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166 results on '"Gasnault, O"'

1. Sustained wet–dry cycling on early Mars

Author: Rapin, W., Dromart, G., Clark, B. C., Schieber, J., Kite, E. S., Kah, L. C., Thompson, L. M., Gasnault, O., Lasue, J., Meslin, P.-Y., Gasda, P. J., and Lanza, N. L.
Published: 2023
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2. Iron Mobility During Diagenesis at Vera Rubin Ridge, Gale Crater, Mars

Author: l'Haridon, J, Mangold, N, Fraeman, A, Johnson, J, Cousin, A, Rapin, W, David, G, Dehouck, E, Sun, V, Frydenvang, J, Gasnault, O, Gasda, P, Lanza, N, Forni, O, Meslin, P. -Y, Schwenzer, S, Bridges, J, Horgan, B, House, C, Maurice, S, and Wiens, R
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The Curiosity rover investigated a topographic structure known as Vera Rubin ridge, associated with a hematite signature in orbital spectra. There, Curiosity encountered mudstones interpreted as lacustrine deposits, in continuity with the 300 m-thick underlying sedimentary rocks of the Murray formation at the base of Mount Sharp. While the presence of hematite ($\alpha$-Fe2O3) was confirmed insitu by both Mastcam and ChemCam spectral observations and by the CheMin instrument, neither ChemCam nor APXS observed any significant increase in FeO$_T$ (total iron oxide) abundances compared to the Murray formation. Instead, Curiosity discovered dark-toned diagenetic features displaying anomalously high FeO$_T$ abundances, commonly observed in association with light-toned Ca-sulfate veins but also as crystal pseudomorphs in the host rock. These iron-rich diagenetic features are predominantly observed in "grey" outcrops on the upper part of the ridge, which lack the telltale ferric signature of other Vera Rubin ridge outcrops. Their composition is consistent with anhydrous Fe-oxide, as the enrichment in iron is not associated with enrichment in any other elements, nor with detections of volatiles. The lack of ferric absorption features in the ChemCam reflectance spectra and the hexagonal crystalline structure associated with dark-toned crystals points toward coarse "grey" hematite. In addition, the host rock adjacent to these features appears bleached and show low-FeO$_T$ content as well as depletion in Mn, indicating mobilization of these redox-sensitive elements during diagenesis. Thus, groundwater fluid circulations could account for the remobilization of iron and recrystallization as crystalline hematite during diagenesis as well as color variations observed in the Vera Rubin ridge outcrops.
Published: 2021
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3. 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., and Williford, K.
Published: 2022
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4. Manganese-Rich Sandstones as an Indicator of Ancient Oxic Lake Water Conditions in Gale Crater, Mars

Author: Gasda, P. J., Lanza, N. L., Meslin, P. Y., Lamm, S. N., Cousin, A., Anderson, R., Forni, O., Swanner, E., L’Haridon, J., Frydenvang, J., Thomas, N., Gwizd, S., Stein, N., Fischer, W. W., Hurowitz, J., Sumner, D., Rivera-Hernández, F., Crossey, L., Ollila, A., Essunfeld, A., Newsom, H. E., Clark, B., Wiens, R. C., Gasnault, O., Clegg, S. M., Maurice, S., Delapp, D., Reyes-Newell, A., Gasda, P. J., Lanza, N. L., Meslin, P. Y., Lamm, S. N., Cousin, A., Anderson, R., Forni, O., Swanner, E., L’Haridon, J., Frydenvang, J., Thomas, N., Gwizd, S., Stein, N., Fischer, W. W., Hurowitz, J., Sumner, D., Rivera-Hernández, F., Crossey, L., Ollila, A., Essunfeld, A., Newsom, H. E., Clark, B., Wiens, R. C., Gasnault, O., Clegg, S. M., Maurice, S., Delapp, D., and Reyes-Newell, A.
Abstract: Manganese has been observed on Mars by the NASA Curiosity rover in a variety of contexts and is an important indicator of redox processes in hydrologic systems on Earth. Within the Murray formation, an ancient primarily fine-grained lacustrine sedimentary deposit in Gale crater, Mars, have observed up to 45× enrichment in manganese and up to 1.5× enrichment in iron within coarser grained bedrock targets compared to the mean Murray sediment composition. This enrichment in manganese coincides with the transition between two stratigraphic units within the Murray: Sutton Island, interpreted as a lake margin environment, and Blunts Point, interpreted as a lake environment. On Earth, lacustrine environments are common locations of manganese precipitation due to highly oxidizing conditions in the lakes. Here, we explore three mechanisms for ferromanganese oxide precipitation at this location: authigenic precipitation from lake water along a lake shore, authigenic precipitation from reduced groundwater discharging through porous sands along a lake shore, and early diagenetic precipitation from groundwater through porous sands. All three scenarios require highly oxidizing conditions and we discuss oxidants that may be responsible for the oxidation and precipitation of manganese oxides. This work has important implications for the habitability of Mars to microbes that could have used Mn redox reactions, owing to its multiple redox states, as an energy source for metabolism.
Published: 2024

5. Author Correction: 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., and Williford, K.
Published: 2022
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6. 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

7. Diverse Lava Flow Morphologies in the Stratigraphy of the Jezero Crater Floor

Author: Alwmark, S., Horgan, B., Udry, A., Bechtold, A., Fagents, S., Ravanis, E., Crumpler, L., Schmitz, N., Cloutis, E., Brown, A., Flannery, D., Gasnault, O., Grotzinger, J., Gupta, S., Kah, L., Kelemen, P., Kinch, K., Núñez, J., Alwmark, S., Horgan, B., Udry, A., Bechtold, A., Fagents, S., Ravanis, E., Crumpler, L., Schmitz, N., Cloutis, E., Brown, A., Flannery, D., Gasnault, O., Grotzinger, J., Gupta, S., Kah, L., Kelemen, P., Kinch, K., and Núñez, J.
Abstract: We present a combined geomorphologic, multispectral, and geochemical analysis of crater floor rocks in Jezero crater based on data obtained by the Mast Camera Zoom and SuperCam instruments onboard the NASA Mars 2020 Perseverance rover. The combined data from this analysis together with the results of a comparative study with geologic sites on Earth allows us to interpret the origins of rocks exposed along the Artuby ridge, a ∼900 m long scarp of lower Máaz formation rocks. The ridge exposes rocks belonging to two morphologically distinct members, Artuby and Rochette, both of which have basaltic composition and are spectrally indistinguishable in our analysis. Artuby rocks consist of morphologically distinct units that alternate over the ridge, bulbous, hummocky, layers with varying thicknesses that in places appear to have flowed over underlying strata, and sub-planar thinner laterally continuous layers with variable friability. The Rochette member has a massive appearance with pronounced pitting and sub-horizontal partings. Our findings are most consistent with a primary igneous emplacement as lava flows, through multiple eruptions, and we propose that the thin layers result either from preferential weathering, interbedded ash/tephra layers, ʻaʻā clinker layers, or aeolian deposition. Our analyses provide essential geologic context for the Máaz formation samples that will be returned to Earth and highlight the diversity and complexity of geologic processes on Mars not visible from orbit.
Published: 2023

8. Compositional Variations in Sedimentary Deposits in Gale Crater as Observed by ChemCam Passive and Active Spectra

Author: Manelski, H. T., Sheppard, R. Y., Fraeman, A. A., Wiens, R. C., Johnson, J. R., Rampe, E. B., Frydenvang, J., Lanza, N. L., Gasnault, O., Manelski, H. T., Sheppard, R. Y., Fraeman, A. A., Wiens, R. C., Johnson, J. R., Rampe, E. B., Frydenvang, J., Lanza, N. L., and Gasnault, O.
Abstract: During the first 2934 sols of the Curiosity rover's mission 33,468 passive visible/near-infrared (NIR) reflectance spectra were taken of the surface by the mast-mounted Chemistry and Camera (ChemCam) instrument on a range of target types. ChemCam spectra of bedrock targets from the Murray and Carolyn Shoemaker formations on Mt. Sharp were investigated using principal component analysis and various spectral parameters including the band depth at 535 nm and the slope between 840 and 750 nm. Four end-member spectra were identified. Passive spectra were compared to Laser Induced Breakdown Spectroscopy (LIBS) data to search for correlations between spectral properties and elemental abundances. The correlation coefficient between FeOT reported by LIBS and BD535 from passive spectra was used to search for regions where iron may have been added to the bedrock through oxidation of ferrous-bearing fluids but no correlations were found. Rocks in the Blunts Point-Sutton Island transition that have unique spectral properties compared to surrounding rocks, that is flat NIR slopes and weak 535 nm absorptions, are associated with higher Mn and Mg in the LIBS spectra of bedrock. Additionally, calcium-sulfate cements, previously identified by Ca and S enrichments in the LIBS spectra of bedrock, were also shown to be associated with spectral trends seen in Blunts Point. A shift toward a steeper NIR slope is seen in the Hutton interval, indicative of changing depositional conditions or increased diagenesis.
Published: 2023

9. The sound of geological targets on Mars from the absolute intensity of laser-induced sparks shock waves

Author: Alvarez-Llamas, C., Laserna, J., Moros, J., Purohit, P., García-Gómez, L., Angel, S.M., Bernardi, P., Bousquet, B., Cadu, A., Dauson, E., Forni, O., Fouchet, T., Gasnault, O., Jacob, X., Lacombe, G., Lanza, N.L., Larmat, C., Lasue, J., Lorenz, R.D., Meslin, P.-Y., Mimoun, D., Montmessin, F., Murdoch, N., Ollila, A.M., Pilleri, P., Randazzo, N., Reyes-Newell, A.L., Schröder, Susanne, Stott, A., Ten Cate, J., Udry, A., Vogt, D., Clegg, S., Cousin, A., Maurice, S., Wiens, R.C., Departamento de Química Analítica [Rosario], Facultad de Ciencias Bioquımicas y Farmaceuticas [Rosario] (FBIOyF), Universidad Nacional de Rosario [Santa Fe]-Universidad Nacional de Rosario [Santa Fe], Department of Chemistry and Biochemistry [Columbia, South Carolina], University of South Carolina [Columbia], 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), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), 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 mécanique des fluides de Toulouse (IMFT), Université de Toulouse (UT)-Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), PLANETO - LATMOS, 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), University of Alberta, DLR Institute of Optical Sensor Systems, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), University of Nevada [Las Vegas] (WGU Nevada), Department of Earth, Atmospheric, and Planetary Sciences [West Lafayette] (EAPS), and Purdue University [West Lafayette]
Subjects: LIBS, Mars, Acoustics, Perseverance, Jezero, Atomic and Molecular Physics, and Optics, Analytical Chemistry, Geological material, in-situ, [SDU]Sciences of the Universe [physics], rover, Instrumentation, Spectroscopy, in-situ science
Abstract: International audience; Inspection of geological material is one of the main goals of the Perseverance rover during its journey across the landscape of the Jezero crater in Mars. NASA's rover integrates SuperCam, an instrument capable of performing standoff characterization of samples using a variety of techniques. Among those tools, SuperCam can perform laser-induced breakdown spectroscopy (LIBS) studies to elucidate the chemical composition of the targets of interest. Data from optical spectroscopy can be supplemented by simultaneously-produced laser-produced plasma acoustics in order to expand the information acquired from the probed rocks thanks to the SuperCam's microphone (MIC) as it can be synchronized with the LIBS laser. Herein, we report cover results from LIBS and MIC during Perseverance's first 380 sols on the Martian surface. We study the correlation between both recorded signals, considering the main intrasample and environmental sources of variation for each technique, to understand their behavior and how they can be interpreted together towards complimenting LIBS with acoustics. We find that louder and more stable acoustic signals are recorded from rock with compact surfaces, i.e., low presence loose particulate material, and harder mineral phases in their composition. Reported results constitute the first description of the evolution of the intensity in the time domain of shockwaves from laser-produced plasmas on geological targets recorded in Mars. These signals are expected contain physicochemical signatures pertaining to the inspected sampling positions. As the dependence of the acoustic signal recorded on the sample composition, provided by LIBS, is unveiled, the sound from sparks become a powerful tool for the identification of mineral phases with similar optical emission spectra.
Published: 2023

10. The Mastcam‐Z Radiometric Calibration Targets on NASA's Perseverance Rover: Derived Irradiance Time‐Series, Dust Deposition, and Performance Over the First 350 Sols on Mars

Author: Merusi, M., primary, Kinch, K. B., additional, Madsen, M. B., additional, Bell, J. F., additional, Maki, J. N., additional, Hayes, A. G., additional, Joseph, J., additional, Johnson, J. R., additional, Rice, M., additional, Cloutis, E. A., additional, Applin, D., additional, Lemmon, M. T., additional, Vaughan, A. F., additional, Núñez, J. I., additional, Jensen, E., additional, Kristensen, J. Z., additional, Paris, K., additional, Cisneros, E., additional, Kennedy, M. R., additional, and Gasnault, O., additional
Published: 2022
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11. Evidence for Amorphous Sulfates as the Main Carrier of Soil Hydration in Gale Crater, Mars

Author: David, G., primary, Dehouck, E., additional, Meslin, P.‐Y., additional, Rapin, W., additional, Cousin, A., additional, Forni, O., additional, Gasnault, O., additional, Lasue, J., additional, Mangold, N., additional, Beck, P., additional, Maurice, S., additional, Wiens, R. C., additional, Berger, G., additional, Fabre, S., additional, Pinet, P., additional, Clark, B. C., additional, Smith, J. R., additional, and Lanza, N. L., additional
Published: 2022
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12. Consolidated Chemical Provinces on Mars: Implications for Geologic Interpretations

Author: Rani, A., Basu Sarbadhikari, A., Hood, D., Gasnault, O., Nambiar, S., Karunatillake, S., Indian Institute of Technology [Gandhinagar] ( IIT Gandhinagar ), Physical Research Laboratory [Ahmedabad] (PRL), Indian Space Research Organisation (ISRO), Baylor University, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Louisiana State University (LSU)
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract: International audience; Chemical provinces were defined on Mars a decade ago using orbital nuclear spectroscopy of K, Th, Fe, Si, Ca, Cl, and H2O. However, past multivariate analyses yielded three sets of provinces, suggesting methodologic variability. Province-stability to the inclusion of Al and S is also unknown, presenting additional uncertainties for geologic insight. Here we consolidate key multivariate methods to define the first cross-validated provinces. In southern highlands, the highly incompatible K and Th show non-uniform distribution with higher values in mid Noachian and Hesperian than late Noachian – early Hesperian volcanic terrains. Silica- and Al-depletion trends from Noachian to Amazonian indicate highly differentiated mantle with variable degree of melting. Late Hesperian lowlands are highly depleted in Al and enriched in K and Th, consistent with volcanic resurfacing from a low-degree partially melted, garnet-rich mantle. Furthermore, older volatile-rich regions such as Medusae Fossae Formation exhibit igneous geochemistry, consistent with water-limited isochemical weathering throughout Mars's history.
Published: 2022

13. Homogeneity assessment of the SuperCam calibration targets onboard rover perseverance

Author: Química analítica, Kimika analitikoa, Madariaga Mota, Juan Manuel, Aramendia Gutiérrez, Julene, Arana Momoitio, Gorka, Gómez Nubla, Leticia, Fernández Ortiz de Vallejuelo, Silvia, García-Florentino, Cristina, Maguregui Hernando, Maite, Manrique, José Antonio, Lopez-Reyes, G., Moros, J., Cousin, A., Maurice, S., Ollila, A.M., Wiens, R.C, Rull, F., Laserna, J., Garcia-Baonza, V., Madsen, M.B., Forni, O., Lasue, J., Clegg, S.M., Robinson, S., Bernardi, P., Brown, A.J., Caïs, P., Martinez-Frias, J., Beck, P., Bernard, S., Bernt, M.H., Beyssac, O., Cloutis, E., Drouet, C., Dromart, G., Dubois, B., Fabre, C., Gasnault, O., Gontijo, I., Johnson, J.R., Medina, J., Meslin, P.-Y., Montagnac, G., Sautter, V., Sharma, S.K., Veneranda, Marco, Williss, P.A., Química analítica, Kimika analitikoa, Madariaga Mota, Juan Manuel, Aramendia Gutiérrez, Julene, Arana Momoitio, Gorka, Gómez Nubla, Leticia, Fernández Ortiz de Vallejuelo, Silvia, García-Florentino, Cristina, Maguregui Hernando, Maite, Manrique, José Antonio, Lopez-Reyes, G., Moros, J., Cousin, A., Maurice, S., Ollila, A.M., Wiens, R.C, Rull, F., Laserna, J., Garcia-Baonza, V., Madsen, M.B., Forni, O., Lasue, J., Clegg, S.M., Robinson, S., Bernardi, P., Brown, A.J., Caïs, P., Martinez-Frias, J., Beck, P., Bernard, S., Bernt, M.H., Beyssac, O., Cloutis, E., Drouet, C., Dromart, G., Dubois, B., Fabre, C., Gasnault, O., Gontijo, I., Johnson, J.R., Medina, J., Meslin, P.-Y., Montagnac, G., Sautter, V., Sharma, S.K., Veneranda, Marco, and Williss, P.A.
Abstract: The SuperCam instrument, onboard the Perseverance rover (Mars 2020 mission) is designed to perform remote analysis on the Martian surface employing several spectroscopic techniques such as Laser Induced Breakdown Spectroscopy (LIBS), Time-Resolved Raman (TRR), Time-Resolved Fluorescence (TRF) and Visible and Infrared (VISIR) reflectance. In addition, SuperCam also acquires high-resolution images using a color remote micro-imager (RMI) as well as sounds with its microphone. SuperCam has three main subsystems, the Mast Unit (MU) where the laser for chemical analysis and collection optics are housed, the Body Unit (BU) where the different spectrometers are located inside the rover, and the SuperCam Calibration Target (SCCT) located on the rover's deck to facilitate calibration tests at similar ambient conditions as the analyzed samples. To perform adequate calibrations on Mars, the 22 mineral samples included in the complex SCCT assembly must have a very homogeneous distribution of major and minor elements. The analysis and verification of such homogeneity for the 5-6 replicates of the samples included in the SCCT has been the aim of this work. To verify the physic-chemical homogeneity of the calibration targets, micro Energy Dispersive X-ray Fluorescence (EDXRF) imaging was first used on the whole surface of the targets, then the relative abundances of the detected elements were computed on 20 randomly distributed areas of 100*100 mum. For those targets showing a positive Raman response, micro-Raman spectroscopy imaging was performed on the whole surface of the targets at a resolution of 100*100 mum. The %RSD values (percent of relative standard deviation of mean values) for the major elements measured with EDXRF were compared with similar values obtained by two independent LIBS set-ups at spot sizes of 300 mum in diameter. The statistical analysis showed which elements were homogeneously distributed in the 22 mineral targets of the SCCT, providing their uncertainty v
Published: 2022

14. Homogeneity assessment of the SuperCam calibration targets onboard rover perseverance

Author: Madariaga, J. M., Aramendia, J., Arana, G., Castro, K., Gomez-Nubla, L., de Vallejuelo, S. Fdez-Ortiz, Garcia-Florentino, C., Maguregui, M., Manrique, J. A., Lopez-Reyes, G., Moros, J., Cousin, A., Maurice, S., Ollila, A. M., Wiens, R. C., Rull, F., Laserna, J., Garcia-Baonza, V., Madsen, M. B., Forni, O., Lasue, J., Clegg, S. M., Robinson, S., Bernardi, P., Brown, A. J., Cais, P., Martinez-Frias, J., Beck, P., Bernard, S., Bernt, M. H., Beyssac, O., Cloutis, E., Drouet, C., Dromart, G., Dubois, B., Fabre, C., Gasnault, O., Gontijo, I., Johnson, J. R., Medina, J., Meslin, P. -Y., Montagnac, G., Sautter, V., Sharma, S. K., Veneranda, M., Willis, P. A., Madariaga, J. M., Aramendia, J., Arana, G., Castro, K., Gomez-Nubla, L., de Vallejuelo, S. Fdez-Ortiz, Garcia-Florentino, C., Maguregui, M., Manrique, J. A., Lopez-Reyes, G., Moros, J., Cousin, A., Maurice, S., Ollila, A. M., Wiens, R. C., Rull, F., Laserna, J., Garcia-Baonza, V., Madsen, M. B., Forni, O., Lasue, J., Clegg, S. M., Robinson, S., Bernardi, P., Brown, A. J., Cais, P., Martinez-Frias, J., Beck, P., Bernard, S., Bernt, M. H., Beyssac, O., Cloutis, E., Drouet, C., Dromart, G., Dubois, B., Fabre, C., Gasnault, O., Gontijo, I., Johnson, J. R., Medina, J., Meslin, P. -Y., Montagnac, G., Sautter, V., Sharma, S. K., Veneranda, M., and Willis, P. A.
Abstract: The SuperCam instrument, onboard the Perseverance rover (Mars 2020 mission) is designed to perform remote analysis on the Martian surface employing several spectroscopic techniques such as Laser Induced Breakdown Spectroscopy (LIBS), Time-Resolved Raman (TRR), Time-Resolved Fluorescence (TRF) and Visible and Infrared (VISIR) reflectance. In addition, SuperCam also acquires high-resolution images using a color remote micro imager (RMI) as well as sounds with its microphone. SuperCam has three main subsystems, the Mast Unit (MU) where the laser for chemical analysis and collection optics are housed, the Body Unit (BU) where the different spectrometers are located inside the rover, and the SuperCam Calibration Target (SCCT) located on the rover's deck to facilitate calibration tests at similar ambient conditions as the analyzed samples. To perform adequate calibrations on Mars, the 22 mineral samples included in the complex SCCT assembly must have a very homogeneous distribution of major and minor elements. The analysis and verification of such homogeneity for the 5-6 replicates of the samples included in the SCCT has been the aim of this work. To verify the physic chemical homogeneity of the calibration targets, micro Energy Dispersive X-ray Fluorescence (EDXRF) imaging was first used on the whole surface of the targets, then the relative abundances of the detected elements were computed on 20 randomly distributed areas of 100 x 100 mu m. For those targets showing a positive Raman response, micro-Raman spectroscopy imaging was performed on the whole surface of the targets at a resolution of 100 x 100 mu m. The %RSD values (percent of relative standard deviation of mean values) for the major elements measured with EDXRF were compared with similar values obtained by two independent LIBS set-ups at spot sizes of 300 mu m in diameter. The statistical analysis showed which elements were homogeneously distributed in the 22 mineral targets of the SCCT, providing their unc
Published: 2022

15. Understanding The Correlation Of Libs And Acoustic Measurements Of Rocks And Soils Found In The Traverse Of The Perseverance Rover Across The Jezero Crater, Mars

Author: Laserna-Vázquez, José Javier, Álvarez, C., Moros, J., Purohit, P., Ángel, S.M., Bernardi, P., Beyssac, O., Bousquet, B., Cadu, A., Chide, B., Clavé, E, Clegg, S., Dauson, E., Forni, O., Fouchet, T., Gasnault, O., Jacob, X., Lacombe, G., Lanza, N.L., Larmat, C., Lasue, J., Lorenz, R.D., Meslin, P. -Y., Montmessin, F., Murdoch, N., Ollila, A.M., Pilleri, P., Reyes-Newell, A.L., Schröder, S., Stott, A., Cate, J. Ten, Vogh, D., Maurice, S., Wiens, R.C., and Mimoun, D.
Subjects: Rocks, Minerals, LIBS, Marte (Planeta), Sonido ultrasónico, Mars, Rocas, Acoustic
Abstract: The SuperCam instrument of the NASA MARS 2020 Perseverance rover combines a suite of atomic and molecular spectroscopies intended for an extensive description of rocks, soils and minerals in the surroundings of the landing site of the mission – the Jezero crater. The microphone installed on the SuperCam instrument allows the acquisition of acoustic signals resulting from the expansion of laser-induced plasmas towards the atmosphere. Apart from being affected by the propagation characteristics of the Mars atmosphere, the acoustic signal has an additional component related to the properties of the target including surface morphology, hardness, deformation parameters, and elasticity, among others. This information is currently being investigated as a complementary resource for characterization of the ablated material and may well supplement the LIBS data gathered from coincident laser shots. This talk will present SuperCam acoustic data of rocks and minerals found in the traverse of the Perseverance rover and will discuss its correlation with LIBS spectra. Universidad de Málaga. Campus de Excelencia Internacional Andalucía Tech
Published: 2022

16. LIBS and Acoustic Measurements of Rocks and Regolith Found in the Traverse of the Perseverance Rover Across the Jezero Crater, Mars

Author: Laserna-Vázquez, José Javier, Moros, Javier, Álvarez, César, Purohit, Pablo, Ángel, S. M., Bernardi, P., Bousquet, O., Cadú, A., Chide, B., Clavé, E., Clegg, S., Dauson, E., Forni, O., Fouchet, T., Gasnault, O., Jacob, X., Lacombe, G., Lanza, N. L., Larmat, C., Lasue, J., Lorenz, R. D., Meslin, P. - Y., Montmessin, F., Murdoch, N., Ollila, A. M., Pilleri, P., Reyes-Newell, A. L., Schroder, S., Stott, A., Cate, J Ten, Vogt, D., Maurice, S., Wiens, R.C., and Mimoun, D.
Subjects: Rocks, Minerals, LIBS, Imágenes ultrasónicas, Marte (Planeta) - Superficie, Mars, Rocas, Acoustic
Abstract: The SuperCam instrument of the NASA MARS 2020 Perseverance rover combines a suite of atomic and molecular spectroscopies intended for an extensive description of rocks, soils and minerals in the surroundings of the landing site of the mission – the Jezero crater. The microphone installed on the SuperCam instrument allows the acquisition of acoustic signals resulting from the expansion of laser-induced plasmas towards the atmosphere. Apart from being affected by the propagation characteristics of the Mars atmosphere, the acoustic signal has an additional component related to the properties of the target including surface morphology, hardness, deformation parameters, and elasticity, among others. This information is currently being investigated as a complementary resource for characterization of the ablated material and may well supplement the LIBS data gathered from coincident laser shots. This talk will present SuperCam acoustic data of rocks and minerals found in the traverse of the Perseverance rover and will discuss its correlation with LIBS spectra. Universidad de Málaga. Campus de Excelencia Internacional Andalucía Tech
Published: 2022

17. SuperCam on the Perseverance Rover for Exploration of Jezero Crater: Remote LIBS, VISIR, Raman, and Time-Resolved Luminescence Spectroscopies Plus Micro-Imaging and Acoustics

Author: Wiens, Roger C., Maurice, Sylvestre, Gasnault, O., Anderson, Ryan B., Beyssac, Olivier, Bonal, L., Clegg, Samuel M., DeFlores, Lauren, Dromart, G, Fischer, W. W., Forni, Olivier, Grotzinger, J. P., Johnson, J. R., Martinez-Frias, J., Mangold, Nicolas, McLennan, S., Montmessin, Franck, Rull, Fernando, Sharma, Shiv K., Cousin, Agnès, Pilleri, Paolo, Sautter, V, Lewin, E, Cloutis, E., Poulet, F., Bernard, Sylvain, McConnochie, T., Lanza, N., Newsom, H., Ollila, A., Leveille, R., Le Mouelic, S., Lasue, J, Melikechi, N., Meslin, P-Y, Grasset, O, Angel, S. M., Fouchet, T., Beck, Pierre, Bousquet, Bruno, Fabre, C., Pinet, P., Benzerara, K., Montagnac, Gilles, Arana, Gorka, Castro, Kepa, Laserna, Javier, Madariaga, Juan Manuel, Manrique, Jose Antonio, Lopez, G., Lorenz, R., Mimoun, D., Acosta-Maeda, T., Alvarez, C., Dehouck, E., Delory, G., Doressoundiram, A., Francis, R., Frydenvang, J., Gabriel, T. S. J., Jacob, Xavier, Madsen, M. B., Moros, J., Murdoch, N, Newell, Raymond T., Porter, J. M., Quantin-Nataf, C., Rapin, William, Schröder, Susanne, Sobron, Pablo, Toplis, M., Brown, A.J., Veneranda, M., Chide, Baptiste, Legett, Carey, Royer, Clement, Stott, A., Vogt, David, Robinson, Scott H., DeLapp, D., Clave, E., Connell, S., Essunfeld, A., Gallegos, Z., Garcia-Florentino, C., Gibbons, E., Huidobro, J., Kelly, E., Kalucha, H., Ruiz, P., Torre-Fdez, Imanol, Shkolyar, Svetlana, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), 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), United States Geological Survey (USGS), 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, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Instituto de Geociencias [Madrid] (IGEO), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Stony Brook University [SUNY] (SBU), 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), Universidad de Valladolid [Valladolid] (UVa), University of Hawai‘i [Mānoa] (UHM), Université Grenoble Alpes (UGA), University of Winnipeg, 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), NASA Goddard Space Flight Center (GSFC), The University of New Mexico [Albuquerque], McGill University = Université McGill [Montréal, Canada], University of Massachusetts [Lowell] (UMass Lowell), University of Massachusetts System (UMASS), University of South Carolina [Columbia], 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, 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), Université de Lorraine (UL), Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), Universidad de Málaga [Málaga] = University of Málaga [Málaga], Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Université de Lyon, University of Copenhagen = Københavns Universitet (UCPH), University of Hawai'i [Honolulu] (UH), Deutsches Zentrum für Luft- und Raumfahrt (DLR), Search for Extraterrestrial Intelligence Institute (SETI), Plancius Research LLC, University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Cardon, Catherine, Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), University of Málaga, and University of Copenhagen = Københavns Universitet (KU)
Subjects: [SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU]Sciences of the Universe [physics], Mars2020 SuperCam Perseverance Mars Planetenforschung Spektroskopie Kamera Laser, ComputingMilieux_MISCELLANEOUS, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience
Published: 2021

18. Perseverance rover reveals an ancient delta-lake system and flood deposits at Jezero crater, Mars

Author: Mangold, N., Gupta, S., Gasnault, O., Dromart, G., Tarnas, J. D., Sholes, S. F., Horgan, B., Quantin-Nataf, C., Brown, A. J., Le Mouélic, S., Yingst, R., Bell, J. F., Beyssac, O., Bosak, T., Calef, F., III, Ehlmann, B. L., Farley, K. A., Grotzinger, J. P., Hickman-Lewis, K., Holm-Alwmark, S., Kah, L. C., Martínez-Frías, J., McLennan, S. M., Maurice, S., Nuñez, J. I., Ollila, A. M., Pilleri, P., Rice, J. W., Jr., Rice, M., Simon, J. I., Shuster, D. L., Stack, K. M., Sun, V. Z., Treiman, A. H., Weiss, B. P., Wiens, R. C., Williams, A. J., Williams, N. R., Williford, K. H., Mangold, N., Gupta, S., Gasnault, O., Dromart, G., Tarnas, J. D., Sholes, S. F., Horgan, B., Quantin-Nataf, C., Brown, A. J., Le Mouélic, S., Yingst, R., Bell, J. F., Beyssac, O., Bosak, T., Calef, F., III, Ehlmann, B. L., Farley, K. A., Grotzinger, J. P., Hickman-Lewis, K., Holm-Alwmark, S., Kah, L. C., Martínez-Frías, J., McLennan, S. M., Maurice, S., Nuñez, J. I., Ollila, A. M., Pilleri, P., Rice, J. W., Jr., Rice, M., Simon, J. I., Shuster, D. L., Stack, K. M., Sun, V. Z., Treiman, A. H., Weiss, B. P., Wiens, R. C., Williams, A. J., Williams, N. R., and Williford, K. H.
Abstract: Observations from orbital spacecraft have shown that Jezero crater, Mars, contains a prominent fan-shaped body of sedimentary rock deposited at its western margin. The Perseverance rover landed in Jezero crater in February 2021. We analyze images taken by the rover in the three months after landing. The fan has outcrop faces that were invisible from orbit, which record the hydrological evolution of Jezero crater. We interpret the presence of inclined strata in these outcrops as evidence of deltas that advanced into a lake. In contrast, the uppermost fan strata are composed of boulder conglomerates, which imply deposition by episodic high-energy floods. This sedimentary succession indicates a transition, from a sustained hydrologic activity in a persistent lake environment, to highly energetic short-duration fluvial flows.
Published: 2021

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

Author: Maurice, S., Wiens, R. C., Bernardi, P., Caïs, P., Robinson, S., Nelson, T., Gasnault, O., Reess, J. M., Deleuze, M., Rull, F., Manrique, J. A., Abbaki, S., Anderson, R. B., André, Y., Angel, S. M., Arana, G., Battault, T., Beck, P., Benzerara, K., Bernard, S., Berthias, J. P., Beyssac, O., Bonafous, M., Bousquet, B., Boutillier, M., Cadu, A., Castro, K., Chapron, F., Chide, B., Clark, K., Clavé, E., Clegg, S., Cloutis, E., Collin, C., Cordoba, E. C., Cousin, A., Dameury, J. C., D’Anna, W., Daydou, Y., Debus, A., Deflores, L., Dehouck, E., Delapp, D., De Los Santos, G., Donny, C., Doressoundiram, A., Dromart, G., Dubois, B., Dufour, A., Dupieux, M., Egan, M., Ervin, J., Fabre, C., Fau, A., Fischer, W., Forni, O., Fouchet, T., Frydenvang, J., Gauffre, S., Gauthier, M., Gharakanian, V., Gilard, O., Gontijo, I., Gonzalez, R., Granena, D., Grotzinger, J., Hassen-Khodja, R., Heim, M., Hello, Y., Hervet, G., Humeau, O., Jacob, X., Jacquinod, S., Johnson, J. R., Kouach, D., Lacombe, G., Lanza, N., Lapauw, L., Laserna, J., Lasue, J., Le Deit, L., Le Mouélic, S., Le Comte, E., Lee, Q. M., Legett, C., Leveille, R., Lewin, E., Leyrat, C., Lopez-Reyes, G., Lorenz, R., Lucero, B., Madariaga, J. M., Madsen, S., Madsen, M., Mangold, N., Manni, F., Mariscal, J. F., Martinez-Frias, J., Mathieu, K., Mathon, R., McCabe, K. P., McConnochie, T., McLennan, S. M., Mekki, J., Melikechi, N., Meslin, P.-Y., Micheau, Y., Michel, Y., Michel, J. M., Mimoun, D., Misra, A., Montagnac, G., Montaron, C., Montmessin, F., Moros, J., Mousset, V., Morizet, Y., Murdoch, N., Newell, R. T., Newsom, H., Nguyen Tuong, N., Ollila, A. M., Orttner, G., Oudda, L., Pares, L., Parisot, J., Parot, Y., Pérez, R., Pheav, D., Picot, L., Pilleri, P., Pilorget, C., Pinet, P., Pont, G., Poulet, F., Quantin-Nataf, C., Quertier, B., Rambaud, D., Rapin, W., Romano, P., Roucayrol, L., Royer, C., Ruellan, M., Sandoval, B. F., Sautter, V., Schoppers, M. J., Schröder, S., Seran, H. C., Sharma, S. K., Sobron, P., Sodki, M., Sournac, A., Sridhar, V., Standarovsky, D., Storms, S., Striebig, N., Tatat, M., Toplis, M., Torre-Fdez, I., Toulemont, N., Velasco, C., Veneranda, M., Venhaus, D., Virmontois, C., Viso, M., Willis, P., Wong, K. W., Maurice, S., Wiens, R. C., Bernardi, P., Caïs, P., Robinson, S., Nelson, T., Gasnault, O., Reess, J. M., Deleuze, M., Rull, F., Manrique, J. A., Abbaki, S., Anderson, R. B., André, Y., Angel, S. M., Arana, G., Battault, T., Beck, P., Benzerara, K., Bernard, S., Berthias, J. P., Beyssac, O., Bonafous, M., Bousquet, B., Boutillier, M., Cadu, A., Castro, K., Chapron, F., Chide, B., Clark, K., Clavé, E., Clegg, S., Cloutis, E., Collin, C., Cordoba, E. C., Cousin, A., Dameury, J. C., D’Anna, W., Daydou, Y., Debus, A., Deflores, L., Dehouck, E., Delapp, D., De Los Santos, G., Donny, C., Doressoundiram, A., Dromart, G., Dubois, B., Dufour, A., Dupieux, M., Egan, M., Ervin, J., Fabre, C., Fau, A., Fischer, W., Forni, O., Fouchet, T., Frydenvang, J., Gauffre, S., Gauthier, M., Gharakanian, V., Gilard, O., Gontijo, I., Gonzalez, R., Granena, D., Grotzinger, J., Hassen-Khodja, R., Heim, M., Hello, Y., Hervet, G., Humeau, O., Jacob, X., Jacquinod, S., Johnson, J. R., Kouach, D., Lacombe, G., Lanza, N., Lapauw, L., Laserna, J., Lasue, J., Le Deit, L., Le Mouélic, S., Le Comte, E., Lee, Q. M., Legett, C., Leveille, R., Lewin, E., Leyrat, C., Lopez-Reyes, G., Lorenz, R., Lucero, B., Madariaga, J. M., Madsen, S., Madsen, M., Mangold, N., Manni, F., Mariscal, J. F., Martinez-Frias, J., Mathieu, K., Mathon, R., McCabe, K. P., McConnochie, T., McLennan, S. M., Mekki, J., Melikechi, N., Meslin, P.-Y., Micheau, Y., Michel, Y., Michel, J. M., Mimoun, D., Misra, A., Montagnac, G., Montaron, C., Montmessin, F., Moros, J., Mousset, V., Morizet, Y., Murdoch, N., Newell, R. T., Newsom, H., Nguyen Tuong, N., Ollila, A. M., Orttner, G., Oudda, L., Pares, L., Parisot, J., Parot, Y., Pérez, R., Pheav, D., Picot, L., Pilleri, P., Pilorget, C., Pinet, P., Pont, G., Poulet, F., Quantin-Nataf, C., Quertier, B., Rambaud, D., Rapin, W., Romano, P., Roucayrol, L., Royer, C., Ruellan, M., Sandoval, B. F., Sautter, V., Schoppers, M. J., Schröder, S., Seran, H. C., Sharma, S. K., Sobron, P., Sodki, M., Sournac, A., Sridhar, V., Standarovsky, D., Storms, S., Striebig, N., Tatat, M., Toplis, M., Torre-Fdez, I., Toulemont, N., Velasco, C., Veneranda, M., Venhaus, D., Virmontois, C., Viso, M., Willis, P., and Wong, K. W.
Abstract: On the NASA 2020 rover mission to Jezero crater, the remote determination of the texture, mineralogy and chemistry of rocks is essential to quickly and thoroughly characterize an area and to optimize the selection of samples for return to Earth. As part of the Perseverance payload, SuperCam is a suite of five techniques that provide critical and complementary observations via Laser-Induced Breakdown Spectroscopy (LIBS), Time-Resolved Raman and Luminescence (TRR/L), visible and near-infrared spectroscopy (VISIR), high-resolution color imaging (RMI), and acoustic recording (MIC). SuperCam operates at remote distances, primarily 2–7 m, while providing data at sub-mm to mm scales. We report on SuperCam’s science objectives in the context of the Mars 2020 mission goals and ways the different techniques can address these questions. The instrument is made up of three separate subsystems: the Mast Unit is designed and built in France; the Body Unit is provided by the United States; the calibration target holder is contributed by Spain, and the targets themselves by the entire science team. This publication focuses on the design, development, and tests of the Mast Unit; companion papers describe the other units. The goal of this work is to provide an understanding of the technical choices made, the constraints that were imposed, and ultimately the validated performance of the flight model as it leaves Earth, and it will serve as the foundation for Mars operations and future processing of the data.
Published: 2021

20. Alternating wet and dry depositional environments recorded in the stratigraphy of Mount Sharp at Gale crater, Mars

Author: Rapin, W., primary, Dromart, G., additional, Rubin, D., additional, Deit, L. Le, additional, Mangold, N., additional, Edgar, L.A., additional, Gasnault, O., additional, Herkenhoff, K., additional, Le Mouélic, S., additional, Anderson, R.B., additional, Maurice, S., additional, Fox, V., additional, Ehlmann, B.L., additional, Dickson, J.L., additional, and Wiens, R.C., additional
Published: 2021
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21. SuperCam Calibration Targets:Design and Development

Author: Manrique, J. A., Lopez-Reyes, G., Cousin, A., Rull, F., Maurice, S., Wiens, R. C., Madsen, M. B., Madariaga, J. M., Gasnault, O., Aramendia, J., Arana, G., Beck, P., Bernard, S., Bernardi, P., Bernt, M. H., Berrocal, A., Beyssac, O., Cais, P., Castro, C., Castro, K., Clegg, S. M., Cloutis, E., Dromart, G., Drouet, C., Dubois, B., Escribano, D., Fabre, C., Fernandez, A., Forni, O., Garcia-Baonza, V., Gontijo, I., Johnson, J., Laserna, J., Lasue, J., Madsen, S., Mateo-Marti, E., Medina, J., Meslin, P. -Y., Montagnac, G., Moral, A., Moros, J., Ollila, A. M., Ortega, C., Prieto-Ballesteros, O., Reess, J. M., Robinson, S., Rodriguez, J., Saiz, J., Sanz-Arranz, J. A., Sard, I., Sautter, V., Sobron, P., Toplis, M., Veneranda, M., Manrique, J. A., Lopez-Reyes, G., Cousin, A., Rull, F., Maurice, S., Wiens, R. C., Madsen, M. B., Madariaga, J. M., Gasnault, O., Aramendia, J., Arana, G., Beck, P., Bernard, S., Bernardi, P., Bernt, M. H., Berrocal, A., Beyssac, O., Cais, P., Castro, C., Castro, K., Clegg, S. M., Cloutis, E., Dromart, G., Drouet, C., Dubois, B., Escribano, D., Fabre, C., Fernandez, A., Forni, O., Garcia-Baonza, V., Gontijo, I., Johnson, J., Laserna, J., Lasue, J., Madsen, S., Mateo-Marti, E., Medina, J., Meslin, P. -Y., Montagnac, G., Moral, A., Moros, J., Ollila, A. M., Ortega, C., Prieto-Ballesteros, O., Reess, J. M., Robinson, S., Rodriguez, J., Saiz, J., Sanz-Arranz, J. A., Sard, I., Sautter, V., Sobron, P., Toplis, M., and Veneranda, M.
Abstract: SuperCam is a highly integrated remote-sensing instrumental suite for NASA's Mars 2020 mission. It consists of a co-aligned combination of Laser-Induced Breakdown Spectroscopy (LIBS), Time-Resolved Raman and Luminescence (TRR/L), Visible and Infrared Spectroscopy (VISIR), together with sound recording (MIC) and high-magnification imaging techniques (RMI). They provide information on the mineralogy, geochemistry and mineral context around the Perseverance Rover. The calibration of this complex suite is a major challenge. Not only does each technique require its own standards or references, their combination also introduces new requirements to obtain optimal scientific output. Elemental composition, molecular vibrational features, fluorescence, morphology and texture provide a full picture of the sample with spectral information that needs to be co-aligned, correlated, and individually calibrated. The resulting hardware includes different kinds of targets, each one covering different needs of the instrument. Standards for imaging calibration, geological samples for mineral identification and chemometric calculations or spectral references to calibrate and evaluate the health of the instrument, are all included in the SuperCam Calibration Target (SCCT). The system also includes a specifically designed assembly in which the samples are mounted. This hardware allows the targets to survive the harsh environmental conditions of the launch, cruise, landing and operation on Mars during the whole mission. Here we summarize the design, development, integration, verification and functional testing of the SCCT. This work includes some key results obtained to verify the scientific outcome of the SuperCam system.
Published: 2020

22. The Chemostratigraphy of the Murray Formation and Role of Diagenesis at Vera Rubin Ridge in Gale Crater, Mars, as Observed by the ChemCam Instrument

Author: Frydenvang, J., Mangold, N., Wiens, R. C., Fraeman, A. A., Edgar, L. A., Fedo, C. M., L'Haridon, J., Bedford, C. C., Gupta, Sanjeev, Grotzinger, J. P., Bridges, J. C., Clark, B. C., Rampe, E. B., Gasnault, O., Maurice, S., Gasda, P. J., Lanza, N. L., Olilla, A. M., Meslin, P. Y., Payré, V., Calef, F., Salvatore, Mark, House, C. H., Frydenvang, J., Mangold, N., Wiens, R. C., Fraeman, A. A., Edgar, L. A., Fedo, C. M., L'Haridon, J., Bedford, C. C., Gupta, Sanjeev, Grotzinger, J. P., Bridges, J. C., Clark, B. C., Rampe, E. B., Gasnault, O., Maurice, S., Gasda, P. J., Lanza, N. L., Olilla, A. M., Meslin, P. Y., Payré, V., Calef, F., Salvatore, Mark, and House, C. H.
Abstract: Geochemical results are presented from Curiosity's exploration of Vera Rubin ridge (VRR), in addition to the full chemostratigraphy of the predominantly lacustrine mudstone Murray formation up to and including VRR. VRR is a prominent ridge flanking Aeolis Mons (informally Mt. Sharp), the central mound in Gale crater, Mars, and was a key area of interest for the Mars Science Laboratory mission. ChemCam data show that VRR is overall geochemically similar to lower-lying members of the Murray formation, even though the top of VRR shows a strong hematite spectral signature as observed from orbit. Although overall geochemically similar, VRR is characterized by a prominent decrease in Li abundance and Chemical Index of Alteration across the ridge. This decrease follows the morphology of the ridge rather than elevation and is inferred to reflect a nondepositionally controlled decrease in clay mineral abundance in VRR rocks. Additionally, a notable enrichment in Mn above baseline levels is observed on VRR. While not supporting a single model, the results suggest that VRR rocks were likely affected by multiple episodes of postdepositional groundwater interactions that made them more erosionally resistant than surrounding Murray rocks, thus resulting in the modern-day ridge after subsequent erosion.
Published: 2020

23. Boron and Lithium in Calcium Sulfate Veins:Tracking Precipitation of Diagenetic Materials in Vera Rubin Ridge, Gale Crater

Author: Das, D., Gasda, Patrick J., Wiens, R. C., Berlo, K., Leveille, R. J., Frydenvang, J., Mangold, N., Kronyak, R. E., Schwenzer, S. P., Forni, O., Cousin, A., Maurice, S., Gasnault, O., Das, D., Gasda, Patrick J., Wiens, R. C., Berlo, K., Leveille, R. J., Frydenvang, J., Mangold, N., Kronyak, R. E., Schwenzer, S. P., Forni, O., Cousin, A., Maurice, S., and Gasnault, O.
Abstract: The NASA Curiosity rover's ChemCam instrument suite has detected boron in calcium-sulfate-filled fractures throughout the sedimentary strata of Gale crater including Vera Rubin ridge. The presence of elevated B concentration provides insights into Martian subsurface aqueous processes. In this study we extend the data set of B in Ca-sulfate veins across Gale crater, comparing the detection frequency and relative abundances with Li. We report 33 new detections of B within veins analyzed between Sols 1548 and 2311 where detections increase in Pettegrove Point and Jura members, which form Vera Rubin ridge. The presence of B and Li in the Ca-sulfate veins is possibly due to dissolution of preexisting B in clays of the bedrock by acids or neutral water and redistribution of the elements into the veins. Elevated frequency of B detection in veins of Gale crater correlates with presence of dehydration features such as desiccation cracks, altered clay minerals and detections of evaporites such as Mg-sulfates and chloride salts in the host rocks. The increased observations of B also coincide with decreased Li concentration in the veins (average Li concentration of veins drops by ~15 ppm). Boron and Li have varying solubilities, and Li does not form salts as readily upon dehydration as B, causing it to remain in the solution. So the weak negative correlation between B and Li may reflect the crystallization sequence during dehydration on Vera Rubin ridge.
Published: 2020

24. Geochemical variation in the Stimson formation of Gale crater:Provenance, mineral sorting, and a comparison with modern Martian dunes

Author: Bedford, C. C., Schwenzer, S. P., Bridges, J.C., Banham, S., Wiens, R. C., Gasnault, O., Rampe, E. B., Frydenvang, J., Gasda, Patrick J., Bedford, C. C., Schwenzer, S. P., Bridges, J.C., Banham, S., Wiens, R. C., Gasnault, O., Rampe, E. B., Frydenvang, J., and Gasda, Patrick J.
Abstract: The Mars Science Laboratory Curiosity rover has encountered both ancient lithified and modern active aeolian dune deposits within Gale crater, providing an opportunity to study how aeolian processes have changed during Gale crater's geological history. This study uses data from the Chemistry and Camera (ChemCam) and Chemistry and Mineralogy (CheMin) instrument suites onboard Curiosity to; (1) constrain the diagenetic processes that lithified and altered the ancient aeolian Stimson formation, (2) investigate whether the geochemical signature in the Stimson formation is consistent with the aeolian mafic-felsic mineral sorting trend identified in the modern Bagnold dune fields in Gale crater, and (3) discuss the provenance of the Stimson sediments, comparing it to those identified in the modern dune and ancient river and lake deposits also analyzed along Curiosity's traverse. The ancient Stimson dune deposits that stratigraphically overlie the Gale fluvio-lacustrine units were analyzed in two locations; the Emerson and the Naukluft plateaus. ChemCam data show that the Stimson formation has subtle variations in MgO, Al2O3, Na2O, and K2O between the two localities. An agglomerative cluster analysis of the constrained Stimson dataset reveals five clusters, four of which relate to different proportions of mafic and felsic minerals analyzed by ChemCam. In general, the cluster analysis shows that the Emerson plateau has a greater proportion of mafic minerals and fewer coarse, felsic grains relative to the Naukluft plateau. This variation in mafic and felsic minerals between localities suggests a southwest to northeast net sediment transport direction due to aeolian mineral sorting dynamics preferentially transporting mafic minerals that are easier to saltate than the elongate, often coarser, felsic minerals. This derived transport direction for the Stimson formation supports that determined by sedimentological evidence and is op
Published: 2020

25. Distribution of hydrogen in the near surface of Mars: evidence for subsurface ice deposits. (Reports)

Author: Boynton, W.V., Feldman, W.C., Squyres, S.W., Prettyman, T.H., Bruckner, J., Evans, L.G., Reedy, R.C., Starr, R., Arnold, J.R., Drake, D.M., Englert, P.A.J., Metzger, A.E., Mitrofanov, Igor, Trombka, J.I., d'Uston, C., Wanke, H., Gasnault, O., Hamara, D.K., Janes, D.M., Marcialis, R.L., Maurice, S., Mikheeva, I., Taylor, G.J., Tokar, R., and Shinohara, C.
Subjects: Planets -- Discovery and exploration, Water, Underground -- Discovery and exploration, Mars (Planet) -- Discovery and exploration, Science and technology, Discovery and exploration
Abstract: Using the Gamma-Ray Spectrometer on the Mars Odyssey, we have identified two regions near the poles that are enriched in hydrogen. The data indicate the presence of a subsurface layer enriched in hydrogen overlain by a hydrogenpoor layer. The thickness of the upper layer decreases with decreasing distance to the pole, ranging from a column density of about 150 grams per square centimeter at -42° latitude to about 40 grams per square centimeter at -77°. The hydrogen-rich regions correlate with regions of predicted ice stability. We suggest that the host of the hydrogen in the subsurface layer is ice, which constitutes 35 ± 15% of the layer by weight., There is ample evidence that water has been important in shaping the martian surface (1, 2) and that water is present on Mars today in the north polar residual cap [...]
Published: 2002

26. Global distribution of neutrons from Mars: results from Mars Odyssey

Author: Feldman, W.C., Boynton, W.V., Tokar, R.L., Prettyman, T.H., Gasnault, O., Squyres, S.W., Elphic, R.C., Lawrence, D.J., Lawson, S.L., Maurice, S., McKinney, G.W., Moore, K.R., and Reedy, R.C.
Subjects: Mars Odyssey (Space probe) -- Research, Neutrons -- Scattering, Mars (Planet) -- Spectra -- Research, Science and technology, Research, Spectra
Abstract: Global distributions of thermal, epithermal, and fast neutron fluxes have been mapped during late southern summer/northern winter using the Mars Odyssey Neutron Spectrometer. These fluxes are selectively sensitive to the vertical and lateral spatial distributions of H and [CO.sub.2] in the uppermost meter of the martian surface. Poleward of ± 60° latitude is terrain rich in hydrogen, probably [H.sub.2]O ice buried beneath tens of centimeter-thick hydrogen-poor soil. The central portion of the north polar cap is covered by a thick [CO.sub.2] layer, as is the residual south polar cap. Portions of the low to middle latitudes indicate subsurface deposits of chemically and/or physically bound [H.sub.2]O and/or OH., Neutron spectroscopy can be used to survey planetary bodies for hydrogen (1). The epithermal neutron energy range (0.4 to about 500 keV) is most sensitive for this purpose. Measurements of [...]
Published: 2002

27. Contrasting Regional Soil Alteration Across the Topographic Dichotomy of Mars

Author: Hood, D. R., primary, Karunatillake, S., additional, Gasnault, O., additional, Williams, A. J., additional, Dutrow, B., additional, Ojha, L., additional, Kobs, S., additional, Kim, K., additional, Heldmann, J., additional, and Fralick, C., additional
Published: 2019
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28. Feldspathic Cumulate Samples and Plutonic Rocks in Gale Crater: Comparisons to Martian Meteorites

Author: Bridges, J. C., Cousin, A., Sautter, V., William Rapin, Bowden, D., Thompson, L., Schwenzer, S. P., Bedford, C., Payre, V., Gasnault, O., Forni, O., Pinet, P., Wiens, R., Yingst, R. A., Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Los Alamos National Laboratory (LANL)
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract: The Curiosity Rover of Mars Science Laboratory has identified igneous float rocks in Gale Crater which offer new insights about the differentiation of the martian lithosphere. Here we describe likely origins for some unique Gale plutonic and cumulate rocks and compare to the martian meteorites. At the Ireson Hill locality around sol 1606 a group of float rocks with resistant, dreikanter morphologies were identified which include igneous textures, notably the 10 cm Pogy sample. On sol 2016 of the MSL mission, a group of float rocks were studied in detail, including Askival, which is a light toned rock igneous rock similar to Peacock_Hills (sol 19) and Bindi (sol 544).
Published: 2019

29. Mars Science Laboratory Observations of Chloride Salts in Gale Crater, Mars

Author: Thomas, N. H., primary, Ehlmann, B. L., additional, Meslin, P.‐Y., additional, Rapin, W., additional, Anderson, D. E., additional, Rivera‐Hernández, F., additional, Forni, O., additional, Schröder, S., additional, Cousin, A., additional, Mangold, N., additional, Gellert, R., additional, Gasnault, O., additional, and Wiens, R. C., additional
Published: 2019
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30. Martian Eolian Dust Probed by ChemCam

Author: Lasue, J., Cousin, A., Meslin, P. -Y., Mangold, N., Wiens, R. C., Berger, G., Dehouck, E., Forni, O., Goetz, W., Gasnault, O., Rapin, W., Schroeder, S., Ollila, A., Johnson, J., Le Mouelic, S., Maurice, S., Anderson, R., Blaney, D., Clark, B., Clegg, S. M., d'Uston, C., Fabre, C., Lanza, N., Madsen, M. B., Martin-Torres, J., Melikechi, N., Newsom, H., Sautter, V., Zorzano, M. P., Lasue, J., Cousin, A., Meslin, P. -Y., Mangold, N., Wiens, R. C., Berger, G., Dehouck, E., Forni, O., Goetz, W., Gasnault, O., Rapin, W., Schroeder, S., Ollila, A., Johnson, J., Le Mouelic, S., Maurice, S., Anderson, R., Blaney, D., Clark, B., Clegg, S. M., d'Uston, C., Fabre, C., Lanza, N., Madsen, M. B., Martin-Torres, J., Melikechi, N., Newsom, H., Sautter, V., and Zorzano, M. P.
Published: 2018

31. Martian aeolian activity at the Bagnold Dunes, Gale Crater: The view from the surface and orbit

Author: Bridges, N., Sullivan, R., Newman, C., Navarro, S., Van Beek, J., Ewing, R., Ayoub, F., Silvestro, S., Gasnault, O., Le Mouélic, Stéphane, Lapotre, M., Rapin, W., Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Cornell University [New York], Aeolis Research, Instituto Nacional de Técnica Aeroespacial (INTA), Malin Space Science Systems (MSSS), Texas A&M University [College Station], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), INAF - Osservatorio Astronomico di Capodimonte (OAC), Istituto Nazionale di Astrofisica (INAF), Search for Extraterrestrial Intelligence Institute (SETI), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Gasnault, Olivier, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - 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 -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), Depertment of Polymer Chemistry, Division of Geological and Planetary Sciences [Pasadena], Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS), Université d'Angers (UA)-Université de Nantes - Faculté des Sciences et des Techniques, California Institute of Technology (CALTECH)-NASA, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, [SDU]Sciences of the Universe [physics], [SDU.STU.PL] Sciences of the Universe [physics]/Earth Sciences/Planetology, ComputingMilieux_MISCELLANEOUS
Abstract: The first in situ investigation of an active dune field on another planetary surface occurred in 2015–2016 when the Mars Science Laboratory Curiosity rover investigated the Bagnold Dunes on Mars. High Resolution Imaging Science Experiment images show clear seasonal variations that are in good agreement with atmospheric model predictions of intra-annual sand flux and migration directions that together indicate that the campaign occurred during a period of low wind activity. Curiosity surface images show that limited changes nevertheless occurred, with movement of large grains, particularly on freshly exposed surfaces, two occurrences of secondary grain flow on the slip face of Namib Dune, and a slump on a freshly exposed surface of a large ripple. These changes are seen at Martian solar day (sol)-to-sol time scales. Grains on a rippled sand deposit and unconsolidated dump piles show limited movement of large grains over a few hours during which mean friction speeds are estimated at 0.3–0.4 m s?1. Overall, the correlation between changes and peak Rover Environmental Monitoring Station (REMS) winds is moderate, with high wind events associated with changes in some cases, but not in others, suggesting that other factors are also at work. The distribution of REMS 1 Hz wind speeds shows a significant tail up to the current 20 m s?1 calibration limit, indicating that even higher speed winds occur. Nonaeolian triggering mechanisms are also possible. The low activity period at the dunes documented by Curiosity provides clues to processes that dominated in the Martian past under conditions of lower obliquity.
Published: 2017

32. Geochemistry of the Bagnold dune field as observed by ChemCam and comparison with other aeolian deposits at Gale crater

Author: Cousin, Agnes, Dehouck, Erwin, Meslin, P.-Y., Forni, O., Williams, A., Stein, Nathan, Gasnault, O., Bridges, N., Ehlmann, Bethany, Schröder, Susanne, Payré, V., Rapin, W., Pinet, P., Sautter, V., Lanza, N., Lasue, J., Maurice, S., Wiens, R. C., Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Department of Physics, Astronomy, and Geosciences [Towson], Towson University [Towson, MD, United States], University of Maryland System-University of Maryland System, Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Justus-Liebig-Universität Gießen (JLU), GeoRessources, Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS), Muséum national d'Histoire naturelle (MNHN), Los Alamos National Laboratory (LANL), 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), Justus-Liebig-Universität Gießen = Justus Liebig University (JLU), and 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)
Subjects: LIBS, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, dunes, ChemCam, Mars, soils, ComputingMilieux_MISCELLANEOUS
Abstract: The Curiosity rover conducted the first field investigation of an active extraterrestrial dune. This study of the Bagnold dunes focuses on the ChemCam chemical results and also presents findings on the grain size distributions based on the ChemCam Remote Micro-Imager and Mars Hand Lens Imager images. These active dunes are composed of grains that are mostly 150 μm grain-size dump piles have shown that coarser grains (150–250 μm) are enriched in the mafic elements Fe and Mn, suggesting a larger content in olivine compared to smaller grains (
Published: 2017

33. Characterization of Laser-Induced Breakdown Spectroscopy (LIBS) emission lines for the identification of chlorides, carbonates, and sulfates in salt/basalt mixtures for the application to MSL ChemCam data

Author: Anderson, D. E., Ehlmann, B. L., Forni, O., Clegg, S. M., Cousin, A., Thomas, N. H., Lasue, J., Delapp, D. M., McInroy, R. E., Gasnault, O., Dyar, M. D., Schröder, S., Maurice, S., and Wiens, R. C.
Abstract: Ancient environmental conditions on Mars can be probed through the identification of minerals on its surface, including water-deposited salts and cements dispersed in the pore space of sedimentary rocks. Laser-induced breakdown spectroscopy (LIBS) analyses by the Martian rover Curiosity's ChemCam instrument can indicate salts, and ChemCam surveys aid in identifying and selecting sites for further, detailed in situ analyses. We performed laboratory LIBS experiments under simulated Mars conditions with a ChemCam-like instrument on a series of mixtures containing increasing concentrations of salt in a basaltic background to investigate the potential for identifying and quantifying chloride, carbonate, and sulfate salts found only in small amounts, dispersed in bulk rock with ChemCam, rather than concentrated in veins. Data indicate that the presence of emission lines from the basalt matrix limited the number of Cl, C, and S emission lines found to be useful for quantitative analysis; nevertheless, several lines with intensities sensitive to salt concentration were identified. Detection limits for the elements based on individual emission lines ranged from ~20 wt % carbonate (2 wt % C), ~5–30 wt % sulfate (1–8 wt % S), and ~5–10 wt % chloride (3–6 wt % Cl) depending on the basaltic matrix and/or salt cation. Absolute quantification of Cl, C, and S in the samples via univariate analysis depends on the cation-anion pairing in the salt but appears relatively independent of matrices tested, following normalization. These results are promising for tracking relative changes in the salt content of bulk rock on the Martian surface with ChemCam.
Published: 2017

34. Martian Eolian Dust Probed by ChemCam

Author: Lasue, J., primary, Cousin, A., additional, Meslin, P.‐Y., additional, Mangold, N., additional, Wiens, R. C., additional, Berger, G., additional, Dehouck, E., additional, Forni, O., additional, Goetz, W., additional, Gasnault, O., additional, Rapin, W., additional, Schroeder, S., additional, Ollila, A., additional, Johnson, J., additional, Le Mouélic, S., additional, Maurice, S., additional, Anderson, R., additional, Blaney, D., additional, Clark, B., additional, Clegg, S. M., additional, d'Uston, C., additional, Fabre, C., additional, Lanza, N., additional, Madsen, M. B., additional, Martin‐Torres, J., additional, Melikechi, N., additional, Newsom, H., additional, Sautter, V., additional, and Zorzano, M. P., additional
Published: 2018
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35. Estimation method of planetary fast neutron flux by a Ge gamma-ray spectrometer

Author: Hareyama, Makoto, Fujibayashi, Y., Yamashita, Y., Karouji, Yuzuru, Nagaoka, Hiroshi, Kobayashi, Shingo, Reedy, R. C., Gasnault, O., Forni, O., d'Uston, C., Kim, K. J., Hasebe, Nobuyuki, 晴山, 慎, 唐牛, 譲, 長岡, 央, 小林, 進悟, 長谷部, 信行, Hareyama, Makoto, Fujibayashi, Y., Yamashita, Y., Karouji, Yuzuru, Nagaoka, Hiroshi, Kobayashi, Shingo, Reedy, R. C., Gasnault, O., Forni, O., d'Uston, C., Kim, K. J., Hasebe, Nobuyuki, 晴山, 慎, 唐牛, 譲, 長岡, 央, 小林, 進悟, and 長谷部, 信行
Abstract: 著者人数: 12名, Accepted: 2016-05-10
Published: 2017

36. Quantification of water content by laser induced breakdown spectroscopy on Mars

Author: Rapin, W, Meslin, PY, Maurice, S, Wiens, RC, Laporte, D, Chauviré, B, Gasnault, O, Schröder, S, Beck, P, Bender, S, Beyssac, O, Cousin, A, Dehouck, E, Drouet, C, Forni, O, Nachon, M, Melikechi, N, Rondeau, B, Mangold, N, Thomas, NH, Rapin, W, Meslin, PY, Maurice, S, Wiens, RC, Laporte, D, Chauviré, B, Gasnault, O, Schröder, S, Beck, P, Bender, S, Beyssac, O, Cousin, A, Dehouck, E, Drouet, C, Forni, O, Nachon, M, Melikechi, N, Rondeau, B, Mangold, N, and Thomas, NH
Abstract: © 2017 Elsevier B.V. Laser induced breakdown spectroscopy (LIBS), as performed by the ChemCam instrument, provides a new technique to measure hydrogen at the surface of Mars. Using a laboratory replica of the LIBS instrument onboard the Curiosity rover, different types of hydrated samples (basalts, calcium and magnesium sulfates, opals and apatites) covering a range of targets observed on Mars have been characterized and analyzed. A number of factors related to laser parameters, atmospheric conditions and differences in targets properties can affect the standoff LIBS signal, and in particular the hydrogen emission peak. Dedicated laboratory tests were run to identify a normalization of the hydrogen signal which could best compensate for these effects and enable the application of the laboratory calibration to Mars data. We check that the hydrogen signal increases linearly with water content; and normalization of the hydrogen emission peak using to oxygen and carbon emission peaks (related to the breakdown of atmospheric carbon dioxide) constitutes a robust approach. Moreover, the calibration curve obtained is relatively independent of the samples types.
Published: 2017

37. AEGIS autonomous targeting for ChemCam on Mars Science Laboratory:Deployment and results of initial science team use

Author: Francis, R., Estlin, T., Doran, G., Johnstone, S., Gaines, D., Verma, V., Burl, M., Frydenvang, Jens, Montaño, S., Wiens, R. C., Schaffer, S., Gasnault, O., Deflores, L., Blaney, Diana L., Bornstein, B., Francis, R., Estlin, T., Doran, G., Johnstone, S., Gaines, D., Verma, V., Burl, M., Frydenvang, Jens, Montaño, S., Wiens, R. C., Schaffer, S., Gasnault, O., Deflores, L., Blaney, Diana L., and Bornstein, B.
Published: 2017

38. Roughness effects on the hydrogen signal in laser-induced breakdown spectroscopy

Author: Rapin, W., Bousquet, B., Lasue, J., Meslin, P. Y., Lacour, J. L., Fabre, C., Wiens, R. C., Frydenvang, Jens, Dehouck, E., Maurice, S., Gasnault, O., Forni, O., Cousin, A., Rapin, W., Bousquet, B., Lasue, J., Meslin, P. Y., Lacour, J. L., Fabre, C., Wiens, R. C., Frydenvang, Jens, Dehouck, E., Maurice, S., Gasnault, O., Forni, O., and Cousin, A.
Abstract: On Mars, Laser-Induced Breakdown Spectroscopy (LIBS) as performed by the ChemCam instrument can be used to measure the hydrogen content of targets in situ, under a low pressure CO2 atmosphere. However, unexpected variations observed in the Martian dataset suggest an effect related to target roughness. Here, we present a series of laboratory experiments that reproduce the effect observed on Mars and explore possible causes. We show that the hydrogen peak intensity increases significantly with increasing exposure of the target surface to the LIBS plasma, and that these variations are specific to hydrogen, as other emission lines in the spectra are not affected. The increase of the signal could be related to an addition of hydrogen to the plasma due to interaction with the surrounding target surface, yet the exact physical process to explain such effect remains to be identified. More generally, this effect should be taken into account for the quantification of hydrogen in any LIBS applications where the roughness of the target is significant.
Published: 2017

39. The South Pole-Aitken basin region, Moon: GIS-based geologic investigation using Kaguya elemental information

Author: Kim, K.J., J.-P., Williams Dohm, Ruiz, J., Hare, T.M., Hasebe, N., Karouji, Y., Kobayashi, S., Hareyama, M., Shibamura, E., Kobayashi, M., C., d’Uston, Gasnault, O., Forni, O., and Maurice, S.
Abstract: Using Geographic Information Systems (GIS), we performed comparative analysis among stratigraphic information and the Kaguya (SELENE) GRS data of the ∼2500-km-diameter South Pole-Aitken (SPA) basin and its surroundings. Results indicate that the surface rock materials (including ancient crater materials, mare basalts, and possible SPA impact melt) are average to slightly elevated in K and Th with respect to the rest of the Moon. Also, this study demonstrates that K and Th have not significantly changed since the formation of SPA. The elemental signatures of the impact basin of Fe, Ti, Si, O through time include evidence for resurfacing by ejecta materials and late-stage volcanism. The oldest surfaces of SPA are found to be oxygen-depleted during the heavy bombardment period relative to later stages of geologic development, followed by both an increase in silicon and oxygen, possibly due to ejecta sourced from outside of SPA, and subsequent modification due to mare basaltic volcanism, which increased iron and titanium within SPA. The influence of the distinct geologic history of SPA and surroundings on the mineralogic and elemental abundances is evident as shown in our investigation.
Published: 2012

40. The potassic sedimentary rocks in Gale Crater, Mars, as seen by ChemCam on board Curiosity

Author: Le Deit, L, Mangold, N, Forni, O, Cousin, A, Lasue, J, Schroder, S, Wiens, RC, Sumner, D, Fabre, C, Stack, KM, Anderson, RB, Blaney, D, Clegg, S, Dromart, G, Fisk, M, Gasnault, O, Grotzinger, JP, Gupta, S, Lanza, N, Le Mouelic, S, Maurice, S, McLennan, SM, Meslin, P-Y, Nachon, M, Newsom, H, Payre, V, Rapin, W, Rice, M, Sautter, V, Treiman, AH, DLR Institute of Planetary Research, German Aerospace Center (DLR), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), University of California [Davis] (UC Davis), University of California, California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Oregon State University (OSU), Department of Physics and Materials Science & Centre for Functional Photonics (CFP), The University of Hong Kong (HKU), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], Laboratoire Ecologie Fonctionnelle et Environnement (ECOLAB), Institut Ecologie et Environnement (INEE), Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Institute [Houston] (LPI), 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 California (UC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire Ecologie Fonctionnelle et Environnement (LEFE), Université de Toulouse (UT)-Université de Toulouse (UT)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut 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 National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH)-NASA, Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut Ecologie et Environnement (INEE), Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Science and Technology Facilities Council (STFC)
Subjects: Geochemistry & Geophysics, SANDSTONE, Science & Technology, INSTRUMENT SUITE, ORIGIN, IN-SITU, ROVER, K-FELDSPAR, EVOLUTION, [SDU]Sciences of the Universe [physics], Physical Sciences, OLIVINE, OUTCROP, SYSTEM, ComputingMilieux_MISCELLANEOUS
Abstract: The Mars Science Laboratory rover Curiosity encountered potassium-rich clastic sedimentary rocks at two sites in Gale Crater, the waypoints Cooperstown and Kimberley. These rocks include several distinct meters thick sedimentary outcrops ranging from fine sandstone to conglomerate, interpreted to record an ancient fluvial or fluvio-deltaic depositional system. From ChemCam Laser-Induced Breakdown Spectroscopy (LIBS) chemical analyses, this suite of sedimentary rocks has an overall mean K2O abundance that is more than 5 times higher than that of the average Martian crust. The combined analysis of ChemCam data with stratigraphic and geographic locations reveals that the mean K2O abundance increases upward through the stratigraphic section. Chemical analyses across each unit can be represented as mixtures of several distinct chemical components, i.e., mineral phases, including K-bearing minerals, mafic silicates, Fe-oxides, and Fe-hydroxide/oxyhydroxides. Possible K-bearing minerals include alkali feldspar (including anorthoclase and sanidine) and K-bearing phyllosilicate such as illite. Mixtures of different source rocks, including a potassium-rich rock located on the rim and walls of Gale Crater, are the likely origin of observed chemical variations within each unit. Physical sorting may have also played a role in the enrichment in K in the Kimberley formation. The occurrence of these potassic sedimentary rocks provides additional evidence for the chemical diversity of the crust exposed at Gale Crater.
Published: 2016

41. Fluorine in the Pahrump outcrop, Gale Crater: Implications for fluid circulation and alteration

Author: Forni, O., Nachon, M., Mangold, N., Blaney, D. L., Wiens, R. C., Clegg, S. M., Meslin, P. -Y, Gasnault, O., Maurice, S., Cousin, A., Frydenvand, J., Susanne Petra Schwenzer, and Eigenbrode, J. L.
Published: 2016

42. ChemCam activities and discoveries during the nominal mission of the Mars Science Laboratory in Gale crater, Mars

Author: Thompson, L., Williams, A., Williams, R., Blaney, D., Calef, F., Dietrich, W., Edgett, K., Fisk, M., Gellert, R., Grotzinger, J., Kah, L., McLennan, S., Palucis, M., Siebach, K., Stack, K., Sumner, D., Yingst, A., Maurice, S., Clegg, S., Wiens, R., Gasnault, O., Rapin, W., Forni, O., Cousin, A., Sautter, V., Mangold, N., Le Deit, L., Nachon, M., Anderson, R., Lanza, N., Fabre, C., Payré, V., Lasue, J., Meslin, P.-Y., Léveillé, R., Barraclough, B., Beck, P., Bender, S., Berger, G., Bridges, J., Bridges, N., Dromart, G., Dyar, M., Francis, R., Frydenvang, J., Gondet, B., Ehlmann, B., Herkenhoff, K., Johnson, J., Langevin, Y., Madsen, M., Melikechi, N., Lacour, J.-L., Le Mouélic, Stéphane, Lewin, E., Newsom, H., Ollila, A., Pinet, P., Schröder, S., Sirven, J.-B., Tokar, R., Toplis, M., D'Uston, C., Vaniman, D., Vasavada, A., Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Oregon State University (OSU), Department of Physics [Guelph], University of Guelph, California Institute of Technology (CALTECH), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley], University of California-University of California, Division of Geological and Planetary Sciences [Pasadena], University of California [Davis] (UC Davis), University of California, Planetary Science Institute [Tucson] (PSI), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS)-Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC), Laboratoire de Planétologie et Géodynamique UMR6112 (LPG), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Université d'Angers (UA), DLR Institute of Planetary Research, German Aerospace Center (DLR), Laboratoire Ecologie Fonctionnelle et Environnement (ECOLAB), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Canadian Space Agency (CSA), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Space Research Centre [Leicester], University of Leicester, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), Centre for Infection and Immunity, Optical Science Center for Applied Research (OSCAR), Delaware State University (DSU), Service d'études analytiques et de réactivité des surfaces (SEARS), Département de Physico-Chimie (DPC), CEA-Direction de l'Energie Nucléaire (CEA-DEN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction de l'Energie Nucléaire (CEA-DEN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut des Sciences de la Terre (ISTerre), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-PRES Université de Grenoble-Institut de recherche pour le développement [IRD] : UR219-Institut national des sciences de l'Univers (INSU - CNRS)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Université Joseph Fourier - Grenoble 1 (UJF), Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], Technologies et systèmes d'information pour les agrosystèmes (UR TSCF), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Commissariat à l'Energie Atomique et aux Energies Alternatives, Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Dynamique terrestre et planétaire (DTP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Centre d'étude spatiale des rayonnements (CESR), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA-California Institute of Technology (CALTECH), University of California [Berkeley] (UC Berkeley), University of California (UC)-University of California (UC), University of California (UC), 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), Muséum national d'Histoire naturelle (MNHN)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Ecologie Fonctionnelle et Environnement (LEFE), Institut Ecologie et Environnement (INEE), Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Observatoire Midi-Pyrénées (OMP), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut 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 National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), 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), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de recherche pour le développement [IRD] : UR206-Muséum national d'Histoire naturelle (MNHN)-Centre National de la Recherche Scientifique (CNRS), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3)
Subjects: 010504 meteorology & atmospheric sciences, atomic Emission spectroscopy, Mars, Mineralogy, Context (language use), 01 natural sciences, Analytical Chemistry, Atmosphere, laser-spectroscopy, Spectroscopy, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, LIBS, Chemistry, 010401 analytical chemistry, Noachian, Gale crater, Crust, Mars Exploration Program, 15. Life on land, Gale Crater, 0104 chemical sciences, Characterization (materials science), Geochemistry, in-situ, ChemCam, 13. Climate action, [SDU]Sciences of the Universe [physics]
Abstract: At Gale crater, Mars, ChemCam acquired its first laser-induced breakdown spectroscopy (LIBS) target on Sol 13 of the landed portion of the mission (a Sol is a Mars day). Up to Sol 800, more than 188 000 LIBS spectra were acquired on more than 5800 points distributed over about 650 individual targets. We present a comprehensive review of ChemCam scientific accomplishments during that period, together with a focus on the lessons learned from the first use of LIBS in space. For data processing, we describe new tools that had to be developed to account for the uniqueness of Mars data. With regard to chemistry, we present a summary of the composition range measured on Mars for major-element oxides (SiO_2, TiO_2, Al_2O_3, FeO_T, MgO, CaO, Na_2O, K_2O) based on various multivariate models, with associated precisions. ChemCam also observed H, and the non-metallic elements C, O, P, and S, which are usually difficult to quantify with LIBS. F and Cl are observed through their molecular lines. We discuss the most relevant LIBS lines for detection of minor and trace elements (Li, Rb, Sr, Ba, Cr, Mn, Ni, and Zn). These results were obtained thanks to comprehensive ground reference datasets, which are set to mimic the expected mineralogy and chemistry on Mars. With regard to the first use of LIBS in space, we analyze and quantify, often for the first time, each of the advantages of using stand-off LIBS in space: no sample preparation, analysis within its petrological context, dust removal, sub-millimeter scale investigation, multi-point analysis, the ability to carry out statistical surveys and whole-rock analyses, and rapid data acquisition. We conclude with a discussion of ChemCam performance to survey the geochemistry of Mars, and its valuable support of decisions about selecting where and whether to make observations with more time and resource-intensive tools in the rover's instrument suite. In the end, we present a bird's-eye view of the many scientific results: discovery of felsic Noachian crust, first observation of hydrated soil, discovery of manganese-rich coatings and fracture fills indicating strong oxidation potential in Mars' early atmosphere, characterization of soils by grain size, and wide scale mapping of sedimentary strata, conglomerates, and diagenetic materials.
Published: 2016

43. Overview of ChemCam Activities and Discoveries During 4 Years at Gale Crater, Mars

Author: Schröder, Susanne, Wiens, R. C., Maurice, S., Gasnault, O., and Cousin, A.
Subjects: LIBS, ChemCam, Mars, MSL, Mars Science Laboratory, Institut für Optische Sensorsysteme
Published: 2016

44. The Chandrayaan-1 X-ray Spectrometer: First results

Author: Weider, S. Z., Kellett, B. J., Swinyard, B. M., Crawford, I. A., Joy, K. H., Grande, M., Howe, C. J., Huovelin, J., Narendranath, S., Alha, L., Anand, M., Athiray, P. S., Bhandari, N., Carter, J. A., Cook, A. C., d'Uston, L. C., Fernandes, V. A., Gasnault, O., Goswami, J. N., Gow, J. P. D., Holland, A. D., Koschny, D., Lawrence, D. J., Maddison, B. J., Maurice, S., McKay, D. J., Pieters, C., Rothery, D. A., Russell, S. S., Okada, Tatsuaki, Space Science Department, Planetary and Space Sciences [Milton Keynes] (PSS), School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU)-Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), The Open University [Milton Keynes] (OU), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), University of Oulu, Department of Mineralogy, Natural History Museum, Department of Mineralogy, Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), 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), Agence Spatiale Européenne = European Space Agency (ESA), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics, 01 natural sciences, Spectral line, law.invention, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, law, 0103 physical sciences, Gamma spectroscopy, Gamma-ray spectroscopy, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Basalt, Physics, Solar flare, Spectrometer, Lunar chemistry, Lunar regolith, Gamma ray, Astronomy, Astronomy and Astrophysics, Regolith, Space and Planetary Science, Lunar X-ray spectroscopy, Lunar crust, Flare
Abstract: 著者人数: 33名, Accepted: 2011-08-26, 資料番号: SA1003185000
Published: 2012

45. Fluidized-sediment pipes in Gale crater, Mars, and possible Earth analogs

Author: Rubin, David M., primary, Fairén, A.G., additional, Martínez-Frías, J., additional, Frydenvang, J., additional, Gasnault, O., additional, Gelfenbaum, G., additional, Goetz, W., additional, Grotzinger, J.P., additional, Le Mouélic, S., additional, Mangold, N., additional, Newsom, H., additional, Oehler, D.Z., additional, Rapin, W., additional, Schieber, J., additional, and Wiens, R.C., additional
Published: 2016
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46. SuperCam Remote Micro-Imager on Mars 2020

Author: Gasnault, O., Maurice, S., Wiens, R. C., Le Mouélic, S., Fischer, W. W., Cais, Ph., Mccabe, K., Reess, J.-M., Virmontois, C., Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), ELECTRONIQUE 2015, 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)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (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), Centre National d'Études Spatiales [Toulouse] (CNES), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA]
Abstract: International audience; SuperCam was selected on the Mars 2020 rover to perform high-resolution chemistry, mineralogy, and imaging at stand-off distances. We describe the imaging part.
Published: 2015

47. Chemostratigraphy of potassic sedimentary rocks in Gale crater, Mars, as seen by ChemCam onboard Curiosity

Author: Le Deit, L., Mangold, N., Forni, Olivier, Schröder, S.E., Stack, K M, Sumner, D., Fisk, M., Dromart, G., Blaney, D., Fabre, Cecile, Gasnault, O., Lanza, Nina, Lasue, J., Mouélic, S. Le, Maurice, S., McLennan, S M, Rapin, W., Rice, M., Sautter, V., and Wiens, R. C.
Subjects: Planetengeologie, Mars, Gale crater
Published: 2015

48. ChemCam activities and discoveries during the nominal mission of the Mars Science Laboratory in Gale crater, Mars

Author: Maurice, S., Clegg, S. M., Wiens, R. C., Gasnault, O., Rapin, W., Cousin, A., Mangold, N., Nachon, M., Anderson, R. B., Lanza, N. L., Fabre, C., Lasue, J., Meslin, P. -Y., Dyar, M. D., Francis, R., Frydenvang, J., Gondet, B., Ehlmann, B. L., Herkenhoff, K. E., Johnson, J. R., Langevin, Y., Madsen, M. B., Melikechi, N., Lacour, J. -L., Le Mouelic, S., Lewin, E., Ollila, A. M., Schroeder, S., Sirven, J. -B., Tokar, R. L., Toplis, M. J., d'Uston, C., Vaniman, D. T., Vasavada, A. R., Maurice, S., Clegg, S. M., Wiens, R. C., Gasnault, O., Rapin, W., Cousin, A., Mangold, N., Nachon, M., Anderson, R. B., Lanza, N. L., Fabre, C., Lasue, J., Meslin, P. -Y., Dyar, M. D., Francis, R., Frydenvang, J., Gondet, B., Ehlmann, B. L., Herkenhoff, K. E., Johnson, J. R., Langevin, Y., Madsen, M. B., Melikechi, N., Lacour, J. -L., Le Mouelic, S., Lewin, E., Ollila, A. M., Schroeder, S., Sirven, J. -B., Tokar, R. L., Toplis, M. J., d'Uston, C., Vaniman, D. T., and Vasavada, A. R.
Published: 2016

49. Elemental geochemistry of sedimentary rocks at Yellowknife Bay, Gale crater, Mars

Author: McLennan, S.M., Anderson, R.B., Bell III, J.F., Bridges, J.C., Calef III, F., Campbell, J.L., Clark, B.C., Clegg, S., Conrad, P., Cousin, A., Des Marais, D.J., Dromart, G., Dyar, M.D., Edgar, L.A., Ehlmann, B.L., Fabre, C., Forni, O., Gasnault, O., Gellert, R., Gordon, S., Grant, J.A., Grotzinger, J.P., Gupta, S., Herkenhoff, K.E., Hurowitz, J.A., King, P.L., Mouélic, S.L., Leshin, L.A., Léveillé, R., Lewis, K.W., Mangold, N., Maurice, S., Ming, D.W., Morris, R.V., Nachon, M., Newsom, H.E., Ollila, A.M., Perrett, G.M., Rice, M.S., Schmidt, M.E., Schwenzer, S.P., Stack, K., Stolper, E.M., Sumner, D.Y., Treiman, A.H., VanBommel, S., Vaniman, D.T., Vasavada, A., Wiens, R.C., NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, NWO-NSO: The role of perchlorates in the preservation of organic compounds on Mars, Petrology, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), GeoRessources, Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS), MSL Science Team, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), and Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Geologic Sediments, 010504 meteorology & atmospheric sciences, Extraterrestrial Environment, Iron, Curiosity rover, Geochemistry, Mars, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, Weathering, 01 natural sciences, Calcium Sulfate, Sedimentary depositional environment, Halogens, 0103 physical sciences, Exobiology, MSL, Magnesium, Geochemistry of sedimentary rocks, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Basalt, Martian, Multidisciplinary, Silicates, Water, Mars Exploration Program, Hydrogen-Ion Concentration, Ferrosoferric Oxide, Diagenesis, Bays, Rocknest, Sedimentary rock, Chlorine, Geology
Abstract: International audience; Sedimentary rocks examined by the Curiosity rover at Yellowknife Bay, Mars, were derived from sources that evolved from an approximately average martian crustal composition to one influenced by alkaline basalts. No evidence of chemical weathering is preserved, indicating arid, possibly cold, paleoclimates and rapid erosion and deposition. The absence of predicted geochemical variations indicates that magnetite and phyllosilicates formed by diagenesis under low-temperature, circumneutral pH, rock-dominated aqueous conditions. Analyses of diagenetic features (including concretions, raised ridges, and fractures) at high spatial resolution indicate that they are composed of iron-and halogen-rich components, magnesium-iron-chlorine-rich components, and hydrated calcium sulfates, respectively. Composition of a cross-cutting dike-like feature is consistent with sedimentary intrusion. The geochemistry of these sedimentary rocks provides further evidence for diverse depositional and diagenetic sedimentary environments during the early history of Mars.
Published: 2014

50. Igneous mineralogy at Bradbury Rise: The first ChemCam campaign at Gale crater

Author: Sautter, V., Fabre, C., Forni, O., J. Toplis, M., Cousin, A., M. Ollila, A., Y. Meslin, P., Maurice, S., C. Wiens, R., Baratoux, David, Mangold, N., Le Mouélic, S., Gasnault, O., Berger, G., Lasue, J., A. Anderson, R., Lewin, E., Schmidt, M., Dyar, D., L. Ehlmann, B., Bridges, J., Clark, B., Pinet, P., Muséum national d'Histoire naturelle (MNHN), GeoRessources, Centre National de la Recherche Scientifique (CNRS)-Université de Lorraine (UL)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Institut national des sciences de l'Univers (INSU - CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Institute of Meteoritics [Albuquerque] (IOM), The University of New Mexico [Albuquerque], Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), United States Geological Survey [Reston] (USGS), Institut des Sciences de la Terre (ISTerre), Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-PRES Université de Grenoble-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Department of Earth Sciences [St. Catharines], Brock University [Canada], Department of Astronomy of the Mount Holyoke College, Mount Holyoke College, Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Space Research Centre [Leicester], University of Leicester, Space Science Institute [Boulder] (SSI), Centre National de la Recherche Scientifique (CNRS)-PRES Université de Grenoble-Université Joseph Fourier - Grenoble 1 (UJF)-Institut Français des Sciences et Technologies des Transports, de l'Aménagement et des Réseaux (IFSTTAR)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de recherche pour le développement [IRD] : UR219-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Institut national des sciences de l'Univers (INSU - CNRS)-Centre de recherches sur la géologie des matières premières minérales et énergétiques (CREGU)-Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.STU]Sciences of the Universe [physics]/Earth Sciences
Abstract: International audience; Textural and compositional analyses using Chemistry Camera (ChemCam) remotemicroimager and laser-induced breakdown spectroscopy (LIBS) have been performed on fivefloat rocks and coarse gravels along the first 100 m of the Curiosity traverse at Bradbury Rise.ChemCam, the first LIBS instrument sent to another planet, offers the opportunity to assessmineralogic diversity at grain-size scales (~ 100 μm) and, from this, lithologic diversity. Depthprofiling indicates that targets are relatively free of surface coatings. One type of igneous rock isvolcanic and includes both aphanitic (Coronation) and porphyritic (Mara) samples. Theporphyritic sample shows dark grains that are likely pyroxene megacrysts in a fine-grainedmesostasis containing andesine needles. Both types have magnesium-poor basalticcompositions and in this respect are similar to the evolved JakeMatijevic rock analyzed furtheralong the Curiosity traverse both with Alpha-Particle X-ray Spectrometer and ChemCaminstruments. The second rock type encountered is a coarse-grained intrusive rock (Thor Lake)showing equigranular texture with millimeter size crystals of feldspars and Fe-Ti oxides. Such arock is not unique at Gale as the surrounding coarse gravels (such as Beaulieu) and theconglomerate Link are dominated by feldspathic (andesine-bytownite) clasts. Finally, alkalifeldspar compositions associated with a silica polymorph have been analyzed in fractured fillingmaterial of Preble rock and in Stark, a putative pumice or an impact melt. These observationsdocument magmatic diversity at Gale and describe the first fragments of feldspar-richlithologies (possibly an anorthosite) that may be ancient crust transported from the crater rimand now forming float rocks, coarse gravel, or conglomerate clasts.
Published: 2014

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