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1. Unambiguous detection of mesospheric CO2 clouds on Mars using 2.7 {\mu}m absorption band from the ACS/TGO solar occultations

Author

Luginin, M., Trokhimovskiy, A., Fedorova, A., Belyaev, D., Ignatiev, N., Korablev, O., Montmessin, F., and Grigoriev, A.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

Mesospheric CO2 clouds are one of two types of carbon dioxide clouds known on Mars. We present observations of mesospheric CO2 clouds made by Atmospheric Chemistry Suit (ACS) onboard the ESA-Roscosmos ExoMars Trace Gas Orbiter (TGO). We analyzed 1663 solar occultation sessions of Thermal InfraRed (TIRVIM) and Middle InfraRed (MIR) channels of ACS covering more than two Martian years that contain spectra of 2.7 {\mu}m carbon dioxide ice absorption band. That allowed us to unambiguously discriminate carbon dioxide ice aerosols from mineral dust and water ice aerosols, not relying on the information of atmospheric thermal conditions. CO2 clouds were detected in eleven solar occultation observations at altitudes from 39 km to 90 km. In five cases, there were two or three layers of CO2 clouds that were vertically separated by 5-15 km gaps. Effective radius of CO2 aerosol particles is in the range of 0.1-2.2 {\mu}m. Spectra produced by the smallest particles indicate a need for a better resolved CO2 ice refractive index. Nadir optical depth of CO2 clouds is in the range 5*10^{-4}-4*10^{-2} at both 2.7 {\mu}m and 0.8 {\mu}m. Asymmetrical diurnal distribution of detections observed by ACS is potentially due to local time variations of temperature induced by thermal tides. Two out of five cases of carbon dioxide cloud detections made by the TIRVIM instrument reveal the simultaneous presence of CO2 ice and H2O ice aerosols. Temperature profiles measured by the Near InfraRed (NIR) channel of ACS are used to calculate CO2 saturation ratio S at locations of carbon dioxide clouds. Supersaturation S > 1 is detected in only 5 out of 19 cases of CO2 cloud layers; extremely low values of S < 0.1 are found in 9 out of 19 cases., Comment: 29 pages, 10 figures. Submitted to Icarus

Published
2024
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7. Martian Atmospheric Thermal Structure and Dust Distribution During the MY 34 Global Dust Storm From ACS TIRVIM Nadir Observations

Author

Vlasov, P., primary, Ignatiev, N., additional, Guerlet, S., additional, Grassi, D., additional, Korablev, O., additional, Grigoriev, А., additional, Shakun, A., additional, Patsaev, D., additional, Maslov, I., additional, Zasova, L., additional, Luginin, M., additional, Trokhimovskiy, A., additional, Millour, E., additional, Forget, F., additional, Haus, R., additional, Arnold, G., additional, and Montmessin, F., additional

Published
2022
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8. 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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9. Seasonal reappearance of HCl in the atmosphere of Mars during the Mars year 35 dusty season

Author

Olsen, K. S., primary, Trokhimovskiy, A., additional, Montabone, L., additional, Fedorova, A. A., additional, Luginin, M., additional, Lefèvre, F., additional, Korablev, O. I., additional, Montmessin, F., additional, Forget, F., additional, Millour, E., additional, Bierjon, A., additional, Baggio, L., additional, Alday, J., additional, Wilson, C. F., additional, Irwin, P. G. J., additional, Belyaev, D. A., additional, Patrakeev, A., additional, and Shakun, A., additional

Published
2021
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11. Martian Aerosols in the 3µm Spectral Range, During and Outside the 2018 Global Dust Event Based on the TGO/ACS-MIR Channel

Author

Stcherbinine, Aurélien, Vincendon, M., Montmessin, Franck, Wolff, M. J., Korablev, O., Fedorova, A., Trokhimovskiy, Alexander, Shakun, A., Ignatiev, N., Belyaev, D., Luginin, M., PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), 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), Space Science Institute [Boulder] (SSI), Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), and Cardon, Catherine

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

International audience; We present vertical profiles of water ice clouds in the Martian atmosphere, and the effects of the last global dust storm on them. To this end, we used the data produced by the ACS MIR channel during solar occultations that senses the atmospheric opacity in the 3 μm spectral range. We observe very rapidchanges in the aerosol profile associated with the onset of the global dust event, initiating water ice cloud layer formation above 80 km in a period of days or so, sug- gesting a sudden intensification in the circulation re- gime. More work is needed to extract more infor- mation, such as particle size, yet this preliminary study already provides some insightful data about water ice during the 2018 global dust storm.

Published
2019

12. One Year of ACS/TGO Observations of the Mars Atmosphere

Author

Korablev, O. I., Montmessin, Franck, Fedorova, A. A., Trokhimovskiy, Alexander, Luginin, M., Ignatiev, N. I., Lefèvre, Franck, Shakun, A., Patrakeev, A., Belyaev, D. A., Bertaux, Jean-Loup, Olsen, Kevin, Baggio, Lucio, Alday, J., Wilson, C. F., Guerlet, S., Young, R. M. B., Millour, E., Forget, F., Grigoriev, A. V., Maslov, I., Patsaev, D., Arnold, G., Grassi, Davide, Space Research Institute of the Russian Academy of Sciences (IKI), Russian Academy of Sciences [Moscow] (RAS), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Department of Physics [Oxford], University of Oxford [Oxford], Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), and Cardon, Catherine

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

International audience; ACS onboard the ExoMars TGO) observes the martian atmosphere, using solar occultations and nadir. Status update of the ACS results obtained during one year of observations with the emphasis on trace gases, and the major dust event will be given.

Published
2019

13. 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
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14. Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

Author

Ministerio de Ciencia e Innovación (España), European Space Agency, Belgian Science Policy Office, European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Centre National de la Recherche Scientifique (France), Russian Government, Vandaele, Ann Carine, Korablev, O., Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, F., López-Valverde, M. A., Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, M. D., Erwin, Justin T., Trompet, L., Fedorova, A. A., Montmessin, Franck, Trokhimovskiy, A., Belyaev, D.A., Ignatiev, N. I., Luginin, M., Olsen, K. S., Baggio, L., Alday, J., Bertaux, J.L., Betsis, D., Bolsée, D., Clancy, R. Todd, Cloutis, E., Depiesse, C., Funke, Bernd, García Comas, Maia, Gérard, Jean-Claude, Giuranna, M., González-Galindo, F., Grigoriev, A.V., Ivanov, Y. S., Kaminski, J., Karatekin, O., Lefèvre, F., Lewis, S., López-Puertas, Manuel, Mahieux, A., Maslov, I., Mason, J., Mumma, M.J., Neary, L., Neefs, E., Patrakeev, A., Patsaev, D., Ristic, Bojan, Robert, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Martín-Torres, F. J., Vazquez, L., Zorzano, María Paz, Ministerio de Ciencia e Innovación (España), European Space Agency, Belgian Science Policy Office, European Commission, UK Space Agency, Agenzia Spaziale Italiana, Ministerio de Ciencia, Innovación y Universidades (España), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Centre National de la Recherche Scientifique (France), Russian Government, Vandaele, Ann Carine, Korablev, O., Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, F., López-Valverde, M. A., Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, M. D., Erwin, Justin T., Trompet, L., Fedorova, A. A., Montmessin, Franck, Trokhimovskiy, A., Belyaev, D.A., Ignatiev, N. I., Luginin, M., Olsen, K. S., Baggio, L., Alday, J., Bertaux, J.L., Betsis, D., Bolsée, D., Clancy, R. Todd, Cloutis, E., Depiesse, C., Funke, Bernd, García Comas, Maia, Gérard, Jean-Claude, Giuranna, M., González-Galindo, F., Grigoriev, A.V., Ivanov, Y. S., Kaminski, J., Karatekin, O., Lefèvre, F., Lewis, S., López-Puertas, Manuel, Mahieux, A., Maslov, I., Mason, J., Mumma, M.J., Neary, L., Neefs, E., Patrakeev, A., Patsaev, D., Ristic, Bojan, Robert, S., López-Moreno, José Juan, Alonso-Rodrigo, G., Martín-Torres, F. J., Vazquez, L., and Zorzano, María Paz

Abstract

Global dust storms on Mars are rare1,2 but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere3, primarily owing to solar heating of the dust3. In turn, changes in atmospheric dynamics can affect the distribution of atmospheric water vapour, with potential implications for the atmospheric photochemistry and climate on Mars4. Recent observations of the water vapour abundance in the Martian atmosphere during dust storm conditions revealed a high-altitude increase in atmospheric water vapour that was more pronounced at high northern latitudes5,6, as well as a decrease in the water column at low latitudes7,8. Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. We report the vertical distribution of the HDO/H2O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilometres. Our findings suggest that before the onset of the dust storm, HDO abundances were reduced to levels below detectability at altitudes above 40 kilometres. This decrease in HDO coincided with the presence of water-ice clouds. During the storm, an increase in the abundance of H2O and HDO was observed at altitudes between 40 and 80 kilometres. We propose that these increased abundances may be the result of warmer temperatures during the dust storm causing stronger atmospheric circulation and preventing ice cloud formation, which may confine water vapour to lower altitudes through gravitational fall and subsequent sublimation of ice crystals3. The observed changes in H2O and HDO abundance occurred within a few days during the development of the dust storm, suggesting a fast impact of dust storms on the Martian atmosphere. © 2019, The Author(s), under exclusive licence to Springer Nature Limited.

Published
2019

15. 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

16. SPICAV/SOIR mesospheric aerosols observations and characterization

Author

EGU (Vol. 16, EGU2014-11491-1: Vienna, Austria), Wilquet, Valérie, Fedorova, A., Belyaev, Denis, Luginin, M., Drummond, Rachel, Mahieux, Arnaud, Robert, Séverine, Vandaele, Ann Carine, Montmessin, Frank, Bertaux, J.-L., EGU (Vol. 16, EGU2014-11491-1: Vienna, Austria), Wilquet, Valérie, Fedorova, A., Belyaev, Denis, Luginin, M., Drummond, Rachel, Mahieux, Arnaud, Robert, Séverine, Vandaele, Ann Carine, Montmessin, Frank, and Bertaux, J.-L.

Abstract

info:eu-repo/semantics/nonPublished

Published
2014

20. Normal-incidence Sb/B4C multilayer mirrors for the 80 Å < ? < 120 Å wavelength range

Author

Vishnyakov, E A, Voronov, D L, Gullikson, E M, Kondratenko, V V, Kopylets, I A, Luginin, M S, Pirozhkov, A S, Ragozin, Evgenii N, and Shatokhin, A N

Abstract

Periodic and aperiodic Sb/B4C multilayer structures have been theoretically calculated and synthesised for the first time for the application in soft X-ray optics in the 80 A < l < 120 A range. The reflection spectra of the periodic multilayer mirrors are measured using synchrotron radiation and laser plasma-generated radiation. The experimental spectra are theoretically interpreted with the inclusion of transition layers and substrate roughness. The density of antimony layers is supposedly r(Sb) = 6.0 g cm-3, and the thickness of transition layers (if any) in the Sb/B4C multilayer structures does not exceed 10 A. A peak reflectivity of 19 % is attained at a wavelength of 85 A. An aperiodic mirror optimised for maximum uniform reflectivity in the 100 - 120 A range is tested employing the laser plasma radiation source.

Published
2013

22. 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, Nicolas, Vazquez, L., Vincendon, M., Wilquet, V., Wilson, C. F., Zasova, L. V., Zelenyi, L. M., and Zorzano, M. P.

Subjects
520 Astronomy, 620 Engineering, 7. Clean energy
Abstract

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.

23. 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., 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.

Abstract

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 instrum

24. X/Y platinum(II) complexes: some features of supramolecular assembly via halogen bonding.

Author

Gitlina AY, Petrovskii S, Luginin M, Melnikov A, Rychagova E, Ketkov S, and Grachova E

Abstract

Four series of new luminescent cyclometalated complexes [Pt(C^N)(IPy)Y] (HC^N = 2-phenylpyridine (Hppy), 2-(1-benzofuran-3-yl)pyridine (Hbfpy), methyl-2-phenylquinoline-4-carboxylate (Hmpqc), 2-(1-benzothiophen-3-yl)pyridine (Hbtpy), IPy = 4-iodopyridine, and Y = Cl, Br, I) have been investigated as X/Y 'building blocks' for the construction of a supramolecular network utilizing the I atom in IPy as a halogen bond (XB) donor (the X atom). The σ-hole of the X atom was found to provide non-covalent X⋯Y, X⋯Pt and X⋯π (π system of the metalated chelate ring) interactions for the complexes in the crystal state. NBO analysis confirms donation of the platinum electron density to iodine upon the X⋯Pt interaction. The nature of the X counterpart in XB depends on the nature of the Y atom and the cyclometalating ligand of the Pt(II) complex. DFT calculations show that the HOMO of [Pt(C^N)(IPy)Y] in the S 0 state is delocalized over Pt, Y and a C-coordinating fragment of C^N, while the LUMO in most complexes is formed by the Py orbitals of IPy. However, the α-HOMO in the lowest triplet state of [Pt(C^N)(IPy)Y] contains no contribution of the IPy wavefunctions. All Pt(II) complexes exhibited triplet luminescence in solution and in the solid state ( Φ up to 0.129), which is determined by the nature of the C^N ligand. The emission profile is independent of the nature of the ligand Y, while the quantum yield decreases from Cl to I. Accordingly, on the basis of DFT calculation, this emission is interpreted as a C^N intraligand charge transfer predominantly. The XB formation did not show an effect on the luminescence of the complexes in the solid phase, however grinding of crystals results in an increase of brightness.

Published
2023
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25. The Tail Wags the Dog: The Far Periphery of the Coordination Environment Manipulates the Photophysical Properties of Heteroleptic Cu(I) Complexes.

Author

Paderina A, Melnikov A, Slavova S, Sizov V, Gurzhiy V, Petrovskii S, Luginin M, Levin O, Koshevoy I, and Grachova E

Subjects
Copper chemistry, Ligands, Luminescence, Spectrum Analysis, Coordination Complexes chemistry
Abstract

In this work we show, using the example of a series of [Cu(Xantphos)(N^N)] + complexes (N^N being substituted 5-phenyl-bipyridine) with different peripheral N^N ligands, that substituents distant from the main action zone can have a significant effect on the physicochemical properties of the system. By using the C≡C bond on the periphery of the coordination environment, three hybrid molecular systems with -Si(CH 3 ) 3 , -Au(PR 3 ), and -C 2 HN 3 (CH 2 )C 10 H 7 fragments were produced. The Cu(I) complexes thus obtained demonstrate complicated emission behaviour, which was investigated by spectroscopic, electrochemical, and computational methods in order to understand the mechanism of energy transfer. It was found that the -Si(CH 3 ) 3 fragment connected to the peripheral C≡C bond changes luminescence to long-lived intra-ligand phosphorescence, in contrast to MLCT phosphorescence or TADF. The obtained results can be used for the design of new materials based on Cu(I) complexes with controlled optoelectronic properties on the molecular level, as well as for the production of hybrid systems.

Published
2022
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26. Stormy water on Mars: The distribution and saturation of atmospheric water during the dusty season.

Author

Fedorova AA, Montmessin F, Korablev O, Luginin M, Trokhimovskiy A, Belyaev DA, Ignatiev NI, Lefèvre F, Alday J, Irwin PGJ, Olsen KS, Bertaux JL, Millour E, Määttänen A, Shakun A, Grigoriev AV, Patrakeev A, Korsa S, Kokonkov N, Baggio L, Forget F, and Wilson CF

Abstract

The loss of water from Mars to space is thought to result from the transport of water to the upper atmosphere, where it is dissociated to hydrogen and escapes the planet. Recent observations have suggested large, rapid seasonal intrusions of water into the upper atmosphere, boosting the hydrogen abundance. We use the Atmospheric Chemistry Suite on the ExoMars Trace Gas Orbiter to characterize the water distribution by altitude. Water profiles during the 2018-2019 southern spring and summer stormy seasons show that high-altitude water is preferentially supplied close to perihelion, and supersaturation occurs even when clouds are present. This implies that the potential for water to escape from Mars is higher than previously thought., (Copyright © 2020 The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. No claim to original U.S. Government Works.)

Published
2020
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27. Publisher Correction: Martian dust storm impact on atmospheric H 2 O and D/H observed by ExoMars Trace Gas Orbiter.

Author

Vandaele AC, Korablev O, Daerden F, Aoki S, Thomas IR, Altieri F, López-Valverde M, Villanueva G, Liuzzi G, Smith MD, Erwin JT, Trompet L, Fedorova AA, Montmessin F, Trokhimovskiy A, Belyaev DA, Ignatiev NI, Luginin M, Olsen KS, Baggio L, Alday J, Bertaux JL, Betsis D, Bolsée D, Clancy RT, Cloutis E, Depiesse C, Funke B, Garcia-Comas M, Gérard JC, Giuranna M, Gonzalez-Galindo F, Grigoriev AV, Ivanov YS, Kaminski J, Karatekin O, Lefèvre F, Lewis S, López-Puertas M, Mahieux A, Maslov I, Mason J, Mumma MJ, Neary L, Neefs E, Patrakeev A, Patsaev D, Ristic B, Robert S, Schmidt F, Shakun A, Teanby NA, Viscardy S, Willame Y, Whiteway J, Wilquet V, Wolff MJ, Bellucci G, Patel MR, López-Moreno JJ, Forget F, Wilson CF, Young R, Svedhem H, Vago JL, and Rodionov D

Abstract

The surname of author Cathy Quantin-Nataf was misspelled 'Quantin-Nata' , authors Ehouarn Millour and Roland Young were missing from the ACS Science Team list, and minor changes have been made to the author and affiliation lists; see accompanying Amendment. These errors have been corrected online.

Published
2019
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28. Martian dust storm impact on atmospheric H 2 O and D/H observed by ExoMars Trace Gas Orbiter.

Author

Vandaele AC, Korablev O, Daerden F, Aoki S, Thomas IR, Altieri F, López-Valverde M, Villanueva G, Liuzzi G, Smith MD, Erwin JT, Trompet L, Fedorova AA, Montmessin F, Trokhimovskiy A, Belyaev DA, Ignatiev NI, Luginin M, Olsen KS, Baggio L, Alday J, Bertaux JL, Betsis D, Bolsée D, Clancy RT, Cloutis E, Depiesse C, Funke B, Garcia-Comas M, Gérard JC, Giuranna M, Gonzalez-Galindo F, Grigoriev AV, Ivanov YS, Kaminski J, Karatekin O, Lefèvre F, Lewis S, López-Puertas M, Mahieux A, Maslov I, Mason J, Mumma MJ, Neary L, Neefs E, Patrakeev A, Patsaev D, Ristic B, Robert S, Schmidt F, Shakun A, Teanby NA, Viscardy S, Willame Y, Whiteway J, Wilquet V, Wolff MJ, Bellucci G, Patel MR, López-Moreno JJ, Forget F, Wilson CF, Svedhem H, Vago JL, and Rodionov D

Abstract

Global dust storms on Mars are rare 1,2 but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere 3 , primarily owing to solar heating of the dust 3 . In turn, changes in atmospheric dynamics can affect the distribution of atmospheric water vapour, with potential implications for the atmospheric photochemistry and climate on Mars 4 . Recent observations of the water vapour abundance in the Martian atmosphere during dust storm conditions revealed a high-altitude increase in atmospheric water vapour that was more pronounced at high northern latitudes 5,6 , as well as a decrease in the water column at low latitudes 7,8 . Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. We report the vertical distribution of the HDO/H 2 O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilometres. Our findings suggest that before the onset of the dust storm, HDO abundances were reduced to levels below detectability at altitudes above 40 kilometres. This decrease in HDO coincided with the presence of water-ice clouds. During the storm, an increase in the abundance of H 2 O and HDO was observed at altitudes between 40 and 80 kilometres. We propose that these increased abundances may be the result of warmer temperatures during the dust storm causing stronger atmospheric circulation and preventing ice cloud formation, which may confine water vapour to lower altitudes through gravitational fall and subsequent sublimation of ice crystals 3 . The observed changes in H 2 O and HDO abundance occurred within a few days during the development of the dust storm, suggesting a fast impact of dust storms on the Martian atmosphere.

Published
2019
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