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1. Depositional History of the Upper Sequence of the Western Fan: Evidence for Late-Stage Fluvial and Potential Igneous Activity, Jezero Crater, Mars

Author: S Gwizd, K M Stack, L Ives, S Gupta, N Randazzo, M Lamb, N Cavallo, N Williams, L Crumpler, J Rice, B Horgan, L C Kah, O Cianciolo, C Quantin-Nataf, O Beyssac, A Vaughan, J I Simon, K Siebach, M Nachon, R Kronyak, V Sun, S Sholes, D Shuster, and J Bell
Subjects: Lunar and Planetary Science and Exploration
Abstract: Within Jezero crater, a 45 km diameter Noachian-aged crater on Mars, the Upper Fan group (UFg) stratigraphy records the youngest interval of sediment deposition via aqueous activity on the western fan. From orbital images, the UFg surface is characterized by ridges interpreted to be associated with channels that can be group based on orientation into distinct elongate and fan-shaped deposits. UFg deposits primarily consist of a sandstone to granule conglomerate facies covered by a lithified boulder conglomerate or dense accumulations of loose boulders along the surface. The coarse-grained nature of UFg deposits and the unconformable contact with the underlying fan stratigraphy suggest that the UFg represents a higher-energy shift from the relatively longer-lived, lower-energy aqueous systems interpreted in underlying fan stratigraphy. The Mars 2020 Perseverance rover encountered the main exposures of the UFg deposits beginning on Sol 755 and has been continuously collecting data along its northwestward traverse across the fan, enabling reconciliation of orbitally-derived geomorphology with in-situ observations from the rover and Ingenuity helicopter. This work represents a combined assessment of the geomorphology and the sedimentology and stratigraphy of the UFg in order to establish its depositional and emplacement history. Determining the origins of the Upper Fan sequence will clarify how, when, and in what order aqueous environments evolved through time within Jezero crater (e.g. crater infill, overflow, breach, and lake level drop;). Finally, this work will provide critical context for the three rock samples within the UFg sample suite.
Published: 2024

2. Key Perseverance Sampling Locations for the Ancient Martian Crust and Implications for Mars Science

Author: E. L. Scheller, J. I. Simon, B. P. Weiss, C. Quantin-Nataf, B. L. Ehlmann, L. Mayhew, T. Bosak, J. F. Bell, III, A. Brown, C. Herd, A. Udry, and R. C. Wiens
Subjects: Lunar and Planetary Science and Exploration
Abstract: Since Feb 2021, the Perseverance rover has collected samples in the Jezero crater. The plan baselined at the 2018 landing site selection, subsequently further developed by the Mars-2020 team, and presented to the Decadal Survey included the exploration and sampling of the Jezero crater rim and the Nili Planum area, a rock record that is important to preserving the science return of the endeavor. Specifically, the science team identified the following prioritized science objectives aligned with community objectives that are not covered by the current sample cache: 1) Investigate the habitable environments with potential biosignatures from a more ancient time interval and from a diverse set of geological environments (incl. exposed subsurface) than the Jezero crater sedimentary deposits (Fig. 2). (2) Determine radioisotopic ages for well-defined craterretaining surfaces and/or the Isidis basin impact event. (3) Characterize ancient aqueous environments to study climate, environmental transitions, and habitability on ancient Mars. (4) Investigate planetary accretion, crustal evolution, and dynamo activity through analysis and sampling of igneous lithologies. (5) Study the geology of basin-forming impacts. In addition, for the Jezero rim and any Jezero ejecta: (6) Analyze Jezero impactites for potentially habitable hydrothermal environments and radioisotopic dating of the Jezero crater formation. From 2018 to now, we used a combination of High Resolution Imaging Experiment (HiRISE) and Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) data to further characterize Jezero rim and Nili Planum, culminating in our prioritized sample location recommendations: (1) Monument Valley and (2) Northwest Jezero rim.
Published: 2024

3. What Are the Olivine-Rich Boulders in the Upper Fan and Margin Unit at Jezero Crater, Mars?

Author: O Beyssac, E Clavé, A Udry, E Dehouck, O Forni, C Quantin-Nataf, G Lopez-Reyes, P Beck, C Royer, T Gabriel, L Kah, S Schroeder, J R Johnson, T Fouchet, J Simon, A Cousin, S Maurice, and R C Wiens
Subjects: Lunar and Planetary Science and Exploration
Abstract: Since February 2021, the Perseverance rover has explored Jezero Crater in the Nili Fossae region of Mars which hosts large outcrops of a regional olivine-carbonate unit. In the crater floor, Perseverance investigated two igneous formations: Máaz, composed of basaltic lava and/or pyroclastic flows, and Séítah, an olivine-rich cumulate] below Máaz. Then, Perseverance explored the western fan composed by diverse sedimentary rocks of variable composition, but often containing olivine On the upper fan and margin unit, Perseverance encountered number of centimetric to metric boulder rocks. Two main types of boulders were identified based on texture and composition: the olivine-rich and pyroxene-bearing boulders. Here, we use SuperCam data to describe the texture, geochemistry and mineralogy of the olivine-rich boulders. Then, we discuss their possible petrological origin and some possible implications for the regional Nili Fossae olivine-carbonate unit.
Published: 2024

4. The Scientific Value of Collecting Samples From the Jezero Crater Rim

Author: L. E. Mayhew, C. Quantin-Nataf, E. Scheller, J. I. Simon, B. P. Weiss, B. Horgan, M. Deahn, S. Alwmark, C. C. Bedford, E. M. Hausrath, A. Klidaras, K. M. Stack, K. Farley, C. D. K. Herd, S. Siljeström, and M. Wadhwa
Subjects: Lunar and Planetary Science and Exploration
Abstract: The Mars 2020 mission has been conducting ground-based investigation of the geology, habitability, and biosignature preservation potential and collecting samples for return to Earth in Jezero crater, Mars for nearly 3 years. Analysis of these samples will address outstanding questions in Mars science including potential habitability and how and why the climate the interior of the planet evolved through time. As of December 2023, samples of 4 igneous rocks of the Jezero crater floor and 9 sedimentary rocks of the Jezero fan and inner margin, remain on the rover. 15 tubes remain to be filled to enhance the diversity of the cache and broaden the scope of the science questions that can be addressed with returned sample studies. The next step in the mission is to explore the Jezero crater rim. It will be imperative to investigate and sample the diversity of crater rim rocks because they represent materials from Mars’ most ancient crust older than those sampled in Jezero crater, a diversity of geologic processes, and potential ancient habitable environments that have not yet been investigated or sampled. Ongoing mapping efforts are using orbiter data and long-distance images from Perseverance to identify and interpret the geologic context of the crater rim. Building on this effort and the broader geologic context for the crater rim put forward by previous studies, we identify diverse targets for in situ investigation and potential sampling by Mars 2020.
Published: 2024

5. The Complex Exhumation History of Jezero Crater Floor Unit and Its Implication for Mars Sample Return

Author: C Quantin-Nataf, S Alwmark, F J Calef, J Lasue, K Kinch, K M Stack, V Sun, N R Williams, E Dehouck, L Mandon, N Mangold, O Beyssac, E Clave, S H G Walter, J I Simon, A M Annex, B Horgan, James W Rice Jr, D Shuster, B Cohen, L Kah, Steven Sholes, and B P Weiss
Subjects: Geosciences (General), Lunar and Planetary Science and Exploration
Abstract: During the first year of NASA's Mars 2020 mission, Perseverance rover has investigated the dark crater floor unit of Jezero crater and four samples of this unit have been collected. The focus of this paper is to assess the potential of these samples to calibrate the crater-based Martian chronology. We first review the previous estimation of crater-based model age of this unit. Then, we investigate the impact crater density distribution across the floor unit. It reveals that the crater density is heterogeneous from areas which have been exposed to the bombardment during the last 3 Ga to areas very recently exposed to bombardment. It suggests a complex history of exposure to impact cratering. We also display evidence of several remnants of deposits on the top of the dark floor unit across Jezero below which the dark floor unit may have been buried. We propose the following scenario of burying/exhumation: the dark floor unit would have been initially buried below a unit that was a few tens of meters thick. This unit then gradually eroded away due to Aeolian processes from the northeast to the west, resulting in uneven exposure to impact bombardment over 3 Ga. A cratering model reproducing this scenario confirms the feasibility of this hypothesis. Due to the complexity of its exposure history, the Jezero dark crater floor unit will require additional detailed analysis to understand how the Mars 2020 mission samples of the crater floor can be used to inform the Martian cratering chronology.
Published: 2023
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6. ROMA: A Database of Rock Reflectance Spectra for Martian In Situ Exploration

Author: L. Mandon, P. Beck, C. Quantin‐Nataf, E. Dehouck, P. Thollot, D. Loizeau, and M. Volat
Subjects: reflectance spectroscopy, rocks, Martian rovers, database, Astronomy, QB1-991, Geology, QE1-996.5
Abstract: Abstract The ROMA database (ROck reflectance for MArtian in situ exploration, https://roma.univ-lyon1.fr) provides the reflectance spectra between 0.4 and 3–4 μm of various terrestrial, Martian, and synthetic samples, as a means to document reference measurements for comparison with data acquired by visible and near‐infrared spectrometers on planetary surfaces, with a focus on current and future Martian observations by the Perseverance (Mars 2020 mission) and Rosalind Franklin (ExoMars) rovers. The main specificity of this database is to include a significant fraction of spectra of unprocessed rock, which are more realistic analogs and often have different spectral features than the fine powders more commonly analyzed in reflectance spectroscopy. Additionally, these measurements were acquired with a spectrometer whose spot size is similar to those of the SuperCam instrument (Mars 2020 mission) at a few meters from a target. Supplementary information are provided in the ROMA database: higher‐level data (such as absorption band parameters) as well as sample mineralogy estimated by whole‐rock X‐ray diffraction analyses. Future comparisons with this database will help improve the interpretation of spectral measurements acquired on the Martian surface. This work introduces the aim of the library and its current state, but additional data on intact natural rock surfaces will likely be added in the future.
Published: 2022
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7. Stratigraphic Relationships in Jezero Crater, Mars: Constraints on the Timing of Fluvial‐Lacustrine Activity From Orbital Observations

Author: S. Holm‐Alwmark, K. M. Kinch, M. D. Hansen, S. Shahrzad, K. Svennevig, W. J. Abbey, R. B. Anderson, F. J. Calef, S. Gupta, E. Hauber, B. H. N. Horgan, L. C. Kah, J. Knade, N. B. Miklusicak, K. M. Stack, V. Z. Sun, J. D. Tarnas, and C. Quantin‐Nataf
Published: 2021
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8. Samples Collected from the Floor of Jezero Crater with the Mars 2020 Perseverance Rover

Author: J. I. Simon, K. Hickman‐Lewis, B. A. Cohen, L.E. Mayhew, D.L. Shuster, V. Debaille, E. M. Hausrath, B.P. Weiss, T. Bosak, M.‐P. Zorzano, H. E. F. Amundsen, L.W. Beegle, J.F. Bell, K. C. Benison, E. L. Berger, O. Beyssac, A.J. Brown, F. Calef, T. M. Casademont, B. Clark, E. Clavé, L. Crumpler, A. D. Czaja, A. G. Fairén, K. A. Farley, D. T. Flannery, T. Fornaro, O. Forni, F. Gómez, Y. Goreva, A. Gorin, K. P. Hand, S.‐E. Hamran, J. Henneke, C. D. K. Herd, B. H. N. Horgan, J. R. Johnson, J. Joseph, R. E. Kronyak, J. M. Madariaga, J. N. Maki, L. Mandon, F. M. McCubbin, S. M. McLennan, R. C. Moeller, C. E. Newman, J. I. Núñez, A. C. Pascuzzo, D. A. Pedersen, G. Poggiali, P. Pinet, C. Quantin‐Nataf, M. Rice, J. W. Rice, C. Royer, M. Schmidt, M. Sephton, S. Sharma, S. Siljeström, K. M. Stack, A. Steele, V. Z. Sun, A. Udry, S. VanBommel, M. Wadhwa, R. C. Wiens, A. J. Williams, and K. H. Williford
Subjects: Mars Sample Return, rock core, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Jezero Crater, Mars 2020, Earth and Planetary Sciences (miscellaneous)
Abstract: The first samples collected by the Mars 2020 mission represent units exposed on the Jezero Crater floor, from the potentially oldest Séítah formation outcrops to the potentially youngest rocks of the heavily cratered Máaz formation. Surface investigations reveal landscape-to-microscopic textural, mineralogical, and geochemical evidence for igneous lithologies, some possibly emplaced as lava flows. The samples contain major rock-forming minerals such as pyroxene, olivine, and feldspar, accessory minerals including oxides and phosphates, and evidence for various degrees of aqueous activity in the form of water-soluble salt, carbonate, sulfate, iron oxide, and iron silicate minerals. Following sample return, the compositions and ages of these variably altered igneous rocks are expected to reveal the geophysical and geochemical nature of the planet’s interior at the time of emplacement, characterize martian magmatism, and place timing constraints on geologic processes, both in Jezero Crater and more widely on Mars. Petrographic observations and geochemical analyses, coupled with geochronology of secondary minerals, can also reveal the timing of aqueous activity as well as constrain the chemical and physical conditions of the environments in which these minerals precipitated, and the nature and composition of organic compounds preserved in association with these phases. Returned samples from these units will help constrain the crater chronology of Mars and the global evolution of the planet’s interior, for understanding the processes that formed Jezero Crater floor units, and for constraining the style and duration of aqueous activity in Jezero Crater, past habitability, and cycling of organic elements in Jezero Crater.
Published: 2023
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9. 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

10. Rivers and Lakes in Western Arabia Terra: The Fluvial Catchment of the ExoMars 2022 Rover Landing Site

Author: Peter Fawdon, C. Quantin-Nataf, John Bridges, Joel Davis, Sanjeev Gupta, and Matthew R. Balme
Subjects: geography, geography.geographical_feature_category, Drainage basin, Sediment, Fluvial, Structural basin, Chryse Planitia, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Geomorphology, Geology, Channel (geography)
Abstract: Oxia Planum, the landing site for the ExoMars rover mission, is a shallow basin on the southern margin of Chryse Planitia that hosts remnants of fan-shaped sedimentary deposits associated with the ancient channel system Coogoon Vallis. This indicates runoff from a catchment in Arabia Terra has transported sediment into the landing site. To explore this fluvial system we created a model catchment for Oxia Planum and, using 6 m/pixel ConTeXt camera (CTX) orbital remote sensing image data, we digitised the fluvial and lacustrine landforms in Western Arabia Terra in and around this catchment. We find: (1) The catchment has a minimum area of ∼2.1×105 km2 and has been episodically deformed by tectonic activity; (2) There were at least two phases of fluvial activity. The first created a mature landscape associated with Coogoon Vallis, which may have deposited alluvial or deltaic deposits in the Oxia Basin. After a substantial hiatus, a second phase of activity incised U-section channels into the pre-existing landscape and channel systems; and (3) Evidence for numerous possible paleolake deposits within the catchment. These are not well connected to the fluvial system and were probably sustained by groundwater activity contemporaneous with both phases of fluvial activity. This groundwater might have modified the mineralogy of Oxia Planum. Oxia Planum probably experienced an alluvial or distal deltaic/lacustrine depositional environment during the mid Noachian, which was later overprinted by a younger phase of fluvial activity.
Published: 2022

11. Assessing slope uncertainties of martian Digital Elevation Models from numerical propagation of errors on synthetic geological surfaces

Author: C. Millot, C. Quantin-Nataf, C. Leyrat, V. Lherm, and M. Volat
Subjects: Space and Planetary Science, Astronomy and Astrophysics
Published: 2023
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12. Perseverance rover reveals an ancient delta-lake system and flood deposits at Jezero crater, Mars

Author: C. Quantin-Nataf, Keyron Hickman-Lewis, Adrian J. Brown, Tanja Bosak, Scott M. McLennan, David L. Shuster, Kenneth H. Williford, R. A. Yingst, Kenneth A. Farley, Benjamin P. Weiss, James F. Bell, Sylvestre Maurice, Amy J. Williams, Linda C. Kah, S. F. Sholes, Gilles Dromart, Vivian Z. Sun, Justin I. Simon, S. Holm-Alwmark, Jorge I. Nunez, Olivier Gasnault, Sunetra Gupta, Ann Ollila, Melissa S. Rice, Allan H. Treiman, K. M. Stack, John P. Grotzinger, N. Mangold, J. Martinez-Frias, Bethany L. Ehlmann, Roger C. Wiens, J. W. Rice, Olivier Beyssac, P. Pilleri, Fred Calef, Briony Horgan, J. D. Tarnas, Nathan R. Williams, S. Le Mouélic, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institut 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), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: Delta, Hydrology Geomorphology fluvial 1625, 010504 meteorology & atmospheric sciences, Geochemistry, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Mars, 01 natural sciences, Jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Impact crater, Margin (machine learning), 0103 physical sciences, 010303 astronomy & astrophysics, CORINTH, 0105 earth and related environmental sciences, ARCHITECTURE, Multidisciplinary, Flood myth, ORIGIN, Mars Exploration Program, SCIENCE, Sedimentology, 13. Climate action, RIFT, Sedimentary rock, Geology
Abstract: Perseverance images of a delta on Mars The Perseverance rover landed in Jezero crater, Mars, in February 2021. Earlier orbital images showed that the crater contains an ancient river delta that was deposited by water flowing into a lake billions of years ago. Mangold et al . analyzed rover images taken shortly after landing that show distant cliff faces at the edge of the delta. The exposed stratigraphy and sizes of boulders allowed them to determine the past lake level and water discharge rates. An initially steady flow transitioned into intermittent floods as the planet dried out. This history of the delta’s geology provides context for the rest of the mission and improves our understanding of Mars’ ancient climate. —KTS
Published: 2021
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13. Crustal and time-varying magnetic fields at the InSight landing site on Mars

Author: Christopher T. Russell, Matthew Fillingim, Sabine Stanley, Lu Pan, Benoit Langlais, William B. Banerdt, Peter Chi, Catherine L. Johnson, Chloé Michaut, Aymeric Spiga, Philippe Lognonné, Don Banfield, François Forget, Veronique Ansan, Steve Joy, Yanan Yu, Mark A. Wieczorek, Anna Mittelholz, Suzanne E. Smrekar, Shea N. Thorne, C. Quantin-Nataf, Matthew P. Golombek, H. Haviland, Xinping Liu, Department of Earth, Ocean and Atmospheric Sciences [Vancouver] (UBC EOAS), University of British Columbia (UBC), Planetary Science Institute [Tucson] (PSI), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Earth, Planetary and Space Sciences [Los Angeles] (EPSS), University of California [Los Angeles] (UCLA), University of California-University of California, Cornell University [New York], Earth, Planetary and Space Sciences, University of California, Los Angeles, CA, USA., Space Sciences Laboratory [Berkeley] (SSL), University of California [Berkeley], Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Marshall Space Flight Center, Huntsville, AL, USA, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Earth, Planetary and Space Sciences, University of California, Los Angeles, CA, USA, Institut de Physique du Globe de Paris (IPGP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA, Morton K. Blaustein Department of Earth and Planetary Sciences [Baltimore], Johns Hopkins University (JHU), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), InSight Project at the Jet Propulsion Laboratory, California Institute of Technology National Aeronautics & Space Administration (NASA) InSight Participating Scientist Program Canadian Space Agency Centre National D'etudes Spatiales Green Foundation for Earth Sciences during leave at the Institute of Geophysics and Planetary Physics, Scripps Institution of Oceanography (2019-2020), University of California (UC)-University of California (UC), University of California [Berkeley] (UC Berkeley), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Martian, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Field (physics), MANTLE, Mars Exploration Program, Geophysics, 010502 geochemistry & geophysics, 01 natural sciences, Physics::Geophysics, Magnetic field, Atmosphere, Magnetization, Solar wind, ELECTRICAL-CONDUCTIVITY, [SDU]Sciences of the Universe [physics], 13. Climate action, Physics::Space Physics, General Earth and Planetary Sciences, Astrophysics::Earth and Planetary Astrophysics, MOON, Geology, 0105 earth and related environmental sciences, Dynamo
Abstract: Magnetic fields provide a window into a planet’s interior structure and evolution, including its atmospheric and space environments. Satellites at Mars have measured crustal magnetic fields indicating an ancient dynamo. These crustal fields interact with the solar wind to generate transient fields and electric currents in Mars’s upper atmosphere. Surface magnetic field data play a key role in understanding these effects and the dynamo. Here we report measurements of magnetic field strength and direction at the InSight (Interior Exploration using Seismic Investigations, Geodesy and Heat Transport) landing site on Mars. We find that the field is ten times stronger than predicted by satellite-based models. We infer magnetized rocks beneath the surface, within ~150 km of the landing site, consistent with a past dynamo with Earth-like strength. Geological mapping and InSight seismic data suggest that much or all of the magnetization sources are carried in basement rocks, which are at least 3.9 billion years old and are overlain by between 200 m and ~10 km of lava flows and modified ancient terrain. Daily variations in the magnetic field indicate contributions from ionospheric currents at 120 km to 180 km altitude. Higher-frequency variations are also observed; their origin is unknown, but they probably propagate from even higher altitudes to the surface. We propose that the time-varying fields can be used to investigate the electrical conductivity structure of the martian interior. The magnetic field measured by the InSight lander on Mars varies daily and is ten times stronger than expected. The field is inferred to originate from components of basement rocks magnetized by an ancient dynamo of Earth-like strength.
Published: 2020
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14. Martian meteorites reflectance and implications for rover missions

Author: Pierre Beck, C. Quantin-Nataf, Violaine Sautter, M. Martinot, Lu Pan, Erwin Dehouck, Antoine Pommerol, Romain Cerubini, Lucia Mandon, Zurine Yoldi, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Universität Bern [Bern] (UNIBE), Physikalisches Institut [Bern], Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), and Universität Bern [Bern]
Subjects: spectroscopy, 010504 meteorology & atmospheric sciences, Imaging spectrometer, Mineralogy, FOS: Physical sciences, Mars, 01 natural sciences, Spectral line, meteorites, Physics - Geophysics, 0103 physical sciences, surface, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 0105 earth and related environmental sciences, Martian, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Spectrometer, 520 Astronomy, Hyperspectral imaging, Astronomy and Astrophysics, Mars Exploration Program, 620 Engineering, Geophysics (physics.geo-ph), Imaging spectroscopy, Meteorite, Space and Planetary Science, Astrophysics - Instrumentation and Methods for Astrophysics, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract: International audience; During this decade, two rovers will characterize in situ the mineralogy of rocks on Mars, using for the first time near-infrared reflectance spectrometers: SuperCam onboard the Mars 2020 rover and MicrOmega onboard the ExoMars rover, although this technique is predominantly used in orbit for mineralogical investigations. Until successful completion of sample-return missions from Mars, Martian meteorites are currently the only samples of the red planet available for study in terrestrial laboratories and comparison with in situ data. However, the current spectral database available for these samples does not represent their diversity and consists primarily of spectra acquired on finely crushed samples, albeit grain size is known to greatly affect spectral features. Here, we measured the reflected light of a broad Martian meteorite suite as a means to catalogue and characterize their spectra between 0.4 and 3 μm. These measurements are achieved using a point spectrometer acquiring data comparable to SuperCam, and an imaging spectrometer producing hyperspectral cubes, similarly to MicrOmega. Our results indicate that point spectrometry is sufficient to discriminate the different Martian meteorites families, to identify their primary petrology based on band parameters, and to detect their low content in alteration minerals. However, significant spectral mixing occurs in the point measurements, even at spot sizes down to a few millimeters, and high-resolution imaging spectroscopy is needed to correctly identify the various mineral phases in the meteorites. Additional bidirectional spectral measurements on a consolidated and powdered shergottite confirm their non-Lambertian behavior, with backward and suspected forward scattering peaks. With changing observation geometry, the main absorption strengths show variations up to ~10–15%. The variation of reflectance levels is reduced for the rock surface compared to the powder. All the spectra presented are provided in the supplementary data for further comparison with in situ and orbital measurements.
Published: 2021
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15. Voluminous Silica Precipitated from Martian Waters during Late-stage Aqueous Alteration

Author: Lu Pan, M. Pineau, Boris Chauviré, C. Quantin-Nataf, John Carter, Laetitia Le Deit, Nicolas Mangold, Benjamin Rondeau, Vincent Chevrier, 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), Centre for Star and Planet Formation (STARPLAN), Globe Institute, Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), 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 Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences de la Terre (ISTerre), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Gustave Eiffel-Université Grenoble Alpes (UGA), Arkansas Center for Space and Planetary Sciences, University of Arkansas [Fayetteville], ANR-16-CE31-0012,MARS-PRIME,Environnement Primitif de Mars(2016), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Health and Medical Sciences, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Amazonian, Geochemistry, FOS: Physical sciences, 010502 geochemistry & geophysics, 01 natural sciences, chemistry.chemical_compound, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Martian surface, Earth and Planetary Sciences (miscellaneous), ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Martian, geography, geography.geographical_feature_category, Hydrated silica, Alluvial fan, Astronomy and Astrophysics, Mars Exploration Program, 15. Life on land, CRISM, Geophysics, chemistry, 13. Climate action, Space and Planetary Science, Hesperian, Geology, Astrophysics - Earth and Planetary Astrophysics
Abstract: Mars’ transition from an early “warm and wet” to a “cold and dry” environment left fingerprints on the geological record of fluvial activity on Mars. The morphological and mineralogical observations of aqueous activity provided varying constraints on the condition and duration of liquid water on the Martian surface. In this study, we surveyed the mineralogy of Martian alluvial fans and deltas and investigated the hydrated silica-bearing deposits associated with some of these landforms. Using CRISM data, we identified 35 locations across Mars with hydrated silica in proximity to fans/deltas, where the spectral characteristics are consistent with immature or dehydrated opal-A. In a few stepped fans/deltas, we find hydrated silica occurs within the bulk fan deposits and form sedimentary layers correlated with elevation. Meanwhile, in the older fans/deltas, silica mostly occurs at distal locations, and the relation to primary sedimentary deposits is more complex. We propose that the hydrated silica-bearing deposits in stepped fans/deltas likely formed authigenically from Martian surface waters, mainly during the Late Hesperian and Early Amazonian. These silica-bearing deposits could be a tracer for the temperature or duration of water involved in the formation of these deposits, given more precise and detailed observations of the sedimentary context, accessory minerals, the concentration of hydrated silica, and sediment-to-water ratio. Therefore, we consider that silica-bearing deposits should be among the most critical samples to investigate for future Mars missions, which are accessible in the landing sites of Mars 2020 and ExoMars 2022 missions.
Published: 2021
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16. The SuperCam Instrument Suite on the Mars 2020 Rover: Science Objectives and Mast-Unit Description

Author: I. Torre-Fdez, V. Gharakanian, E. Cordoba, Jérôme Parisot, R. Perez, Amaury Fau, Peter Willis, Ruth A. Anderson, Pablo Sobron, K. W. Wong, A. Debus, Julien Mekki, Noureddine Melikechi, K. Mathieu, S. Gauffre, M. Toplis, Jesús Martínez-Frías, Alexandre Cadu, Francois Poulet, B. Quertier, Horton E. Newsom, H. Seran, C. Quantin-Nataf, W. D’anna, Jens Frydenvang, Frédéric Chapron, Pierre Beck, Jean-François Mariscal, B. Chide, Y. André, Y. Michel, G. Orttner, N. Toulemont, A. Dufour, Briana Lucero, Olivier Gilard, Marion Bonafous, D. Pheav, Q.-M. Lee, D. Standarovsky, Franck Montmessin, R. Gonzalez, S. Le Mouélic, Cedric Virmontois, L. Roucayrol, I. Gontijo, M. Deleuze, L. Parès, L. Oudda, Y. Micheau, F. Manni, Bruno Dubois, Bruno Bousquet, G. de los Santos, D. M. Delapp, Guillermo Lopez-Reyes, L. Picot, Clément Royer, E. Clave, Richard Leveille, Erwin Dehouck, Gaetan Lacombe, J. Javier Laserna, Olivier Beyssac, P. Romano, Y. Daydou, Scott M. McLennan, John Michel, V. Sridhar, Driss Kouach, Gabriel Pont, M. Dupieux, Michel Gauthier, Jean-Michel Reess, J. Moros, J.-C. Dameury, T. Fouchet, Ann Ollila, Sophie Jacquinod, P. Y. Meslin, M. Egan, Juan Manuel Madariaga, Karim Benzerara, G. Hervet, Gilles Montagnac, Woodward W. Fischer, Olivier Gasnault, T. Nelson, Stanley M. Angel, Lauren DeFlores, Violaine Sautter, Marco Veneranda, C. Leyrat, Olivier Humeau, Y. Morizet, Jose Antonio Manrique, M. Sodki, P. Pilleri, C. Velasco, Naomi Murdoch, M. J. Schoppers, S. A. Storms, Sylvestre Maurice, Benigno Sandoval, Cedric Pilorget, N. Striebig, S. Robinson, V. Mousset, David Mimoun, Morten Madsen, M. Heim, A. Doressoundiram, Christophe Montaron, Eric Lewin, Patrick Pinet, C. Donny, Susanne Schröder, Agnès Cousin, Sadok Abbaki, John P. Grotzinger, Claude Collin, Xavier Jacob, Jeffrey R. Johnson, Cécile Fabre, K. McCabe, C. Legett, J. P. Berthias, Shiv K. Sharma, Timothy H. McConnochie, A. Sournac, Ralph D. Lorenz, M. Viso, Yann Parot, N. Mangold, W. Rapin, Jérémie Lasue, Gorka Arana, Joan Ervin, E. Le Comte, N. Nguyen Tuong, P. Cais, Olivier Forni, D. Rambaud, T. Battault, D. Venhaus, Anupam K. Misra, K. Clark, M. Tatat, Laurent Lapauw, P. Bernardi, Roger C. Wiens, Samuel M. Clegg, Nina Lanza, Sylvain Bernard, Soren N. Madsen, Kepa Castro, M. Boutillier, Raymond Newell, D. Granena, Y. Hello, Fernando Rull, M. Ruellan, R. Mathon, Edward A. Cloutis, Gilles Dromart, L. Le Deit, Rafik Hassen-Khodja, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Universidad de Valladolid [Valladolid] (UVa), Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), US Geological Survey [Flagstaff], United States Geological Survey [Reston] (USGS), University of South Carolina [Columbia], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), University of Winnipeg, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France, University of Hawai‘i [Mānoa] (UHM), GeoRessources, Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), University of Copenhagen = Københavns Universitet (UCPH), Institut de mécanique des fluides de Toulouse (IMFT), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), PLANETO - LATMOS, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universidad de Málaga [Málaga] = University of Málaga [Málaga], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), McGill University = Université McGill [Montréal, Canada], Institut des Sciences de la Terre (ISTerre), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Gustave Eiffel-Université Grenoble Alpes (UGA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Maryland [College Park], University of Maryland System, Stony Brook University [SUNY] (SBU), State University of New York (SUNY), University of Massachusetts [Lowell] (UMass Lowell), University of Massachusetts System (UMASS), Laboratoire de Planétologie et Géodynamique - Angers (LPG-ANGERS), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), The University of New Mexico [Albuquerque], Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut für Optische Sensorsysteme, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), SETI Institute, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Bordeaux (UB), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD), Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS), University of Copenhagen = Københavns Universitet (KU), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées, Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), and Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées
Subjects: Rocks, 010504 meteorology & atmospheric sciences, Computer science, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Mars, Context (language use), Perseverance, Imaging on Mars, Mars 2020 Perseverance rover, 01 natural sciences, SuperCam Instrument, Unit (housing), Mast (sailing), Jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, imaging on Mars, Microphone on Mars, 0103 physical sciences, Calibration, Rover, [PHYS.COND]Physics [physics]/Condensed Matter [cond-mat], infrared spectroscopy, Raman, 010303 astronomy & astrophysics, Infrared spectroscopy, 0105 earth and related environmental sciences, [SPI.ACOU]Engineering Sciences [physics]/Acoustics [physics.class-ph], M2020, LIBS, Payload, Suite, Mars2020, Astronomy and Astrophysics, Laser-Induced Breakdown Spectroscopy, Mars Exploration Program, microphone on Mars, Planetary science, SuperCam, Space and Planetary Science, Raman spectroscopy, Systems engineering, [PHYS.COND.CM-MS]Physics [physics]/Condensed Matter [cond-mat]/Materials Science [cond-mat.mtrl-sci], Mars 2020 PERSEVERANCE rover
Abstract: On the NASA 2020 rover mission to Jezero crater, the remote determination of the texture, mineralogy and chemistry of rocks is essential to quickly and thoroughly characterize an area and to optimize the selection of samples for return to Earth. As part of the Perseverance payload, SuperCam is a suite of five techniques that provide critical and complementary observations via Laser-Induced Breakdown Spectroscopy (LIBS), Time-Resolved Raman and Luminescence (TRR/L), visible and near-infrared spectroscopy (VISIR), high-resolution color imaging (RMI), and acoustic recording (MIC). SuperCam operates at remote distances, primarily 2-7 m, while providing data at sub-mm to mm scales. We report on SuperCam's science objectives in the context of the Mars 2020 mission goals and ways the different techniques can address these questions. The instrument is made up of three separate subsystems: the Mast Unit is designed and built in France; the Body Unit is provided by the United States; the calibration target holder is contributed by Spain, and the targets themselves by the entire science team. This publication focuses on the design, development, and tests of the Mast Unit; companion papers describe the other units. The goal of this work is to provide an understanding of the technical choices made, the constraints that were imposed, and ultimately the validated performance of the flight model as it leaves Earth, and it will serve as the foundation for Mars operations and future processing of the data. In France was provided by the Centre National d'Etudes Spatiales (CNES). Human resources were provided in part by the Centre National de la Recherche Scientifique (CNRS) and universities. Funding was provided in the US by NASA's Mars Exploration Program. Some funding of data analyses at Los Alamos National Laboratory (LANL) was provided by laboratory-directed research and development funds.
Published: 2021
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17. Morphological and Spectral Diversity of the Clay-Bearing Unit at the ExoMars Landing Site Oxia Planum

Author: Lu Pan, John Carter, Erwin Dehouck, C. Quantin-Nataf, Lucia Mandon, Patrick Thollot, Livio L. Tornabene, John Bridges, Matthieu Volat, Nicolas Thomas, Gabriele Cremonese, Pierre Beck, Adam Parkes Bowen, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), University of Leicester, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-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)-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), University of Bern, Istituto Nazionale di Astrofisica (INAF), University of Western Ontario (UWO), 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 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), and 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
Subjects: Spectroscopy, Minerals, 010504 meteorology & atmospheric sciences, Extraterrestrial Environment, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Planum temporale, Water, Mars, Geology, Mars Exploration Program, 15. Life on land, Spectral diversity, 01 natural sciences, Agricultural and Biological Sciences (miscellaneous), Astrobiology, Space and Planetary Science, 0103 physical sciences, Exobiology, Clay, 14. Life underwater, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Landing site
Abstract: International audience; The European Space Agency and Roscosmos' ExoMars rover mission, which is planned to land in the Oxia Planum region, will be dedicated to exobiology studies at the surface and subsurface of Mars. Oxia Planum is a clay-bearing site that has preserved evidence of long-term interaction with water during the Noachian era. Fe/Mg-rich phyllosilicates have previously been shown to occur extensively throughout the landing area. Here, we analyze data from the High Resolution Imaging Science Experiment (HiRISE) and from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instruments onboard NASA's Mars Reconnaissance Orbiter and the Colour and Stereo Surface Imaging System (CaSSIS) onboard ESA's Trace Gas Orbiter to characterize, at a high spatial resolution, the morphological and spectral variability of Oxia Planum's surface deposits. Two main types of bedrocks are identified within the clay-bearing, fractured unit observed throughout the landing site: (1) an orange type in HiRISE correlated with the strongest detections of secondary minerals (dominated by Fe/Mg-rich clay minerals) with, in some locations, an additional spectral absorption near 2.5 μm, suggesting the mixture with an additional mineral, plausibly carbonate or another type of clay mineral; (2) a more bluish bedrock associated with weaker detections of secondary minerals, which exhibits at certain locations a ∼1 μm broad absorption feature consistent with olivine. Coanalysis of the same terrains with the recently acquired CaSSIS images confirms the variability in the color and spectral properties of the fractured unit. Of interest for the ExoMars mission, both types of bedrocks are extensively outcropping in the Oxia Planum region, and the one corresponding to the most intense spectral signals of clay minerals (the primary scientific target) is well exposed within the landing area, including near its center.
Published: 2021
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18. Critical knowledge gaps in the Martian geological record: A rationale for regional-scale in situ exploration by rotorcraft mid-air deployment

Author: Valerie Payre, Bethany L. Ehlmann, N. Mangold, Robert Lillis, J. Bapst, Sylvestre Maurice, Violaine Sautter, A. A. Fraeman, William Rapin, Benoit Langlais, Jessica Flahaut, Anna Mittelholz, Arya Udry, David Baratoux, James Tuttle Keane, Gilles Dromart, C. Quantin-Nataf, and Briony Horgan
Subjects: Martian, Scale (ratio), Software deployment, Earth science, Geologic record, Geology
Published: 2021
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19. Team Mapping of Oxia Planum for the ExoMars 2022 Rover-Surface Platform Mission

Author: Peter Grindrod, Elliot Sefton-Nash, Ottaviano Ruesch, Andrea Nass, Ernst Hauber, Jorge L. Vago, Alessandro Frigeri, Peter Fawdon, Solmaz Adeli, Matthieu Volat, Csilla Orgel, Laetitia Le Deit, Joel Davis, Sander de Witte, Damien Loizeau, C. Quantin-Nataf, and Matthew R. Balme
Subjects: geology, Planum temporale, Mars, mapping, ExoMars, Landing Site, Geology, Astrobiology
Abstract: Oxia Planum (OP), located at the transition between the ancient terrain of Arabia Terra and the low lying basin of Chryse Planitia, will be the landing site for the ESA-Roscosmos ExoMars Programme’s 2022 mission [1]. The descent module and landing platform, Kazachock, will transport the Rosalind Franklin Rover to search for signs of past and present life on Mars, and investigate the geochemical environment in the shallow subsurface over a 211-sol nominal mission.OP forms a shallow basin, open to the north, characterized by clay-bearing bedrock, and episodic geological activity spans from the ~mid-Noachian to ~early Amazonian in age [2,3,4]. Building a thorough understanding of Oxia Planum prior to operations will provide testable hypotheses that facilitate interpretation of results, and hence provide an effective approach to address the mission’s science objectives. To this end, we have run a detailed group mapping campaign at HiRISE-scale using the Multi-Mission Geographic Information System (MMGIS) [5], co-registered HRSC [6], CaSSIS and HiRISE mosaics [7], and 116 1km2 quads covering the 1-sigma landing ellipse envelope. Complementary CTX-scale mapping covers the wider area around the landing site and is described elsewhere [8].Throughout 2020, 84 mapping volunteers associated with the mission’s Rover Science Operations Working Group followed a pre-formulated programme of training, familiarisation and mapping. With the mapping phase complete, a small sub-team are focused on map reconciliation phase, comprising data cleaning and science decision making. The process will culminate in map finalisation and submission for publication, and use in activities to plan rover science activities.This campaign yields important advances for overall science readiness of the ExoMars 2022 mission:Team experience working, communicating and learning together, valuable for operations. Building team knowledge of the landing site, and the main scientific interpretations. Curated datasets and software available for team use in ongoing planning. High-resolution map data representing our geologic understanding of Oxia Planum. This is an input to ongoing RSOWG work to construct the mission strategic plan, which provides science traceability from mission objectives to rover activities.Acknowledgments: We thank Fred Calef and Tariq Soliman at JPL for their support regarding MMGIS.References: [1] Vago, J. L. et al., (2017) Astrobiology 17 (6–7), 471–510. [2] Carter, J. et al., (2013) J. Geophys. Res. 118 (4), 831–858. [3] Quantin-Nataf, C. et al., (2021) Astrobiol. 21 (3), doi:10.1089/ast.2019.2191. [4] Fawdon P. et al., (2019) LPSC50 #2132. [5] Calef, F. J. et al., (2019) in 4th Planet. Data Work., Vol. 2151. [6] Gwinner, K. et al., (2016) Planet. Space Sci. 126, 93–138. [7] Volat, M. et al., (2020), EPSC, #564. [8] Hauber, E. et al. (2021), LPSC52.
Published: 2021
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20. MarsSI: Martian surface data processing service

Author: Matthieu Volat, Lucia Mandon, Patrick Thollot, and C. Quantin-Nataf
Subjects: Service (business), Data processing, Martian surface, Environmental science, Remote sensing
Abstract: MarsSI is a platform to help find and process Mars orbital data. Originaly developed in the context of the e-Mars project (2012-2017) funded by the European Research Council, it was certified in 2017 as french national Research Infrastructure by the Centre National de la Recherche Scientifique (CNRS) as part of the Planetary Surface Portal (PSUP) [2].MarsSI client interface is a web application. The user is provided a map based interface where available products are displayed as footprints. The user can browse and select data from here. A workspace view, allows the user to better review product selection individually. This is also the view where user will be able to request dataset processing.All MarsSI proposed pipelines are fully automated and do not require user parametrization. This allows us to keep our global catalog reasonable and have only one version of a single product at a time, that is shared between all users. To retrieve a product, the user will request a copy operation to its home directory, where it will be available for 30 days through SFTP access (the product is kept can be copied again after this).As of 2021, MarsSI indexes and give access to the optical data (visible, multi and hyperspectral) and derived products from three missions: Mars Odyssey, Mars Express and Mars Reconnaissance Orbiter. Our emphasis was to provide ”ready-to-use” products in regards of calibration, refinements and georeferencing. The user will be able to visualize and interpret the data in GIS or remote sensing software.MarsSI provides access to various optical datasets for visible, multi- and hypespectral data from the various martian orbital missions over the years. We also offer multiple Digital Elevation Model (DEM) datasets. Some of them are provided from external sources (such as those provided by the HiRISE and HSRC teams). But users can also requests med- and high-resolution DEMs generated using the Ames Stereo Pipeline software that are computed on our platform using a custom developed workflow.MarsSI is open to the world wide scientific community. As of december 2020, we count 215 registered users across 128 institutes. Since it is a french service, 25% of the users are from France, but we also offer data to scientists from the USA, UK, India and China.Built upon opensource frameworks and using standardized protocols, MarsSI offers the scientific communities an easy way to process data, most notably DEMs that can be derived from CTX and HiRISE data collection.
Published: 2021
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21. Tracing Martian volcanic activity using crater obliteration rate

Author: Clément Brustel, C. Quantin-Nataf, Sylvain Breton, Lu Pan, and Jessica Flahaut
Subjects: Martian, geography, geography.geographical_feature_category, Impact crater, Volcano, Geochemistry, Tracing, Geology
Abstract: Impact craters are often used to date planetary surfaces, the density of crater increasing with the exposure age of the surface. However, some geologic event, such as lava flows, do not totally “reset” the crater clock. Indeed, larger craters, rather than being totally recovered by the lava flow will be only partially filled.In that case, the crater size frequency distribution differs from cratering models. In order to better describe crater populations, additional parameters can be included. To this purpose we build crater size and depth frequency distributions that offers a snapshot of the current degradation state of the population.We used cratering models to interpret crater size and depth frequency distributions in terms of crater infilling rates. Using both global crater database and more local high resolution crater maps, we estimated crater obliteration rates on various Martian volcanic provinces.Our method proven efficient to track activity of the main Martian volcanic provinces. Resurfacing rates reach several thousands of m/Gy. Pic activity differs from provinces. Syrtis and Hesperia are the oldest with the highest and oldest observed rates around 3.7 Gy. The activity of those provinces quickly decreases reaching few hundreds of m/Gy around 3.4 Gy. During Hesperian, Tharsis is the most active surface of Mars with high resurfacing until 3.3 Gy. Finally, our result shows an increase of resurfacing, reaching few hundreds of m/Gy in Amazonis planitia from 2 Gy to present.
Published: 2021
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22. Mapping and characterisation of the Oxia Planum clay-bearing unit using CaSSIS imagery

Author: Nicolas Thomas, C. Quantin-Nataf, John Bridges, Jemima Briggs, Lucia Mandon, Adam Parkes Bowen, Livio L. Tornabene, and Gabriele Cremonese
Subjects: Bearing (mechanical), biology, law, Planum temporale, Cassis, Mineralogy, biology.organism_classification, Geology, law.invention
Abstract: Current knowledge of the clay unit at Oxia Planum, the Rosalind Franklin rovers landing site, is based in large part on spectroscopy data from the OMEGA and CRISM instruments. While these instruments have proved useful for creating a broad map of this unit, along with identifying candidates for the clay making up the unit, their usefulness is limited by their spatial resolution. Mapping at Oxia has primarily been carried out using 1200-300m/pixel OMEGA or 200-100m/pixel CRISM data and, even accounting for the intermittent 18m/pixel CRISM hyperspectral data available, existing clay maps are insufficient for the purposes of rover traverse planning.Images from the Colour and Stereo Surface Imaging System1 (CaSSIS), which has a resolution of 4m/pixel, can improve upon this. Work done by members of the CaSSIS science team identified certain CaSSIS band ratios which can aid in identifying the presence of ferric/ferrous minerals2. In a more recent study CRISM, HiRISE colour and CaSSIS data were used to identify that at least two spectrally and morphologically distinct subunits make up the Oxia clay unit3. These sub units are divided into a lower and upper member. The lower member appears orange in CaSSIS/HiRISE VNIR images, shows extensive metre-scale fracturing and possesses CRISM spectral signatures consistent with the presence of a Fe/Mg-rich clay mineral. The upper member, blue in CaSSIS/HiRISE VNIR images, shows metre-decametre scale fracturing along with CRISM spectral signatures consistent with a mix of a Fe/Mg-rich clay mineral and olivine.This work demonstrates that ferric detections within CaSSIS band ratios correlate well with CRISM, and that the lower clay member appears to have a higher ferric content than the upper member. Given this a new, higher resolution clay map is being created using CaSSIS band ratios in conjunction with HiRISE greyscale imagery to observe fracture size. This map, currently being constructed over the 1-sigma landing ellipses, delineates between the two subunits well in addition to revealing those areas where the two subunits are too intermixed to reliably differentiate at CaSSIS’s resolution. Given that CaSSIS has higher resolution in comparison to the CRISM/OMEGA instruments, that it can differentiate between the clay sub-units, and that it provides higher landing site coverage compared to CRISM hyperspectral data, means this map will provide a significant improvement over what is currently available for the sites clay unit.References; 1; Thomas N. et al. (2017). "The Colour and Stereo Surface Imaging System (CaSSIS) for the ExoMars Trace Gas Orbiter." Space Science Reviews 212(3-4): 1897-1944. 2; Tornabene L. L. et al. (2017). "Image Simulation and Assessment of the Colour and Spatial Capabilities of the Colour and Stereo Surface Imaging System (CaSSIS) on the ExoMars Trace Gas Orbiter." Space Science Reviews 214(1). 3; Mandon L. et al. (in review). "Spectral Diversity and Stratigraphy of the Clay-Bearing Unit at the Exomars 2020 Landing Site Oxia Planum." AstrobiologyAcknowledgement; CaSSIS is a project of the University of Bern, with instrument hardware development supported by INAF/Astronomical Observatory of Padova (ASI-INAF agreement n.2020-17-HH.0), and the Space Research Center (CBK) in Warsaw.
Published: 2021
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23. Initial results of the first visible and near-infrared spectrometer on the Martian surface: SuperCam unveils Jezero crater’s ground mineralogy

Author: Clément Royer, Pierre Beck, Lucia Mandon, P. Bernardi, Sylvestre Maurice, Francois Poulet, Olivier Forni, C. Quantin-Nataf, Thierry Fouchet, Jean-Michel Reess, Ann Ollila, Olivier Gasnault, Cedric Pilorget, Raymond Newell, Jeffrey R. Johnson, and Roger C. Wiens
Subjects: Impact crater, Martian surface, Near infrared spectrometer, Mineralogy, Geology
Published: 2021
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24. The geography of Oxia Planum

Author: C. Quantin-Nataf, Gabriele Cremonese, Laetitia Le Deit, Peter Fawdon, Adam Parks-Bowen, Peter Grindrod, Matthieu Volat, N. Thomas, Andrea Nass, C. Orgel, Joel Davis, Elliot Sefton-Nash, Matthew R. Balme, Alessandro Frigeri, Jorge L. Vago, Damien Loizeau, Solmaz Adeli, and Ernst Hauber
Subjects: oxia planum, G3180-9980, cassis, Data products, Planum temporale, Geography, Planning and Development, Context (language use), Mars Exploration Program, geography, Panchromatic film, Geography, ctx dem, exomars, Maps, Earth and Planetary Sciences (miscellaneous), mars, Digital elevation model, Scale (map), Cartography, High Resolution Stereo Camera
Abstract: We present the geography of Oxia Planum, the landing site for the ExoMars 2022 mission. This map provides the planetary science community with a framework to understand this, until recently, unexplored area. The map comprises (1) a mosaic of the panchromatic Context Camera (CTX) Digital Elevation Models (DEM) and Ortho Rectified Images (ORI) controlled to the High Resolution Stereo Camera (HRSC) multiorbit Digital Elevation Models (DEM) and (2) a mosaic of Colour and Stereo Surface Imaging System (CaSSIS) synthetic colour data products, registered to the CTX ORI mosaic. We define a grid of exploration quadrangles (quads) and an informal group of geographic regions to describe Oxia Planum. These regions bridge the scale gap between features observed on large areas (��100s km2) and the local geography (10s km2) relevant to the Rosalind Franklin rover��s operations in Oxia Planum.
Published: 2021

25. Providing unbiased IR spectra on Mars: the ground calibration of the infrared spectrometer onboard Perseverance rover

Author: Cedric Pilorget, Jeffrey R. Johnson, Jean-Michel Reess, C. Quantin-Nataf, Clément Royer, Lucia Mandon, Ann Ollila, Olivier Forni, Raymond Newell, Sylvestre Maurice, P. Bernardi, Thierry Fouchet, Pierre Beck, Olivier Gasnault, Roger C. Wiens, and Francois Poulet
Subjects: Materials science, Calibration, Infrared spectroscopy, Mars Exploration Program, Remote sensing
Published: 2021
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26. Spectral endmember variability on hyperspectral datasets of a Martian meteorite - Implications for planetary surfaces

Author: Pierre Beck, Lu Pan, Mélissa Martinot, C. Quantin-Nataf, L. Mandon, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and 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
Subjects: Martian, Endmember, Opacity, Mineralogy, Hyperspectral imaging, Mars, Astronomy and Astrophysics, Context (language use), Spectral line, Physics::Geophysics, Surface, Meteorite, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Radiative transfer, Astrophysics::Earth and Planetary Astrophysics, Geology, Spectroscopy, Meteorites
Abstract: International audience; Visible-near-infrared reflectance spectra reveal clues about the mineralogy and composition of planetary surfaces. In most cases, light interacts with a mixture of various components on planetary surfaces. While radiative transfer models have been developed to simulate mixture in particulate surfaces, the extent to which spectral features represent the bulk composition of rock remains unclear. In this study, we present the analysis of a new dataset with hyperspectral imaging of rock slabs at different resolutions to characterize the scaling of spectral data. We address the problem of spectral mixing with high-resolution imaging of Martian meteorite NWA480 at a microscopic scale. The linear combination of each pixel provide an approximate to the rock's bulk spectra. However, we find the impurities, fractures and zoning create wide spectral variability in the mineral crystals. In addition, the widespread opaque minerals may also darken the spectra, resulting in non-unique interpretation of the bulk spectra. These complexities in the natural samples prevent an accurate mineral abundance retrieval using unmixing algorithms with select spectral endmembers. We suggest applying recently developed algorithms on unmixing with spectral variability with the consideration of the petrologic context would be necessary to improve the quantitative analysis of planetary surfaces.
Published: 2021
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27. Local topography effects on the surface temperatures on Mars - Application to the case of Recurring Slope Lineae (RSL)

Author: Maxime Enjolras, C. Quantin-Nataf, C. Millot, Cedric Leyrat, 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 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, and 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)
Subjects: Martian, Morphology, Modern Mars, Temperatures, Topography, 010504 meteorology & atmospheric sciences, RSL, Astronomy and Astrophysics, Context (language use), Mars Exploration Program, 01 natural sciences, Impact crater, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, High spatial resolution, 010303 astronomy & astrophysics, Geomorphology, Geology, 0105 earth and related environmental sciences
Abstract: International audience; Recurring Slope Lineae (RSL) are dark linear recurrent features which incrementally lengthen and fade each year on Martian slopes. Their activity during warmest seasons rises the question of modern martian water related process. To investigate this question, this study focuses on the thermal context of slopes hosting RSL. The paper presents a numerical study of surface and subsurface temperatures at high spatial resolution (1 m/pix) of three well-described RSL sites: Palikir Crater, Coprates Chasma and Rauna Crater. We then compare our local thermal simulations to quantitative measurements of the length and timing of RSL lengthening and fading in these three sites. We underline that RSL sites surface temperatures are poorly correlated with RSL morphology's changes. Indeed, lineae lengthening occurs while surface temperature are under the melting point of pure water (273 K) for at least two sites: Coprates Chasma and Rauna Crater, for two different sets of surface physical properties. We also highlight the significant differences in temperature range while lengthening occurs for all the sites, from ~220 K in Coprates Chasma site to a maximum of ~300 K in Palikir Crater. RSL are sometimes associated with signals in topography, involving significant heating variations of the surface, which can yield to the formation of local winds. Facing the thermal inconsistency between wet triggering processes and RSL reported activity, we suggest that RSL are more probably dry processes.
Published: 2021
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28. Initial results of Mars2020: characterization of the geological context of the future samples of Mars Sample return

Author: Nicolas Mangold, C. Quantin-Nataf, Adrian J. Brown, Kenneth H. Williford, Kenneth A. Farley, and Kathryn M. Stack
Subjects: Mars sample return, Earth science, Context (language use), Geology, Characterization (materials science)
Published: 2021
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29. Deposition and erosion of a Light-Toned Yardang-forming unit of Mt Sharp, Gale crater, Mars

Author: Horton E. Newsom, C. Quantin-Nataf, Jérémie Lasue, L. A. Scuderi, Sylvestre Maurice, S. Le Mouélic, William Rapin, Patrick Pinet, Olivier Gasnault, N. Mangold, L. Le Deit, Roger C. Wiens, Gilles Dromart, D. M. Rubin, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), 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 Sciences [Santa Cruz], University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), The University of New Mexico [Albuquerque], Los Alamos National Laboratory (LANL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UCSC), University of California-University of California, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA)
Subjects: 010504 meteorology & atmospheric sciences, Stratigraphy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Context (language use), 010502 geochemistry & geophysics, 01 natural sciences, Yardang, Paleontology, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Impact crater, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Eolian, [SDU.STU.GM]Sciences of the Universe [physics]/Earth Sciences/Geomorphology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, geography, geography.geographical_feature_category, Stack (geology), Mars Exploration Program, 15. Life on land, Mars Climate, Gale Crater, Geophysics, Erg (landform), 13. Climate action, Space and Planetary Science, ChemCam, [SDU.STU.ST]Sciences of the Universe [physics]/Earth Sciences/Stratigraphy, Hesperian, Aeolian processes, Geology
Abstract: International audience; Gale crater is a large impact crater with a ca 5 km thick sequence of stratified rocks in it, expressed today as a central eroded mound (i.e., Aeolis Mons informally named Mt. Sharp). A goal of the current Mars Science Laboratory mission in Gale crater is to investigate the processes that deposited, lithified, and eroded this fill. The Light-Toned Yardang Unit (LTYu) unit, the subject of the present research, is one of the geological units of Mt Sharp. Our specific purpose here is to refine and interpret the imaging documentation of the morphologic and stratal components of the LTYu, at large outcrop scale. In combination with established orbital images, we use the Remote Micro-Imager (RMI) of ChemCam, a remote sensing instrument currently operated onboard Curiosity rover, which provides several types of context imaging. RMI capabilities now include “Long Distance” acquisitions of targets several kilometers away. In these new acquisitions, substantial differences are visible in LTYu yardang attitudes from lowest to uppermost elevations allowing tentative subdivision of the LTYu into subunits. Bedding geometries in the lower LTYu are consistent with eolian dune foresets which collectively prograde towards an average N134° direction. Based on stratal architectures, the LTYu is viewed as an amalgamated stack of at least two, and possibly four, ancient erg systems bounded by large deflationary “supersurfaces”. Observations point to a multistory generation of yardangs interpreted to have been successively buried during the stratigraphic building of Mt Sharp. We conclude that the successive sequences of eolian deposition-erosion recorded by the LTYu have been generated by cyclic changes from semi-arid to arid conditions, coupled in climatic cycles, including wind regime change. The regional unconformity that tops the Lower mound formation of Mt Sharp, and the subsequent emplacement of the LTYu, collectively express a clear tendency toward sustained arid environments for this region of Mars around the Early – Late Hesperian transition. Given the large time scale involved (i.e., a few tens of million years as a minimum), we consider it likely that the local evidence for increased aridity in the Mt Sharp stratigraphy is a manifestation of climate change affecting the whole planet.
Published: 2021
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30. Estimating crater obliteration rate through crater depth statistics

Author: Lu Pan, Sylvain Breton, and C. Quantin-Nataf
Subjects: Impact crater, Geomorphology, Geology, Crater depth
Abstract: Introduction Impact craters are widely used to investigate the geologic history of planetary surfaces. For example, their morphology bears clues on past surfaces processes that affected the surface such as erosion, sedimentary deposit and volcanic processes. One of the most interesting use of impact craters is the dating of planetary surfaces using their size frequency distribution (Hartmann and Neukum 2001; Stöffler and Ryder 2001; Young 1940). This method has been used in almost every study that provide an age for geologic bodies other than Earth. If lunar crater size frequency distributions are most often pristine, craters on many other bodies are degraded over time. Hence crater size frequency distributions often present a depletion of small craters compared to the lunar ones. Mars is a good example of this phenomenon that has been named Opik effect (Opik 1966). Taking into account crater degradation when dating planetary surface will not only improve this method, but also provides new insights into the geological processes which resulted in the crater degradation. In this study we combine statistic and morphology of craters in order to investigate the timing and intensity of surface processes. We introduce the notion of crater size and depth frequency distributions, adding a dimension to classic size and depth frequency distribution. Using crater chronology models, those crater size and depth frequency distributions can be interpreted in term of crater depth depletion speed that we refer as crater obliteration. Method Craters populations are already widely referenced. On Mars, Robbins & Hynek, 2012 proposed a huge crater database that they estimate complete down to 1 km of diameter. In this database, most craters above 6 km of diameter are provided with a morphology. We computed crater depth from the elevation of the floor and the median elevation of the rims. Crater size and depth frequency distribution are then constructed using probability density distribution as recommended by Robbins et al., 2018. Each crater is convoluted by a 2D gaussian determined by the analytical error on the measured depth and diameter. Assuming that the deepest craters are the freshest ones, we used crater chronology models (Ivanov 2001; Neukum, Ivanov, and Hartmann 2001) to associate a depth for each diameter and age (Figure 1). For each diameter, we then derivate depth according to age to compute obliteration. We observe strong noise at the limit of the distribution, that cause an increase in computed obliteration for recent ages. This is caused by the spreading of the crater size and depth frequency distribution beyond the observed craters as a result of convolution. To remove this bias, we only keep obliterations measured when the model number of crater is more than 5. Results From Robbins & Hynek, 2012 crater databases, we computed crater size and depth frequency distribution for geologic areas of Mars simplified from the geologic map of Tanaka et al., 2014. We computed obliteration rates from those We presents here the obliterations rates obtained for 3 Martian geologic areas, namely the Southern Highland, Tharsis Province and the Hesperian lowlands, that illustrate our main results. Only the most cratered surfaces, such as the Southern Highlands present a number of craters large enough to investigate Noachian obliteration rates (Figure 2). During this era, obliteration rates reach several thousands m/Gy, but rapidly decrease during early Hesperian and are close to 0 during Amazonian. Volcanic provinces such as Tharsis, Isidis and Elysium present obliterations rates more important than the rest of the planet during Hesperian. This suggest that our method is sensitive to volcanic activity. We show here the example of the province of Tharsis (Figure 3), where obliteration rates decreased slower than on the rest of the planet, suggesting a persistence of volcanic activity until early Amazonian. Northern lowlands witness Amazonian obliteration rates one order of magnitude higher than the rest of the planet (Figure 4). This observation is still under further investigation, but may suggest a continuous emplacement of geologic material during middle Amazonian which may be related to Vastitas Borealis Formation. We have developed a new method to model crater distribution and degradation taking into account of the size and depth of impact craters. Using this model, we were able to retrace the variations of crater obliteration through Martian era, and provide insight into the geological processes dominating crater degradation. The method with additional inputs from crater depths provides novel insights into the geological processes dominating crater degradation at different epochs in Martian history. Combined with higher resolution datasets, this method has potential to be applied to understand regional geological processes on Mars and other planetary bodies. Bibliography Hartmann, William K., and Gerhard Neukum. 2001. “Cratering Chronology and the Evolution of Mars.” Space Science Reviews 96(1–4): 165–94. Ivanov, Boris A. 2001. “Mars/Moon Cratering Rate Ratio Estimates.” Space Science Reviews (November 2000). Neukum, Gerhard, Boris A. Ivanov, and William K. Hartmann. 2001. “Cratering Records in the Inner Solar System in Relation to the Lunar Reference System.” Space Science Reviews 96(1–4): 55–86. Opik, E. J. 1966. “The Martian Surface.” Science 153(3733): 255–65. http://www.sciencemag.org/cgi/doi/10.1126/science.153.3733.255. Robbins, Stuart J. et al. 2018. “Revised Recommended Methods for Analyzing Crater Size-Frequency Distributions.” Meteoritics and Planetary Science 53(4): 891–931. Robbins, Stuart J., and Brian M. Hynek. 2012. “A New Global Database of Mars Impact Craters ≥1 Km: 1. Database Creation, Properties, and Parameters.” Journal of Geophysical Research E: Planets 117(5): 1–18. Stöffler, D., and G Ryder. 2001. “Stratigraphy and Isotope Ages of Lunar Geologics Units: Chronological Standard for the Inner Solar System.” : 9–54. Tanaka, Kenneth L. et al. 2014. “Geologic Map of Mars.” USGS. Young, J. 1940. “A Statistical Investigation of Diameter and Distribution of Lunar Craters.” Journal of the British Astronomical Association.
Published: 2020
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31. Assessing slope precision from numerical propagation of DEM (Digital Elevation Model) vertical errors

Author: C. Quantin-Nataf, C. Millot, and Cedric Leyrat
Subjects: Digital elevation model, Geodesy, Geology
Abstract: Digital Elevation Models (DEM) are widely used tools in planetary sciences. Geometric parameters such as pixel orientations and local slopes can be derived from these DEM. However, as any data, DEM have a limited precision (i.e. errors), which yields to the propagation of errors on geometric parameters. Assessing local slopes is necessary for many morphological studies: then, how do the DEM vertical errors propagate on the slope values? To answer to this question, we develop a simple and fast numerical method based on the addition of noise on synthetic DEM. We evaluate the different components of slope errors to define the relationship between input DEM noise and output slope errors. Results can be used as first order estimations to discuss slope maps precision.
Published: 2020
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32. MarsSI: Martian surface data processing service

Author: Matthieu Volat, Patrick Thollot, C. Quantin-Nataf, and Lucia Mandon
Subjects: Service (business), Data processing, Martian surface, Environmental science, Remote sensing
Abstract: MarsSI (“Mars Système d’Information”, french for Mars Information System) is a platform and service to catalog, process and retrieve data from orbiters. https://marssi.univ-lyon1.fr/MarsSI. 1. Introduction Geological investigations of planetary surfaces require the combination of orbital datasets. Missions being often multiple-instruments platforms from multiple space agencies, the quantity of data available increased quickly. MarsSI [3] is a platform designed to explore, calibrate, process and retrieve Mars orbital data. It was certified in 2017 as french national Research Infras- tructure by the Centre National de la Recherche Scientifique (CNRS) as part of the Planetary Surface Portal (PSUP) [2]. As of 2020, it indexes the optical (visible, multi and hyper-spectral) data from the recent orbiter missions, and allow to request the creation of Digital Elevation Models on demand. The focus, as highlighted by figure 1 is to allow the user to browse and request ”ready-to-use” products in regards of calibration, refinements and georeferencing. The user will be able to visualize and interpret the data in GIS or remote sensing software. 2 Architecture MarsSI’s hardware is hosted at the Université Lyon 1 and is composed of a frontend server, a storage bay and a 80 core cluster. The software stack heavily relies on the OGC-defined standards for interoperability between components. 2.1 Catalog MarsSI retrieve the footprints provided by the NASA Planetary Data System (PDS) in a database. These footprint information, alongside rasters that will be used as layers of our map display, is made available through a Mapserver instance. One issue we faced is the lack of Coordinates Referencing Systems definitions readily available in the WMS/WFS protocols, who rely on EPSG definitions codes. Adding and using non-standard EPSG definitions was a workaround to this issue. Once the catalog, we proceed over the CTX and HiRISE data collections to find for each dataset overlapping images by at least 60% and a maximum differ- ence of acquisition angle of 10° to generate a list of potential Digital Elevation Models (DEMs). 2.2 Pipelines Alongside the catalog, MarsSI uses several processing pipelines. Those pipelines defines steps and procedures to fetch, calibrate and refine products. A notable pipeline is the use of the Ames Stereo Pipeline [1] software to generate on- demand DEMs. The pipeline execution is managed using the OAR (oar.imag.fr) batch scheduler. One design choice of MarsSI was to present the products, including those created by the service, as global to all users (in contrast to service creating user-specific products). This was done to have only one reference to products like generated DEMs and reduce storage use. As a result, we only designed fully automated pipelines. 2.3 Frontend MarsSI client interface is a web component based on Geomajas (www.geomajas. org), a free and open source GIS toolkit. Geomajas interface directly with the mapserver instance and provide widget for the main interface, shown on figure 3. 3 Usage and data volumes MarsSI is open to the scientific communities around the world. As of june 2020, we count 294 registered users across more than 128 institutes. Storage-wise, we benefited to progressively download data as requested, reaching 34To in 2020. 4 Perspectives We are currently working on integrating other data types in MarsSI, such as the MARSIS and SHARRAD radar datasets. Another aspect we are working on is a more eﬀicient and intuitive web in- terface not based on Geomajas. The rewrite would also take into account other maps such as polar projections and other planetary bodies. As DEMs are our most requested products, we are investigating how to pro- vide qualitative assessment for those datasets. We are also looking for methods to generate large scale DEMs using mosaicking. 5 Conclusion Built upon frameworks using standardized protocols, MarsSI offers the scientific communities a way to search and request data, most notably DEMs that can be derived from CTX and HiRISE data collection. We are now looking to modernize and extend the service with a newer interface that can present other planets and moons data. Acknowledgments MarsSI is a national Research Infrastructure, recognised as such by the French Ministry of Higher Education and Research. It was supported by the Pro- gramme National de Planétologie (PNP) of CNRS/INSU, co-funded by CNES. It was initialy supported by the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013)/ERC Grant agreement No.280168. References [1] Zachary M Moratto et al. “Ames Stereo Pipeline, NASA’s open source automated stereogrammetry software”. In: Lunar and Planetary Science Conference. Vol. 41. 2010, p. 2364. [2] François Poulet et al. “PSUP: A Planetary SUrface Portal”. In: Planetary and Space Science 150 (2018), pp. 2–8. [3] C. Quantin-Nataf et al. “MarsSI: Martian surface data processing informa- tion system”. In: Planetary and Space Science 150 (2018), pp. 157 –170. issn: 0032-0633. doi: https://doi.org/10.1016/j.pss.2017.09. 014. url: http://www.sciencedirect.com/science/article/pii/ S0032063316304718.
Published: 2020
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33. Mineralogical survey of the anorthositic Feldspathic Highlands Terrane crust using Moon Mineralogy Mapper data

Author: W. van Westrenen, Jessica Flahaut, Sebastien Besse, C. Quantin-Nataf, M. Martinot, Geology and Geochemistry, Earth Sciences, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Centre 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), European Space Astronomy Centre (ESAC), European Space Agency (ESA), Vrije Universiteit Amsterdam [Amsterdam] (VU), 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 Agence Spatiale Européenne = European Space Agency (ESA)
Subjects: 010504 meteorology & atmospheric sciences, Mineralogy, Astronomy and Astrophysics, Crust, Pyroxene, Moon Mineralogy Mapper, engineering.material, 01 natural sciences, Impact crater, 13. Climate action, Space and Planetary Science, Homogeneous, 0103 physical sciences, engineering, Plagioclase, Mafic, Ejecta, 010303 astronomy & astrophysics, Geology, Feldspathic Highlands Terrane, Spectroscopy, 0105 earth and related environmental sciences, Terrane, [SDU.STU.MI]Sciences of the Universe [physics]/Earth Sciences/Mineralogy
Abstract: International audience; Spectroscopic data from the Moon Mineralogy Mapper (M 3) instrument are used to study the mineralogy of the central peak or peak ring of 75 craters located in the lunar anorthositic Feldspathic Highlands Terrane (FHT-a), as defined by Jolliff et al. (2000). The thickness of South-Pole Aitken (SPA) ejecta at the location of the selected craters is estimated. Crustal thickness models are used with empirical cratering equations to estimate the depth of origin of the material excavated in the studied central peaks, and its distance to the crust-mantle interface. The goal of this survey is to study the composition of the FHT-a crust, and the extent of its potential lateral and vertical heterogeneities. High-Calcium Pyroxene (HCP) and featureless spectra are mostly detected throughout the entire FHT-a, whereas the number of pure plagioclase detections is small. No relationship between the central peak composition and the distance to SPA or the depth within the SPA ejecta is observed. The SPA ejecta material cannot be spectrally distinguished from crustal material. We interpret the paucity of plagioclase spectra in the FHT-a, which contrasts with more frequent plagioclase detections in the central peaks of craters sampling the crust in younger lunar terranes using identical spectroscopic techniques Martinot et al. (2018b), as a possible effect of terrane maturation, or of mixing with mafic components that mask their signature in the visible near-infrared. Overall, the FHT-a appears homogeneous laterally. However, data hint at a pyroxene compositional change with increasing depth, from high-calcium content in the upper crust towards less calcic compositions with increasing depth, which is consistent with prior studies of the architecture of the lunar crust.
Published: 2020
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34. Mineralogical Diversity and Geology of Humboldt Crater Derived Using Moon Mineralogy Mapper Data

Author: M. Martinot, L. Lozac'H, Jessica Flahaut, Sebastien Besse, W. van Westrenen, and C. Quantin-Nataf
Subjects: geography, geography.geographical_feature_category, Felsic, 010504 meteorology & atmospheric sciences, Pluton, Mineralogy, Crust, engineering.material, 01 natural sciences, Geophysics, Impact crater, Volcano, Space and Planetary Science, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), engineering, Plagioclase, Mafic, Ejecta, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract: Moon Mineralogy Mapper (M3) spectroscopic data and high-resolution imagery data sets were used to study the mineralogy and geology of the 207 km diameter Humboldt crater. Analyses of M3 data, using a custom-made method for M3 spectra continuum removal and spectral parameters calculation, reveal multiple pure crystalline plagioclase detections within the Humboldt crater central peak complex, hinting at its crustal origin. However, olivine, spinel, and glass are observed in the crater walls and rims, suggesting these minerals derive from shallower levels than the plagioclase of the central peak complex. High-calcium pyroxenes are detected in association with volcanic deposits emplaced on the crater's floor. Geologic mapping was performed, and the age of Humboldt crater's units was estimated from crater counts. Results suggest that volcanic activity within this floor-fractured crater spanned over a billion years. The felsic mineralogy of the central peak complex region, which presumably excavated deeper material, and the shallow mafic minerals (olivine and spinel) detected in Humboldt crater walls and rim are not in accordance with the general view of the structure of the lunar crust. Our observations can be explained by the presence of a mafic pluton emplaced in the anorthositic crust prior to the Humboldt-forming impact event. Alternatively, the excavation of Australe basin ejecta could explain the observed mineralogical detections. This highlights the importance of detailed combined mineralogical and geological remote sensing studies to assess the heterogeneity of the lunar crust.
Published: 2018
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35. Identification and characterization of new feldspar-bearing rocks in the walls of Valles Marineris, Mars

Author: C. Quantin-Nataf, Marie Barthez, Jessica Flahaut, Frank Fueten, Martin Guitreau, Pascal Allemand, and Vincent Payet
Subjects: Bearing (mechanical), law, visual_art, visual_art.visual_art_medium, Geochemistry, Identification (biology), Mars Exploration Program, Feldspar, Geology, Characterization (materials science), law.invention
Abstract: VNIR spectroscopy has previously led to many discoveries pertaining to Mars geologic history (e.g., the discovery of hydrated minerals associated to ancient terrains with OMEGA, Bibring et al., 2006). Plagioclase feldspar minerals can also be identified with spectroscopic techniques thanks to a 1.3 microns absorption in the VNIR domain (e.g., Adams and Goullaud, 1978). Previous lunar analog studies show however that when mixing powders of Ca plagioclase and a mafic component (olivine or pyroxene), the feldspars absorption band is quickly masked (e.g., Cheek and Pieters, 2014). This study further demonstrates that the 1.3 micron feature is only detectable if the plagioclase abundance is > 90 %. Based on this observation, previous feldspar absorptions on Mars have been interpreted as evidence for nearly pure anorthositic rocks (e.g., Carter and Poulet, 2013). A recent study by Rogers and Nekvasil (2015) however suggests that phenocryst basalts with less than 90% plagioclase could reproduce the 1.3 micron feature if large crystals are involved, although no whole rock measurements were made.In the present study, we describe new feldspar signatures detected with the CRISM VNIR spectral-imager in the walls of the Valles Marineris grand canyon, on Mars. The associated rock textures and elevations were assessed from CTX and HiRISE images and DTMs. In parallel, we are collecting VNIR spectra of various (uncrushed) terrestrial rocks containing a large range of feldspar abundances and grain sizes. Analyses are carried out between 0.35 and 2.5 microns with an ASD Fieldspec at CRPG Nancy, France, and will be presented at the conference time. By combining laboratory measurements of a range of possible terrestrial analog rocks with the study of Mars feldspar-bearing outcrops, we should bring more clues on the nature and origin of these feldspathic rocks.
Published: 2020
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36. Refining the age, emplacement and alteration scenarios of the olivine-rich unit in the Nili Fossae region, Mars

Author: N. Mangold, C. Quantin-Nataf, Gilles Dromart, Pierre Beck, Erwin Dehouck, L. Lozac'h, L. Mandon, Sylvain Breton, Matthieu Volat, C. Millot, Patrick Thollot, 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 Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de 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 Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)
Subjects: geography, geography.geographical_feature_category, Olivine, 010504 meteorology & atmospheric sciences, Bedrock, Geochemistry, Noachian, Pyroclastic rock, Astronomy and Astrophysics, Crust, Volcanism, Mars Exploration Program, engineering.material, 01 natural sciences, Impact crater, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, engineering, 010303 astronomy & astrophysics, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: The Nili Fossae region of Mars exhibits from remote sensing spectral data the largest exposures of olivine-rich materials on the planet. However, it is not clearly constrained how and when these terrains formed. Some of the proposed scenarios favor a mode of formation closely related to Isidis impact basin: either under intense effusive volcanism following the impact, from cooling of an immediate impact melt sheet or silicate impact vapor condensate. These deposits might also be pyroclastic products ejected from now eroded or buried vents. Recent studies also proposed that lag deposits could be responsible for enrichment in olivine after deposition. In this contribution, we mapped the olivine-rich unaltered and altered bedrock exposures using near infrared and thermal inertia data, investigated the geometry and key contacts of the olivine-rich unit, and determined its surface age using crater counts and stratigraphical relationships. We find that the olivine-rich bedrock extends over at least ~18,000 km2 in the Nili Fossae region, with a large part of it being unaltered. Olivine-rich material that overlaps the northern rim of Jezero crater corresponds to a primary deposit (i.e. rather than reworked material). Since this crater is younger than Isidis, we favor the hypothesis of a post-Isidis origin, rather than the impact melt (consistently with Bramble et al., 2017) and impact condensate origin. Based on our observations and crater counts, we estimate an emplacement age of 3.82 ± 0.07 Ga (Mid to Late Noachian). We discuss the origin of the unit, with the most likely scenarios being ash falls and/or pyroclastic surges. To explain the circum-Isidis distribution of these deposits, we favor the hypothesis of a thinned and weakened crust in the region subsequently to the giant impact of Isidis, as suggested by Tornabene et al. (2008). Finally, the distribution of altered bedrock conflicts with the contact metamorphism scenario. As the olivine-rich unit exposed at Jezero crater, future home of the Mars 2020 rover, is a regional stratigraphic marker, return samples for precise dating of this unit should be made one of the major mission targets.
Published: 2020
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37. Decline of crater obliteration rates during early martian history

Author: F. Dubuffet, L. Lozac'h, M. Martinot, C. Quantin-Nataf, Robert A. Craddock, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and 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)
Subjects: Martian, 010504 meteorology & atmospheric sciences, Global climate, Earth science, Noachian, Climate change, Astronomy and Astrophysics, Mars Exploration Program, 01 natural sciences, Impact crater, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Erosion, Hesperian, 010303 astronomy & astrophysics, Geology, 0105 earth and related environmental sciences
Abstract: A change in the global climate on early Mars is suspected from the geologic evidence of warmer wetter conditions that prevailed during the Noachian but stands in contrast to the dry and cold conditions observed currently. However, the timing and evolution of this climatic change represents a gap in our understanding of the history of Mars. Here, we document the time-dependence of the crater obliteration rates on Mars that decreased continuously between 3.8 Ga and 3 Ga. Our results indicate that the erosion responsible for crater modification and obliteration declined gradually through the Noachian and into the Hesperian periods. These results suggest that the climatic conditions also changed gradually and the amount of water available on the surface of Mars slowly decreased over time.
Published: 2019
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38. Crater Statistics on the Dark-Toned, Mafic Floor Unit in Jezero Crater, Mars

Author: Timothy A. Goudge, Caleb I. Fassett, Cecillie P. Knudsen, Stephanie Shahrzad, D. H. Needham, C. Quantin-Nataf, Kjartan M. Kinch, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and 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)
Subjects: 010504 meteorology & atmospheric sciences, Mars 2020, Geochemistry, Mars, Mars Exploration Program, 01 natural sciences, Crater counting, Jezero crater, Geophysics, age, Impact crater, [SDU]Sciences of the Universe [physics], 0103 physical sciences, General Earth and Planetary Sciences, crater counting, Mafic, 010303 astronomy & astrophysics, Geology, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: International audience
Published: 2019
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39. Compositional Variations in the Vicinity of the Lunar Crust-Mantle Interface From Moon Mineralogy Mapper Data

Author: M. Martinot, Jessica Flahaut, Sebastien Besse, W. van Westrenen, C. Quantin-Nataf, 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), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Faculty of Earth and Life Sciences, University of Amsterdam [Amsterdam] (UvA), 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), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Netherlands Organization for Scientific Research (NWO) Vici grant, User Support Space Research grant from the Netherlands Space Office (NSO), APR-CNES Luna, European Project: 280168,EC:FP7:ERC,ERC-2011-StG_20101014,E-MARS(2011), Geology and Geochemistry, and Earth Sciences
Subjects: spectroscopy, 010504 meteorology & atmospheric sciences, crust‐mantle interface, Mineralogy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Pyroxene, engineering.material, 01 natural sciences, Spectral line, Mantle (geology), Impact crater, Geochemistry and Petrology, 0103 physical sciences, Earth and Planetary Sciences (miscellaneous), Plagioclase, Spectroscopy, 010303 astronomy & astrophysics, Planetary Sciences: Solid Surface Planets, Research Articles, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Mineralogy and Petrology, crust-mantle interface, Olivine, central peak, Crust, proximity value, Planetology, peak ring, History of Geophysics, Planetary Mineralogy and Petrology, Geophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], engineering, mineralogy, Geology, Composition, Research Article
Abstract: Moon Mineralogy Mapper spectroscopic data were used to investigate the mineralogy of a selection of impact craters' central peaks or peak rings, in order to characterize the lunar crust‐mantle interface, and assess its lateral and vertical heterogeneity. The depth of origin of the craters' central peaks or peak rings was calculated using empirical equations, and compared to Gravity Recovery and Interior Laboratory crustal thickness models to select craters tapping within +10/−20 km of the crust‐mantle interface. Our results show that plagioclase is widely detected, including in craters allegedly sampling lower crustal to mantle material, except in central peaks where Low‐Calcium Pyroxene was detected. Olivine detections are scarce, and identified in material assumed to be derived from both above and below the crust‐mantle interface. Mineralogical detections in central peaks show that there is an evolution of the pyroxene composition with depth, that may correspond to the transition from the crust to the mantle. The correlation between High‐Calcium Pyroxene and some pyroxene‐dominated mixture spectra with the location of maria and cryptomaria hints at the existence of lateral heterogeneities as deep as the crust‐mantle interface., Key Points Plagioclase is widely detected in the central peaks of craters allegedly sampling the lower crust or mantle, except where LCP is observedLateral heterogeneities at the crust‐mantle interface and a pyroxene compositional evolution with depth (from HCP to LCP) were observedThis study's mineralogical observations support the GRAIL crustal thickness model 1 better than the model 3
Published: 2018
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40. Quantifying widespread aqueous surface weathering on Mars: The plateaus south of Coprates Chasma

Author: Loic Lozac'H, C. Quantin-Nataf, Jessica Flahaut, P. Thollot, C. Millot, John Carter, Damien Loizeau, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and 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)
Subjects: geography, Plateau, geography.geographical_feature_category, 010504 meteorology & atmospheric sciences, Geochemistry, Noachian, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Astronomy and Astrophysics, Weathering, Mars Exploration Program, 01 natural sciences, Head (geology), Pedogenesis, Impact crater, Space and Planetary Science, [SDU]Sciences of the Universe [physics], 0103 physical sciences, Erosion, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: Pedogenesis has been previously proposed on the plateaus around Coprates Chasma, Valles Marineris to explain the presence of widespread clay sequences with Al-clays and possible hydrated silica over Fe/Mg-clays on the surface of the plateaus (Le Deit et al., 2012; Carter et al., 2015). We use previous observations together with new MRO targeted observations and DEMs to constrain the extent and thickness of the plateau clay unit: the Al-clay unit is less than 3 m thick, likely ∼1 m, while the Fe/Mg-clays underneath are few tens of meters thick. We also refine the age of alteration by retrieving crater retention ages of the altered plateau and of later deposits: the observed clay sequence was created by surface pedogenesis between model ages of 4.1 Ga and 3.75 Ga. Using a leaching model from Zolotov and Mironenko (2016), we estimate the quantity of atmospheric precipitations needed to create such a clay sequence, that strongly depends on the chemistry of the precipitating fluid. A few hundreds of meters of cumulated precipitations of highly acidic fluids could explain the observed clay sequence, consistent with estimates based on late Noachian valley erosion for example (Rosenberg and Head, 2015). We show finally that the maximum quantity of sulfates potentially formed during this surface weathering event can only contribute minimally to the volume of sulfates deposited in Valles Marineris.
Published: 2018
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41. PSUP: a Planetary SUrface Portal

Author: Chiara Marmo, Hervé Ballans, John Carter, C. Quantin-Nataf, Lucie Riu, J. Audouard, Francois Poulet, Loic Lozac'H, Antoine Séjourné, Brigitte Gondet, K. Dassas, Jean-Christophe Malapert, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), 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), 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), Centre National d’Études Spatiales [Paris] (CNES), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), and Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Planetary surface, Database, Computer science, business.industry, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Data management, Astronomy and Astrophysics, Mars Exploration Program, computer.software_genre, 01 natural sciences, Space exploration, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Data access, 13. Climate action, Space and Planetary Science, Martian surface, 0103 physical sciences, User interface, business, 010303 astronomy & astrophysics, computer, Interactive visualization, 0105 earth and related environmental sciences, Remote sensing
Abstract: International audience; The large size and complexity of planetary data acquired by spacecraft during the last two decades create a demand within the planetary community for access to the archives of raw and high level data and for the tools necessary to analyze these data. Among the different targets of the Solar System, Mars is unique as the combined datasets from the Viking, Mars Global Surveyor, Mars Odyssey, Mars Express and Mars Reconnaissance Orbiter missions provide a tremendous wealth of information that can be used to study the surface of Mars. The number and the size of the datasets require an information system to process, manage and distribute data. The Observatories of Paris Sud (OSUPS) and Lyon (OSUL) have developed a portal, called PSUP (Planetary SUrface Portal), for providing users with efficient and easy access to data products dedicated to the Martian surface. The objectives of the portal are: 1) to allow processing and downloading of data via a specific application called MarsSI (Martian surface data processing Information System); 2) to provide the visualization and merging of high level (image, spectral, and topographic) products and catalogs via a web-based user interface (MarsVisu), and 3) to distribute some of these specific high level data with an emphasis on products issued by the science teams of OSUPS and OSUL. As the MarsSI service is extensively described in a companion paper (Quantin-Nataf et al., companion paper, submitted to this special issue), the present paper focus on the general architecture and the functionalities of the web-based user interface MarsVisu. This service provides access to many data products for Mars: albedo, mineral and thermal inertia global maps from spectrometers; mosaics from imagers; image footprints and rasters from the MarsSI tool; high level specific products (defined as catalogs or vectors). MarsVisu can be used to quickly assess the visualized processed data and maps as well as identify areas that have not been mapped yet. It also allows overlapping of these data products on a virtual Martian globe, which can be difficult to use collectively. The architecture of PSUP data management layer and visualization is based on SITools2 ( Malapert and Marseille, 2012) and MIZAR (Module for Interactive visualiZation from Astronomical Repositories) respectively, two CNES generic tools developed by a joint effort between the French space agency (CNES) and French scientific laboratories. Future developments include the addition of high level products of Mars (regional geological maps, new global compositional maps…) and tools (spectra extraction from hyperspectral cubes). Ultimately, PSUP will be adapted to other planetary surfaces and space missions in which the French research institutes are involved.
Published: 2018
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42. MarsSI: Martian surface data processing information system

Author: Harold Clenet, B. Bultel, J. Fernando, F. Dubuffet, Pascal Allemand, A. Ody, L. Lozac'h, S. Harrisson, Patrick Thollot, Francois Poulet, D. Loizeau, C. Quantin-Nataf, Cedric Leyrat, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Interactions et dynamique des environnements de surface (IDES), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Sciences de la Terre (LST), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Dynamique terrestre et planétaire (DTP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Geographic information system, 010504 meteorology & atmospheric sciences, Computer science, Context (language use), computer.software_genre, 01 natural sciences, Martian surface, 0103 physical sciences, Information system, media_common.cataloged_instance, European union, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Remote sensing, media_common, [PHYS]Physics [physics], Data processing, Database, business.industry, Astronomy and Astrophysics, Pipeline (software), Data access, Space and Planetary Science, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], computer
Abstract: International audience; MarsSI (Acronym for Mars System of Information, https://emars.univ-lyon1.fr/MarsSI/) is a web Geographic Information System application which helps managing and processing martian orbital data. The MarsSI facility is part of the web portal called PSUP (Planetary SUrface Portal) developed by the Observatories of Paris Sud (OSUPS) and Lyon (OSUL) to provide users with efficient and easy access to data products dedicated to the martian surface. The portal proposes 1) the management and processing of data thanks to MarsSI and 2) the visualization and merging of high level (imagery, spectral, and topographic) products and catalogs via a web-based user interface (MarsVisu). The portal PSUP as well as the facility MarsVisu is detailed in a companion paper (Poulet et al., 2018). The purpose of this paper is to describe the facility MarsSI. From this application, users are able to easily and rapidly select observations, process raw data via automatic pipelines, and get back final products which can be visualized under Geographic Information Systems. Moreover, MarsSI also contains an automatic stereo-restitution pipeline in order to produce Digital Terrain Models (DTM) on demand from HiRISE (High Resolution Imaging Science Experiment) or CTX (Context Camera) pair-images. This application is funded by the European Union's Seventh Framework Programme (FP7/2007–2013) (ERC project eMars, No. 280168) and has been developed in the scope of Mars, but the design is applicable to any other planetary body of the solar system.
Published: 2018
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43. Mineralogical Diversity and Geology of Humboldt Crater Derived Using Moon Mineralogy Mapper Data

Author: M, Martinot, S, Besse, J, Flahaut, C, Quantin-Nataf, L, Lozac'h, and W, van Westrenen
Abstract: Moon Mineralogy Mapper (M
Published: 2017

44. Deep alteration between Hellas and Isidis Basins

Author: C. Quantin-Nataf, M. Andréani, B. Bultel, L. Lozac'h, Harold Clenet, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and 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)
Subjects: Martian, Outcrop, Geochemistry, Mars, Astronomy and Astrophysics, Crust, Mars Exploration Program, 15. Life on land, Mineralogy, Hydrothermal circulation, CRISM, Impact crater, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], surface, Ejecta, Geology, Spectroscopy
Abstract: Recent investigations of alteration of martian crustal outcrops suggest putative crustal hydrothermal systems, which are favorable environments for the emergence of life. In this study, we perform an analysis of the CRISM targeted observations covering crustal outcrops in the region between the Hellas and Isidis basins with the goal of investigating the alteration phases. Over the wide studied region, we detect the presence of possible serpentines, chlorites, smectites and carbonates. These detections occur within ejecta blankets, crater walls and central uplifts of impact craters. We investigate the relation between the observed associations of minerals and the ages of the impact craters assessed by crater count. No clear relation is observed. We also investigate the relationship between the group of detected mineral and the pre-impact depth of the studied outcrops assessed from the size of the impact craters. This method allows us to reconstruct the pre-impact cross-section. We suggest that alteration of the first 7 km of the crust between the Hellas and Isidis basins may have undergone alteration processes. (C) 2015 Elsevier Inc. All rights reserved.
Published: 2015
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45. JWST/NIRSpec Prospects on Transneptunian Objects

Author: Bryan J. Holler, Robin Métayer, Frederic Merlin, N. Cabral, Pierre Ferruit, C. Quantin-Nataf, Aurelie Guilbert-Lepoutre, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - 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 national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), and Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)
Subjects: Solar System, lcsh:Astronomy, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics, Stellar classification, 01 natural sciences, Spectral line, lcsh:QB1-991, telescope: JWST, 0103 physical sciences, method: observational, Absorption (electromagnetic radiation), Spectroscopy, kuiper belt: general, 010303 astronomy & astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Wavelength range, lcsh:QC801-809, Astronomy and Astrophysics, lcsh:Geophysics. Cosmic physics, minor planets and asteroids: general, 13. Climate action, Nir spectra, Water ice, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], technique: spectroscopic
Abstract: International audience; The transneptunian region has proven to be a valuable probe to test models of the formation and evolution of the solar system. To further advance our current knowledge of these early stages requires an increased knowledge of the physical properties of Transneptunian Objects (TNOs). Colors and albedos have been the best way so far to classify and study the surface properties of a large number TNOs. However, they only provide a limited fraction of the compositional information, required for understanding the physical and chemical processes to which these objects have been exposed since their formation. This can be better achieved by near-infrared (NIR) spectroscopy, since water ice, hydrocarbons, and nitrile compounds display diagnostic absorption bands in this wavelength range. Visible and NIR spectra taken from ground-based facilities have been observed for ∼80 objects so far, covering the full range of spectral types: from neutral to extremely red with respect to the Sun, featureless to volatile-bearing and volatile-dominated (Barkume et al., 2008; Guilbert et al., 2009; Barucci et al., 2011; Brown, 2012). The largest TNOs are bright and thus allow for detailed and reliable spectroscopy: they exhibit complex surface compositions, including water ice, methane, ammonia, and nitrogen. Smaller objects are more difficult to observe even from the largest telescopes in the world. In order to further constrain the inventory of volatiles and organics in the solar system, and understand the physical and chemical evolution of these bodies, high-quality NIR spectra of a larger sample of TNOs need to be observed. JWST/NIRSpec is expected to provide a substantial improvement in this regard, by increasing both the quality of observed spectra and the number of observed objects. In this paper, we review the current knowledge of TNO properties and provide diagnostics for using NIRSpec to constrain TNO surface compositions.
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46. Crust stratigraphy and heterogeneities of the first kilometers at the dichotomy boundary in western Elysium Planitia and implications for InSight lander

Author: Tamara Gudkova, P. H. Lognonné, Chloé Michaut, Benoit Langlais, C. Quantin-Nataf, Lu Pan, Sebastien Rodriguez, Benoit Tauzin, Peter Grindrod, Matthew P. Golombek, Antoine Lucas, I. E. Stepanova, 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Department of Earth and Planetary Sciences [UCL/Birkbeck], Birkbeck College [University of London], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Schmidt United Institute of Physics of the Earth [Moscow] (IPE), Russian Academy of Sciences [Moscow] (RAS), European Project: MSCA No. 793824,NoLiMit, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH)-NASA, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Lava, [SDU.STU.GP]Sciences of the Universe [physics]/Earth Sciences/Geophysics [physics.geo-ph], Geochemistry, Mars, 01 natural sciences, Elysium, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Impact crater, 0103 physical sciences, [SDU.STU.GM]Sciences of the Universe [physics]/Earth Sciences/Geomorphology, [SDU.ENVI]Sciences of the Universe [physics]/Continental interfaces, environment, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Spectroscopy, 0105 earth and related environmental sciences, Martian, geography, geography.geographical_feature_category, Astronomy and Astrophysics, Crust, Mars Exploration Program, Mineralogy, Volcano, Stratigraphy, 13. Climate action, Space and Planetary Science, Geological processes, Geology, Cratering
Abstract: InSight landed on Mars on November 26, 2018, in western Elysium Planitia. The Mars crust beneath the lander is subject to complex geologic history next to the great topographic and crustal dichotomy of Mars. Understanding this part of the Martian crust in the subsurface would aid future investigations of the internal structure of the planet based on seismic datasets collected by the Seismic Experiment for Interior Structure (SEIS) instrument. Here, we investigate the subsurface structure and composition from the analysis of mineralogy and morphology of exposures in impact craters as well as on scarps and knobs in the general region of Elysium Planitia. Using a combination of orbital datasets, we identify exposures of subsurface materials with distinct composition and physical properties. We find olivine and pyroxene detections associated with small impact craters (1.5–7 km) rim in the vicinity of InSight lander, as well as in the transition unit and Elysium volcanic unit. Fe/Mg phyllosilicates have been identified in the central peak of the 51-km diameter Kalpin crater and on knobs in the transition unit between the dichotomy and the plains. In addition, eroded meter-scale layered unit subject to erosion has been identified in six impact craters to the north-east of the landing site, including Kalpin crater. Massive bedrock and layered, weak materials co-occur in the transition unit, indicating a complex origin. These results together suggest both materials with altered composition and layered deposit occur as distinct geologic units beneath the basaltic lava flow units. Through analogy with terrestrial sedimentary rocks or clay-bearing sediments, we suggest physically weak materials exist beneath the lava flow units in the general region of Elysium Planitia. The spatial distribution and continuity of these materials are unclear due to the lack of exposures within the lava flow unit where the InSight lander is located. These subsurface materials of distinct physical properties may result in increased attenuation or reverberations of seismic waves, to be collected by SEIS. The findings suggest a close investigation of the potential effects of subsurface stratigraphy on seismic data would help inform future data interpretation and understanding of the internal structure of Mars.
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47. Aqueously altered igneous rocks sampled on the floor of Jezero crater, Mars.

Author: Farley KA, Stack KM, Shuster DL, Horgan BHN, Hurowitz JA, Tarnas JD, Simon JI, Sun VZ, Scheller EL, Moore KR, McLennan SM, Vasconcelos PM, Wiens RC, Treiman AH, Mayhew LE, Beyssac O, Kizovski TV, Tosca NJ, Williford KH, Crumpler LS, Beegle LW, Bell JF 3rd, Ehlmann BL, Liu Y, Maki JN, Schmidt ME, Allwood AC, Amundsen HEF, Bhartia R, Bosak T, Brown AJ, Clark BC, Cousin A, Forni O, Gabriel TSJ, Goreva Y, Gupta S, Hamran SE, Herd CDK, Hickman-Lewis K, Johnson JR, Kah LC, Kelemen PB, Kinch KB, Mandon L, Mangold N, Quantin-Nataf C, Rice MS, Russell PS, Sharma S, Siljeström S, Steele A, Sullivan R, Wadhwa M, Weiss BP, Williams AJ, Wogsland BV, Willis PA, Acosta-Maeda TA, Beck P, Benzerara K, Bernard S, Burton AS, Cardarelli EL, Chide B, Clavé E, Cloutis EA, Cohen BA, Czaja AD, Debaille V, Dehouck E, Fairén AG, Flannery DT, Fleron SZ, Fouchet T, Frydenvang J, Garczynski BJ, Gibbons EF, Hausrath EM, Hayes AG, Henneke J, Jørgensen JL, Kelly EM, Lasue J, Le Mouélic S, Madariaga JM, Maurice S, Merusi M, Meslin PY, Milkovich SM, Million CC, Moeller RC, Núñez JI, Ollila AM, Paar G, Paige DA, Pedersen DAK, Pilleri P, Pilorget C, Pinet PC, Rice JW Jr, Royer C, Sautter V, Schulte M, Sephton MA, Sharma SK, Sholes SF, Spanovich N, St Clair M, Tate CD, Uckert K, VanBommel SJ, Yanchilina AG, and Zorzano MP
Abstract: The Perseverance rover landed in Jezero crater, Mars, to investigate ancient lake and river deposits. We report observations of the crater floor, below the crater's sedimentary delta, finding that the floor consists of igneous rocks altered by water. The lowest exposed unit, informally named Séítah, is a coarsely crystalline olivine-rich rock, which accumulated at the base of a magma body. Magnesium-iron carbonates along grain boundaries indicate reactions with carbon dioxide-rich water under water-poor conditions. Overlying Séítah is a unit informally named Máaz, which we interpret as lava flows or the chemical complement to Séítah in a layered igneous body. Voids in these rocks contain sulfates and perchlorates, likely introduced by later near-surface brine evaporation. Core samples of these rocks have been stored aboard Perseverance for potential return to Earth.
Published: 2022
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48. Compositionally and density stratified igneous terrain in Jezero crater, Mars.

Author: Wiens RC, Udry A, Beyssac O, Quantin-Nataf C, Mangold N, Cousin A, Mandon L, Bosak T, Forni O, McLennan SM, Sautter V, Brown A, Benzerara K, Johnson JR, Mayhew L, Maurice S, Anderson RB, Clegg SM, Crumpler L, Gabriel TSJ, Gasda P, Hall J, Horgan BHN, Kah L, Legett C 4th, Madariaga JM, Meslin PY, Ollila AM, Poulet F, Royer C, Sharma SK, Siljeström S, Simon JI, Acosta-Maeda TE, Alvarez-Llamas C, Angel SM, Arana G, Beck P, Bernard S, Bertrand T, Bousquet B, Castro K, Chide B, Clavé E, Cloutis E, Connell S, Dehouck E, Dromart G, Fischer W, Fouchet T, Francis R, Frydenvang J, Gasnault O, Gibbons E, Gupta S, Hausrath EM, Jacob X, Kalucha H, Kelly E, Knutsen E, Lanza N, Laserna J, Lasue J, Le Mouélic S, Leveille R, Lopez Reyes G, Lorenz R, Manrique JA, Martinez-Frias J, McConnochie T, Melikechi N, Mimoun D, Montmessin F, Moros J, Murdoch N, Pilleri P, Pilorget C, Pinet P, Rapin W, Rull F, Schröder S, Shuster DL, Smith RJ, Stott AE, Tarnas J, Turenne N, Veneranda M, Vogt DS, Weiss BP, Willis P, Stack KM, Williford KH, and Farley KA
Abstract: Before Perseverance, Jezero crater's floor was variably hypothesized to have a lacustrine, lava, volcanic airfall, or aeolian origin. SuperCam observations in the first 286 Mars days on Mars revealed a volcanic and intrusive terrain with compositional and density stratification. The dominant lithology along the traverse is basaltic, with plagioclase enrichment in stratigraphically higher locations. Stratigraphically lower, layered rocks are richer in normative pyroxene. The lowest observed unit has the highest inferred density and is olivine-rich with coarse (1.5 millimeters) euhedral, relatively unweathered grains, suggesting a cumulate origin. This is the first martian cumulate and shows similarities to martian meteorites, which also express olivine disequilibrium. Alteration materials including carbonates, sulfates, perchlorates, hydrated silicates, and iron oxides are pervasive but low in abundance, suggesting relatively brief lacustrine conditions. Orbital observations link the Jezero floor lithology to the broader Nili-Syrtis region, suggesting that density-driven compositional stratification is a regional characteristic.
Published: 2022
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49. Morphological and Spectral Diversity of the Clay-Bearing Unit at the ExoMars Landing Site Oxia Planum.

Author: Mandon L, Parkes Bowen A, Quantin-Nataf C, Bridges JC, Carter J, Pan L, Beck P, Dehouck E, Volat M, Thomas N, Cremonese G, Tornabene LL, and Thollot P
Subjects: Clay, Exobiology, Minerals, Water, Extraterrestrial Environment, Mars
Abstract: The European Space Agency and Roscosmos' ExoMars rover mission, which is planned to land in the Oxia Planum region, will be dedicated to exobiology studies at the surface and subsurface of Mars. Oxia Planum is a clay-bearing site that has preserved evidence of long-term interaction with water during the Noachian era. Fe/Mg-rich phyllosilicates have previously been shown to occur extensively throughout the landing area. Here, we analyze data from the High Resolution Imaging Science Experiment (HiRISE) and from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) instruments onboard NASA's Mars Reconnaissance Orbiter and the Colour and Stereo Surface Imaging System (CaSSIS) onboard ESA's Trace Gas Orbiter to characterize, at a high spatial resolution, the morphological and spectral variability of Oxia Planum's surface deposits. Two main types of bedrocks are identified within the clay-bearing, fractured unit observed throughout the landing site: (1) an orange type in HiRISE correlated with the strongest detections of secondary minerals (dominated by Fe/Mg-rich clay minerals) with, in some locations, an additional spectral absorption near 2.5 μm, suggesting the mixture with an additional mineral, plausibly carbonate or another type of clay mineral; (2) a more bluish bedrock associated with weaker detections of secondary minerals, which exhibits at certain locations a ∼1 μm broad absorption feature consistent with olivine. Coanalysis of the same terrains with the recently acquired CaSSIS images confirms the variability in the color and spectral properties of the fractured unit. Of interest for the ExoMars mission, both types of bedrocks are extensively outcropping in the Oxia Planum region, and the one corresponding to the most intense spectral signals of clay minerals (the primary scientific target) is well exposed within the landing area, including near its center.
Published: 2021
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50. Oxia Planum: The Landing Site for the ExoMars "Rosalind Franklin" Rover Mission: Geological Context and Prelanding Interpretation.

Author: Quantin-Nataf C, Carter J, Mandon L, Thollot P, Balme M, Volat M, Pan L, Loizeau D, Millot C, Breton S, Dehouck E, Fawdon P, Gupta S, Davis J, Grindrod PM, Pacifici A, Bultel B, Allemand P, Ody A, Lozach L, and Broyer J
Subjects: Extraterrestrial Environment, Geology, Water, Exobiology, Mars
Abstract: The European Space Agency (ESA) and Roscosmos ExoMars mission will launch the "Rosalind Franklin" rover in 2022 for a landing on Mars in 2023.The goals of the mission are to search for signs of past and present life on Mars, investigate the water/geochemical environment as a function of depth in the shallow subsurface, and characterize the surface environment. To meet these scientific objectives while minimizing the risk for landing, a 5-year-long landing site selection process was conducted by ESA, during which eight candidate sites were down selected to one: Oxia Planum. Oxia Planum is a 200 km-wide low-relief terrain characterized by hydrous clay-bearing bedrock units located at the southwest margin of Arabia Terra. This region exhibits Noachian-aged terrains. We show in this study that the selected landing site has recorded at least two distinct aqueous environments, both of which occurred during the Noachian: (1) a first phase that led to the deposition and alteration of ∼100 m of layered clay-rich deposits and (2) a second phase of a fluviodeltaic system that postdates the widespread clay-rich layered unit. Rounded isolated buttes that overlie the clay-bearing unit may also be related to aqueous processes. Our study also details the formation of an unaltered mafic-rich dark resistant unit likely of Amazonian age that caps the other units and possibly originated from volcanism. Oxia Planum shows evidence for intense erosion from morphology (inverted features) and crater statistics. Due to these erosional processes, two types of Noachian sedimentary rocks are currently exposed. We also expect rocks at the surface to have been exposed to cosmic bombardment only recently, minimizing organic matter damage.
Published: 2021
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59 results on '"C Quantin-Nataf"'

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