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1. Intense alteration on early Mars revealed by high-aluminum rocks at Jezero crater

Author

Royer, C., Bedford, C. C., Johnson, J. R., Horgan, B. H. N., Broz, A., Forni, O., Connell, S., Wiens, R. C., Mandon, L., Kathir, B. S., Hausrath, E. M., Udry, A., Madariaga, J. M., Dehouck, E., Anderson, R. B., Beck, P., Beyssac, O., Clavé, É., Clegg, S. M., Cloutis, E., Fouchet, T., Gabriel, T. S. J., Garczynski, B. J., Klidaras, A., Manelski, H. T., Mayhew, L., Núñez, J., Ollila, A. M., Schröder, S., Simon, J. I., Wolf, U., Stack, K. M., Cousin, A., and Maurice, S.

Published
2024
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5. Diagenetic History and Biosignature Preservation Potential of Fine‐Grained Rocks at Hogwallow Flats, Jezero Crater, Mars.

Author

Broz, A. P., Horgan, B., Kalucha, H., Johnson, J. R., Royer, C., Dehouck, E., Mandon, L., Cardarelli, E. L., Garczynski, B., Haber, J. H., Benison, K. C., Ives, E., Stack, K. M., Mangold, N., Bosak, T., Simon, J. I., Gasda, P., Clave, E., Kathir, B. S., and Zawaski, M.

Subjects
MARTIAN craters, SULFATE minerals, LIFE on Mars, BEDROCK, CLASTIC rocks
Abstract

The Mars 2020 Perseverance rover discovered fine‐grained clastic sedimentary rocks in the "Hogwallow Flats" member of the "Shenandoah" formation at Jezero crater, Mars. The Hogwallow Flats member shows evidence of multiple phases of diagenesis including Fe/Mg‐sulfate‐rich (20–30 wt. %) outcrop transitioning downward into red‐purple‐gray mottled outcrop, Fe/Mg clay minerals and oxides, putative concretions, occasional Ca sulfate‐filled fractures, and variable redox state over small (cm) spatial scales. This work uses Mastcam‐Z and SuperCam instrument data to characterize and interpret the sedimentary facies, mineralogy and diagenetic features of the Hogwallow Flats member. The lateral continuity of bedrock similar in tone and morphology to Hogwallow Flats that occurs over several km within the western Jezero sedimentary fan suggests widespread deposition in a lacustrine or alluvial floodplain setting. Following deposition, sediments interacted with multiple fluids of variable redox state and salinity under habitable conditions. Three drilled sample cores were collected from this interval of the Shenandoah formation as part of the Mars Sample Return campaign. These samples have very high potential to preserve organic compounds and biosignatures. Drill cores may partially include dark‐toned mottled outcrop that lies directly below light‐toned, sulfate‐cemented outcrop. This facies may represent some of the least oxidized material observed at this interval of the Shenandoah formation. This work reconstructs the diagenetic history of the Hogwallow Flats member and discusses implications for biosignature preservation in rock samples for possible return to Earth. Plain Language Summary: The Mars 2020 Perseverance rover discovered sedimentary rocks in Jezero crater during the second year of its mission. Some of these rocks were informally named the "Hogwallow Flats" member of the "Shenandoah" formation. These rocks contain abundant clay minerals and sulfates, indicating ancient interactions with liquid water. They may preserve organic matter and signs of life that could tell us whether life was ever present in Jezero crater billions of years ago. The sediments here appear to have undergone physical and chemical changes after deposition—called diagenesis—when interacting with liquid water. These changes, which may have occurred in a lake or a shallow river plain and later when the sediments were shallowly buried, are often associated with favorable conditions for preserving signs of ancient life. However, these changes may also have resulted in the breakdown of these signs of life. This work reconstructs the geologic history of the Hogwallow Flats member and discusses the importance of these rocks for the search for ancient life on Mars. A total of three rock cores were collected by Perseverance from these rocks for return to Earth. These samples have very high potential to preserve organic matter and signs of ancient life. Key Points: Fine‐grained clastic sedimentary rocks at the Hogwallow Flats member underwent limited diagenesisDiagenesis may have occurred in a lake or a shallow river plain and later when the sediments were shallowly buriedMottling features, sulfates and clay minerals within drilled rock core samples for Mars Sample Return have high astrobiological potential [ABSTRACT FROM AUTHOR]

Published
2024
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7. Astrobiological Potential of Rocks Acquired by the Perseverance Rover at a Sedimentary Fan Front in Jezero Crater, Mars

Author

Bosak, T., Shuster, D. L., Scheller, E. L., Siljeström, S., Zawaski, M. J., Mandon, L., Simon, J. I., Weiss, B. P., Stack, K. M., Mansbach, E. N., Treiman, A. H., Benison, K. C., Brown, A. J., Czaja, A. D., Farley, K. A., Hausrath, E. M., Hickman-Lewis, K., Herd, C. D.K., Johnson, J. R., Mayhew, L. E., Minitti, M. E., Williford, K. H., Wogsland, B. V., Zorzano, M. P., Allwood, A. C., Amundsen, H. E.F., Bell, J. F., Benzerara, K., Bernard, S., Beyssac, O., Buckner, D. K., Cable, M., Calef, F., Caravaca, G., Catling, D. C., Clavé, E., Cloutis, E., Cohen, B. A., Cousin, A., Dehouck, E., Fairén, A. G., Flannery, D. T., Fornaro, T., Forni, O., Fouchet, T., Gibbons, E., Gomez, F. Gomez, Gupta, S., Hand, K. P., Hurowitz, J. A., Kalucha, H., Pedersen, D. A.K., Lopes-Reyes, G., Maki, J. N., Maurice, S., Nuñez, J. I., Randazzo, N., Rice, J. W., Royer, C., Sephton, M. A., Sharma, S., Steele, A., Tate, C. D., Uckert, K., Udry, A., Wiens, R. C., Williams, A., Bosak, T., Shuster, D. L., Scheller, E. L., Siljeström, S., Zawaski, M. J., Mandon, L., Simon, J. I., Weiss, B. P., Stack, K. M., Mansbach, E. N., Treiman, A. H., Benison, K. C., Brown, A. J., Czaja, A. D., Farley, K. A., Hausrath, E. M., Hickman-Lewis, K., Herd, C. D.K., Johnson, J. R., Mayhew, L. E., Minitti, M. E., Williford, K. H., Wogsland, B. V., Zorzano, M. P., Allwood, A. C., Amundsen, H. E.F., Bell, J. F., Benzerara, K., Bernard, S., Beyssac, O., Buckner, D. K., Cable, M., Calef, F., Caravaca, G., Catling, D. C., Clavé, E., Cloutis, E., Cohen, B. A., Cousin, A., Dehouck, E., Fairén, A. G., Flannery, D. T., Fornaro, T., Forni, O., Fouchet, T., Gibbons, E., Gomez, F. Gomez, Gupta, S., Hand, K. P., Hurowitz, J. A., Kalucha, H., Pedersen, D. A.K., Lopes-Reyes, G., Maki, J. N., Maurice, S., Nuñez, J. I., Randazzo, N., Rice, J. W., Royer, C., Sephton, M. A., Sharma, S., Steele, A., Tate, C. D., Uckert, K., Udry, A., Wiens, R. C., and Williams, A.

Abstract

The Perseverance rover has collected seven oriented samples of sedimentary rocks, all likely older than the oldest signs of widespread life on Earth, at the exposed base of the western fan in Jezero crater, Mars. The samples include a sulfate- and clay-bearing mudstone and sandstone, a fluvial sandstone from a stratigraphically low position at the fan front, and a carbonate-bearing sandstone deposited above the sulfate-bearing strata. All samples contain aqueously precipitated materials and most or all were aqueously deposited. Although the rover instruments have not confidently detected organic matter in the rocks from the fan front, the much more sensitive terrestrial instruments will still be able to search for remnants of prebiotic chemistries and past life, and study Mars's past habitability in the samples returned to Earth. The hydrated, sulfate-bearing mudstone has the highest potential to preserve organic matter and biosignatures, whereas the carbonate-bearing sandstones can be used to constrain when and for how long Jezero crater contained liquid water. Returned sample science analyses of sulfate, carbonate, clay, phosphate and igneous minerals as well as trace metals and volatiles that are present in the samples acquired at the fan front would provide transformative insights into past habitable environments on Mars, the evolution of its magnetic field, atmosphere and climate and the past and present cycling of atmospheric and crustal water, sulfur and carbon.

Published
2024

8. From hydrated silica to quartz: Potential hydrothermal precipitates found in Jezero crater, Mars

Author

Beck, P., Beyssac, O., Dehouck, E., Bernard, S., Pineau, M., Mandon, L., Royer, C., Clavé, E., Schröder, S., Forni, O., Francis, R., Mangold, N., Bedford, C.C., Broz, A.P., Cloutis, E.A., Johnson, J.R., Poulet, F., Fouchet, T., Quantin-Nataf, C., Pilorget, C., Rapin, W., Meslin, P.-Y., Gabriel, T.S.J., Arana, G., Madariaga, J.M., Brown, A.J., Maurice, S., Clegg, S.M., Gasnault, O., Cousin, A., and Wiens, R.C.

Published
2025
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9. Probable Concretions Observed in the Shenandoah Formation of Jezero Crater, Mars and Comparison With Terrestrial Analogs.

Author

Kalucha, H., Broz, A., Randazzo, N., Aramendia, J., Madariaga, J. M., Garczynski, B., Lanza, N., Mandon, L., Fouchet, T., Catling, D. C., Fairén, A. G., Kivrak, L., Gasda, P. J., Núñez, J. I., Cloutis, E., Hand, K. P., Rice, J. W., Fischer, W. W., Maurice, S., and Wiens, R. C.

Subjects
MARTIAN craters, BEDROCK, MICROBIAL metabolism, CLAY minerals, CALCIUM salts
Abstract

The Mars 2020 Perseverance Rover imaged diagenetic textural features in four separate sedimentary units in its exploration of the 25‐m‐thick Shenandoah formation at Jezero Crater, Mars, that we interpreted as probable concretions. These concretions were most abundant in the Hogwallow Flats member of the Shenandoah formation and were restricted to the light‐toned, platy, sulfur‐cemented bedrock at outcrop surfaces, whereas the finely laminated, darker toned, mottled and deformed strata lack concretions. The concretions also had a wide range of morphologies including concentric, oblate, urn, and spheroidal shaped forms that were not clustered, and ranged in size from ∼1 to 16 mm with a median of 2.65 mm. The elemental composition of the concretions compared to the bedrock had greater abundance of magnesium and calcium salts, silicates, and possibly hematite. We compared these Jezero Crater concretions to the geochemistry of concretions from previously published studies and from two new terrestrial analog sites (Gallup Formation, New Mexico and Torrey Pines, California). In addition, we measured organic carbon content of three terrestrial sedimentary analogs of increasing age that contain concretions (Torrey Pines (Pleistocene), Gallup Formation (∼89 Ma), and Moodies Group (∼3.2 Ga)). All measured concretions contained significant concentrations of organic carbon with the maximum organic carbon content (∼2 wt. % Total organic carbon) found in the Moodies Group concretions. Organic carbon abundances in terrestrial concretions was controlled more by the formation mechanism and relative timing of concretion development rather than deposit age. These findings suggested that concretions at Jezero Crater reflect local sites of enhanced biosignature preservation potential. Plain Language Summary: The Perseverance Rover discovered concretions in its exploration of the rock packages at Jezero Crater, Mars and one of the sample return cores was collected from concretion‐rich bedrock. Concretions are resistant cement in the rock that are found in many shapes (usually spherical or oblate) and range from millimeter to meter size scales on Earth; they can be formed through inorganic water‐rock reactions or facilitated by microbial metabolisms. We documented the abundance, size, composition, and shape of the concretions to understand how these features were formed. We found that the concretions are mixtures of salts, clay minerals, and iron oxides. We compared these results to terrestrial concretions with similar mineral compositions and measured the organic carbon in four terrestrial analogs. Comparisons with terrestrial concretions in this study and the literature suggested that the concretion composition in Jezero Crater could have high organic preservation potential. Thus, the concretions in Jezero Crater may retain organic carbon and other biosignatures and might therefore be considered as high priority samples of astrobiological interest out of the current sample suite for return to Earth. Key Points: Jezero Crater concretions are variably enriched in Si, Ca, and Mg salts, and Fe oxidesTerrestrial concretions of similar mineralogy analyzed in this study contain significant organic carbon phasesBased on terrestrial analogs, Jezero Crater concretions may represent sites of enhanced biosignature preservation potential [ABSTRACT FROM AUTHOR]

Published
2024
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10. Variable Iron Mineralogy and Redox Conditions Recorded in Ancient Rocks Measured by In Situ Visible/Near‐Infrared Spectroscopy at Jezero Crater, Mars.

Author

Mandon, L., Ehlmann, B. L., Wiens, R. C., Garczynski, B. J., Horgan, B. H. N., Fouchet, T., Loche, M., Dehouck, E., Gasda, P., Johnson, J. R., Broz, A., Núñez, J. I., Rice, M. S., Vaughan, A., Royer, C., Gómez, F., Annex, A. M., Beyssac, O., Forni, O., and Brown, A.

Subjects
HEMATITE, SEDIMENTARY rocks, SEDIMENTATION & deposition, REFLECTANCE measurement, IGNEOUS rocks
Abstract

Using relative reflectance measurements from the Mastcam‐Z and SuperCam instruments on the Mars 2020 Perseverance rover, we assess the variability of Fe mineralogy in Noachian/Hesperian‐aged rocks at Jezero crater. The results reveal diverse Fe3+ and Fe2+ minerals. The igneous crater floor, where small amounts of Fe3+‐phyllosilicates and poorly crystalline Fe3+‐oxyhydroxides have been reported, is spectrally similar to most oxidized basalts observed at Gusev crater. At the base of the western Jezero sedimentary fan, new spectral type points to an Fe‐bearing mineral assemblage likely dominated by Fe2+. By contrast, most strata exposed at the fan front show signatures of Fe3+‐oxides (mostly fine‐grained crystalline hematite), Fe3+‐sulfates (potentially copiapites), strong signatures of hydration, and among the strongest signatures of red hematite observed in situ, consistent with materials having experienced vigorous water‐rock interactions and/or higher degrees of diagenesis under oxidizing conditions. The fan top strata show hydration but little to no signs of Fe oxidation likely implying that some periods of fan construction occurred either during a reduced atmosphere era or during short‐lived aqueous activity of liquid water in contact with an oxidized atmosphere. We also report the discovery of alternating cm‐scale bands of red and gray layers correlated with hydration and oxide variability, which has not yet been observed elsewhere on Mars. This could result from syn‐depositional fluid chemistry variations, possibly as seasonal processes, or diagenetic overprint of oxidized fluids percolating through strata having variable permeability. Plain Language Summary: The oxidation states of the atmosphere and waters (whether rich or poor in oxidants such as oxygen) of Mars and their evolution are poorly constrained but can be recorded in the iron (Fe) mineralogy of rocks. Using data from the Perseverance rover, we analyzed the Fe mineralogy of ∼4–3 Ga old rocks from an ancient lake at Jezero crater. Oxidized Fe is found in igneous rocks and lowermost portions of sedimentary rocks, carried by clays and poorly crystalline oxides in the former and by sulfates and crystalline oxides in the latter, pointing to past action of oxidizing fluids, affecting more intensely the sedimentary rocks. Fe shows poor to no signs of oxidation in the uppermost strata, which might be evidence for a reducing atmosphere during sediment deposition or that the aqueous environment was too cold or too short‐lived to oxidize minerals. We also report Fe mineralogy variability at the cm‐scale in alternating colored layers, which has not been observed previously on Mars and could possibly mean that seasonal processes are recorded at Jezero crater. Key Points: In situ reflectance data measured with Mars 2020 show variable Fe mineralogy in sedimentary rocks at Jezero craterStrata exposed at the fan front experienced stronger oxidative water‐rock interactions compared to the upper fan and igneous crater floorWe identify cm‐scale color banding correlated with Fe‐oxide variability that likely indicates time variation in redox [ABSTRACT FROM AUTHOR]

Published
2024
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11. An olivine cumulate outcrop on the floor of Jezero crater, Mars

Author

Liu, Y, Tice, MM, Schmidt, ME, Treiman, AH, Kizovski, TV, Hurowitz, JA, Allwood, AC, Henneke, J, Pedersen, DAK, VanBommel, SJ, Jones, MWM, Knight, AL, Orenstein, BJ, Clark, BC, Elam, WT, Heirwegh, CM, Barber, T, Beegle, LW, Benzerara, K, Bernard, S, Beyssac, O, Bosak, T, Brown, AJ, Cardarelli, EL, Catling, DC, Christian, Cloutis, EA, Cohen, BA, Davidoff, S, Fairén, AG, Farley, KA, Flannery, DT, Galvin, A, Grotzinger, JP, Gupta, S, Hall, J, Herd, CDK, Hickman-Lewis, K, Hodyss, RP, Horgan, BHN, Johnson, Jørgensen, JL, Kah, LC, Maki, JN, Mandon, L, Mangold, N, McCubbin, FM, McLennan, SM, Moore, K, Nachon, M, Nemere, P, Nothdurft, LD, Núñez, JI, O'Neil, L, Quantin-Nataf, CM, Sautter, V, Shuster, DL, Siebach, KL, Simon, JI, Sinclair, KP, Stack, KM, Steele, A, Tarnas, JD, Tosca, NJ, Uckert, K, Udry, A, Wade, LA, Weiss, BP, Wiens, RC, Williford, KH, Zorzano, M-P, Mangold, Nicolas, Cosmochimie [IMPMC] (IMPMC_COSMO), 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)-Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Laboratoire 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), Liu, Y [0000-0003-0308-0942], Tice, MM [0000-0003-2560-1702], Schmidt, ME [0000-0003-4793-7899], Treiman, AH [0000-0002-8073-2839], Kizovski, TV [0000-0001-8188-9769], Hurowitz, JA [0000-0002-5857-8652], Henneke, J [0000-0002-3195-7417], Pedersen, DAK [0000-0001-7182-8567], VanBommel, SJ [0000-0002-6565-0827], Jones, MWM [0000-0002-0720-8715], Knight, AL [0000-0001-6832-8190], Orenstein, BJ [0000-0002-6586-4227], Clark, BC [0000-0002-5546-8757], Beegle, LW [0000-0002-4944-4353], Benzerara, K [0000-0002-0553-0137], Bernard, S [0000-0001-5576-7020], Beyssac, O [0000-0001-8879-4762], Bosak, T [0000-0001-5179-5323], Brown, AJ [0000-0002-9352-6989], Cardarelli, EL [0000-0001-5451-2309], Catling, DC [0000-0001-5646-120X], Christian, JR [0000-0003-4646-2852], Cloutis, EA [0000-0001-7301-0929], Cohen, BA [0000-0001-5896-5903], Davidoff, S [0000-0002-4417-7268], Fairén, AG [0000-0002-2938-6010], Flannery, DT [0000-0001-8982-496X], Grotzinger, JP [0000-0001-9324-1257], Gupta, S [0000-0001-6415-1332], Hall, J [0000-0003-0884-3777], Herd, CDK [0000-0001-5210-4002], Hickman-Lewis, K [0000-0001-8014-233X], Hodyss, RP [0000-0002-6523-3660], Horgan, BHN [0000-0001-6314-9724], Johnson, JR [0000-0002-5586-4901], Jørgensen, JL [0000-0002-0343-239X], Kah, LC [0000-0001-7172-2033], Maki, JN [0000-0002-7887-0343], Mandon, L [0000-0002-9310-0742], Mangold, N [0000-0002-0022-0631], McCubbin, FM [0000-0002-2101-4431], McLennan, SM [0000-0003-4259-7178], Nachon, M [0000-0003-0417-7076], Nothdurft, LD [0000-0001-9646-9070], Núñez, JI [0000-0003-0930-6674], O'Neil, L [0000-0003-1555-8229], Quantin-Nataf, CM [0000-0002-8313-8595], Shuster, DL [0000-0003-2507-9977], Siebach, KL [0000-0002-6628-6297], Simon, JI [0000-0002-3969-8958], Sinclair, KP [0000-0001-6261-4591], Stack, KM [0000-0003-3444-6695], Steele, A [0000-0001-9643-2841], Tarnas, JD [0000-0002-6256-0826], Tosca, NJ [0000-0003-4415-4231], Uckert, K [0000-0002-0859-5526], Udry, A [0000-0002-0074-8110], Wade, LA [0000-0001-8254-8181], Weiss, BP [0000-0003-3113-3415], Wiens, RC [0000-0002-3409-7344], Zorzano, M-P [0000-0002-4492-9650], and Apollo - University of Cambridge Repository

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Multidisciplinary, 5101 Astronomical Sciences, 37 Earth Sciences, 3705 Geology, 5109 Space Sciences, [SDU.STU.PL] Sciences of the Universe [physics]/Earth Sciences/Planetology, 51 Physical Sciences, 3703 Geochemistry
Abstract

International audience; The geological units on the floor of Jezero crater, Mars, are part of a wider regional stratigraphy of olivine-rich rocks, which extends well beyond the crater. We investigate the petrology of olivine and carbonate-bearing rocks of the Séítah formation in the floor of Jezero. Using multispectral images and x-ray fluorescence data, acquired by the Perseverance rover, we performed a petrographic analysis of the Bastide and Brac outcrops within this unit. We find that these outcrops are composed of igneous rock, moderately altered by aqueous fluid. The igneous rocks are mainly made of coarse-grained olivine, similar to some Martian meteorites. We interpret them as an olivine cumulate, formed by settling and enrichment of olivine through multi-stage cooling of a thick magma body.

Published
2022
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12. A Mars 2020 Perseverance SuperCam Perspective on the Igneous Nature of the Máaz Formation at Jezero Crater and Link With Séítah, Mars

Author

Udry, A., Ostwald, A., Sautter, V., Cousin, A., Beyssac, O., Forni, O., Dromart, G., Benzerara, K., Nachon, M., Horgan, B., Mandon, L., Clavé, E., Dehouck, E., Gibbons, E., Alwmark, S., Ravanis, E., Wiens, R. C., Legett, C., Anderson, R., Pilleri, P., Mangold, N., Schmidt, M., Liu, Y., Núñez, J. I., Castro, K., Madariaga, J. M., Kizovski, T., Beck, P., Bernard, S., Bosak, T., Brown, A., Clegg, S., Cloutis, E., Cohen, B., Connell, S., Crumpler, L., Debaille, V., Flannery, D., Fouchet, T., Gabriel, T. S.J., Gasnault, O., Herd, C. D.K., Johnson, J., Manrique, J. A., Maurice, S., McCubbin, F. M., McLennan, S., Ollila, A., Pinet, P., Quantin-Nataf, C., Udry, A., Ostwald, A., Sautter, V., Cousin, A., Beyssac, O., Forni, O., Dromart, G., Benzerara, K., Nachon, M., Horgan, B., Mandon, L., Clavé, E., Dehouck, E., Gibbons, E., Alwmark, S., Ravanis, E., Wiens, R. C., Legett, C., Anderson, R., Pilleri, P., Mangold, N., Schmidt, M., Liu, Y., Núñez, J. I., Castro, K., Madariaga, J. M., Kizovski, T., Beck, P., Bernard, S., Bosak, T., Brown, A., Clegg, S., Cloutis, E., Cohen, B., Connell, S., Crumpler, L., Debaille, V., Flannery, D., Fouchet, T., Gabriel, T. S.J., Gasnault, O., Herd, C. D.K., Johnson, J., Manrique, J. A., Maurice, S., McCubbin, F. M., McLennan, S., Ollila, A., Pinet, P., and Quantin-Nataf, C.

Abstract

The Máaz formation consists of the first lithologies in Jezero crater analyzed by the Mars 2020 Perseverance rover. This formation, investigated from Sols (Martian days) 1 to 201 and from Sols 343 to 382, overlies the Séítah formation (previously described as an olivine-rich cumulate) and was initially suggested to represent an igneous crater floor unit based on orbital analyses. Using SuperCam data, we conducted a detailed textural, chemical, and mineralogical analyses of the Máaz formation and the Content member of the Séítah formation. We conclude that the Máaz formation and the Content member are igneous and consist of different lava flows and/or possibly pyroclastic flows with complex textures, including vesicular and non-vesicular rocks with different grain sizes. The Máaz formation rocks exhibit some of the lowest Mg# (=molar 100 × MgO/MgO + FeO) of all Martian igneous rocks analyzed so far (including meteorites and surface rocks) and show similar basaltic to basaltic-andesitic compositions. Their mineralogy is dominated by Fe-rich augite to possibly ferrosilite and plagioclase, and minor phases such as Fe-Ti oxides and Si-rich phases. They show a broad diversity of both compositions and textures when compared to Martian meteorites and other surface rocks. The different Máaz and Content lava or pyroclastic flows all originate from the same parental magma and/or the same magmatic system, but are not petrogenetically linked to the Séítah formation. The study of returned Máaz samples in Earth-based laboratories will help constrain the formation of these rocks, calibrate Martian crater counting, and overall, improve our understanding of magmatism on Mars.

Published
2023

13. Samples Collected from the Floor of Jezero Crater with the Mars 2020 Perseverance Rover

Author

Simon, J. I., Hickman-Lewis, K., Cohen, B. A., Mayhew, L.E., Shuster, D.L., Debaille, V., Hausrath, E. M., Weiss, B.P., Bosak, T., Zorzano, M.-P., Amundsen, H. E. F., Beegle, L.W., Bell III, J.F., Benison, K. C., Berger, E. L., Beyssac, O., Brown, A.J., Calef, F., Casademont, T. M., Clark, B., Clavé, E., Crumpler, L., Czaja, A. D., Fairén, A. G., Farley, K. A., Flannery, D. T., Fornaro, T., Forni, O., Gómez, F., Goreva, Y., Gorin, A., Hand, K. P., Hamran, S.-E., Henneke, J., Herd, C. D. K., Horgan, B. H. N., Johnson, J. R., Joseph, J., Kronyak, R. E., Madariaga, J. M., Maki, J. N., Mandon, L., McCubbin, F. M., McLennan, S. M., Moeller, R. C., Newman, C. E., Núñez, J. I., Pascuzzo, A. C., Pedersen, D. A., Poggiali, G., Pinet, P., Quantin-Nataf, C., Rice, M., Rice Jr., J. W., Royer, C., Schmidt, M., Sephton, M., Sharma, S., Siljeström, S., Stack, K. M., Steele, A., Sun, V. Z., Udry, A., VanBommel, S., Wadhwa, M., Wiens, R. C., Williams, A. J., Williford, K. H., Simon, J. I., Hickman-Lewis, K., Cohen, B. A., Mayhew, L.E., Shuster, D.L., Debaille, V., Hausrath, E. M., Weiss, B.P., Bosak, T., Zorzano, M.-P., Amundsen, H. E. F., Beegle, L.W., Bell III, J.F., Benison, K. C., Berger, E. L., Beyssac, O., Brown, A.J., Calef, F., Casademont, T. M., Clark, B., Clavé, E., Crumpler, L., Czaja, A. D., Fairén, A. G., Farley, K. A., Flannery, D. T., Fornaro, T., Forni, O., Gómez, F., Goreva, Y., Gorin, A., Hand, K. P., Hamran, S.-E., Henneke, J., Herd, C. D. K., Horgan, B. H. N., Johnson, J. R., Joseph, J., Kronyak, R. E., Madariaga, J. M., Maki, J. N., Mandon, L., McCubbin, F. M., McLennan, S. M., Moeller, R. C., Newman, C. E., Núñez, J. I., Pascuzzo, A. C., Pedersen, D. A., Poggiali, G., Pinet, P., Quantin-Nataf, C., Rice, M., Rice Jr., J. W., Royer, C., Schmidt, M., Sephton, M., Sharma, S., Siljeström, S., Stack, K. M., Steele, A., Sun, V. Z., Udry, A., VanBommel, S., Wadhwa, M., Wiens, R. C., Williams, A. J., and Williford, K. H.

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

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

Author

Quantin-Nataf, C., Alwmark, S., Calef, F. J., Lasue, J., Kinch, K., Stack, K. M., Sun, V., Williams, N. R., Dehouck, E., Mandon, L., Mangold, N., Beyssac, O., Clave, E., Walter, S. H.G., Simon, J. I., Annex, A. M., Horgan, B., Rice, James W., Shuster, D., Cohen, B., Kah, L., Sholes, Steven, Weiss, B. P., Quantin-Nataf, C., Alwmark, S., Calef, F. J., Lasue, J., Kinch, K., Stack, K. M., Sun, V., Williams, N. R., Dehouck, E., Mandon, L., Mangold, N., Beyssac, O., Clave, E., Walter, S. H.G., Simon, J. I., Annex, A. M., Horgan, B., Rice, James W., Shuster, D., Cohen, B., Kah, L., Sholes, Steven, and Weiss, B. P.

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., 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

15. Samples Collected From the Floor of Jezero Crater With the Mars 2020 Perseverance Rover

Author

Simon, J. I., primary, Hickman‐Lewis, K., additional, Cohen, B. A., additional, Mayhew, L. E., additional, Shuster, D. L., additional, Debaille, V., additional, Hausrath, E. M., additional, Weiss, B. P., additional, Bosak, T., additional, Zorzano, M.‐P., additional, Amundsen, H. E. F., additional, Beegle, L. W., additional, Bell, J. F., additional, Benison, K. C., additional, Berger, E. L., additional, Beyssac, O., additional, Brown, A. J., additional, Calef, F., additional, Casademont, T. M., additional, Clark, B., additional, Clavé, E., additional, Crumpler, L., additional, Czaja, A. D., additional, Fairén, A. G., additional, Farley, K. A., additional, Flannery, D. T., additional, Fornaro, T., additional, Forni, O., additional, Gómez, F., additional, Goreva, Y., additional, Gorin, A., additional, Hand, K. P., additional, Hamran, S.‐E., additional, Henneke, J., additional, Herd, C. D. K., additional, Horgan, B. H. N., additional, Johnson, J. R., additional, Joseph, J., additional, Kronyak, R. E., additional, Madariaga, J. M., additional, Maki, J. N., additional, Mandon, L., additional, McCubbin, F. M., additional, McLennan, S. M., additional, Moeller, R. C., additional, Newman, C. E., additional, Núñez, J. I., additional, Pascuzzo, A. C., additional, Pedersen, D. A., additional, Poggiali, G., additional, Pinet, P., additional, Quantin‐Nataf, C., additional, Rice, M., additional, Rice, J. W., additional, Royer, C., additional, Schmidt, M., additional, Sephton, M., additional, Sharma, S., additional, Siljeström, S., additional, Stack, K. M., additional, Steele, A., additional, Sun, V. Z., additional, Udry, A., additional, VanBommel, S., additional, Wadhwa, M., additional, Wiens, R. C., additional, Williams, A. J., additional, and Williford, K. H., additional

Published
2023
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16. The Complex Exhumation History of Jezero Crater Floor Unit and Its Implication for Mars Sample Return

Author

Quantin‐Nataf, C., primary, Alwmark, S., additional, Calef, F. J., additional, Lasue, J., additional, Kinch, K., additional, Stack, K. M., additional, Sun, V., additional, Williams, N. R., additional, Dehouck, E., additional, Mandon, L., additional, Mangold, N., additional, Beyssac, O., additional, Clave, E., additional, Walter, S. H. G., additional, Simon, J. I., additional, Annex, A. M., additional, Horgan, B., additional, Rice, James W., additional, Shuster, D., additional, Cohen, B., additional, Kah, L., additional, Sholes, Steven, additional, and Weiss, B. P., additional

Published
2023
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17. Coarse-grained olivine-rich regolith at jezero crater, mars: nature, source and transport

Author

Beyssac, O., Chide, B., Cousin, A., Ayoub, F., Bertrand, T., Forni, O., Mandon, L., Beck, P., Johnson, J. R., Lasue, J., Clavé, E., Sullivan, R., Nataf, C. Quantin, Udry, A., Dehouck, E., Poulet, F., Pilorget, C., Fouchet, T., Meslin, P.Y., Gasnault, O., Maurice, S., Wiens, R.C., Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université 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 d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-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)-Centre National de la Recherche Scientifique (CNRS), Department of Computer Science [Purdue], Purdue University [West Lafayette], and Lunar and Planetary Institute

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience

Published
2023

18. Analysis of co-located supercam and sherloc observations on abrasion patches in Jezero crater

Author

Connell, S. A., Wiens, R. C., Cardarelli, E. L., Deen, R., Mandon, L., Sharma, S., Beyssac, O., Clavé, E., Siljeström, S., Czaja, A.I., Pilleri, P., Gasnault, O., Lopez-Reyes, G., Johnson, J.R., Bhartia, R., Maurice, S., Teams, Supercam And Sherloc, Purdue University [West Lafayette], California Institute of Technology (CALTECH), 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), Université de Bordeaux (UB), University of Cincinnati (UC), 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), Universidad de Valladolid [Valladolid] (UVa), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Photon Systems Inc., and Lunar and Planetary Institute

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience

Published
2023

19. Petrological traverse of the olivine cumulate Séítah formation at Jezero crater, Mars : A perspective from SuperCam onboard Perseverance

Author

Beyssac, O., Forni, O., Cousin, A., Udry, A., Kah, L.C., Mandon, L., Clavé, E., Liu, Y., Poulet, F., Quantin Nataf, C., Gasnault, O., Johnson, J., Benzerara, K., Beck, P., Dehouck, E., Mangold, N., Alvarez Llamas, C., Anderson, R., Arana, G., Barnes, R., Bernard, S., Bosak, T., Brown, A.J., Castro, K., Chide, B., Clegg, S., Cloutis, E., Fouchet, T., Gabriel, T., Gupta, S., Lacombe, G., Lasue, J., Le Mouelic, S., Lopez‐Reyes, G., Madariaga, J.M., McCubbin, F.M., McLennan, S., Manrique, J.A., Meslin, P.Y., Montmessin, F., Núñez, J., Ollila, A.M., Ostwald, A., Pilleri, P., Pinet, P., Royer, C., Sharma, S.K., Schröder, Susanne, Simon, J.I., Toplis, M.J., Veneranda, M., Willis, P.A., Maurice, S., Wiens, R.C., Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Department of Geoscience [Las Vegas], University of Nevada [Las Vegas] (WGU Nevada), Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Laboratoire de Planétologie et Géosciences - Angers (LPG-ANGERS), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Department of Analytical Chemistry [Malaga], Universidad de Málaga [Málaga] = University of Málaga [Málaga], Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Department of Analytical Chemistry [Leioa], University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Department of Earth Science and Engineering [Imperial College London], Imperial College London, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Plancius Research LLC, Los Alamos National Laboratory (LANL), University of Winnipeg, Laboratoire Energie Signal Images et Automatique [Univ Ngaoundéré] (LESIA), Université de Ngaoundéré/University of Ngaoundéré [Cameroun] (UN), Universidad de Valladolid [Valladolid] (UVa), NASA Johnson Space Center (JSC), NASA, Department of Geosciences [Stony Brook], Stony Brook University [SUNY] (SBU), State University of New York (SUNY)-State University of New York (SUNY), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Hawaii Institute of Geophysics and Planetology (HIGP), University of Hawai‘i [Mānoa] (UHM), DLR Institute of Optical Sensor Systems, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Department of Earth, Atmospheric, and Planetary Sciences [West Lafayette] (EAPS), and Purdue University [West Lafayette]

Subjects
spectroscopy, LIBS, m2020, Mars, Perseverance, Jezero, Jezero crater, reflectance spectroscopy, in-situ, [SDU]Sciences of the Universe [physics], rover, Seitah, VisIR, Raman, in-situ science
Abstract

International audience; Séítah is the stratigraphically lowest formation visited by Perseverance in the Jezero crater floor. We present the data obtained by SuperCam: texture by imagery, chemistry by LIBS, and mineralogy by VISIR and Raman spectroscopy. The Séítah formation consists of igneous, weakly altered, rocks dominated by millimeter-size grains of olivine with the presence of low-Ca and high-Ca pyroxenes, and other primary minerals (e.g., plagioclase, Cr-Fe-Ti oxides, phosphates). Along a ∼140 m long section in Séítah, SuperCam analyses showed evidence of geochemical and mineralogical variations, from the contact with the overlying Máaz formation, going deeper in the formation. Bulk rock and olivine Mg#, grain size, olivine content increase gradually further from the contact. Along the section, olivine Mg# are not in equilibrium with the bulk rock Mg#, indicating local olivine accumulation. These observations are consistent with Séítah being the deep ultramafic member of a cumulate series derived from the fractional crystallization and slow cooling of the parent magma at depth. Possible magmatic processes and exhumation mechanisms of Séítah are discussed. Séítah rocks show some affinity with some rocks at Gusev crater, and with some martian meteorites suggesting that such rocks are not rare on the surface of Mars. Séítah is part of the Nili Fossae regional olivine-carbonate unit observed from orbit. Future exploration of Perseverance on the rim and outside of the crater will help determine if the observations from the crater floor can be extrapolated to the whole unit, or if this unit is composed of distinct sub-units with various origins.

Published
2023
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20. Reflectance of Jezero Crater Floor: 1. Data Processing and Calibration of the Infrared Spectrometer (IRS) on SuperCam

Author

Royer, Clément, Fouchet, T., Mandon, L., Montmessin, Franck, Poulet, F., Forni, O., Johnson, J., Legett, C., Le Mouélic, S., Gasnault, O., Quantin-Nataf, C., Beck, Pierre, Dehouck, E., Clavé, E., Ollila, A., Pilorget, C., Bernardi, P., Reess, J.‐M., Pilleri, P., Brown, A., Newell, R., Cloutis, E., Maurice, S., Wiens, R., Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), 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 de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), 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, 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), Los Alamos National Laboratory (LANL), Plancius Research LLC, Department of Geography [Winnipeg], University of Winnipeg, Department of Earth, Atmospheric, and Planetary Sciences [West Lafayette] (EAPS), and Purdue University [West Lafayette]

Subjects
Geophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous)
Abstract

International audience; The $Perseverance$ rover, Mars 2020 mission, landed on the surface of the Jezero Crater, on February, 18th 2021. This Martian crater is suspected to have hosted a paleolake as evidenced by the numerous detections of aqueously-altered phases and thus is a promising candidate for the search for past Martian life. The SuperCam instrument, a collaboration by a consortium of American and European laboratories, plays a leading role in this investigation thanks to its highly versatile payload providing rapid, synergistic, fine-scale mineralogy, chemistry, and color imaging. After its landing, the first measurements of Martian targets with the infrared spectrometer of SuperCam (IRS) showed new instrumental behaviors that had to be characterized and calibrated to derive unbiased science data. The IRS radiometric response has thus been calibrated using periodic observations of the Aluwhite SuperCam Calibration Target (SCCT). Parasitic effects were understood and mitigated, and the instrumental dark and noise are characterized and modeled. The reflectance calibrated data products, provided periodically on the NASA Planetary Data System, are corrected for the main instrumental features. This radiometric calibration allowed us to study the 2.5 μm absorption band which has been discovered in the Séítah unit and is associated with phyllosilicates-carbonates mixtures.

Published
2023
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21. Surface Energy Budget, Albedo, and Thermal Inertia at Jezero Crater, Mars, as Observed From the Mars 2020 MEDA Instrument

Author

Martínez, G. M., primary, Sebastián, E., additional, Vicente‐Retortillo, A., additional, Smith, M. D., additional, Johnson, J. R., additional, Fischer, E., additional, Savijärvi, H., additional, Toledo, D., additional, Hueso, R., additional, Mora‐Sotomayor, L., additional, Gillespie, H., additional, Munguira, A., additional, Sánchez‐Lavega, A., additional, Lemmon, M. T., additional, Gómez, F., additional, Polkko, J., additional, Mandon, L., additional, Apéstigue, V., additional, Arruego, I., additional, Ramos, M., additional, Conrad, P., additional, Newman, C. E., additional, Torre‐Juarez, M. de la, additional, Jordan, F., additional, Tamppari, L. K., additional, McConnochie, T. H., additional, Harri, A.‐M., additional, Genzer, M., additional, Hieta, M., additional, Zorzano, M.‐P., additional, Siegler, M., additional, Prieto, O., additional, Molina, A., additional, and Rodríguez‐Manfredi, J. A., additional

Published
2023
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22. A comparison of the igneous máaz formation at jezero crater with martian meteorites

Author

Udry, A., Ostwald, A., Sautter, V., Cousin, A., Wiens, R. C., Forni, O., Benzerara, K., Beyssac, O., Nachon, M., Dromart, G., Quantin, C., Mandon, L., Clavé, E., Pinet, P., Ollila, A., Bosak, T., Mangold, N., Dehouck, E., Johnson, J., Schmidt, M., Horgan, B., Gabriel, T., Mclennan, S., Maurice, S., Simon, J.I., Herd, C. D. K., M.Madiaraga, J., Brown, A, Connell, S., Flannery, D., Tosca, N., Cohen, B., Liu, Y., Mccubbin, F. M., Cloutis, E., Fouchet, T., Royer, C., Alwmark, S., Sharma, S., Anderson, R., Pilleri, P, University of Nevada [Las Vegas] (WGU Nevada), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Texas A&M University System, École normale supérieure de Lyon (ENS de Lyon), Massachusetts Institute of Technology (MIT), Johns Hopkins University (JHU), Brock University [Canada], Purdue University [West Lafayette], United States Geological Survey (USGS), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, University of Alberta, University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), NASA, University of Winnipeg, Queensland University of Technology [Brisbane] (QUT), University of Cambridge [UK] (CAM), California Institute of Technology (CALTECH), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), University of Copenhagen = Københavns Universitet (UCPH), Hawaii Institute of Geophysics and Planetology (HIGP), and University of Hawai‘i [Mānoa] (UHM)

Subjects
jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], rover, mars mineralogy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, supercam, meteorites
Abstract

International audience

Published
2022

23. Reflectance of Jezero Crater Floor: 2. Mineralogical Interpretation.

Author

Mandon, L., Quantin‐Nataf, C., Royer, C., Beck, P., Fouchet, T., Johnson, J. R., Dehouck, E., Le Mouélic, S., Poulet, F., Montmessin, F., Pilorget, C., Gasnault, O., Forni, O., Mayhew, L. E., Beyssac, O., Bertrand, T., Clavé, E., Pinet, P., Brown, A. J., and Legett, C.

Subjects
MINERAL dusts, GEODIVERSITY, IMPACT craters, BEDROCK, MARS rovers, REFLECTANCE, CARBONACEOUS chondrites (Meteorites)
Abstract

The Perseverance rover landed in the ancient lakebed of Jezero crater, Mars on February 2021. Here, we assess the mineralogy of the rocks, regolith, and dust measured during the first year of the mission on the crater floor, using the visible and near‐infrared spectrometer of SuperCam onboard the Perseverance rover. Most of the minerals detected from orbit are present in the bedrock, with olivine‐bearing rocks at the bottom of the stratigraphy and high‐Ca pyroxene‐bearing rocks at the top. This is distinct from the overall low‐Ca pyroxene‐bearing composition of the watershed of Jezero and points toward an igneous origin. Alteration mineral phases were detected in most of the rocks analyzed in low proportions, suggesting that aqueous alteration of the crater floor has been spatially widespread, but limited in intensity and/or time. The diverse aqueous mineralogy suggests that the aqueous alteration history of the crater floor consists of at least two stages, to form phyllosilicates and oxyhydroxides, and later sulfates. We interpret their formation in a lake or under deeper serpentinization conditions and in an evaporative environment, respectively. Spectral similarities of dust with some rock coatings suggest widespread past processes of dust induration under liquid water activity late in the history of Jezero. Analysis of the regolith revealed some local inputs from the surrounding rocks. Relevant to the Mars Sample Return mission, the spectral features exhibited by the rocks sampled on the crater floor are representative of the diversity of spectra measured on the geological units investigated by the rover. Plain Language Summary: We present the results of the analysis of rocks and regolith measured during the first year after landing of the Perseverance rover on Mars. The analytical technique used is reflectance spectroscopy (the measurement of the light reflected by surfaces), which primarily provides information on mineralogy. The mineralogical composition of the magmatic rocks located near the landing site indicates that they have experienced several distinct episodes of interaction with water in the past, of relatively low intensity. Soil analysis reveals a composition similar to what has been observed at other sites on Mars, with a contribution from the disintegration of local rocks. The samples that are collected by Perseverance at the crater floor and brought back to Earth are representative of the diversity of the different geological units explored by the rover. Key Points: Mineralogy of rocks, regolith, and dust of the crater floor of Jezero, Mars was inferred from SuperCam reflectance dataAssemblages suggest limited aqueous alteration of igneous rocks, followed by evaporation‐induced deposition of sulfatesSamples collected on the crater floor for return to Earth are representative of the geological diversity and witness past‐aqueous processes [ABSTRACT FROM AUTHOR]

Published
2023
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24. Aqueously altered igneous rocks sampled on the floor of Jezero crater, Mars

Author

Farley, K. A., primary, Stack, K. M., additional, Shuster, D. L., additional, Horgan, B. H. N., additional, Hurowitz, J. A., additional, Tarnas, J. D., additional, Simon, J. I., additional, Sun, V. Z., additional, Scheller, E. L., additional, Moore, K. R., additional, McLennan, S. M., additional, Vasconcelos, P. M., additional, Wiens, R. C., additional, Treiman, A. H., additional, Mayhew, L. E., additional, Beyssac, O., additional, Kizovski, T. V., additional, Tosca, N. J., additional, Williford, K. H., additional, Crumpler, L. S., additional, Beegle, L. W., additional, Bell, J. F., additional, Ehlmann, B. L., additional, Liu, Y., additional, Maki, J. N., additional, Schmidt, M. E., additional, Allwood, A. C., additional, Amundsen, H. E. F., additional, Bhartia, R., additional, Bosak, T., additional, Brown, A. J., additional, Clark, B. C., additional, Cousin, A., additional, Forni, O., additional, Gabriel, T. S. J., additional, Goreva, Y., additional, Gupta, S., additional, Hamran, S.-E., additional, Herd, C. D. K., additional, Hickman-Lewis, K., additional, Johnson, J. R., additional, Kah, L. C., additional, Kelemen, P. B., additional, Kinch, K. B., additional, Mandon, L., additional, Mangold, N., additional, Quantin-Nataf, C., additional, Rice, M. S., additional, Russell, P. S., additional, Sharma, S., additional, Siljeström, S., additional, Steele, A., additional, Sullivan, R., additional, Wadhwa, M., additional, Weiss, B. P., additional, Williams, A. J., additional, Wogsland, B. V., additional, Willis, P. A., additional, Acosta-Maeda, T. A., additional, Beck, P., additional, Benzerara, K., additional, Bernard, S., additional, Burton, A. S., additional, Cardarelli, E. L., additional, Chide, B., additional, Clavé, E., additional, Cloutis, E. A., additional, Cohen, B. A., additional, Czaja, A. D., additional, Debaille, V., additional, Dehouck, E., additional, Fairén, A. G., additional, Flannery, D. T., additional, Fleron, S. Z., additional, Fouchet, T., additional, Frydenvang, J., additional, Garczynski, B. J., additional, Gibbons, E. F., additional, Hausrath, E. M., additional, Hayes, A. G., additional, Henneke, J., additional, Jørgensen, J. L., additional, Kelly, E. M., additional, Lasue, J., additional, Le Mouélic, S., additional, Madariaga, J. M., additional, Maurice, S., additional, Merusi, M., additional, Meslin, P.-Y., additional, Milkovich, S. M., additional, Million, C. C., additional, Moeller, R. C., additional, Núñez, J. I., additional, Ollila, A. M., additional, Paar, G., additional, Paige, D. A., additional, Pedersen, D. A. K., additional, Pilleri, P., additional, Pilorget, C., additional, Pinet, P. C., additional, Rice, J. W., additional, Royer, C., additional, Sautter, V., additional, Schulte, M., additional, Sephton, M. A., additional, Sharma, S. K., additional, Sholes, S. F., additional, Spanovich, N., additional, St. Clair, M., additional, Tate, C. D., additional, Uckert, K., additional, VanBommel, S. J., additional, Yanchilina, A. G., additional, and Zorzano, M.-P., additional

Published
2022
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25. Aqueously altered igneous rocks sampled on the floor of Jezero crater, Mars

Author

Farley, K. A., Stack, K. M., Shuster, D. L., Horgan, B. H. N., Hurowitz, J. A., Tarnas, J. D., Simon, J. I., Sun, V. Z., Scheller, E. L., Moore, K. R., McLennan, S. M., Vasconcelos, P. M., Wiens, R. C., Treiman, A. H., Mayhew, L. E., Beyssac, O., Kizovski, T. V., Tosca, N. J., Williford, K. H., Crumpler, L. S., Beegle, L. W., Bell, J. F., Ehlmann, B. L., Liu, Y., Maki, J. N., Schmidt, M. E., Allwood, A. C., Amundsen, H. E. F., Bhartia, R., Bosak, T., Brown, A. J., Clark, B. C., Cousin, A., Forni, O., Gabriel, T. S. J., Goreva, Y., Gupta, S., Hamran, S.-E., Herd, C. D. K., Hickman-Lewis, K., Johnson, J. R., Kah, L. C., Kelemen, P. B., Kinch, K. B., Mandon, L., Mangold, N., Quantin-Nataf, C., Rice, M. S., Russell, P. S., Sharma, S., Siljeström, S., Steele, A., Sullivan, R., Wadhwa, M., Weiss, B. P., Williams, A. J., Wogsland, B. V., Willis, P. A., Acosta-Maeda, T. A., Beck, P., Benzerara, K., Bernard, S., Burton, A. S., Cardarelli, E. L., Chide, B., Clavé, E., Cloutis, E. A., Cohen, B. A., Czaja, A. D., Debaille, V., Dehouck, E., Fairén, A. G., Flannery, D. T., Fleron, S. Z., Fouchet, T., Frydenvang, J., Garczynski, B. J., Gibbons, E. F., Hausrath, E. M., Hayes, A. G., Henneke, J., Jørgensen, J. L., Kelly, E. M., Lasue, J., Le Mouélic, S., Madariaga, J. M., Maurice, S., Merusi, M., Meslin, P.-Y., Milkovich, S. M., Million, C. C., Moeller, R. C., Nuñez, J. I., Ollila, A. M., Paar, G., Paige, D. A., Pedersen, D. A. K., Pilleri, P., Pilorget, C., Pinet, P. C., Rice, J. W., Royer, C., Sautter, V., Schulte, M., Sephton, M. A., Sharma, S. K., Sholes, S. F., Spanovich, N., Clair, M. St., Tate, C. D., Uckert, K., VanBommel, S. J., Yanchilina, A. G., Zorzano, M.-P., Farley, K. A., Stack, K. M., Shuster, D. L., Horgan, B. H. N., Hurowitz, J. A., Tarnas, J. D., Simon, J. I., Sun, V. Z., Scheller, E. L., Moore, K. R., McLennan, S. M., Vasconcelos, P. M., Wiens, R. C., Treiman, A. H., Mayhew, L. E., Beyssac, O., Kizovski, T. V., Tosca, N. J., Williford, K. H., Crumpler, L. S., Beegle, L. W., Bell, J. F., Ehlmann, B. L., Liu, Y., Maki, J. N., Schmidt, M. E., Allwood, A. C., Amundsen, H. E. F., Bhartia, R., Bosak, T., Brown, A. J., Clark, B. C., Cousin, A., Forni, O., Gabriel, T. S. J., Goreva, Y., Gupta, S., Hamran, S.-E., Herd, C. D. K., Hickman-Lewis, K., Johnson, J. R., Kah, L. C., Kelemen, P. B., Kinch, K. B., Mandon, L., Mangold, N., Quantin-Nataf, C., Rice, M. S., Russell, P. S., Sharma, S., Siljeström, S., Steele, A., Sullivan, R., Wadhwa, M., Weiss, B. P., Williams, A. J., Wogsland, B. V., Willis, P. A., Acosta-Maeda, T. A., Beck, P., Benzerara, K., Bernard, S., Burton, A. S., Cardarelli, E. L., Chide, B., Clavé, E., Cloutis, E. A., Cohen, B. A., Czaja, A. D., Debaille, V., Dehouck, E., Fairén, A. G., Flannery, D. T., Fleron, S. Z., Fouchet, T., Frydenvang, J., Garczynski, B. J., Gibbons, E. F., Hausrath, E. M., Hayes, A. G., Henneke, J., Jørgensen, J. L., Kelly, E. M., Lasue, J., Le Mouélic, S., Madariaga, J. M., Maurice, S., Merusi, M., Meslin, P.-Y., Milkovich, S. M., Million, C. C., Moeller, R. C., Nuñez, J. I., Ollila, A. M., Paar, G., Paige, D. A., Pedersen, D. A. K., Pilleri, P., Pilorget, C., Pinet, P. C., Rice, J. W., Royer, C., Sautter, V., Schulte, M., Sephton, M. A., Sharma, S. K., Sholes, S. F., Spanovich, N., Clair, M. St., Tate, C. D., Uckert, K., VanBommel, S. J., Yanchilina, A. G., and Zorzano, M.-P.

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 Seitah, 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 Seitah is a unit informally named Maaz, which we interpret as lava flows or the chemical complement to Seitah 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

26. In situ recording of Mars soundscape

Author

Maurice, S., Chide, B., Murdoch, N., Lorenz, R. D., Mimoun, D., Wiens, R. C., Stott, A., Jacob, X., Bertrand, T., Montmessin, F., Lanza, N. L., Alvarez-Llamas, C., Angel, S. M., Aung, M., Balaram, J., Beyssac, O., Cousin, A., Delory, G., Forni, O., Fouchet, T., Gasnault, O., Grip, H., Hecht, M., Hoffman, J., Laserna, J., Lasue, J., Maki, J., McClean, J., Meslin, P.-Y., Le Mouélic, S., Munguira, A., Newman, C. E., Rodríguez Manfredi, J. A., Moros, J., Ollila, A., Pilleri, P., Schröder, S., de la Torre Juárez, M., Tzanetos, T., Stack, K. M., Farley, K., Williford, K., Acosta-Maeda, T., Anderson, R. B., Applin, D. M., Arana, G., Bassas-Portus, M., Beal, R., Beck, P., Benzerara, K., Bernard, S., Bernardi, P., Bosak, T., Bousquet, B., Brown, A., Cadu, A., Caïs, P., Castro, K., Clavé, E., Clegg, S. M., Cloutis, E., Connell, S., Debus, A., Dehouck, E., Delapp, D., Donny, C., Dorresoundiram, A., Dromart, G., Dubois, B., Fabre, C., Fau, A., Fischer, W., Francis, R., Frydenvang, J., Gabriel, T., Gibbons, E., Gontijo, I., Johnson, J. R., Kalucha, H., Kelly, E., Knutsen, E. W., Lacombe, G., Legett, C., Leveille, R., Lewin, E., Lopez-Reyes, G., Lorigny, E., Madariaga, J. M., Madsen, M., Madsen, S., Mandon, L., Mangold, N., Mann, M., Manrique, J.-A., Martinez-Frias, J., Mayhew, L. E., McConnochie, T., McLennan, S. M., Melikechi, N., Meunier, F., Montagnac, G., Mousset, V., Nelson, T., Newell, R. T., Parot, Y., Pilorget, C., Pinet, P., Pont, G., Poulet, F., Quantin-Nataf, C., Quertier, B., Rapin, W., Reyes-Newell, A., Robinson, S., Rochas, L., Royer, C., Rull, F., Sautter, V., Sharma, S., Shridar, V., Sournac, A., Toplis, M., Torre-Fdez, I., Turenne, N., Udry, A., Veneranda, M., Venhaus, D., Vogt, D., Willis, P., Maurice, S., Chide, B., Murdoch, N., Lorenz, R. D., Mimoun, D., Wiens, R. C., Stott, A., Jacob, X., Bertrand, T., Montmessin, F., Lanza, N. L., Alvarez-Llamas, C., Angel, S. M., Aung, M., Balaram, J., Beyssac, O., Cousin, A., Delory, G., Forni, O., Fouchet, T., Gasnault, O., Grip, H., Hecht, M., Hoffman, J., Laserna, J., Lasue, J., Maki, J., McClean, J., Meslin, P.-Y., Le Mouélic, S., Munguira, A., Newman, C. E., Rodríguez Manfredi, J. A., Moros, J., Ollila, A., Pilleri, P., Schröder, S., de la Torre Juárez, M., Tzanetos, T., Stack, K. M., Farley, K., Williford, K., Acosta-Maeda, T., Anderson, R. B., Applin, D. M., Arana, G., Bassas-Portus, M., Beal, R., Beck, P., Benzerara, K., Bernard, S., Bernardi, P., Bosak, T., Bousquet, B., Brown, A., Cadu, A., Caïs, P., Castro, K., Clavé, E., Clegg, S. M., Cloutis, E., Connell, S., Debus, A., Dehouck, E., Delapp, D., Donny, C., Dorresoundiram, A., Dromart, G., Dubois, B., Fabre, C., Fau, A., Fischer, W., Francis, R., Frydenvang, J., Gabriel, T., Gibbons, E., Gontijo, I., Johnson, J. R., Kalucha, H., Kelly, E., Knutsen, E. W., Lacombe, G., Legett, C., Leveille, R., Lewin, E., Lopez-Reyes, G., Lorigny, E., Madariaga, J. M., Madsen, M., Madsen, S., Mandon, L., Mangold, N., Mann, M., Manrique, J.-A., Martinez-Frias, J., Mayhew, L. E., McConnochie, T., McLennan, S. M., Melikechi, N., Meunier, F., Montagnac, G., Mousset, V., Nelson, T., Newell, R. T., Parot, Y., Pilorget, C., Pinet, P., Pont, G., Poulet, F., Quantin-Nataf, C., Quertier, B., Rapin, W., Reyes-Newell, A., Robinson, S., Rochas, L., Royer, C., Rull, F., Sautter, V., Sharma, S., Shridar, V., Sournac, A., Toplis, M., Torre-Fdez, I., Turenne, N., Udry, A., Veneranda, M., Venhaus, D., Vogt, D., and Willis, P.

Abstract

Prior to the Perseverance rover landing, the acoustic environment of Mars was unknown. Models predicted that: (i) atmospheric turbulence changes at centimeter scales or smaller at the point where molecular viscosity converts kinetic energy into heat1, (ii) the speed of sound varies at the surface with frequency, and (iii) high frequency waves are strongly attenuated with distance in CO₂. However, theoretical models were uncertain because of a lack of experimental data at low pressure, and the difficulty to characterize turbulence or attenuation in a closed environment. Here using Perseverance microphone recordings, we present the first characterization of Mars’ acoustic environment and pressure fluctuations in the audible range and beyond, from 20 Hz to 50 kHz. We find that atmospheric sounds extend measurements of pressure variations down to 1,000 times smaller scales than ever observed before, revealing a dissipative regime extending over 5 orders of magnitude in energy. Using point sources of sound (Ingenuity rotorcraft, laser-induced sparks), we highlight two distinct values for the speed of sound that are ~10 m/s apart below and above 240 Hz, a unique characteristic of low-pressure CO₂-dominated atmosphere. We also provide the acoustic attenuation with distance above 2 kHz, allowing us to elucidate the large contribution of the CO₂ vibrational relaxation in the audible range. These results establish a ground truth for modelling of acoustic processes, which is critical for studies in atmospheres like Mars and Venus ones.

Published
2022

27. Aqueously altered igneous rocks sampled on the floor of Jezero crater, Mars

Author

Farley, K A, Stack, K M, Shuster, D L, Horgan, B H N, Hurowitz, J A, Tarnas, J D, Simon, J I, Sun, V Z, Scheller, E L, Moore, K R, McLennan, S M, Vasconcelos, P M, Wiens, R C, Treiman, A H, Mayhew, L E, Beyssac, O, Kizovski, T V, Tosca, N J, Williford, K H, Crumpler, L S, Beegle, L W, Bell, J F, Ehlmann, B L, Liu, Y, Maki, J N, Schmidt, M E, Allwood, A C, Amundsen, H E F, Bhartia, R, Bosak, T, Brown, A J, Clark, B C, Cousin, A, Forni, O, Gabriel, T S J, Goreva, Y, Gupta, S, Hamran, S-E, Herd, C D K, Hickman-Lewis, K, Johnson, J R, Kah, L C, Kelemen, P B, Kinch, K B, Mandon, L, Mangold, N, Quantin-Nataf, C, Rice, M S, Russell, P S, Sharma, S K, Siljeström, S, Steele, A, Sullivan, R, Wadhwa, M, Weiss, B P, Williams, A J, Wogsland, B V, Willis, P A, Acosta-Maeda, T A, Beck, P, Benzerara, K, Bernard, S, Burton, A S, Cardarelli, E L, Chide, B, Clavé, E, Cloutis, E A, Cohen, B A, Czaja, A D, Debaille, V, Dehouck, E, Fairén, A G, Flannery, D T, Fleron, S Z, Fouchet, T, Frydenvang, J, Garczynski, B J, Gibbons, E F, Hausrath, E M, Hayes, A G, Henneke, J, Jørgensen, J L, Kelly, E M, Lasue, J, Le Mouélic, S, Madariaga, J M, Maurice, S, Merusi, M, Meslin, P-Y, Milkovich, S M, Million, C C, Moeller, R C, Núñez, J I, Ollila, A M, Paar, G, Paige, D A, Pedersen, D A K, Pilleri, P, Pilorget, C, Pinet, P C, Rice, J W, Royer, C, Sautter, V, Schulte, M, Sephton, M A, Sholes, S F, Spanovich, N, St Clair, M, Tate, C D, Uckert, K, VanBommel, S J, Yanchilina, A G, Zorzano, M-P, Farley, K A, Stack, K M, Shuster, D L, Horgan, B H N, Hurowitz, J A, Tarnas, J D, Simon, J I, Sun, V Z, Scheller, E L, Moore, K R, McLennan, S M, Vasconcelos, P M, Wiens, R C, Treiman, A H, Mayhew, L E, Beyssac, O, Kizovski, T V, Tosca, N J, Williford, K H, Crumpler, L S, Beegle, L W, Bell, J F, Ehlmann, B L, Liu, Y, Maki, J N, Schmidt, M E, Allwood, A C, Amundsen, H E F, Bhartia, R, Bosak, T, Brown, A J, Clark, B C, Cousin, A, Forni, O, Gabriel, T S J, Goreva, Y, Gupta, S, Hamran, S-E, Herd, C D K, Hickman-Lewis, K, Johnson, J R, Kah, L C, Kelemen, P B, Kinch, K B, Mandon, L, Mangold, N, Quantin-Nataf, C, Rice, M S, Russell, P S, Sharma, S K, Siljeström, S, Steele, A, Sullivan, R, Wadhwa, M, Weiss, B P, Williams, A J, Wogsland, B V, Willis, P A, Acosta-Maeda, T A, Beck, P, Benzerara, K, Bernard, S, Burton, A S, Cardarelli, E L, Chide, B, Clavé, E, Cloutis, E A, Cohen, B A, Czaja, A D, Debaille, V, Dehouck, E, Fairén, A G, Flannery, D T, Fleron, S Z, Fouchet, T, Frydenvang, J, Garczynski, B J, Gibbons, E F, Hausrath, E M, Hayes, A G, Henneke, J, Jørgensen, J L, Kelly, E M, Lasue, J, Le Mouélic, S, Madariaga, J M, Maurice, S, Merusi, M, Meslin, P-Y, Milkovich, S M, Million, C C, Moeller, R C, Núñez, J I, Ollila, A M, Paar, G, Paige, D A, Pedersen, D A K, Pilleri, P, Pilorget, C, Pinet, P C, Rice, J W, Royer, C, Sautter, V, Schulte, M, Sephton, M A, Sholes, S F, Spanovich, N, St Clair, M, Tate, C D, Uckert, K, VanBommel, S J, Yanchilina, A G, and Zorzano, M-P

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 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. Fe-Mg carbonates along grain boundaries indicate reactions with CO2-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 were stored aboard Perseverance for potential return to Earth.

Published
2022

28. The detection of spectral signatures with IRS/SuperCam, Perseverance rover: instrument performance

Author

Royer, C., Fouchet, T., Montmessin, Franck, Poulet, F., Forni, O., Johnson, J., Gasnault, Olivier, Mandon, L., Quantin- Nataf, C., Wiens, R., Beck, P., Ollila, A., Pilorget, Cédric, Bernardi, P., Reess, J.-M, Newell, R., Maurice, Sylvestre, 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), Pôle Planétologie du LESIA, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), 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 de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Laboratoire de 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), Los Alamos National Laboratory (LANL), 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, and Lunar and Planetary Institute

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract

International audience

Published
2022

29. Infrared Reflectance of Rocks and Regolith at Jezero Crater: One Year of SuperCam Observations

Author

Mandon, L., Quantin-Nataf, C., Royer, C., Beck, P., Fouchet, T., Johnson, J. R., Forni, O., Montmessin, Franck, Pilorget, C., Poulet, F., Le Mouélic, S., Dehouck, E., Beyssac, O., Brown, A., Tarnas, J., Maurice, S., Wiens, R. C., Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), 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), 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), 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 Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Plancius Research LLC, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), and Los Alamos National Laboratory (LANL)

Subjects
[SDU]Sciences of the Universe [physics]
Abstract

International audience; We present the initial results of the SuperCam IR spectrometer, with data collected on rocks and soils present in the vicinity of the rover.

Published
2022

30. Composition and density stratification observed by supercam in the first 300 sols in Jezero crater

Author

Wiens, R.C., Udry, A., Mangold, N., Beyssac, O., Quantin, C., Sautter, V., Cousin, A., Brown, A., Bosak, T., Mandon, L., Forni, O., Johnson, J.R., Mclennan, S., Legett, C., Maurice, S., Mayhew, L., Crumpler, L., Anderson, R.B., Clegg, S.M., Ollila, A.M., Hall, J., Meslin, P.-Y., Kah, L.C., Gabriel, T.S.J., Gasda, P., Simon, J.I., Hausrath, E.M., Horgan, B., Poulet, F., Beck, P., Gupta, S., Chide, B., Clavé, E., Connell, S., Dehouck, E., Dromart, G., Fouchet, T., Royer, C., Frydenvang, J., Gasnault, Olivier, Gibbons, E., Kalucha, H., Lanza, N., Lasue, J., Mouelic, S. Le, Leveillé, R., Cloutis, E., Reyes, G. Lopez, Arana, G., Castro, K., Madariaga, J.M., Manrique, J.-A., Pilorget, C., Pinet, P., Laserna, J., Sharma, S.K., Acosta-Maeda, T., Kelly, E., Montmessin, Franck, Fischer, W., Francis, R., Stack, K., Farley, K., Los Alamos National Laboratory (LANL), Purdue University [West Lafayette], Plancius Research LLC, Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Massachusetts Institute of Technology (MIT), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), University of Colorado [Boulder], New Mexico Museum of Natural History and Science (NMMNHS), United States Geological Survey (USGS), The University of Tennessee [Knoxville], NASA Johnson Space Center (JSC), NASA, University of Nevada [Las Vegas] (WGU Nevada), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Grenoble Alpes (UGA), Imperial College London, Université de Bordeaux (UB), University of Winnipeg, Université de Lyon, Observatoire de Paris, Université Paris sciences et lettres (PSL), McGill University = Université McGill [Montréal, Canada], California Institute of Technology (CALTECH), Universidad de Valladolid [Valladolid] (UVa), University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Universidad de Málaga [Málaga] = University of Málaga [Málaga], University of Hawaii, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), and pinet, patrick

Subjects
[SDU] Sciences of the Universe [physics], jezero crater, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], perseverance in situ exploration, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], supercam, [SDU.STU.PL] Sciences of the Universe [physics]/Earth Sciences/Planetology, mars geology, mineralogy, petrology
Abstract

International audience

Published
2022

31. Visible wavelength spectroscopy (400-1020 nm) of surface materials at jezero crater, mars, from supercam and mastcam-z

Author

Johnson, J., Leget, C., Wiens, R., Newell R., T., Cloutis, E., Forni, O., Beck, P., Pinet, P.C., Mandon, L., Poulet, F., Mcconnochie, T., Maurice, S., Bell J., F., Rice, M., Horgan, B., Kinch, K., Hayes, A., Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Los Alamos National Laboratory (LANL), University of Winnipeg, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Space Science Institute [Boulder] (SSI), Arizona State University [Tempe] (ASU), Western Washington University (WWU), Purdue University [West Lafayette], University of Copenhagen = Københavns Universitet (UCPH), Cornell University [New York], and Mars-2020

Subjects
spectroscopy, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], rover, visible spectroscopy, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], mars in situ exploration
Abstract

International audience

Published
2022

32. Soil diversity at mars: comparison of dataset from gale and jezero craters

Author

Cousin, A, Meslin, P, Hausrath, E, Cardarelli, E, Lasue, J, Forni, O, Beyssac, O, Kah, L, Mandon, L, Gasnault, Olivier, Dehouck, E, Poulet, F, Quantin-Nataf, C, Pilleri, P, Gasda, P, Schröder, S, Wiens, R, Maurice, S, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), University of Nevada [Las Vegas] (WGU Nevada), NASA, 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), The University of Tennessee [Knoxville], Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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 d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Los Alamos National Laboratory (LANL), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), and Lunar and Planetary Institute

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract

International audience

Published
2022

33. Modal Mineralogy of Seitah Unit in Jezero Crater (Mars) Retrieved from Nonlinear Unmixing Analyses of IRS/SUPERCAM

Author

Poulet, F., Royer, C., Beck, P., Mandon, L., Quantin-Nataf, C., Johnson, J. R., Beyssac, O., Forni, O., Cousin, A., Montmessin, Franck, Pilorget, C., Le Mouélic, S., Dehouck, E., Brown, A., Tarnas, J., Benzerara, K., Fouchet, T., Maurice, S., Wiens, R. C., 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), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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 (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), 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), Plancius Research LLC, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), and Los Alamos National Laboratory (LANL)

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract

International audience; We present the modal mineralogy of the olivine-rich, carbonate-bearing rocks observed in Jezero Crater retrieved from IRS/Supercam data.

Published
2022

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

Author

Udry, A., Sautter, V., Cousin, A., Wiens, R. C., Forni, O., Benzerara, K., Beyssac, O., Nachon, M., Dromart, G., Quantin, C., Mandon, L., Clavé, E., Pinet, P., Ollila, A., Bosak, T., Mangold, N., Dehouck, E., Johnson, J., Schmidt, M., Horgan, B., Gabriel, T., Mclennan, S., Maurice, S., Simon, J.I., Herd, C., Madiaraga., J. M., University of Nevada [Las Vegas] (WGU Nevada), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon), Massachusetts Institute of Technology (MIT), Brock University [Canada], Purdue University [West Lafayette], United States Geological Survey (USGS), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Astromaterials Research and Exploration Science (ARES), NASA Johnson Space Center (JSC), NASA-NASA, University of Alberta, and University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU)

Subjects
Supercam, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, in situ exploration, [SDU]Sciences of the Universe [physics], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], mars mineralogy, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Perseverance
Abstract

International audience

Published
2022

35. Carbonate detection with supercam in the jezero crater, mars

Author

Clavé, E., Benzerara, K., Beck, P., Meslin, P.-Y., Beyssac, O., Forni, O., Cousin, A., Bosak, T., Bousquet, B., Castro, K., Clegg, S., Cloutis, E., Gasnault, Olivier, Lopez-Reyes, G., Madriaga, J.M., Mandon, L., Maurice, S., Mouélic, S. Le, Ollila, A., Pilorget, C., Pinet, P., Quantin-Nataf, C., Schröder, S., Wiens, R.C., Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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 recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Los Alamos National Laboratory (LANL), University of Winnipeg, Universidad de Valladolid [Valladolid] (UVa), 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 de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), and pinet, patrick

Subjects
[SDU] Sciences of the Universe [physics], carbonate, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], in situ mars exploration, supercam, [SDU.STU.PL] Sciences of the Universe [physics]/Earth Sciences/Planetology, mars geology
Abstract

International audience

Published
2022

36. HYDROGEN IN ROCKS FROM JEZERO CRATER INVESTIGATED WITH SUPERCAM LIBS

Author

Pierre Beck, Forni, O., Y Meslin, P., Benzerara, K., Beyssac, O., Lasue, J., Quantin-Nataf, C., Poulet, F., Royer, C., Mandon, L., William Rapin, Clavé, E., Cousin, A., Schröder, S., Le Mouélic, S., Olivier Gasnault, Ollila, A. M., Hausrath, E., Maurice, S., Wiens, R. C., 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), Centre National d’Étude Spatiale, and Lunar and Planetary Institute

Subjects
LIBS, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract

International audience

Published
2022

37. Carbonate Detection with SuperCam in Igneous Rocks on the floor of Jezero Crater, Mars

Author

Clavé, E., Benzerara, K., Meslin, P.‐Y., Forni, O., Royer, C., Mandon, L., Beck, P., Quantin‐Nataf, C., Beyssac, O., Cousin, A., Bousquet, B., Wiens, R.C., Maurice, S., Dehouck, E., Schröder, Susanne, Gasnault, O., Mangold, N., Dromart, G., Bosak, T., Bernard, S., Udry, A., Anderson, R.B., Arana, G., Brown, A.J., Castro, K., Clegg, S.M., Cloutis, E., Fairén, A.G., Flannery, D.T., Gasda, P.J., Johnson, J.R., Lasue, J., Lopez‐Reyes, G., Madariaga, J.M., Manrique, J.A., Le Mouélic, S., Núñez, J.I., Ollila, A.M., Pilleri, P., Pilorget, C., Pinet, P., Poulet, F., Veneranda, M., and Wolf, Z.U.

Subjects
spectroscopy, LIBS, M2020, Mars 2020, Mars, carbonates, Perseverance, VISIR, exploration, Geophysics, SuperCam, in-situ, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous), Raman
Published
2022
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38. Evidence for perchlorate and sulfate salts in jezero crater, mars, from supercam observations

Author

Meslin, P.-Y, Forni, O, Beck, P, Cousin, A, Beyssac, O, Lopez-Reyes, G, Benzerara, K, Ollila, A, Mandon, L, Wiens, R, Clegg, S, Montagnac, G, Clavé, E, Manrique, J.-A, Chide, B, Maurice, S, Gasnault, Olivier, Lasue, J, Quantin-Nataf, C, Dehouck, E, Sharma, S, Arana, G, Madariaga, J, Castro, K, Schröder, S, Mangold, N, Poulet, F, Johnson, J, Le Mouélic, S, Zorzano, M.-P, Gasnault, Olivier, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, 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), Universidad de Valladolid [Valladolid] (UVa), 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 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 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), University of Hawaii, University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Institut 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), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Instituto Nacional de Técnica Aeroespacial (INTA), and Lunar and Planetary Institute

Subjects
[SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU.STU.PL] Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract

International audience

Published
2022

40. Carbonate Detection With SuperCam in Igneous Rocks on the Floor of Jezero Crater, Mars.

Author

Clavé, E., Benzerara, K., Meslin, P.‐Y., Forni, O., Royer, C., Mandon, L., Beck, P., Quantin‐Nataf, C., Beyssac, O., Cousin, A., Bousquet, B., Wiens, R. C., Maurice, S., Dehouck, E., Schröder, S., Gasnault, O., Mangold, N., Dromart, G., Bosak, T., and Bernard, S.

Subjects
IGNEOUS rocks, MARTIAN atmosphere, CARBONATE minerals, MARTIAN meteorites, NEAR infrared reflectance spectroscopy, LASER-induced breakdown spectroscopy, CARBONATES, MARS (Planet), CRATER lakes
Abstract

Perseverance explored two geological units on the floor of Jezero Crater over the first 420 Martian days of the Mars2020 mission. These units, the Máaz and Séítah formations, are interpreted to be igneous in origin, with traces of alteration. We report the detection of carbonate phases along the rover traverse based on laser‐induced breakdown spectroscopy (LIBS), infrared reflectance spectroscopy (IRS), and time‐resolved Raman (TRR) spectroscopy by the SuperCam instrument. Carbonates are identified through direct detection of vibrational modes of CO3 functional groups (IRS and TRR), major oxides content, and ratios of C and O signal intensities (LIBS). In Séítah, the carbonates are consistent with magnesite‐siderite solid solutions (Mg# of 0.42–0.70) with low calcium contents (<5 wt.% CaO). They are detected together with olivine in IRS and TRR spectra. LIBS and IRS also indicate a spatial association of the carbonates with clays. Carbonates in Máaz are detected in fewer points, as: (a) siderite (Mg# as low as 0.03); (b) carbonate‐containing coatings, enriched in Mg (Mg# ∼0.82) and spatially associated with different salts. Overall, using conservative criteria, carbonate detections are rare in LIBS (∼30/2,000 points), IRS (∼15/2,000 points), and TRR (1/150 points) data. This is best explained by (a) a low carbonate content overall, (b) small carbonate grains mixed with other phases, (c) intrinsic complexity of in situ measurements. This is consistent with orbital observations of Jezero crater, and similar to compositions of carbonates previously reported in Martian meteorites. This suggests a limited carbonation of Jezero rocks by locally equilibrated fluids. Plain Language Summary: Carbonates are mineral phases that generally form by alteration of primary, magmatic minerals. This alteration process may occur under a variety of environmental conditions, which affect the resulting carbonate phase: its abundance, composition, spatial distribution and the mineral phases it is associated with. Consequently, carbonates keep track of the environmental conditions under which they formed, and in particular, the amount of CO2 and liquid water involved in their formation. Understanding the history of both water and CO2 on Mars is critical to better understand the evolution of the red planet and its atmosphere, but also the origin of the water on Earth, and possibly the origin of life. Since the beginning of the Mars2020 mission in Jezero Crater, the SuperCam instrument has analyzed more than 200 rocks of the crater floor, and detected carbonates along Perseverance's traverse. Carbonates are found in low amounts, and are therefore complex to identify; we use SuperCam's combination of investigation techniques and a specifically developed methodology to strengthen the identification of carbonate phases and their characterization. Even though Jezero crater hosted a lake billions of years ago, the detected carbonates appear to have formed in smaller amounts of water, after the lake had disappeared. Key Points: Carbonates are detected along Perseverance's traverse in Jezero Crater with SuperCam using laser‐induced breakdown spectroscopy, IR and Raman spectroscopyCarbonate abundance is low overall, consistent with the weak carbonate signatures observed from orbit in the explored unitsThe detected carbonates have variable compositions within the magnesite‐siderite series, and likely reflect multiple alteration episodes [ABSTRACT FROM AUTHOR]

Published
2023
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43. Author Correction: In situ recording of Mars soundscape

Author

Maurice, S., Chide, B., Murdoch, N., Lorenz, R, Mimoun, D., Wiens, R., Stott, A., Jacob, X., Bertrand, T., Montmessin, Franck, Lanza, N, Alvarez-Llamas, C., Angel, S, Aung, M., Balaram, J., Beyssac, O., Cousin, A., Delory, G., Forni, O., Fouchet, T., Gasnault, O., Grip, H., Hecht, M., Hoffman, J., Laserna, J., Lasue, Jérémie, Maki, J., Mcclean, J., Meslin, P.-Y., Le Mouélic, S., Munguira, A., Newman, C., Rodríguez Manfredi, J., Moros, J., Ollila, A., Pilleri, P., Schröder, S., de La Torre Juárez, M., Tzanetos, T., Stack, K., Farley, K., Williford, K., Acosta-Maeda, T., Anderson, R., Applin, D., Arana, G., Bassas-Portus, M., Beal, R., Beck, P., Benzerara, K., Bernard, S., Bernardi, P., Bosak, T., Bousquet, B., Brown, A., Cadu, A., Caïs, P., Castro, K., Clavé, E., Clegg, S, Cloutis, E., Connell, S., Debus, A., Dehouck, E., Delapp, D., Donny, C., Dorresoundiram, A., Dromart, G., Dubois, B., Fabre, C., Fau, A., Fischer, W., Francis, R., Frydenvang, J., Gabriel, T., Gibbons, E., Gontijo, I., Johnson, J., Kalucha, H., Kelly, E., Knutsen, Elise Wright, Lacombe, Gaetan, Legett, C., Leveille, R., Lewin, E., Lopez-Reyes, G., Lorigny, E., Madariaga, J., Madsen, M., Madsen, S., Mandon, L., Mangold, N., Mann, M., Manrique, J.-A., Martinez-Frias, J., Mayhew, L., Mcconnochie, T., Mclennan, S., Melikechi, N., Meunier, F., Montagnac, G., Mousset, V., Nelson, T., Newell, R, Parot, Y., Pilorget, C., Pinet, P., Pont, G., Poulet, F., Quantin-Nataf, C., Quertier, B., Rapin, W., Reyes-Newell, A., Robinson, S., Rochas, L., Royer, C., Rull, F., Sautter, V., Sharma, S., Shridar, V., Sournac, A., Toplis, M., Torre-Fdez, I., Turenne, N., Udry, A., Veneranda, M., Venhaus, D., Vogt, D., Willis, P., Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Department of Earth, Atmospheric, and Planetary Sciences [West Lafayette] (EAPS), Purdue University [West Lafayette], 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), 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), 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), Universidad de Málaga [Málaga] = University of Málaga [Málaga], Department of Chemistry and Biochemistry [Columbia, South Carolina], University of South Carolina [Columbia], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), 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), Heliospace Corporation, MIT Haystack Observatory, Massachusetts Institute of Technology (MIT), Department of Aeronautics and Astronautics [Cambridge], 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), Escuela de Ingeniería de Bilbao, Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), Aeolis Corporation, Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), DLR Institute of Optical Sensor Systems, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Blue Marble Space Institute of Science (BMSIS), University of Hawai‘i [Mānoa] (UHM), US Geological Survey [Flagstaff], United States Geological Survey [Reston] (USGS), University of Winnipeg, University of the Basque Country/Euskal Herriko Unibertsitatea (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, Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), 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), Plancius Research LLC, 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), 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, Université de Lyon, 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), McGill University = Université McGill [Montréal, Canada], Universidad de Valladolid [Valladolid] (UVa), IT University of Copenhagen (ITU), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Geological Sciences [Boulder], University of Colorado [Boulder], University of Maryland [College Park], University of Maryland System, Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Department of Physics and Applied Physics [Lowell], University of Massachusetts [Lowell] (UMass Lowell), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), 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 Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), University of Nevada [Las Vegas] (WGU Nevada), and NASA’s Mars Exploration ProgramCNES

Subjects
Multidisciplinary, Carbon dioxide, Modélisation, [SDU]Sciences of the Universe [physics], Atmospheric Turbulence, Atmospheric Sound, Microphone, Mars, Attenuation, CO2, Perseverance, Acoustic Environment
Abstract

International audience

Published
2022
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45. Collection and In Situ Analyses of Regolith Samples by the Mars 2020 Rover: Implications for Their Formation and Alteration History

Author

Hausrath, E. M., Sullivan, R., Goreva, Y., Zorzano, M. P., Vaughan, A., Cousin, A., Siljeström, S., Sharma, S., Shumway, A. O., Kizovski, T., VanBommel, S. J., Tice, M., Knight, A., Martinez, G., Vicente‐Retortillo, A., Mandon, L., Adcock, C. T., Madariaga, J. M., Población, I., Johnson, J. R., Lasue, J., Gasnault, O., Randazzo, N., Cardarelli, E. L., Kronyak, R., Bechtold, A., Paar, G., Udry, A., Forni, O., Bedford, C. C., Carman, N. A., Bell, J. F., Benison, K., Bosak, T., Brown, A., Broz, A., Calef, F., Clark, B. C., Cloutis, E., Czaja, A. D., Fornaro, T., Fouchet, T., Golombek, M., Gómez, F., Herd, C. D. K., Herkenhoff, K., Jakubek, R. S., Jandura, L., Martinez‐Frias, J., Mayhew, L. E., Meslin, P.‐Y., Newman, C. E., Núñez, J. I., Poulet, F., Royer, C., Russell, P., Sephton, M. A., Sharma, S. K., Shuster, D., Simon, J. I., Tirona, I., Wiens, R. C., Weiss, B. P., Williams, A. J., Williford, K., and Wolf, Z. U.

Abstract

The Perseverancerover has sampled mm‐size lithic fragments containing olivine likely from at least two source regions from the surface of an inactive megaripple surface, and fine‐grained material from the surface and to a depth of ∼4–6 cm. Some of the mm‐size grains lack a coherent diffraction pattern measured by PIXL, consistent with the presence of poorly ordered secondary phases that have been altered. Analysis of these materials on Earth will allow examination of materials that have experienced aqueous, potentially habitable environments that could contain biosignatures. Fluorescence of three different patterns was detected, consistent with inorganic emissions from silica defects or rare earth elements in certain mineral phases, although organic origin cannot be excluded. Analysis of Autofocus Context Imager and Wide Angle Topographic Sensor for Operations and eNgineering images of the subsurface material and MEDA thermal inertia measurements indicate average grain sizes of ∼125 and ∼150 μm, respectively, for the bulk material within the megaripple. The fine‐grained material in the sampling location indicates chemical compositions similar to previously proposed global components as well as airfall dust. In situ and associated atmospheric measurements provide evidence of recent processes likely including water vapor in soil crust formation. The sampled material will therefore help elucidate the formation of Martian soils; current surface‐atmosphere interactions; the composition, shape, and size distribution of dust grains valuable for studies of past and present Martian climate and for assessing potential health and other risks to human missions; and ancient, aqueously altered environments that could have been habitable, and, if Mars contained life, possibly contain biosignatures. The first samples of soil/regolith/loose sediment have recently been collected from Jezero crater Mars. The Perseverancerover is able to sample loose material less than 8 mm in size from the surface to a depth of ∼4–6 cm, which is then sealed in a sample tube and either deposited on the surface of Mars or stored in the rover similarly to the rock samples for potential return to Earth by the planned Mars Sample Return campaign. Soil samples include mm‐size grains that are aqueously altered, are likely from at least two different source regions, and indicate potentially habitable environments that, if Mars contained life, could potentially contain biosignatures. Fluorescence of three different patterns was detected, which could be due to inorganic emissions from silica defects or rare earth elements in certain mineral phases, though organic origin cannot be excluded. The 125–150 μm fine grains appear similar to a previously proposed global soil component, and the collection of airfall dust and soil crust components includes material that has been affected by interactions with the atmosphere, and sheds light on topics ranging from climate to the safety of future human missions. Regolith samples contain aqueous alteration potentially resulting from past habitable environments that could contain biosignaturesFluorescence detections are consistent with variable concentration of inorganic emitters, though small aromatic organics are also possibleBoth samples include grain sizes from microns (dust) to a few mm, and soil crust due to atmospheric interactions likely involving water Regolith samples contain aqueous alteration potentially resulting from past habitable environments that could contain biosignatures Fluorescence detections are consistent with variable concentration of inorganic emitters, though small aromatic organics are also possible Both samples include grain sizes from microns (dust) to a few mm, and soil crust due to atmospheric interactions likely involving water

Published
2025
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49. Dietary guidelines for school catering: do they affect the cost of primary school meals?

Author

Darmon, Nicole, Allègre, L., Vieux, Florent, Mandon, L., Ciantar, L., Nutriments Lipidiques et Prévention des Maladies Métaboliques, Institut National de la Santé et de la Recherche Médicale (INSERM)-Institut National de la Recherche Agronomique (INRA)-Université de la Méditerranée - Aix-Marseille 2, Nutrition, obésité et risque thrombotique (NORT), Aix Marseille Université (AMU)-Institut National de la Recherche Agronomique (INRA)-Institut National de la Santé et de la Recherche Médicale (INSERM), ProdInra, Migration, and Université de la Méditerranée - Aix-Marseille 2-Institut National de la Recherche Agronomique (INRA)-Institut National de la Santé et de la Recherche Médicale (INSERM)

Subjects
[SDV] Life Sciences [q-bio], school catering, children, school, [SDV]Life Sciences [q-bio], dietary recommendations, france, nutritional policies, ComputingMilieux_MISCELLANEOUS
Abstract

International audience

Published
2011

50. An Examination of Soil Crusts on the Floor of Jezero Crater, Mars

Author

Hausrath, E. M., Adcock, C. T., Bechtold, A., Beck, P., Benison, K., Brown, A., Cardarelli, E. L., Carman, N. A., Chide, B., Christian, J., Clark, B. C., Cloutis, E., Cousin, A., Forni, O., Gabriel, T. S. J., Gasnault, O., Golombek, M., Gómez, F., Hecht, M. H., Henley, T. L. J., Huidobro, J., Johnson, J., Jones, M. W. M., Kelemen, P., Knight, A., Lasue, J. A., Le Mouélic, S., Madariaga, J. M., Maki, J., Mandon, L., Martinez, G., Martínez‐Frías, J., McConnochie, T. H., Meslin, P.‐Y., Zorzano, M.‐P., Newsom, H., Paar, G., Randazzo, N., Royer, C., Siljeström, S., Schmidt, M. E., Schröder, S., Sephton, M. A., Sullivan, R., Turenne, N., Udry, A., VanBommel, S., Vaughan, A., Wiens, R. C., and Williams, N.

Abstract

Martian soils are critically important for understanding the history of Mars, past potentially habitable environments, returned samples, and future human exploration. This study examines soil crusts on the floor of Jezero crater encountered during initial phases of the Mars 2020 mission. Soil surface crusts have been observed on Mars at other locations, starting with the two Viking Lander missions. Rover observations show that soil crusts are also common across the floor of Jezero crater, revealed in 45 of 101 locations where rover wheels disturbed the soil surface, two out of seven helicopter flights that crossed the wheel tracks, and four of eight abrasion/drilling sites. Most soils measured by the SuperCam laser‐induced breakdown spectroscopy (LIBS) instrument show high hydrogen content at the surface, and fine‐grained soils also show a visible/near infrared (VISIR) 1.9 μm H2O absorption feature. The Planetary Instrument for X‐ray Lithochemistry (PIXL) and SuperCam observations suggest the presence of salts at the surface of rocks and soils. The correlation of S and Cl contents with H contents in SuperCam LIBS measurements suggests that the salts present are likely hydrated. On the “Naltsos” target, magnesium and sulfur are correlated in PIXL measurements, and Mg is tightly correlated with H at the SuperCam points, suggesting hydrated Mg‐sulfates. Mars Environmental Dynamics Analyzer (MEDA) observations indicate possible frost events and potential changes in the hydration of Mg‐sulfate salts. Jezero crater soil crusts may therefore form by salts that are hydrated by changes in relative humidity and frost events, cementing the soil surface together. Martian soils are important for understanding the history of Mars as well as future sample return and human exploration. Soil crusts in Jezero crater, which are also broadly found across Mars, can be observed when they are disturbed, such as by rover wheels or coring/abrasion activities. Jezero crater soil crusts are examined using images from the Perseverance and Ingenuity cameras, as well as using data from the SuperCam, PIXL, Mastcam‐Z, and MEDA instruments. Soil crusts are common in Jezero crater and show characteristics including hydration at the surface and the presence of salts that might contain water. MEDA instrument measurements indicate that changes in the hydration state of salts may result during conditions measured at Jezero crater. Jezero crater soil crusts may therefore form by salts that are present on the surface that can add or lose water during changes in relative atmospheric humidity and frost events. These changes in the amount of water present in the salts may result in soil surfaces that are cemented together, forming the crusts observed at Jezero crater. A better understanding of Mars soil crusts will help in the understanding of samples returned to Earth from Mars, as well as future human exploration. Soil crusts are prevalent across the Jezero crater floorSoil surfaces are largely hydratedSoil crusts likely contain salts and may form during changes in atmospheric relative humidity at the surface Soil crusts are prevalent across the Jezero crater floor Soil surfaces are largely hydrated Soil crusts likely contain salts and may form during changes in atmospheric relative humidity at the surface

Published
2023
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