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1. Addendum to “Description, accessibility and usage of SOIR/Venus Express atmospheric profiles of Venus distributed in VESPA (Virtual European Solar and Planetary Access)”

Author

Trompet, L., primary, Geunes, Y., additional, Ooms, T., additional, Mahieux, A., additional, Wilquet, V., additional, Chamberlain, S., additional, Robert, S., additional, Thomas, I.R., additional, Erard, S., additional, Cecconi, B., additional, Le Sidaner, P., additional, and Vandaele, A.C., additional

Published
2024
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2. Multilayer modeling of the aureole photometry during the Venus transit: comparison between SDO/HMI and VEx/SOIR data

Author

Pere, C., Tanga, P., Widemann, Th., Bendjoya, Ph., Mahieux, A., Wilquet, V., and Vandaele, A. C.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The mesosphere of Venus is a critical range of altitudes in which complex temperature variability has been extensively studied by the space mission Venus Express (Vex) during its eight-years mission (2006-2014). Data collected at different epochs and latitudes show evidence of short and medium timescale variability as well as latitudinal differences. Spatial and temporal variability is also predicted in mesospheric and thermosphere terminator models with lower boundary conditions at 70 km near cloud tops. The Venus transit on June 5-6 2012 was the first to occur with a spacecraft in orbit around Venus. It has been shown that sunlight refraction in the mesosphere of Venus is able to provide useful constraints on mesospheric temperatures at the time of the transit. The European Space Agency's Venus Express provided space-based observations of Venus during the transit. Simultaneously, the Venus aureole photometry was observed using ground-based facilities and solar telescopes orbiting Earth (NASA Solar Dynamic Observatory, JAXA HINODE). As the properties of spatial and temporal variability of the mesosphere are still debated, the opportunity of observing it at all latitudes at the same time, offered by the transit, is rather unique. In this first paper, we establish new methods for analyzing the photometry of the so-called aureole that is produced by refraction of the solar light, and we investigate the choice of physical models that best reproduce the observations. We obtain an independent constraint of 4.8 +/- 0.5 km for the aerosol scale height in the upper haze region above 80 km. We show that a full multiple-layer approach is required to adequately reproduce the aureole photometry, which appears to be sensitive to several second-order variations in the vertical refractivity., Comment: Astronomy and Astrophysics, in press; 9 pages, 8 figures

Published
2016
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10. PLANET TOPERS: Planets, Tracing the Transfer, Origin, Preservation, and Evolution of their ReservoirS

Author

Dehant, V., Asael, D., Baland, R. M., Baludikay, B. K., Beghin, J., Belza, J., Beuthe, M., Breuer, D., Chernonozhkin, S., Claeys, Ph., Cornet, Y., Cornet, L., Coyette, A., Debaille, V., Delvigne, C., Deproost, M. H., De WInter, N., Duchemin, C., El Atrassi, F., François, C., De Keyser, J., Gillmann, C., Gloesener, E., Goderis, S., Hidaka, Y., Höning, D., Huber, M., Hublet, G., Javaux, E. J., Karatekin, Ö., Kodolanyi, J., Revilla, L. Lobo, Maes, L., Maggiolo, R., Mattielli, N., Maurice, M., McKibbin, S., Morschhauser, A., Neumann, W., Noack, L., Pham, L. B. S., Pittarello, L., Plesa, A. C., Rivoldini, A., Robert, S., Rosenblatt, P., Spohn, T., Storme, J. -Y., Tosi, N., Trinh, A., Valdes, M., Vandaele, A. C., Vanhaecke, F., Van Hoolst, T., Van Roosbroek, N., Wilquet, V., and Yseboodt, M.

Published
2016
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11. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Author

Vandaele, A. C., Lopez-Moreno, J.-J., Patel, M. R., Bellucci, G., Daerden, F., Ristic, B., Robert, S., Thomas, I. R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S., Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, B., González-Galindo, F., Geminale, A., Gérard, J.-C., Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, M., López-Valverde, M., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Willame, Y., Wolff, M., and the NOMAD Team

Published
2018
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12. The Atmospheric Chemistry Suite (ACS) of Three Spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., Martin Torres, J., Medvedev, A. S., Millour, E., Olsen, K. S., Patel, M. R., Quantin-Nataf, C., Rodin, A. V., Shematovich, V. I., Thomas, I., Thomas, N., Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C. F., Zasova, L. V., Zelenyi, L. M., and Zorzano, M. P.

Published
2017
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18. Water Vapor Vertical Profiles on Mars in Dust Storms Observed by TGO/NOMAD

Author

Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Smith, M.D., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, S., Gomez, A., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, R., Perez-grande, I., Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), and Canadian Space Agency

Subjects
010504 meteorology & atmospheric sciences, Storm, Atmosphere of Mars, Mars Exploration Program, Atmospheric sciences, 01 natural sciences, Trace gas, Atmosphere, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Dust storm, Earth and Planetary Sciences (miscellaneous), Environmental science, Hadley cell, Water vapor, 0105 earth and related environmental sciences
Abstract

It has been suggested that dust storms efficiently transport water vapor from the near-surface to the middle atmosphere on Mars. Knowledge of the water vapor vertical profile during dust storms is important to understand water escape. During Martian Year 34, two dust storms occurred on Mars: a global dust storm (June to mid-September 2018) and a regional storm (January 2019). Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). We show a significant increase of water vapor abundance in the middle atmosphere (40–100 km) during the global dust storm. The water enhancement rapidly occurs following the onset of the storm (Ls~190°) and has a peak at the most active period (Ls~200°). Water vapor reaches very high altitudes (up to 100 km) with a volume mixing ratio of ~50 ppm. The water vapor abundance in the middle atmosphere shows high values consistently at 60°S-60°N at the growth phase of the dust storm (Ls = 195°–220°), and peaks at latitudes greater than 60°S at the decay phase (Ls = 220°–260°). This is explained by the seasonal change of meridional circulation: from equinoctial Hadley circulation (two cells) to the solstitial one (a single pole-to-pole cell). We also find a conspicuous increase of water vapor density in the middle atmosphere at the period of the regional dust storm (Ls = 322–327°), in particular at latitudes greater than 60°S. ©2019. American Geophysical Union. All Rights Reserved., S. A. is >Charge de Recherches> of the F.R.S.-FNRS. ExoMars is a space mission of the European Space Agency and Roscosmos. The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASBBIRA), assisted by Co-PI teams from Spain (IAA-CSIC), Italy (INAF-IAPS), and the United Kingdom (Open University). This project acknowledges funding by the Belgian Science Policy Office, with the financial and contractual coordination by the European Space Agency Prodex Office (PEA 4000103401 and 4000121493), by the Spanish MICINN through its Plan Nacional and by European funds under grants PGC2018-101836-B-I00 and ESP2017-87143-R (MINECO/FEDER), as well as by UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, and ST/S00145X/1 and 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 numbers 30442502 (ET_HOME) and T.0171.16 (CRAMIC) and Belgian Science Policy Office BrainBe SCOOP Project. U.S. investigators were supported by the National Aeronautics and Space Administration. Canadian investigators were supported by the Canadian Space Agency. The results retrieved from the NOMAD measurements used in this article are available on the BIRA-IASB data repository: http://repository.aeronomie.be/?doi= 10.18758/71021054 (Aoki et al., 2019).

Published
2019

19. Water Vapor Vertical Profiles on Mars in Dust Storms Observed by TGO/NOMAD

Author

Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), Canadian Space Agency, Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Pérez Grande, Isabel, Ristic, Bojan, Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Smith, M.D., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Patel, Manish R., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, Samuel, Gomez, A., Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), National Aeronautics and Space Administration (US), Canadian Space Agency, Aoki, Shohei, Vandaele, Ann Carine, Daerden, Frank, Villanueva, Geronimo L., Liuzzi, Giuliano, Thomas, Ian R., Erwin, Justin T., Trompet, L., Robert, S., Neary, L., Viscardy, S., Hathi, B., Zafra, J.J., Leese, M., Maes, J., Pastor-Morales, M., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Pérez Grande, Isabel, Ristic, Bojan, Queirolo, C., Ristic, R., Gomez, J.R., Saggin, B., Smith, M.D., Samain, V., Sanz Andres, A., Altieri, F., Sanz, R., Simar, J.-F., Patel, Manish R., Thibert, T., the NOMAD team, López-Valverde, M. A., Hill, Brittany, Bellucci, Giancarlo, Bauduin, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Fussen, D., Bolsée, D., Carrozzo, G., Clancy, R. Todd, Cloutis, E., Crismani, M., Da Pieve, F., D'Aversa, E., Kaminski, J., Depiesse, C., Garcia-Comas, M., Etiope, G., Fedorova, A.A., Funke, Bernd, Geminale, A., Gérard, Jean-Claude, Giuranna, M., Karatekin, O., Gkouvelis, L., González-Galindo, F., Holmes, J., Hubert, B., Mumma, M.J., Ignatiev, N.I., Kasaba, Y., Kass, D., Kleinböhl, A., Lanciano, O., Lefèvre, F., Lewis, S., López-Puertas, M., Schneider, Nicholas, Nakagawa, H., Hidalgo López, Ana, Mahieux, A., Mason, J., Mege, D., Neefs, E., Novak, R.E., Oliva, F., Sindoni, G., Piccialli, A., Renotte, E., Ritter, B., Willame, Y., Schmidt, F., Teanby, N.A., Thiemann, E., Trokhimovskiy, A., Auwera, J.V., Wolff, M.J., Clairquin, R., Whiteway, J., Wilquet, V., Wolkenberg, P., Yelle, R., del Moral Beatriz, A., Barzin, P., Beeckman, B., Cubas, J., BenMoussa, A., Berkenbosch, S., Orban, A., Biondi, D., Bonnewijn, S., Candini, G.P., Giordanengo, B., Gissot, Samuel, and Gomez, A.

Abstract

It has been suggested that dust storms efficiently transport water vapor from the near-surface to the middle atmosphere on Mars. Knowledge of the water vapor vertical profile during dust storms is important to understand water escape. During Martian Year 34, two dust storms occurred on Mars: a global dust storm (June to mid-September 2018) and a regional storm (January 2019). Here we present water vapor vertical profiles in the periods of the two dust storms (Ls = 162–260° and Ls = 298–345°) from the solar occultation measurements by Nadir and Occultation for Mars Discovery (NOMAD) onboard ExoMars Trace Gas Orbiter (TGO). We show a significant increase of water vapor abundance in the middle atmosphere (40–100 km) during the global dust storm. The water enhancement rapidly occurs following the onset of the storm (Ls~190°) and has a peak at the most active period (Ls~200°). Water vapor reaches very high altitudes (up to 100 km) with a volume mixing ratio of ~50 ppm. The water vapor abundance in the middle atmosphere shows high values consistently at 60°S-60°N at the growth phase of the dust storm (Ls = 195°–220°), and peaks at latitudes greater than 60°S at the decay phase (Ls = 220°–260°). This is explained by the seasonal change of meridional circulation: from equinoctial Hadley circulation (two cells) to the solstitial one (a single pole-to-pole cell). We also find a conspicuous increase of water vapor density in the middle atmosphere at the period of the regional dust storm (Ls = 322–327°), in particular at latitudes greater than 60°S. ©2019. American Geophysical Union. All Rights Reserved.

Published
2019

21. The Atmospheric Chemistry Suite (ACS) of three spectrometers for the ExoMars 2016 Trace Gas Orbiter

Author

Korablev, O., Montmessin, F., Trokhimovskiy, A., Fedorova, A. A., Shakun, A. V., Grigoriev, A. V., Moshkin, B. E., Ignatiev, N. I., Forget, F., Lefèvre, F., Anufreychik, K., Dzuban, I., Ivanov, Y. S., Kalinnikov, Y. K., Kozlova, T. O., Kungurov, A., Makarov, V., Martynovich, F., Maslov, I., Merzlyakov, D., Moiseev, P. P., Nikolskiy, Y., Patrakeev, A., Patsaev, D., Santos-Skripko, A., Sazonov, O., Semena, N., Semenov, A., Shashkin, V., Sidorov, A., Stepanov, A. V., Stupin, I., Timonin, D., Titov, A. Y., Viktorov, A., Zharkov, A., Altieri, F., Arnold, G., Belyaev, D. A., Bertaux, J. L., Betsis, D. S., Duxbury, N., Encrenaz, T., Fouchet, T., Gérard, J.-C., Grassi, D., Guerlet, S., Hartogh, P., Kasaba, Y., Khatuntsev, I., Krasnopolsky, V. A., Kuzmin, R. O., Lellouch, E., Lopez-Valverde, M. A., Luginin, M., Määttänen, A., Marcq, E., Martin Torres, J., Medvedev, A. S., Millour, E., Olsen, K. S., Patel, M. R., Quantin-Nataf, C., Rodin, A. V., Shematovich, V. I., Thomas, I., Thomas, N., Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C. F., Zasova, L. V., Zelenyi, L. M., Zorzano, M. P., Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), IMPEC - 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 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)-École normale supérieure - Paris (ENS Paris), Main Astronomical Observatory of NAS of Ukraine (MAO), National Academy of Sciences of Ukraine (NASU), National Research Institute for Physical-technical and Radiotechnical Measurements (VNIIFTRI), Scientific Production Enterprise Astron Electronics, Faculty of Physics [MSU, Moscow], Lomonosov Moscow State University (MSU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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, Tohoku University [Sendai], Moscow Institute of Physics and Technology [Moscow] (MIPT), Catholic University of America, Vernadsky Institute of Geochemistry and Analytical Chemistry (GEOKHI), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Department of Computer Science [Kiruna], Luleå University of Technology (LUT), Instituto Andaluz de Ciencias de la Tierra (IACT), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universidad de Granada (UGR), The Open University [Milton Keynes] (OU), 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), Institute of Astronomy of the Russian Academy of Sciences (INASAN), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Universität Bern [Bern], Facultad de Informática [Madrid], Universidad Complutense de 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), Department of Physics [Oxford], University of Oxford [Oxford], Centro de Astrobiologia [Madrid] (CAB), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), PLANETO - 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), 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), 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), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada (UGR), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), 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), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universidad de Granada = University of Granada (UGR), 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), Universität Bern [Bern] (UNIBE), 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), University of Oxford, and Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)

Subjects
Cross-dispersion, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Atmosphere, 520 Astronomy, Mars, Echelle, Fourier-spectrometer, 620 Engineering, High-resolution spectrometer, [PHYS.PHYS.PHYS-SPACE-PH]Physics [physics]/Physics [physics]/Space Physics [physics.space-ph]
Abstract

International audience; The Atmospheric Chemistry Suite (ACS) package is an element of the Russian contribution to the ESA-Roscosmos ExoMars 2016 Trace Gas Orbiter (TGO) mission. ACS consists of three separate infrared spectrometers, sharing common mechanical, electrical, and thermal interfaces. This ensemble of spectrometers has been designed and developed in response to the Trace Gas Orbiter mission objectives that specifically address the requirement of high sensitivity instruments to enable the unambiguous detection of trace gases of potential geophysical or biological interest. For this reason, ACS embarks a set of instruments achieving simultaneously very high accuracy (ppt level), very high resolving power (>10,000) and large spectral coverage (0.7 to 17 μm—the visible to thermal infrared range). The near-infrared (NIR) channel is a versatile spectrometer covering the 0.7–1.6 μm spectral range with a resolving power of ∼20,000. NIR employs the combination of an echelle grating with an AOTF (Acousto-Optical Tunable Filter) as diffraction order selector. This channel will be mainly operated in solar occultation and nadir, and can also perform limb observations. The scientific goals of NIR are the measurements of water vapor, aerosols, and dayside or night side airglows. The mid-infrared (MIR) channel is a cross-dispersion echelle instrument dedicated to solar occultation measurements in the 2.2–4.4 μm range. MIR achieves a resolving power of >50,000. It has been designed to accomplish the most sensitive measurements ever of the trace gases present in the Martian atmosphere. The thermal-infrared channel (TIRVIM) is a 2-inch double pendulum Fourier-transform spectrometer encompassing the spectral range of 1.7–17 μm with apodized resolution varying from 0.2 to 1.3 cm−1. TIRVIM is primarily dedicated to profiling temperature from the surface up to ∼60 km and to monitor aerosol abundance in nadir. TIRVIM also has a limb and solar occultation capability. The technical concept of the instrument, its accommodation on the spacecraft, the optical designs as well as some of the calibrations, and the expected performances for its three channels are described.

Published
2018

22. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Author

Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Vandaele, Ann Carine, López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Daerden, Frank, Ristic, Bojan, Robert, S., Thomas, Ian R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, Bernd, González-Galindo, F., Geminale, A., Gérard, Jean-Claude, Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wolff, Michael T., Patel, M., D’aversa, E., Fussen, D., García Comas, Maia, Hewson, W., McConnel, J., Novak, R., Oliva, F., Piccialli, A., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G. P., Clairquin, R., Cubas, J., De-Lanoye, S., Giordanengo, B., Gissot, Samuel, Gomez, A., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Pérez Grande, Isabel, Queirolo, C., Saggin, B., Samain, V., Sanz Andres, A., Sanz Mesa, Rosario, Simar, J.-F., Thibert, T., Jerónimo, José María, The NOMAD Team, Belgian Science Policy Office, European Space Agency, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Agenzia Spaziale Italiana, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Vandaele, Ann Carine, López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Daerden, Frank, Ristic, Bojan, Robert, S., Thomas, Ian R., Wilquet, V., Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Depiesse, C., Drummond, R., Fedorova, A., Formisano, V., Funke, Bernd, González-Galindo, F., Geminale, A., Gérard, Jean-Claude, Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Renotte, E., Rodriguez-Gomez, J., Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wolff, Michael T., Patel, M., D’aversa, E., Fussen, D., García Comas, Maia, Hewson, W., McConnel, J., Novak, R., Oliva, F., Piccialli, A., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G. P., Clairquin, R., Cubas, J., De-Lanoye, S., Giordanengo, B., Gissot, Samuel, Gomez, A., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Pérez Grande, Isabel, Queirolo, C., Saggin, B., Samain, V., Sanz Andres, A., Sanz Mesa, Rosario, Simar, J.-F., Thibert, T., Jerónimo, José María, and The NOMAD Team

Abstract

The NOMAD (“Nadir and Occultation for MArs Discovery”) spectrometer suite on board the ExoMars Trace Gas Orbiter (TGO) has been designed to investigate the composition of Mars’ atmosphere, with a particular focus on trace gases, clouds and dust. The detection sensitivity for trace gases is considerably improved compared to previous Mars missions, compliant with the science objectives of the TGO mission. This will allow for a major leap in our knowledge and understanding of the Martian atmospheric composition and the related physical and chemical processes. The instrument is a combination of three spectrometers, covering a spectral range from the UV to the mid-IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and explain the technical principles of the three spectrometers. We also discuss the expected performance of the instrument in terms of spatial and temporal coverage and detection sensitivity.© 2018, The Author(s).

Published
2018

23. Description, accessibility and usage of SOIR/Venus Express atmospheric profiles of Venus distributed in VESPA (Virtual European Solar and Planetary Access)

Author

Trompet, L., primary, Geunes, Y., additional, Ooms, T., additional, Mahieux, A., additional, Wilquet, V., additional, Chamberlain, S., additional, Robert, S., additional, Thomas, I.R., additional, Erard, S., additional, Cecconi, B., additional, Le Sidaner, P., additional, and Vandaele, A.C., additional

Published
2018
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24. Expected performances of the NOMAD/ExoMars instrument

Author

Robert, S, Vandaele, A. C., Thomas, I., Willame, Y., Daerden, F., Delanoye, S., Depiesse, C., Drummond, R., Neefs, E., Neary, L., Ristic, B., Mason, J., Lopez Moreno, J. J., Rodriguez Gomez, J., Patel, M. R., Bellucci, G., Patel, M., Allen, M., Altieri, F., Aoki, S., Bolsée, D., Clancy, T., Cloutis, E., Fedorova, A., Formisano, V., Funke, B., Fussen, D., Garcia Comas, M., Geminale, A., Gérard, J. C., Gillotay, D., Giuranna, M., Gonzalez Galindo, F., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Lefèvre, F., Lewis, S., López Puertas, M., López Valverde, M., Mahieux, A., Mcconnell, J., Mumma, M., Novak, R., Renotte, E., Robert, S., Sindoni, G., Smith, M., Thomas, I. R., Trokhimovskiy, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Wilquet, V., Wolff, M., Alonso Rodrigo, G., Aparicio Del Moral, B., Barzin, P., Ben Moussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G., Clairquin, R., Cubas, J., Giordanengo, B., Gissot, S., Gomez, A., Zafra, J. J., Leese, M., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, R., Orban, A., Pastor Morales, M., Perez Grande, I., Saggin, Bortolino, Samain, V., Sanz Andres, A., Sanz, R., Simar, J. F., Thibert, T., UK Space Agency, Belgian Science Policy Office, European Commission, and European Space Agency

Subjects
ExoMars ESA mission, 010504 meteorology & atmospheric sciences, Mars, NOMAD instrument, 01 natural sciences, Occultation, law.invention, Orbiter, law, 0103 physical sciences, Nadir, Radiative transfer, Abundances, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing, atmosphere [Mars], Spectrometer, Mars, atmosphere, Astronomy and Astrophysics, Space and Planetary Science, Astronomy, Mars Exploration Program, Atmosphere of Mars, Trace gas, 13. Climate action, atmosphere, Mars: atmosphere, Environmental science
Abstract

NOMAD (Nadir and Occultation for MArs Discovery) is one of the four instruments on board the ExoMars Trace Gas Orbiter, scheduled for launch in March 2016. It consists of a suite of three high-resolution spectrometers - SO (Solar Occultation), LNO (Limb, Nadir and Occultation) and UVIS (Ultraviolet and Visible Spectrometer). Based upon the characteristics of the channels and the values of Signal-to-Noise Ratio obtained from radiometric models discussed in (Vandaele et al., 2015a, 2015b; Thomas et al., 2016), the expected performances of the instrument in terms of sensitivity to detection have been investigated. The analysis led to the determination of detection limits for 18 molecules, namely CO, HO, HDO, CH, CH, CH, HCO, CH, SO, HS, HCl, HCN, HO, NH, NO, NO, OCS, O. NOMAD should have the ability to measure methane concentrations, NOMAD has been made possible thanks to funding by the Belgian Science Policy Office (BELSPO) and financial and contractual coordination by the ESA Prodex Office (PlanetADAM no 4000107727). The research was performed as part of the >Inter-university Attraction Poles> programme financed by the Belgian Government (Planet TOPERS no P7-15) and a BRAIN Research Grant BR/143/A2/SCOOP. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under Grant Agreement no. 607177 CrossDrive. UK funding is acknowledged under the UK Space Agency Grant ST/I003061/1.

Published
2016

25. Optical and radiometric models of the NOMAD instrument part II: The infrared channels - SO and LNO

Author

Thomas, I. R., Vandaele, A. C., Robert, S., Neefs, E., Drummond, R., Daerden, F., Delanoye, S., Ristic, B., Berkenbosch, S., Clairquin, R., Maes, J., Bonnewijn, S., Depiesse, C., Mahieux, A., Trompet, L., Neary, L., Willame, Y., Wilquet, V., Nevejans, D., Aballea, L., Moelans, W., De Vos, L., Lesschaeve, S., Van Vooren, N., Lopez Moreno, J. J., Patel, M. R., Bellucci, G., Vandaele, Ann Carine, Moreno, Lopez, Juan, Jose, Bellucci, Giancarlo, Patel, Manish, Allen, Mark, Altieri, Francesca, Aoki, Shohei, Bolsée, David, Clancy, Todd, Cloutis, Edward, Daerden, Frank, Depiesse, Cédric, Fedorova, Anna, Formisano, Vittorio, Funke, Bernd, Fussen, Didier, Garcia Comas, Maya, Geminale, Anna, Gérard, Jean Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez Galindo, Francisco, Ignatiev, Nicolai, Kaminski, Jacek, Karatekin, Ozgur, Kasaba, Yasumasa, Lefèvre, Franck, Lewis, Stephen, López Puertas, Manuel, López Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mcconnell, Jack, Mumma, Mike, Neary, Lori, Neefs, Eddy, Novak, Robert, Renotte, Etienne, Robert, Séverine, Sindoni, Giuseppe, Smith, Mike, Thomas, Ian R., Trokhimovsky, Sacha, Vander Auwera, Jean, Villanueva, Geronimo, Whiteway, Jim, Willame, Yannick, Wilquet, Valerie, Wolff, Mike, Alonso Rodrigo, Gustavo, Aparicio Del Moral, Beatriz, Barzin, Pascal, Benmoussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, Sabrina, Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Delanoye, Sofie, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Zafra, Jose Jeronimo, Leese, Mark, Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, Jose, Morales, Rafael, Orban, Anne, Del Carmen Pastor Morales, Maria, Perez Grande, Isabel, Ristic, Bojan, Rodriguez Gomez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan Felipe, Thibert, Tanguy, Belgian Science Policy Office, European Space Agency, and UK Space Agency

Subjects
Physics, Martian, 010504 meteorology & atmospheric sciences, Spectrometer, Atmospheric composition, Spectrometers and spectroscopic instrumentation, 01 natural sciences, Occultation, Atomic and Molecular Physics, and Optics, Trace gas, law.invention, Remote sensing and sensors, Orbiter, Space instrumentation, Atmosphere of Earth, law, Atomic and Molecular Physics, Martian surface, 0103 physical sciences, Nadir, Radiative transfer, and Optics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Remote sensing
Abstract

NOMAD is a suite of three spectrometers that will be launched in 2016 as part of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument contains three channels that cover the IR and UV spectral ranges and can perform solar occultation, nadir and limb observations, to detect and map a wide variety of Martian atmospheric gases and trace species. Part I of this work described the models of the UVIS channel; in this second part, we present the optical models representing the two IR channels, SO (Solar Occultation) and LNO (Limb, Nadir and Occultation), and use them to determine signal to noise ratios (SNRs) for many expected observational cases. In solar occultation mode, both the SO and LNO channel exhibit very high SNRs >5000. SNRs of around 100 were found for the LNO channel in nadir mode, depending on the atmospheric conditions, Martian surface properties, and observation geometry., NOMAD has been made possible thanks to funding by the Belgian Science Policy Office (BELSPO) and financial and contractual coordination by the ESA Prodex Office. The research was performed as part of the “Interuniversity Attraction Poles” programme financed by the Belgian government (Planet TOPERS). UK funding is acknowledged under the UK Space Agency grant ST/I003061/1.

Published
2016

26. Optical and radiometric models of the NOMAD instrument part I: the UVIS channel

Author

Vandaele, Ann C., Willame, Yannick, Depiesse, Cédric, Thomas, Ian R., Robert, Séverine, Bolsée, David, Patel, Manish R., Mason, Jon P., Leese, Mark, Lesschaeve, Stefan, Antoine, Philippe, Daerden, Frank, Delanoye, Sofie, Drummond, Rachel, Neefs, Eddy, Ristic, Bojan, Lopez Moreno, José Juan, Bellucci, Giancarlo, Allen, M., Altieri, F., Aoki, S., Clancy, T., Cloutis, E., Fedorova, A., Formisano, V., Funke, B., Fussen, D., Garcia Comas, M., Geminale, A., Gérard, J. C., Gillotay, D., Giuranna, M., Gonzalez Galindo, F., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Lefèvre, F., Lewis, S., López Puertas, M., López Valverde, M., Mahieux, A., Mumma, M., Neary, L., Novak, R., Renotte, E., Sindoni, G., Smith, M., Trokhimovskiy, A., Vander Auwera, J., Villanueva, G., Viscardy, S., Whiteway, J., Wilquet, V., Wolff, M., Alonso Rodrigo, G., Aparicio Del Moral, B., Barzin, P., Benmoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G., Clairquin, R., Cubas, J., Giordanengo, B., Gissot, S., Gomez, A., Zafra, J. J., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, R., Orban, A., Pastor Morales, M., Perez Grande, I., Rodriguez Gomez, J., Saggin, Bortolino, Samain, V., Sanz Andres, A., Sanz, R., Simar, J. F., Thibert, T., European Space Agency, UK Space Agency, and Belgian Science Policy Office

Subjects
Solar occultation, Radiometric model, Occultation, Signal, law.invention, Orbiter, Optics, law, Atomic and Molecular Physics, Nadir, Optical constants, Science objectives, Remote sensing, Physics, Martian, business.industry, Signal to noise, Atmosphere of Mars, IR spectral range, Atomic and Molecular Physics, and Optics, Trace gas, Wavelength, Optical models, Atmospheric absorption, and Optics, business, Martian atmospheres
Abstract

The NOMAD instrument has been designed to best fulfil the science objectives of the ExoMars Trace Gas Orbiter mission that will be launched in 2016. The instrument is a combination of three channels that cover the UV, visible and IR spectral ranges and can perform solar occultation, nadir and limb observations. In this series of two papers, we present the optical models representing the three channels of the instrument and use them to determine signal to noise levels for different observation modes and Martian conditions. In this first part, we focus on the UVIS channel, which will sound the Martian atmosphere using nadir and solar occultation viewing modes, covering the 200-650nm spectral range. High SNR levels (, NOMAD has been made possible thanks to funding by the Belgian Science Policy Office (BELSPO) and financial and contractual coordination by the ESA Prodex Office (contracts no 4000107727 and 4000103401). The research was performed as part of the >Interuniversity Attraction Poles> programme financed by the Belgian government (Planet TOPERS, contract PAI no P7/15). UK funding is acknowledged under the UK Space Agency grant ST/I003061/1.

Published
2015

27. A compilation of all CO observations performed by SOIR during the Venus Express mission

Author

Vandaele, A.C., Mahieux, A., Chamberlain, S., Ristic, B., Robert, S., Thomas, I. R., Trompet, L., Wilquet, V., Bertaux, Jean-Loup, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), 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), and Cardon, Catherine

Subjects
[SDU.ASTR.IM] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.SR] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract

International audience; The SOIR instrument on board the ESA Venus Express spacecraft has been operational during the complete duration of the mission, from April 2006 up to November 2014. Spectra are recorded in the IR spectral region (2.2 -4.3 m) using the solar occultation geometry and give access to a vast number of ro-vibrational lines and bands of several key species of the atmosphere of Venus. Here we present the complete set of vertical profiles of carbon monoxide (CO) densities and volume mixing ratios (vmr) obtained during the mission. These profiles are spanning the 65-150 km altitude range. We discuss the variability which is observed on short term, but also the long term trend as well as variation of CO with solar local time (LST) and latitude.

Published
2015

28. The Clouds of Venus – an overview of Venus Express results

Author

Wilson, C. F., Marcq, Emmanuel, Markiewicz, W.J., Montmessin, Franck, Fedorova, A., Wilquet, V., Petrova, E.V., Ignatiev, N.I., Shalygina, O.S., Määttänen, Anni, McGouldrick, K.M., Hashimoto, G.L., Imamura, T., Rossi, Loïc, Luginin, M., Oschlisniok, J., Haus, R., Parkinson, C.D., Titov, D.V., Esposito, L. W., Limaye, Sanjay S., Vandaele, A.-C., Zasova, Liudmila V., Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), University of Oxford [Oxford], IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Max-Planck-Institut für Sonnensystemforschung ( MPS ), 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 ), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] ( IGEP ), Technische Universität Braunschweig [Braunschweig], Laboratory for Atmospheric and Space Physics [Boulder] ( LASP ), University of Colorado Boulder [Boulder], Okoyama University, Institute of Space and Astronautical Science ( ISAS ), Rhenish Institute for Environmental Research ( RIU ), University of Cologne, Westfälische Wilhelms-Universität Münster ( WWU ), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), University of Michigan [Ann Arbor], European Space Research and Technology Centre ( ESTEC ), European Space Agency ( ESA ), Space Science and Engineering Center [Madison] ( SSEC ), University of Wisconsin-Madison [Madison], Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, 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), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, 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), Institut für Geophysik und Extraterrestrische Physik [Braunschweig] (IGEP), Technische Universität Braunschweig = Technical University of Braunschweig [Braunschweig], Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Okayama University, Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Rhenish Institute for Environmental Research (RIU), Westfälische Wilhelms-Universität Münster = University of Münster (WWU), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan System-University of Michigan System, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), Space Science and Engineering Center [Madison] (SSEC), University of Wisconsin-Madison, Max-Planck-Institut für Sonnensystemforschung (MPS), Westfälische Wilhelms-Universität Münster (WWU), and European Space Agency (ESA)

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; Venus is completely enveloped by clouds. The main cloud layers stretch from altitudes of 48 – 75 km, with additional tenuous hazes found at altitudes 30 – 100 km. Clouds play a crucial role in governing atmospheric circulation, chemistry and climate on all planets, but particularly so on Venus due to the optical thickness of the atmosphere. The European Space Agency’s Venus Express (VEx) satellite has carried out a wealth of observations of Venus clouds since its arrival at Venus in April 2006. Many VEx observations are relevant to cloud science – from imagers and spectrometers to solar, stellar and radio occultation – each covering different altitude ranges, spectral ranges and atmospheric constituents.We have formed an International Team at the International Space Science Institute to bring together scientists from each of the relevant Venus Express investigation teams as well as from previous missions, as well as those developing computational and analytical models of clouds and hazes. The aims of the project are (1) to perform intercomparisons of cloud parameters measured using different techniques, (1) to create self-consistent reference cloud/haze models which capture not only a mean cloud structure but also its main modes of variability; and (2) to bring together modelers and observers, to reach an understanding of clouds and hazes on Venus which matches all observables and is physically consistent.This talk will present an overview of Venus Express cloud observations of all different types, and discuss progress towards a new reference cloud model to be submitted to an update of the Venus International Reference Atmosphere.

Published
2015

30. Sulfur Dioxide variability in the Venus atmosphere

Author

Vandaele, A. C., Korablev, O., Mahieux, A., Wilquet, V., Chamberlain, S., Belyaev, Denis, Encrenaz, Thérèse, Esposito, L., Jessup, K.L., Lefèvre, Franck, Limaye, S., Marcq, Emmanuel, Mils, F., Parkinson, C., Sandor, B., Stolzenbach, Aurélien, Wilson, C., 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), 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), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], Southwest Research Institute [Boulder] (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), Department of Atmospheric Oceanic and Space Sciences [Madison], University of Wisconsin-Madison, Space Science Institute [Boulder] (SSI), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] (AOSS), University of Michigan [Ann Arbor], University of Michigan System-University of Michigan System, Clarendon Laboratory [Oxford], University of Oxford [Oxford], Space Science and Engineering Center [Madison] (SSEC), Australian National University (ANU), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, 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 ), 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 Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratory for Atmospheric and Space Physics [Boulder] ( LASP ), University of Colorado Boulder [Boulder], Southwest Research Institute [Boulder] ( SwRI ), IMPEC - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales ( LATMOS ), Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Space Science and Engineering Center [Madison] ( SSEC ), University of Wisconsin-Madison [Madison], Australian National University ( ANU ), Department of Atmospheric, Oceanic, and Space Sciences [Ann Arbor] ( AOSS ), and Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP )

Subjects
[SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, Atmosphere, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Sulfur Dioxide, Variability, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Venus
Abstract

International audience; Recent observations of sulfur oxides (SO2, SO, OCS, and H2SO4) in Venus’ mesosphere have generated controversy and great interest in the scientific community. These observations revealed unexpected spatial patterns and spatial/temporal variability that have not been satisfactorily explained by models. Particularly intriguing are the layer of enhanced gas- phase SO2 and SO in the upper mesosphere, and variability in the maximum observed SO2 abundance and the equator-to-pole SO2 abundance gradient, seemingly on multi-year cycles, that is not uniquely linked to local time variations. Sulfur oxide chemistry on Venus is closely linked to the global- scale cloud and haze layers, which are composed primarily of concentrated sulfuric acid. Consequently, sulfur oxide observations provide important insight into the ongoing chemical evolution of Venus’ atmosphere, atmospheric dynamics, and possible volcanism.Existing observations have been obtained using multiple platforms, observing techniques, and wavelengths. Each has its own unique strengths and limitations. Although there is strong agreement on some features, there are significant unresolved apparent disagreements among current observations and between observations and models. These apparent disagreements need to be analyzed and assessed carefully to synthesize a clear understanding of sulfur oxide chemistry on Venus. These investigations have been performed via 1) the comparison and validation of observations, from past missions, Venus Express, Earth-based telescopes, and the Earth-orbiting Hubble Space Telescope; and 2) modelling of the SO2 and sulfur-oxide family photochemistry. The current study has been carried out within the frame of the ISSI International Team entitled ‘SO2 variability in the Venus atmosphere’.

Published
2015

31. Science objectives and performances of NOMAD, a spectrometer suite for the ExoMars TGO mission

Author

Vandaele, A. C, Neefs, E., Drummond, R., Thomas, I. R., Daerden, F., Lopez Moreno, J. J., Rodriguez, J., Patel, M. R., Bellucci, G., Allen, M., Altieri, F., Bolsée, D., Clancy, T., Delanoye, S., Depiesse, C., Cloutis, E., Fedorova, A., Formisano, V., Funke, B., Fussen, D., Geminale, A., Gérard, J. C., Giuranna, M., Ignatiev, N., Kaminski, J., Karatekin, O., Lefèvre, F., López Puertas, M., López Valverde, M., Mahieux, A., Mcconnell, J., Mumma, M., Neary, L., Renotte, E., Ristic, B., Robert, S., Smith, M., Trokhimovsky, S., Vanderauwera, J., Villanueva, G., Whiteway, J., Wilquet, V., Wolff, M., Vandaele, Ann Carine, Lopez Moreno, Jose Juan, Bellucci, Giancarlo, Patel, Manish, Allen, Mark, Altieri, Francesca, Aoki, Shohei, Bolsée, David, Clancy, Todd, Cloutis, Edward, Daerden, Frank, Depiesse, Cédric, Fedorova, Anna, Formisano, Vittorio, Funke, Bernd, Fussen, Didier, Garcia Comas, Maya, Geminale, Anna, Gérard, Jean Claude, Gillotay, Didier, Giuranna, Marco, Gonzalez Galindo, Francisco, Ignatiev, Nicolai, Kaminski, Jacek, Karatekin, Ozgur, Kasabe, Yasumasa, Lefèvre, Franck, Lewis, Stephen, López Puertas, Manuel, López Valverde, Miguel, Mahieux, Arnaud, Mason, Jon, Mumma, Mike, Neary, Lori, Neefs, Eddy, Renotte, Etienne, Robert, Séverine, Sindoni, Giuseppe, Smith, Mike, Thomas, Ian R., Trokhimovsky, Sacha, Vander Auwera, Jean, Villanueva, Geronimo, Whiteway, Jim, Willame, Yannick, Wilquet, Valerie, Wolff, Mike, Alonso Rodrigo, Gustavo, Aparicio Del Moral, Beatriz, Barzin, Pascal, Ben Moussa, Ali, Berkenbosch, Sophie, Biondi, David, Bonnewijn, Sabrina, Candini, Gian Paolo, Clairquin, Roland, Cubas, Javier, Delanoye, Sofie, Giordanengo, Boris, Gissot, Samuel, Gomez, Alejandro, Zafra, Jose Jeronimo, Leese, Mark, Maes, Jeroen, Mazy, Emmanuel, Mazzoli, Alexandra, Meseguer, Jose, Morales, Rafael, Orban, Anne, Pastor Morales, Maria Del Carmen, Perez Grande, Isabel, Ristic, Bojan, Rodriguez Gomez, Julio, Saggin, Bortolino, Samain, Valérie, Sanz Andres, Angel, Sanz, Rosario, Simar, Juan Felipe, Thibert, Tanguy, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), The Open University [Milton Keynes] (OU), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Science Institute [Boulder] (SSI), Department of Geography [Winnipeg], University of Winnipeg, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, York University [Toronto], Royal Observatory of Belgium [Brussels] (ROB), 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), NASA Goddard Space Flight Center (GSFC), Centre Spatial de Liège (CSL), Spectroscopie de l'atmosphère, Service de Chimie Quantique et Photophysique, Université libre de Bruxelles (ULB), and Catholic University of America

Subjects
[SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Solar, Occultation, law.invention, Orbiter, Mars atmosphere, law, Nadir, Aerosol, Observations, Spectroscopy, Ultraviolet, Remote sensing, Spectrometer, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Suite, Astronomy and Astrophysics, Mars Exploration Program, Atmosphere of Mars, ExoMars, Trace gas, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, Visible, Composition, Infrared, Methane, Occultation Nadir, Environmental science
Abstract

International audience; The NOMAD spectrometer suite on the ExoMars Trace Gas Orbiter will map the composition and distribution of Mars' atmospheric trace species in unprecedented detail, fulfilling many of the scientific objectives of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument is a combination of three channels, covering a spectral range from the UV to the IR, and can perform solar occultation, nadir and limb observations. In this paper, we present the science objectives of the instrument and how these objectives have influenced the design of the channels. We also discuss the expected performance of the instrument in terms of coverage and detection sensitivity.

Published
2015

32. Venus Express 太陽掩蔽観測による金星上部もや層の研究

Author

Mahieux, A., Robert, S., Wilquet, V., Drummond, R., Vandaele, A.C., Takagi, Seiko, and Iwagami, Naomoto

Abstract

第28回大気圏シンポジウム（2014年12月8日-9日. 宇宙航空研究開発機構宇宙科学研究所（JAXA)(ISAS)）, 相模原市, 神奈川県, 28th Atmospheric Science Symposium (December 8-9, 2014. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS)), Sagamihara, Kanagawa Japan, 資料番号: SA6000069017, レポート番号: Ⅱ-11

Published
2014

33. Expected performances of the NOMAD/ExoMars instrument

Author

UK Space Agency, Belgian Science Policy Office, European Commission, European Space Agency, Vandaele, Ann Carine, López-Moreno, José Juan, Bellucci, Giancarlo, Patel, M., Allen, M., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Daerden, Frank, Depiesse, C., Fedorova, A., Formisano, V., Funke, Bernd, Fussen, D., García Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, D., Giuranna, M., González-Galindo, F., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Lefèvre, F., Lewis, S., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Novak, R., Renotte, E., Robert, S., Sindoni, G., Smith, M., Thomas, Ian R., Trokhimovskiy, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wilquet, V., Wolff, Michael T., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G., Clairquin, R., Cubas, J., Delanoye, S., Giordanengo, B., Gissot, Samuel, Gomez, A., Zafra, J.-J., Leese, M., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Pérez Grande, Isabel, Ristic, Bojan, Rodríguez Gómez, Julio, Saggin, B., Samain, V., Sanz Andres, A., Sanz, R., Simar, J.-F., Thibert, T., Alonso-Rodrigo, G., UK Space Agency, Belgian Science Policy Office, European Commission, European Space Agency, Vandaele, Ann Carine, López-Moreno, José Juan, Bellucci, Giancarlo, Patel, M., Allen, M., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Daerden, Frank, Depiesse, C., Fedorova, A., Formisano, V., Funke, Bernd, Fussen, D., García Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, D., Giuranna, M., González-Galindo, F., Ignatiev, N., Kaminski, J., Karatekin, O., Kasaba, Y., Lefèvre, F., Lewis, S., López-Puertas, Manuel, López-Valverde, M. A., Mahieux, A., Mason, J., McConnell, J., Mumma, M., Neary, L., Neefs, E., Novak, R., Renotte, E., Robert, S., Sindoni, G., Smith, M., Thomas, Ian R., Trokhimovskiy, A., Vander Auwera, J., Villanueva, Geronimo L., Viscardy, S., Whiteway, J., Willame, Y., Wilquet, V., Wolff, Michael T., Aparicio del Moral, Beatriz, Barzin, P., BenMoussa, A., Berkenbosch, S., Biondi, D., Bonnewijn, S., Candini, G., Clairquin, R., Cubas, J., Delanoye, S., Giordanengo, B., Gissot, Samuel, Gomez, A., Zafra, J.-J., Leese, M., Maes, J., Mazy, E., Mazzoli, A., Meseguer, J., Morales, Rafael, Orban, A., Pastor, Carmen, Pérez Grande, Isabel, Ristic, Bojan, Rodríguez Gómez, Julio, Saggin, B., Samain, V., Sanz Andres, A., Sanz, R., Simar, J.-F., Thibert, T., and Alonso-Rodrigo, G.

Abstract

NOMAD (Nadir and Occultation for MArs Discovery) is one of the four instruments on board the ExoMars Trace Gas Orbiter, scheduled for launch in March 2016. It consists of a suite of three high-resolution spectrometers - SO (Solar Occultation), LNO (Limb, Nadir and Occultation) and UVIS (Ultraviolet and Visible Spectrometer). Based upon the characteristics of the channels and the values of Signal-to-Noise Ratio obtained from radiometric models discussed in (Vandaele et al., 2015a, 2015b; Thomas et al., 2016), the expected performances of the instrument in terms of sensitivity to detection have been investigated. The analysis led to the determination of detection limits for 18 molecules, namely CO, HO, HDO, CH, CH, CH, HCO, CH, SO, HS, HCl, HCN, HO, NH, NO, NO, OCS, O. NOMAD should have the ability to measure methane concentrations <25 parts per trillion (ppt) in solar occultation mode, and 11 parts per billion in nadir mode. Occultation detections as low as 10 ppt could be made if spectra are averaged (Drummond et al., 2011). Results have been obtained for all three channels in nadir and in solar occultation.© 2016 The Authors. Published by Elsevier Ltd.

Published
2016

34. Optical and radiometric models of the NOMAD instrument part II: The infrared channels - SO and LNO

Author

Belgian Science Policy Office, European Space Agency, UK Space Agency, Thomas, Ian R., Vandaele, Ann Carine, Robert, S., Neefs, E., Drummond, R., Daerden, Frank, Delanoye, S., Ristic, Bojan, Berkenbosch, S., Clairquin, R., Maes, J., Bonnewijn, S., Depiesse, C., Mahieux, A., Trompet, L., Neary, L., Willame, Y., Wilquet, V., Nevejans, D., Aballea, L., Moelans, W., De Vos, L., Lesschaeve, S., Van Vooren, N., López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Moreno, L., Juan, J., Patel, M., Allen, M., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Fedorova, A., Formisano, V., Funke, Bernd, Fussen, D., García Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, D., Giuranna, M., Belgian Science Policy Office, European Space Agency, UK Space Agency, Thomas, Ian R., Vandaele, Ann Carine, Robert, S., Neefs, E., Drummond, R., Daerden, Frank, Delanoye, S., Ristic, Bojan, Berkenbosch, S., Clairquin, R., Maes, J., Bonnewijn, S., Depiesse, C., Mahieux, A., Trompet, L., Neary, L., Willame, Y., Wilquet, V., Nevejans, D., Aballea, L., Moelans, W., De Vos, L., Lesschaeve, S., Van Vooren, N., López-Moreno, José Juan, Patel, Manish R., Bellucci, Giancarlo, Moreno, L., Juan, J., Patel, M., Allen, M., Altieri, F., Aoki, Shohei, Bolsée, D., Clancy, T., Cloutis, E., Fedorova, A., Formisano, V., Funke, Bernd, Fussen, D., García Comas, Maia, Geminale, A., Gérard, Jean-Claude, Gillotay, D., and Giuranna, M.

Abstract

NOMAD is a suite of three spectrometers that will be launched in 2016 as part of the joint ESA-Roscosmos ExoMars Trace Gas Orbiter mission. The instrument contains three channels that cover the IR and UV spectral ranges and can perform solar occultation, nadir and limb observations, to detect and map a wide variety of Martian atmospheric gases and trace species. Part I of this work described the models of the UVIS channel; in this second part, we present the optical models representing the two IR channels, SO (Solar Occultation) and LNO (Limb, Nadir and Occultation), and use them to determine signal to noise ratios (SNRs) for many expected observational cases. In solar occultation mode, both the SO and LNO channel exhibit very high SNRs >5000. SNRs of around 100 were found for the LNO channel in nadir mode, depending on the atmospheric conditions, Martian surface properties, and observation geometry.

Published
2016

35. Thermal structure of Venus' nightside upper atmosphere measured by SPICAV UV on Venus Express

Author

Arianna Piccialli, Montmessin, F., Belyaev, D., Mahieux, A., Wilquet, V., Fedorova, A., Marcq, E., Bertaux, J. -L, Vandaele, A. C., Korablev, O., 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), Moscow Institute of Physics and Technology [Moscow] (MIPT), 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), and Cardon, Catherine

Subjects
Thermal structure, SPICAV, [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], Venus express, Instrument, Planet, Stellar occultation, Venus, UV
Abstract

International audience; The SPICAV UV instrument offers the possibility to probe the nightside of Venus upper atmosphere by means of stellar occultation. Here we analyze the entire SPICAV database, collected during seven years of operations, which consists of more than 550 vertical density and temperature profiles. The thermal structure of Venus mesosphere and thermosphere shows a large temporal and spatial variability

Published
2014

36. SOIR and NOMAD: Characterization of Planetary Atmospheres

Author

Robert, S., Chamberlain, S., Mahieux, A., Thomas, I., Wilquet, V., and Vandaele, A. C.

Subjects
Astronomy and Astrophysics, Astronomical spectroscopy
Abstract

The Belgian Institute for Space Aeronomy is involved in the Venus Express mission (VeX), launched in 2006 and in the ExoMars Trace Gas Orbiter mission (TGO), due for launch in 2016. BISA is responsible for one instrument in each mission, SOIR onboard VeX and NOMAD onboard TGO respectively. The SOIR instrument onboard Venus Express allows observations of trace gases in the Venus atmosphere, at the terminator for both the morning and evening sides of the planet and for almost all latitudes. It has been designed to measure spectra in the IR region (2.2 – 4.3 µm) of the Venus atmosphere using the solar occultation technique1. This method derives unique information on the vertical composition and structure of the mesosphere and lower thermosphere2,3,4,5. It is unique in terms of spectral coverage and spectral resolution (0.15 cm-1), and is ideally designed to probe the Venus atmosphere for CO2 as well as trace gases, such as H2O, CO, HCl and HF. SOIR is capable of (1) providing vertical information on a broad series of species, such as CO2, CO, H2O, HCl, HF, SO26 and aerosols 7, covering the so far sparsely known region located above the clouds, (2) contributing to a better understanding of the dynamics and stability of the atmosphere by delivering total density and kinetic temperature profiles at the terminator, an up-to-now still unchartered region, and (3) detecting weak absorption bands of rare CO2 isotopologues8, due to the sensitivity of SOIR, the high concentration of CO2 on Venus and the long absorption paths sounded during solar occultations.

Published
2014
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37. Venus' Robotic Exploration at Upper Cloud Level: A US-European Perspective

Author

Widemann, Thomas, Wilquet, V., Mcgouldrick, K., Määttänen, Anni, Cutts, J., Wilson, C., Jessup, K. L., Limaye, S., Polidan, R., Griffin, K., 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), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], 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), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Cardon, Catherine, and California Institute of Technology (CALTECH)-NASA

Subjects
[PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Physics::Space Physics, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

The European mission has improved our knowledge of both upper cloud and haze regions by providing global long-term remote sensing observations of chemistry and winds with coverage in latitude and local solar time. However major questions remain.

Published
2014

38. Update of the Venus density and temperature profiles at high altitude measured by SOIR on board Venus Express

Author

Mahieux, A., Vandaele, A. C., Bougher, S. W., Drummond, R., Robert, S., Wilquet, V., Chamberlain, S., Piccialli, A., Montmessin, F., Tellmann, S., Paetzold, M., Haeusler, B., Bertaux, J. L., Mahieux, A., Vandaele, A. C., Bougher, S. W., Drummond, R., Robert, S., Wilquet, V., Chamberlain, S., Piccialli, A., Montmessin, F., Tellmann, S., Paetzold, M., Haeusler, B., and Bertaux, J. L.

Abstract

The SOIR instrument on board Venus Express regularly sounds the Venus atmosphere using the solar occultation technique. The density and temperature profiles are inferred from SOIR spectra recorded in the infrared. The method has been described in a previous publication (Mahieux et al., 2012. J. Geophys. Res. 117. doi:10.1029/2012JE004058.). This paper is devoted to the update of the VAST (Venus Atmosphere from SOIR measurements at the Terminator) compilation that was initiated in the above cited work, which gives the mean CO2 number density and temperature profiles for different latitude bins. The method has been improved and has been applied to more data. The new compilation which is given on the same latitudinal grid now distinguishes between the two sides of the terminator. The compilation also confirms the main thermal layering characteristics that were identified in the earlier version: the succession of a warm layer (230 +/- 30K, 1 - sigma. standard deviation) at a pressure level of 3.2 x 10(-7) mbar (similar to 140 km), a very cold layer (125 +/- 32K) at 2.5 x 10(-5) mbar (similar to 123 km), a warm layer (204 +/- 17 K) at 0.01 mbar (similar to 102 km) and finally a colder layer at 0.4 mbar (171 +/- 34K, similar to 87 km). The layering of all the temperature profiles is explained by radiative rather than dynamical processes. The temporal temperature variation is larger than the mean latitudinal temperature variation. VAST is compared with temperature profiles obtained from other Venus Express instruments, VeRa and SPICAV-UV, and ground based measurements. (C) 2015 Elsevier Ltd. All rights reserved.

Published
2015

39. Climatology of the Venus upper haze as measured by SOIR onboard Venus Express

Author

Wilquet, V., Drummond, R., Mahieux, A., Robert, S., Vandaele, A. C., Bertaux, Jean-Loup, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)

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

International audience

Published
2010

41. Update of the Venus density and temperature profiles at high altitude measured by SOIR on board Venus Express

Author

Mahieux, A., primary, Vandaele, A.C., additional, Bougher, S.W., additional, Drummond, R., additional, Robert, S., additional, Wilquet, V., additional, Chamberlain, S, additional, Piccialli, A., additional, Montmessin, F., additional, Tellmann, S., additional, Pätzold, M., additional, Häusler, B., additional, and Bertaux, J.L., additional

Published
2015
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46. Discovery of an Ozone Layer on Venus by SPICAV on Venus Express

Author

Montmessin, Franck, Bertaux, Jean-Loup, Lefèvre, Franck, Vandaele, A., Korablev, O., Marcq, Emmanuel, Fedorova, Anna, Royer, Emilie, Mahieux, A., Belyaev, Denis, Wilquet, V., 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), 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), and Cardon, Catherine

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

The SPICAV instrument onboard the Venus Express spacecraft is a multi-channel suite covering the far ultraviolet to the mid-infrared. In this presentation, we will focus on the results obtained by the UV channel during stellar occultations observations. Stellar occultation technique possesses well-known advantages: self-calibration, low sensitivity to instrument aging, simple laws of radiative transfer. In addition, occultation with stars permit to cover a broad range of latitudes at any given season and they provide optimal geometrical registration. Since Venus Express orbit insertion, several hundreds of occultations have been performed by SPICAV, yielding profiles of atmospheric constituents between 80 and 140 km. In the SPICAV UV range, CO2 possesses a broad signature shortward of 200 nm which allows one to retrieve CO2 concentration and subsequently to deduce atmospheric pressure and temperature profiles in the upper mesosphere and in the thermosphere. The Venusian thermosphere shows excessive variability, with the equivalent of more than three scale heights change in density in less than a few days. No other spectral signature besides that of CO2 and haze particles was expected to appear in SPICAV ultraviolet spectra at this altitude range but a consistent search was undertaken, revealing the presence of ozone at 100 km (

Published
2009

47. Minor gaseous constituents and aerosols of the Venus mesosphere measured by SPICAV/SOIR on board Venus Express

Author

Mahieux, A., Drummond, R., Wilquet, V., Vandaele, A., Fedorova, A., Korablev, O., Villard, Eric, Montmessin, Franck, Bertaux, Jean-Loup, 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)

Subjects
[SDU]Sciences of the Universe [physics], Middle atmosphere: composition and chemistry, ATMOSPHERIC COMPOSITION AND STRUCTURE
Abstract

International audience; The SOIR instrument performs solar occultation measurements in the IR region (2.2 - 4.3 μm) at a resolution of 0.12 cm-1, the highest on board Venus Express. It combines an echelle spectrometer and an AOTF (Acousto-Optical Tunable Filter) for the order selection. A brief description of the instrument and its in- flight measured performances will be presented. The wavelength range probed by SOIR allows a detailed chemical inventory of the Venus atmosphere above the cloud layer (65 to 150 km) with an emphasis on vertical distribution of the gases. In particular, measurements of HDO, H2O, HCl, HF, CO and CO2 vertical profiles have been routinely performed. Temperature retrieval will be described and tentative results presented. Aerosols extinction profiles are also simultaneously retrieved from the SOIR spectra. Some results for selected orbits will be investigated and discussed. It will be shown that size distribution can be addressed but only when considering all three channels of the SPICAV/SOIR instrument.

Published
2009

48. CO measurements and climatology from SOIR measurements in the upper atmosphere of Venus

Author

Mahieux, A., Drummond, R., Wilquet, V., Vandaele, A. C., Fedorova, A., Villard, Eric, Montmessin, Franck, Bertaux, Jean-Loup, 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)

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

International audience; Previous measurements of the Venus atmosphere were performed essentially in the mesosphere below 100 km and below the clouds. Information about minor atmospheric constituents, their concentration, reactions, sources and sinks is incomplete, as for example only scarce measurements have been performed above 100 km altitude. SOIR is designed to measure the atmospheric transmission in the IR (2.2-4.3 µm) at high resolution (0.12 cm-1) using solar occultations. This technique allows for the derivation of unique information about the vertical structure and composition of the Venus mesosphere [1,2]. The primary source of CO in the atmosphere of Venus is the photodissociation of CO2 by solar UV at altitudes higher than 120 km. It was shown that CO exhibits a significant diurnal variation and strong year to year variations [3,4], but also latitudinal variations. CO concentration and vmr between 70 and 125 km have been recently retrieved from SOIR data for both terminators. The solar occultations with a high vertical resolution are mainly located at latitudes comprised between 60° and 90° N, but the latitudinal coverage of CO measurements is more complete if we also consider occultations for which the vertical resolution is coarser. We will present an overview of the CO measurements obtained by the SOIR instrument over the last 3 years in order to complete the climatology of CO above the clouds in the atmosphere of Venus. We will also discuss a puzzling strong minimum of the CO vmr in the 80-90 km region found by SOIR, which had escaped detection up to now. 1. A. Mahieux, S. Berkenbosch, R. Clairquin, D. Fussen, N. Mateshvili, E. Neefs, D. Nevejans, B. Ristic, A. C. Vandaele, V. Wilquet, D. Belyaev, A. Fedorova, O. Korablev, E. Villard, F. Montmessin and J.-L. Bertaux, "In-Flight performance and calibration of SPICAV SOIR on board Venus Express", Applied Optics 47 (13), 2252-65 (2008). 2. D. Nevejans, E. Neefs, E. Van Ransbeeck, S. Berkenbosch, R. Clairquin, L. De Vos, W. Moelans, S. Glorieux, A. Baeke, O. Korablev, I. Vinogradov, Y. Kalinnikov, B. Bach, J.-P. Dubois and E. Villard, "Compact high-resolution space-borne echelle grating spectrometer with AOTF based on order sorting for the infrared domain from 2.2 to 4.3 micrometer", Applied Optics 45 (21), 5191-5206 (2006). 3. R. T. Clancy, B. Sandor and G. H. Moriarty-Schieven, "Observational definition of the Venus mesopause: vertical structure, diurnal variation, and temporal instability", Icarus 161 (1), 1-16 (2003). 4. M. Gurwell, D. O. Muhleman, K. Shah, G. Berge, D. J. Rudy and A. W. Grossman, "Observations of the CO bulge on Venus and implications for mesospheric winds", Icarus 115 (1), 141-158 (1995).

Published
2009

49. CO2 catalogue from SOIR on board Venus Express

Author

Borkov, Y., Perevalov, V., Tashkun, S., Vandaele, A. C., Drummond, R., Mahieux, A., Wilquet, V., Bertaux, Jean-Loup, V.E. Zuev Institute of Atmospheric Optics (IAO), Siberian Branch of the Russian Academy of Sciences (SB RAS), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), and 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)

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

International audience; The SOIR instrument performs solar occultation measurements in the IR region (2.2 - 4.3 µm) at a resolution of 0.12 cm-1, the highest on board Venus Express. It combines an echelle spectrometer and an AOTF (Acousto-Optical Tunable Filter) for the order selection. The wavelength range probed by SOIR allows a detailed chemical inventory of the Venus atmosphere above the cloud layer (65 to 150 km) with an emphasis on vertical distribution of the gases. In particular, measurements of CO2 vertical profiles have been routinely performed. Its isotopologues have also been studied. The detection of the up to then unobserved 01111-00001 absorption band of 12C16O18O [1, 2] initiated a extensive and systematic search of other such unobserved CO2 bands. Here we report the detection of several new absorption bands of different isotopologues of CO2 as observed by SOIR on board the Venus Express mission. 1. Bertaux, J.-L., A.C. Vandaele, V. Wilquet, F. Montmessin, R. Dahoo, E. Villard, O. Korablev, and A. Fedorova, First observation of 628 CO2 isotopologue band at 3.3 mm in the atmosphere of Venus by solar occultation from Venus Express, Icarus, 195(1), 28-33, 2008. 2. Wilquet, V., A. Mahieux, A.C. Vandaele, V.I. Perevalov, S.A. Tashkun, A. Fedorova, O. Korablev, F. Montmessin, R. Dahoo, and J.-L. Bertaux, Line parameters for the 01111-00001 band of 12C16O18O from SOIR measurements of the Venus atmosphere, Journal of Quantitative Spectroscopy and Radiative Transfer, 109, 895-905, 2008.

Published
2009

50. An overview of SPICAV/SOIR results on the atmosphere of Venus from Venus Express Mission

Author

Bertaux, Jean-Loup, Vandaele, A., Korablev, O., Montmessin, Franck, Marcq, Emmanuel, Chaufray, Jean-Yves, Wilquet, V., Fedorova, Anna, Mahieux, A., Belyaev, Denis, Villard, Eric, Gerard, J., Royer, Emilie, Quémerais, Eric, Cardon, Catherine, 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), 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), Space Science and Engineering Division [San Antonio], Southwest Research Institute [San Antonio] (SwRI), Moscow Institute of Physics and Technology [Moscow] (MIPT), and HELIOS - LATMOS

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

SPICAV/SOIR is a suite of three spectrometers in the UV and IR range flying on ESA Venus Express orbiter, dedicated to the study of the atmosphere of Venus : UV (110-320 nm), Vis-Nir (0.65-1.65 µm), and mid IR (2.3-4.4 µm). The UV spectrometer discovered a high altitude layer of SO2 ( 85-105 km), apparently correlated with the density of haze particles. Ozone is detected for the first time in the atmosphere of Venus. The night side γ and δ bands of NO intensities are maximal at 2 am (influence of super-rotation), while the O2 emission mapped simultaneously by Virtis peaking at 95 km altitude ( 10 km below NO emission) is centered at midnight, a puzzle for general circulation models. The hot hydrogen component of the exosphere, extending at more than 30,000 km, is variable. The SPICAV VIS-IR sensor (0.7-1.7 μm, resolution 0.5-1.2 nm) employs a pioneering technology: acousto-optical tunable filter (AOTF). Day side observations indicate a variable latitude distribution of cloud top altitude (decreasing toward the pole) and water vapor mixing ratio. The SOIR spectrometer is a new Solar Occultation IR spectrometer in the range λ=2.2-4.3 µm, with a spectral resolution λ/Δλ>20,000, the highest ever flown in a planetary mission. This new concept includes a combination of an echelle grating and an AOTF crystal to sort out one order at a time. Vertical profiles of CO, HDO, H2O, HCl, SO2, CO2 isotopes and temperature are regularly retrieved, as well as aerosols. The CO mixing ratio (80-130 km), a tracer of atmospheric exchange from thermosphere to lower atmosphere, is 10 times less than the VIRA model prescription, showing also some time variability.

Published
2009

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