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1,279 results on '"NASA Johnson Space"'

1. THE DISTRIBUTION OF FLUORINE, CHLORINE, AND HYDROGEN DURING PLANETARY DIFFERENTIATION: IMPLICATIONS FOR APATITE COMPOSITIONS IN PLANETARY MATERIALS

Author: Francis McCubbin and Nasa Johnson Space Centermailcode Xi
Subjects: Hydrogen, chemistry, Distribution (number theory), Chemical engineering, visual_art, visual_art.visual_art_medium, Fluorine, Chlorine, chemistry.chemical_element, Apatite, Planetary differentiation
Published: 2020
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2. NASA to send Cedar Falls native to the moon

Author: Markowitz, Robert and Center, Nasa-Johnson Space
Subjects: United States. Air Force, Space exploration, Air Force officers, Astronauts, Air forces, News, opinion and commentary, Sports and fitness
Abstract: Byline: Robert Markowitz, NASA-Johnson Space Center CEDAR FALLS -- Cedar Falls native Raja Chari has been selected by NASA to the team of astronauts who will go to the moon [...]
Published: 2020

3. 50 astronauts, in their own words

Author: Center, NASA/Johnson Space
Subjects: Apollo 11 (Spacecraft), Astronauts -- Beliefs, opinions and attitudes -- Practice, Public relations executives, Public relations, Marketing, Marketing industry, Space shuttles, Public relations firms, Editors, General interest, News, opinion and commentary
Abstract: Byline: NASA/Johnson Space Center (EDITORS: This project was produced with the help of the Uniphi Space Agency, a public relations and marketing agency that represents astronauts.) - - - To [...]
Published: 2019

4. CLASSIFICATION OF BOLIDES AND METEORS IN DOPPLER RADAR WEATHER DATA USING UNSUPERVISED MACHINE LEARNING

Author: Karpenko, Mark, Abell, Paul, NASA Johnson Space Center, Whitaker, Lyn R., Mechanical and Aerospace Engineering (MAE), Smeresky, Brendon P., Karpenko, Mark, Abell, Paul, NASA Johnson Space Center, Whitaker, Lyn R., Mechanical and Aerospace Engineering (MAE), and Smeresky, Brendon P.
Abstract: This thesis presents a method for detecting outlier meteors and bolides within Doppler radar data using unsupervised machine learning. Principal Component Analysis (PCA), k-means Clustering, and t-Distributed Statistical Neighbor Embedding (t-SNE) algorithms are introduced as existing methods for outlier detection. A combined PCA and t-SNE method that uses a Nearest Neighbor Density Pruning method for dataset size reduction is also described. These methods are implemented to classify unlabeled radar data from four radar data sites from two bolide events: the KFWS radar for the Ash Creek bolide and the KDAX, KRGX, and KBBX radars for the Sutter’s Mill bolide. The combined PCA + t-SNE method gives an accuracy rate of 99.7% and can classify the data in less than 8 minutes for a 121,000 return sized dataset. However, the classifier’s recall and precision rates remained low due to difficulties in correctly classifying true positive bolides. Some ideas for improving algorithm accuracy, speed, and related follow-on applications are proposed. Overall, the algorithm presented in this research is a viable method to help NASA scientists with bolide detection and meteorite recovery.
Published: 2019

5. Developing Decision Aids to Enable Human Spaceflight Autonomy

Author: Frank, Jeremy D., NASA Ames Research Center, McGuire, Kerry, NASA Johnson Space Center, Moses, Haifa R., and Stephenson, Jerri
Abstract: As NASA explores destinations beyond the Moon, the distance between Earth and spacecraft will increase communication delays between astronauts and Mission Control. Today, astronauts coordinate with Mission Control to request assistance and await approval to perform tasks. Many of these coordination tasks require multiple exchanges of information, (for example, taking turns). In the presence of long communication delays, the length of time between turns may lead to inefficiency, or increased mission risk. Future astronauts will need software-based decision aids to enable them to work autonomously from Mission Control. These tools require the right combination of mission operations functions, for example, automated planning and fault management, troubleshooting recommendations, easy to access information, and just-in-time training. Ensuring these elements are properly designed and integrated requires an integrated human factors approach. This article describes a recent demonstration of autonomous mission operations using a novel software-based decision aid onboard the International Space Station. We describe how this new technology changes the way astronauts coordinate with mission control, and how the lessons learned from these early demonstrations will enable the operational autonomy needed to ensure astronauts can safely journey to Mars, and beyond.
Published: 2017

6. Structure and soot properties of nonbuoyant ethylene/air laminar jet diffusion flames

Author: Michigan, Univ., Ann Arbor, NASA, Lewis Research Center, Cleveland, OH, NASA, Johnson Space Center, Houston, TX, Urban, D. L., Yuan, Z. -G., Sunderland, P. B., Linteris, G. T., Voss, J. E., Lin, K. -C., Dai, Z., Sun, K., Faeth, G. M., Michigan, Univ., Ann Arbor, NASA, Lewis Research Center, Cleveland, OH, NASA, Johnson Space Center, Houston, TX, Urban, D. L., Yuan, Z. -G., Sunderland, P. B., Linteris, G. T., Voss, J. E., Lin, K. -C., Dai, Z., Sun, K., and Faeth, G. M.
Published: 2010

7. Impact of space shuttle orbiter reentry on mesospheric NOx.

Author: Michigan, University, Ann Arbor, Mich., NASA, Johnson Space Center, Houston, Tex., Stolarski, R. S., Cicerone, R. J., Nagy, A. F., Michigan, University, Ann Arbor, Mich., NASA, Johnson Space Center, Houston, Tex., Stolarski, R. S., Cicerone, R. J., and Nagy, A. F.
Published: 2010

8. Drug Marker Absorption in Relation to Pellet Size, Gastric Motility and Viscous Meals in Humans

Author: College of Pharmacy, University of Michigan, Ann Arbor, Michigan; College of Pharmacy, Nagoya City University, Nagoya, Japan, Department of Internal Medicine, Division of Gastroenterology and University of Michigan Medical School, University of Michigan Health Systems, Ann Arbor, Michigan, College of Pharmacy, University of Michigan, Ann Arbor, Michigan, College of Pharmacy, University of Michigan, Ann Arbor, Michigan; NIH Bldg 29B Rm 2E06, Bethesda, Maryland, 20892, College of Pharmacy, University of Michigan, Ann Arbor, Michigan; Department of Pharmacy, University of Michigan Health Systems, Ann Arbor, Michigan, Pharmacia and Upjohn, Kalamazoo, Michigan, NASA-Johnson Space Center, Houston, Texas, Ann Arbor, Putcha, Lakshmi, Amidon, Gregory E., Wald, Randy J., Barnett, Jeffrey L., Amidon, Gordon L., Rhie, Julie K., Hayashi, Yayoi, Frens, Jeremy, Welage, Lynda S., College of Pharmacy, University of Michigan, Ann Arbor, Michigan; College of Pharmacy, Nagoya City University, Nagoya, Japan, Department of Internal Medicine, Division of Gastroenterology and University of Michigan Medical School, University of Michigan Health Systems, Ann Arbor, Michigan, College of Pharmacy, University of Michigan, Ann Arbor, Michigan, College of Pharmacy, University of Michigan, Ann Arbor, Michigan; NIH Bldg 29B Rm 2E06, Bethesda, Maryland, 20892, College of Pharmacy, University of Michigan, Ann Arbor, Michigan; Department of Pharmacy, University of Michigan Health Systems, Ann Arbor, Michigan, Pharmacia and Upjohn, Kalamazoo, Michigan, NASA-Johnson Space Center, Houston, Texas, Ann Arbor, Putcha, Lakshmi, Amidon, Gregory E., Wald, Randy J., Barnett, Jeffrey L., Amidon, Gordon L., Rhie, Julie K., Hayashi, Yayoi, Frens, Jeremy, and Welage, Lynda S.
Abstract: Purpose . The objective of this study was to evaluate drug marker absorption in relation to the gastric emptying (GE) of 0.7 mm and 3.6 mm enteric coated pellets as a function of viscosity and the underlying gastric motility.
Published: 2006

9. CLASSIFICATION OF BOLIDES AND METEORS IN DOPPLER RADAR WEATHER DATA USING UNSUPERVISED MACHINE LEARNING

Author: Karpenko, Mark, Abell, Paul, NASA Johnson Space Center, Whitaker, Lyn R., Mechanical and Aerospace Engineering (MAE), Smeresky, Brendon P., Karpenko, Mark, Abell, Paul, NASA Johnson Space Center, Whitaker, Lyn R., Mechanical and Aerospace Engineering (MAE), and Smeresky, Brendon P.
Abstract: This thesis presents a method for detecting outlier meteors and bolides within Doppler radar data using unsupervised machine learning. Principal Component Analysis (PCA), k-means Clustering, and t-Distributed Statistical Neighbor Embedding (t-SNE) algorithms are introduced as existing methods for outlier detection. A combined PCA and t-SNE method that uses a Nearest Neighbor Density Pruning method for dataset size reduction is also described. These methods are implemented to classify unlabeled radar data from four radar data sites from two bolide events: the KFWS radar for the Ash Creek bolide and the KDAX, KRGX, and KBBX radars for the Sutter’s Mill bolide. The combined PCA + t-SNE method gives an accuracy rate of 99.7% and can classify the data in less than 8 minutes for a 121,000 return sized dataset. However, the classifier’s recall and precision rates remained low due to difficulties in correctly classifying true positive bolides. Some ideas for improving algorithm accuracy, speed, and related follow-on applications are proposed. Overall, the algorithm presented in this research is a viable method to help NASA scientists with bolide detection and meteorite recovery., http://archive.org/details/classificationof1094564069, Outstanding Thesis, Lieutenant Commander, United States Navy, Approved for public release; distribution is unlimited.

10. Organic matter preserved in 3-billion-year-old mudstones at Gale crater, Mars

Author: Patrice Coll, Arnaud Buch, Paul R. Mahaffy, Pamela G. Conrad, John P. Grotzinger, Heather B. Franz, Sanjeev Gupta, Caroline Freissinet, Daniel P. Glavin, Brad Sutter, Maeva Millan, Dawn Y. Sumner, Andrew Steele, P. D. Archer, Joel A. Hurowitz, Amy McAdam, Jennifer L. Eigenbrode, Rafael Navarro-González, Cyril Szopa, Charles Malespin, D. W. Ming, Roger E. Summons, NASA Goddard Space Flight Center (GSFC), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Geophysical Laboratory [Carnegie Institution], Carnegie Institution for Science [Washington], PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Georgetown University [Washington] (GU), Instituto de Ciencias Nucleares [Mexico], Universidad Nacional Autónoma de México (UNAM), Jacobs Technology ESCG, Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Department of Earth and Planetary Sciences [Davis], University of California [Davis] (UC Davis), University of California-University of California, Laboratoire de Génie des Procédés et Matériaux - EA 4038 (LGPM), CentraleSupélec, Laboratoire Interuniversitaire des Systèmes Atmosphériques (LISA (UMR_7583)), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS), NASA Goddard Space Flight Center ( GSFC ), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] ( EAPS ), Massachusetts Institute of Technology ( MIT ), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Georgetown University [Washington] ( GU ), Universidad Nacional Autónoma de México ( UNAM ), Astromaterials Research and Exploration Science ( ARES ), NASA Johnson Space Center ( JSC ), Stony Brook University [The State University of New York] ( SBU ), California Institute of Technology ( CALTECH ), Department of Earth Science and Engineering [London], University of California [Davis] ( UC Davis ), Laboratoire de Génie des Procédés et Matériaux - EA 4038 ( LGPM ), Laboratoire inter-universitaire des systèmes atmosphèriques ( LISA ), Centre National de la Recherche Scientifique ( CNRS ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Carnegie Institution for Science, 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 Nacional Autónoma de México = National Autonomous University of Mexico (UNAM), Department of Earth and Planetary Sciences [Univ California Davis] (EPS - UC Davis), University of California (UC)-University of California (UC), Laboratoire de Génie des Procédés et Matériaux (LGPM), CentraleSupélec-Université Paris-Saclay, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Science and Technology Facilities Council (STFC)
Subjects: 010504 meteorology & atmospheric sciences, Evolved gas analysis, General Science & Technology, chemistry.chemical_element, 01 natural sciences, Astrobiology, PHASES, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, 0103 physical sciences, Organic matter, 010303 astronomy & astrophysics, [ SDU.ASTR ] Sciences of the Universe [physics]/Astrophysics [astro-ph], 0105 earth and related environmental sciences, Total organic carbon, Martian, chemistry.chemical_classification, Science & Technology, Multidisciplinary, [ SDU.STU.PL ] Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], PYROLYSIS, Mars Exploration Program, 15. Life on land, Multidisciplinary Sciences, chemistry, 13. Climate action, Sample Analysis at Mars, Science & Technology - Other Topics, Environmental science, Carbon, Pyrolysis
Abstract: Measuring martian organics and methane The Curiosity rover has been sampling on Mars for the past 5 years (see the Perspective by ten Kate). Eigenbrode et al. used two instruments in the SAM (Sample Analysis at Mars) suite to catch traces of complex organics preserved in 3-billion-year-old sediments. Heating the sediments released an array of organics and volatiles reminiscent of organic-rich sedimentary rock found on Earth. Most methane on Earth is produced by biological sources, but numerous abiotic processes have been proposed to explain martian methane. Webster et al. report atmospheric measurements of methane covering 3 martian years and found that the background level varies with the local seasons. The seasonal variation provides an important clue for determining the origin of martian methane. Science , this issue p. 1096 , p. 1093 ; see also p. 1068
Published: 2018
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11. Origin of nitrogen on Mars: First in situ N isotope analyses of martian meteorites

Author: Deligny, C., Füri, E., Deloule, E., Peslier, A.H., Faure, F., Marrocchi, Y., Swedish Museum of Natural History (NRM), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), NASA Johnson Space Center (JSC), NASA, and European Project: 715028,VOLATILIS
Subjects: Nitrogen, [SDU]Sciences of the Universe [physics], Geochemistry and Petrology, Mars, Nakhlites, Chassigny, Volatile accretion, SIMS
Abstract: International audience; Martian meteorites are key for assessing the isotopic characteristics of nitrogen in different martian reservoirs (i.e., mantle, crust, and atmosphere), and, ultimately, for constraining the source(s) of nitrogen trapped during the earliest stages of planetary accretion in the terrestrial planet-forming region. In this study, we analysed, for the first time, the nitrogen content and isotopic composition of glassy melt inclusions of Chassigny and of the mesostasis of five nakhlites (MIL 03346, Nakhla, NWA 6148, NWA 998, and Y 000593) by in situ secondary ion mass spectrometry. The nitrogen content of Chassigny melt inclusions, corrected for olivine overgrowth on the inclusion walls, varies from 4 ± 1 to 860 ± 45 ppm N, and the majority of δ 15 N values range from-35 ± 41 to +73 ± 36‰. The estimated nitrogen isotopic signature of the primitive melt, prior to degassing of N 2 or NH 3 , is 0 ± 32‰. The mesostasis of nakhlites contains 2.7 ± 0.2 to 943 ± 156 ppm N, with δ 15 N values from-30 ± 37 to +348 ± 43‰. Whereas degassing of N 2 or NH 3 can explain the lowest nitrogen isotopic ratios measured in the nakhlite mesostasis, the 15 N-enriched isotopic composition (δ 15 N > 150‰) of four nakhlites (MIL 03346, Nakhla, NWA 6148, and Y 000593) likely results from interaction of the mesostasis melt with the martian atmosphere during ejection. The δ 15 N values (+25 ± 42 and +77 ± 19‰) of two melt inclusions in Y 000593 are comparable to those of Chassigny, further confirming that these meteorites likely sample a common volatile reservoir in the martian interior. Overall, the new results indicate that the chassignitenakhlite reservoir did not inherit nitrogen from the solar nebula but, instead, from chondritic-like materials. These findings further confirm that planetary bodies in the inner solar system accreted (isotopically) chondritic nitrogen during the first few million years of solar system history.
Published: 2023
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12. Systematic identification of genes and transduction pathways involved in radio-adaptive response

Author: Wu, Honglu [NASA Johnson Space Center, Houston, TX (United States)]
Published: 2015

13. Physical Sedimentology and Stratigraphy of the lower Western Fan (Shenandoah formation) Jezero Crater, Mars:: Results from the Mars 2020 'Delta Front' Campaign

Author: Ives, Libby, Stack‐Morgan, Katie, Gupta, Sanjeev, Caravaca, Gwénaël, Russell, Patrick, Shuster, David L., Williams, Amy, Holm-Alwmark, Sanna, Barnes, Robert, Bell, Jim F., Beyssac, Olivier, Brown, Adrian, Flannery, David, Frydenvang, Jens, Grotzinger, John, Lamb, Michael P., Horgan, Briony, Hurowitz, Joel A., Kalucha, Hemani, Kanine, Oak, Núñez, Jorge, Randazzo, Nicolas, Seeger, Christina, Simon, Justin I., Tice, Michael M., Tebolt, Michelle, Kah, Linda C., Williams, Rebecca M.E., Amundsen, Hans, Annex, Andrew M., Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Earth Science and Engineering [Imperial College London], Imperial College London, 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), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), Berkeley Geochronology Center (BGC), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), University of Copenhagen = Københavns Universitet (UCPH), Arizona State University [Tempe] (ASU), 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), NASA Headquarters, Queensland University of Technology [Brisbane] (QUT), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Purdue University [West Lafayette], Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), University of Alberta, NASA Johnson Space Center (JSC), NASA, Texas A&M University [College Station], University of Texas at Austin [Austin], Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], Planetary Science Institute [Tucson] (PSI), and Vestfonna Geophysical
Subjects: jezero crater, delta, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Shenandoah formatin, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars 2020, perseverance, Mars, sedimentology, stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences
Abstract: International audience; The Perseverance rover is exploring a sedimentary deposit within the Late Noachian-aged (4.0-4.8 Ga) Jezero Crater interpreted to be the remnants of a delta. From April 2022 through February 2023, Perseverance investigated the basal 25 m of sediments exposed in the fan’s eastern scarp. Rover instruments collected a suite of imaging, geochemical, mineralogical, and ground-penetrating radar data.Perseverance made detailed observations through two sections of the lower fan ~600 m apart. Similar facies and stratigraphic trends are present in both sections. Each section contains two coarsening-up successions. While some finer-grained units are laterally continuous between the two sections, the coarser-grained bodies that cap each section are laterally discontinuous and do not extend between sections.Both sequences are 10 - 15 m thick. Their lower strata are dominated by sulfate-cemented, planar laminated, very fine- to medium-grained sandstone and siltstone with rare low-angle truncations. Soft-sediment deformation occurs in the form of decimeter-scale lateral folds. Laminae are normally graded. These sequences are capped by meter-scale thick sheets of coarse-grained sandstone, pebbly sandstones, and conglomerates that are variably low-angle cross-bedded, trough cross-bedded, and planar-stratified. Plane beds are massive or normally graded.Two hypotheses for the depositional environment have emerged for this succession: a sub-aerial setting with extensive “overbank” facies and shallow braided channels and a proximal pro-deltaic setting with deposition driven by hyperpycnal flows. These hypotheses will be tested against observations made by Perseverance as it traverses the “Fan Top” and by more comprehensive studies of the “Delta Front” data.
Published: 2023

14. Landscape of somatic mutations in 560 breast cancer whole-genome sequences

Author: John W.M. Martens, Sandrine Boyault, David Jones, Stefania Tommasi, Jeong-Yeon Lee, Germán Fg Rodríguez-González, Inigo Martincorena, Sung-Min Ahn, Alastair M Thompson, Manasa Ramakrishna, Gilles Thomas, Helen Davies, Savitri Krishnamurthy, Stian Knappskog, Steven Van Laere, Lucy Stebbings, Andrea L. Richardson, Andrew Tutt, Anne Lise Børresen-Dale, Olafur Oa Stefansson, Sunil R. Lakhani, Michiel M. Smid, Gerrit Gk Hooijer, Young Seok Ju, Tari Ta King, Rebecca Shepherd, Luc Dirix, Xavier Pivot, Adam Butler, Aquila Fatima, Peter Pt Simpson, Serena Nik-Zainal, Sancha Martin, Hyung-Yong Kim, Hendrik G. Stunnenberg, Jos Jonkers, Michael R. Stratton, Jon W. Teague, Se Jin Jang, Sandro Morganella, Ville Mustonen, Moritz Gerstung, Gu Kong, Carlos Caldas, Anne Vincent-Salomon, Anieta M. Sieuwerts, Lucy R. Yates, Sarah O’Meara, Peter B. Vermeulen, Dominik Glodzik, Peter Van Loo, Naoto T. Ueno, Arie B. Brinkman, Stuart McLaren, Yang Li, Marc J. van de Vijver, Laura Van't Veer, P. Andrew Futreal, Markus Ringnér, Christos Sotiriou, Ewan Birney, Kamna Ramakrishnan, Miriam Ragle Aure, Johan Staaf, Jane E. Brock, Benita Kiat Tee Bk Tan, Alain Viari, Xueqing Zou, Anita Langerød, David C. Wedge, Hee Jin Lee, Christine Desmedt, Gilles Romieu, Paul N. Span, Jorunn E. Eyfjord, Annegien Broeks, Isabelle Treilleux, Åke Borg, Colin Ca Purdie, Ole Christian Lingjærde, Gert Van den Eynden, John A. Foekens, Serge Dronov, Andrew Menzies, Peter J. Campbell, Iris Pauporté, Ludmil B. Alexandrov, Keiran Raine, The Wellcome Trust Sanger Institute [Cambridge], Lund University [Lund], Erasmus University Medical Center [Rotterdam] (Erasmus MC), Radboud university [Nijmegen], Oslo University Hospital Radiumhospitalet, University of Oslo (UiO), Gachon University Hospital, Génomique Fonctionnelle des Tumeurs Solides (U1162), Université Paris 13 (UP13)-Université Paris Diderot - Paris 7 (UPD7)-Université Paris Descartes - Paris 5 (UPD5)-Institut National de la Santé et de la Recherche Médicale (INSERM), Brigham and Women's Hospital [Boston], Netherlands Cancer Institute (NKI), Antoni van Leeuwenhoek Hospital, Breast Cancer Translational Research Laboratory, Institut Jules Bordet [Bruxelles], Faculté de Médecine [Bruxelles] (ULB), Université libre de Bruxelles (ULB)-Université libre de Bruxelles (ULB)-Faculté de Médecine [Bruxelles] (ULB), Université libre de Bruxelles (ULB)-Université libre de Bruxelles (ULB), Algemeen Ziekenhuis St Augustinus Oncology, Dana-Farber Cancer Institute [Boston], Academic Medical Center - Academisch Medisch Centrum [Amsterdam] (AMC), University of Amsterdam [Amsterdam] (UvA), University of Ulsan, NASA Johnson Space Center (JSC), NASA, University of Stuttgart, Esso UK Ltd, Department of Exploration, Esso UK Ltd, Department of Computer Science & Engineering [Riverside] (CSE), University of California [Riverside] (UCR), University of California-University of California, Department of Geriatric Medicine [Singapore] (Alexandra Hospital), Institut national du cancer [Boulogne] (INCA), Centre Hospitalier Régional Universitaire de Besançon (CHRU Besançon), Department of Pathology [Dundee], Ninewells Hospital and Medical School [Dundee], Canary Institute for Cancer Research (ICIC), Department of Biochemistry and Physiology, Faculty of Health Sciences, University of Las Palmas de Gran Canaria (ULPGC), Institut de Recherche en Cancérologie de Montpellier (IRCM - U1194 Inserm - UM), CRLCC Val d'Aurelle - Paul Lamarque-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Montpellier (UM), Department of Medical Oncology [Rotterdam], Cancer Genomics Centre, University of Queensland [Brisbane], University of Iceland [Reykjavik], Beckman Research Institute [Duarte, CA], Centre de Recherche en Cancérologie de Lyon (UNICANCER/CRCL), Centre Léon Bérard [Lyon]-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de la Santé et de la Recherche Médicale (INSERM), University of Antwerp (UA), European Central Bank (ECB), European Central Bank, Unité de génétique et biologie des cancers (U830), Université Paris Descartes - Paris 5 (UPD5)-Institut Curie [Paris]-Institut National de la Santé et de la Recherche Médicale (INSERM), Department of Tumor Biology, Institut Curie [Paris], University of Cambridge [UK] (CAM), Division of Diagnostic Oncology, Netherlands Cancer Institute, Agendia BV, Breakthrough Breast Cancer Centre, London Institute of Cancer, University of Bergen (UiB), National Cancer Centre Singapore (NCCS), National Cancer Centre Singapore, Division of Molecular Biology, National Institutes of Natural Sciences, The Graduate University for Advanced Studies, Baobab, Département PEGASE [LBBE] (PEGASE), Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire de Biométrie et Biologie Evolutive - UMR 5558 (LBBE), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique (Inria)-VetAgro Sup - Institut national d'enseignement supérieur et de recherche en alimentation, santé animale, sciences agronomiques et de l'environnement (VAS)-Centre National de la Recherche Scientifique (CNRS), Equipe de recherche européenne en algorithmique et biologie formelle et expérimentale (ERABLE), Inria Grenoble - Rhône-Alpes, Institut National de Recherche en Informatique et en Automatique (Inria)-Institut National de Recherche en Informatique et en Automatique (Inria), Department of Radiation Oncology 874, Radboud University Medical Center [Nijmegen], Department of Laboratory Medicine, Department Medical Oncology, Department of Pathology, Ospedale 'Mater Salutis', Goddard Earth Sciences and Technology and Research (GESTAR), NASA-Universities Space Research Association (USRA), Department of Molecular Biology [Nijmegen], Department of Organismic and Evolutionary Biology [Cambridge] (OEB), Harvard University [Cambridge], Department of Computing [London], Biomedical Image Analysis Group [London] (BioMedIA), Imperial College London-Imperial College London, Synergie Lyon Cancer [Lyon], Centre Léon Bérard [Lyon], Sagot, Marie-France, Radboud University [Nijmegen], University of California [Riverside] (UC Riverside), University of California (UC)-University of California (UC), Université de Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS), Nik-Zainal, Serena [0000-0001-5054-1727], Zou, Xueqing [0000-0003-1143-1028], Caldas, Carlos [0000-0003-3547-1489], Apollo - University of Cambridge Repository, Medical Oncology, Harvard University, Fondation Synergie Lyon Cancer [Lyon], CCA -Cancer Center Amsterdam, Pathology, Erasmus University Medical Center [Rotterdam], University of Oslo ( UiO ), Genomique Fonctionnelle des Tumeurs Solides, Université Paris Diderot - Paris 7 ( UPD7 ) -IFR105-Université Paris Descartes - Paris 5 ( UPD5 ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ), Netherlands Cancer Institute ( NKI ), Institut Jules Bordet, Academic Medical Center [Amsterdam] ( AMC ), University of Amsterdam [Amsterdam] ( UvA ), NASA Johnson Space Center ( JSC ), Department of Computer Science & Engineering [Riverside] ( CSE ), University of California [Riverside] ( UCR ), Institut national du cancer [Boulogne] ( INCA ), Hôpital Jean Minjoz, Centre Hospitalier Régional Universitaire [Besançon] ( CHRU Besançon ), Department of Medical Oncology, Erasmus Medical Center Rotterdam, Josephine Nefkens Institute and Cancer Genomics Centre, University of Las Palmas de Gran Canaria ( ULPGC ), Institut de Recherche en Cancérologie de Montpellier ( IRCM - U1194 Inserm - UM ), CRLCC Val d'Aurelle - Paul Lamarque-Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Université de Montpellier ( UM ), Erasmus MC, Beckman Research Institute, Centre de Recherche en Cancérologie de Lyon ( CRCL ), Centre Léon Bérard [Lyon]-Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre National de la Recherche Scientifique ( CNRS ), University of Antwerp ( UA ), European Central Bank ( ECB ), U 830, Institut National de la Santé et de la Recherche Médicale, Institut Curie, University of Cambridge [UK] ( CAM ), University of Bergen ( UIB ), National Cancer Centre Singapore ( NCCS ), Laboratoire de Biométrie et Biologie Evolutive ( LBBE ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Recherche en Informatique et en Automatique ( Inria ) -Centre National de la Recherche Scientifique ( CNRS ), Equipe de recherche européenne en algorithmique et biologie formelle et expérimentale ( ERABLE ), Institut National de Recherche en Informatique et en Automatique ( Inria ) -Institut National de Recherche en Informatique et en Automatique ( Inria ), Goddard Earth Sciences and Technology and Research ( GESTAR ), NASA-Universities Space Research Association ( USRA ), Department of Organismic and Evolutionary Biology ( OEB ), and Biomedical Image Analysis Group [London] ( BioMedIA )
Subjects: 0301 basic medicine, DNA Replication, Male, Mutation rate, DNA repair, [SDV]Life Sciences [q-bio], DNA Mutational Analysis, Genes, BRCA2, Genes, BRCA1, Breast Neoplasms, Biology, medicine.disease_cause, Genome, Cohort Studies, 03 medical and health sciences, Germline mutation, SDG 3 - Good Health and Well-being, Mutation Rate, medicine, Humans, Gene, Molecular Biology, Genetics, Mutation, Multidisciplinary, [ SDV ] Life Sciences [q-bio], Genome, Human, Recombinational DNA Repair, DNA, Neoplasm, Genomics, Oncogenes, Women's cancers Radboud Institute for Health Sciences [Radboudumc 17], 3. Good health, [SDV] Life Sciences [q-bio], 030104 developmental biology, Mutagenesis, Human genome, Female, Engineering sciences. Technology
Abstract: Item does not contain fulltext We analysed whole-genome sequences of 560 breast cancers to advance understanding of the driver mutations conferring clonal advantage and the mutational processes generating somatic mutations. We found that 93 protein-coding cancer genes carried probable driver mutations. Some non-coding regions exhibited high mutation frequencies, but most have distinctive structural features probably causing elevated mutation rates and do not contain driver mutations. Mutational signature analysis was extended to genome rearrangements and revealed twelve base substitution and six rearrangement signatures. Three rearrangement signatures, characterized by tandem duplications or deletions, appear associated with defective homologous-recombination-based DNA repair: one with deficient BRCA1 function, another with deficient BRCA1 or BRCA2 function, the cause of the third is unknown. This analysis of all classes of somatic mutation across exons, introns and intergenic regions highlights the repertoire of cancer genes and mutational processes operating, and progresses towards a comprehensive account of the somatic genetic basis of breast cancer.
Published: 2016
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15. THE MARKER BAND IN GALE CRATER:: A SYNTHESIS OF ORBITAL AND GROUND OBSERVATIONS

Author: Weitz, Catherine, Lewis, Kevin W., Kite, Edwin, Dietrich, William, Thompson, Lucy M., O’connell-Cooper, Catherine, Schieber, Juergen, Rubin, David M., Gasda, Patrick, Mondro, C. A., Seeger, Christina, Rapin, William, Gupta, Sanjeev, Roberts, Amelie, Frydenvang, Jens, Berger, Jeff, Newsom, Horton, Bryk, Alexander, Lamb, Michael P., Grotzinger, John, Fischer, W., Cowart, Aster, Davis, Joel, Grant, John A., Aileen Yingst, R., Farrand, William, Parker, Tim, Vasavada, Ashwin, Fraeman, Abigail, Milliken, Ralph, Sheppard, Rachel, Minitti, Michelle, Ming, Douglas W., Simpson, Sarah, Rampe, Elizabeth B., Mclennan, Scott, Fey, Deirdra M., Kubacki, Tex, Williams, Rebecca M.E., Arvidson, Ray, Caravaca, Gwénaël, Planetary Science Institute [Tucson] (PSI), Johns Hopkins University (JHU), University of Chicago, Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), University of New Brunswick (UNB), Indiana University [Bloomington], Indiana University System, University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), Los Alamos National Laboratory (LANL), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), 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), Department of Earth Science and Engineering [Imperial College London], Imperial College London, University of Copenhagen = Københavns Universitet (UCPH), NASA Johnson Space Center (JSC), NASA, The University of New Mexico [Albuquerque], 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), Birkbeck College [University of London], Smithsonian Institution, Space Science Institute [Boulder] (SSI), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Brown University, Planetary Geosciences Institute [Knoxville], Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville]-The University of Tennessee [Knoxville], Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Malin Space Science Systems (MSSS), Department of Earth and Planetary Sciences [St Louis], Washington University in Saint Louis (WUSTL), and Lunar and Planetary Institute
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars, sedimentology, stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, MSL, Marker Band, Gale crater, mineralogy
Abstract: International audience; The “Marker Band” (previously called the Marker Bed and Marker Horizon [1-4]) in Gale crater is a distinctive indurated and dark-toned unit observed in the strata of Mount Sharp. From orbital data, the Marker Band (MB) was mapped across much of the western and southern edges of Mount Sharp, spanning over 80 km in distance and 1.6 km in elevation [4]. CRISM spectra of the MB show no hydration signatures and broad absorptions around~1 and 2 μm interpreted to be from high-Ca pyroxene [4]. Favored origins for the MB based upon orbital observations included a more indurated sulfate, a sandstone, and a volcanic ash deposit. The Curiosity rover recently reached the MB and is now collecting critical in situ measurements to test these postulated and other origins and make new discoveries at the finer mm- to cm-scale that could not be assessed from orbital data. Here we provide a summary of several of the most crucial MB observations made by the rover thus far from sols 3640-3645 and 3668-present.
Published: 2023

16. Fine-scale sedimentary architecture of the upper part of the Jezero western delta front

Author: Gupta, Sanjeev, Bell III, J.F., Caravaca, Gwénaël, Mangold, Nicolas, Stack‐Morgan, Katie, Kanine, Oak, Tate, Christian, Tice, Michael M., Williams, Amy, Russell, Patrick, Núñez, Jorge, Dromart, Gilles, Williams, R, Le Mouélic, Stéphane, Barnes, Robert, Annex, Andrew, Paar, Gerhard, Holm-Alwmark, Sanna, Rice, Melissa S., Rice, James, Horgan, Briony, Grotzinger, John, Maki, Justin, Hickman Lewis, Keyron, Kah, Lindah, Shuster, David L., Simon, Justin I., Minitti, Michelle, Siebach, Kirsten, Gasnault, Olivier, Wiens, Roger, Maurice, Sylvestre, Farley, Kenneth A., Department of Earth Science and Engineering [Imperial College London], Imperial College London, Arizona State University [Tempe] (ASU), 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 Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Cornell University [New York], Texas A&M University [College Station], Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), 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), Planetary Science Institute [Tucson] (PSI), Joanneum Research, University of Copenhagen = Københavns Universitet (UCPH), Geology Department, Western Washington University, Western Washington University (WWU), School of Earth and Space Exploration [Tempe] (SESE), Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, The Natural History Museum [London] (NHM), The University of Tennessee [Knoxville], Berkeley Geochronology Center (BGC), NASA Johnson Space Center (JSC), NASA, Planetary Geosciences Institute [Knoxville], Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville]-The University of Tennessee [Knoxville], Rice University [Houston], and Lunar and Planetary Institute
Subjects: Jezero crater, delta, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], Mars 2020, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, sedimentology
Abstract: International audience; Orbital and rover observations of relict geomorphic features and stratigraphic architectures indicate Mars once had a warmer, wetter climate. Constraining the character, relative timing and persistence of ancient aqueous activity on Mars is possible through detailed interrogation of the stratal geometry of aqueously deposited sedimentary bodies. Such analyses inform interpretations of Martian climate evolution, potential habitability, and search strategies for rocks that might contain potential biosignatures. NASA’s Mars 2020 Perseverance rover mission is seeking signs of ancient life in Jezero crater and is collecting a cache of Martian rock and soil samples for planned return to Earth by a future mission.A prominent sedimentary fan deposit at the western margin of Jezero crater has been interpreted to be a riverdelta that built into an ancient lake basin during the Late Noachian-Early Hesperian epochs on Mars (~3.6-3.8Ga) [1, 2]. The Perseverance rover landed on 18 February 2021 ~2.2 km from the western fan. In March-April 2022, the rover conducted a rapid traverse along the eastern and southeastern side of Jezero fan onlyobtaining a few remote sensing observations along the way. In April 2022, the rover arrived at the base of theancient delta in the Three Forks region of the crater floor adjacent to the delta front (Fig. 1). During the ‘rapidtraverse’ and the exploration of two sections at the delta front - Cape Nukshak and Hawksbill Gap –Perseverance obtained striking images from the Mastcam-Z and SuperCam’s Remote Micro-Imagerinstruments of the stratigraphy exposed stratigraphically higher up in the fan’s erosional front [3]. Images providenew views of the stratigraphy exposed in the erosional front of the western Jezero delta; in particular, showingsections of the delta previously not visible from long distance observations and at much higher resolution.Here, we report its stratigraphy and sedimentology, which provide new constraints on the nature of the fandeposits, and therefore paleoenvironmental implications.
Published: 2023

17. THE PETROGENETIC HISTORY OF THE JEZERO CRATER DELTA FRONT FROM MICROSCALE OBSERVATIONS BY THE MARS 2020 PIXL INSTRUMENT

Author: Hurowitz, Joel, Tice, Michael M., Allwood, Abbigail, Cable, Morgan L., Bosak, T., Broz, Adrian, Caravaca, Gwénaël, Clark, Benton, Dehouck, Erwin, Fairén, Alberto, Gomez, F., Grotzinger, John, Gupta, Sanjeev, Johnson, Jeffrey, Kah, Linda, Kalucha, Hemani, Labrie, J., Li, A., Mandon, Lucia, Núñez, Jorge, Pedersen, D., Poulet, François, Randazzo, Nicolas, Scheller, Eva, Schmidt, Mariek E., Shuster, David L., Siebach, Kirsten, Siljeström, Sandra, Simon, Justin I., Tosca, Nicholas, Treiman, Allan, Vanbommel, Scott, Wade, Lawrence, Williford, Kenneth H., Yanchilina, Anastasia, Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Texas A&M University [College Station], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, 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), Space Science Institute [Boulder] (SSI), 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), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), The University of Tennessee [Knoxville], Department of Earth Sciences, Brock University, Department of Earth and Space Sciences, University of Washington, Danish Technical University, 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), University of Alberta, Berkeley Geochronology Center (BGC), Rice University [Houston], RISE Research Institutes of Sweden, NASA Johnson Space Center (JSC), NASA, University of Cambridge [UK] (CAM), Lunar and Planetary Institute [Houston] (LPI), Washington University in Saint Louis (WUSTL), Blue Marble Space Institute of Science (BMSIS), Impossible Sensing Inc., and Lunar and Planetary Institute
Subjects: Jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars 2020, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Mineralogy, geochemistry, delta front
Abstract: International audience; On ~sol 370 of the Perseverance rover mission, the Mars 2020 Science Team completed its investigation of igneous units of the Jezero crater floor [1] and directed Perseverance to drive towards the topographic scarp that marks the interface between the crater floor and Jezero’s western delta. The “Delta Front Campaign” consisted of close-up investigation and sampling of lithologies located there.Here, we report on the major findings relevant to the provenance and diagenetic history of these lithologies deduced from measurements made by the Planetary Instrument for X-ray Lithochemistry (PIXL), a micro-focus X-ray fluorescence (XRF) microscope [2]. Data were collected from two sections at Cape Nukshak and Hawksbill Gap; outcrop and member names are from [3]. Lithologies are described here in order from base to top of each section.
Published: 2023

18. A JOURNEY ACROSS THE TRANSITION BETWEEN THE IGNEOUS SÉÍTAH FLOOR UNIT AND THE DELTA WITH THE MARS2020 SUPERCAM INSTRUMENT AT JEZERO CRATER, MARS

Author: Beyssac, Olivier, Clavé, Elise, Dehouck, Erwin, Forni, Olivier, Udry, Arya, Beck, Pierre, Cousin, Agnès, Mangold, Nicolas, Quantin-Nataf, Cathy, Royer, Clément, Mandon, Lucia, Johnson, Jeffrey, Simon, Justin I., Meslin, Pierre-Yves, Fouchet, Thierry, Le Mouélic, Stéphane, Pilorget, Cédric, Caravaca, Gwénaël, Poulet, François, Lasue, Jérémie, Pilleri, Paolo, M. Ollila, Ann, Clegg, Samuel, Núñez, Jorge, Maurice, Sylvestre, Wiens, Roger, 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), 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 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), University of Nevada [Las Vegas] (WGU Nevada), 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, Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), NASA Johnson Space Center (JSC), NASA, 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), 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), Los Alamos National Laboratory (LANL), and Lunar and Planetary Institute
Subjects: Jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, SuperCam, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars 2020, seitah, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, mars, mineralogy
Abstract: International audience; During the first scientific campaign, Perseverance explored the Jezero crater floor and found two main igneous formations: the basaltic Máaz unit, and Séítah, consisting of an olivine-rich cumulate. Then the rover did a rapid traverse towards the second campaign region, Jezero’s delta. Just before reaching the lowest part of the delta, Perseverance encountered the Séítah formation again, with some variability in the degree of alteration. Here, we use the data obtained by the SuperCam instrument to document the structure and texture of rocks at the transition between Séítah and the delta front, its geochemistry and its primary and secondary mineralogy. Then, we discuss the simi-larities/differences between these rocks and discuss a geological scenario to account for these observations.
Published: 2023

19. The impact of compositional changes on random forest predictions: applica-tion to chemcam libs data from gale crater, mars

Author: Rammelkamp, K., Gasnault, O., Bedford, C. C., Dehouck, E., Schroder, S., German Aerospace Center (DLR), DLR Institute of Optical Sensor Systems, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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), Universities Space Research Association (USRA), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, 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), and Lunar and Planetary Institute
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: International audience
Published: 2023

20. OVERVIEW OF THE BEDROCK GEOCHEMISTRY AND MINERALOGY OBSERVED BY SUPERCAM DURING PERSEVERANCE'S DELTA FRONT CAMPAIGN

Author: Dehouck, Erwin, Forni, Olivier, Quantin-Nataf, Cathy, Beck, Pierre, Mangold, Nicolas, Royer, Clément, Clavé, Elise, Beyssac, Olivier, Johnson, Jeffrey, Mandon, Lucia, Poulet, François, Le Mouélic, Stéphane, Caravaca, Gwénaël, Kalucha, Hemani, Gibbons, Erin, Dromart, Gilles, Gasda, Patrick, Meslin, Pierre-Yves, Schroeder, Susanne, Udry, Arya, Anderson, Ryan B., Clegg, Samuel, Cousin, Agnès, Gabriel, Travis, Lasue, Jérémie, Fouchet, Thierry, Pilleri, Paolo, Pilorget, Cédric, Hurowitz, Joel, Núñez, Jorge, Williams, Amy, Russell, Patrick, Simon, Justin I., Maurice, Sylvestre, Wiens, Roger, 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 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 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, Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, 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 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), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), 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), McGill University = Université McGill [Montréal, Canada], Los Alamos National Laboratory (LANL), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), University of Nevada [Las Vegas] (WGU Nevada), US Geological Survey [Flagstaff], United States Geological Survey [Reston] (USGS), United States Geological Survey (USGS), 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), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), NASA Johnson Space Center (JSC), NASA, and Lunar and Planetary Institute
Subjects: jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars 2020, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, mars, delta front, geochemistry
Abstract: International audience; In February 2021, the Perseverance rover landed in Jezero crater, Mars. The crater floor was found to be composed of lava flows and cumulate rocks [1-5]. These magmatic rocks appear to have undergone some limited aqueous alteration; however, it is not clear whether this alteration is related to the lacustrine phase of the crater [1,3,6,7].After completing its exploration of the crater floor, Perseverance reached the foot of the Jezero western fan in late April 2022 (sol ~422). Long-distance images acquired earlier in the mission had already confirmed the deltaic nature of the fan [8], which had long been suspected from orbital observations [9,10]. Between April and December 2022, Perseverance investigated the basal layers of the delta at two locations named Hawksbill Gap and Cape Nukshak, which are ~400 m apart [11]. Here, we present an overview of the geo-chemistry and mineralogy of the delta rocks as observed by SuperCam, and show that these rocks record a diver-sity of past aqueous alteration environments.
Published: 2023

21. SEDIMENTOLOGY AND STRATIGRAPHY OF THE LOWER DELTA SEQUENCE, JEZERO CRATER,MARS

Author: Stack‐Morgan, Katie, Gupta, Sanjeev, Tebolt, Michelle, Caravaca, Gwénaël, Ives, Libby, Russell, Patrick, Shuster, David L., Williams, Amy, Holm-Alwmark, Sanna, Barnes, Robert, Bell, Jim F., Beyssac, Olivier, Brown, Adrian, Flannery, David, Grotzinger, John, Horgan, Briony, Hurowitz, Joel, Kalucha, Hemani, Kanine, Oak, Núñez, Jorge, Randazzo, Nicolas, Seeger, Christina, Simon, Justin I., Tice, Michael M., Williams, Rebecca M.E., Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Department of Earth Science and Engineering [Imperial College London], Imperial College London, University of Texas at Austin [Austin], 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), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), Berkeley Geochronology Center (BGC), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), University of Copenhagen = Københavns Universitet (UCPH), Arizona State University [Tempe] (ASU), 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), NASA Headquarters, Plancius Research LLC, Queensland University of Technology [Brisbane] (QUT), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Purdue University [West Lafayette], Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), University of Alberta, NASA Johnson Space Center (JSC), NASA, Texas A&M University [College Station], Planetary Science Institute [Tucson] (PSI), and Lunar and Planetary Institute
Subjects: Jezero crater, delta, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], shenandoah formation, [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars 2020, Mars, stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Sedimentology
Abstract: International audience; In April 2022, the Mars 2020 Perseverance rover arrived at the base of the ancient delta in Jezero crater after completing the first year of its mission exploring and sampling aqueously altered igneous rocks of the present-day crater floor [1]. Perseverance then spent ~200 sols exploring the lower ~25 m of rock exposed within the eastern scarp of the Jezero delta [2], a sedimentary sequence informally named the ‘Shenandoah’ formation. This studydescribes the sedimentology and stratigraphy of the Shenandoah formation explored by Perseverance at two sections—'Cape Nukshak’ and ‘Hawksbill Gap’— including a description, interpretation, and depositional framework for the facies that comprise it.
Published: 2023

22. EXPLORING THE JEZERO DELTA FRONT: OVERVIEW OF RESULTS FROM THE MARS 2020 PERSEVERANCE ROVER'S SECOND SCIENCE CAMPAIGN

Author: Williams, Amy, Russell, Patrick, Sun, Vivian Z., Shuster, David L., Stack‐Morgan, Katie, Farley, Kenneth A., del Sesto, Tyler, Kronyak, Rachel E., Bell, Jim F., Beyssac, Olivier, Brown, Adrian J., Caravaca, Gwénaël, Gupta, Sanjeev, Núñez, Jorge, Randazzo, Nicolas, Simon, Justin I., Wadhwa, Meenakshi, Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Berkeley Geochronology Center (BGC), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), California Institute of Technology (CALTECH), Arizona State University [Tempe] (ASU), 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), Plancius Research LLC, 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), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), University of Alberta, NASA Johnson Space Center (JSC), NASA, and Lunar and Planetary Institute
Subjects: jezero crater, delta, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars, mars 2020, sedimentology, stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, delta front campaign
Abstract: International audience; The Perseverance rover landed in Jezero crater on February 18, 2021, with the mission goals to explore the geology, astrobiological potential, and modern environment of the crater floor and delta, and to collect and cache well-documented samples for Mars Sample Return. After completion of the “Crater Floor” science campaign [1], the rover conducted a rapid traverse (sols 379-414) to the Three Forks region of the crater floor adjacent to the delta front. From here, Perseverance’s second “Delta Front” science campaign (DFC) began on Sol 415, April 20, 2022. The DFC has explored two lobes of the delta front, the neighboring crater floor, and their contact zone, focusing on the lowest geologic exposures composing the Jezero delta (largely mapped within the delta “thin layered unit” [2]). As of January 1, 2023, Perseverance has covered 14325 km of traverse distance and collected 15 rock sample cores, 2 regolith samples, 1 atmospheric sample, and 3 witness tubes, employing a sample pair strategy where each unique sample is paired with a companion sample core from the same location, to enable the construction of two different caches [3]. After sample depot construction at Three Forks, the DFC will conclude upon re-ascent of the delta front, and the next “Delta Top” science campaign will start.
Published: 2023

23. Rb-Sr, Sm-Nd and Ar-Ar isotopic systematics of Antarctic nakhlite Yamato 000593

Author: Misawa,Keiji, Shih,Chi-Yu, Wiesmann,Henry, Garrison,Daniel H., Nyquist,Laurence E., Bogard,Donald D., and Antarctic Meteorite Research Center, National Institute of Polar Research/Mail Code C23, Lockheed-Martin Space Operations/Mail Code C23, Lockheed-Martin Space Operations/Mail Code C23, Lockheed-Martin Space Operations/Mail Code SR, NASA Johnson Space Center/Mail Code SR, NASA Johnson Space Center
Subjects: Yamato 000593, nakhlite, Ar-Ar, Rb-Sr, Sm-Nd, chronology, crystallization, aqueous alteration, source material
Abstract: sotopic analysis of the newly found Antarctic nakhlite Yamato (Y) 000593 yields a Rb-Sr age of 1.30±0.02Ga with an initial ^(87)Sr/^(86)Sr of 0.702525±0.000027, a Sm-Nd age of 1.31±0.03Ga with an initial ε_(Nd) of + 16.0±0.2 and an Ar-Ar isochron age of
Published: 2005

24. Dark microbiome and extremely low organics in Atacama fossil delta unveil Mars life detection limits

Author: Armando Azua-Bustos, Alberto G. Fairén, Carlos González-Silva, Olga Prieto-Ballesteros, Daniel Carrizo, Laura Sánchez-García, Victor Parro, Miguel Ángel Fernández-Martínez, Cristina Escudero, Victoria Muñoz-Iglesias, Maite Fernández-Sampedro, Antonio Molina, Miriam García Villadangos, Mercedes Moreno-Paz, Jacek Wierzchos, Carmen Ascaso, Teresa Fornaro, John Robert Brucato, Giovanni Poggiali, Jose Antonio Manrique, Marco Veneranda, Guillermo López-Reyes, Aurelio Sanz-Arranz, Fernando Rull, Ann M. Ollila, Roger C. Wiens, Adriana Reyes-Newell, Samuel M. Clegg, Maëva Millan, Sarah Stewart Johnson, Ophélie McIntosh, Cyril Szopa, Caroline Freissinet, Yasuhito Sekine, Keisuke Fukushi, Koki Morida, Kosuke Inoue, Hiroshi Sakuma, Elizabeth Rampe, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Instituto de Ciencias Biomédicas [Santiago] (ICB), Universidad Autonoma de Chile, Department of Astronomy [Ithaca], Cornell University [New York], Universidad de Tarapaca, Departamento de Ecología [Madrid], Universidad Autónoma de Madrid (UAM), Museo Nacional de Ciencias Naturales [Madrid] (MNCN), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Universidad de Valladolid [Valladolid] (UVa), 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), Department of Earth, Atmospheric, and Planetary Sciences [West Lafayette] (EAPS), Purdue University [West Lafayette], Southwest Sciences, Inc., GSFC Solar System Exploration Division, NASA Goddard Space Flight Center (GSFC), Department of Biology [Washington], Georgetown University [Washington] (GU), 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), Earth-Life Science Institute [Tokyo] (ELSI), Tokyo Institute of Technology [Tokyo] (TITECH), Institute of Nature and Environmental [Kanazawa], Kanazawa University (KU), National Institute for Materials Science (NIMS), NASA Johnson Space Center (JSC), NASA, European Commission, Ministerio de Economía y Competitividad (España), Comunidad de Madrid, Ministerio de Ciencia e Innovación (España), and Agencia Estatal de Investigación (España)
Subjects: Multidisciplinary, [SDU]Sciences of the Universe [physics], General Physics and Astronomy, General Chemistry, General Biochemistry, Genetics and Molecular Biology
Abstract: Identifying unequivocal signs of life on Mars is one of the most important objectives for sending missions to the red planet. Here we report Red Stone, a 163-100 My alluvial fan–fan delta that formed under arid conditions in the Atacama Desert, rich in hematite and mudstones containing clays such as vermiculite and smectites, and therefore geologically analogous to Mars. We show that Red Stone samples display an important number of microorganisms with an unusual high rate of phylogenetic indeterminacy, what we refer to as “dark microbiome”, and a mix of biosignatures from extant and ancient microorganisms that can be barely detected with state-of-the-art laboratory equipment. Our analyses by testbed instruments that are on or will be sent to Mars unveil that although the mineralogy of Red Stone matches that detected by ground-based instruments on the red planet, similarly low levels of organics will be hard, if not impossible to detect in Martian rocks depending on the instrument and technique used. Our results stress the importance in returning samples to Earth for conclusively addressing whether life ever existed on Mars., The research leading to these results is a contribution from the Project “MarsFirstWater”, funded by the European Research Council, Consolidator Grant no 818602 to AGF, and by the Human Frontiers Science Program grant n° RGY0066/2018 to A.A.-B. Additional funding provided was provided by MINECO grant PID2019-107442RB-C32 (O.P.-B. and A.M.), Grants-in-Aid for Scientific Research from the Japan Society for Promotion of Science grant numbers 17H06458 and 21H04515 (K.F.), grant numbers 17H06456, 17H06458, 20H00195, and 21H04515 (K.F. and Y.S.), Consejería de Educación e Investigación, Comunidad Autónoma de Madrid/European Social Fund program (MAFM), grant n° ESP2017-87690-C3-3-R (DC), Ramón y Cajal grant n° RYC2018-023943-I (L.S.-G.), AEI grant MDM-2017-0737 and MCIN/AEI grant PID2019-107442RB-C32 (V.M.-I.), MCIU/AEI (Spain) and FEDER (UE) grant n° PGC2018-094076-B-I00 (J.W. and C.A.), Italian Space Agency agreement 2017-48-H.0 (T.F., J.R.B. and G.P.), the Ministry of Science of Spain grant PID2019-107442RB-C31 (J.A.M., M.V., G.L.R., A.A. and F.R.), María Zambrano’ excellence grant program (CA3/RSUE/2021-00405), funded by the Spanish Ministry of Universities (MFM), NASA Mars Exploration Program contracts NNH13ZDA018O, NNH15AZ24I, NNH13ZDA018O and LANL Laboratory Directed Research and Development (LDRD) funding XX5V (A.M.O, R.C.W., A.R. and S.M.C.), NASA-GSFC grant NNX17AJ68G (M.M. and S.S.J.), NES focused on Sample Analysis at Mars of the Mars Science Laboratory mission, and Mars Organic Molecules Analyzer of the Exomars 2022 mission (O.M., C.S., and C.F.), and grants RTI2018-094368-B-I00 and MDM-2017-0737 Unidad de Excelencia “Maria de Maeztu”- Centro de Astrobiología (INTA-CSIC) by the Spanish Ministry of Science and Innovation/State Agency of Research MCIN/AEI/ 10.13039/501100011033 and by “ERDF A way of making Europe” (C.E., M.G.V., M.M.-P., and V.P.). R.C.W. thanks Dot Delapp for performing pre-processing of the LIBS data., With funding from the Spanish government through the "Severo Ochoa Center of Excellence" accreditation MDM-2017-0737.
Published: 2023
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25. Petrological traverse of the olivine cumulate Séítah formation at Jezero crater, Mars : A perspective from SuperCam onboard Perseverance

Author: Beyssac, O., Forni, O., Cousin, A., Udry, A., Kah, L.C., Mandon, L., Clavé, E., Liu, Y., Poulet, F., Quantin Nataf, C., Gasnault, O., Johnson, J., Benzerara, K., Beck, P., Dehouck, E., Mangold, N., Alvarez Llamas, C., Anderson, R., Arana, G., Barnes, R., Bernard, S., Bosak, T., Brown, A.J., Castro, K., Chide, B., Clegg, S., Cloutis, E., Fouchet, T., Gabriel, T., Gupta, S., Lacombe, G., Lasue, J., Le Mouelic, S., Lopez‐Reyes, G., Madariaga, J.M., McCubbin, F.M., McLennan, S., Manrique, J.A., Meslin, P.Y., Montmessin, F., Núñez, J., Ollila, A.M., Ostwald, A., Pilleri, P., Pinet, P., Royer, C., Sharma, S.K., Schröder, Susanne, Simon, J.I., Toplis, M.J., Veneranda, M., Willis, P.A., Maurice, S., Wiens, R.C., 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 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), Department of Geoscience [Las Vegas], University of Nevada [Las Vegas] (WGU Nevada), Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], 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), 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 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), 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), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Laboratoire de Planétologie et Géosciences - Angers (LPG-ANGERS), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Department of Analytical Chemistry [Malaga], Universidad de Málaga [Málaga] = University of Málaga [Málaga], Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Department of Analytical Chemistry [Leioa], University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Plancius Research LLC, Los Alamos National Laboratory (LANL), University of Winnipeg, Laboratoire Energie Signal Images et Automatique [Univ Ngaoundéré] (LESIA), Université de Ngaoundéré/University of Ngaoundéré [Cameroun] (UN), Universidad de Valladolid [Valladolid] (UVa), NASA Johnson Space Center (JSC), NASA, Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), 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), Hawaii Institute of Geophysics and Planetology (HIGP), University of Hawai‘i [Mānoa] (UHM), DLR Institute of Optical Sensor Systems, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Department of Earth, Atmospheric, and Planetary Sciences [West Lafayette] (EAPS), and Purdue University [West Lafayette]
Subjects: spectroscopy, LIBS, m2020, Mars, Perseverance, Jezero, Jezero crater, reflectance spectroscopy, in-situ, [SDU]Sciences of the Universe [physics], rover, Seitah, VisIR, Raman, in-situ science
Abstract: International audience; Séítah is the stratigraphically lowest formation visited by Perseverance in the Jezero crater floor. We present the data obtained by SuperCam: texture by imagery, chemistry by LIBS, and mineralogy by VISIR and Raman spectroscopy. The Séítah formation consists of igneous, weakly altered, rocks dominated by millimeter-size grains of olivine with the presence of low-Ca and high-Ca pyroxenes, and other primary minerals (e.g., plagioclase, Cr-Fe-Ti oxides, phosphates). Along a ∼140 m long section in Séítah, SuperCam analyses showed evidence of geochemical and mineralogical variations, from the contact with the overlying Máaz formation, going deeper in the formation. Bulk rock and olivine Mg#, grain size, olivine content increase gradually further from the contact. Along the section, olivine Mg# are not in equilibrium with the bulk rock Mg#, indicating local olivine accumulation. These observations are consistent with Séítah being the deep ultramafic member of a cumulate series derived from the fractional crystallization and slow cooling of the parent magma at depth. Possible magmatic processes and exhumation mechanisms of Séítah are discussed. Séítah rocks show some affinity with some rocks at Gusev crater, and with some martian meteorites suggesting that such rocks are not rare on the surface of Mars. Séítah is part of the Nili Fossae regional olivine-carbonate unit observed from orbit. Future exploration of Perseverance on the rim and outside of the crater will help determine if the observations from the crater floor can be extrapolated to the whole unit, or if this unit is composed of distinct sub-units with various origins.
Published: 2023
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26. 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
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27. Insights into the Sedimentary Record and Processes of the Western Delta of Jezero crater (Mars) as observed by the Mars 2020 rover Perseverance. (Invited)

Author: Caravaca, Gwénaël, Mangold, Nicolas, Gupta, Sanjeev, Stack, Kathryn, Núñez, Jorge, Dromart, Gilles, Kanine, Oak, Tate, Christian, Minitti, Michelle, Sholes, Steven, Tice, Michael M., Nachon, Marion, Siebach, Kirsten, Grotzinger, John, Flannery, David, Simon, Justin I., Horgan, Briony, Le Mouélic, Stéphane, Shuster, David L., Williams, Amy, Russell, Patrick, Farley, Kenneth A., 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 Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), 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), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Cornell University [New York], Planetary Geosciences Institute [Knoxville], Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville]-The University of Tennessee [Knoxville], Texas A&M University [College Station], Rice University [Houston], Queensland University of Technology [Brisbane] (QUT), NASA Johnson Space Center (JSC), NASA, Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, Berkeley Geochronology Center (BGC), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), University of California [Los Angeles] (UCLA), University of California (UC), American Geophysical Union, and CARAVACA, Gwénaël
Subjects: paleoenvironment, shenandoah formation, Mars 2020, sedimentology, stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, [SDU] Sciences of the Universe [physics], Jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, [SDU.STU] Sciences of the Universe [physics]/Earth Sciences, [SDU.STU.ST] Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, [SDU.STU.PL] Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract: International audience; Since its landing in Jezero crater in February 2021, the western delta of Jezero has been one of the main targets for the Perseverance rover to explore and sample sedimentary rocks that lead us to better understand the environmental evolution of the region, and could host traces of past biosignatures.During the first year, the rover explored the floor of Jezero crater, focusing on aqueously altered igneous rocks. It also provided the opportunity to remotely observe the main delta front and its remnants (e.g., the Kodiak butte). This allowed us to distinguish several beds of sandstones (with local occurrences of boulders up to 30 cm) arranged into bottomsets, foresets and topsets morphologies. This tripartite geometry and steep slopes of foresets are characteristic of a Gilbert-type delta, formed by the deposition of fluvial sediments prograding into a standing body of water, here a paleolake whose level can be constrained by the transition from the foresets to topsets. Massive beds of boulder conglomerates (with boulders up to 1.5 m) have also been observed at or close to the top of many locations along the delta’s front, hinting at a transition to higher energy flows. Collectively, these elements argue for a polyphase complex depositional history of the delta through time.The toe of the current delta front was reached by the rover on Sol 422 (April 2022) when Perseverance arrived at the Enchanted Lake outcrop, at the base of the southeastern end of the promontory informally named Cape Nukshak on the distal end of the delta. The first in-place sedimentary rocks that were observed were a succession of thinly-laminated medium/coarse sandstones and mudstones. Then, Perseverance pursued its route towards the delta and started its ascension at Hawksbill Gap to assess the first half of the lower delta succession. Strata at the base of Hawksbill Gap are mostly composed of fine to coarse-grained rocks ranging from mudstones to granule conglomerates, displaying planar to low-angle cross-stratifications.These fine-grained detrital rocks are likely to have been deposited by fluvial to deltaic processes. There, the rover collected the first sets of paired sedimentary rock samples (coarse sandstone to micro-conglomerate) that will represent the fine- and coarse-grained lower delta succession once returned to Earth.
Published: 2022

28. Jezero Crater Floor and Delta Chemistry and Mineralogy Observed by SuperCam in the First 1.5 Years of the Perseverance Rover Mission

Author: Wiens, Roger, Maurice, Sylvestre, Clegg, Samuel, Cousin, Agnès, Dehouck, Erwin, Udry, Arya, Beyssac, Olivier, Quantin-Nataf, Cathy, Mangold, Nicolas, Mandon, Lucia, Forni, Olivier, Benzerara, Karim, Johnson, Jeffrey Roy, Anderson, Ryan, Gasda, Patrick, Royer, Clément, Madariaga, Juan Manuel, Pinedo, Kepa Castro Ortiz De, Arana, Gorka, Meslin, Pierre-Yves, Ollila, Ann, Legett, Carey, Poulet, François, Sharma, Shiv, Comellas, Jade, Chide, Baptiste, Acosta-Maeda, Tayro, Clave, Elise, Hausrath, Elisabeth, Simon, Justin, Bosak, Tanja, Brown, Adrian, Laserna, Javier, Alvarez, César, Lasue, Jérémie, Cloutis, Edward, Caravaca, Gwénaël, Connell, Stephanie, Wolf, Uriah, Sidhu, Sahejpal, Turenne, Nathalie, Ostwald, Amanda, Mouélic, Stéphane Le, Lopez-Reyes, Guillermo, Manrique, José, Veneranda, Marco, Pilleri, Paolo, Fouchet, Thierry, Pilorget, Cédric, Gabriel, Travis, Gibbons, Erin, Lanza, Nina, Larmat, Carene, Horgan, Briony, Nachon, Marion, Rapin, William, Manelski, Henry, Martinez-Frias, Jesus, Pinet, Patrick, 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 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), University of Nevada [Las Vegas] (WGU Nevada), 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 Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), 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), 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), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), United States Geological Survey (USGS), University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), 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), University of Hawaii, University of Hawai‘i [Mānoa] (UHM), 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), NASA Johnson Space Center (JSC), NASA, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), NASA Headquarters, Plancius Research LLC, Universidad de Málaga [Málaga] = University of Málaga [Málaga], University of Winnipeg, Universidad de Valladolid [Valladolid] (UVa), Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), McGill University = Université McGill [Montréal, Canada], Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, Texas A&M University [Galveston], Purdue University [West Lafayette], Instituto de Geociencias [Madrid] (IGEO), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and American Geophysical Union
Subjects: Jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, SuperCam, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars 2020, sedimentology, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, mineralogy, geochemistry, petrography
Abstract: International audience; Jezero crater was chosen for exploration and sample collection by Perseverance due to its history as a lake with river deltas, its diverse mineralogy, including carbonates observed from orbit, and as a potential site to calibrate crater counting ages with radiometric dates of samples to be returned to Earth. This presentation focuses on the results of SuperCam, which uses LIBS for remote elemental chemistry, VISIR and remote Raman spectroscopy for mineral compositions and alteration, includes a microphone, and performs high-resolution imaging for textures and morphology. In the first year after landing, SuperCam and other instruments were used to explore Jezero’s floor. We found that all of the floor units are igneous, with lava flows comprising the upper units as part of the Máaz formation, while the lower formation, Séítah, is an olivine cumulate, produced by gravitational settling of olivine crystals in a large melt body. Artuby ridge, just outside the SW portion of Séítah and stratigraphically just above it, contains up to 60% pyroxene. The upper portions of the Máaz formation are more enriched in plagioclase, with the uppermost Ch’al member having the most evolved composition, along with the Content member, pitted rocks directly overlying the main cumulate portion of Séítah. After exploring the floor, Perseverance drove to the delta formation and began a walk-about style of observations starting at Enchanted Lake, just below an arm of the delta formation, and then moving into Hawksbill Gap, climbing 18 m in elevation between Devil’s Tanyard, Sunset Hill, and Hogwallow flats. Delta compositions initially displayed higher phyllosilicate contents, identified by absorptions at 1.4, 1.9, and 2.3 µm, and by higher LIBS H peak areas. Farther up, compositions changed to sulfur-bearing in lower locations within the continuous fine-grained light-toned strata (e.g., Pignut Mountain, Sol 463) and carbonate-rich in upper strata. Veins were observed, consisting of Mg-Fe carbonate (Elder Ridge, Sol 459) and anhydrite (Reid’s Gap, Sol 466). The sulfates suggest precipitation of these salts at a later stage, as the lake was evaporating. Carbonates and sulfates in veins in different locations indicate that groundwater was active in the lithified sediments and had significantly different chemistry at different intervals.
Published: 2022

29. Fine-Scale Sedimentary Architecture of the Jezero Western Delta Front

Author: Gupta, Sanjeev, Bell, Jim F., Caravaca, Gwénaël, Kanine, Oak, Mangold, Nicolas, Stack, Kathryn, Tate, Christian, Tice, Michael M., Williams, Amy, Russell, Patrick, Núñez, Jorge, Dromart, Gilles, Williams, Rebecca M. E., Le Mouélic, Stéphane, Barnes, Robert, Annex, Andrew, Paar, Gerhard, Holm-Alwmark, Sanna, Rice, Melissa S., Rice, James, Horgan, Briony, Grotzinger, John, Maki, Justin, Hickman-Lewis, Keyron, Kah, Linda, Shuster, David L., Simon, Justin I., Minitti, Michelle, Siebach, Kirsten, Gasnault, Olivier, Wiens, Roger, Maurice, Sylvestre, Farley, Kenneth A., Department of Earth Science and Engineering [Imperial College London], Imperial College London, Arizona State University [Tempe] (ASU), 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), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Cornell University [New York], Texas A&M University [College Station], Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), 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), Planetary Science Institute [Tucson] (PSI), Joanneum Research, University of Copenhagen = Københavns Universitet (UCPH), Geology Department, Western Washington University, Western Washington University (WWU), School of Earth and Space Exploration [Tempe] (SESE), Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, The Natural History Museum [London] (NHM), The University of Tennessee [Knoxville], Berkeley Geochronology Center (BGC), NASA Johnson Space Center (JSC), NASA, Planetary Geosciences Institute [Knoxville], Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville]-The University of Tennessee [Knoxville], Rice University [Houston], and American Geophysical Union
Subjects: gibert-delta, Jezero crater, delta, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars 2020, sedimentology, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, sedimentary architecture
Abstract: International audience; A key exploration target for the Perseverance rover mission is a sedimentary fan deposit at the western margin of Jezero crater, which has been interpretated to be a river delta that built into a lake basin during the Late Noachian-Early Hesperian epochs on Mars (~3.6-3.8 Ga). Images from the Mastcam-Z and SuperCam Remote Micro-Imager instruments provide striking views of the stratigraphy exposed in the fan’s erosional front. Here, we report its stratigraphy and sedimentology, which place constraints on the nature of the fan deposits and their paleoenvironmental implications.Multiple Mastcam-Z mosaics show spectacular views of the stratigraphy of a prominent embayment in the delta scarp that has been informally named Hawksbill Gap, the lower section of which the rover is investigating and sampling. The prominent cliffs of the eastern and western margin of Hawksbill Gap show distinctive stratal geometries with complex stratigraphic relations. The basal succession comprises poorly exposed thinly bedded, planar laminated sandstones that are interpreted as the deposits of low-density turbidity currents. A locally prominent, resistant unit named Rocky Top comprises planar stratified pebbly sandstones also likely to be high-density turbidite deposits. The stratigraphic mid-sections of the scarps are characterized by packages of decameter-scale inclined tabular strata. These tabular beds are locally conglomeratic but predominantly comprise finer-than-conglomerate lithologies, likely pebbly sandstones. Interstratified within these are poorly sorted matrix-supported conglomerates interpreted to be debris flow deposits. The inclined strata are overlain across a sharp truncation surface by generally planar parallel thin-bedded horizontal strata that we interpret as topset beds. Conglomerate beds containing bouldersare located within the overlying topset strata. The stratal patterns are broadly consistent with deposition in a Gilbert-type delta setting with basal strata representing deposition from sediment gravity flows, inclined strata representing foreset beds, and overlying topset beds deposition from fluvial processes in a delta top environment. The boulder conglomerates indicate sediment-transport on the delta top by episodic high-discharge floods.
Published: 2022

30. How Mercury can be the most reduced terrestrial planet and still store iron in its mantle

Author: Kevin Righter, Roger H. Hewins, Thomas Smith, Suzy Surblé, Caroline Raepsaet, Hélène Bureau, Valérie Malavergne, Fabrice Brunet, Brigitte Zanda, Ahmed Addad, E. Charon, Patrick Cordier, Laboratoire Géomatériaux et Environnement (LGE), Université Paris-Est Marne-la-Vallée (UPEM), Laboratoire de géologie de l'ENS (LGENS), Institut national des sciences de l'Univers (INSU - CNRS)-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), Unité Matériaux et Transformations - UMR 8207 (UMET), Institut National de la Recherche Agronomique (INRA)-Ecole Nationale Supérieure de Chimie de Lille (ENSCL)-Institut de Chimie du CNRS (INC)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), NASA Johnson Space Center (JSC), NASA, 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), 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), Department of Earth and Planetary Sciences [Piscataway], Rutgers, The State University of New Jersey [New Brunswick] (RU), Rutgers University System (Rutgers)-Rutgers University System (Rutgers), Service Interdisciplinaire sur les Systèmes Moléculaires et les Matériaux (ex SCM) (SIS2M UMR 3299), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Programme National de Planetologie of the Institut National des Sciences de l'Univers (INSU), Lunar and Planetary Institute, NASA Johnson Space Center (Houston, TX, USA), Conseil Regional du Nord-Pas de Calais, European Regional Development Fund (ERDF), INSU, CNRS, Laboratoire de géologie de l'ENS (LGE), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Ecole Nationale Supérieure de Chimie de Lille (ENSCL)-Institut National de la Recherche Agronomique (INRA), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF), 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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), and Institut de Chimie du CNRS (INC)-Institut National de la Recherche Agronomique (INRA)-Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Ecole Nationale Supérieure de Chimie de Lille (ENSCL)
Subjects: planetary differentiation, sulfides, Inorganic chemistry, Mineralogy, chemistry.chemical_element, Mercury, Mantle (geology), Outer core, Troilite, Silicate, Mercury (element), chemistry.chemical_compound, Geophysics, chemistry, 13. Climate action, Space and Planetary Science, Geochemistry and Petrology, Core–mantle boundary, Earth and Planetary Sciences (miscellaneous), enstatitechondrites, primitive mantle, Primitive mantle, Planetary differentiation, Geology, [SDU.STU.MI]Sciences of the Universe [physics]/Earth Sciences/Mineralogy
Abstract: International audience; Mercury is notorious as the most reduced planet with the highest metal/silicate ratio, yet paradoxically data from the MESSENGER spacecraft show that its iron-poor crust is high in sulfur (up to ∼6 wt%, ∼80× Earth crust abundance) present mainly as Ca-rich sulfides on its surface. These particularities are simply impossible on the other terrestrial planets. In order to understand the role played by sulfur during the formation of Mercury, we investigated the phase relationships in Mercurian analogs of enstatite chondrite-like composition experimentally under conditions relevant to differentiation of Mercury (∼1 GPa and 1300–2000 °C). Our results show that Mg-rich and Ca-rich sulfides, which both contain Fe, crystallize successively from reduced silicate melts upon cooling below 1550 °C. As the iron concentration in the reduced silicates stays very low (≪1 wt%), these sulfides represent new host phases for both iron and sulfur in the run products. Extrapolated to Mercury, these results show that Mg-rich sulfide crystallization provides the first viable and fundamental means for retaining iron as well as sulfur in the mantle during differentiation, while sulfides richer in Ca would crystallize at shallower levels. The distribution of iron in the differentiating mantle of Mercury was mainly determined by its partitioning between metal (or troilite) and Mg–Fe–Ca-rich sulfides rather than by its partitioning between metal (or troilite) and silicates. Moreover, the primitive mantle might also be boosted in Fe by a reaction at the core mantle boundary (CMB) between Mg-rich sulfides of the mantle and FeS-rich outer core materials to produce (Fe, Mg)S. The stability of Mg–Fe–Ca-rich sulfides over a large range of depths up to the surface of Mercury would be consistent with sulfur, calcium and iron abundances measured by MESSENGER.
Published: 2014
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31. Formation and evolution of carbonaceous asteroid Ryugu: Direct evidence from returned samples

Author: T. Nakamura, M. Matsumoto, K. Amano, Y. Enokido, M. E. Zolensky, T. Mikouchi, H. Genda, S. Tanaka, M. Y. Zolotov, K. Kurosawa, S. Wakita, R. Hyodo, H. Nagano, D. Nakashima, Y. Takahashi, Y. Fujioka, M. Kikuiri, E. Kagawa, M. Matsuoka, A. J. Brearley, A. Tsuchiyama, M. Uesugi, J. Matsuno, Y. Kimura, M. Sato, R. E. Milliken, E. Tatsumi, S. Sugita, T. Hiroi, K. Kitazato, D. Brownlee, D. J. Joswiak, M. Takahashi, K. Ninomiya, T. Takahashi, T. Osawa, K. Terada, F. E. Brenker, B. J. Tkalcec, L. Vincze, R. Brunetto, A. Aléon-Toppani, Q. H. S. Chan, M. Roskosz, J.-C. Viennet, P. Beck, E. E. Alp, T. Michikami, Y. Nagaashi, T. Tsuji, Y. Ino, J. Martinez, J. Han, A. Dolocan, R. J. Bodnar, M. Tanaka, H. Yoshida, K. Sugiyama, A. J. King, K. Fukushi, H. Suga, S. Yamashita, T. Kawai, K. Inoue, A. Nakato, T. Noguchi, F. Vilas, A. R. Hendrix, C. Jaramillo-Correa, D. L. Domingue, G. Dominguez, Z. Gainsforth, C. Engrand, J. Duprat, S. S. Russell, E. Bonato, C. Ma, T. Kawamoto, T. Wada, S. Watanabe, R. Endo, S. Enju, L. Riu, S. Rubino, P. Tack, S. Takeshita, Y. Takeichi, A. Takeuchi, A. Takigawa, D. Takir, T. Tanigaki, A. Taniguchi, K. Tsukamoto, T. Yagi, S. Yamada, K. Yamamoto, Y. Yamashita, M. Yasutake, K. Uesugi, I. Umegaki, I. Chiu, T. Ishizaki, S. Okumura, E. Palomba, C. Pilorget, S. M. Potin, A. Alasli, S. Anada, Y. Araki, N. Sakatani, C. Schultz, O. Sekizawa, S. D. Sitzman, K. Sugiura, M. Sun, E. Dartois, E. De Pauw, Z. Dionnet, Z. Djouadi, G. Falkenberg, R. Fujita, T. Fukuma, I. R. Gearba, K. Hagiya, M. Y. Hu, T. Kato, T. Kawamura, M. Kimura, M. K. Kubo, F. Langenhorst, C. Lantz, B. Lavina, M. Lindner, J. Zhao, B. Vekemans, D. Baklouti, B. Bazi, F. Borondics, S. Nagasawa, G. Nishiyama, K. Nitta, J. Mathurin, T. Matsumoto, I. Mitsukawa, H. Miura, A. Miyake, Y. Miyake, H. Yurimoto, R. Okazaki, H. Yabuta, H. Naraoka, K. Sakamoto, S. Tachibana, H. C. Connolly, D. S. Lauretta, M. Yoshitake, M. Yoshikawa, K. Yoshikawa, K. Yoshihara, Y. Yokota, K. Yogata, H. Yano, Y. Yamamoto, D. Yamamoto, M. Yamada, T. Yamada, T. Yada, K. Wada, T. Usui, R. Tsukizaki, F. Terui, H. Takeuchi, Y. Takei, A. Iwamae, H. Soejima, K. Shirai, Y. Shimaki, H. Senshu, H. Sawada, T. Saiki, M. Ozaki, G. Ono, T. Okada, N. Ogawa, K. Ogawa, R. Noguchi, H. Noda, M. Nishimura, N. Namiki, S. Nakazawa, T. Morota, A. Miyazaki, A. Miura, Y. Mimasu, K. Matsumoto, K. Kumagai, T. Kouyama, S. Kikuchi, K. Kawahara, S. Kameda, T. Iwata, Y. Ishihara, M. Ishiguro, H. Ikeda, S. Hosoda, R. Honda, C. Honda, Y. Hitomi, N. Hirata, T. Hayashi, M. Hayakawa, K. Hatakeda, S. Furuya, R. Fukai, A. Fujii, Y. Cho, M. Arakawa, M. Abe, Y. Tsuda, Tohoku University [Sendai], NASA Johnson Space Center (JSC), NASA, The University of Tokyo (UTokyo), Tokyo Institute of Technology [Tokyo] (TITECH), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Planetary Exploration Research Center [Chiba] (PERC), Chiba Institute of Technology (CIT), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Nagoya University, Department of Earth and Planetary Science [Tokyo], Graduate School of Science [Tokyo], The University of Tokyo (UTokyo)-The University of Tokyo (UTokyo), Pôle Planétologie du LESIA, 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)-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), Guangzhou Institute of Geochemistry, Ritsumeikan University, Japan Synchrotron Radiation Research Institute [Hyogo] (JASRI), Institute of Low Temperature Science [Sapporo], Hokkaido University [Sapporo, Japan], Department of Earth, Environmental and Planetary Sciences [Providence], Brown University, The University of Aizu, University of Washington [Seattle], Osaka University, Kavli Institute for the Physics and Mathematics of the Universe [Tokyo] (Kavli IPMU), The University of Tokyo Institutes for Advanced Study (UTIAS), Japan Atomic Energy Agency, Goethe-University Frankfurt am Main, Department of Inorganic and Physical Chemistry, Ghent University, Universiteit Gent = Ghent University (UGENT), 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), Department of Earth Sciences, Royal Holloway, University of London, Egham, 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 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, Advanced Photon Source [ANL] (APS), Argonne National Laboratory [Lemont] (ANL)-University of Chicago-US Department of Energy, Kindai University, Kyushu University, Department of Earth and Atmospheric Sciences [Houston], University of Houston, Texas Materials Institute (TMI), University of Texas at Austin [Austin], Department of Geoscience, Virginia Tech, Blacksburg, VA, United States, National Institute for Materials Science (NIMS), Department of Earth Sciences [NHM London] (DES-NHM), The Natural History Museum [London] (NHM), Kanazawa University (KU), Graduate University for Advanced Studies [Hayama] (SOKENDAI), Division of Earth and Planetary Sciences [Kyoto], Kyoto University, Planetary Science Institute [Tucson] (PSI), Pennsylvania State University (Penn State), Penn State System, California State University [San Marcos] (CSUSM), Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), University of Shizuoka, Ehime University [Matsuyama, Japon], European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), KEK (High energy accelerator research organization), Hitachi, Ltd, Institute for integrated Radiation and Nuclear Science (KURNS), National Metrology Institute of Japan, National Institute of Advanced Industrial Science and Technology (AIST), Department of Physics, Rikkyo University, Tokyo, Japan Fine Ceramics Center (JFCC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), The Aerospace Corporation, Earth-Life Science Institute [Tokyo] (ELSI), University of Chinese Academy of Sciences [Beijing] (UCAS), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Photone Sciences, Deutsches Elektronen-Synchrotron (DESY), Graduate School of Life Science, University of Hyogo, International Christian University, Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Center for Advanced Radiation Sources [University of Chicago] (CARS), University of Chicago, Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Institut de Chimie Physique (ICP), Institut de Chimie du CNRS (INC)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Graduate School of Information Science [Nagoya], Department of Natural History Sciences, Department of Earth and Planetary Sciences [Fukuoka], Graduate School of Advanced Science and Engineering [Higashi-Hiroshima], Hiroshima University, Rowan University, Lunar and Planetary Laboratory [University of Arizona] (LPL), University of Arizona, Kanagawa Institute of Technology, Marine Works Japan Ltd., Faculty of Science, Niigata University, National Astronomical Observatory of Japan (NAOJ), Department of Physics and Astronomy [Seoul], Seoul National University [Seoul] (SNU), Kochi University, Department of Planetology, Graduate School of Science, Graduate School of Science [Kobe], Kobe University-Kobe University, Kobe University, Supported by KAKENHI from the Japanese Society for Promotion of Science (JSPS), grants JP20H00188 and 19H05183 to T.N., JP19K14776 to M.M., 21K18645 to T.M. and K.S., JP20H00205 to A.Ts., M.M., A.M. and J.M., 17H06458 to K.F., Y.T., S.Y. and M.K., JP17H06459 to T.N., T.U., S.W., M.M., N.N., T.M., T.O., Y.S., N.S., and R.N., JP15H05695 to A.Ts. and K.U., 20H05846 to S.T., JP17H06457 to H.G., JP17H06458 to Y. T. and K. F., JP19H00726 to K.K., H. G., and T.M., JP21J13337 to K.A., and JP18H05456,JP20H00189 to K.S., 18H05463 to T.T., S.N., and S.W., 18H05460 to K.N. and T.O., 18H05464 to Y.M., 18H05457 to K.N., T.T., S.W., and Y.M., and JP18H05479 to M.U. Also supported by the JSPS Core-to-Core program ' International Network of Planetary Sciences', and from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) (grants JPMXS0450200421 and JPMXS0450200521) to SS. A.K. acknowledges funding support from UK Research and Innovation (UKRI) grant MR/T020261/1. A.B. acknowledges funding support from NASA Emerging Worlds grant - 80NSSC18K0731. P.B. acknowledges funding from the European Research Council (ERC) under grant agreement no. 771691 (Solarys) and the CNES., and European Project: 771691,SOLARYS
Subjects: Multidisciplinary, [SDU]Sciences of the Universe [physics], Ryugu Hayabusa2 Carbonaceous asteroid Sample return
Abstract: Samples of the carbonaceous asteroid Ryugu were brought to Earth by the Hayabusa2 spacecraft. We analyzed 17 Ryugu samples measuring 1 to 8 millimeters. Carbon dioxide–bearing water inclusions are present within a pyrrhotite crystal, indicating that Ryugu’s parent asteroid formed in the outer Solar System. The samples contain low abundances of materials that formed at high temperatures, such as chondrules and calcium- and aluminum-rich inclusions. The samples are rich in phyllosilicates and carbonates, which formed through aqueous alteration reactions at low temperature, high pH, and water/rock ratios of
Published: 2022
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32. Investigation of the stratigraphic and chemical relationships between Bradbury and Siccar Point lithostratigraphic groups in Gale crater, Mars

Author: Laetitia Le Deit, Gwénaël Caravaca, Nicolas Mangold, Stéphane Le Mouélic, Erwin Dehouck, Candice C. Bedford, Roger C. Wiens, Jeffrey R. Johnson, Olivier Gasnault, Olivier Forni, Nina Lanza, Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), 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), Lunar and Planetary Institute [Houston] (LPI), NASA Johnson Space Center (JSC), NASA, Los Alamos National Laboratory (LANL), Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), and Europlanet
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences
Abstract: Over the past 10 years, the Mars Science Laboratory (MSL) rover Curiosity has been investigating the plains of Aeolis Palus and the lower reaches of Aeolis Mons (informally known as Mount Sharp), a 5 km tall mound of sedimentary rocks in Gale crater (Figure 1). After traversing 27 km and nearly 600 m of vertical stratigraphy, three lithostratigraphic groups have been identified: Bradbury, Mount Sharp, and Siccar Point (SP). The Bradbury group consists of fluvial, deltaic, and lacustrine sedimentary rocks [1-2]. The Mt. Sharp group mainly consists of laminated mudstones with minor fluvial sandstones, interpreted as evidence of a long-lived lacustrine environment [1]. Locally, exposures of the Mt. Sharp group are unconformably overlain by aeolian cross-bedded sandstones of the SP group, interpreted to have deposited on an aeolian deflation surface [3]. While these three groups show evidence of deposition in specific environmental and climatic conditions, knowledge of their stratigraphic relationships is a key information to understand the evolution of environmental conditions in Gale. Yet, no clear stratigraphic contact has been observed at the boundary between the Bradbury and the Mt. Sharp groups. Because the mean dip of the Bradbury group is approximately horizontal, the MSL team suggested that the Bradbury group might be stratigraphically lower than the Mt. Sharp group, and therefore lower than the SP group [1]. Nonetheless, orbital analyses of the region suggested that capping strata of the Bradbury group could be part of the SP group [4]. Chemical data from the ChemCam and APXS instrument suites of Bradbury and SP group rocks have recently shown that both groups have similar compositions and possibly similar sediment sources [5-8]. In this study, we aim to reappraise the stratigraphic and chemical relationships between the Bradbury and SP groups using Mastcam [9-10] and ChemCam data [11-12] to characterize the evolution of Gale’s ancient environment. Lithostratigraphy of Zabriskie Plateau One of the best candidates to assess the potential contact between Bradbury and SP group rocks is located at the Zabriskie Plateau outcrop in the Pahrump Hills area (Figure 1). To better appreciate the facies and 3D geometry of the contacts, this outcrop has been reconstructed as a Digital Outcrop Model (Figure 2, https://skfb.ly/o9ZAq) [13]. In this model, we observe that most of the outcrop is composed of fine to medium-grained sandstones, arranged in dm- to meter-scale cross-stratifications, similar to some of the aeolian facies of the SP group [3]. These sandstones exist as “capping rocks” similar to previously described examples [4], suggesting that they are locally well-cemented on the topmost meter. Near the base of the DOM, we observe a meter-scale, ~30-cm thick, cross-stratified lens-shaped interval of coarser medium to pebble conglomerate. This level represents deposition under energetic aqueous conditions to transport clasts up to the pebble size, more likely to pertain to a fluvial channel. Interestingly, this conglomerate interval is at similar elevation (within one meter) to the surrounding sandstones, with no apparent unconformity, likely evidencing a conformable emplacement of this level within the finer sandstone succession. This would argue that the conglomerate level was deposited synchronously with the finer-grained sandstones during the same depositional event. Chemical composition of Bradbury and Siccar Point groups The average compositions of Bradbury and SP group rocks are overall quite similar (Table 1), and clearly distinct from Mount Sharp group rocks (Figures 3 and 4). By analyzing the rock compositions of Bradbury and SP groups, we sorted them into five major chemical groups, which are, in order of increasing average K2O/Na2O ratio and average K2O content for groups 1 to 4: group 1 has a basaltic composition; group 2 has low SiO2, intermediate TiO2, high FeOT and Na2O contents; group 3 has low CaO, high TiO2, FeOT, and K2O contents; group 4 has low TiO2 and Al2O3, and very high K2O contents; and group 5 has a composition close to group 1 with higher SiO2 and alkali contents (Table 1, Figure 3). Overall, the MgO and Al2O3 contents are quite variable. The composition of these rocks suggests mixing between mafic minerals and feldspars, including alkali feldspars in various proportions (Figure 4). Interestingly, both Bradbury and SP rocks occur in the first three chemical groups, which suggests similar source rocks for both groups of at least two types: a relatively low-potassium basaltic rock and a potassic-rich rock. The relative abundance of potassic-rich source rock in the mixture is interpreted to increase from group 1 to group 4. Besides, Bradbury and SP group rocks have a low Chemical Index of Alteration (CIA), which is indicative of limited chemical weathering (Figure 4). Conclusion 3D observations in the Pahrump Hills area suggest that Bradbury and Siccar Point units are intermingled and synchronous in an environment allowing fluvial episodes to occasionally occur among a drier setting, as observed on Earth [14]. This is consistent with the chemical compositions of Bradbury and Siccar Point groups which suggest similar source rocks in different relative abundances. This relationship implies that the Bradbury group could be younger than Mount Sharp group (Figure 5). To summarize, these observations are in favor of a common origin for both Bradbury and Siccar Point as a single clastic group, representing a temporal evolution from clement conditions during the deposition of Mount Sharp group to a colder and drier environment with still transient episodes of fluvial activity during the deposition of Bradbury and Siccar Point groups. [1] Grotzinger et al., Science 2015. [2] Mangold et al., JGR 2016. [3] Banham et al., Sedimentology 2018. [4] Williams et al., Icarus 2018. [5] Bedford et al., Icarus 2020. [6] Bedford et al., JGR 2022. [7] Thompson et al., LPSC 2022. [8] Thompson et al., this conference. [9] Malin et al., LPSC 2010. [10] Bell et al., Earth and Space Science 2017. [11] Wiens et al., Space Sci Rev. 2012. [12] Maurice et al., Space Sci. Rev. 2012. [13] Caravaca et al., PSS 2020. [14] Newell, Marine and Petroleum Geology 2001.
Published: 2022
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33. Sedimentary and stratigraphic observations at the Jezero western delta front using Perseverance cameras: initial constraints on palaeoenvironments

Author: Gupta, Sanjeev, Bell, Jim F., Kanine, Oak, Tate, Christian, Caravaca, Gwénaël, Núñez, Jorge, Mangold, Nicolas, Dromart, Gilles, Le Mouélic, Stéphane, Annex, Andrew, Paar, Gerhard, Holm-Alwmark, Sanna, Rice, Melissa S., Rice, Jim, Horgan, Briony, Grotzinger, John, Maki, Justin, Hickman Lewis, Keyron, Kah, Lindah, Shuster, David L., Simon, Justin I., Gasnault, Olivier, Wiens, Roger, Maurice, Sylvestre, Stack, Kathryn, Farley, Kenneth A., Department of Earth Science and Engineering [Imperial College London], Imperial College London, Arizona State University [Tempe] (ASU), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), 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), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), 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), Joanneum Research, Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), The University of Tennessee [Knoxville], Berkeley Geochronology Center (BGC), Center for Isotope Cosmochemistry and Geochronology, NASA Johnson Space, and Europlanet
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences
Abstract: International audience; NASA’s Mars 2020 Perseverance rover mission is seeking signs of ancient life in Jezero crater and is collecting a cache of Martian rock and soil samples for planned return to Earth by a future mission. A key exploration target for the mission is a prominent sedimentary fan deposit at the western margin of Jezero crater that has been interpretated to be a river delta that built into an ancient lake basin during the Late Noachian-Early Hesperian epochs on Mars (~3.6-3.8 Ga) [1, 2]. Long distance observations of a remnant butte (informally named Kodiak) related to the western fan demonstrated that it comprised two distinct Gilbert-type delta units [2, 3].In her approach to the western fan, Perseverance drove alongside the east-facing scarp of the western fan and arrived at a key location called Three Forks - a setting off point for delta exploration - in April 2022. Images from the Mastcam-Z and SuperCam Remote Micro-Imager instrumentsprovide new views of the stratigraphy exposed in the erosional front of the western Jezero delta; in particular, showing sections of the delta previously not visible from long distance observations and at much higher resolution. These observations provide the first direct evidence of delta geometries in the main western fan deposit. Here, we report its stratigraphy and sedimentology, which providenew constraints on the nature of the fan deposits, and therefore paleoenvironmental implications.
Published: 2022
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34. Antioxidant Supplementation Does Not Affect Bone Turnover Markers During 60 Days of 6° Head-Down Tilt Bed Rest: Results from an Exploratory Randomized Controlled Trial

Author: Natalie Baecker, Jean-Pol Frippiat, Katharina Austermann, Peter Stehle, Scott M. Smith, Rolf Fimmers, Martina Heer, Sara R. Zwart, Rheinische Friedrich-Wilhelms-Universität Bonn, The University of Texas Medical Branch (UTMB), Stress, Immunité, Pathogènes (SIMPA), Université de Lorraine (UL), NASA Johnson Space Center (JSC), and NASA
Subjects: Adult, Male, 0301 basic medicine, medicine.medical_specialty, [SDV]Life Sciences [q-bio], medicine.medical_treatment, Medicine (miscellaneous), Parathyroid hormone, 030209 endocrinology & metabolism, Antioxidants, Collagen Type I, Bone resorption, Bone remodeling, Head-Down Tilt, Selenium, Young Adult, 03 medical and health sciences, 0302 clinical medicine, Internal medicine, Fatty Acids, Omega-3, medicine, Humans, Vitamin E, Single-Blind Method, Bone Resorption, 2. Zero hunger, Calcium metabolism, 030109 nutrition & dietetics, Nutrition and Dietetics, biology, business.industry, Polyphenols, Urinary calcium, 3. Good health, Endocrinology, Dietary Supplements, Osteocalcin, biology.protein, Calcium, Bone Remodeling, business, Bed Rest, Biomarkers, Type I collagen
Abstract: International audience; Background Immobilization and related oxidative stress are associated with bone loss. Antioxidants like polyphenols, omega-3 fatty acids, vitamins, and micronutrients may mitigate these negative effects on bone metabolism through scavenging of free radicals. Objectives We hypothesized that antioxidant supplementation during 60 days of 6° head-down tilt bed rest (HDBR) would reduce bone resorption and increase bone formation compared to nonsupplemented controls. Methods This exploratory randomized, controlled, single-blind intervention study conducted in a parallel design included 20 healthy male volunteers (age, 34 ± 8 years; weight, 74 ± 6 kg). The study consisted of a 14-day adaptation phase [baseline data collection (BDC)], followed by 60 days of HDBR and a 14-day recovery period (R). In the antioxidant group, volunteers received an antioxidant cocktail (741 mg/d polyphenols, 2.1 g/d omega-3 fatty acids, 168 mg/d vitamin E, and 80 μg/d selenium) with their daily meals. In the control group, volunteers received no supplement. Based on their body weight, all volunteers received an individually tailored and strictly controlled diet, consistent with DRIs. We analyzed biomarkers of calcium homeostasis, bone formation, and bone resorption during BDC, HDBR, and R, as well as for 30 days after the end of HDBR. Data were analyzed by linear mixed models. Results The antioxidant supplement did not affect serum calcium, parathyroid hormone, urinary C-telopeptide of type I collagen (CTX), urinary N-telopeptide of type I collagen, serum β–C-telopeptide of type I collagen (β-CTX), bone alkaline phosphatase, aminoterminal propeptide of type I collagen, osteocalcin, or urinary calcium excretion. In both groups, typical bed rest–related changes were observed. Conclusions Supplementation of an antioxidant cocktail to a diet matching the DRIs did not affect bone resorption or formation during 60 days of HDBR in healthy young men. This trial was registered at clinicaltrials.gov as NCT03594799.
Published: 2021
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35. Possible thermal metamorphism on the C, G, B, and F asteroids detected from their reflectance spectra in comparison with carbonaceous chondrites

Author: Hiroi,Takahiro, Pieters,Carle M., Zolensky,Michael E., Lipschutz,Michael E., and SN3, NASA Johnson Space Center/Departmet of Geological Sciences, Brown University/SN2, NASA Johnson Space Center/Departmet of Chemistry, Purdue University
Abstract: Reflectance spectra (0.3-2.6μm) of the C, G, B, and F asteroids and carbonaceous chondrites are compared in detail. Mixing calculations of 13 carbonaceous chondrite powders including three unusual CI/CM meteorites are done to characterize reflectance spectra of the 23 C, G, B, and F asteroids. Similar calculations are done with Murchison (CM2) samples heated at 400-1000℃. Both of two sets of calculations show that the C, G, B, and F asteroids may contain a significant amount of thermally metamorphosed materials. Comparison of ultraviolet absorption strengths between 160 C, G, B, and F asteroids and 21 carbonaceous chondrite powders suggests that surface minerals of most of those asteroids are thermally metamorphosed at temperatures around 600-1000℃.
Published: 1994

36. A mineralogical study of the proposed paired eucrites Y-792769 and Y-793164 with reference to cratering events on their parent body

Author: Hiroshi, Takeda, Akira , Yamaguchi, L. E., Nyquist, D. D., Bogard, and Mineralogical Institute, Faculty of Science, University of Tokyo/Mineralogical Institute, Faculty of Science, University of Tokyo/Mail Code SN, NASA Johnson Space Center/Mail Code SN, NASA Johnson Space Center
Abstract: A comparison of the mineralogy of Yamato (Y-) 792769 and Y-793164 has been performed to confirm the proposed pairing of these two specimens and to correlate their common shock-sintered textures with the resetting of their isotopic ages. The matrices of the two meteorites share this common texture as described for Y-792769,but their clast types are different. Y-792769 contains pyroxene fragments with Mg-rich compositions, which are not present in the matrix. A large basaltic clast present in Y-793164 includes acicular plagioclase crystals replacing the pyroxene grains. Pyroxene clasts in the matrix of the two meteorites showed a small compositional range between 30 and 45 in Mg×100/(Mg+Fe) mol% and are similar to the more comminuted matrix pyroxenes, but lithic clast pyroxenes are uniform in bulk chemistry within a single clast type. The event which produced these monomict eucrites with minor compositional differences may have taken place earlier than the reset ^Ar-^Ar age of 3.99 Ga previously found for Y-792769. Some pyroxenes are more Fe-rich than those of common monomict eucrites such as Juvinas. The common pyroxene components and the shock-sintered textures support the proposed pairing of Y-792769 and Y-793164. Rb and Sr abundances and isotopic data do not strongly support the proposed pairing of the meteorites, but could be consistent with observed compositional heterogeneities within and between them. Sm and Nd abundances and isotopic data are similar for matrix samples of the meteorites and are consistent with their pairing.
Published: 1994

37. A comparison of the igneous máaz formation at jezero crater with martian meteorites

Author: Udry, A., Ostwald, A., Sautter, V., Cousin, A., Wiens, R. C., Forni, O., Benzerara, K., Beyssac, O., Nachon, M., Dromart, G., Quantin, C., Mandon, L., Clavé, E., Pinet, P., Ollila, A., Bosak, T., Mangold, N., Dehouck, E., Johnson, J., Schmidt, M., Horgan, B., Gabriel, T., Mclennan, S., Maurice, S., Simon, J.I., Herd, C. D. K., M.Madiaraga, J., Brown, A, Connell, S., Flannery, D., Tosca, N., Cohen, B., Liu, Y., Mccubbin, F. M., Cloutis, E., Fouchet, T., Royer, C., Alwmark, S., Sharma, S., Anderson, R., Pilleri, P, University of Nevada [Las Vegas] (WGU Nevada), 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), 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), Texas A&M University System, École normale supérieure de Lyon (ENS de Lyon), Massachusetts Institute of Technology (MIT), Johns Hopkins University (JHU), Brock University [Canada], Purdue University [West Lafayette], United States Geological Survey (USGS), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, University of Alberta, University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), NASA, University of Winnipeg, Queensland University of Technology [Brisbane] (QUT), University of Cambridge [UK] (CAM), California Institute of Technology (CALTECH), 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 Copenhagen = Københavns Universitet (UCPH), Hawaii Institute of Geophysics and Planetology (HIGP), and University of Hawai‘i [Mānoa] (UHM)
Subjects: jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], rover, mars mineralogy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, supercam, meteorites
Abstract: International audience
Published: 2022

38. Formation and destruction of clay minerals in Glen Torridon, Gale crater, Mars

Author: Dehouck, Erwin, Cousin, Agnès, Mangold, Nicolas, Frydenvang, Jens, Gasnault, Olivier, Forni, Olivier, Rapin, William, Gasda, Patrick, Caravaca, Gwénaël, David, Gaël, Bedford, Candice, Lasue, Jérémie, Meslin, Pierre-Yves, Rammelkamp, Kristin, Desjardin, Marine, Le Mouélic, Stéphane, Thorpe, Michael, Fox, Valerie, Bennett, Kristen, Bryk, Alexander, Lanza, Nina, Maurice, Sylvestre, Wiens, Roger, 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 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 Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), University of Copenhagen = Københavns Universitet (UCPH), Los Alamos National Laboratory (LANL), Lunar and Planetary Institute [Houston] (LPI), UniLaSalle, NASA Johnson Space Center (JSC), NASA, University of Minnesota [Twin Cities] (UMN), University of Minnesota System, Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences
Abstract: International audience; From 2019 to 2021, the Curiosity rover explored the Glen Torridon (GT) region, a topographic troughlocated on the slope of Aeolis Mons, the central mound of Gale crater. GT corresponds to what was previously referred toas the “clay-bearing unit”, due to the detection of smectite signatures by orbital spectro-imagers. One of the objectives ofthis campaign was to better understand the context of formation of the clay minerals, as well as the overall alterationhistory of GT.Here, we used the ChemCam instrument to survey the major-element composition of the bedrock throughout the region.Overall, the GT bedrock is characterized by elevated values of the Chemical Index of Alteration (CIA), which indicatesthat the clay minerals were formed in a context of open-system weathering, i.e., through the interaction of the sediments(or their source rocks) with dilute meteoric fluids at relatively high water-to-rock ratio. We also observed geochemicalvariations correlated with outcrop expression – for example, in the northern part of GT, the spatially dominant type ofbedrock has a distinctive “rubbly” appearance and displays enrichments in both K2O and SiO2, which are best explainedby the presence of illite or a mixed-layer illite/smectite phase.Finally, in the southern part GT, in an area of lighter-toned rocks named the Hutton interval, we found significantly lowerCIA values that are correlated with reduced abundances of clay minerals. We interpret these “anomalous” compositionsas a local diagenetic overprint, and propose that the clay minerals of the Hutton interval have been partially destroyed bythe circulation of concentrated fluids late in the history of Gale.
Published: 2022

39. The Curiosity Rover’s Exploration of Glen Torridon, Gale crater, Mars: An Overview of the Campaign and Scientific Results

Author: Kristen A. Bennett, Valerie K. Fox, Alex Bryk, William Dietrich, Christopher Fedo, Lauren Edgar, Michael T. Thorpe, Amy J. Williams, Gregory M. Wong, Erwin Dehouck, Amy McAdam, Brad Sutter, Maëva Millan, Steven G. Banham, Candice C. Bedford, Thomas Bristow, Abigail Fraeman, Ashwin R. Vasavada, John Grotzinger, Lucy Thompson, Catherine O’Connell‐Cooper, Patrick Gasda, Amanda Rudolph, Robert Sullivan, Ray Arvidson, Agnes Cousin, Briony Horgan, Kathryn M. Stack, Allan Treiman, Jennifer Eigenbrode, Gwénaël Caravaca, Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Department of Earth Sciences [Minneapolis], University of Minnesota [Twin Cities] (UMN), University of Minnesota System-University of Minnesota System, Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Department of Earth and Planetary Sciences [UC Berkeley, USA], University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], Texas State University, NASA Johnson Space Center (JSC), NASA, Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), Department of Geosciences [Pennsylvania], Pennsylvania State University (Penn State), Penn State System-Penn State System, 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), NASA Goddard Space Flight Center (GSFC), Jacobs Technology ESCG, Georgetown University [Washington] (GU), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Lunar and Planetary Institute [Houston] (LPI), NASA Ames Research Center (ARC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Planetary and Space Science Centre (PASSC), University of New Brunswick (UNB), Los Alamos National Laboratory (LANL), Department of Earth, Atmospheric, and Planetary Sciences, Purdue University, Cornell Center for Astrophysics and Planetary Science (CCAPS), Cornell University [New York], Department of Earth and Planetary Sciences [St Louis], Washington University in Saint Louis (WUSTL), 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), Department of Earth and Planetary Science [UC Berkeley] (EPS), Department of Geosciences [PennState], College of Earth and Mineral Sciences, Penn State System-Penn State System-Pennsylvania State University (Penn State), 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), Department of Earth, Atmospheric, and Planetary Sciences [West Lafayette] (EAPS), and Purdue University [West Lafayette]
Subjects: Geophysics, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Space and Planetary Science, Geochemistry and Petrology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Earth and Planetary Sciences (miscellaneous), [SDU.STU]Sciences of the Universe [physics]/Earth Sciences
Abstract: International audience; The Mars Science Laboratory rover, Curiosity, explored the clay mineral-bearing Glen Torridon region for one martian year between January 2019 and January 2021, including a short campaign onto the Greenheugh pediment. The Glen Torridon campaign sought to characterize the geologyof the area, seek evidence of habitable environments, and document the onset of a potentially global climatic transition during the Hesperian era. Curiosity roved 5 km in total throughout Glen Torridon, from the Vera Rubin ridge to the northern margin of the Greenheugh pediment. Curiosityacquired samples from 11 drill holes during this campaign and conducted the first martian thermochemolytic-based organics detection experiment with the Sample Analysis at Mars instrument suite. The lowest elevations within Glen Torridon represent a continuation of lacustrine Murray formation deposits, but overlying widespread cross bedded sandstones indicate an interval of more energetic fluvial environments and prompted the definition of a new stratigraphic formation in the Mount Sharp group called the Carolyn Shoemaker formation. Glen Torridon hostsabundant phyllosilicates yet remains compositionally and mineralogically comparable to the rest of the Mount Sharp group. Glen Torridon samples have a great diversity and abundance of sulfurbearing organic molecules, which are consistent with the presence of ancient refractory organicmatter. The Glen Torridon region experienced heterogeneous diagenesis, with the most striking alteration occurring just below the Siccar Point unconformity at the Greenheugh pediment. Results from the pediment campaign show that the capping sandstone formed within the StimsonHesperian aeolian sand sea that experienced seasonal variations in wind direction.
Published: 2022
Full Text: View/download PDF

40. Time-Sensitive Aspects of Mars Sample Return (MSR) Science

Author: Tosca, N. J., Agee, Carl, Cockell, C., Glavin, D P, Hutzler, Aurore, Marty, B., McCubbin, F. M., Regberg, Aaron, Velbel, Michael, Kminek, G., Meyer, M., Beaty, D.W., Carrier, B. L., Haltigin, T., Hays, Lindsay, Busemann, H., Cavalazzi, Barbara, Debaille, V, Grady, M., Hauber, Ernst, Pratt, Lisa, Smith, Alvin, Smith, C., Summons, R E, Swindle, T. D., Tait, Kimberly, Udry, Arya, Usui, Tomohiro, Wadhwa, M., Westall, F., Zorzano, M.-P., Tosca N. J., Beaty D. W., Carrier B. L., Agee C. B., Cockell C. S., Glavin D. P., Hutzler A., Marty B., McCubbin F. M., Regberg A. B., Velbel M. A., Kminek G., Meyer M. A., Haltigin T., Busemann H., Cavalazzi B., Debaille V., Grady M. M., Hauber E., Hays L. E., Pratt L. M., Smith A. L., Smith C. L., Summons R. E., Swindle T. D., Tait K. T., Udry A., Usui T., Wadhwa M., Westall F., Zorzano M. -P., University of Cambridge [UK] (CAM), The University of New Mexico [Albuquerque], University of Edinburgh, NASA Goddard Space Flight Center (GSFC), European Space Agency (ESA), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), NASA Johnson Space Center (JSC), NASA, Michigan State University [East Lansing], Michigan State University System, Smithsonian Institution, NASA Headquarters, California Institute of Technology (CALTECH), Canadian Space Agency (CSA), Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Bologna, Université libre de Bruxelles (ULB), The Open University [Milton Keynes] (OU), German Aerospace Center (DLR), Indiana University [Bloomington], Indiana University System, The Natural History Museum [London] (NHM), University of Glasgow, Massachusetts Institute of Technology (MIT), University of Arizona, Royal Ontario Museum, University of Nevada [Las Vegas] (WGU Nevada), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Arizona State University [Tempe] (ASU), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Aberdeen, Tosca, Nicholas [0000-0003-4415-4231], and Apollo - University of Cambridge Repository
Subjects: Minerals, geology, Extraterrestrial Environment, laboratory experiments, Sulfates, [SDV]Life Sciences [q-bio], astrobiology, Mars, Space Flight, Mars Sample Return (MSR) Science, sample return, Agricultural and Biological Sciences (miscellaneous), Space and Planetary Science, Exobiology, Clay, Gases
Abstract: Samples returned from Mars would be placed under quarantine at a Sample Receiving Facility (SRF) until they are considered safe to release to other laboratories for further study. The process of determining whether samples are safe for release, which may involve detailed analysis and/or sterilization, is expected to take several months. However, the process of breaking the sample tube seal and extracting the headspace gas will perturb local equilibrium conditions between gas and rock and set in motion irreversible processes that proceed as a function of time. Unless these time-sensitive processes are understood, planned for, and/or monitored during the quarantine period, scientific information expected from further analysis may be lost forever. At least four processes underpin the time-sensitivity of Mars returned sample science: (1) degradation of organic material of potential biological origin, (2) modification of sample headspace gas composition, (3) mineral-volatile exchange, and (4) oxidation/reduction of redox-sensitive materials. Available constraints on the timescales associated with these processes supports the conclusion that an SRF must have the capability to characterize attributes such as sample tube headspace gas composition, organic material of potential biological origin, as well as volatiles and their solid-phase hosts. Because most time-sensitive investigations are also sensitive to sterilization, these must be completed inside the SRF and on timescales of several months or less. To that end, we detail recommendations for how sample preparation and analysis could complete these investigations as efficiently as possible within an SRF. Finally, because constraints on characteristic timescales that define time-sensitivity for some processes are uncertain, future work should focus on: (1) quantifying the timescales of volatile exchange for core material physically and mineralogically similar to samples expected to be returned from Mars, and (2) identifying and developing stabilization or temporary storage strategies that mitigate volatile exchange until analysis can be completed. Executive Summary Any samples returned from Mars would be placed under quarantine at a Sample Receiving Facility (SRF) until it can be determined that they are safe to release to other laboratories for further study. The process of determining whether samples are safe for release, which may involve detailed analysis and/or sterilization, is expected to take several months. However, the process of breaking the sample tube seal and extracting the headspace gas would perturb local equilibrium conditions between gas and rock and set in motion irreversible processes that proceed as a function of time. Unless these processes are understood, planned for, and/or monitored during the quarantine period, scientific information expected from further analysis may be lost forever. Specialist members of the Mars Sample Return Planning Group Phase 2 (MSPG-2), referred to here as the Time-Sensitive Focus Group, have identified four processes that underpin the time-sensitivity of Mars returned sample science: (1) degradation of organic material of potential biological origin, (2) modification of sample headspace gas composition, (3) mineral-volatile exchange, and (4) oxidation/reduction of redox-sensitive materials (Figure 2). Consideration of the timescales and the degree to which these processes jeopardize scientific investigations of returned samples supports the conclusion that an SRF must have the capability to characterize: (1) sample tube headspace gas composition, (2) organic material of potential biological origin, (3) volatiles bound to or within minerals, and (4) minerals or other solids that host volatiles (Table 4). Most of the investigations classified as time-sensitive in this report are also sensitive to sterilization by either heat treatment and/or gamma irradiation (Velbel et al., 2022). Therefore, these investigations must be completed inside biocontainment and on timescales that minimize the irrecoverable loss of scientific information (i.e., several months or less; Section 5). To that end, the Time-Sensitive Focus Group has outlined a number of specific recommendations for sample preparation and instrumentation in order to complete these investigations as efficiently as possible within an SRF (Table 5). Constraints on the characteristic timescales that define time-sensitivity for different processes can range from relatively coarse to uncertain (Section 4). Thus, future work should focus on: (1) quantifying the timescales of volatile exchange for variably lithified core material physically and mineralogically similar to samples expected to be returned from Mars, and (2) identifying and developing stabilization strategies or temporary storage strategies that mitigate volatile exchange until analysis can be completed. List of Findings FINDING T-1: Aqueous phases, and oxidants liberated by exposure of the sample to aqueous phases, mediate and accelerate the degradation of critically important but sensitive organic compounds such as DNA. FINDING T-2: Warming samples increases reaction rates and destroys compounds making biological studies much more time-sensitive. MAJOR FINDING T-3: Given the potential for rapid degradation of biomolecules, (especially in the presence of aqueous phases and/or reactive O-containing compounds) Sample Safety Assessment Protocol (SSAP) and parallel biological analysis are time sensitive and must be carried out as soon as possible. FINDING T-4: If molecules or whole cells from either extant or extinct organisms have persisted under present-day martian conditions in the samples, then it follows that preserving sample aliquots under those same conditions (i.e., 6 mbar total pressure in a dominantly CO2 atmosphere and at an average temperature of -80°C) in a small isolation chamber is likely to allow for their continued persistence. FINDING T-5: Volatile compounds (e.g., HCN and formaldehyde) have been lost from Solar System materials stored under standard curation conditions. FINDING T-6: Reactive O-containing species have been identified in situ at the martian surface and so may be present in rock or regolith samples returned from Mars. These species rapidly degrade organic molecules and react more rapidly as temperature and humidity increase. FINDING T-7: Because the sample tubes would not be closed with perfect seals and because, after arrival on Earth, there will be a large pressure gradient across that seal such that the probability of contamination of the tube interiors by terrestrial gases increases with time, the as-received sample tubes are considered a poor choice for long-term gas sample storage. This is an important element of time sensitivity. MAJOR FINDING T-8: To determine how volatiles may have been exchanged with headspace gas during transit to Earth, the composition of martian atmosphere (in a separately sealed reservoir and/or extracted from the witness tubes), sample headspace gas composition, temperature/time history of the samples, and mineral composition (including mineral-bound volatiles) must all be quantified. When the sample tube seal is breached, mineral-bound volatile loss to the curation atmosphere jeopardizes robust determination of volatile exchange history between mineral and headspace. FINDING T-9: Previous experiments with mineral powders show that sulfate minerals are susceptible to H2O loss over timescales of hours to days. In addition to volatile loss, these processes are accompanied by mineralogical transformation. Thus, investigations targeting these minerals should be considered time-sensitive. FINDING T-10: Sulfate minerals may be stabilized by storage under fixed relative-humidity conditions, but only if the identity of the sulfate phase(s) is known a priori. In addition, other methods such as freezing may also stabilize these minerals against volatile loss. FINDING T-11: Hydrous perchlorate salts are likely to undergo phase transitions and volatile exchange with ambient surroundings in hours to days under temperature and relative humidity ranges typical of laboratory environments. However, the exact timescale over which these processes occur is likely a function of grain size, lithification, and/or cementation. FINDING T-12: Nanocrystalline or X-ray amorphous materials are typically stabilized by high proportions of surface adsorbed H2O. Because this surface adsorbed H2O is weakly bound compared to bulk materials, nanocrystalline materials are likely to undergo irreversible ripening reactions in response to volatile loss, which in turn results in decreases in specific surface area and increases in crystallinity. These reactions are expected to occur over the timescale of weeks to months under curation conditions. Therefore, the crystallinity and specific surface area of nanocrystalline materials should be characterized and monitored within a few months of opening the sample tubes. These are considered time-sensitive measurements that must be made as soon as possible. FINDING T-13: Volcanic and impact glasses, as well as opal-CT, are metastable in air and susceptible to alteration and volatile exchange with other solid phases and ambient headspace. However, available constraints indicate that these reactions are expected to proceed slowly under typical laboratory conditions (i.e., several years) and so analyses targeting these materials are not considered time sensitive. FINDING T-14: Surface adsorbed and interlayer-bound H2O in clay minerals is susceptible to exchange with ambient surroundings at timescales of hours to days, although the timescale may be modified depending on the degree of lithification or cementation. Even though structural properties of clay minerals remain unaffected during this process (with the exception of the interlayer spacing), investigations targeting H2O or other volatiles bound on or within clay minerals should be considered time sensitive upon opening the sample tube. FINDING T-15: Hydrated Mg-carbonates are susceptible to volatile loss and recrystallization and transformation over timespans of months or longer, though this timescale may be modified by the degree of lithification and cementation. Investigations targeting hydrated carbonate minerals (either the volatiles they host or their bulk mineralogical properties) should be considered time sensitive upon opening the sample tube. MAJOR FINDING T-16: Current understanding of mineral-volatile exchange rates and processes is largely derived from monomineralic experiments and systems with high surface area; lithified sedimentary rocks (accounting for some, but not all, of the samples in the cache) will behave differently in this regard and are likely to be associated with longer time constants controlled in part by grain boundary diffusion. Although insufficient information is available to quantify this at the present time, the timescale of mineral-volatile exchange in lithified samples is likely to overlap with the sample processing and curation workflow (i.e., 1-10 months; Table 4). This underscores the need to prioritize measurements targeting mineral-hosted volatiles within biocontainment. FINDING T-17: The liberation of reactive O-species through sample treatment or processing involving H2O (e.g., rinsing, solvent extraction, particle size separation in aqueous solution, or other chemical extraction or preparation protocols) is likely to result in oxidation of some component of redox-sensitive materials in a matter of hours. The presence of reactive O-species should be examined before sample processing steps that seek to preserve or target redox-sensitive minerals. Electron paramagnetic resonance spectroscopy (EPR) is one example of an effective analytical method capable of detecting and characterizing the presence of reactive O-species. FINDING T-18: Environments that maintain anoxia under inert gas containing <
Published: 2022
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41. Final report of the MSR Science Planning Group 2 (MSPG2)

Author: Meyer, Michael A, Kminek, Gerhard, Beaty, David W, Carrier, Brandi Lee, Haltigin, Timothy, Hays, Lindsay E, Agee, Carl B., Busemann, Henner, Cavalazzi, Barbara, Cockell, Charles S., Debaille, Vinciane, Glavin, Daniel P., Grady, Monica M., Hauber, Ernst, Hutzler, Aurore, Marty, Bernard, McCubbin, Francis M., Pratt, Lisa M, Regberg, Aaron B., Smith, Alvin L, Smith, Caroline L, Summons, Roger E., Swindle, Timothy D, Tait, Kimberly T, Tosca, Nicholas J., Udry, Arya, Usui, Tomohiro, Velbel, Michael A., Wadhwa, Meenakshi, Westall, Frances, Zorzano, Maria-Paz, NASA Headquarters, European Space Agency (ESA), California Institute of Technology (CALTECH), Canadian Space Agency (CSA), The University of New Mexico [Albuquerque], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), University of Bologna, University of Edinburgh, Université libre de Bruxelles (ULB), NASA Goddard Space Flight Center (GSFC), The Open University [Milton Keynes] (OU), German Aerospace Center (DLR), Centre de Recherches Pétrographiques et Géochimiques (CRPG), Institut national des sciences de l'Univers (INSU - CNRS)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, Indiana University [Bloomington], Indiana University System, NASA, The Natural History Museum [London] (NHM), University of Glasgow, Massachusetts Institute of Technology (MIT), University of Arizona, Royal Ontario Museum, University of Cambridge [UK] (CAM), University of Nevada [Las Vegas] (WGU Nevada), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Michigan State University [East Lansing], Michigan State University System, Smithsonian Institution, Arizona State University [Tempe] (ASU), Centre de biophysique moléculaire (CBM), Université d'Orléans (UO)-Institut National de la Santé et de la Recherche Médicale (INSERM)-Centre National de la Recherche Scientifique (CNRS)-Institut de Chimie du CNRS (INC), University of Aberdeen, Meyer M. A., Kminek G., Beaty D. W., Carrier B. L., Haltigin T., Hays L. E., Agee C. B., Busemann H., Cavalazzi B., Cockell C. S., Debaille V., Glavin D. P., Grady M. M., Hauber E., Hutzler A., Marty B., McCubbin F. M., Pratt L. M., Regberg A. B., Smith A. L., Smith C. L., Summons R. E., Swindle T. D., Tait K. T., Tosca N. J., Udry A., Usui T., Velbel M. A., Wadhwa M., Westall F., and Zorzano M. -P.
Subjects: [SDU]Sciences of the Universe [physics], Mars Sample Return (MSR) Campaign
Abstract: International audience; The Mars Sample Return (MSR) Campaign must meet a series of scientific and technical achievements to be successful. While the respective engineering responsibilities to retrieve the samples have been formalized through a Memorandum of Understanding between ESA and NASA, the roles and responsibilities of the scientific elements have yet to be fully defined. In April 2020, ESA and NASA jointly chartered the MSR Science Planning Group 2 (MSPG2) to build upon previous planning efforts in defining 1) an end-to-end MSR Science Program and 2) needed functionalities and design requirements for an MSR Sample Receiving Facility (SRF). The challenges for the first samples brought from another planet include not only maintaining and providing samples in pristine condition for study, but also maintaining biological containment until the samples meet sample safety criteria for distribution outside of biocontainment. The MSPG2 produced six reports outlining 66 findings. Abbreviated versions of the five additional high-level MSPG2 summary findings are: Summary-1. A long-term NASA/ESA MSR Science Program, along with the necessary funding and human resources, will be required to accomplish the end-to-end scientific objectives of MSR. Summary-2. MSR curation will need to be done concurrently with Biosafety Level-4 containment. This would lead to complex first-of-a-kind curation implementations and require further technology development. Summary-3. Most aspects of MSR sample science can, and should, be performed on samples deemed safe in laboratories outside of the SRF. However, other aspects of MSR sample science are both time-sensitive and sterilization-sensitive and would need to be carried out in the SRF. Summary-4. To meet the unique science, curation, and planetary protection needs of MSR, substantial analytical and sample management capabilities would be required in an SRF. Summary-5. Because of the long lead-time for SRF design, construction, and certification, it is important that preparations begin immediately, even if there is delay in the return of samples.
Published: 2022
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42. The polymict carbonaceous breccia Aguas Zarcas: A potential analog to samples being returned by the OSIRIS‐REx and Hayabusa2 missions

Author: Andreas Pack, Loan Le, Motoo Ito, Dennis Harries, M. Patzek, Romy D. Hanna, Yoko Kebukawa, Marc Fries, Zia Ur Rahman, Addi Bischoff, Michael E. Zolensky, I. Kerraouch, Bischoff, Addi, 1Institut für Planetologie University of Münster Wilhelm‐Klemm Str. 10 Münster D‐48149 Germany, Zolensky, Michael E., 2Astromaterials Research and Exploration Science NASA Johnson Space Center Houston Texas 77058 USA, Pack, Andreas, 4Universität Göttingen Geowissenschaftliches Zentrum Goldschmidtstr. 1 Göttingen D‐37077 Germany, Patzek, Markus, Hanna, Romy D., 5Jackson School of Geosciences University of Texas Austin Texas 78712 USA, Fries, Marc D., Harries, Dennis, 6Institut für Geowissenschaften Friedrich‐Schiller‐Universität Jena Carl‐Zeiss‐Promenade 10 Jena 07745 Germany, Kebukawa, Yoko, 7Faculty of Engineering Division of Materials Science and Chemical Engineering Yokohama National University 79‐1 Tokiwadai, Hodogaya Ward Yokohama Kanagawa 240‐8501 Japan, Le, Loan, 8Jacobs JETS Johnson Space Center 2101 NASA Parkway Houston Texas 77058 USA, Ito, Motoo, 9Japan Agency for Marine‐Earth Science Technology (JAMSTEC) Kochi Institute for Core Sample Research 200 Monobe Otsu Nankoku City Kochi 783‐8502 Japan, and Rahman, Zia
Subjects: 552.6, Costa Rica, biology, Geochemistry, 010502 geochemistry & geophysics, biology.organism_classification, 01 natural sciences, carbonaceous chondrite, Geophysics, 13. Climate action, Space and Planetary Science, Carbonaceous chondrite, 0103 physical sciences, Breccia, Osiris, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract: On April 23, 2019, a meteorite fall occurred in Aguas Zarcas, Costa Rica. According to the Meteoritical Bulletin, Aguas Zarcas is a brecciated CM2 chondrite dominated by two lithologies. Our X‐ray computed tomography (XCT) results show many different lithologies. In this paper, we describe the petrographic and mineralogical investigation of five different lithologies of the Aguas Zarcas meteorite. The bulk oxygen isotope compositions of some lithologies were also measured. The Aguas Zarcas meteorite is a breccia at all scales. From two small fragments, we have noted five main lithologies, including (1) Met‐1: a metal‐rich lithology; (2) Met‐2: a second metal‐rich lithology which is distinct from Met‐1; (3) a brecciated CM lithology with clasts of different petrologic subtypes; (4) a C1/2 lithology; and (5) a C1 lithology. The Met‐1 lithology is a new and unique carbonaceous chondrite which bears similarities to CR and CM chondrite groups, but is distinct from both based on oxygen isotope data. Met‐2 also represents a new type of carbonaceous chondrite, but it is more similar to the CM chondrite group, albeit with a very high abundance of metal. We have noted some similarities between the Met‐1 and Met‐2 lithologies and will explore possible genetic relationships. We have also identified a brecciated CM lithology with two primary components: a chondrule‐poor lithology and a chondrule‐rich lithology showing different petrologic subtypes. The other two lithologies, C1 and C1/2, are very altered and possibly related to the CM chondrite group. In this article, we describe all the lithologies in detail and attempt a classification of each in order to understand the origin and the history of formation of the Aguas Zarcas parent body., ProjektDEAL, Deutsche Forschungsgemeinschaft http://dx.doi.org/10.13039/501100001659, Japan Society for the Promotion of Science http://dx.doi.org/10.13039/501100001691
Published: 2021
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43. Dynamo action in dissipative, forced, rotating MHD turbulence

Author: Shebalin, John [Astromaterials Research Office, NASA Johnson Space Center, Houston, Texas 77058-3696 (United States)]
Published: 2016
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44. STELLAR ORIGINS OF EXTREMELY {sup 13}C- AND {sup 15}N-ENRICHED PRESOLAR SIC GRAINS: NOVAE OR SUPERNOVAE?

Author: Nguyen, Ann [Robert M. Walker Laboratory for Space Science, Astromaterials Research and Exploration Science Directorate, NASA Johnson Space Center, Houston, TX 77058 (United States)]
Published: 2016
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45. MINERALOGY OF PRESOLAR SILICATE AND OXIDE GRAINS OF DIVERSE STELLAR ORIGINS

Author: Messenger, Scott [Robert M. Walker Laboratory for Space Science, EISD Directorate, Astromaterials Research and Exploration Science, NASA Johnson Space Center, Houston, TX 77058 (United States)]
Published: 2016
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46. Composition and density stratification observed by supercam in the first 300 sols in Jezero crater

Author: Wiens, R.C., Udry, A., Mangold, N., Beyssac, O., Quantin, C., Sautter, V., Cousin, A., Brown, A., Bosak, T., Mandon, L., Forni, O., Johnson, J.R., Mclennan, S., Legett, C., Maurice, S., Mayhew, L., Crumpler, L., Anderson, R.B., Clegg, S.M., Ollila, A.M., Hall, J., Meslin, P.-Y., Kah, L.C., Gabriel, T.S.J., Gasda, P., Simon, J.I., Hausrath, E.M., Horgan, B., Poulet, F., Beck, P., Gupta, S., Chide, B., Clavé, E., Connell, S., Dehouck, E., Dromart, G., Fouchet, T., Royer, C., Frydenvang, J., Gasnault, Olivier, Gibbons, E., Kalucha, H., Lanza, N., Lasue, J., Mouelic, S. Le, Leveillé, R., Cloutis, E., Reyes, G. Lopez, Arana, G., Castro, K., Madariaga, J.M., Manrique, J.-A., Pilorget, C., Pinet, P., Laserna, J., Sharma, S.K., Acosta-Maeda, T., Kelly, E., Montmessin, Franck, Fischer, W., Francis, R., Stack, K., Farley, K., Los Alamos National Laboratory (LANL), Purdue University [West Lafayette], Plancius Research LLC, Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), 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 (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 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), Massachusetts Institute of Technology (MIT), 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), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), University of Colorado [Boulder], New Mexico Museum of Natural History and Science (NMMNHS), United States Geological Survey (USGS), The University of Tennessee [Knoxville], NASA Johnson Space Center (JSC), NASA, University of Nevada [Las Vegas] (WGU Nevada), 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), Université Grenoble Alpes (UGA), Imperial College London, Université de Bordeaux (UB), University of Winnipeg, Université de Lyon, Observatoire de Paris, Université Paris sciences et lettres (PSL), McGill University = Université McGill [Montréal, Canada], California Institute of Technology (CALTECH), Universidad de Valladolid [Valladolid] (UVa), University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Universidad de Málaga [Málaga] = University of Málaga [Málaga], University of Hawaii, 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), and pinet, patrick
Subjects: [SDU] Sciences of the Universe [physics], jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], perseverance in situ exploration, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], supercam, [SDU.STU.PL] Sciences of the Universe [physics]/Earth Sciences/Planetology, mars geology, mineralogy, petrology
Abstract: International audience
Published: 2022

47. A DELTA-LAKE SYSTEM AT JEZERO CRATER (MARS) FROM LONG DISTANCE OBSERVATIONS

Author: Sanjeev Gupta, Nicolas Mangold, Bell, Jim F., Olivier Gasnault, Tarnas, J. D., Sholes, S., Briony Horgan, Cathy Quantin-Nataf, Brown, A., Stéphane Le Mouélic, Roberta Yingst, Olivier Beyssac, Bosak, T., Fred Calef, Gwénaël CARAVACA, Ehlmann, B., Kenneth Farley, Grotzinger, John P., Hickman-Lewis, K., Holm-Alwmark, S., Kah, Linda C., Kanine, M., Martinez-Frias, J., Mclennan, Scott M., Sylvestre Maurice, Nuñez, J., Ollila, A. M., Gerhard Paar, Paolo Pilleri, Rice, J., Rice, M., Simon, J., Shuster, D., Katie Stack‐morgan, Vivian Sun, Treiman, Allan H., Weiss, B., Wiens, Roger C., Williams, A., Williams, N., Williford, Kenneth H., Department of Earth Science and Engineering [Imperial College London], Imperial College London, Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Arizona State University [Tempe] (ASU), 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Purdue University [West Lafayette], 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), Plancius Research LLC, Planetary Science Institute [Tucson] (PSI), 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), Massachusetts Institute of Technology (MIT), California Institute of Technology (CALTECH), The Natural History Museum [London] (NHM), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Lund University [Lund], Natural History Museum of Denmark, The University of Tennessee [Knoxville], Instituto de Geociencias [Madrid] (IGEO), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), JHUAPL, Los Alamos National Laboratory (LANL), Joanneum Research, College of Engineering and Science [Louisiana], Louisiana Tech University, Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), Lunar and Planetary Institute [Houston] (LPI), Department of Geological Sciences [Gainesville] (UF|Geological), University of Florida [Gainesville] (UF), and Lunar and Planetary Institute
Subjects: Jezero crater, delta, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Mars 2020, Mars, sedimentolgoy, stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences
Abstract: International audience; Orbital and rover observations of relictgeomorphic features and stratigraphic architectures indicate Mars once had a warmer, wetter climate. Constraining the character, relative timing and persistence of ancient aqueous activity on Mars is possible through detailed interrogation of the stratal geometry of aqueously deposited sedimentary bodies. Such analyses inform interpretations of Martian climate evolution, potential habitability, and search strategies for rocks that might contain potential biosignatures. A prominent sedimentary fan deposit at the westernmargin of Jezero crater has been inferred to be a river delta that built into an ancient lake basin during the Late Noachian-Early Hesperian epochs on Mars (~3.6-3.8 Ga) [1, 2, 3]. The Perseverance rover landed on 18 February 2021 ~2.2 km from the western fan. During the early phase of mission investigations, highresolution images obtained from the Mastcam-Z camera and from the Remote Micro-Imager of the SuperCaminstrument provided the first ground-based observations of the western fan and an associated remnant outcrop, named Kodiak. Here, we report its sedimentology, which provide new constraints on the nature of the fan deposits, and their paleoenvironmental implications (4).
Published: 2022

48. A Mars 2020 Perseverance SuperCam Perspective on the Igneous Nature of the Máaz formation at Jezero crater, Mars

Author: Udry, A., Sautter, V., Cousin, A., Wiens, R. C., Forni, O., Benzerara, K., Beyssac, O., Nachon, M., Dromart, G., Quantin, C., Mandon, L., Clavé, E., Pinet, P., Ollila, A., Bosak, T., Mangold, N., Dehouck, E., Johnson, J., Schmidt, M., Horgan, B., Gabriel, T., Mclennan, S., Maurice, S., Simon, J.I., Herd, C., Madiaraga., J. M., University of Nevada [Las Vegas] (WGU Nevada), 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), 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), École normale supérieure de Lyon (ENS de Lyon), Massachusetts Institute of Technology (MIT), Brock University [Canada], Purdue University [West Lafayette], United States Geological Survey (USGS), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, University of Alberta, and University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU)
Subjects: Supercam, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, in situ exploration, [SDU]Sciences of the Universe [physics], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], mars mineralogy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Perseverance
Abstract: International audience
Published: 2022

49. Tensor component analysis as a tool for investigating depth trends in chem-cam libs data from gale crater, mars

Author: Rammelkamp, Kristin, Gasnault, Olivier, Forni, Olivier, Dehouck, Erwin, Bedford, Candice C., Lasue, Jeremie, Cousin, Agnès, Schröder, Susanne, Wiens, Roger C., Lanza, Nina, Institut für Optische Sensorsysteme, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), 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), Lunar and Planetary Institute [Houston] (LPI), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, Los Alamos National Laboratory (LANL), and Lunar and Planetary Institute
Subjects: LIBS, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, ChemCam, pattern recognition, Mars
Abstract: International audience
Published: 2022

50. A Komatiite Succession as an analog for the Olivine Bearing Rocks at Jezero

Author: A., Brown, R.C., Wiens, S., Maurice, K., Uckert, M., Tice, D. Flannery R.G., Deen, A.H., Treiman, K. L., Siebach, L.W., Beegle, W.J., Abbey, J.F., Bell, L.E., Mayhew, J.I., Simon, O., Beyssac, P.A., Willis, R., Bhartia, R.J., Smith, T., Fouchet, C., Quantin-Nataf., Pinet, P.C., L., Mandon, S. Le, Mouélic, A., Udry, B., Horgan, F., Calef, E., Cloutis, N., Turenne, C., Royer, M.-P., Zorzano, E., Ravanis, S., Fagents, A., Fairen, S., Gupta, V., Sautter, Y., Liu, M., Schmidt, K., Hickman-Lewis, Tennessee State University, 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Jackson School of Geosciences (JSG), University of Texas at Austin [Austin], Rice University [Houston], NASA Johnson Space Center (JSC), NASA, 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), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Cornell University [New York], Imperial College London, Brock University [Canada], The Natural History Museum [London] (NHM), and pinet, patrick
Subjects: [SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics], [SDU.STU] Sciences of the Universe [physics]/Earth Sciences, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, planetary surface, mars, mineralogy, petrology
Abstract: International audience
Published: 2022

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