Walter Goetz, Sylvestre Maurice, Roger C. Wiens, Samuel M. Clegg, S. Schroeder, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, The University of New Mexico [Albuquerque], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Centre d'étude spatiale des rayonnements (CESR), Laboratoire Kastler Brossel (LKB (Jussieu)), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Optical Science Center for Applied Research (OSCAR), Delaware State University (DSU), Institute of Meteoritics [Albuquerque] (IOM), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Max-Planck-Institut für Sonnensystemforschung (MPS), Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Pierre et Marie Curie - Paris 6 (UPMC)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-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), and 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)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
Martian, 010504 meteorology & atmospheric sciences, Rock cycle, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, Mineralogy, Mars Exploration Program, 15. Life on land, 01 natural sciences, Atmosphere, Geophysics, [SDU]Sciences of the Universe [physics], ChemCam, 13. Climate action, Planet, 0103 physical sciences, General Earth and Planetary Sciences, Environmental science, Aeolian processes, dust, 010303 astronomy & astrophysics, Chemical composition, Volatiles, 0105 earth and related environmental sciences
Abstract

International audience; The ubiquitous eolian dust on Mars plays important roles in the current sedimentary and atmospheric processes of the planet. The ChemCam instrument retrieves a consistent eolian dust composition at the submillimeter scale from every first laser shot on Mars targets. Its composition presents significant differences with the Aeolis Palus soils and the Bagnold dunes as it contains lower CaO and higher SiO2. The dust FeO and TiO2 contents are also higher, probably associated with nanophase oxide components. The dust spectra show the presence of volatile elements (S and Cl), and the hydrogen content is similar to Bagnold sands but lower than Aeolis Palus soils. Consequently, the dust may be a contributor to the amorphous component of soils, but differences in composition indicate that the two materials are not equivalent. Plain Language Summary Eolian dust on Mars is very fine dust that covers the entire surface of the planet, gives it its typical red hue, and is mobilized by wind. It plays a significant role in the current rock cycle of the planet and for the temperature of the atmosphere. ChemCam uses a series of pulsed laser shots to analyze the chemical composition of target materials. Each first laser shot by ChemCam gives the composition of the deposited dust. These measurements have been constant over the duration of the Mars Science Laboratory mission. The dust is homogeneous at the millimeter scale (approximately the size of the ChemCam analysis spot). Compared to local soils and sands at Gale crater, the dust contains higher levels of iron and titanium, associated with volatile elements like hydrogen, sulfur, and chlorine. We infer from this difference that the dust does not entirely originate locally and may be part of a separate global cycle.

Published
2018

19. Oxidation of manganese in an ancient aquifer, Kimberley formation, Gale crater, Mars

Author

John P. Grotzinger, David T. Vaniman, Javier Martin-Torres, Fred Calef, Jeffrey R. Johnson, Kenneth S. Edgett, Cécile Fabre, Stéphane Le Mouélic, Jérémie Lasue, Susanne Schröder, Raymond E. Arvidson, Violaine Sautter, Ann Ollila, John L. Campbell, Jens Frydenvang, Jeff A. Berger, Nicolas Mangold, Allan H. Treiman, Craig Hardgrove, María Paz Zorzano, James F. Bell, Douglas W. Ming, Scott VanBommel, Agnes Cousin, Horton E. Newsom, Woodward W. Fischer, Nathan T. Bridges, Marie J. McBride, Olivier Forni, Michael C. Malin, Roger C. Wiens, Samuel M. Clegg, Richard V. Morris, Martin R. Fisk, Sylvestre Maurice, Scott M. McLennan, Ralf Gellert, Nina Lanza, Benton C. Clark, Diana L. Blaney, Melissa S. Rice, Lucy M. Thompson, Joel A. Hurowitz, and Keian R. Hardy

Subjects
010504 meteorology & atmospheric sciences, Evaporite, Mineralogy, chemistry.chemical_element, Manganese, Mars Exploration Program, 01 natural sciences, Atmosphere, Geophysics, Planetary science, Deposition (aerosol physics), chemistry, 13. Climate action, 0103 physical sciences, General Earth and Planetary Sciences, Trace metal, 010303 astronomy & astrophysics, Earth (classical element), Geology, 0105 earth and related environmental sciences
Abstract

The Curiosity rover observed high Mn abundances (>25 wt % MnO) in fracture-filling materials that crosscut sandstones in the Kimberley region of Gale crater, Mars. The correlation between Mn and trace metal abundances plus the lack of correlation between Mn and elements such as S, Cl, and C, reveals that these deposits are Mn oxides rather than evaporites or other salts. On Earth, environments that concentrate Mn and deposit Mn minerals require water and highly oxidizing conditions; hence, these findings suggest that similar processes occurred on Mars. Based on the strong association between Mn-oxide deposition and evolving atmospheric dioxygen levels on Earth, the presence of these Mn phases on Mars suggests that there was more abundant molecular oxygen within the atmosphere and some groundwaters of ancient Mars than in the present day.

Published
2016

20. The potassic sedimentary rocks in Gale Crater, Mars, as seen by ChemCam on boardCuriosity

Author

Horton E. Newsom, Jérémie Lasue, K. M. Stack, Diana L. Blaney, Dawn Y. Sumner, Martin R. Fisk, William Rapin, S. Le Mouélic, Valerie Payre, Gilles Dromart, Scott M. McLennan, P. Y. Meslin, Allan H. Treiman, Olivier Gasnault, Ryan B. Anderson, Nina Lanza, Cécile Fabre, N. Mangold, Olivier Forni, Melissa S. Rice, S. Maurice, John P. Grotzinger, Susanne Schröder, Sanjeev Gupta, Violaine Sautter, Agnès Cousin, Roger C. Wiens, Samuel M. Clegg, L. Le Deit, and Marion Nachon

Subjects
Basalt, Martian, Olivine, 010504 meteorology & atmospheric sciences, Outcrop, Geochemistry, Crust, Mars Exploration Program, engineering.material, 01 natural sciences, On board, Geophysics, Space and Planetary Science, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), engineering, Sedimentary rock, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

Key Points: • Mean K2O abundance in sedimentary rocks >5 times higher than that of the average Martian crust • Presence of alkali feldspars and K-phyllosilicates in basaltic sedimentary rocks along the traverse • The K-bearing minerals likely have a detrital origin

Published
2016

21. Chemical variations in Yellowknife Bay formation sedimentary rocks analyzed by ChemCam on board the Curiosity rover on Mars

Author

Horton E. Newsom, Fred Calef, Mariek E. Schmidt, Linda C. Kah, Gilles Dromart, Gilles Berger, James F. Bell, Jérémie Lasue, Cécile Fabre, Ryan B. Anderson, S. Le Mouélic, Nina Lanza, A. Mezzacappa, Olivier Forni, Ann Ollila, Sanjeev Gupta, Sylvestre Maurice, K. E. Herkenhoff, Olivier Gasnault, Agnes Cousin, Martin R. Fisk, Scott M. McLennan, Claude d’Uston, Eric Lewin, John Bridges, Jeffrey R. Johnson, Ralph E. Milliken, Susanne Schröder, B. L. Barraclough, John P. Grotzinger, Marion Nachon, Noureddine Melikechi, Rebecca M. E. Williams, Richard Leveille, Scott K. Rowland, K. M. Stack, Diana L. Blaney, P.-Y. Meslin, Bethany L. Ehlmann, Dawn Y. Sumner, D. T. Vaniman, Michael C. Malin, Roger C. Wiens, Samuel M. Clegg, Lauren A. Edgar, B. C. Clark, N. Mangold, Violaine Sautter, Kenneth S. Edgett, Joel A. Hurowitz, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Space Remote Sensing Group (ISR-2), Los Alamos National Laboratory (LANL), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), United States Geological Survey [Reston] (USGS), Planetary Science Institute [Tucson] (PSI), ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Space Research Centre [Leicester], University of Leicester, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Science Institute [Boulder] (SSI), 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), College of Earth, Ocean and Atmospheric Sciences [Corvallis] (CEOAS), Oregon State University (OSU), Department of Earth Science and Technology [Imperial College London], Imperial College London, Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), College of Marine and Environmental Sciences [Cairns], James Cook University (JCU), C2O Consulting, Department of Natural Resource Sciences, McGill University = Université McGill [Montréal, Canada], Institut des Sciences de la Terre (ISTerre), Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), State University of New York (SUNY), Optical Science Center for Applied Research (OSCAR), Delaware State University (DSU), Department of Civil and Environmental Engineering and Earth Science [Notre Dame] (CEEES), University of Notre Dame [Indiana] (UND), Department of Earth and Planetary Sciences [Albuquerque] (EPS), The University of New Mexico [Albuquerque], Institute of Meteoritics [Albuquerque] (IOM), Muséum national d'Histoire naturelle (MNHN), Institut für Umweltphysik [Heidelberg], Universität Heidelberg [Heidelberg] = Heidelberg University, ICG-2, Centre d'étude spatiale des rayonnements (CESR), Centre for Ultrahigh Bandwidth Devices for Optical Systems (CUDOS), Macquarie University, Université d'Angers (UA)-Université de Nantes - Faculté des Sciences et des Techniques, Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), California Institute of Technology (CALTECH)-NASA, University of California [Davis] (UC Davis), University of California, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire de Photophysique et Photochimie Supramoléculaires et Macromoléculaires (PPSM), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Cachan (ENS Cachan), Division of Geological and Planetary Sciences [Pasadena], Department of Physics and Materials Science & Centre for Functional Photonics (CFP), The University of Hong Kong (HKU), Astrogeology Science Center [Flagstaff], Centre for Infection and Immunity, Canadian Space Agency (CSA), Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), University of Hawaii, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), 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), 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), 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), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Berkeley], University of California-University of California, 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), Universität Heidelberg [Heidelberg], Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, and 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)

Subjects
LIBS, Outcrop, Earth science, sediments, Geochemistry, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Mars Exploration Program, Gale crater, Diagenesis, Sedimentary depositional environment, Geophysics, [SDU]Sciences of the Universe [physics], ChemCam, Space and Planetary Science, Geochemistry and Petrology, Stratigraphic section, Earth and Planetary Sciences (miscellaneous), Sedimentary rock, Lithification, ComputingMilieux_MISCELLANEOUS, Geology, Stratigraphic column
Abstract

International audience; The Yellowknife Bay formation represents a similar to 5m thick stratigraphic section of lithified fluvial and lacustrine sediments analyzed by the Curiosity rover in Gale crater, Mars. Previous works have mainly focused on the mudstones that were drilled by the rover at two locations. The present study focuses on the sedimentary rocks stratigraphically above the mudstones by studying their chemical variations in parallel with rock textures. Results show that differences in composition correlate with textures and both manifest subtle but significant variations through the stratigraphic column. Though the chemistry of the sediments does not vary much in the lower part of the stratigraphy, the variations in alkali elements indicate variations in the source material and/or physical sorting, as shown by the identification of alkali feldspars. The sandstones contain similar relative proportions of hydrogen to the mudstones below, suggesting the presence of hydrous minerals that may have contributed to their cementation. Slight variations in magnesium correlate with changes in textures suggesting that diagenesis through cementation and dissolution modified the initial rock composition and texture simultaneously. The upper part of the stratigraphy (similar to 1m thick) displays rocks with different compositions suggesting a strong change in the depositional system. The presence of float rocks with similar compositions found along the rover traverse suggests that some of these outcrops extend further away in the nearby hummocky plains.

Published
2015

22. Centimeter to decimeter hollow concretions and voids in Gale Crater sediments, Mars

Author

Ashwin R. Vasavada, John P. Grotzinger, William Rapin, S. Johnstone, Fred Calef, Valerie Payre, Ralph E. Milliken, Cécile Fabre, Scott K. Rowland, Kathryn M. Stack, Roger C. Wiens, Samuel M. Clegg, S. Schroeder, David T. Vaniman, Stéphane Le Mouélic, Diana L. Blaney, Susanne P. Schwenzer, Olivier Gasnault, Marion Nachon, Marjorie A. Chan, Olivier Forni, Walter Goetz, Sylvestre Maurice, Dorothy Z. Oehler, Jeffrey R. Johnson, Nicolas Mangold, B. C. Clark, Alberto G. Fairén, Agnes Cousin, David M. Rubin, Violaine Sautter, Los Alamos National Laboratory (LANL), The University of Chicago Medicine [Chicago], Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Centre for Earth, Planetary, Space and Astronomical Research [Milton Keynes] (CEPSAR), The Open University [Milton Keynes] (OU), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Department of Civil and Environmental Engineering and Earth Science [Notre Dame] (CEEES), University of Notre Dame [Indiana] (UND), Space Science Institute [Boulder] (SSI), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Planetary Science Institute [Tucson] (PSI), Department of Geology and Geophysics [Mānoa], University of Hawai‘i [Mānoa] (UHM), University of Utah, 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), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Observatoire Midi-Pyrénées (OMP), 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, Rice University [Houston], 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), University of California [Davis] (UC Davis), University of California (UC), 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), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Centre National de la Recherche Scientifique (CNRS), Institut National des Sciences de l'Univers (INSU), Centre National D'etudes Spatiales, NASA Mars Exploration Program in the US, Max Planck Institute for Solar System Research (MPS), 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), 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), Collège René Cassin, 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
010504 meteorology & atmospheric sciences, Geochemistry, Voids, Mars, engineering.material, 01 natural sciences, Astrobiology, Siderite, chemistry.chemical_compound, Spherules, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Concretion, 0103 physical sciences, Concretions, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Felsic, Nodules, Astronomy and Astrophysics, Gale crater, Diagenesis, Igneous rock, chemistry, Mars science laboratory, Space and Planetary Science, engineering, Pyrite, Mafic, Volcanic bomb, Geology
Abstract

International audience; Voids and hollow spheroids between ∼1 and 23 cm in diameter occur at several locations along the traverse of the Curiosity rover in Gale crater, Mars. These hollow spherical features are significantly different from anything observed in previous landed missions. The voids appear in dark-toned, rough-textured outcrops, most notably at Point Lake (sols 302–305) and Twin Cairns Island (sol 343). Point Lake displays both voids and cemented spheroids in close proximity; other locations show one or the other form. The spheroids have 1–4 mm thick walls and appear relatively dark-toned in all cases, some with a reddish hue. Only one hollow spheroid (Winnipesaukee, sol 653) was analyzed for composition, appearing mafic (Fe-rich), in contrast to the relatively felsic host rock. The interior surface of the spheroid appears to have a similar composition to the exterior with the possible exceptions of being more hydrated and slightly depleted in Fe and K. Origins of the spheroids as Martian tektites or volcanic bombs appear unlikely due to their hollow and relatively fragile nature and the absence of in-place clearly igneous rocks. A more likely explanation to both the voids and the hollow spheroids is reaction of reduced iron with oxidizing groundwater followed by some re-precipitation as cemented rind concretions at a chemical reaction front. Although some terrestrial concretion analogs are produced from a precursor siderite or pyrite, diagenetic minerals could also be direct precipitates for other terrestrial concretions. The Gale sediments differ from terrestrial sandstones in their high initial iron content, perhaps facilitating a higher occurrence of such diagenetic reactions

Published
2017

23. Trace element geochemistry (Li, Ba, Sr, and Rb) usingCuriosity's ChemCam: Early results for Gale crater from Bradbury Landing Site to Rocknest

Author

Ryan B. Anderson, Olivier Forni, Ann Ollila, Penelope L. King, Noureddine Melikechi, Josh Williams, B. L. Barraclough, Scott M. McLennan, M. Darby Dyar, Benton C. Clark, Dorothea Delapp, Jérémie Lasue, Eric Lewin, Anya Rosen-Gooding, Horton E. Newsom, Olivier Gasnault, J. G. Blank, John Campbell, John Bridges, Nina Lanza, Sylvestre Maurice, R. L. Tokar, Violaine Sautter, Nicolas Mangold, Agnes Cousin, Cécile Fabre, Pierre-Yves Meslin, S. Johnstone, Roger C. Wiens, Samuel M. Clegg, G. M. Perrett, and D. T. Vaniman

Subjects
010504 meteorology & atmospheric sciences, Trace element, Geochemistry, Mineralogy, Mars Exploration Program, 010502 geochemistry & geophysics, Feldspar, 01 natural sciences, Mars rover, Geophysics, Bradbury Landing, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, visual_art, Rocknest, Earth and Planetary Sciences (miscellaneous), visual_art.visual_art_medium, Igneous differentiation, Laser-induced breakdown spectroscopy, Geology, 0105 earth and related environmental sciences
Abstract

The ChemCam instrument package on the Mars rover, Curiosity, provides new capabilities to probe the abundances of certain trace elements in the rocks and soils on Mars using the laser-induced breakdown spectroscopy technique. We focus on detecting and quantifying Li, Ba, Rb, and Sr in targets analyzed during the first 100 sols, from Bradbury Landing Site to Rocknest. Univariate peak area models and multivariate partial least squares models are presented. Li, detected for the first time directly on Mars, is generally low ( 100 ppm and >1000 ppm, respectively. These analysis locations tend to have high Si and alkali abundances, consistent with a feldspar composition. Together, these trace element observations provide possible evidence of magma differentiation and aqueous alteration.

Published
2014

24. Geochemical diversity in first rocks examined by the Curiosity Rover in Gale Crater: Evidence for and significance of an alkali and volatile-rich igneous source

Author

Kevin W. Lewis, A. Olilla, Michelle E. Minitti, L. A. Leshin, I. Pradler, Roger C. Wiens, Scott VanBommel, Olivier Forni, Penelope L. King, K. M. Stack, Diana L. Blaney, John Bridges, G. M. Perrett, Edward M. Stolper, S. W. Squyres, Mariek E. Schmidt, B. Elliott, D. W. Ming, Jeff A. Berger, Allan H. Treiman, Scott M. McLennan, Fred Calef, Bethany L. Ehlmann, John P. Grotzinger, Violaine Sautter, Horton E. Newsom, Lucy M. Thompson, Ralf Gellert, Lauren A. Edgar, John Campbell, and Joel A. Hurowitz

Subjects
Basalt, 010504 meteorology & atmospheric sciences, Water on Mars, Partial melting, Mineralogy, Pyroclastic rock, Weathering, 01 natural sciences, Igneous rock, Geophysics, Meteorite, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Composition of Mars, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

The first four rocks examined by the Mars Science Laboratory Alpha Particle X-ray Spectrometer indicate that Curiosity landed in a lithologically diverse region of Mars. These rocks, collectively dubbed the Bradbury assemblage, were studied along an eastward traverse (sols 46–102). Compositions range from Na- and Al-rich mugearite Jake_Matijevic to Fe-, Mg-, and Zn-rich alkali-rich basalt/hawaiite Bathurst_Inlet and span nearly the entire range in FeO* and MnO of the data sets from previous Martian missions and Martian meteorites. The Bradbury assemblage is also enriched in K and moderately volatile metals (Zn and Ge). These elements do not correlate with Cl or S, suggesting that they are associated with the rocks themselves and not with salt-rich coatings. Three out of the four Bradbury rocks plot along a line in elemental variation diagrams, suggesting mixing between Al-rich and Fe-rich components. ChemCam analyses give insight to their degree of chemical heterogeneity and grain size. Variations in trace elements detected by ChemCam suggest chemical weathering (Li) and concentration in mineral phases (e.g., Rb and Sr in feldspars). We interpret the Bradbury assemblage to be broadly volcanic and/or volcaniclastic, derived either from near the Gale crater rim and transported by the Peace Vallis fan network, or from a local volcanic source within Gale Crater. High Fe and Fe/Mn in Et_Then likely reflect secondary precipitation of Fe^(3+) oxides as a cement or rind. The K-rich signature of the Bradbury assemblage, if igneous in origin, may have formed by small degrees of partial melting of metasomatized mantle.

Published
2014

25. Characteristics of pebble- and cobble-sized clasts along the Curiosity rover traverse from Bradbury Landing to Rocknest

Author

Penelope L. King, Violaine Sautter, S. Le Mouélic, James B. Garvin, A. Koefoed, Marisa C. Palucis, Nicolas Mangold, Roger C. Wiens, Victoria E. Hamilton, Horton E. Newsom, Robert G. Deen, J. K. Jensen, Nathan T. Bridges, Jack D. Farmer, Morten Madsen, V. Hipkin, John Bridges, R. A. Yingst, Linda C. Kah, Rebecca M. E. Williams, Walter Goetz, E. McCartney, S. Maurice, Oleg Pariser, Olivier Gasnault, and Jesús Martínez-Frías

Subjects
education.field_of_study, Cobble, Population, Geochemistry, Porphyritic, Geophysics, Bradbury Landing, Impact crater, Space and Planetary Science, Geochemistry and Petrology, Rocknest, Earth and Planetary Sciences (miscellaneous), Pebble, education, Ejecta, Geomorphology, Geology
Abstract

[1] We have assessed the characteristics of clasts along Curiosity's traverse to shed light on the processes important in the genesis, modification, and transportation of surface materials. Pebble- to cobble-sized clasts at Bradbury Landing, and subsequently along Curiosity's traverse to Yellowknife Bay, reflect a mixing of two end-member transport mechanisms. The general clast population likely represents material deposited via impact processes, including meteorite fragments, ejecta from distant craters, and impactites consisting of shocked and shock-melted materials from within Gale Crater, which resulted predominantly in larger, angular clasts. A subset of rounded pebble-sized clasts has likely been modified by intermittent alluvial or fluvial processes. The morphology of this rounded clast population indicates that water was a more important transporting agent here than at other Mars sites that have been studied in situ. Finally, we identified populations of basalt clasts and porphyritic clasts of undetermined composition by their morphologic and textural characteristics; basalts are confirmed by geochemical data provided by ChemCam.

Published
2013

26. The petrological expression of early Mars volcanism

Author

Michael J. Toplis, David Baratoux, Violaine Sautter, and Marc Monnereau

Subjects
Martian, 010504 meteorology & atmospheric sciences, Amazonian, Geochemistry, Noachian, Crust, Mars Exploration Program, Pyroxene, 01 natural sciences, Mantle (geology), Geophysics, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Hesperian, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

[1] Crystallization products of liquids produced by partial melting of a possible Martian mantle for conditions covering the earliest Noachian era to the most recent Amazonian times have been modeled using the MELTS thermodynamic calculator. The results imply a transition from low-calcium pyroxene dominated assemblages in the Noachian to high-calcium pyroxene assemblages in the Hesperian and Amazonian, which is remarkably consistent with observations made by orbiting visible and near-infrared spectrometers. This transition is interpreted as the consequence of the thermal evolution of the mantle, with no need for exotic conditions, such as higher water content or nonchondritic Ca/Al ratio of the mantle source, to produce low-calcium pyroxene rich lithologies. Our results are compatible with numerical models of the thermal evolution of Mars that predict high production rates of crust on early Mars, implying that Noachian rocks exposed at the surface may be petrological expressions of this volcanism rather than being associated with mantle overturn following the crystallization of a magma ocean.

Published
2013

27. Northwest Africa 5790: Revisiting Nakhlite Petrogenesis

Author

Omar Boudouma, J. Gattacceca, Albert Jambon, Violaine Sautter, Pierre Rochette, Dominique Badia, Jean-Alix Barrat, Bertrand Devouard, Institut des Sciences de la Terre de Paris (iSTeP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), 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), Domaines Océaniques (LDO), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Brest (UBO)-Observatoire des Sciences de l'Univers-Institut d'écologie et environnement-Centre National de la Recherche Scientifique (CNRS), Centre européen de recherche et d'enseignement des géosciences de l'environnement (CEREGE), Institut de Recherche pour le Développement (IRD)-Institut National de la Recherche Agronomique (INRA)-Aix Marseille Université (AMU)-Collège de France (CdF (institution))-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Magmas et Volcans (LMV), Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Collège de France (CdF)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Institut National de la Recherche Agronomique (INRA), Centre National de la Recherche Scientifique (CNRS)-Université Jean Monnet [Saint-Étienne] (UJM)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Collège de France (CdF (institution))-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Recherche Agronomique (INRA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet [Saint-Étienne] (UJM)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Observatoire de Physique du Globe de Clermont-Ferrand (OPGC), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Olivine, 010504 meteorology & atmospheric sciences, Geochemistry, Pyroxene, Iddingsite, engineering.material, 010502 geochemistry & geophysics, Picrite basalt, 01 natural sciences, Augite, Geochemistry and Petrology, Nakhlite, [SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, Magma, engineering, Geology, 0105 earth and related environmental sciences, Petrogenesis
Abstract

International audience; Northwest Africa 5790, the latest nakhlite find, is composed of 58 vol.% augite, 6% olivine and 36% vitrophyric intercumulus material. Its petrology is comparable to previously discovered nakhlites but with key differences: (1) Augite cores display an unusual zoning between Mg# 54 and 60; (2) Olivine macrocrysts have a primary Fe-rich core composition (Mg#= 35); (3) the modal proportion of mesostasis is the highest ever described in a nakhlite; (4) It is the most magnetite-rich nakhlite, together with MIL 03346, and exhibits the least anisotropic fabric. Complex primary zoning in cumulus augite indicates resorption due to complex processes such as remobilization of former cumulates in a new magma batch. Textural relationships indicate unambiguously that olivine was growing around resorbed augite, and that olivine growth was continuous while pyroxene growth resumed at a final stage. Olivine core compositions (Mg#= 35) are out of equilibrium with the augite core compositions (Mg# 60-63) and with the previously inferred nakhlite parental magma (Mg#= 29). The presence of oscillatory zoning in olivine and augite precludes subsolidus diffusion that could have modified olivine compositions. NWA 5790 evidences at least two magma batches before eruption, with the implication that melt in equilibrium with augite cores was never in contact with olivine. Iddingsite is absent.

Published
2016

28. Composition of conglomerates analyzed by the Curiosity rover: Implications for Gale Crater crust and sediment sources

Author

Sylvestre Maurice, Cécile Fabre, Nicolas Mangold, Martin R. Fisk, Fred Calef, William Rapin, R. Gellert, Amy J. Williams, Olivier Gasnault, Gilles Dromart, Dawn Y. Sumner, Roger C. Wiens, Samuel M. Clegg, Rebecca M. E. Williams, P.-Y. Meslin, S. Le Mouélic, Marisa C. Palucis, Kirsten L. Siebach, Agnes Cousin, Lucy M. Thompson, K. M. Stack, Diana L. Blaney, William E. Dietrich, L. Le Deit, Ryan B. Anderson, Olivier Forni, John P. Grotzinger, A. Yingst, H. E. Newsom, Kenneth S. Edgett, Violaine Sautter, Linda C. Kah, Scott M. McLennan, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), DLR Institute of Planetary Research, German Aerospace Center (DLR), Los Alamos National Laboratory (LANL), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Oregon State University (OSU), Department of Physics [Guelph], University of Guelph, California Institute of Technology (CALTECH), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley], University of California-University of California, 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), Division of Geological and Planetary Sciences [Pasadena], University of California [Davis] (UC Davis), University of California, Planetary Science Institute [Tucson] (PSI), NASA-California Institute of Technology (CALTECH), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), 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), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), University of California (UC), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, Earth science, Geochemistry, sedimentary rocks, Mars, Igneous textures, 01 natural sciences, Conglomerate, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Felsic, fluvial, Crust, Gale Crater, Diagenesis, Igneous rock, Geophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Clastic rock, Sedimentary rock, Geology
Abstract

International audience; The Curiosity rover has analyzed various detrital sedimentary rocks at Gale Crater, among which fluvial and lacustrine rocks are predominant. Conglomerates correspond both to the coarsest sediments analyzed and the least modified by chemical alteration, enabling us to link their chemistry to that of source rocks on the Gale Crater rims. In this study, we report the results of six conglomerate targets analyzed by Alpha-Particle X-ray Spectrometer and 40 analyzed by ChemCam. The bulk chemistry derived by both instruments suggests two distinct end-members for the conglomerate compositions. The first group (Darwin type) is typical of conglomerates analyzed before sol 540; it has a felsic alkali-rich composition, with a Na2O/K2O\textgreater5. The second group (Kimberley type) is typical of conglomerates analyzed between sols 540 and 670 in the vicinity of the Kimberley waypoint; it has an alkali-rich potassic composition with Na2O/K2O\textless2. The variety of chemistry and igneous textures (when identifiable) of individual clasts suggest that each conglomerate type is a mixture of multiple source rocks. Conglomerate compositions are in agreement with most of the felsic alkali-rich float rock compositions analyzed in the hummocky plains. The average composition of conglomerates can be taken as a proxy of the average igneous crust composition at Gale Crater. Differences between the composition of conglomerates and that of finer-grained detrital sediments analyzed by the rover suggest modifications by diagenetic processes (especially for Mg enrichments in fine-grained rocks), physical sorting, and mixing with finer-grained material of different composition.

Published
2016

29. Hydration state of calcium sulfates in Gale crater, Mars: Identification of bassanite veins

Author

P.-Y. Meslin, Sylvestre Maurice, William Rapin, Violaine Sautter, D. Archer, D. T. Vaniman, Olivier Gasnault, Jérémie Lasue, Roger C. Wiens, Agnes Cousin, Elizabeth B. Rampe, Marion Nachon, Olivier Forni, N. Mangold, Susanne Schröder, German Martinez, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), and 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)

Subjects
Gypsum, 010504 meteorology & atmospheric sciences, Hydrogen, Geochemistry, Mineralogy, chemistry.chemical_element, Mars, bassanite, Calcium, engineering.material, 01 natural sciences, calcium sulfate, chemistry.chemical_compound, Bassanite, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), medicine, Dehydration, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Martian, Anhydrite, LIBS, Mars Exploration Program, medicine.disease, Geophysics, chemistry, Space and Planetary Science, ChemCam, [SDU]Sciences of the Universe [physics], hydrogen, engineering, Geology
Abstract

International audience; In-situ analyses reveal the presence of hydrogen within calcium sulfate veins crosscutting the sediments found in Gale crater. Laboratory experiments were performed to calibrate the hydrogen signal measured by laser induced breakdown spectroscopy (LIBS) in a range applicable to martian data. The analyses indicate that all veins targeted so far at Gale consist predominantly of bassanite which most likely formed by dehydration of gypsum. This scenario suggests that the percolating water produced gypsum, possibly by hydration of anhydrite in aqueous solution, and remained at temperatures below ∼60 °C at that time. Desiccating conditions followed, consistent with a hyperarid climate and favored by burial or impacts. Additionally, anhydrite with lesser bassanite has been found by XRD in samples of sediments hosting the veins. Our result suggests bassanite is likely found in the veins and anhydrite may be more common as a fine-grained component within the sediments.

Published
2016

30. Laser induced breakdown spectroscopy library for the Martian environment

Author

Johan Mazoyer, Violaine Sautter, Olivier Gasnault, Roger C. Wiens, Agnès Cousin, Olivier Forni, Cécile Fabre, and Sylvestre Maurice

Subjects
Martian, Chemistry, Analytical chemistry, Atmosphere of Mars, Mars Exploration Program, Atomic and Molecular Physics, and Optics, Spectral line, Analytical Chemistry, Laser-induced breakdown spectroscopy, Emission spectrum, Spectroscopy, Instrumentation, Data reduction
Abstract

The NASA Mars Science Laboratory rover will carry the first Laser Induced Breakdown Spectroscopy experiment in space: ChemCam. We have developed a laboratory model which mimics ChemCam's main characteristics. We used a set of target samples relevant to Mars geochemistry, and we recorded individual spectra. We propose a data reduction scheme for Laser Induced Breakdown Spectroscopy data incorporating de-noising, continuum removal, and peak fitting. Known effects of the Martian atmosphere are confirmed with our experiment: better Signal-to-Noise Ratio on Mars compared to Earth, narrower peak width, and essentially no self-absorption. The wavelength shift of emission lines from air to Mars pressure is discussed. The National Institute of Standards and Technology vacuum database is used for wavelength calibration and to identify the elemental lines. Our Martian database contains 1336 lines for 32 elements: H, Li, Be, B, C, N, O, F, Na, Mg, Al, Si, P, S, Cl, K, Ar, Ca, Ti, V, Cr, Mn, Fe, Ni, Cu, Zn, As, Rb, Sr, Cs, Ba, and Pb. It is a subset of the National Institute of Standards and Technology database to be used for Martian geochemistry. Finally, synthetic spectra can be built from the Martian database. Correlation calculations help to distinguish between elements in case of uncertainty. This work is used to create tools and support data for the interpretation of ChemCam results.

Published
2011

31. Sulfide petrology of four nakhlites: Northwest Africa 817, Northwest Africa 998, Nakhla, and Governador Valadares

Author

Vincent Chevrier, Violaine Sautter, and Jean-Pierre Lorand

Subjects
chemistry.chemical_classification, Olivine, Sulfide, Chalcopyrite, Geochemistry, Mineralogy, engineering.material, Sulfide minerals, Geophysics, chemistry, Meteorite, Space and Planetary Science, Nakhlite, visual_art, engineering, visual_art.visual_art_medium, Pyrrhotite, Geology, Melt inclusions
Abstract

The nakhlites Martian meteorites contain small proportions of Cu-Fe-Ni sulfide minerals; we have studied these sulfides in Northwest Africa (NWA) 998, Nakhla, Governador Valadares, and NWA 817 with optical microscopy, scanning electron microscope, and electron microprobe. The meteorites studied are thought to derive from the bottom, inner part and top of hypothetical nakhlite lava flow(s), respectively. Modal abundances of magmatic sulfides, as estimated by image analysis on thin section, are uniformly low (0.02 to 0.05 ± 0.03 vol%), i.e., a factor 5 lower than in shergottites. Sulfides occur within the glassy mesostasis, as composite two-phase Fe-Ti oxide-sulfide grains, intimately associated with interstitial grains or locally enclosed in postcumulus melt inclusions (e.g., Governador Valadares) in olivine. They exhibit a uniform low-Ni monoclinic pyrrhotite composition ± chalcopyrite. There is a gradation of sulfide grain sizes and textures across the nakhlites flow(s): droplets in NWA 817, resorbed blebs in Governador Valadares; more massive, true intercumulus blebs in Nakhla and NWA 998. These nakhlites also show evidence for sulfide weathering. Hot desert finds (e.g., NWA 998 and NWA 817) show a few percent fracture-filling iron (oxy) hydroxides of likely terrestrial origin. Original sulfides are 50% altered in our NWA 998 section, with iron (oxy) hydroxides at grain boundaries and as complete pseudomorphs. The compositions of unaltered pyrrhotites are homogeneous, close to that of the monoclinic endmember Fe7S8, and are too sulfur-rich to have been in chemical equilibrium with the late-magmatic redox state fixed by the fayalite-magnetite-quartz buffer. Therefore, the compositions of the pyrrhotites must have been altered during the later stages of magmatic crystallization, by assimilation of S-rich regolith and hydrothermal circulation.

Published
2011

32. Onboard calibration igneous targets for the Mars Science Laboratory Curiosity rover and the Chemistry Camera laser induced breakdown spectroscopy instrument

Author

Olivier Forni, Sylvestre Maurice, Violaine Sautter, Agnès Cousin, Damien Guillaume, Roger C. Wiens, and Cécile Fabre

Subjects
Microprobe, Calibration curve, Chemistry, Mineralogy, Mars Exploration Program, Atomic and Molecular Physics, and Optics, Analytical Chemistry, Martian surface, Calibration, Laser-induced breakdown spectroscopy, Spectroscopy, Instrumentation, Chemical composition, Remote sensing
Abstract

article i nfo Accurate characterization of the Chemistry Camera (ChemCam) laser-induced breakdown spectroscopy (LIBS) on-board composition targets is of prime importance for the ChemCam instrument. The Mars Science Laboratory (MSL) science and operations teams expect ChemCam to provide the first compositional results at remote distances (1.5-7 m) during the in situ analyses of the Martian surface starting in 2012. Thus, establishing LIBS reference spectra from appropriate calibration standards must be undertaken diligently. Considering the global mineralogy of the Martian surface, and the possible landing sites, three specific compositions of igneous targets have been determined. Picritic, noritic, and shergottic glasses have been produced, along with a Macusanite natural glass. A sample of each target will fly on the MSL Curiosity rover deck, 1.56 m from the ChemCam instrument, and duplicates are available on the ground. Duplicates are considered to be identical, as the relative standard deviation (RSD) of the composition dispersion is around 8%. Electronic microprobe and laser ablation inductively coupled plasma mass spectrometry (LA ICP-MS) analyses give evidence that the chemical composition of the four silicate targets is very homogeneous at microscopic scales larger than the instrument spot size, with RSD b5% for concentration variations N0.1 wt.% using electronic microprobe, and b10% for concentration variations N0.01 wt.% using LA ICP-MS. The LIBS campaign on the igneous targets performed under flight-like Mars conditions establishes reference spectra for the entire mission. The LIBS spectra between 240 and 900 nm are extremely rich, hundreds of lines with high signal-to-noise, and a dynamical range sufficient to identify unambiguously major, minor and trace elements. For instance, a first LIBS calibration curve has been established for strontium from (Sr)=284 ppm to (Sr)=1480 ppm, showing the potential for the future calibrations for other major or minor elements.

Published
2011

33. Cooling rate of chondrules in ordinary chondrites revisited by a new geospeedometer based on the compensation rule

Author

Frédéric Béjina, Olivier Jaoul, and Violaine Sautter

Subjects
Olivine, Physics and Astronomy (miscellaneous), Thermodynamics, Mineralogy, Chondrule, Astronomy and Astrophysics, Forsterite, engineering.material, Geophysics, Meteorite, Space and Planetary Science, Planet, Chondrite, engineering, Formation and evolution of the Solar System, Diffusion (business), Geology
Abstract

For several decades efforts to constrain chondrite cooling rates from diffusion zoning in olivine gave rise to a range of values from 5 to 8400 K/h (Desch, S.J., Connolly Jr., H.C., 2002. A model for the thermal processing of particles in solar nebula shocks: application to cooling rates of chondrules. Meteorit. Planet. Sci. 37, 183–208; Greeney, S., Ruzicka, A., 2004. Relict forsterite in chondrules: implications for cooling rates. Lunar Planet. Sci. XXXV, abstract # 1246.). Such large uncertainties directly reflect the variability of diffusion data. Alternatively, from this variability results a compensation rule, log D 0 = a + bE (diffusion coefficients are written D = D 0 exp(− E / RT )). We test a new geospeemetry approach, based on this rule, on cooling of chondrules in chondrites, Sahara-97210 LL 3.2 and Wells LL 3.3. Greeney and Ruzicka (2004) matched Fe–Mg diffusion profiles in olivine from these chondrites with cooling rates between 200 and 6000 K/h. In our geospeedometry model, the use of the compensation rule greatly reduces the uncertainties by avoiding the choice of one diffusion coefficient among many. The cooling rates we found are between 700 and 3600 K/h for Sahara and 700–1600 K/h for Wells. Finally, we discuss the influence of our analytical model parameters on our cooling rate estimates.

Published
2009

34. New columnar texture of carbonado: Cathodoluminescence study

Author

Julien Barjon, Benjamin Rondeau, and Violaine Sautter

Subjects
Open fracture, Materials science, Mechanical Engineering, Carbonado, Diamond, Cathodoluminescence, General Chemistry, engineering.material, Electronic, Optical and Magnetic Materials, law.invention, Crystallography, law, Materials Chemistry, engineering, Grain boundary, Irradiation, Electrical and Electronic Engineering, Electron microscope, Spectroscopy
Abstract

We investigated a very unusual sample of carbonado by optical and electron microscopy, and cathodoluminescence imaging and spectroscopy. We observed two textures: a microporphyritic texture, and columnar transparent diamonds growing perpendicularly. We propose that this sample grew in three stages: the slow growth of large porphyrocrysts (step 1), followed by a fast growth period that produced the fine-grained cement (step 2), and ultimate growth of columnar diamond perpendicular to the initial material (step 3). The first two steps growth have been extensively documented in the literature, and the third one is described for the first time in carbonado. The classical texture suggests a growth from flowing fluids while the columnar texture evidences diamond development in an open fracture. The orange (N–V 0 center) and green (N 2 V center) cathodoluminescence observed around pores, grain boundaries and fractures throughout the sample is due to irradiation of uranium-rich fluids. As uranium was not mobile at the time of carbonado formation (between 3.8 and 2.6 Ga), we propose that irradiation occurred most likely long after diamond growth. The blue CL of the porphyrocrysts and of the columnar diamond, preserved from late transient irradiation, is due to N 3 V centers (and, to a lesser extent, N 2 V centers). It is a primary feature which reveals a certain degree of nitrogen aggregation. This is more likely related to some high-temperature events that remain to be determined.

Published
2008

35. ChemCam results from the Shaler outcrop in Gale crater, Mars

Author

Gilles Dromart, Kevin W. Lewis, S. Maurice, John Bridges, Susanne P. Schwenzer, Richard Leveille, Violaine Sautter, Jérémie Lasue, Ann Ollila, S. Le Mouélic, Martin R. Fisk, J. M. Williams, Marion Nachon, Ryan B. Anderson, Amy J. Williams, Juergen Schieber, Lauren A. Edgar, A. Mezzacappa, Olivier Forni, Roger C. Wiens, Samuel M. Clegg, Eric Lewin, Sanjeev Gupta, Olivier Gasnault, Nina Lanza, D. T. Vaniman, B. C. Clark, Diana L. Blaney, Nicolas Mangold, H. E. Newsom, Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Space Research Centre [Leicester], University of Leicester, Department of Earth and Planetary Sciences [Santa Cruz], University of California [Santa Cruz] (UCSC), University of California-University of California, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Department of Earth and Planetary Sciences [Albuquerque] (EPS), The University of New Mexico [Albuquerque], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), College of Earth, Ocean and Atmospheric Sciences [Corvallis] (CEOAS), Oregon State University (OSU), Department of Geological Sciences [Bloomington], Indiana University [Bloomington], Indiana University System-Indiana University System, Department of Earth Science and Technology [Imperial College London], Imperial College London, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), Optical Science Center for Applied Research (OSCAR), Delaware State University (DSU), 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Science Institute [Boulder] (SSI), Department of Natural Resource Sciences, McGill University = Université McGill [Montréal, Canada], Institut des Sciences de la Terre (ISTerre), Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Johns Hopkins University (JHU), Dept. of Physical Sciences, The Open University [Milton Keynes] (OU), Planetary Science Institute [Tucson] (PSI), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Université de Toulouse (UT), 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), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)

Subjects
Basalt, Outcrop, Geochemistry, Mars, Astronomy and Astrophysics, Pyroxene, surface Mineralogy, Feldspar, Astrobiology, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], visual_art, Stratigraphic section, Clastic dike, Facies, visual_art.visual_art_medium, Sedimentary rock, Geology, Spectroscopy
Abstract

International audience; The ChemCam campaign at the fluvial sedimentary outcrop ‘‘Shaler’’ resulted in observations of 28non-soil targets, 26 of which included active laser induced breakdown spectroscopy (LIBS), and all ofwhich included Remote Micro-Imager (RMI) images. The Shaler outcrop can be divided into seven faciesbased on grain size, texture, color, resistance to erosion, and sedimentary structures. The ChemCamobservations cover Facies 3 through 7. For all targets, the majority of the grains were below the limitof the RMI resolution, but many targets had a portion of resolvable grains coarser than 0.5 mm. The Shalerfacies show significant scatter in LIBS spectra and compositions from point to point, but several keycompositional trends are apparent, most notably in the average K2O content of the observed facies. Facies3 is lower in K2O than the other facies and is similar in composition to the ‘‘snake,’’ a clastic dike thatoccurs lower in the Yellowknife Bay stratigraphic section. Facies 7 is enriched in K2O relative to the otherfacies and shows some compositional and textural similarities to float rocks near Yellowknife Bay. Theremaining facies (4, 5, and 6) are similar in composition to the Sheepbed and Gillespie Lake members,although the Shaler facies have slightly elevated K2O and FeOT. Several analysis points within Shaler suggestthe presence of feldspars, though these points have excess FeOT which suggests the presence of Feoxide cement or inclusions. The majority of LIBS analyses have compositions which indicate that theyhttp://dx.doi.org/10.1016/j.icarus.2014.07.0250019-1035/Published by Elsevier Inc.⇑ Corresponding author.E-mail addresses: rbanderson@usgs.gov (R. Anderson), jcb36@leicester.ac.uk (J.C. Bridges), amywill@ucdavis.edu (A. Williams), ledgar1@asu.edu (L. Edgar), aollila@unm.edu (A. Ollila), josh505@unm.edu (J. Williams), marion.nach@gmail.com (M. Nachon), nicolas.mangold@univ-nantes.fr (N. Mangold), Martin.Fisk@oregonstate.edu (M. Fisk),jschiebe@indiana.edu (J. Schieber), s.gupta@imperial.ac.uk (S. Gupta), gilles.dromart@ens-lyon.fr (G. Dromart), rwiens@lanl.gov (R. Wiens), stephane.lemouelic@univ-nantes.fr (S. Le Mouélic), olivier.forni@irap.omp.eu (O. Forni), nlanza@lanl.gov (N. Lanza), amezzacappa09@students.desu.edu (A. Mezzacappa), vsautter@mnhn.fr (V. Sautter), diana.l.blaney@jpl.nasa.gov (D. Blaney), bclark@spacescience.org (B. Clark), sclegg@lanl.gov (S. Clegg), olivier.gasnault@irap.omp.eu (O. Gasnault), jeremie.lasue@irap.omp.eu (J.Lasue), rich.leveille@gmail.com (R. Léveillé), Eric.LEWIN@obs.ujf-grenoble.fr (E. Lewin), sylvestre.maurice@irap.omp.eu (S. Maurice), newsom@unm.edu (H. Newsom),dvaniman@psi.edu (D. Vaniman).Icarus 249 (2015) 2–21Contents lists available at ScienceDirectIcarusjournal homepage: www.elsevier.com/ locate/ icarusare mixtures of pyroxene and feldspar. The Shaler feldspathic compositions are more alkaline than typicalfeldspars from shergottites, suggesting an alkaline basaltic source region, particularly for the K2OenrichedFacies 7. Apart from possible iron-oxide cement, there is little evidence for chemical alterationat Shaler, although calcium-sulfate veins comparable to those observed lower in the stratigraphic sectionare present. The differing compositions, and inferred provenances at Shaler, suggest compositionally heterogeneousterrain in the Gale crater rim and surroundings, and intermittent periods of deposition

Published
2015

36. Hydrogen detection with ChemCam at Gale crater

Author

P.-Y. Meslin, Violaine Sautter, Jeffrey R. Johnson, William Rapin, N. Mangold, M. D. Dyar, S. Le Mouélic, Patrick Pinet, Olivier Forni, Sylvestre Maurice, Susanne Schröder, Ann Ollila, Agnes Cousin, Roger C. Wiens, Samuel M. Clegg, Olivier Gasnault, Marion Nachon, D. T. Vaniman, Jérémie Lasue, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Department of Astronomy, University of Massachusetts System (UMASS), 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), The University of New Mexico [Albuquerque], Technologies et systèmes d'information pour les agrosystèmes (UR TSCF), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC), Planetary Science Institute [Tucson] (PSI), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), 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), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Institute of Meteoritics [Albuquerque] (IOM), Muséum national d'Histoire naturelle (MNHN), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Université d'Angers (UA)-Université de Nantes - Faculté des Sciences et des Techniques, and 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)

Subjects
Felsic, Hydrogen, chemistry.chemical_element, Mineralogy, Astronomy and Astrophysics, Context (language use), Mars Exploration Program, Astrobiology, Diagenesis, Atmosphere, chemistry, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Mafic, Spectroscopy, Geology, ComputingMilieux_MISCELLANEOUS
Abstract

One of the main advantages of ChemCam’s LIBS (Laser-Induced Breakdown Spectroscopy) instrument onboard the Curiosity rover is its potential to detect light elements such as hydrogen at fine scales, which has never been achieved on Mars. Hydrogen lines are detected in most of the data obtained within the first 320 sols of the mission at Gale crater, Mars. This work is a description of the hydrogen signal and its variability in the ChemCam LIBS spectra; it discusses the challenges of qualitative and quantitative analysis. Data acquisition and processing steps are investigated and optimized for the detection of hydrogen on Mars. Subtraction of an appropriate dark spectrum and the deconvolution of the superimposed emission of carbon from the low-pressure CO2-dominated atmosphere are particularly important. Because the intensities of hydrogen are also affected by matrix effects, the hydrogen signal was investigated within groups of targets sharing common chemical features and similar matrices. The different groups cover a variety of rock and soil compositions encountered along the traverse (calcium sulfate veins, mafic soils, felsic, Mg-rich and Fe-rich rocks) including data from both drill holes and their tailings. Almost all these targets were found to be hydrated to variable extents. Soils have systematically higher hydrogen signals than rocks and pebbles, probably as a result of their alteration. The results from rocks suggest that various alteration processes leading to their hydration have taken place, which is consistent with the fluvial lacustrine context, the diagenetic features, and the mineralogy observed by Curiosity in Yellowknife Bay.

Published
2015

37. First detection of fluorine on Mars: Implications for Gale Crater's geochemistry

Author

Michael J. Toplis, Nina Lanza, M. D. Dyar, Sylvestre Maurice, Rhonda E. McInroy, Marion Nachon, Stéphane Le Mouélic, John Bridges, Violaine Sautter, Roger C. Wiens, Samuel M. Clegg, Nicolas Mangold, Ann Ollila, Agnes Cousin, Olivier Forni, Olivier Gasnault, Michael Gaft, Pierre-Yves Meslin, Institut de recherche en astrophysique et planétologie (IRAP), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Laser Distance Spectrometry, Petah Tikva, Los Alamos National Laboratory (LANL), 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), Muséum national d'Histoire naturelle (MNHN), Chevron Energy Technology Company, Space Research Centre [Leicester], University of Leicester, Department of Astronomy, University of Massachusetts System (UMASS), 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), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), 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), Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], Mount Holyoke College, 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
Mineral, Geochemistry, Mineralogy, chemistry.chemical_element, Gale crater, Mars Exploration Program, Low calcium, On board, Geophysics, chemistry, 13. Climate action, Aluminosilicate, [SDU.STU.GC]Sciences of the Universe [physics]/Earth Sciences/Geochemistry, [SDU]Sciences of the Universe [physics], Fluorine, General Earth and Planetary Sciences, High calcium, Geology
Abstract

International audience; Volatiles and especially halogens (F and Cl) have been recognized as important species in the genesis and melting of planetary magmas. Data from the Chemical Camera instrument on board the Mars Science Laboratory rover Curiosity now provide the first in situ analyses of fluorine at the surface of Mars. Two principal F-bearing mineral assemblages are identified. The first is associated with high aluminum and low calcium contents, in which the F-bearing phase is an aluminosilicate. It is found in conglomerates and may indicate petrologically evolved sources. This is the first time that such a petrologic environment is found on Mars. The second is represented by samples that have high calcium contents, in which the main F-bearing minerals are likely to be fluorapatites and/or fluorites. Fluorapatites are found in some sandstone and may be detrital, while fluorites are also found in the conglomerates, possibly indicating low-T alteration processes.

Published
2015

38. Cl-amphibole in the nakhlite MIL 03346: Evidence for sediment contamination in a Martian meteorite

Author

Albert Jambon, Omar Boudouma, and Violaine Sautter

Subjects
Meridiani Planum, Olivine, Geochemistry, engineering.material, Geophysics, Augite, Meteorite, Space and Planetary Science, Geochemistry and Petrology, Nakhlite, Earth and Planetary Sciences (miscellaneous), engineering, Halite, Phenocryst, Amphibole, Geology
Abstract

The Pathfinder, Spirit and Opportunity missions revealed that Martian soils and rocks are enriched in chlorine (up to 0.6 wt.% Cl). Significant piles of evaporitic sedimentary rocks have also been observed at Meridiani Planum. The SNC meteorites, inferred to come from Mars, hardly ever contain Cl-rich minerals except in secondary alteration products such as clay-rich veinlets and massive halite trapped within olivine from Nakhla. Here we describe the first extra-terrestrial Cl-rich amphibole, in the newly found nakhlite MIL 03346. It is a chloro-potassichastingsite (up to 8% Cl wt.%) that crystallized exclusively as a daughter mineral in some of the melt patches sequestered inside augite phenocryst clusters. It is never found as fracture-filling material nor as discrete grains in the mesostasis. This Cl-rich amphibole crystallized from the evolved residual liquid at some intermediate magmatic stage. This heterogeneous contamination at a magmatic stage provides the first evidence for contamination of a nakhlite parent magma by Cl-rich particles of evaporitic sediments. Such a contamination appears to be very limited to melt patches present in a small number of augite crystals. Because of dilution and devolatilization effects, this contamination remains cryptic in the mesostasis.

Published
2006

39. Synchrotron FTIR microanalysis of volatiles in melt inclusions and exsolved particles in ultramafic deep-seated garnets

Author

Nicole Guilhaumou, Violaine Sautter, and Paul Dumas

Subjects
Geochemistry and Petrology, Ultramafic rock, Transition zone, Partial melting, Geochemistry, Mineralogy, Geology, Xenolith, Pyroxene, Kimberlite, Mantle (geology), Melt inclusions
Abstract

Silicon-rich deep-seated garnets uplifted in the Jagersfontein kimberlite pipe (South Africa) are unique samples from the asthenospheric deep mantle (more than 300 km: [Haggerty, S.E., Sautter, V., 1990: Ultradeep (greater than 300 Kilometers) Ultramafic upper mantle Xenoliths. Science 248 993–996.]; [Sautter, V., Haggerty, S.E., Field, S., 1991. Ultradeep (> 300 Kilometres) Ultramafic Xenoliths: petrological evidence from the transition Zone. Science 252 827–830.]). During their complex multistage ascent from the asthenosphere through the lithosphere, they have preserved evidence of a variety of fluid-rock interactions ranging from deep mantle conditions to metasomatized lithospheric root zones and, finally, superficial alteration. Synchrotron Fourier Transform Infrared Microspectrometry (SFTIR; [Guilhaumou, N., Dumas, P., Carr, G.L., Williams, G.P., 1998. Synchrotron Infrared Microspectrometry applied to petrography in the micron scale range: fluid chemical analysis and mapping. Applied Spectroscopy 52 (8) 176–184.]) of primary and secondary melt inclusions combined with optical microscopy allow the recognition of two markedly different fluids at the micron scale in two representatives garnet samples from Jagerfontain xenoliths. Some primary melt inclusions (P1) form cloudy areas scattered in the garnets, representing an initial hydrated degassed glassy material that could result from an Early Partial Melting of the garnet host. Glassy material is also found as clusters of melt inclusion rimming orthopyroxene and clinopyroxene exsolved in these garnets. These inclusions (P2) probably result from volume change of the hydrated pyroxenes during ascent. The pyroxene exsolutions themselves contain significant amounts of water currently present as OH in their structure. The detection of OH dissolved in P1 and P2 melt inclusions (contained in nominally anhydrous pyroxene) is evidence for an unusual level of hydroxyl incorporation in the primary ultradeep garnet before exsolution, recording uplift from 300 km depth to the base of the lithosphere. A later fluid event is recognized from secondary melt inclusions (S-type) sometimes containing mechanically entrapped clinopyroxene and displaying typical “edge pitch” trails in the garnets. The S-type melt inclusions nucleated preferentially on pre-existing dislocations in garnets by late chemical alteration. These inclusions consist of a highly hydrated glassy phase containing CO 3 − ions, associated with a vapour phase with CO 2 and H 2 O. This fluid represents a carbonaceous magma rich in dissolved CO 2 . The CO 2 density of these gaseous phases measured by Raman microspectrometry shows that they were entrapped at shallow depth (0,4 GPa for 1000 °C). Some of this fluid material may be derived from carbonaceous magma, i.e. the host kimberlite or precursor fluids that metasomatized the pyroxene–garnet interface to produce tremolite (recognized by SFTIR) whilst the xenolith sample was in the lithosphere.

Published
2005

40. Sulfide mineralogy and redox conditions in some shergottites

Author

Jean-Pierre Lorand, Violaine Sautter, and Vincent Chevrier

Subjects
chemistry.chemical_classification, Olivine, Sulfide, Chalcopyrite, Pentlandite, Geochemistry, Cubanite, Mineralogy, engineering.material, Geophysics, chemistry, Space and Planetary Science, Mineral redox buffer, visual_art, engineering, visual_art.visual_art_medium, Pyrrhotite, Geology, Melt inclusions
Abstract

Magmatic sulfide mineralogy has been studied in 2 olivine-phyric shergottites (DaG 476 and SaU 005) and 4 basaltic shergottites (Zagami, Shergotty, Los Angeles, and NWA 480). Modal abundances of magmatic sulfides, as estimated by image analysis on thin section, are high (0.16 to 0.53 area percent) and correlate positively with abundances of Fe-Ti oxides. Sulfides are mesostasis minerals, being mostly interstitial grains or locally enclosed in post-cumulus melt inclusions (e.g., SaU 005) in olivine. Sulfides in shergottites are composed of major pyrrhotite containing pentlandite exsolutions associated with minor amounts of Cu sulfides (chalcopyrite and/or cubanite). Hot desert finds (e.g., DaG 476) show abundant fracture-filling iron (oxy)hydroxides of probable terrestrial origin. Unaltered sulfides show metal-rich hexagonal pyrrhotite compositions with metal/sulfur (M/ S) ratio ranging between 0.936 ± 0.005 and 0.962 ± 0.01. This compositional range corresponds to the two-phase structural domain 2C + nC of the Fe-S system; however, the high-temperature disordered hexagonal 1C pyrrhotite structure would be in better agreement with magnetic properties of shergottites. Ni contents in pyrrhotite increase from Los Angeles (

Published
2005

41. Petrology and geochemistry of the unbrecciated achondrite Northwest Africa 1240 (NWA 1240): an HED parent body impact melt

Author

Ph. Gillet, Albert Jambon, Janne Blichert-Toft, Jean-Alix Barrat, Christa Göpel, Violaine Sautter, Marcel Bohn, Omar Boudouma, and F. Keller

Subjects
Eucrite, Geochemistry, Mineralogy, Pyroxene, engineering.material, Troilite, Porphyritic, Geochemistry and Petrology, engineering, Plagioclase, Phenocryst, Pyroxferroite, Achondrite, Geology
Abstract

NWA 1240 is an unusual eucrite recently recovered in Morocco as a single stone of 98 g. It is an unbrecciated greenish-brown rock nearly devoid of fusion crust. It displays porphyritic texture consisting of skeletal hollow low-Ca pyroxene phenocrysts set in a variolitic (fan-spherulitic) mesostasis of fine elongate pyroxene and plagioclase crystals. Minor phases are skeletal chromite, iron, silica, troilite, ilmenite and minute amounts of phosphate and fayalite. Pyroxenes are unequilibrated and show one of the widest ranges of composition so far described for a eucrite, from En(76.0)Wo(1.9)FS(22.1) to compositions nearly devoid of Mg (unusual ferrosilite and Fe-augite symplectites and possibly pyroxferroite). Plagioclase crystals contain significant amounts of Fe and Mg, which are possibly controlled by the Ca(Mg,Fe2+)Si3O8 plagioclase component.

Published
2003

42. Combined in situ X-ray diffraction and Raman spectroscopy on majoritic garnet inclusions in diamonds

Author

Jeff W. Harris, Pamela Conrad, Guillaume Fiquet, Heinz Graafsma, Martin Kunz, Violaine Sautter, and Philippe Gillet

Subjects
Majorite, Analytical chemistry, Mineralogy, Pyroxene, majorite, engineering.material, omphacite, Transformation, symbols.namesake, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), diamond inclusions, Chemical composition, Diamond, Silicate, Solid-Solution, Geophysics, Space and Planetary Science, transition zone, X-ray crystallography, symbols, engineering, Mantle, Omphacite, Raman spectroscopy, Geology, Solid solution
Abstract

Mineral inclusions in Sao Luiz diamonds have been characterized using angle dispersive X-ray diffraction and Raman spectroscopy. We identified two different garnet phases coexisting with an omphacitic pyroxene. They represent disintegration products of a former homogeneous majorite-rich garnet phase. The two garnets have significantly different cell parameters but are tightly intergrown with their unit cells parallel to each other. The garnets are oriented relative to the diamond host with [100](garnet), parallel to [110](diamond). Combining the measured cell parameters of the garnet inclusions with chemical analyses of similar inclusions from the same source allows the extraction of a residual pressure between 1 and 3 GPa, depending on the exact chemical composition assumed. Depth-resolved Raman spectra at the diamond-garnet interface indicate a residual pressure of about 1 GPa, Such a low residual pressure is unexpected at first glance for a garnet assemblage from the transition zone. The inclusion pressure is lowered due to pyroxene crystals, which surround the garnet inclusions and act as cushions reducing the residual inclusion pressure. (C) 2002 Elsevier Science B.V. All rights reserved.

Published
2002

43. Petrology and chemistry of the basaltic shergottite North West Africa 480

Author

Jean-Alix Barrat, Violaine Sautter, M. Lesourd, F. Keller, Marc Javoy, Christa Göpel, Ph. Gillet, Albert Jambon, and E. Petit

Subjects
Nd Isotopic Systematics, Snc Meteorites, Basalt, Siderophile Elements, Geochemistry, Trace element, Mars, Mineralogy, Maskelynite, Pyroxene, engineering.material, Dar Al Gani-476, Bulk Chemistry, Geophysics, Meteorite, Zagami, Space and Planetary Science, Differentiation, Martian Meteorites, engineering, Fayalite, Plagioclase, Chromite, Crystallization, Geology
Abstract

North West Africa (NWA) 480 is a new martian meteorite of 28 g found in the Moroccan Sahara in November 2000. It consists mainly of large gray pyroxene crystals (the largest grains are up to 5 mm in length) and plagioclase converted to maskelynite. Excluding the melt pocket areas, modal analyses indicate the following mineral proportions: 72 vol% pyroxenes extensively zoned, 25% maskelynite, 1% phosphates (merrillite and chlorapatite), 1% opaque oxides (ilmenite, ulvospinel and chromite) and sulfides, and 1% others such as silica and fayalite. The compositional trend of NWA 480 pyroxenes is similar to that of Queen Alexandra Range (QUE) 94201 but in NWA 480 the pyroxene cores are more Mg-rich (En(77)-En(65)). Maskelynites display a limited zoning (An(42-50)Ab(54-48)Or(2-4)). Our observations suggest that NWA 480 formed from a melt with a low nuclei density at a slow cooling rate. The texture was achieved via a single-stage cooling where pyroxenes grew continuously. A similar model was previously proposed for QUE 94201 by McSween et al. (1996). NWA 480 is an Al-poor ferroan basaltic rock and resembles Zagami or Shergotty for major elements and compatible trace element abundances. The bulk rock analysis for oxygen isotopes yields Delta(17)O = +0.42parts per thousand, a value in agreement at the high margin, with those measured on other shergottites (Clayton and Mayeda, 1996; Romanek et al., 1998; Franchi et al., 1999). Its CI-normalized rare earth element pattern is similar to those of peridotitic shergottites such as Allan Hills (ALH)A77005, suggesting that these shergottites shared a similar parent liquid, or at least the same mantle source.

Published
2002

44. A new Martian meteorite from Morocco: the nakhlite North West Africa 817

Author

Marc Javoy, J. L. Joron, Jean-Pierre Lorand, Ph. Gillet, Albert Jambon, Violaine Sautter, M. Lesourd, and Jean-Alix Barrat

Subjects
Petrography, Geochemistry, Mars, Mineralogy, Cumulate rock, alteration, Pyroxene, engineering.material, Geochemistry and Petrology, Nakhlite, Chondrite, Systematics, Earth and Planetary Sciences (miscellaneous), skeletal titanomagnetite, SNC meteorites, Petrogenesis, Snc Meteorite, Abundances, Chondritic Meteorites, Olivine, Mineral, Geophysics, Augite, Meteorite, Space and Planetary Science, nakhlite, Parent Magma, Inclusions, engineering, Aqueous Alteration, Geology
Abstract

North West Africa (NWA 817) is a single stone of 104 g found in the Sahara (Morocco) by meteorite hunters in November 2000. The meteorite is an unbrecciated, medium-grained olivine-bearing clinopyroxenite with a cumulate texture. It consists of zoned euhedral subcalcic augite (Wo(42)En(38-22)F(20-36)), olivine spanning a wide range of compositions (from Fa(56) in the core to Fa(86)) With rare magmatic inclusions and an intercumulus mesostasis made of Fe-bearing albitic plagioclase, Si-rich glass, Ti-magnetite with unusual skeletal growth morphologies containing ilmenite exsolutions, acicular pyroxene, olivine and cristobalite. Trace minerals are sulfide droplets and Cl-apatite. Mineral modes (in vol%) are augite 69%, olivine 10%, mesostasis 20% and Fe-Ti oxides 1%. Pervasive alteration produced a reddish clay mineral (hydrous ferrous silicate) in both olivine crystals and the mesostasis. The major element composition of NWA 817 is very similar to that of the other nakhlites: high FeO, MgO and CaO concentrations reflect the abundance of cumulus augite and olivine. Key element ratios such as FeO/MnO (=37), Na/Al (=0.40), K/La (= 449), Ga/Al (= 3.9 X 10(-4)) and oxygen isotopic composition (Delta(17)O = +0.37parts per thousand) are clear evidence for a Martian origin. The incompatible trace element pattern as in Nakhla displays a strong light rare earth element enrichment relative to chondrite (La-n/Yb-n = 4.89). However, when compared to the other nakhlites, NWA 817 has specific features: (1) a higher modal proportion of mesostasis; (2) quench textures of Ti-magnetite and Fe-rich clinopyroxene; (3) more Mg-rich olivine core compositions whereas the augite core composition is identical for all nakhlites; (4) a stronger Fe enrichment toward crystal rims of these cumulus minerals. The intercumulus minerals (Ti-magnetite with skeletal growth morphology, acicular chains of clinopyroxene and Fe3+-rich feldspar) indicate rapid crystallization in response to a high degree of undercooling at the end of the sample story. (C) 2002 Elsevier Science B.V. All rights reserved.

Published
2002

45. In situ calibration using univariate analyses based on the onboard ChemCam targets: first prediction of Martian rock and soil compositions

Author

Agnes Cousin, Noureddine Melikechi, Ann Ollila, Jérémie Lasue, Olivier Forni, Olivier Gasnault, Sylvestre Maurice, Violaine Sautter, R. L. Tokar, D. T. Vaniman, Roger C. Wiens, Cécile Fabre, 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), Los Alamos National Laboratory (LANL), The University of New Mexico [Albuquerque], Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), 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), Planetary Science Institute [Tucson] (PSI), Optical Science Center for Applied Research (OSCAR), Delaware State University (DSU), 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), 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), and 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)

Subjects
Martian, 010504 meteorology & atmospheric sciences, Calibration curve, 010401 analytical chemistry, Trace element, Mineralogy, Mars Exploration Program, Martian soil, 01 natural sciences, Atomic and Molecular Physics, and Optics, 0104 chemical sciences, Analytical Chemistry, Curiosity, Univariate calibration, 13. Climate action, ChemCam, Soil water, Calibration, [CHIM]Chemical Sciences, Spectroscopy, Instrumentation, 0105 earth and related environmental sciences, Remote sensing
Abstract

International audience; Curiosity rover landed on August 6th, 2012 in Gale Crater, Mars and it possesses unique analytical capabilities to investigate the chemistry and mineralogy of the Martian soil. In particular, the LIBS technique is being used for the first time on another planet with the ChemCam instrument, and more than 75,000 spectra have been returned in the first year on Mars. Curiosity carries body-mounted calibration targets specially designed for the ChemCam instrument, some of which are homgeneous glasses and others that are fine-grained glass-ceramics. We present direct calibrations, using these onboard standards to infer elements and element ratios by ratioing relative peak areas. As the laser spot size is around 300 μm, the LIBS technique provides measurements of the silicate glass compositions representing homogeneous material and measurements of the ceramic targets that are comparable to fine-grained rock or soil. The laser energy and the auto-focus are controlled for all sequences used for calibration. The univariate calibration curves present relatively to very good correlation coefficients with low RSDs for major and ratio calibrations. Trace element calibration curves (Li, Sr, and Mn), down to several ppm, can be used as a rapid tool to draw attention to remarkable rocks and soils along the traverse. First comparisons to alpha-particle X-ray spectroscopy (APXS) data, on selected targets, show good agreement for most elements and for Mg# and Al/Si estimates. SiO2 estimates using univariate cannot be yet used. Na2O and K2O estimates are relevant for high alkali contents, but probably under estimated due to the CCCT initial compositions. Very good results for CaO and Al2O3 estimates and satisfactory results for FeO are obtained.

Published
2014

46. High manganese concentrations in rocks at Gale crater, Mars

Author

Horton E. Newsom, Nicolas Mangold, Craig Hardgrove, Marion Nachon, Stéphane Le Mouélic, Jeff A. Berger, Benton C. Clark, Ann Ollila, John P. Grotzinger, Noureddine Melikechi, S. Maurice, Ryan B. Anderson, Violaine Sautter, Olivier Forni, Roger C. Wiens, Samuel M. Clegg, Woodward W. Fischer, Mariek E. Schmidt, Agnes Cousin, Ralf Gellert, Nina Lanza, Los Alamos National Laboratory (LANL), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], Now at Chevron Energy Technology Company, US Geological Survey [Flagstaff], United States Geological Survey [Reston] (USGS), Space Science Institute [Boulder] (SSI), Department of Physics [Guelph], University of Guelph, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), Department of Earth Sciences [St. Catharines], Brock University [Canada], Department of Earth Sciences [London, ON], University of Western Ontario (UWO), ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Department of Physics and Engineering, Delaware State University (DSU), Muséum national d'Histoire naturelle (MNHN), 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), and 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)

Subjects
010504 meteorology & atmospheric sciences, Geochemistry, chemistry.chemical_element, Weathering, Manganese, Mars Exploration Program, 01 natural sciences, Redox, Astrobiology, Redox indicator, Geophysics, chemistry, 13. Climate action, [SDU]Sciences of the Universe [physics], Martian surface, 0103 physical sciences, Oxidizing agent, General Earth and Planetary Sciences, Composition of Mars, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract

International audience; The surface of Mars has long been considered a relatively oxidizing environment, an ideasupported by the abundance of ferric iron phases observed there. However, compared to iron, manganeseis sensitive only to high redox potential oxidants, and when concentrated in rocks, it provides a more specificredox indicator of aqueous environments. Observations from the ChemCam instrument on the Curiosityrover indicate abundances of manganese in and on some rock targets that are 1–2 orders of magnitudehigher than previously observed on Mars, suggesting the presence of an as-yet unidentified manganese-richphase. These results show that the Martian surface has at some point in time hosted much more highlyoxidizing conditions than has previously been recognized

Published
2014

47. The rock abrasion record at Gale Crater: Mars Science Laboratory results from Bradbury Landing to Rocknest

Author

Fred Calef, R. A. Yingst, Nina Lanza, Yves Langevin, K. E. Herkenhoff, P. Y. Meslin, Roger C. Wiens, Diana L. Blaney, Sylvestre Maurice, Nilton O. Renno, Claire E. Newman, M. E. Richardson, Melissa S. Rice, M. A. de Pablo, Bernard Hallet, Violaine Sautter, Nathan T. Bridges, Gary Kocurek, R. S. Sletten, N. Mangold, Patrick Pinet, S. Le Mouélic, Kevin W. Lewis, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Earth and Space Sciences [Seattle], University of Washington [Seattle], United States Geological Survey [Reston] (USGS), Los Alamos National Laboratory (LANL), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ashima Research, Universidad de Alcalá - University of Alcalá (UAH), Department of Geological Sciences [Austin], Jackson School of Geosciences (JSG), University of Texas at Austin [Austin]-University of Texas at Austin [Austin], Institute d’Astrophysique Spatiale, Université Paris-Sud, Department of Geosciences [Princeton], Princeton University, Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), Department of Earth and Atmospheric Sciences [Michigan], Central Michigan University (CMU), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Lab Mineral and Cosmochim Museum, Planetary Science Institute [Tucson] (PSI), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), and 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)

Subjects
Outcrop, Ventifact, Gale crater, Mars Exploration Program, Abrasion (geology), Lineation, Geophysics, Bradbury Landing, Space and Planetary Science, Geochemistry and Petrology, [SDU]Sciences of the Universe [physics], Rocknest, Earth and Planetary Sciences (miscellaneous), Geomorphology, Geology
Abstract

International audience; Ventifacts, rocks abraded by wind-borne particles, are found in Gale Crater, Mars. In the eastwarddrive from “Bradbury Landing” to “Rocknest,” they account for about half of the float and outcrop seen byCuriosity’s cameras. Many are faceted and exhibit abrasion textures found at a range of scales, fromsubmillimeter lineations to centimeter-scale facets, scallops, flutes, and grooves. The drive path geometryin the first 100 sols of the mission emphasized the identification of abrasion facets and textures formedby westerly flow. This upwind direction is inconsistent with predictions based on models and the orientationof regional dunes, suggesting that these ventifact features formed from very rare high-speed winds. Theabsence of active sand and evidence for deflation in the area indicates that most of the ventifacts are fossilfeatures experiencing little abrasion today.

Published
2014

48. A Habitable Fluvio-Lacustrine Environment at Yellowknife Bay, Gale Crater, Mars

Author

J. P. Grotzinger, D. Y. Sumner, L. C. Kah, K. Stack, S. Gupta, L. Edgar, D. Rubin, K. Lewis, J. Schieber, N. Mangold, R. Milliken, P. G. Conrad, D. DesMarais, J. Farmer, K. Siebach, F. Calef, J. Hurowitz, S. M. McLennan, D. Ming, D. Vaniman, J. Crisp, A. Vasavada, K. S. Edgett, M. Malin, D. Blake, R. Gellert, P. Mahaffy, R. C. Wiens, S. Maurice, J. A. Grant, S. Wilson, R. C. Anderson, L. Beegle, R. Arvidson, B. Hallet, R. S. Sletten, M. Rice, J. Bell, J. Griffes, B. Ehlmann, R. B. Anderson, T. F. Bristow, W. E. Dietrich, G. Dromart, J. Eigenbrode, A. Fraeman, C. Hardgrove, K. Herkenhoff, L. Jandura, G. Kocurek, S. Lee, L. A. Leshin, R. Leveille, D. Limonadi, J. Maki, S. McCloskey, M. Meyer, M. Minitti, H. Newsom, D. Oehler, A. Okon, M. Palucis, T. Parker, S. Rowland, M. Schmidt, S. Squyres, A. Steele, E. Stolper, R. Summons, A. Treiman, R. Williams, A. Yingst, MSL Science Team, Osku Kemppinen, Nathan Bridges, Jeffrey R. Johnson, David Cremers, Austin Godber, Meenakshi Wadhwa, Danika Wellington, Ian McEwan, Claire Newman, Mark Richardson, Antoine Charpentier, Laurent Peret, Penelope King, Jennifer Blank, Gerald Weigle, Shuai Li, Kevin Robertson, Vivian Sun, Michael Baker, Christopher Edwards, Kenneth Farley, Hayden Miller, Megan Newcombe, Cedric Pilorget, Claude Brunet, Victoria Hipkin, Richard Léveillé, Geneviève Marchand, Pablo Sobrón Sánchez, Laurent Favot, George Cody, Lorenzo Flückiger, David Lees, Ara Nefian, Mildred Martin, Marc Gailhanou, Frances Westall, Guy Israël, Christophe Agard, Julien Baroukh, Christophe Donny, Alain Gaboriaud, Philippe Guillemot, Vivian Lafaille, Eric Lorigny, Alexis Paillet, René Pérez, Muriel Saccoccio, Charles Yana, Carlos Armiens-Aparicio, Javier Caride Rodríguez, Isaías Carrasco Blázquez, Felipe Gómez Gómez, Javier Gómez-Elvira, Sebastian Hettrich, Alain Lepinette Malvitte, Mercedes Marín Jiménez, Jesús Martínez-Frías, Javier Martín-Soler, F. Javier Martín-Torres, Antonio Molina Jurado, Luis Mora-Sotomayor, Guillermo Muñoz Caro, Sara Navarro López, Verónica Peinado-González, Jorge Pla-García, José Antonio Rodriguez Manfredi, Julio José Romeral-Planelló, Sara Alejandra Sans Fuentes, Eduardo Sebastian Martinez, Josefina Torres Redondo, Roser Urqui-O’Callaghan, María-Paz Zorzano Mier, Steve Chipera, Jean-Luc Lacour, Patrick Mauchien, Jean-Baptiste Sirven, Heidi Manning, Alberto Fairén, Alexander Hayes, Jonathan Joseph, Robert Sullivan, Peter Thomas, Audrey Dupont, Angela Lundberg, Noureddine Melikechi, Alissa Mezzacappa, Julia DeMarines, David Grinspoon, Günther Reitz, Benito Prats, Evgeny Atlaskin, Maria Genzer, Ari-Matti Harri, Harri Haukka, Henrik Kahanpää, Janne Kauhanen, Mark Paton, Jouni Polkko, Walter Schmidt, Tero Siili, Cécile Fabre, James Wray, Mary Beth Wilhelm, Franck Poitrasson, Kiran Patel, Stephen Gorevan, Stephen Indyk, Gale Paulsen, David Bish, Brigitte Gondet, Yves Langevin, Claude Geffroy, David Baratoux, Gilles Berger, Alain Cros, Claude d’Uston, Olivier Forni, Olivier Gasnault, Jérémie Lasue, Qiu-Mei Lee, Pierre-Yves Meslin, Etienne Pallier, Yann Parot, Patrick Pinet, Susanne Schröder, Mike Toplis, Éric Lewin, Will Brunner, Ezat Heydari, Cherie Achilles, Brad Sutter, Michel Cabane, David Coscia, Cyril Szopa, François Robert, Violaine Sautter, Stéphane Le Mouélic, Marion Nachon, Arnaud Buch, Fabien Stalport, Patrice Coll, Pascaline François, François Raulin, Samuel Teinturier, James Cameron, Sam Clegg, Agnès Cousin, Dorothea DeLapp, Robert Dingler, Ryan Steele Jackson, Stephen Johnstone, Nina Lanza, Cynthia Little, Tony Nelson, Richard B. Williams, Andrea Jones, Laurel Kirkland, Burt Baker, Bruce Cantor, Michael Caplinger, Scott Davis, Brian Duston, Donald Fay, David Harker, Paul Herrera, Elsa Jensen, Megan R. Kennedy, Gillian Krezoski, Daniel Krysak, Leslie Lipkaman, Elaina McCartney, Sean McNair, Brian Nixon, Liliya Posiolova, Michael Ravine, Andrew Salamon, Lee Saper, Kevin Stoiber, Kimberley Supulver, Jason Van Beek, Tessa Van Beek, Robert Zimdar, Katherine Louise French, Karl Iagnemma, Kristen Miller, Fred Goesmann, Walter Goetz, Stubbe Hviid, Micah Johnson, Matthew Lefavor, Eric Lyness, Elly Breves, M. Darby Dyar, Caleb Fassett, Laurence Edwards, Robert Haberle, Tori Hoehler, Jeff Hollingsworth, Melinda Kahre, Leslie Keely, Christopher McKay, Lora Bleacher, William Brinckerhoff, David Choi, Jason P. Dworkin, Melissa Floyd, Caroline Freissinet, James Garvin, Daniel Glavin, Daniel Harpold, David K. Martin, Amy McAdam, Alexander Pavlov, Eric Raaen, Michael D. Smith, Jennifer Stern, Florence Tan, Melissa Trainer, Arik Posner, Mary Voytek, Andrew Aubrey, Alberto Behar, Diana Blaney, David Brinza, Lance Christensen, Lauren DeFlores, Jason Feldman, Sabrina Feldman, Gregory Flesch, Insoo Jun, Didier Keymeulen, Michael Mischna, John Michael Morookian, Betina Pavri, Marcel Schoppers, Aaron Sengstacken, John J. Simmonds, Nicole Spanovich, Manuel de la Torre Juarez, Christopher R. Webster, Albert Yen, Paul Douglas Archer, Francis Cucinotta, John H. Jones, Richard V. Morris, Paul Niles, Elizabeth Rampe, Thomas Nolan, Martin Fisk, Leon Radziemski, Bruce Barraclough, Steve Bender, Daniel Berman, Eldar Noe Dobrea, Robert Tokar, Timothy Cleghorn, Wesley Huntress, Gérard Manhès, Judy Hudgins, Timothy Olson, Noel Stewart, Philippe Sarrazin, Edward Vicenzi, Mark Bullock, Bent Ehresmann, Victoria Hamilton, Donald Hassler, Joseph Peterson, Scot Rafkin, Cary Zeitlin, Fedor Fedosov, Dmitry Golovin, Natalya Karpushkina, Alexander Kozyrev, Maxim Litvak, Alexey Malakhov, Igor Mitrofanov, Maxim Mokrousov, Sergey Nikiforov, Vasily Prokhorov, Anton Sanin, Vladislav Tretyakov, Alexey Varenikov, Andrey Vostrukhin, Ruslan Kuzmin, Benton Clark, Michael Wolff, Oliver Botta, Darrell Drake, Keri Bean, Mark Lemmon, Susanne P. Schwenzer, Ella Mae Lee, Robert Sucharski, Miguel Ángel de Pablo Hernández, Juan José Blanco Ávalos, Miguel Ramos, Myung-Hee Kim, Charles Malespin, Ianik Plante, Jan-Peter Muller, Rafael Navarro-González, Ryan Ewing, William Boynton, Robert Downs, Mike Fitzgibbon, Karl Harshman, Shaunna Morrison, Onno Kortmann, Amy Williams, Günter Lugmair, Michael A. Wilson, Bruce Jakosky, Tonci Balic-Zunic, Jens Frydenvang, Jaqueline Kløvgaard Jensen, Kjartan Kinch, Asmus Koefoed, Morten Bo Madsen, Susan Louise Svane Stipp, Nick Boyd, John L. Campbell, Glynis Perrett, Irina Pradler, Scott VanBommel, Samantha Jacob, Tobias Owen, Hannu Savijärvi, Eckart Boehm, Stephan Böttcher, Sönke Burmeister, Jingnan Guo, Jan Köhler, César Martín García, Reinhold Mueller-Mellin, Robert Wimmer-Schweingruber, John C. Bridges, Timothy McConnochie, Mehdi Benna, Heather Franz, Hannah Bower, Anna Brunner, Hannah Blau, Thomas Boucher, Marco Carmosino, Sushil Atreya, Harvey Elliott, Douglas Halleaux, Nilton Rennó, Michael Wong, Robert Pepin, Beverley Elliott, John Spray, Lucy Thompson, Suzanne Gordon, Ann Ollila, Joshua Williams, Paulo Vasconcelos, Jennifer Bentz, Kenneth Nealson, Radu Popa, Jeffrey Moersch, Christopher Tate, Mackenzie Day, Raymond Francis, Emily McCullough, Ed Cloutis, Inge Loes ten Kate, Daniel Scholes, Susan Slavney, Thomas Stein, Jennifer Ward, Jeffrey Berger, John E. Moores, Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley], University of California-University of California, The University of Tennessee [Knoxville], Department of Earth Science and Technology [Imperial College London], Imperial College London, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), US Geological Survey [Santa Cruz], United States Geological Survey [Reston] (USGS), Princeton University, Department of Geological Sciences [Bloomington], Indiana University [Bloomington], Indiana University System-Indiana University System, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Geological Sciences [Providence], Brown University, NASA Goddard Space Flight Center (GSFC), NASA Ames Research Center (ARC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), State University of New York (SUNY), NASA Johnson Space Center (JSC), NASA, Planetary Science Institute [Tucson] (PSI), Department of Physics [Guelph], University of Guelph, Space Remote Sensing Group (ISR-2), Los Alamos National Laboratory (LANL), Institut de recherche en astrophysique et planétologie (IRAP), 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), 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), Center for Earth and Planetary Studies [Washington] (CEPS), Smithsonian National Air and Space Museum, Smithsonian Institution-Smithsonian Institution, Department of Earth and Space Sciences [Seattle], University of Washington [Seattle], Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Department of Geological Sciences [Austin], Jackson School of Geosciences (JSG), University of Texas at Austin [Austin]-University of Texas at Austin [Austin], Rensselaer Polytechnic Institute (RPI), Canadian Space Agency (CSA), NASA Headquarters, Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], University of Hawaii, Brock University [Canada], Cornell University [New York], Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science [Washington], Massachusetts Institute of Technology (MIT), Lunar and Planetary Institute [Houston] (LPI), 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), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), 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), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Carnegie Institution for Science, 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), NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, and Petrology

Subjects
Geologic Sediments, Salinity, Extraterrestrial Environment, Nitrogen, General Science & Technology, Iron, Curiosity rover, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Astrobiology, MSL Science Team, Exobiology, MSL, Martian, Multidisciplinary, fluvial-lacustrine environments, Biosphere, Water, Phosphorus, Mars Exploration Program, 15. Life on land, Hydrogen-Ion Concentration, Carbon, Oxygen, Planetary science, Bays, 13. Climate action, Rocknest, Sample Analysis at Mars, Sedimentary rock, Oxidation-Reduction, Geology, Sulfur, Hydrogen
Abstract

International audience; The Curiosity rover discovered fine-grained sedimentary rocks, which are inferred to represent an ancient lake and preserve evidence of an environment that would have been suited to support a martian biosphere founded on chemolithoautotrophy. This aqueous environment was characterized by neutral pH, low salinity, and variable redox states of both iron and sulfur species. Carbon, hydrogen, oxygen, sulfur, nitrogen, and phosphorus were measured directly as key biogenic elements; by inference, phosphorus is assumed to have been available. The environment probably had a minimum duration of hundreds to tens of thousands of years. These results highlight the biological viability of fluvial-lacustrine environments in the post-Noachian history of Mars.

Published
2014

49. Mars' surface radiation environment measured with the Mars science laboratory's curiosity rover

Author

Donald M. Hassler, Cary Zeitlin, Robert F. Wimmer-Schweingruber, Bent Ehresmann, Scot Rafkin, Jennifer L. Eigenbrode, David E. Brinza, Gerald Weigle, Stephan Böttcher, Eckart Böhm, Soenke Burmeister, Jingnan Guo, Jan Köhler, Cesar Martin, Guenther Reitz, Francis A. Cucinotta, Myung-Hee Kim, David Grinspoon, Mark A. Bullock, Arik Posner, Javier Gómez-Elvira, Ashwin Vasavada, John P. Grotzinger, MSL Science Team, Osku Kemppinen, David Cremers, James F. Bell, Lauren Edgar, Jack Farmer, Austin Godber, Meenakshi Wadhwa, Danika Wellington, Ian McEwan, Claire Newman, Mark Richardson, Antoine Charpentier, Laurent Peret, Penelope King, Jennifer Blank, Mariek Schmidt, Shuai Li, Ralph Milliken, Kevin Robertson, Vivian Sun, Michael Baker, Christopher Edwards, Bethany Ehlmann, Kenneth Farley, Jennifer Griffes, Hayden Miller, Megan Newcombe, Cedric Pilorget, Melissa Rice, Kirsten Siebach, Katie Stack, Edward Stolper, Claude Brunet, Victoria Hipkin, Richard Léveillé, Geneviève Marchand, Pablo Sobrón Sánchez, Laurent Favot, George Cody, Andrew Steele, Lorenzo Flückiger, David Lees, Ara Nefian, Mildred Martin, Marc Gailhanou, Frances Westall, Guy Israël, Christophe Agard, Julien Baroukh, Christophe Donny, Alain Gaboriaud, Philippe Guillemot, Vivian Lafaille, Eric Lorigny, Alexis Paillet, René Pérez, Muriel Saccoccio, Charles Yana, Carlos Armiens‐Aparicio, Javier Caride Rodríguez, Isaías Carrasco Blázquez, Felipe Gómez Gómez, Sebastian Hettrich, Alain Lepinette Malvitte, Mercedes Marín Jiménez, Jesús Martínez-Frías, Javier Martín-Soler, F. Javier Martín-Torres, Antonio Molina Jurado, Luis Mora-Sotomayor, Guillermo Muñoz Caro, Sara Navarro López, Verónica Peinado-González, Jorge Pla-García, José Antonio Rodriguez Manfredi, Julio José Romeral-Planelló, Sara Alejandra Sans Fuentes, Eduardo Sebastian Martinez, Josefina Torres Redondo, Roser Urqui-O'Callaghan, María-Paz Zorzano Mier, Steve Chipera, Jean-Luc Lacour, Patrick Mauchien, Jean-Baptiste Sirven, Heidi Manning, Alberto Fairén, Alexander Hayes, Jonathan Joseph, Steven Squyres, Robert Sullivan, Peter Thomas, Audrey Dupont, Angela Lundberg, Noureddine Melikechi, Alissa Mezzacappa, Thomas Berger, Daniel Matthia, Benito Prats, Evgeny Atlaskin, Maria Genzer, Ari-Matti Harri, Harri Haukka, Henrik Kahanpää, Janne Kauhanen, Mark Paton, Jouni Polkko, Walter Schmidt, Tero Siili, Cécile Fabre, James Wray, Mary Beth Wilhelm, Franck Poitrasson, Kiran Patel, Stephen Gorevan, Stephen Indyk, Gale Paulsen, Sanjeev Gupta, David Bish, Juergen Schieber, Brigitte Gondet, Yves Langevin, Claude Geffroy, David Baratoux, Gilles Berger, Alain Cros, Claude d’Uston, Olivier Forni, Olivier Gasnault, Jérémie Lasue, Qiu-Mei Lee, Sylvestre Maurice, Pierre-Yves Meslin, Etienne Pallier, Yann Parot, Patrick Pinet, Susanne Schröder, Mike Toplis, Éric Lewin, Will Brunner, Ezat Heydari, Cherie Achilles, Dorothy Oehler, Brad Sutter, Michel Cabane, David Coscia, Cyril Szopa, Gilles Dromart, François Robert, Violaine Sautter, Stéphane Le Mouélic, Nicolas Mangold, Marion Nachon, Arnaud Buch, Fabien Stalport, Patrice Coll, Pascaline François, François Raulin, Samuel Teinturier, James Cameron, Sam Clegg, Agnès Cousin, Dorothea DeLapp, Robert Dingler, Ryan Steele Jackson, Stephen Johnstone, Nina Lanza, Cynthia Little, Tony Nelson, Roger C. Wiens, Richard B. Williams, Andrea Jones, Laurel Kirkland, Allan Treiman, Burt Baker, Bruce Cantor, Michael Caplinger, Scott Davis, Brian Duston, Kenneth Edgett, Donald Fay, Craig Hardgrove, David Harker, Paul Herrera, Elsa Jensen, Megan R. Kennedy, Gillian Krezoski, Daniel Krysak, Leslie Lipkaman, Michael Malin, Elaina McCartney, Sean McNair, Brian Nixon, Liliya Posiolova, Michael Ravine, Andrew Salamon, Lee Saper, Kevin Stoiber, Kimberley Supulver, Jason Van Beek, Tessa Van Beek, Robert Zimdar, Katherine Louise French, Karl Iagnemma, Kristen Miller, Roger Summons, Fred Goesmann, Walter Goetz, Stubbe Hviid, Micah Johnson, Matthew Lefavor, Eric Lyness, Elly Breves, M. Darby Dyar, Caleb Fassett, David F. Blake, Thomas Bristow, David DesMarais, Laurence Edwards, Robert Haberle, Tori Hoehler, Jeff Hollingsworth, Melinda Kahre, Leslie Keely, Christopher McKay, Lora Bleacher, William Brinckerhoff, David Choi, Pamela Conrad, Jason P. Dworkin, Melissa Floyd, Caroline Freissinet, James Garvin, Daniel Glavin, Daniel Harpold, Paul Mahaffy, David K. Martin, Amy McAdam, Alexander Pavlov, Eric Raaen, Michael D. Smith, Jennifer Stern, Florence Tan, Melissa Trainer, Michael Meyer, Mary Voytek, Robert C. Anderson, Andrew Aubrey, Luther W. Beegle, Alberto Behar, Diana Blaney, Fred Calef, Lance Christensen, Joy A. Crisp, Lauren DeFlores, Jason Feldman, Sabrina Feldman, Gregory Flesch, Joel Hurowitz, Insoo Jun, Didier Keymeulen, Justin Maki, Michael Mischna, John Michael Morookian, Timothy Parker, Betina Pavri, Marcel Schoppers, Aaron Sengstacken, John J. Simmonds, Nicole Spanovich, Manuel de la Torre Juarez, Christopher R. Webster, Albert Yen, Paul Douglas Archer, John H. Jones, Douglas Ming, Richard V. Morris, Paul Niles, Elizabeth Rampe, Thomas Nolan, Martin Fisk, Leon Radziemski, Bruce Barraclough, Steve Bender, Daniel Berman, Eldar Noe Dobrea, Robert Tokar, David Vaniman, Rebecca M. E. Williams, Aileen Yingst, Kevin Lewis, Laurie Leshin, Timothy Cleghorn, Wesley Huntress, Gérard Manhès, Judy Hudgins, Timothy Olson, Noel Stewart, Philippe Sarrazin, John Grant, Edward Vicenzi, Sharon A. Wilson, Victoria Hamilton, Joseph Peterson, Fedor Fedosov, Dmitry Golovin, Natalya Karpushkina, Alexander Kozyrev, Maxim Litvak, Alexey Malakhov, Igor Mitrofanov, Maxim Mokrousov, Sergey Nikiforov, Vasily Prokhorov, Anton Sanin, Vladislav Tretyakov, Alexey Varenikov, Andrey Vostrukhin, Ruslan Kuzmin, Benton Clark, Michael Wolff, Scott McLennan, Oliver Botta, Darrell Drake, Keri Bean, Mark Lemmon, Susanne P. Schwenzer, Ryan B. Anderson, Kenneth Herkenhoff, Ella Mae Lee, Robert Sucharski, Miguel Ángel de Pablo Hernández, Juan José Blanco Ávalos, Miguel Ramos, Charles Malespin, Ianik Plante, Jan-Peter Muller, Rafael Navarro-González, Ryan Ewing, William Boynton, Robert Downs, Mike Fitzgibbon, Karl Harshman, Shaunna Morrison, William Dietrich, Onno Kortmann, Marisa Palucis, Dawn Y. Sumner, Amy Williams, Günter Lugmair, Michael A. Wilson, David Rubin, Bruce Jakosky, Tonci Balic-Zunic, Jens Frydenvang, Jaqueline Kløvgaard Jensen, Kjartan Kinch, Asmus Koefoed, Morten Bo Madsen, Susan Louise Svane Stipp, Nick Boyd, John L. Campbell, Ralf Gellert, Glynis Perrett, Irina Pradler, Scott VanBommel, Samantha Jacob, Tobias Owen, Scott Rowland, Hannu Savijärvi, César Martín García, Reinhold Mueller-Mellin, John C. Bridges, Timothy McConnochie, Mehdi Benna, Heather Franz, Hannah Bower, Anna Brunner, Hannah Blau, Thomas Boucher, Marco Carmosino, Sushil Atreya, Harvey Elliott, Douglas Halleaux, Nilton Rennó, Michael Wong, Robert Pepin, Beverley Elliott, John Spray, Lucy Thompson, Suzanne Gordon, Horton Newsom, Ann Ollila, Joshua Williams, Paulo Vasconcelos, Jennifer Bentz, Kenneth Nealson, Radu Popa, Linda C. Kah, Jeffrey Moersch, Christopher Tate, Mackenzie Day, Gary Kocurek, Bernard Hallet, Ronald Sletten, Raymond Francis, Emily McCullough, Ed Cloutis, Inge Loes ten Kate, Raymond Arvidson, Abigail Fraeman, Daniel Scholes, Susan Slavney, Thomas Stein, Jennifer Ward, Jeffrey Berger, John E. Moores, NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, Southwest Research Institute [Boulder] (SwRI), Kiel University, NASA Goddard Space Flight Center (GSFC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), German Aerospace Center (DLR), University of Nevada [Reno], Universities Space Research Association (USRA), Denver Museum of Nature and Science, NASA Headquarters, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), 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
Extraterrestrial Environment, Surface Properties, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Cosmic ray, Radiation Dosage, Exploration of Mars, Astrobiology, Martian surface, Exobiology, galactic cosmic rays, solar energetic particles, Mars Science Laboratory’s Curiosity rover, Humans, Organic Chemicals, Particle radiation, Martian, Radiation Assessment Detector (RAD), Multidisciplinary, Mars Exploration Program, Space Flight, Radiation assessment detector, 13. Climate action, Health threat from cosmic rays, Deinococcus, Cosmic Radiation
Abstract

International audience; The Radiation Assessment Detector (RAD) on the Mars Science Laboratory's Curiosity rover began making detailed measurements of the cosmic ray and energetic particle radiation environment on the surface of Mars on 7 August 2012. We report and discuss measurements of the absorbed dose and dose equivalent from galactic cosmic rays and solar energetic particles on the martian surface for similar to 300 days of observations during the current solar maximum. These measurements provide insight into the radiation hazards associated with a human mission to the surface of Mars and provide an anchor point with which to model the subsurface radiation environment, with implications for microbial survival times of any possible extant or past life, as well as for the preservation of potential organic biosignatures of the ancient martian environment.

Published
2014

50. New analytical and numerical geospeedometers tested on garnet pyroxenites from Bragança Nappe Complex (NE Portugal)

Author

S Duchêne, Violaine Sautter, and Fernando O. Marques

Subjects
geography, Geophysics, geography.geographical_feature_category, Cooling rate, Crust, Massif, Diffusion (business), Petrology, Geology, Earth-Surface Processes, Nappe
Abstract

Two new geospeedometric approaches, an analytical one [Phys. Earth Planet. Inter. 110 (1999) 95] and a numerical one [Am. J. Sci. 29 (1998) 30], are tested to evaluate cooling rate on upper mantle-derived pyroxenites from the Braganca massif (NE Portugal). These estimations, coupled with standard geobarometric techniques, allow theoretically the determination of exhumation rates responsible for incorporation of these rocks within the lower crust. In the present paper, we discuss the most significant sources of uncertainties in geospeedometry (whether numerical or analytical): precision of temperature estimates and input diffusion data. None of the available geospeedometrical tools, when used independently, is able to provide definitive results with less than a factor 10 in precision. Cross-calibration is, thus, required in order to provide reliable cooling rate estimates. We obtain for pyroxenites from the Braganca massif, a minimum cooling rate from 1000 to 750 °C of the order of 250 °C/Ma for a depth interval of 10–15 km.

Published
2001

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