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51. The dynamic atmospheric and aeolian environment of Jezero crater, Mars

Author: Newman, Claire E., primary, Hueso, Ricardo, additional, Lemmon, Mark T., additional, Munguira, Asier, additional, Vicente-Retortillo, Álvaro, additional, Apestigue, Víctor, additional, Martínez, Germán M., additional, Toledo, Daniel, additional, Sullivan, Rob, additional, Herkenhoff, Ken E., additional, de la Torre Juárez, Manuel, additional, Richardson, Mark I., additional, Stott, Alexander E., additional, Murdoch, Naomi, additional, Sanchez-Lavega, Agustín, additional, Wolff, Michael J., additional, Arruego, Ignacio, additional, Sebastián, Eduardo, additional, Navarro, Sara, additional, Gómez-Elvira, Javier, additional, Tamppari, Leslie, additional, Smith, Michael D., additional, Lepinette, Alain, additional, Viúdez-Moreiras, Daniel, additional, Harri, Ari-Matti, additional, Genzer, Maria, additional, Hieta, Maria, additional, Lorenz, Ralph D., additional, Conrad, Pan, additional, Gómez, Felipe, additional, McConnochie, Timothy H., additional, Mimoun, David, additional, Tate, Christian, additional, Bertrand, Tanguy, additional, Bell, James F., additional, Maki, Justin N., additional, Rodriguez-Manfredi, Jose Antonio, additional, Wiens, Roger C., additional, Chide, Baptiste, additional, Maurice, Sylvestre, additional, Zorzano, Maria-Paz, additional, Mora, Luis, additional, Baker, Mariah M., additional, Banfield, Don, additional, Pla-Garcia, Jorge, additional, Beyssac, Olivier, additional, Brown, Adrian, additional, Clark, Ben, additional, Montmessin, Franck, additional, Fischer, Erik, additional, Patel, Priyaben, additional, del Río-Gaztelurrutia, Teresa, additional, Fouchet, Thierry, additional, Francis, Raymond, additional, and Guzewich, Scott D., additional
Published: 2022
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52. First results from Atmospheric Observations of CO2, H2O, O2 and CO Abundances with SuperCam on Mars 2020

Author: Montmessin, Franck, Mcconnochie, T., Fouchet, Thierry, Royer, Clément, Knutsen, Elise Wright, Bertrand, Tanguy, Forni, O., Pilleri, Paolo, Gasnault, Olivier, Lacombe, Gaetan, Lasue, Jérémie, Legett, C., Lemmon, M., Newell, R., Venhaus, D., Maurice, Sylvestre, Wiens, R., 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), Space Science Institute [Boulder] (SSI), University of Maryland [College Park], University of Maryland System, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), and Lunar and Planetary Institute
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology
Abstract: International audience
Published: 2022

53. Compositionally and density stratified igneous terrain in Jezero crater, Mars

Author: Wiens, Roger C., Udry, Arya, Beyssac, Olivier, Quantin-Nataf, Cathy, Mangold, Nicolas, Cousin, Agnès, Mandon, Lucia, Bosak, Tanja, Forni, Olivier, McLennan, Scott M., Sautter, Violaine, Brown, Adrian, Benzerara, Karim, Johnson, Jeffrey R., Mayhew, Lisa, Maurice, Sylvestre, Anderson, Ryan B., Clegg, Samuel M., Crumpler, Larry, Gabriel, Travis S. J., Gasda, Patrick, Hall, James, Horgan, Briony H. N., Kah, Linda, Legett, Carey, Madariaga, Juan Manuel, Meslin, Pierre-Yves, Ollila, Ann M., Poulet, Francois, Royer, Clement, Sharma, Shiv K., Siljeström, Sandra, Simon, Justin I., Acosta-Maeda, Tayro E., Alvarez-Llamas, Cesar, Angel, S. Michael, Arana, Gorka, Beck, Pierre, Bernard, Sylvain, Bertrand, Tanguy, Bousquet, Bruno, Castro, Kepa, Chide, Baptiste, Clavé, Elise, Cloutis, Ed, Connell, Stephanie, Dehouck, Erwin, Dromart, Gilles, Fischer, Woodward, Fouchet, Thierry, Francis, Raymond, Frydenvang, Jens, Gasnault, Olivier, Gibbons, Erin, Gupta, Sanjeev, Hausrath, Elisabeth M., Jacob, Xavier, Kalucha, Hemani, Kelly, Evan, Knutsen, Elise, Lanza, Nina, Laserna, Javier, Lasue, Jeremie, Le Mouélic, Stéphane, Leveille, Richard, Lopez Reyes, Guillermo, Lorenz, Ralph, Manrique, Jose Antonio, Martinez-Frias, Jesus, McConnochie, Tim, Melikechi, Noureddine, Mimoun, David, Montmessin, Franck, Moros, Javier, Murdoch, Naomi, Pilleri, Paolo, Pilorget, Cedric, Pinet, Patrick, Rapin, William, Rull, Fernando, Schröder, Susanne, Shuster, David L., Smith, Rebecca J., Stott, Alexander E., Tarnas, Jesse, Turenne, Nathalie, Veneranda, Marco, Vogt, David S., Weiss, Benjamin P., Willis, Peter, Stack, Kathryn M., Williford, Kenneth H., Farley, Kenneth A., Los Alamos National Laboratory (LANL), University of Nevada [Las Vegas] (WGU Nevada), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'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), Department of Earth, Atmospheric and Planetary Sciences [MIT, Cambridge] (EAPS), Massachusetts Institute of Technology (MIT), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Plancius Research LLC, Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Department of Geological Sciences [Boulder], University of Colorado [Boulder], Astrogeology Science Center [Flagstaff], United States Geological Survey [Reston] (USGS), New Mexico Museum of Natural History and Science (NMMNHS), Department of Earth, Atmospheric, and Planetary Sciences [West Lafayette] (EAPS), Purdue University [West Lafayette], Department of Earth and Planetary Sciences [Knoxville], The University of Tennessee [Knoxville], University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Hawai'i [Honolulu] (UH), RISE Research Institutes of Sweden, Center for Isotope Cosmochemistry and Geochronology, NASA Johnson Space, Universidad de Málaga [Málaga] = University of Málaga [Málaga], Department of Chemistry and Biochemistry [Columbia, South Carolina], University of South Carolina [Columbia], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), University of Winnipeg, California Institute of Technology (CALTECH), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), University of Copenhagen = Københavns Universitet (UCPH), McGill University = Université McGill [Montréal, Canada], Department of Earth Science and Engineering [Imperial College London], Imperial College London, 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), 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), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), University of Maryland [College Park], University of Maryland System, Department of Physics and Applied Physics [Lowell], University of Massachusetts [Lowell] (UMass Lowell), University of Massachusetts System (UMASS)-University of Massachusetts System (UMASS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), DLR Institute of Optical Sensor Systems, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley] (UC Berkeley), and University of California (UC)-University of California (UC)
Subjects: emplacement, LIBS, shergottites, Multidisciplinary, Mars2020, Mars, Perseverance, system, rocks, reflectance spectra, Vis, in-situ, SuperCam, [SDU]Sciences of the Universe [physics], rover, IR, origin, surface, identification, Raman, olivine
Abstract: Before Perseverance, Jezero crater's floor was variably hypothesized to have a lacustrine, lava, volcanic airfall, or aeolian origin. SuperCam observations in the first 286 Mars days on Mars revealed a volcanic and intrusive terrain with compositional and density stratification.The dominant lithology along the traverse is basaltic, with plagioclase enrichment in stratigraphically higher locations. Stratigraphically lower, layered rocks are richer in normative pyroxene. The lowest observed unit has the highest inferred density and is olivine-rich with coarse (1.5 millimeters) euhedral, relatively unweathered grains, suggesting a cumulate origin. This is the first martian cumulate and shows similarities to martian meteorites, which also express olivine disequilibrium. Alteration materials including carbonates, sulfates, perchlorates, hydrated silicates, and iron oxides are pervasive but low in abundance, suggesting relatively brief lacustrine conditions. Orbital observations link the Jezero floor lithology to the broader Nili-Syrtis region, suggesting that density-driven compositional stratification is a regional characteristic. Funding was provided by the following sources: NASA's Mars exploration program, including contracts NNH15AZ24I and NNH13ZDA018O to LANL. LANL LDRD code XWHW contributed to calibrations. A portion of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). NASA RSSPS grants supported J.I.S., grantnumber 80NSSC20K0239 supported L. Hausrath, grant number 80NSSC20K0240 supported L. Mayhew, and grant number 80NSSC21K0330 supported A.U. CNRS and CNES supported the work in France. DLR supported S.Sc. and D.S.V. The Swedish National Space Agency (contracts 137/19 and 2021-00092) supported S.Si. The Natural Sciences and Engineering Research Council of Canada (NSERC) and the Canadian Space Agency (CSA) supported E.C., S.C., and N.T. The Ministry of Economy and Competitiveness (MINECO, SPAIN) grant PID2019-107442RB-C31 supported F.R., G.L.R., J.A.M., and M.
Published: 2022

54. Water vapor at Jezero Crater, Mars

Author: Tamppari, Leslie K., Martínez, Germán, Rodríguez Manfredi, Jose, de la Torre-Juárez, Manuel, Hieta, Maria, Polkko, Jouni, Jaakonaho, Iina, Genzer, Maria, Harri, Ari-Matti, Mcconnochie, Timothy H., Montmessin, Franck, Smith, Michael D., Wolff, Michael, Fischer, Erik, Gomez, Felipe, Zorzano, Maria‐paz, Viudez-Moreiras, Daniel, Patel, Priyaben, Lemmon, Mark, Knutsen, Elise Wright, Pla‐garcía, Jorge, Fouchet, Thierry, and Cardon, Catherine
Subjects: [SDU] Sciences of the Universe [physics]
Abstract: Water on Mars is of interest today to assess the current cycling of water in and out of the regolith, cycling of water on and off of the polar caps, and to understand the current habitability potential of Mars. The regolith at polar and non-polar latitudes is an important reservoir for water storage, and an important resource for human exploration, and exchange of water between the regolith and atmosphere may play an important role in the global water cycle. Understanding water on Mars today helps us model the water cycle during different epochs on Mars, during which there was much more liquid water present in the system and Mars may have been inhabited.Additional time coverage and an additional location on the surface of Mars provided by the Perseverance MEDA relative humidity measurements at Jezero crater help reveal the regional similarities and differences across Mars. In addition, the Perseverance SuperCam or TIRS instruments can be used with the MEDA measurements of relative humidity to detect frost formation [2], to assess diurnal changes in the near-surface water content, possibly due to subsurface exchange (e.g., [5-6, 1]) or consistent with surface frost [2], and to check whether the environmental conditions at the surface and in the near surface are compatible with the formation of liquid brines [3-4].We examine the water vapor in the Martian atmosphere in the vicinity of Jezero Crater, Mars, where the Perseverance Rover is currently operating and acquiring data. We place the new water measurements from the rover instruments into the broader context, relating measurements to those of orbiters and other landers.
Published: 2022

55. The first direct measurement of the saturnian stratospheric winds

Author: Benmahi, Bilal, primary, Cavalié, Thibault, additional, Fouchet, Thierry, additional, Lellouch, Emmanuel, additional, Moreno, Raphael, additional, Guerlet, Sandrine, additional, Spiga, Aymeric, additional, and Bardet, Deborah, additional
Published: 2022
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56. Infrared Reflectance of Jezero geological units from Supercam/Mars2020 Observations

Author: Quantin-Nataf, Cathy, primary, Mandon, Lucia, additional, Royer, Clement, additional, Beck, Pierre, additional, Montmessin, Frank, additional, Forni, Olivier, additional, Le Mouelic, Stephane, additional, Poulet, François, additional, Johnson, Jeffrey, additional, Fouchet, Thierry, additional, Dehouck, Erwin, additional, Brown, Adrian, additional, Tarnas, Jesse, additional, Pilleri, Paolo, additional, Gasnault, Olivier, additional, Mangold, Nicolas, additional, Maurice, Sylvestre, additional, and Wiens, Roger, additional
Published: 2022
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57. Ground-based HDO and SO2 thermal mapping on Venus : An update

Author: Encrenaz, Therese, primary, Greathouse, Thomas, additional, Giles, Rohini, additional, Widemann, Thomas, additional, Bézard, Bruno, additional, and Fouchet, Thierry, additional
Published: 2022
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58. First atmospheric results produced by the SuperCam instrument on Mars2020

Author: Montmessin, Franck, primary, McConnochie, Timothy, additional, Fouchet, Thierry, additional, Forni, Olivier, additional, Pilleri, Paolo, additional, Royer, Clément, additional, Knutsen, Elise, additional, Bertrand, Tanguy, additional, Gasnault, Olivier, additional, Lasue, Jeremie, additional, Legett, Carey, additional, Lemmon, Mark, additional, Newell, Raymond, additional, Venhaus, Dawn, additional, Maurice, Sylvestre, additional, and Wiens, Roger, additional
Published: 2022
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59. Detection of hydration spectral signatures with IRS/SuperCam, Perseverance rover: instrument performance

Author: Royer, Clément, primary, Fouchet, Thierry, additional, Montmessin, Franck, additional, Poulet, Francois, additional, Forni, Olivier, additional, Johnson, Jeffrey, additional, Gasnault, Olivier, additional, Mandon, Lucia, additional, Quantin-Nataf, Cathy, additional, Beck, Pierre, additional, Ollila, Ann, additional, Pilorget, Cédric, additional, Bernardi, Pernelle, additional, Reess, Jean-Michel, additional, Newell, Raymond, additional, Maurice, Sylvestre, additional, and Wiens, Roger, additional
Published: 2022
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60. Alteration minerals assemblage on the floor of Jezero crater, Mars: one year of SuperCam IR observations onboard the Perseverance rover

Author: Mandon, Lucia, primary, Quantin-Nataf, Cathy, additional, Beck, Pierre, additional, Royer, Clément, additional, Fouchet, Thierry, additional, Dehouck, Erwin, additional, Forni, Olivier, additional, Johnson, Jeffrey, additional, Poulet, Francois, additional, Montmessin, Franck, additional, Le Mouélic, Stéphane, additional, Gasnault, Olivier, additional, Maurice, Sylvestre, additional, and Wiens, Roger, additional
Published: 2022
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61. The acoustic properties of the Mars atmosphere at Jezero crater

Author: Chide, Baptiste, Maurice, Sylvestre, Mimoun, David, Murdoch, Naomi, Lorenz, Ralph, Stott, Alexander, Jacob, Xavier, Lanza, Nina, Wiens, Roger, Maki, Justin, Ollila, Ann, Lasue, Jérémie, Montmessin, Franck, Fouchet, Thierry, Alvarez, Cesar, Laserna, Javier, Schroder, Susanne, Vogt, David, and Fouchet, Thierry
Subjects: [SDU] Sciences of the Universe [physics]
Abstract: On February 18, 2021 NASAs Perseverance rover landed in Jezero Crater carrying two microphones operating on the surface of Mars, EDLCAM and Supercam. Therefore, it allows the unique opportunity to observe the atmosphere with continuous recordings and to conduct free-field sound propagation experiments on the Mars atmosphere. Positioned on top of the rovers mast, the Supercam microphone records audible sounds from 20 Hz to 10 kHz that originate from three main sources: the atmosphere (turbulence, wind), the Supercam laser-induced sparks on rocks and other rover sounds, especially the aeroacoustic signal generated by the high-speed rotating blades of the Ingenuity rotorcraft. These sounds spread over the entire frequency domain accessible by the microphone: (i) the turbulence/wind-induced acoustic signal starts from the lowest frequency, continuously up to few hundred Hz depending on the wind activity. It has a decreasing slope consistent with the dissipative regime. (ii) The frequency content of the laser-induced spark lies at higher frequencies (2 - 10 kHz) where it shows destructive interference gaps due to echoes on the mast structure and on nearby rocks. (iii) Rover generated sounds (pump, motor) are often monotonic. For instance, Ingenuity flights are heard at the blades passing frequency of ~84Hz and its first harmonic at 168 Hz. The Supercam microphone is now used daily to capture the diversity and the wealth of these phenomena. This presentation focuses on sound propagation properties of the Mars atmosphere, in particular, the first in situ measurement of the sound speed and acoustic intrinsic attenuation. The average sound speed (~240m/s) along the propagation path is derived from the time of flight of the laser-induced acoustic wave from the ground to the microphone. It is combined with the sound speed measured at the microphone location determined from the destructive interference gap in the spectrum. Then, it gives insights into the high frequency air temperature variations over the first two meters from the ground. Moreover, the evolution of the laser spark amplitude with the distance of the target is used to retrieve an attenuation coefficient between 2 and 10 kHz. At low frequency, the attenuation coefficient is studied with the helicopter tones. It is used to constrain existing models in the literature.
Published: 2021

62. Spectral diversity of rocks and regolith at Jezero crater, Mars, as seen by the SuperCam VISIR spectrometer onboard Perseverance

Author: Mandon, Lucia, Royer, Clement, Beck, Pierre, Quantin-Nataf, Cathy, Fouchet, Thierry, Poulet, Francois, Montmessin, Franck, Johnson, Jeffrey, Forni, Olivier, Le Mouelic, Stephane, Dehouck, Erwin, Pilleri, Paolo, Legett, Chip, Brown, Adrian, Cloutis, Edward, Gasnault, Olivier, Maurice, Sylvestre, Wiens, Roger, Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Los Alamos National Laboratory (LANL), Plancius Research LLC, and University of Winnipeg
Subjects: [SDU]Sciences of the Universe [physics]
Abstract: International audience; The Perseverance rover (Mars 2020 mission, NASA) landed in the ancient lakebed of Jezero crater, Mars on February 2021. The payload includes the SuperCam instrument, which combines various remote-sensing techniques to investigate elemental and mineralogical composition. In particular, the near-infrared spectrometer of SuperCam is a novel instrument on the Martian surface. The spectra, together with data from additional visible spectrometers, cover the 0.390.85 m (VIS) and 1.32.6 m (IR) ranges, allowing the identification of a wide variety of minerals. Here, we present the spectral diversity in the VISIR of rocks and soils in the vicinity of the rovers traverse. As of sol 130, most of the rocks analyzed so far are dark-toned rocks in the crater floor (Cf-fr unit) with variable dust cover. Some variability in reflectance levels and absorption bands is observed within and among the rocks, but overall, they share similar spectral characteristics. In particular, most rocks exhibit an absorption near 1.9 m (indicating the presence of water). This band is usually observed weakly or is absent in local regolith but is detected with a depth up to ~20% in the rocks, indicating probably several wt.% of bound water. While mixing of different phases occurs in the few mm of the field of view of the spectrometer, the following candidates were identified: dust, an oxy-hydroxide (e.g., ferrihydrite), an iron-rich phyllosilicate (e.g., nontronite or hisingerite) and an AlOH-bearing phase. Contrary to what have been inferred from the orbit, no unequivocal mafic mineral signature has yet been identified in a rock target in the VISIR implying low mafic minerals content or small associated grain size. However, the soils exhibit a signature of olivine mixed with pyroxene (intermediate Ca content). Portions of sand ripples are strongly dominated by the olivine signature. The detection of widespread hydration features supports that some pervasive water-rock interactions occurred in the past near the Perseverance landing site. From CRISM orbital data, it is likely that the rover will be driving through areas exhibiting progressively increasing hydration throughout its traverse: future measurements on these potentially more hydrated and diverse rocks are expected to bring new insights into the past environment at Jezero crater.
Published: 2021

63. Long distance observations of Jezero craters geological units by the SuperCam instrument onboard Perseverance/Mars2020

Author: Quantin Nataf, Cathy, Mandon, Lucia, Gasnault, Olivier, Royer, Clement, Beck, Pierre, Forni, Olivier, Montmessin, Franck, Le Mouelic, Stephane, Fouchet, Thierry, Dehouck, Erwin, Poulet, Francois, Johnson, Jeffrey, Brown, Adrian, Tarnas, Jesse, Pilleri, Paolo, Mangold, Nicolas, Maurice, Sylvestre, Wiens, Roger, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Planétologie et Géosciences [UMR_C 6112] (LPG), Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Nantes Université - pôle Sciences et technologie, Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Plancius Research LLC, Wesleyan University, Laboratoire de Planétologie et Géosciences - Le Mans (LPG - Le Mans), Nantes Université (Nantes Univ)-Nantes Université (Nantes Univ)-Université d'Angers (UA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Nantes université - UFR des Sciences et des Techniques (Nantes univ - UFR ST), and Los Alamos National Laboratory (LANL)
Subjects: [SDU]Sciences of the Universe [physics]
Abstract: International audience; On February 18, 2021, NASAs Mars 2020 Perseverance rover landed successfully in Jezero crater. Several geological and compositional units have previously been identified from orbital data analysis [1,2]: a dark pyroxene-bearing floor unit; an olivine-bearing unit exposed in erosional windows partially altered into phyllosilicates and carbonates [3]; a deltaic complex with possible remnants and marginal carbonate-bearing unit [1]. The SuperCam instrument contains a suite of techniques including passive spectroscopy in the 0.40-0.85 (VIS) and 1.3-2.6 microns (IR) wavelength ranges, and a camera (RMI- Remote Micro-Imager) providing high resolution context images [4]. Since the landing, SuperCam has acquired tens of observations on distant targets (from 10s of m to 20 km) with VISIR and RMI techniques. The IFOV of the RMI images ranges from ~100 microns at 10m to ~20 cm at 20 km allowing to solve objects from ~0.5 mm at 10 m to ~1m at 20 km and the VISIR FOV range from 1 cm to 20 m. Distant observations have been acquired on the western delta front, several mesas and hills, on Jezero floor unit (the unit perseverance landed on and investigated in situ), on the olivine-bearing erosional window, and on more distant targets such as the crater rim or marginal carbonate-bearing unit. The observed spectral signatures form different clusters depending on the type of target, confirming the spectral diversity of Jezero geological units. The western delta front and a residual butte informally named Kodiak are clustered together with spectral signatures in agreement with a mixture of olivine, pyroxene and hydrated phases. The spectra of the erosional window into the olivine bearing unit display the strongest red slope between 1.3 and 1.8 microns, suggesting the presence of olivine in both the exposed rocks and the surrounding soils and in addition, the rocks display a strong signature of hydrated phases. The long distance observations of the crater floor unit are in agreement with the spectral signature identified in the vicinity of the rover [5], which confirms the relevance of long distance observations to assess the geological/mineralogical context of Perseverances future traverse. References : [1] Horgan et al., 2020 [2] Goudge et al., 2015 [3] Tarnas, et al., 2019. [4] Wiens, et al., 2021. [5] Mandon et al., this conference
Published: 2021

64. Interferometric millimeter observations of water vapor on Mars and comparison with Mars Express measurements

Author: Fouchet, Thierry, Moreno, Raphael, Lellouch, Emmanuel, Formisano, Vittorio, Giuranna, Marco, and Montmessin, Franck
Published: 2011
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65. First Sounds from Mars

Author: Maurice, sylvestre, primary, Chide, Baptiste, additional, Murdoch, Naomi, additional, Lorenz, Ralph, additional, Mimoun, David, additional, Wiens, Roger, additional, Stott, Alexander, additional, Jacob, Xavier, additional, Bertrand, Tanguy, additional, Montmessin, Franck, additional, Lanza, Nina, additional, Llamas, Cesar Alvarez, additional, Angel, S. M., additional, Aung, M., additional, Balaram, J., additional, Beyssac, Olivier, additional, Cousin, Agnès, additional, Delory, Greg, additional, Forni, Olivier, additional, Fouchet, Thierry, additional, Gasnault, Olivier, additional, Grip, Havard, additional, hecht, Mike, additional, Hoffman, Jeff, additional, Laserna, Javier, additional, Lasue, Jérémie, additional, Maki, Justin, additional, McClean, John, additional, Meslin, Pierre-Yves, additional, Mouélic, Stéphane Le, additional, Munguira, Asier, additional, Newman, Claire, additional, Rodriguez-Manfredi, Jose, additional, Moros, Javier, additional, Pilleri, Paolo, additional, Schroeder, Susanne, additional, Torre, Manuel de la, additional, Ollila, Ann, additional, Tzanetos, Thoedore, additional, Farley, Ken, additional, Stack, Kathryn, additional, and Williford, Ken, additional
Published: 2021
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66. Understanding the Chemistry of the Rocks at Jezero crater, Mars, through the Combined Use of SuperCam Spectroscopic and Optical Techniques

Author: Madariaga, Juan Manuel, primary, Wiens, Roger, additional, Arana, Gorka, additional, Sautter, Violaine, additional, Benzerara, Karim, additional, Udry, Arya, additional, Beyssac, Olivier, additional, Mandon, Lucia, additional, Gasnault, Olivier, additional, Johnson, Jeffrey, additional, Ollila, Ann, additional, Castro, Kepa, additional, Cousin, Agnes, additional, Maurice, Sylvestre, additional, Clegg, Samuel, additional, Anderson, Ryan, additional, Bosak, Tanja, additional, Beck, Pierre, additional, Fouchet, Thierry, additional, Shkolyar, Svetlana, additional, Cloutis, Edward, additional, Quantin-Nataf, Cathy, additional, Torre Fernandez, Imanol, additional, Royer, Clément, additional, Legett, Chip, additional, and Pilleri, Paolo, additional
Published: 2021
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67. Orbital Context and In Situ Observations of Nili Fossae Olivine-Carbonate

Author: Brown, Adrian, primary, Wiens, Roger, additional, Maurice, Sylvestre, additional, Pinet, Patrick, additional, Mandon, Lucia, additional, Le Mouelic, Stephane, additional, Mayhew, Lisa, additional, Udry, Arya, additional, Horgan, Briony, additional, Turenne, Nathalie, additional, Calef, Fred, additional, Cloutis, Edward, additional, Fouchet, Thierry, additional, Royer, Clément, additional, Zorzano, María-Paz, additional, Ravanis, Eleni, additional, Fagents, Sarah, additional, and Fairén, Alberto, additional
Published: 2021
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68. The Supercam Microphone to support LIBS investigation on Mars: review of the first laser-spark recordings

Author: Chide, B., Lanza, Nina, Alvarez, Cesar, Angel, Stanley M., Bernardi, Pernelle, Beyssac, Olivier, Bousquet, Bruno, Cadu, A., Clavé, E., Dehouck, E., Fouchet, Thierry, Gasnault, Olivier, Jacob, X., Laserna, J., Lorenz, Ralph D., Murdoch, Naomi, Stott, A. E., Maurice, Sylestre, Wiens, Roger, Mimoun, David, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), Universidad de Málaga [Málaga] = University of Málaga [Málaga], University of South Carolina, 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, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), Apl, MD, USA, and Europlanet
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The Mars 2020 Perseverance rover, which landed in February 2021, is carrying the SuperCam remote sensing suite [1,2]. It is a multifunctional spectroscopy instrument to analyze Martian rocks and soils with Laser-Induced Breakdown Spectroscopy (LIBS), time resolved Raman and luminescence, Visible and Infrared Reflectance Spectroscopy, and color context imaging. It also includes a microphone (see Fig. 1) that records acoustic pressure fluctuations in the 100 Hz to 10 kHz frequency bandwidth. In particular, it supports LIBS investigation by listening to laser-induced sparks caused by the supersonic expansion of the plasma plume [3, 4]. The microphone also contributes to atmospheric science by recording the ambient noise [wind, turbulence, 5, 6] and it already listened to unique sounds from the Ingenuity Mars Helicopter flights. This abstract focuses on the first analysis of the LIBS acoustic signal recorded on Martian targets near the Octavia E. Butler landing site of Perseverance. Figure 1 - WATSON image of the upper part of the Perseverance Remote Sensing Mast. The microphone is seen in the red rectangle. Credits: NASA/JPL-Caltech/MSSS/ASU Listening to laser-induced sparks on Mars: The LIBS experiment of Supercam uses a pulsed laser in the infrared (1064nm) to ablate rock or soil targets at the Mars surface at distance up to 7 meters. A standard LIBS burst consists of 30 laser shots repeated at the same location on a target. It creates an ablation pit up to hundreds of µm deep, depending on the target hardness (see LIBS pits in Fig. 2) [4, 7]. Longer bursts of 150 shots, called depth profiles, can also be performed to look for any chemical stratification with depth. Figure 2 - Hedgehog target (sol 37) sampled by LIBS (10 points of 30 shots each). (a) Mastcam-Z documentation image. (b) RMI context mosaic highlighting the LIBS pits.Credits: NASA/JPL-Caltech/ASU/MSSS and NASA/JPL-Caltech/LANL/CNES/IRAP It has been shown in lab studies [3, 4] that recording of the LIBS acoustic signal helps to determine the target physical properties (hardness) and also the laser pit volume by looking at the decrease of the signal amplitude with the number of laser shots performed at the same location. In addition, laser sparks may also be used to study rock coatings. In particular, it will help to determine the depth of the transition between a coating and its underlying host rock [8]. Moreover, as the start of the microphone recording is triggered on the laser pulse, the propagation time of the sound wave from the ground up to the microphone height is precisely measured. Therefore, it gives the sound speed along the sound propagation path. This parameter is used to estimate the ‘acoustic temperature’, an average of the air temperature over the two first meters from the ground [9]. First results on Martian targets: Up to sol 78 of the mission, the Supercam microphone has recorded the LIBS acoustic signal from 12 targets, including 3 soil targets and 2 depth profiles. The LIBS acoustic signal recorded on the float rock Hedgehog (sol 37) is represented in Fig. 3. The time series (Fig. 3a) shows a shot-to-shot decrease of the acoustic amplitude over the 30 shots fired in this target. The comparison with the hardness calibration curve presented in [4] suggests a soft target with a Vickers hardness lower than 10 and an ablated volume of about 200 µm. The frequency spectrum (Fig. 3b) is showing an acoustic bandwidth between 2 kHz and 10 kHz (see Fig. 3a), consistent with pre-flight calibrations [10]. Some gaps in the spectrum (5700 Hz, 10900 Hz, 14800 Hz) are indicative of destructive interferences induced by the reflection of the sound wave over the structure of the mast. Some wind-induced signal are also noticed in the time series (see red circles in Fig. 3a). They can be easily filtered, as their frequency content is lower than 500 Hz [6]. However, the influence of the turbulent atmosphere on the LIBS acoustic signal, needs to be assessed, as it was not tested in the laboratory. Figure 3 - Time series (a) and power spectral density (b) of the LIBS acoustic signal recorded on point #5 of the Hedgehog target (sol 37) As for the soil targets, the LIBS acoustic data show a clear decrease with increasing shot number due to shielding within the self-induced hole and also helps to determine whether the laser hit a coarse grain (louder sound) or fine-grained soil. Perspectives: The Supercam microphone has the unique capability to record the acoustic signal induced by the laser-induced plasma. The microphone will help to document the target hardness along the rover traverse and complement the chemical information provided by LIBS by adding an estimation of the ablated depth. This presentation will review results from all the microphone targets observed at the time of the conference. References [1] Wiens R. C et al., SSR 2021 https://doi.org/10.1007/s11214-020-00777-5 [2] Maurice S. et al., SSR 2021, https://doi.org/10.1007/s11214-021-00807-w [3] Chide B. et al, SAB 2019, https://doi.org/10.1016/j.sab.2019.01.008, [4] Chide B et al., SAB 2020 https://doi.org/10.1016/j.sab.2020.106000, 20, [5] Murdoch N. et al, this issue, [6] Stott et al., this issue, [7] Maurice S et al., JAAS 2016, doi:10.1039/c5ja00417a [8] Lanza N.L., LPSC 2020, 2807 [9] Chide B. et al., LPSC 2020 1366, [10] Murdoch N. 2019 PSS doi:10.1016/j.pss.2018.09.009.
Published: 2021

69. The flight radiometric calibration of IRS/SuperCam onboard Perseverance: campaign follow up and performance assessment

Author: Royer, Clement, primary, Fouchet, Thierry, additional, Montmessin, Franck, additional, Poulet, François, additional, Forni, Olivier, additional, Johnson, Jeffrey, additional, Gasnault, Olivier, additional, Quantin-Nataf, Cathy, additional, Beck, Pierre, additional, Ollila, Ann, additional, Mandon, Lucia, additional, Pilorget, Cedric, additional, Bernardi, Pernelle, additional, Reess, Jean-Michel, additional, Newell, Raymond, additional, Maurice, Sylvestre, additional, and Wiens, Roger, additional
Published: 2021
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70. The JWST Giant Planet Atmospheres Programme

Author: Fletcher, Leigh, primary, Hammel, Heidi, additional, Milam, Stefanie, additional, de Pater, Imke, additional, Fouchet, Thierry, additional, Orton, Glenn, additional, Roman, Michael, additional, Rowe-Gurney, Naomi, additional, Melin, Henrik, additional, Wong, Michael, additional, Fry, Patrick, additional, Antuñano, Arrate, additional, Hueso, Ricardo, additional, Tiscareno, Matthew, additional, Irwin, Patrick, additional, Moses, Julianne, additional, Holler, Bryan, additional, Stansberry, John, additional, and Glasse, Alistair, additional
Published: 2021
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71. Comparison of Orbital and in situ NIR-spectra in Jezreo Crater: insight from the first Supercam Infrared Spectrometer data

Author: Quantin-Nataf, Cathy, primary, Mandon, Lucia, additional, Royer, Clement, additional, Tarnas, Jesse, additional, Beck, Pierre, additional, Montmessin, Frank, additional, Forni, Olivier, additional, Le Mouelic, Stephane, additional, Fouchet, Thierry, additional, Gasnault, Olivier, additional, Dehouck, Erwin, additional, Poulet, Francois, additional, Johnson, Jeffey, additional, Brown, Adrian, additional, Pilleri, Paolo, additional, Horgan, Briony, additional, Ehlmann, Bethany, additional, Mangold, Nicolas, additional, Wiens, Roger, additional, and Maurice, Sylvestre, additional
Published: 2021
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72. CH4 abundance in Jupiter's upper atmosphere: A re-analysis of the ISO/SWS 3.3 µm non-LTE emission

Author: López-Puertas, Manuel, primary, Sánchez-López, Alejandro, additional, García-Comas, Maya, additional, Funke, Bernd, additional, Fouchet, Thierry, additional, and Snellen, Ignas, additional
Published: 2021
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73. Observing rocks in Jezero crater, Mars: results of the first months of operation of the SuperCam VISIR spectrometer

Author: Mandon, Lucia, primary, Quantin-Nataf, Cathy, additional, Beck, Pierre, additional, Fouchet, Thierry, additional, Royer, Clément, additional, Montmessin, Franck, additional, Forni, Olivier, additional, Johnson, Jeffrey R., additional, Gasnault, Olivier, additional, Dehouck, Erwin, additional, Poulet, François, additional, Brown, Adrian, additional, Tarnas, Jesse D., additional, Le Mouélic, Stéphane, additional, Bernardi, Pernelle, additional, Reess, Jean-Michel, additional, Newell, Raymond T., additional, Maurice, Sylvestre, additional, and Wiens, Roger C., additional
Published: 2021
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74. First direct measurements of the zonal winds in Saturn's stratosphere

Author: Cavalié, Thibault, primary, Benmahi, Bilal, additional, Fouchet, Thierry, additional, Moreno, Raphael, additional, Lellouch, Emmanuel, additional, Guerlet, Sandrine, additional, Spiga, Aymeric, additional, and Moullet, Arielle, additional
Published: 2021
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75. Mars Atmospheric Science with SuperCam's Visible and Near-Infrared Passive Spectroscopy Modes

Author: Mcconnochie, Timothy H., Fouchet, Thierry, Montmessin, Franck, Beck, P., Chide, B., Francis, R., Gasnault, Olivier, Lasue, Jérémie, Legett, C., Lemmon, Mark T., Maurice, Sylestre, Newell, R. T., Newman, C. E., Venhaus, D. M., Wiens, Roger, Wolff, Michael J., Space Science Institute [Boulder] (SSI), University of Maryland [College Park], University of Maryland System, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Pôle Planétologie du LESIA, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Los Alamos National Laboratory (LANL), and Aeolis Research
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; We present plans to use SuperCam's passive visible and near-infrared ("VISIR") spectroscopy technique for atmospheric science by observing solar radiation scattered by the martian sky. Measurement objectives include O2, CO, H20, and aerosols.
Published: 2021

76. The SuperCam Microphone and Expected First Sounds at Jezero Crater, Mars

Author: Chide, Baptiste, Lanza, N. L., Alvarez, C., Angel, Stanley M., Bernardi, Pernelle, Beyssac, Olivier, Bousquet, Bruno, Cadu, A., Clavé, E., Forni, Olivier, Fouchet, Thierry, Gasnault, Olivier, Jacob, X., Lacombes, G., Laserna, J., Lasue, Jérémie, Lorenz, Ralph D., Meslin, Pierre-Yves, Montmessin, Franck, Moros, J., Murdoch, N., Ollila, Ann, Pilleri, Paolo, Puhorit, P., Reyes-Newell, A. L., Schroder, S., Stott, A., Vogt, D., Maurice, Sylestre, Wiens, Roger, Mimoun, David, 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 Supérieur de l'Aéronautique et de l'Espace (ISAE-SUPAERO), Los Alamos National Laboratory (LANL), Universidad de Málaga [Málaga] = University of Málaga [Málaga], 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, Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Lasers Intenses et Applications (CELIA), Université de Bordeaux (UB)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Institut 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), DLR Institut für Planetenforschung, and Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; This presentation aims to show the expected first results from the SuperCam microphone onboard the NASA Perseverance rover.
Published: 2021

77. Combined LIBS and Acoustics for Differentiating Minerals with Similar LIBS Spectra

Author: Laserna, J., Alvarez-Llamas, C., Purohit, P., Moros, J., Luna, S., Jurado, A., Lopez, F. J., Wiens, Roger, Maurice, Sylestre, Gasnault, Olivier, Beyssac, Olivier, Lanza, Nina, Ollila, Ann, Lasue, Jérémie, Gibbons, E., Fouchet, Thierry, Lorenz, Ralph D., Mimoun, David, Delory, G., Jacob, X., Murdoch, N., Chide, B., Legett, C., Delapp, D., Pilleri, Paolo, Perez, R., Bernardi, Pernelle, Lacombe, Gaétan, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de minéralogie, de physique des matériaux et de cosmochimie (IMPMC), Muséum national d'Histoire naturelle (MNHN)-Institut de recherche pour le développement [IRD] : UR206-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire 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, and Technique
Subjects: [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; The use of the plasma related spectroscopic and acoustic signals combined provide an innovative approach to characterize minerals with similar composition. This approach can help in the interpretation of the future data collected by M2020 mission.
Published: 2021

78. SUPERCAM VISIBLE/NEAR-INFRARED SPECTROSCOPY ONBOARD THE PERSEVERANCE ROVER

Author: Fouchet, Thierry, Johnson, J. R., Forni, O., Reess, J.-M., Bernardi, P., Newell, R. T., Ollila, A., Legett, C., Beck, P., Cousin, A., Royer, C., Pilorget, C., Poulet, F., Pilleri, P., Cloutis, E., Mcconnochie, T., Montmessin, Franck, Brown, A. J., Wiens, R. C., Maurice, S., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), University of Winnipeg, University of Maryland [College Park], University of Maryland System, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (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), 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 national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and 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)
Subjects: [SDU]Sciences of the Universe [physics]
Abstract: International audience; We will present the science objectives and intrument performances of the passive visible/infrared spectroscopy function of the SuperCam instrument suite. We will report on the first spectra that should have been acquired by the time of the conference.
Published: 2021

79. Vertical and meridional distribution of ethane, acetylene and propane in Saturn's stratosphere from CIRS/Cassini limb observations

Author: Guerlet, Sandrine, Fouchet, Thierry, Bezard, Bruno, Simon-Miller, Amy A., and Flasar, F. Michael
Subjects: Atmosphere -- Analysis, Astronomy -- Analysis, Propane -- Analysis, Acetylene -- Analysis, Earth -- Atmosphere, Earth -- Analysis, Astronomy, Earth sciences
Abstract: To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2009.04.002 Byline: Sandrine Guerlet (a), Thierry Fouchet (a), Bruno Bezard (a), Amy A. Simon-Miller (b), F. Michael Flasar (b) Keywords: Saturn; Infrared observations; Atmospheres; Composition Abstract: Measuring the spatial distribution of chemical compounds in Saturn's stratosphere is critical to better understand the planet's photochemistry and dynamics. Here we present an analysis of infrared spectra in the range 600-1400cm.sup.-1 acquired in limb geometry by the Cassini spacecraft between March 2005 and January 2008. We first determine the vertical temperature profiles from 3 to 0.01hPa, at latitudes ranging from 70[degrees]N to 80[degrees]S. We infer a similar meridional temperature gradient at 1-2hPa as in recent previous studies [Fletcher, L.N., Irwin, P.G.J., Teanby, N.A., Orton, G.S., Parrish, P.D., de Kok, R., Howett, C., Calcutt, S.B., Bowles, N., Taylor, F.W., 2007. Icarus 189, 457-478; Howett, C.J.A., Irwin, P.G.J., Teanby, N.A., Simon-Miller, A., Calcutt, S.B., Fletcher, L.N., de Kok, R., 2007. Icarus 190, 556-572]. We then retrieve the vertical profiles of C.sub.2H.sub.6 and C.sub.2H.sub.2 from 3 to 0.01hPa and of C.sub.3H.sub.8 around 1hPa. At 1hPa, the meridional variation of C.sub.2H.sub.2 is found to follow the yearly averaged solar insolation, except for a strong equatorial mole fraction of 8x10.sup.-7, nearly two times higher than expected. This enhancement in abundance can be explained by the descent of hydrocarbon-rich air, with a vertical wind speed at the equator of 0.25[+ or -]0.1 mm/s at 1hPa and 0.4[+ or -]0.15 mm/s at 0.1hPa. The ethane distribution is relatively uniform at 1hPa, with only a moderate 25% increase from 35[degrees]S to 80[degrees]S. Propane is found to increase from north to south by a factor of 1.9, suggesting that its lifetime may be shorter than Saturn's year at 1hPa. At high altitudes (1Pa), C.sub.2H.sub.2 and C.sub.2H.sub.6 abundances depart significantly from the photochemical model predictions of Moses and Greathouse [Moses, J.I., Greathouse, T.K., 2005. J. Geophys. Res. 110, 9007], except at high southern latitudes (62, 70 and 80[degrees]S) and near the equator. The observed abundances are found strongly depleted in the 20-40[degrees]S region and enhanced in the 20-30[degrees]N region, the latter coinciding with the ring's shadow. We favor a dynamical explanation for these anomalies. Author Affiliation: (a) LESIA - Observatoire de Paris, 92195 Meudon, France (b) NASA/Goddard Space Flight Center, Code 693, Greenbelt, MD 20771, USA Article History: Received 18 December 2008; Revised 3 April 2009; Accepted 13 April 2009
Published: 2009

80. Direct detection of auroral and equatorial jets in the stratosphere of Jupiter with ALMA

Author: Cavalié, Thibault, primary, Benmahi, Bilal, additional, Hue, Vincent, additional, Moreno, Raphael, additional, Lellouch, Emmanuel, additional, Fouchet, Thierry, additional, Hartogh, Paul, additional, Rezac, Ladislav, additional, Greathouse, Thomas, additional, Gladstone, Randall, additional, Sinclair, James, additional, Dobrijevic, Michel, additional, Billebaud, Françoise, additional, and Jarchow, Christopher, additional
Published: 2021
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81. Initial SuperCam Visible/Near-Infrared Spectra from the Mars 2020 Perseverance Rover

Author: Johnson, Jeffrey, primary, Fouchet, Thierry, additional, Forni, Olivier, additional, Reess, Jean-Michel, additional, Bernardi, Pernelle, additional, Newell, Raymond, additional, Ollila, Ann, additional, Legett, Chip, additional, Beck, Pierre, additional, Cousin, Agnes, additional, Royer, Clement, additional, Pilorget, Cedric, additional, Poulet, Francois, additional, Cloutis, Ed, additional, McConnochie, Tim, additional, Wiens, Roger C., additional, and Maurice, Sylvestre, additional
Published: 2021
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82. Atmospheric Science with Visible/Near-Infrared Spectra from the Mars 2020 Perseverance Rover

Author: McConnochie, Timothy, primary, Fouchet, Thierry, additional, Montmessin, Franck, additional, Beck, Pierre, additional, Chide, Baptiste, additional, Francis, Raymond, additional, Gasnault, Olivier, additional, Lasue, Jeremie, additional, Legett, Carey, additional, Lemmon, Mark, additional, Maurice, Sylvestre, additional, Newell, Raymond, additional, Newmann, Claire, additional, Venhaus, Dawn, additional, Wiens, Roger, additional, and Wolff, Michael, additional
Published: 2021
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83. Initial results of the first visible and near-infrared spectrometer on the Martian surface: SuperCam unveils Jezero crater’s ground mineralogy

Author: Mandon, Lucia, primary, Fouchet, Thierry, additional, Maurice, Sylvestre, additional, Forni, Olivier, additional, Johnson, Jeffrey, additional, Gasnault, Olivier, additional, Quantin-Nataf, Cathy, additional, Beck, Pierre, additional, Royer, Clément, additional, Ollila, Ann, additional, Poulet, Francois, additional, Pilorget, Cédric, additional, Bernardi, Pernelle, additional, Reess, Jean-Michel, additional, Newell, Raymond, additional, and Wiens, Roger, additional
Published: 2021
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84. Providing unbiased IR spectra on Mars: the ground calibration of the infrared spectrometer onboard Perseverance rover

Author: Royer, Clément, primary, Fouchet, Thierry, additional, Forni, Olivier, additional, Johnson, Jeffrey, additional, Gasnault, Olivier, additional, Quantin-Nataf, Cathy, additional, Beck, Pierre, additional, Ollila, Ann, additional, Mandon, Lucia, additional, Poulet, Francois, additional, Pilorget, Cédric, additional, Bernardi, Pernelle, additional, Reess, Jean-Michel, additional, Newell, Raymond, additional, Maurice, Sylvestre, additional, and Wiens, Roger, additional
Published: 2021
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85. The Calibration of the Infrared Spectrometer of SuperCam/Mars2020: Results and Prediction of the Future Performance on Mars

Author: Royer, C., Poulet, François, Reess, Jean-Michel, Pilorget, C., Hamm, V., Fouchet, Thierry, Maurice, Sylestre, Wiens, Roger, Forni, Olivier, Montmessin, Franck, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire 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, Technique, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Los Alamos National Laboratory (LANL), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Calibration results of the IRS/SuperCam/Mars2020. The transfer function is implemented in an observation simulator to predict instrument's future performance.
Published: 2020

86. HDO and SO2 thermal mapping on Venus

Author: Encrenaz, Thérèse, Greathouse, Thomas K., Marcq, Emmanuel, Sagawa, H., Widemann, Thomas, Bézard, Bruno, Fouchet, Thierry, Lefèvre, Franck, Lebonnois, Sébastien, Atreya, S. K., Lee, Y. J., Giles, R., Watanabe, S., Shao, W., Zhang, Xi, Bierson, C. J., 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), Southwest Research Institute [San Antonio] (SwRI), 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), Kyoto Sangyo University, STRATO - LATMOS, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-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), Planetary Science Laboratory [Ann Arbor] (PSL), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Zentrum für Astronomie und Astrophysik [Berlin] (ZAA), Technical University of Berlin / Technische Universität Berlin (TU), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Hokkaido Information University, Department of Earth and Planetary Sciences [Santa Cruz], University of California [Santa Cruz] (UC Santa Cruz), University of California (UC)-University of California (UC), European Project: 606798,EC:FP7:SPA,FP7-SPACE-2013-1,EUROVENUS(2013), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-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), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Technische Universität Berlin (TU), University of California [Santa Cruz] (UCSC), and University of California-University of California
Subjects: planets and satellites: atmospheres, planets and satellites: terrestrial planets, terrestrial planets [planets and satellites], atmospheres [planets and satellites], planetary systems [infrared], infrared: planetary systems, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience Since January 2012, we have been monitoring the behavior of sulfur dioxide and water on Venus, using the Texas Echelon Cross-Echelle Spectrograph imaging spectrometer at the NASA InfraRed Telescope Facility (IRTF, Mauna Kea Observatory). Here, we present new data recorded in February and April 2019 in the 1345 cm−1 (7.4 μm) spectral range, where SO2, CO2, and HDO (used as a proxy for H2O) transitions were observed. The cloud top of Venus was probed at an altitude of about 64 km. As in our previous studies, the volume mixing ratio (vmr) of SO2 was estimated using the SO2/CO2 line depth ratio of weak transitions; the H2O volume mixing ratio was derived from the HDO/CO2 line depth ratio, assuming a D/H ratio of 200 times the Vienna standard mean ocean water. As reported in our previous analyses, the SO2 mixing ratio shows strong variations with time and also over the disk, showing evidence for the formation of SO2 plumes with a lifetime of a few hours; in contrast, the H2O abundance is remarkably uniform over the disk and shows moderate variations as a function of time. We have used the 2019 data in addition to our previous dataset to study the long-term variations of SO2 and H2O. The data reveal a long-term anti-correlation with a correlation coefficient of −0.80; this coefficient becomes −0.90 if the analysis is restricted to the 2014–2019 time period. The statistical analysis of the SO2 plumes as a function of local time confirms our previous result with a minimum around 10:00 and two maxima near the terminators. The dependence of the SO2 vmr with respect to local time shows a higher abundance at the evening terminator with respect to the morning. The dependence of the SO2 vmr with respect to longitude exhibits a broad maximum at 120–200° east longitudes, near the region of Aphrodite Terra. However, this trend has not been observed by other measurements and has yet to be confirmed.
Published: 2020

87. Latitudinal variation of Saturn photochemistry deduced from spatially-resolved ultraviolet spectra

Author: Prange, ReneE, Fouchet, Thierry, Courtin, ReGis, Connerney, J.E.P., and McConnell, John C.
Subjects: Saturn (Planet) -- Properties, Photochemistry -- Research, Ultraviolet spectroscopy -- Methods, Planets -- Atmosphere, Planets -- Properties, Planets -- Composition, Astronomy, Earth sciences
Abstract: To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2005.11.005 Byline: Renee Prange (a)(b), Thierry Fouchet (a)(c), Regis Courtin (a), J.E.P. Connerney (d), John C. McConnell (e) Keywords: Atmospheres; composition; Photochemistry; Saturn; atmosphere; Ultraviolet observations Abstract: We obtained spatially-resolved ultraviolet spectra of Saturn in 1994 with the Faint Object Spectrometer and Goddard High Resolution Spectrograph of the Hubble Space Telescope. We observed four areas on the planet at 15[degrees]aN, 33[degrees]aS, 41[degrees]aS, and 52[degrees]aS, with a field-of-view of less than 2x2 arcsec.sup.2, compared to the 16-arcsec planet diameter. The wavelength range, 1550-2300 A, encompasses absorption from major hydrocarbons (C.sub.2H.sub.6, C.sub.2H.sub.4, C.sub.2H.sub.2, CH.sub.3C.sub.2H, C.sub.4H.sub.2) and water. We find global hydrocarbon abundances and a C.sub.2H.sub.2 vertical distribution compatible with infrared observations, in contrast with previous analyses of ultraviolet spectra. The stratospheric haze opacity decreases from polar region to the equator. Saturn mid-latitudes are photochemically distinct from the rest of the planet. At 33[degrees]aS, the spectrum requires either (1) a distinctly different C.sub.2H.sub.2 vertical distribution or (2) a locally enhanced water abundance. At 41[degrees]aS, the hydrocarbon abundance exhibits a local minimum, within a global trend of increasing abundance from equator to pole. This global trend may result from an increased abundance of short-lived hydrocarbons such as C.sub.4H.sub.2. Photochemical models predict a depletion of hydrocarbon molecules in the presence of stratospheric water [Moses et al., 2000. Icarus 143, 166-202]. These results are consistent with a localized influx of water, in the form of high charge to mass ratio particles, flowing into Saturn's atmosphere at latitudes magnetically linked to the rings. Author Affiliation: (a) LESIA, Observatoire de Paris, 5 Place Jules Janssen, 92195 Meudon Cedex, France (b) Institut d'astrophysique spatiale, Universite Paris-Sud 11 and CNRS (UMR8617), BAcentstiment 121, F-91405 Orsay, France (c) AOPP, University of Oxford, Clarendon Laboratory, Parks Road, Oxford, OX1 3PU, UK (d) Laboratory for Extraterrestrial Physics, Goddard Space Flight Center, Code 695, Greenbelt, MD 20771, USA (e) Department of Earth and Atmospheric Science, York University, Toronto, Canada M3J 1P3 Article History: Received 7 April 2005; Revised 31 October 2005
Published: 2006

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

Author: Wiens, Roger C., primary, Maurice, Sylvestre, additional, Robinson, Scott H., additional, Nelson, Anthony E., additional, Cais, Philippe, additional, Bernardi, Pernelle, additional, Newell, Raymond T., additional, Clegg, Sam, additional, Sharma, Shiv K., additional, Storms, Steven, additional, Deming, Jonathan, additional, Beckman, Darrel, additional, Ollila, Ann M., additional, Gasnault, Olivier, additional, Anderson, Ryan B., additional, André, Yves, additional, Michael Angel, S., additional, Arana, Gorka, additional, Auden, Elizabeth, additional, Beck, Pierre, additional, Becker, Joseph, additional, Benzerara, Karim, additional, Bernard, Sylvain, additional, Beyssac, Olivier, additional, Borges, Louis, additional, Bousquet, Bruno, additional, Boyd, Kerry, additional, Caffrey, Michael, additional, Carlson, Jeffrey, additional, Castro, Kepa, additional, Celis, Jorden, additional, Chide, Baptiste, additional, Clark, Kevin, additional, Cloutis, Edward, additional, Cordoba, Elizabeth C., additional, Cousin, Agnes, additional, Dale, Magdalena, additional, Deflores, Lauren, additional, Delapp, Dorothea, additional, Deleuze, Muriel, additional, Dirmyer, Matthew, additional, Donny, Christophe, additional, Dromart, Gilles, additional, George Duran, M., additional, Egan, Miles, additional, Ervin, Joan, additional, Fabre, Cecile, additional, Fau, Amaury, additional, Fischer, Woodward, additional, Forni, Olivier, additional, Fouchet, Thierry, additional, Fresquez, Reuben, additional, Frydenvang, Jens, additional, Gasway, Denine, additional, Gontijo, Ivair, additional, Grotzinger, John, additional, Jacob, Xavier, additional, Jacquinod, Sophie, additional, Johnson, Jeffrey R., additional, Klisiewicz, Roberta A., additional, Lake, James, additional, Lanza, Nina, additional, Laserna, Javier, additional, Lasue, Jeremie, additional, Le Mouélic, Stéphane, additional, Legett, Carey, additional, Leveille, Richard, additional, Lewin, Eric, additional, Lopez-Reyes, Guillermo, additional, Lorenz, Ralph, additional, Lorigny, Eric, additional, Love, Steven P., additional, Lucero, Briana, additional, Madariaga, Juan Manuel, additional, Madsen, Morten, additional, Madsen, Soren, additional, Mangold, Nicolas, additional, Manrique, Jose Antonio, additional, Martinez, J. P., additional, Martinez-Frias, Jesus, additional, McCabe, Kevin P., additional, McConnochie, Timothy H., additional, McGlown, Justin M., additional, McLennan, Scott M., additional, Melikechi, Noureddine, additional, Meslin, Pierre-Yves, additional, Michel, John M., additional, Mimoun, David, additional, Misra, Anupam, additional, Montagnac, Gilles, additional, Montmessin, Franck, additional, Mousset, Valerie, additional, Murdoch, Naomi, additional, Newsom, Horton, additional, Ott, Logan A., additional, Ousnamer, Zachary R., additional, Pares, Laurent, additional, Parot, Yann, additional, Pawluczyk, Rafal, additional, Glen Peterson, C., additional, Pilleri, Paolo, additional, Pinet, Patrick, additional, Pont, Gabriel, additional, Poulet, Francois, additional, Provost, Cheryl, additional, Quertier, Benjamin, additional, Quinn, Heather, additional, Rapin, William, additional, Reess, Jean-Michel, additional, Regan, Amy H., additional, Reyes-Newell, Adriana L., additional, Romano, Philip J., additional, Royer, Clement, additional, Rull, Fernando, additional, Sandoval, Benigno, additional, Sarrao, Joseph H., additional, Sautter, Violaine, additional, Schoppers, Marcel J., additional, Schröder, Susanne, additional, Seitz, Daniel, additional, Shepherd, Terra, additional, Sobron, Pablo, additional, Dubois, Bruno, additional, Sridhar, Vishnu, additional, Toplis, Michael J., additional, Torre-Fdez, Imanol, additional, Trettel, Ian A., additional, Underwood, Mark, additional, Valdez, Andres, additional, Valdez, Jacob, additional, Venhaus, Dawn, additional, and Willis, Peter, additional
Published: 2020
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89. Spatial Variations in the Altitude of the CH4 Homopause at Jupiter’s Mid-to-high Latitudes, as Constrained from IRTF-TEXES Spectra

Author: Sinclair, James A., primary, Greathouse, Thomas K., additional, Giles, Rohini S., additional, Antuñano, Arrate, additional, Moses, Julianne I., additional, Fouchet, Thierry, additional, Bézard, Bruno, additional, Tao, Chihiro, additional, Martín-Torres, Javier, additional, Clark, George B., additional, Grodent, Denis, additional, Orton, Glenn S., additional, Hue, Vincent, additional, Fletcher, Leigh N., additional, and Irwin, Patrick G. J., additional
Published: 2020
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90. Monitoring of the temporal evolution of water vapor in the stratosphere of Jupiter with the Odin space telescope between 2002 and 2019

Author: Benmahi, Bilal, primary, Cavalié, Thibault, additional, Dobrijevic, Michel, additional, Biver, Nicolas, additional, Bermudez Diaz, Kenneth, additional, Sandqvist, Aage, additional, Lellouch, Emmanuel, additional, Moreno, Raphael, additional, Fouchet, Thierry, additional, Hue, Vincent, additional, Hartogh, Paul, additional, Billebaud, Francoise, additional, Lecacheux, Alain, additional, Hjalmarson, Ake, additional, Frisk, Urban, additional, and Olberg, Michael, additional
Published: 2020
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91. Search for spatial variation in the jovian [sup.15]N/[sup.14]N ratio from Cassini/CIRS observations

Author: Fouchet, Thierry, Irwin, Patrick G.J., Parrish, Paul, Calcutt, Simon B., Taylor, Frederic W., Nixon, Conor A., and Owen, Tobias
Subjects: Jupiter (Planet) -- Research, Jupiter (Planet) -- Discovery and exploration, Astronomy, Earth sciences
Abstract: We have used the spectra obtained by the Composite Infrared Spectrometer (CIRS) onboard the Cassini spacecraft to search for latitudinal variation in the [sup.15]N/[sup.14]N ratio on Jupiter. We found no variations statistically significant given the observational and model uncertainties. The absence of latitudinal variations demonstrates that [sup.15]N[H.sub.3] is not fractionated in Jupiter's atmosphere, and that the measured [sup.15]N/[sup.14]N represents Jupiter's global value. Our mean value for the global jovian [sup.15]N/[sup.14]N ratio of (2.22 [+ or -] 0.52) x [10.sup.-3] agrees with previous measurements made by Fouchet et al. (2000, Icarus 143,223-243) and Owen et al. (2001, Astrophys. J. 553, L77-L79). We argue that the jovian isotopic [sup.15]N/[sup.14]N ratio must represent the solar nitrogen isotopic composition. The solar [sup.15]N/[sup.14]N ratio hence significantly differs from the terrestrial value: [([sup.15]N/[sup.14]N).sub.[direct sum]] = 3.68 x [10.sup.-3]. This supports the proposition that terrestrial nitrogen originates from a nitrogen reservoir isolated from the main nitrogen reservoir in the proto-solar nebula. The origin and carrier of this isolated reservoir are still unknown. Keywords: Abundances, atmospheres; Atmospheres, composition; Jupiter, atmosphere
Published: 2004

92. Upper limits on hydrogen halides in Jupiter from Cassini/CIRS observations

Author: Fouchet, Thierry, Orton, Glenn, Irwin, Patrick G.J., Calcutt, Simon B., and Nixon, Conor A.
Subjects: Jupiter (Planet) -- Research, Astronomy, Earth sciences
Abstract: We have determined the following upper limits for the mole fraction of hydrogen halides in Jupiter's atmosphere from Cassini/CIRS observations: [HF] < 2.7 x [10.sup.-11], [HCI] < 2.3 x [10.sup.-9], [HBr] < 1.0 x [10.sup.-9], [HI] < 7.6 x [10.sup.-9]. These limits are smaller than solar composition for HF and HC1, and support the halogens' condensation in ammonium salts predicted by thermochemical models for the upper jovian troposphere. Keywords: Jupiter, atmosphere; Atmospheres, composition; Abundances, atmospheres
Published: 2004

93. Meridional Distribution of CH3C2H and C4H2 in Saturn's Stratosphere from CIRS/Cassini Limb and Nadir Observations

Author: Guerlet, Sandrine, Fouchet, Thierry, Bezard, Bruno, Moses, Julianne I, Fletcher, Leigh N, Simon-Miller, Amy A, and Flasar, F. Michael
Subjects: Lunar And Planetary Science And Exploration
Abstract: Limb and nadir spectra acquired by Cassini/CIRS (Composite InfraRed Spectrometer) are analyzed in order to derive, for the first time, the meridional variations of diacetylene (C4H2) and methylacetylene (CH3C2H) mixing ratios in Saturn's stratosphere, from 5 hPa up to 0.05 hPa and 80 deg S to 45 deg N. We find that the C4H2 and CH3C2H meridional distributions mimic that of acetylene (C2H2), exhibiting small-scale variations that are not present in photochemical model predictions. The most striking feature of the meridional distribution of both molecules is an asymmetry between mid-southern and mid-northern latitudes. The mid-southern latitudes are found depleted in hydrocarbons relative to their northern counterparts. In contrast, photochemical models predict similar abundances at north and south mid-latitudes. We favor a dynamical explanation for this asymmetry, with upwelling in the south and downwelling in the north, the latter coinciding with the region undergoing ring shadowing. The depletion in hydrocarbons at mid-southern latitudes could also result from chemical reactions with oxygen-bearing molecules. Poleward of 60 deg S, at 0.1 and 0.05 hPa, we find that the CH3C2H and C4H2 abundances increase dramatically. This behavior is in sharp contradiction with photochemical model predictions, which exhibit a strong decrease towards the south pole. Several processes could explain our observations, such as subsidence, a large vertical eddy diffusion coefficient at high altitudes, auroral chemistry that enhances CH3C2H and C4H2 production, or shielding from photolysis by aerosols or molecules produced from auroral chemistry. However, problems remain with all these hypotheses, including the lack of similar behavior at lower altitudes. Our derived mean mixing ratios at 0.5 hPa of (2.4 +/- 0.3) 10(exp -10) for C4H2 and of (1.1 +/- 0.3) 10(exp -9) for CH3C2H are compatible with the analysis of global-average ISO observations performed by Moses et al. Finally, we provide values for the ratios [CH3C2H]/[C2H2] and [C4H2]/[C2H2] that can constrain the coupled chemistry of these hydrocarbons.
Published: 2010
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94. Ground-based mapping of SO2 and HDO on Venus in the thermal infrared

Author: Encrenaz, Thérèse, Greathouse, T., Marcq, Emmanuel, Sagawa, Hideo, Widemann, Thomas, Bezard, Bruno, Fouchet, Thierry, Lefèvre, Franck, Lebonnois, Sébastien, Atreya, Sushil, Lee, Yeon Joo, Giles, R., Watanabe, Shigeto, 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), Southwest Research Institute [San Antonio] (SwRI), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Kyoto Sangyo University, 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), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, University of Tokyo [Kashiwa Campus], and Hokkaido Information University
Subjects: [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2019

95. Preparing SuperCam for Jezero Crater, Mars: LIBS, Raman, VISIR, Luminescence, Imaging, and Acoustic Analyses

Author: Ollila, A. M., Wiens, R. C., Maurice, Sylvestre, Cousin, Agnès, Anderson, Ryan, Beyssac, Olivier, Bonal, Lydie, Beck, Pierre, Clegg, S., Chide, Baptiste, Deflores, L., Dromart, Gilles, Fischer, W., Forni, Olivier, Fouchet, Thierry, Gasnault, Olivier, Grotzinger, John, Johnson, J., Lasue, Jeremie, Laserna, J., Madariaga, Juan Manuel, Madsen, M., Mangold, Nicolas, Nelson, T., Newell, R., Martinez-Frias, Jesus, McLennan, S., Montmessin, Franck, Robinson, S., Sharma, S., Misra, A., Rull, F., Venhaus, D., Bernardi, Pernelle, Reess, Jean-Michel, Reyes-Newell, A., Poulet, François, Los Alamos National Laboratory (LANL), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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), 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]), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement [Lyon] (LGL-TPE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), California Institute of Technology (CALTECH), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Johns Hopkins University Applied Physics Laboratory [Laurel, MD] (APL), Universidad de Málaga [Málaga] = University of Málaga [Málaga], University of the Basque Country [Bizkaia] (UPV/EHU), University of Copenhagen = Københavns Universitet (KU), 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), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Stony Brook University [SUNY] (SBU), State University of New York (SUNY), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), University of Hawaii, Universidad de Valladolid [Valladolid] (UVa), 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), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), 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), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universidad de Málaga [Málaga], 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), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), IMPEC - 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), NASA-California Institute of Technology (CALTECH), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Cardon, Catherine, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), University of the Basque Country/Euskal Herriko Unibertsitatea (UPV/EHU), University of Copenhagen = Københavns Universitet (UCPH), and 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)
Subjects: [SDU] Sciences of the Universe [physics], [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], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; SuperCam is a multi-functional instrument on the Mars 2020 rover. It will conduct LIBS, Raman, VISIR, luminescence, imaging, and acoustic analyses of the martian surface. Here, we demonstrate the synergy between these techniques.
Published: 2019

96. Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

Author: Vandaele, Ann Carine, Korablev, Oleg, Daerden, Frank, Aoki, Shohei, Thomas, Ian R., ALTIERI, FRANCESCA, López-Valverde, Miguel, Villanueva, Geronimo, Liuzzi, Giuliano, Smith, Michael D., Erwin, Justin T., Trompet, Loïc, Fedorova, Anna A., Montmessin, Franck, Trokhimovskiy, Alexander, Belyaev, Denis A., Ignatiev, Nikolay I., Luginin, Mikhail, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Bertaux, Jean-Loup, Betsis, Daria, Bolsée, David, Clancy, R. Todd, CLOUTIS, EDWARD, Depiesse, Cédric, Funke, Bernd, Garcia-Comas, Maia, Gérard, Jean-Claude, GIURANNA, MARCO, Gonzalez-Galindo, Francisco, Grigoriev, Alexey V., Ivanov, Yuriy S., Kaminski, Jacek, Karatekin, Ozgur, Lefèvre, Franck, Lewis, Stephen, López-Puertas, Manuel, Mahieux, Arnaud, Maslov, Igor, Mason, Jon, Mumma, Michael J., Neary, Lori, Neefs, Eddy, Patrakeev, Andrey, Patsaev, Dmitry, Ristic, Bojan, Robert, Séverine, Schmidt, Frédéric, Shakun, Alexey, Teanby, Nicholas A., Viscardy, Sébastien, Willame, Yannick, Whiteway, James, Wilquet, Valérie, Wolff, Michael J., BELLUCCI, Giancarlo, Patel, Manish R., López-Moreno, Jose-Juan, Forget, François, Wilson, Colin F., Svedhem, Håkan, Vago, Jorge L., Rodionov, Daniel, NOMAD Science Team, Alonso-Rodrigo, Gustavo, Bauduin, Sophie, Carrozzo, Giacomo, Crismani, Matteo, da Pieve, Fabiana, D'AVERSA, EMILIANO, Etiope, Giuseppe, Fussen, Didier, Geminale, Anna, Gkouvelis, Leo, Holmes, James, Hubert, Benoît, Ignatiev, Nicolay I., Kasaba, Yasumasa, Kass, David, Kleinböhl, Armin, LANCIANO, ORIETTA, Nakagawa, Hiromu, Novak, Robert E., Oliva, Fabrizio, Piccialli, Arianna, Renotte, Etienne, Ritter, Birgit, Schneider, Nick, SINDONI, Giuseppe, Thiemann, Ed, Vander Auwera, Jean, Wilquet, Valerie, WOLKENBERG, PAULINA MARIA, Yelle, Roger, ACS Science Team, Anufreychik, Konstantin, Arnold, Gabriele, Duxbury, Natalia, Fouchet, Thierry, GRASSI, Davide, Guerlet, Sandrine, Hartogh, Paul, Khatuntsev, Igor, Kokonkov, Nikita, Krasnopolsky, Vladimir, Kuzmin, Ruslan, Lacombe, Gaétan, Lellouch, Emmanuel, Määttänen, Anni, Marcq, Emmanuel, Martin-Torres, Javier, Medvedev, Alexander, Millour, Ehouarn, Moshkin, Boris, Quantin-Nataf, Cathy, Rodin, Alexander, Shematovich, Valery, Thomas, Nicolas, Trokhimovsky, Alexander, Vazquez, Luis, Vincendon, Matthieu, Young, Roland, Zasova, Ludmila, Zelenyi, Lev, Zorzano, Maria Paz, Parejo, J, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, NASA Goddard Space Flight Center (GSFC), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, 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), Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Agenzia Spaziale Italiana (ASI), Graduate School of Information Sciences [Sendai], Tohoku University [Sendai], Advanced Mechanical and Optical Systems SA (AMOS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], School of Earth Sciences [Bristol], University of Bristol [Bristol], Centre for Research in Earth and Space Science [Toronto] (CRESS), York University [Toronto], Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Department of Physics [Oxford], University of Oxford [Oxford], DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Lomonosov Moscow State University (MSU), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Institute for Astrophysics and Computational Sciences [Washington], Catholic University of America, Department of Computer Science, Electrical and Space Engineering [Luleå], Luleå University of Technology (LUT), 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), Moscow Institute of Physics and Technology [Moscow] (MIPT), Institute of Astronomy of the Russian Academy of Sciences (INASAN), University of Bern, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), 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), Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Libre de Bruxelles [Bruxelles] (ULB), The Open University [Milton Keynes] (OU), Polska Akademia Nauk (PAN), Royal Observatory of Belgium [Brussels], IMPEC - 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), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Universidad Complutense de Madrid [Madrid] (UCM), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Agence Spatiale Européenne = European Space Agency (ESA), University of Oxford, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Ministerio de Ciencia e Innovación (España), European Space Agency, Belgian Science Policy Office, European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Centre National de la Recherche Scientifique (France), and Russian Government
Subjects: Martian, Ice cloud, Multidisciplinary, 010504 meteorology & atmospheric sciences, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Storm, Atmosphere of Mars, Atmospheric sciences, 01 natural sciences, Trace gas, chemistry.chemical_compound, chemistry, 13. Climate action, Dust storm, 0103 physical sciences, Environmental science, Semiheavy water, 010303 astronomy & astrophysics, Water vapor, 0105 earth and related environmental sciences, Sciences exactes et naturelles
Abstract: A publisher correction to this article was published on 17 April 2019, Global dust storms on Mars are rare1,2 but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere3, primarily owing to solar heating of the dust3. In turn, changes in atmospheric dynamics can affect the distribution of atmospheric water vapour, with potential implications for the atmospheric photochemistry and climate on Mars4. Recent observations of the water vapour abundance in the Martian atmosphere during dust storm conditions revealed a high-altitude increase in atmospheric water vapour that was more pronounced at high northern latitudes5,6, as well as a decrease in the water column at low latitudes7,8. Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. We report the vertical distribution of the HDO/H2O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilometres. Our findings suggest that before the onset of the dust storm, HDO abundances were reduced to levels below detectability at altitudes above 40 kilometres. This decrease in HDO coincided with the presence of water-ice clouds. During the storm, an increase in the abundance of H2O and HDO was observed at altitudes between 40 and 80 kilometres. We propose that these increased abundances may be the result of warmer temperatures during the dust storm causing stronger atmospheric circulation and preventing ice cloud formation, which may confine water vapour to lower altitudes through gravitational fall and subsequent sublimation of ice crystals3. The observed changes in H2O and HDO abundance occurred within a few days during the development of the dust storm, suggesting a fast impact of dust storms on the Martian atmosphere. © 2019, The Author(s), under exclusive licence to Springer Nature Limited., This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493); by the Spanish MICINN through its Plan Nacional and by European funds under grants ESP2015-65064-C2-1-P and ESP2017-87143-R (MINECO/FEDER); by the UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, ST/S00145X/1, ST/R001367/1, ST/P001572/1 and ST/R001502/1; and the Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique - FNRS under grant number 30442502 (ET_HOME). The ACS experiment is led by IKI, Space Research Institute in Moscow, assisted by LATMOS in France. The project acknowledges funding by Roscosmos and CNES. The science operations of ACS are funded by Roscosmos and ESA. IKI affiliates acknowledge funding under grant number 14.W03.31.0017 and contract number 0120.0 602993 (0028-2014-0004) of the Russian government.
Published: 2019

97. Thermal structure and aerosol content in the martian atmosphere from ACS-TIRVIM on board ExoMars/TGO

Author: Guerlet, Sandrine, Ignatiev, Nikolay, Forget, François, Fouchet, Thierry, Shakun, Alexey, Millour, Ehouarn, Montabone, Luca, Young, Roland, Grigoriev, Alexey, Trokhimovskiy, Alexander, Montmessin, Franck, Korablev, Oleg, Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Space Science Institute [Boulder] (SSI), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), IMPEC - 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), and Guerlet, Sandrine
Subjects: [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: International audience; The ExoMars Trace Gas Orbiter (TGO), a mission by ESA and Roscosmos, was launched in March 2016 and reached its final, near-circular 400 km orbit around Mars in March, 2018. On board TGO, the Atmospheric Chemistry Suite (ACS) is a set of three spectrometers including a thermal-infrared channel, TIRVIM. This Fourier-transform spectrometer covers the range 600-6000 cm-1 (1.7-17μm) with a spectral resolution of 1.2 cm-1. We focus here on nadir observations in the range 600-1300 cm-1, which covers absorption by CO2 (centered at 667 cm-1), water ice clouds (centered at 820 cm-1) and dust (centered at 1100 cm-1). The advantage of the TIRVIM data set over previous instruments comes from the TGO orbit, which is not sun-synchronous and was designed to sample a complete daily cycle every 55 days. Hence, TIRVIM has the capacity to uniquely study both the diurnal and seasonal variability of the thermal structure, dust and ice cloud opacity. We have developed a radiative transfer model coupled to a retrieval algorithm that exploits TIRVIM spectra to simultaneously retrieve vertical profiles of the temperature from 5 to 45 km, surface temperature, and integrated optical depth of dust and water ice clouds. This algorithm was tested and validated against synthetic observations generated under various conditions (local time, seasons, latitude, aerosol load, ...). We have then applied this algorithm to the first 45 days of TIRVIM data acquired in March-April, 2018. The retrieved temperature profiles have been validated against thousands of co-located measurements acquired by the Mars Climate Sounder around 3am and 3pm, a limb-viewing radiometer onboard Mars Reconnaissance Orbiter. The agreement between the two data sets is very satisfactory. In particular, the amplitude of the diurnal thermal tide as seen by MCS is very well captured by TIRVIM at pressures greater than 10 Pa. However, TIRVIM underestimates it in the range 1-10 Pa, which is due to a much poorer vertical resolution in this region (as expected from a nadir-viewing sounder). We will present these results with an emphasis on the diurnal cycle of the atmospheric temperature and the aerosols load, along with comparisons with predictions from the LMD Mars GCM. Analysis of TIRVIM data acquired during the dust storm in June-July 2018 is in progress and will also be presented. Acknowledgements: The ACS experiment is led by IKI in Moscow. We acknowledge support by CNES and Roscosmos.
Published: 2019

98. No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations

Author: Korablev, Oleg, Avandaele, Ann Carine, Montmessin, Franck, Fedorova, Anna A., Trokhimovskiy, Alexander, Forget, François, Lefèvre, Franck, Daerden, Frank, Thomas, Ian R., Trompet, Loïc, Erwin, Justin T., Kasaba, Yasumasa, Kass, David, Khatuntsev, Igor, Kleinböhl, Armin, Kokonkov, Nikita, Krasnopolsky, Vladimir, Kuzmin, Ruslan, Lacombe, Gaétan, LANCIANO, ORIETTA, Lellouch, Emmanuel, Oliva, Fabrizio, Lewis, Stephen, Luginin, Mikhail, Liuzzi, Giuliano, López-Puertas, Manuel, López-Valverde, Miguel, Määttänen, Anni, Mahieux, Arnaud, Marcq, Emmanuel, Martin-Torres, Javier, Maslov, Igor, Patsaev, Dmitry, Medvedev, Alexander, Millour, Ehouarn, Moshkin, Boris, Mumma, Michael J., Nakagawa, Hiromu, Novak, Robert E., Piccialli, Arianna, Quantin-Nataf, Cathy, Renotte, Etienne, Ritter, Birgit, Rodin, Alexander, Schmidt, Frédéric, Schneider, Nick, Shematovich, Valery, Aoki, Shohei, Smith, Michael D., Teanby, Nicholas A., Thiemann, Ed, Thomas, Nicolas, Vander Auwera, Jean, Vazquez, Luis, Villanueva, Geronimo, Vincendon, Matthieu, Whiteway, James, Wilquet, Valérie, Robert, Séverine, Wolff, Michael J., WOLKENBERG, PAULINA MARIA, Yelle, Roger, Young, Roland, Zasova, Ludmila, Zorzano, Maria Paz, Neary, Lori, Viscardy, Sébastien, Grigoriev, Alexey V., Ignatiev, Nikolay I., Shakun, Alexey, Patrakeev, Andrey, Belyaev, Denis A., Bertaux, Jean-Loup, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Ivanov, Yuriy S., Ristic, Bojan, Mason, Jon, Willame, Yannick, Depiesse, Cédric, Hetey, Laszlo, Berkenbosch, Sophie, Clairquin, Roland, Queirolo, Claudio, Beeckman, Bram, Neefs, Eddy, Patel, Manish R., BELLUCCI, Giancarlo, López-Moreno, Jose-Juan, Wilson, Colin F., Etiope, Giuseppe, Zelenyi, Lev, Svedhem, Håkan, Vago, Jorge L., ACS Science Team, NOMAD Science Team, Alonso-Rodrigo, Gustavo, ALTIERI, FRANCESCA, Anufreychik, Konstantin, Arnold, Gabriele, Bauduin, Sophie, Bolsée, David, CARROZZO, FILIPPO GIACOMO, Clancy, R. Todd, CLOUTIS, EDWARD, Crismani, Matteo, da Pieve, Fabiana, D'AVERSA, EMILIANO, Duxbury, Natalia, Encrenaz, Therese, Fouchet, Thierry, Funke, Bernd, Fussen, Didier, Garcia-Comas, Maia, Gérard, Jean-Claude, GIURANNA, MARCO, Gkouvelis, Leo, Gonzalez-Galindo, Francisco, GRASSI, Davide, Guerlet, Sandrine, Hartogh, Paul, Holmes, James, Hubert, Benoît, Kaminski, Jacek, Karatekin, Ozgur, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), 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), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Physics [Oxford], University of Oxford [Oxford], Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), 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), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Istituto Nazionale di Geofisica e Vulcanologia - Sezione di Roma (INGV), Istituto Nazionale di Geofisica e Vulcanologia, Faculty of Environmental Science and Engineering [Cluj-Napoca], Babes-Bolyai University [Cluj-Napoca] (UBB), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Instituto Universitario de Microgravedad 'Ignacio Da Riva' (IDR), Universidad Politécnica de Madrid (UPM), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, NASA Goddard Space Flight Center (GSFC), Lomonosov Moscow State University (MSU), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Gesellschaft, Institute of Geophysics [Warsaw], Polska Akademia Nauk = Polish Academy of Sciences (PAN), Royal Observatory of Belgium [Brussels] (ROB), Graduate School of Information Sciences [Sendai], Tohoku University [Sendai], Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Institute for Astrophysics and Computational Sciences [Washington], Catholic University of America, Agenzia Spaziale Italiana (ASI), Department of Computer Science, Electrical and Space Engineering [Luleå], Luleå University of Technology (LUT), 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), Advanced Mechanical and Optical Systems SA (AMOS), Moscow Institute of Physics and Technology [Moscow] (MIPT), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Institute of Astronomy of the Russian Academy of Sciences (INASAN), School of Earth Sciences [Bristol], University of Bristol [Bristol], University of Bern, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre for Research in Earth and Space Science [Toronto] (CRESS), York University [Toronto], Lunar and Planetary Laboratory [Tucson] (LPL), University of Arizona, Belgian Science Policy Office, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Centre National de la Recherche Scientifique (France), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Russian Government, Agenzia Spaziale Italiana, European Space Agency, IMPEC - 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), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), The Open University [Milton Keynes] (OU), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Université Libre de Bruxelles [Bruxelles] (ULB), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Polska Akademia Nauk (PAN), Royal Observatory of Belgium [Brussels], Universidad Complutense de Madrid [Madrid] (UCM), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), University of Oxford, Agence Spatiale Européenne = European Space Agency (ESA), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Laboratoire de Géologie de Lyon - Terre, Planètes, Environnement (LGL-TPE), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Université Jean Monnet - Saint-Étienne (UJM)-Centre National de la Recherche Scientifique (CNRS), and 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)
Subjects: Martian, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010504 meteorology & atmospheric sciences, Chemistry, Atmosphere of Mars, Mars Exploration Program, 01 natural sciences, 7. Clean energy, Methane, Trace gas, law.invention, Astrobiology, Atmosphere, Orbiter, chemistry.chemical_compound, 13. Climate action, law, Atmospheric chemistry, 0103 physical sciences, 010303 astronomy & astrophysics, Sciences exactes et naturelles, 0105 earth and related environmental sciences
Abstract: A publisher correction to this article was published on 17 April 2019, The detection of methane on Mars has been interpreted as indicating that geochemical or biotic activities could persist on Mars today1. A number of different measurements of methane show evidence of transient, locally elevated methane concentrations and seasonal variations in background methane concentrations2–5. These measurements, however, are difficult to reconcile with our current understanding of the chemistry and physics of the Martian atmosphere6,7, which—given methane’s lifetime of several centuries—predicts an even, well mixed distribution of methane1,6,8. Here we report highly sensitive measurements of the atmosphere of Mars in an attempt to detect methane, using the ACS and NOMAD instruments onboard the ESA-Roscosmos ExoMars Trace Gas Orbiter from April to August 2018. We did not detect any methane over a range of latitudes in both hemispheres, obtaining an upper limit for methane of about 0.05 parts per billion by volume, which is 10 to 100 times lower than previously reported positive detections2,4. We suggest that reconciliation between the present findings and the background methane concentrations found in the Gale crater4 would require an unknown process that can rapidly remove or sequester methane from the lower atmosphere before it spreads globally. © 2019, The Author(s), under exclusive licence to Springer Nature Limited., ExoMars is the space mission of ESA and Roscosmos. The ACS experiment is led by IKI, the Space Research Institute in Moscow, assisted by LATMOS in France. The project acknowledges funding by Roscosmos and CNES. The science operations of ACS are funded by Roscosmos and ESA. IKI affiliates acknowledge funding under grant number 14.W03.31.0017 and contract number 0120.0 602993 (0028-2014-0004) of the Russian government. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (BIRA-IASB), assisted by co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the UK (Open University). This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with the financial and contractual coordination of the ESA Prodex Office (PEA 4000103401 and PEA 4000121493), by Spanish MICINN through its Plan Nacional and by European funds under grants ESP2015-65064-C2-1-P and ESP2017-87143-R (MINECO/FEDER), as well as by the UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, ST/S00145X/1, ST/R001367/1, ST/P001572/1 and ST/R001502/1, and the Italian Space Agency through grant 2018-2-HH.0. This work was supported by the Belgian Fonds de la Recherche Scientifique-FNRS under grant number 30442502 (ET_HOME).
Published: 2019

99. Investigation of the 2018 Global Dust Event from ACS-TIRVIM on board ExoMars/TGO

Author: Guerlet, Sandrine, Young, Roland, Ignatiev, Nikolay I., Forget, François, Millour, Ehouarn, Fouchet, Thierry, Montabone, Luca, Shakun, Alexey V., Grigoriev, Alexey, Trokhimovskiy, Alexander, Montmessin, Franck, Korablev, Oleg, and Henry, Florence
Subjects: [SDU] Sciences of the Universe [physics], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph]
Abstract: We report on the analysis of thermal infrared emission spectra recordedby ACS-TIRVIM on board the ExoMars Trace Gas Orbiter (TGO). We focus onthe period 13 March 2018 till 15 July 2018, covering quiescent and dustyconditions. From these observations, we retrieve temperature verticalprofiles from 5 to 45 km as well as integrated dust and water iceopacity at various local times. The retrieved temperature profiles arein excellent agreement with co-located observations by Mars ClimateSounder, a limb-viewing radiometer onboard Mars Reconnaissance Orbiter.The global dust event resulted in an up to 40K temperature increase inthe middle atmosphere. We will discuss these results compared to GlobalClimate Model (GCM) simulations run with MY34 dust scenario. We willalso present and discuss the atmospheric state resulting from theassimilation of TIRVIM temperature profiles into the LMD Mars GCM.
Published: 2019

100. In Situ Exploration of the Giant Planets In Situ Exploration of the Giant Planets

Author: Mousis, Olivier, Atkinson, David H., Ambrosi, Richard, Atreya, Sushil, Banfield, Don, Barabash, Stas, Blanc, Michel, Cavalié, Thibault, Coustenis, Athena, Durry, Georges, Ferri, Francesca, Fletcher, Leigh, Fouchet, Thierry, Guillot, Tristan, Hartogh, Paul, Hueso, Ricardo, Hofstadter, Mark, Lebreton, Jean-Pierre, Mandt, Kathleen, Rauer, Heike, Rannou, Pascal, Jean-Baptiste Renard, Sanchez-Lavega, Agustin, Sayanagi, Kunio, Simon, Amy A., Spilker, Thomas, Ethiraj Venkatapathy, J. Hunter Waite, and Wurz, Peter
Published: 2019
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