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115 results on '"Trompet, L."'

1. H2CO, O3, NH3, HCN, N2O, NO2, NO, and HO2 upper limits of detection in the Venus lower-mesosphere using SOIR on board Venus Express

Author: Mahieux, A., Viscardy, S., Jessup, K.L., Mills, F.P., Trompet, L., Robert, S., Aoki, S., Piccialli, A., and Vandaele, A.C.
Published: 2024
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2. The SOIR/Venus Express species concentration and temperature database: CO2, CO, H2O, HDO, H35Cl, H37Cl, HF individual and mean profiles

Author: Mahieux, A., Robert, S., Piccialli, A., Trompet, L., and Vandaele, A.C.
Published: 2023
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3. Virtual European Solar & Planetary Access (VESPA): a Planetary Science Virtual Observatory cornerstone

Author: Erard, S., Cecconi, B., Sidaner, P. Le, Chauvin, C., Rossi, A. P., Minin, M., Capria, T., Ivanovski, S., Schmitt, B., Genot, V., Andre, N., Marmo, C., Vandaele, A. C., Trompet, L., Scherf, M., Hueso, R., Maattanen, A., Carry, B., Achilleos, N., Soucek, J., Pisa, D., Benson, K., Fernique, P., and Millour, E.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The Europlanet-2020 programme, which ended on Aug 31st, 2019, included an activity called VESPA (Virtual European Solar and Planetary Access), which focused on adapting Virtual Observatory (VO) techniques to handle Planetary Science data. This paper describes some aspects of VESPA at the end of this 4-years development phase and at the onset of the newly selected Europlanet-2024 programme starting in 2020. The main objectives of VESPA are to facilitate searches both in big archives and in small databases, to enable data analysis by providing simple data access and online visualization functions, and to allow research teams to publish derived data in an interoperable environment as easily as possible. VESPA encompasses a wide scope, including surfaces, atmospheres, magnetospheres and planetary plasmas, small bodies, helio-physics, exoplanets, and spectroscopy in solid phase. This system relies in particular on standards and tools developed for the Astronomy VO (IVOA) and extends them where required to handle specificities of Solar System studies. It also aims at making the VO compatible with tools and protocols developed in different contexts, for instance GIS for planetary surfaces, or time series tools for plasma-related measurements. An essential part of the activity is to publish a significant amount of high-quality data in this system, with a focus on derived products resulting from data analysis or simulations., Comment: Submitted to Data Science Journal
Published: 2019

4. Update on SO2, detection of OCS, CS, CS2, and SO3, and upper limits of H2S and HOCl in the Venus mesosphere using SOIR on board Venus Express

Author: Mahieux, A., Robert, S., Mills, F.P., Jessup, K.L., Trompet, L., Aoki, S., Piccialli, A., Peralta, J., and Vandaele, A.C.
Published: 2023
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5. VESPA: a community-driven Virtual Observatory in Planetary Science

Author: Erard, S., Cecconi, B., Sidaner, P. Le, Rossi, A. P., Capria, T., Schmitt, B., Génot, V., André, N., Vandaele, A. C., Scherf, M., Hueso, R., Määttänen, A., Thuillot, W., Carry, B., Achilleos, N., Marmo, C., Santolik, O., Benson, K., Fernique, P., Beigbeder, L., Millour, E., Rousseau, B., Andrieu, F., Chauvin, C., Minin, M., Ivanoski, S., Longobardo, A., Bollard, P., Albert, D., Gangloff, M., Jourdane, N., Bouchemit, M., Glorian, J. -M., Trompet, L., Al-Ubaidi, T., Juaristi, J., Desmars, J., Guio, P., Delaa, O., Lagain, A., Soucek, J., and Pisa, D.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The VESPA data access system focuses on applying Virtual Observatory (VO) standards and tools to Planetary Science. Building on a previous EC-funded Europlanet program, it has reached maturity during the first year of a new Europlanet 2020 program (started in 2015 for 4 years). The infrastructure has been upgraded to handle many fields of Solar System studies, with a focus both on users and data providers. This paper describes the broad lines of the current VESPA infrastructure as seen by a potential user, and provides examples of real use cases in several thematic areas. These use cases are also intended to identify hints for future developments and adaptations of VO tools to Planetary Science., Comment: Planetary and Space Sciences (in press), Special Issue "Enabling Open and Interoperable Access to Planetary Science and Heliophysics Databases and Tools". 43 pages, 14 figures, 1 table
Published: 2017
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6. 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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7. Impact of gradients at the martian terminator on the retrieval of ozone from SPICAM/MEx

Author: Piccialli, A., Vandaele, A.C., Trompet, L., Neary, L., Viscardy, S., Erwin, J.T., Määttänen, A., Daerden, F., Willame, Y., Robert, S., Aoki, S., Wilquet, V., Lefèvre, F., and Montmessin, F.
Published: 2021
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8. Strong Localized Pumping of Water Vapor to High Altitudes on Mars During the Perihelion Season.

Author: Brines, A., López‐Valverde, M. A., Funke, B., González‐Galindo, F., Aoki, S., Villanueva, G. L., Holmes, J. A., Belyaev, D. A., Liuzzi, G., Thomas, I. R., Erwin, J. T., Grabowski, U., Forget, F., Lopez‐Moreno, J. J., Rodriguez‐Gomez, J., Daerden, F., Trompet, L., Ristic, B., Patel, M. R., and Bellucci, G.
Subjects: MARTIAN atmosphere, WATER vapor, WATER vapor transport, MARS (Planet), WATER pumps, ATMOSPHERIC water vapor measurement, ALTITUDES
Abstract: Here we present water vapor vertical profiles observed with the ExoMars Trace Gas Orbiter/Nadir and Occultation for MArs Discovery instrument during the perihelion and Southern summer solstice season (LS = 240°–300°) in three consecutive Martian Years 34, 35, and 36. We show the detailed latitudinal distribution of H2O at tangent altitudes from 10 to 120 km, revealing a vertical plume at 60°S–50°S injecting H2O upward, reaching abundance of about 50 ppmv at 100 km. We have observed this event repeatedly in the three Martian years analyzed, appearing at LS = 260°–280° and showing inter‐annual variations in the magnitude and timing due to long term effects of the Martian Year 34 Global Dust Storm. We provide a rough estimate of projected hydrogen escape of 3.2 × 109 cm−2 s−1 associated to these plumes, adding further evidence of the key role played by the perihelion season in the long term evolution of the planet's climate. Plain Language Summary: Studying the vertical distribution of the Martian atmosphere is crucial to understand what happened to the water presumably present in larger abundance on ancient Mars. We have analyzed the vertical profiles of three Martian Years during the Southern summer, revealing a strong vertical transport of water vapor to the upper atmosphere. This seasonal phenomenon seems to be repeated annually, although with variations in the location and time of the year. Our estimation of the associated upward hydrogen flux represents an important loss which could have contributed to the escape of water to space for at least the period in which Mars had its present orbital inclination. Key Points: Latitudinal distributions of water vapor up to 120 km are analyzed in detail using Nadir and Occultation for MArs Discovery (NOMAD) observations with an improved retrieval schemeWater vapor injection during the perihelion localized around 50°–60°S in three consecutive Martian yearsMartian year 34 Global Dust Storm may have affected the driving mechanisms of the plume, delaying its appearance and reducing its magnitude [ABSTRACT FROM AUTHOR]
Published: 2024
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9. SOIR/VEx observations of water vapor at the terminator in the Venus mesosphere

Author: Chamberlain, S., Mahieux, A., Robert, S., Piccialli, A., Trompet, L., Vandaele, A.C., and Wilquet, V.
Published: 2020
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10. H2CO, O3, NH3, HCN, N2O, NO2, NO, and HO2 upper limits of detection in the Venus lower-mesosphere using SOIR on board Venus Express

Author: Mahieux, A., primary, Viscardy, S., additional, Jessup, K.L., additional, Mills, F.P., additional, Trompet, L., additional, Robert, S., additional, Aoki, S., additional, Piccialli, A., additional, and Vandaele, A.C., additional
Published: 2023
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11. Water Vapor Vertical Distribution on Mars During Perihelion Season of MY 34 and MY 35 With ExoMars‐TGO/NOMAD Observations

Author: Brines, A., primary, López‐Valverde, M. A., additional, Stolzenbach, A., additional, Modak, A., additional, Funke, B., additional, Galindo, F. G., additional, Aoki, S., additional, Villanueva, G. L., additional, Liuzzi, G., additional, Thomas, I. R., additional, Erwin, J. T., additional, Grabowski, U., additional, Forget, F., additional, Lopez‐Moreno, J. J., additional, Rodriguez‐Gomez, J., additional, Daerden, F., additional, Trompet, L., additional, Ristic, B., additional, Patel, M. R., additional, Bellucci, G., additional, and Vandaele, A. C., additional
Published: 2023
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12. Depletion of 13C in CO in the Atmosphere of Mars Suggested by ExoMars-TGO/NOMAD Observations

Author: Aoki, S., primary, Shiobara, K., additional, Yoshida, N., additional, Trompet, L., additional, Yoshida, T., additional, Terada, N., additional, Nakagawa, H., additional, Liuzzi, G., additional, Vandaele, A. C., additional, Thomas, I. R., additional, Villanueva, G. L., additional, Lopez-Valverde, M. A., additional, Brines, A., additional, Patel, M. R., additional, Faggi, S., additional, Daerden, F., additional, Erwin, J. T., additional, Ristic, B., additional, Bellucci, G., additional, Lopez-Moreno, J. J., additional, Kurokawa, H., additional, and Ueno, Y., additional
Published: 2023
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13. Carbon Dioxide Retrievals From NOMAD‐SO on ESA's ExoMars Trace Gas Orbiter and Temperature Profile Retrievals With the Hydrostatic Equilibrium Equation: 2. Temperature Variabilities in the Mesosphere at Mars Terminator

Author: Trompet, L., primary, Vandaele, A. C., additional, Thomas, I., additional, Aoki, S., additional, Daerden, F., additional, Erwin, J., additional, Flimon, Z., additional, Mahieux, A., additional, Neary, L., additional, Robert, S., additional, Villanueva, G., additional, Liuzzi, G., additional, López‐Valverde, M. A., additional, Brines, A., additional, Bellucci, G., additional, Lopez‐Moreno, J. J., additional, and Patel, M. R., additional
Published: 2023
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14. Carbon Dioxide Retrievals From NOMAD‐SO on ESA's ExoMars Trace Gas Orbiter and Temperature Profiles Retrievals With the Hydrostatic Equilibrium Equation: 1. Description of the Method

Author: Trompet, L., primary, Vandaele, A. C., additional, Thomas, I., additional, Aoki, S., additional, Daerden, F., additional, Erwin, J., additional, Flimon, Z., additional, Mahieux, A., additional, Neary, L., additional, Robert, S., additional, Villanueva, G., additional, Liuzzi, G., additional, López‐Valverde, M. A., additional, Brines, A., additional, Bellucci, G., additional, López‐Moreno, J. J., additional, and Patel, M. R., additional
Published: 2023
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15. Martian Ozone Observed by TGO/NOMAD‐UVIS Solar Occultation: An Inter‐Comparison of Three Retrieval Methods

Author: Piccialli, A., primary, Vandaele, A. C., additional, Willame, Y., additional, Määttänen, A., additional, Trompet, L., additional, Erwin, J. T., additional, Daerden, F., additional, Neary, L., additional, Aoki, S., additional, Viscardy, S., additional, Thomas, I. R., additional, Depiesse, C., additional, Ristic, B., additional, Mason, J. P., additional, Patel, M. R., additional, Wolff, M. J., additional, Khayat, A. S. J., additional, Bellucci, G., additional, and Lopez‐Moreno, J.‐J., additional
Published: 2023
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16. Carbon Dioxide Retrievals From NOMAD-SO on ESA's ExoMars Trace Gas Orbiter and Temperature Profiles Retrievals With the Hydrostatic Equilibrium Equation: 1. Description of the Method

Author: Ministerio de Ciencia e Innovación (España), European Commission, Belgian Science Policy Office, Trompet, L., Vandaele, A. C., Thomas, I., Aoki, S., Daerden, F., Erwin, J., Flimon, Z., Mahieux, A., Neary, L., Robert, S., Villanueva, G., Liuzzi, G., López-Valverde, M. A., Brines, Adrian, Bellucci, G., López-Moreno, José Juan, Patel, M. R., Ministerio de Ciencia e Innovación (España), European Commission, Belgian Science Policy Office, Trompet, L., Vandaele, A. C., Thomas, I., Aoki, S., Daerden, F., Erwin, J., Flimon, Z., Mahieux, A., Neary, L., Robert, S., Villanueva, G., Liuzzi, G., López-Valverde, M. A., Brines, Adrian, Bellucci, G., López-Moreno, José Juan, and Patel, M. R.
Abstract: The Solar Occultation (SO) channel of the Nadir and Occultation for Mars Discovery (NOMAD) instrument has been scanning the Martian atmosphere for almost 2 Martian years. In this work, we present a subset of the NOMAD SO data measured at the mesosphere at the terminator. From the data set, we investigated 968 vertical profiles of carbon dioxide density and temperature covering the Martian Year (MY) 35 as well as MY 36 up to a solar longitude (Ls) of 135° and altitudes around 60–100 km. While carbon dioxide density profiles are directly retrieved from the spectral signature in the spectra, temperature profiles are more challenging to retrieve as unlike density profiles, temperature profiles can present some spurious features if the regularization is not correctly managed. Comparing seven regularization methods, we found that the expected error estimation method provides the best regularization parameters. The vertical resolution of the profiles is on average 1.6 km. Numerous warm layers and cold pockets appear in this data set. The warm layers are found in the Northern hemisphere at dawn and dusk as well as in the Southern hemisphere at dawn. Strong warm layers are present in more than 13.5% of the profiles. The Southern hemisphere at dusk does not present any warm layer between Ls 50° and 150°. The height and latitudinal distribution of those warm layers were similar in MY 35 and MY 36 during the first half of the year (Ls = 0°–135°). © 2023. The Authors.
Published: 2023

17. Carbon Dioxide Retrievals From NOMAD-SO on ESA's ExoMars Trace Gas Orbiter and Temperature Profile Retrievals With the Hydrostatic Equilibrium Equation: 2. Temperature Variabilities in the Mesosphere at Mars Terminator

Author: Ministerio de Ciencia e Innovación (España), European Commission, Belgian Science Policy Office, Trompet, L., Vandaele, A. C., Thomas, I., Aoki, S., Daerden, F., Erwin, J., Flimon, Z., Mahieux, A., Neary, L., Robert, S., Villanueva, G., Liuzzi, G., López-Valverde, M. A., Brines, Adrian, Bellucci, G., López-Moreno, José Juan, Patel, M. R, Ministerio de Ciencia e Innovación (España), European Commission, Belgian Science Policy Office, Trompet, L., Vandaele, A. C., Thomas, I., Aoki, S., Daerden, F., Erwin, J., Flimon, Z., Mahieux, A., Neary, L., Robert, S., Villanueva, G., Liuzzi, G., López-Valverde, M. A., Brines, Adrian, Bellucci, G., López-Moreno, José Juan, and Patel, M. R
Abstract: The Solar Occultation (SO) channel of the Nadir and Occultation for Mars Discovery (NOMAD) instrument scans the Martian atmosphere since 21 April 2018. In this work, we present a subset of the NOMAD SO data measured at the mesosphere. We focused on a spectral range that started to be recorded in Martian year (MY) 35. A total of 968 vertical profiles of carbon dioxide density and temperature covering MY 35 and the beginning of MY 36 were investigated until 135° of solar longitude. We compared 47 profiles with co-located profiles of the Mars Climate Sounder onboard the Mars Reconnaissance Orbiter. Most profiles show a good agreement as SO temperatures are only 1.8 K higher, but some biases lead to an average absolute difference of 7.4°K. The SO data set is also compared with simulations from the Global Environmental Multiscale-Mars general circulation model. Both data sets are in good agreement except for the presence of a cold layer in the winter hemisphere and a warm layer at dawn in the Northern hemisphere for solar longitudes between 240° and 360°. Five profiles contain temperatures lower than the limit for CO2 condensation. Strong warm layers were found in 13.5% of the profiles. They are present mainly at dawn and in the winter hemisphere, while the Northern dusks appear featureless. The data set mainly covers high latitudes around 60° and we derived some non-migrating tides. In the Southern winter hemisphere, we derived apparent zonal wavenumber-1 (WN-1) and WN-3 tidal components with a maximum amplitude of 10% and 5% at 63 km, respectively. © 2023. The Authors.
Published: 2023

18. Update on SO2, Detection of OCS, CS, CS2, and SO3, and Upper Limits of H2S and HOCl in the Venus Mesosphere Using SOIR on Board Venus Express

Author: Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Belgian Science Policy Office (BELSPO), European Space Agency (ESA), European Union (UE), National Aeronautics and Space Administration (NASA), Mahieux, A., Robert, S., Mills, F. P., Jessup, K. L., Trompet, L., Aoki, S., Piccialli, A., Peralta Calvillo, Javier, Vandaele, A. C., Universidad de Sevilla. Departamento de Física Atómica, Molecular y Nuclear, Belgian Science Policy Office (BELSPO), European Space Agency (ESA), European Union (UE), National Aeronautics and Space Administration (NASA), Mahieux, A., Robert, S., Mills, F. P., Jessup, K. L., Trompet, L., Aoki, S., Piccialli, A., Peralta Calvillo, Javier, and Vandaele, A. C.
Abstract: We report on the update of SO2 and first detections of SO3, CS, and CS2, and detection of OCS above the cloud deck using the SOIR instrument on-board Venus Express, and upper limit profiles of H2S and HOCl. Based on the solar occultation spectra measured by SOIR covering all latitudes over the 2006–2014 period, we find an average SO2 volume mixing ratio of ∼0.02 ppm below 90 km which increases to 5 ppm at 100 km; average OCS abundance of 1 ppb to 1 ppm between 65 and 100 km increasing with altitude; mean SO3 values of 0.1 ppm at 75 km, 1 ppm at 85 km, and 10 ppm at 95 km; CS volume mixing ratios varying from 0.1 ppm at 65 km to 40 ppm at 100 km; finally we report 0.03 ppm of CS2 at 70 km and 5 ppm at 90 km. It is important to note the detections for all of these species may be biased to higher volume mixing ratios at higher altitudes based on the detection limits for SOIR. Upper-limits for H2S and HOCl are determined. All abundances show large variabilities with time and/or latitude equal to at least one order of magnitude at all altitudes. We also study the detection statistics of all detected species as a function of time, latitude, and side of the terminator.
Published: 2023

19. Carbon monoxide observed in Venus’ atmosphere with SOIR/VEx

Author: Vandaele, A.C., Mahieux, A., Chamberlain, S., Ristic, B., Robert, S., Thomas, I.R., Trompet, L., Wilquet, V., and Bertaux, J.L.
Published: 2016
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20. Contribution from SOIR/VEX to the updated Venus International Reference Atmosphere (VIRA)

Author: Vandaele, A.C., Chamberlain, S., Mahieux, A., Ristic, B., Robert, S., Thomas, I., Trompet, L., Wilquet, V., Belyaev, D., Fedorova, A., Korablev, O., and Bertaux, J.L.
Published: 2016
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21. Mesospheric water vapor isotopic ratios at the Venus terminator from SOIR/VEx

Author: Mahieux, A., Vandaele, A., Piccialli , A., Séverine, R., and Trompet, L.
Abstract: The Solar Occultation in the InfraRed (SOIR) instrument onboard Venus Express sounded the Venus mesosphere and lower thermosphere using solar occultation geometry between April 2006 and December 2014. The observations were all taken at the terminator. We report on the water vapor vertical distribution measured from H2O and HDO spectral lines above the clouds and geo-temporal variations, observed across the whole Venus Express mission. Water vapor profiles are sampled between 70 and 120 km, and calculations of the water vapor volume mixing ratio agrees with those from previous studies. Short-term variations of several Earth days dominate the data set. The HDO/H2O profiles are also examined, and compared to a 1D diffusive model to explain the main variations. Similarly to what was found for other trace gases detected with the SOIR instrument, such as HCl, HF and SO2, no significant spatial or long term trends are observed. &nbsp, The 28th IUGG General Assembly (IUGG2023) (Berlin 2023)
Published: 2023
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22. Global Vertical Distribution of Water Vapor on Mars: Results From 3.5 Years of ExoMars‐TGO/NOMAD Science Operations

Author: Aoki, S., primary, Vandaele, A. C., additional, Daerden, F., additional, Villanueva, G. L., additional, Liuzzi, G., additional, Clancy, R. T., additional, Lopez‐Valverde, M. A., additional, Brines, A., additional, Thomas, I. R., additional, Trompet, L., additional, Erwin, J. T., additional, Neary, L., additional, Robert, S., additional, Piccialli, A., additional, Holmes, J. A., additional, Patel, M. R., additional, Yoshida, N., additional, Whiteway, J., additional, Smith, M. D., additional, Ristic, B., additional, Bellucci, G., additional, Lopez‐Moreno, J. J., additional, and Fedorova, A. A., additional
Published: 2022
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23. Explaining NOMAD D/H Observations by Cloud‐Induced Fractionation of Water Vapor on Mars

Author: Daerden, F., Neary, L., Villanueva, G., Liuzzi, G., Aoki, S., Clancy, R. T., Whiteway, J. A., Sandor, B. J., Smith, M. D., Wolff, M. J., Pankine, A., Khayat, A., Novak, R., Cantor, B., Crismani, M., Mumma, M. J., Viscardy, S., Erwin, J., Depiesse, C., Mahieux, A., Piccialli, A., Robert, S., Trompet, L., Willame, Y., Neefs, E., Thomas, I. R., Ristic, B., and Vandaele, A. C.
Subjects: Geophysics, Space and Planetary Science, Geochemistry and Petrology, Earth and Planetary Sciences (miscellaneous)
Published: 2022

24. Global Vertical Distribution of Water Vapor on Mars: Results From 3.5 Years of ExoMars-TGO/NOMAD Science Operations

Author: Ministerio de Ciencia e Innovación (España), European Commission, Belgian Science Policy Office, UK Space Agency, Aoki, S., Vandaele, A. C., Daerden, F., Villanueva, Geronimo L., Liuzzi, G., Clancy, R. T., López-Valverde, M. A., Brines, Adrian, Thomas, I. R., Trompet, L., Erwin, J. T., Neary, L., Robert, S., Piccialli, A., Holmes, J. A., Patel, M. R., Yoshida, N., Whiteway, J., Smith, M. D., Ristic, B., Bellucci, G., López-Moreno, José Juan, Fedorova, A. A., Ministerio de Ciencia e Innovación (España), European Commission, Belgian Science Policy Office, UK Space Agency, Aoki, S., Vandaele, A. C., Daerden, F., Villanueva, Geronimo L., Liuzzi, G., Clancy, R. T., López-Valverde, M. A., Brines, Adrian, Thomas, I. R., Trompet, L., Erwin, J. T., Neary, L., Robert, S., Piccialli, A., Holmes, J. A., Patel, M. R., Yoshida, N., Whiteway, J., Smith, M. D., Ristic, B., Bellucci, G., López-Moreno, José Juan, and Fedorova, A. A.
Abstract: We present water vapor vertical distributions on Mars retrieved from 3.5 years of solar occultation measurements by Nadir and Occultation for Mars Discovery onboard the ExoMars Trace Gas Orbiter, which reveal a strong contrast between aphelion and perihelion water climates. In equinox periods, most of water vapor is confined into the low-middle latitudes. In aphelion periods, water vapor sublimated from the northern polar cap is confined into very low altitudes—water vapor mixing ratios observed at the 0–5 km lower boundary of measurement decrease by an order of magnitude at the approximate altitudes of 15 and 30 km for the latitudes higher than 50°N and 30–50°N, respectively. The vertical confinement of water vapor at northern middle latitudes around aphelion is more pronounced in the morning terminators than evening, perhaps controlled by the diurnal cycle of cloud formation. Water vapor is also observed over the low latitude regions in the aphelion southern hemisphere (0–30°S) mostly below 10–20 km, which suggests north-south transport of water still occurs. In perihelion periods, water vapor sublimated from the southern polar cap directly reaches high altitudes (>80 km) over high southern latitudes, suggesting more effective transport by the meridional circulation without condensation. We show that heating during perihelion, sporadic global dust storms, and regional dust storms occurring annually around 330° of solar longitude (LS) are the main events to supply water vapor to the upper atmosphere above 70 km. © 2022. The Authors.
Published: 2022

25. A Global and Seasonal Perspective of Martian Water Vapor From ExoMars/NOMAD

Author: Crismani, M. M. J., primary, Villanueva, G. L., additional, Liuzzi, G., additional, Smith, M. D., additional, Knutsen, E. W., additional, Daerden, F., additional, Neary, L., additional, Mumma, M. J., additional, Aoki, S., additional, Trompet, L., additional, Thomas, I. R., additional, Ristic, B., additional, Bellucci, G., additional, Piccialli, A., additional, Robert, S., additional, Mahieux, A., additional, Lopez Moreno, J.‐J., additional, Sindoni, G., additional, Giuranna, M., additional, Patel, M. R., additional, and Vandaele, A. C., additional
Published: 2021
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26. Planetary Data in the Virtual Observatory: VESPA (Virtual European Solar and Planetary Access)

Author: Erard, S., Cecconi, B., Le Sinader, P., Rossi, Angelo P., Tomasik, L., Ivanovski, S., Schmitt, B., Andre, N., Trompet, L., Scherf, M, Hueso, R., Demleitner, M., Manaud, N., Taylor, M., Alexeev, I, Määttänen, A., Millour, E., Schmidt, F., Waldmann, I., Fernique, P., D'Amore, A., Brandt, C., Rothkaehl, H., Molinaro, M., Génot, V., Vandaele, A. C., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Direction Informatique de l'Observatoire (DIO ), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Jacobs University [Bremen], Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), INAF - Osservatorio Astronomico di Trieste (OAT), Istituto Nazionale di Astrofisica (INAF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Austrian Academy of Sciences (OeAW), Euskal Herriko Unibertsitatea [Guipúzcoa] (EHU), Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), Universität Heidelberg [Heidelberg], Spacefrog Design, University of Bristol [Bristol], Lomonosov Moscow State University (MSU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire de Météorologie Dynamique (UMR 8539) (LMD), Institut national des sciences de l'Univers (INSU - CNRS)-École polytechnique (X)-École des Ponts ParisTech (ENPC)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Géosciences Paris Saclay (GEOPS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), University College of London [London] (UCL), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Direction Informatique de l'Observatoire (DIO), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg] = Heidelberg University, Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL)
Subjects: vespa, european, [SDU]Sciences of the Universe [physics], virtual, Virtual Observatory, planetary access, solar, Planetary data, padc
Abstract: International audience; In the past 10 years, VESPA has defined an architecture adapted from the astronomy VO, and incorporating concepts and standards from other areas. Progress and new ideas are presented here.
Published: 2021

27. Annual Appearance of Hydrogen Chloride on Mars and a Striking Similarity With the Water Vapor Vertical Distribution Observed by TGO/NOMAD

Author: Aoki, S., primary, Daerden, F., additional, Viscardy, S., additional, Thomas, I. R., additional, Erwin, J. T., additional, Robert, S., additional, Trompet, L., additional, Neary, L., additional, Villanueva, G. L., additional, Liuzzi, G., additional, Crismani, M. M. J., additional, Clancy, R. T., additional, Whiteway, J., additional, Schmidt, F., additional, Lopez‐Valverde, M. A., additional, Ristic, B., additional, Patel, M. R., additional, Bellucci, G., additional, Lopez‐Moreno, J.‐J., additional, Olsen, K. S., additional, Lefèvre, F., additional, Montmessin, F., additional, Trokhimovskiy, A., additional, Fedorova, A. A., additional, Korablev, O., additional, and Vandaele, A. C., additional
Published: 2021
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28. A Global and Seasonal Perspective of Martian Water Vapor From ExoMars/NOMAD

Author: National Aeronautics and Space Administration (US), Belgian Science Policy Office, European Space Agency, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), UK Space Agency, Agenzia Spaziale Italiana, National Fund for Scientific Research (Belgium), Crismani, M. M. J., Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, M. D., Knutsen, E. W., Daerden, Frank, Neary, L., Mumma, M.J., Aoki, Shohei, Trompet, L., Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Piccialli, A., Robert, S., Mahieux, A., López-Moreno, José Juan, Sindoni, G., Giuranna, M., Patel, Manish R., Vandaele, Ann Carine, National Aeronautics and Space Administration (US), Belgian Science Policy Office, European Space Agency, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), UK Space Agency, Agenzia Spaziale Italiana, National Fund for Scientific Research (Belgium), Crismani, M. M. J., Villanueva, Geronimo L., Liuzzi, Giuliano, Smith, M. D., Knutsen, E. W., Daerden, Frank, Neary, L., Mumma, M.J., Aoki, Shohei, Trompet, L., Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Piccialli, A., Robert, S., Mahieux, A., López-Moreno, José Juan, Sindoni, G., Giuranna, M., Patel, Manish R., and Vandaele, Ann Carine
Abstract: Slightly less than a Martian Year of nominal science (March 2018–January 2020) with the ExoMars Trace Gas Orbiter has furthered the ongoing investigation of dayside water vapor column abundance. These dayside observations span latitudes between 75°S and 75°N, and all longitudes, which can provide global snapshots of the total water column abundances. In addition to tracking the seasonal transport of water vapor between poles, geographic enhancements are noted, particularly in the southern hemisphere, both in Hellas Basin, and in other regions not obviously correlated to topography. We report consistent water vapor climatology with previous spacecraft observations, however, note a difference in total water vapor content is noted. Finally, we are unable to find evidence for substantial diurnal variation in the total dayside water vapor column. © 2021. American Geophysical Union. All Rights Reserved.
Published: 2021

29. Annual Appearance of Hydrogen Chloride on Mars and a Striking Similarity With the Water Vapor Vertical Distribution Observed by TGO/NOMAD

Author: Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, European Space Agency, Agenzia Spaziale Italiana, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Belgian Science Policy Office, National Aeronautics and Space Administration (US), UK Space Agency, Aoki, Shohei, Daerden, Frank, Viscardy, S., Thomas, Ian R., Erwin, Justin T., Robert, S., Trompet, L., Neary, L., Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, M. M. J., Clancy, R. Todd, Whiteway, J., Schmidt, F., López-Valverde, M. A., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, José Juan, Olsen, K. S., Lefèvre, F., Montmessin, Franck, Trokhimovskiy, A., Fedorova, A. A., Korablev, O., Vandaele, Ann Carine, Ministerio de Ciencia, Innovación y Universidades (España), Ministerio de Economía y Competitividad (España), European Commission, European Space Agency, Agenzia Spaziale Italiana, Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Belgian Science Policy Office, National Aeronautics and Space Administration (US), UK Space Agency, Aoki, Shohei, Daerden, Frank, Viscardy, S., Thomas, Ian R., Erwin, Justin T., Robert, S., Trompet, L., Neary, L., Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, M. M. J., Clancy, R. Todd, Whiteway, J., Schmidt, F., López-Valverde, M. A., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, José Juan, Olsen, K. S., Lefèvre, F., Montmessin, Franck, Trokhimovskiy, A., Fedorova, A. A., Korablev, O., and Vandaele, Ann Carine
Abstract: Hydrogen chloride (HCl) was recently discovered in the atmosphere of Mars by two spectrometers onboard the ExoMars Trace Gas Orbiter. The reported detection made in Martian Year 34 was transient, present several months after the global dust storm during the southern summer season. Here, we present the full data set of vertically resolved HCl detections obtained by the NOMAD instrument, which covers also Martian year 35. We show that the particular increase of HCl abundances in the southern summer season is annually repeated, and that the formation of HCl is independent from a global dust storm event. We also find that the vertical distribution of HCl is strikingly similar to that of water vapor, which suggests that the uptake by water ice clouds plays an important role. The observed rapid decrease of HCl abundances at the end of the southern summer would require a strong sink independent of photochemical loss. © 2021. American Geophysical Union.
Published: 2021

30. Phosphine in Venus’ atmosphere: Detection attempts and upper limits above the cloud top assessed from the SOIR/VEx spectra

Author: Trompet, L., primary, Robert, S., additional, Mahieux, A., additional, Schmidt, F., additional, Erwin, J., additional, and Vandaele, A. C., additional
Published: 2020
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31. Explanation for the Increase in High‐Altitude Water on Mars Observed by NOMAD During the 2018 Global Dust Storm

Author: Neary, L., primary, Daerden, F., additional, Aoki, S., additional, Whiteway, J., additional, Clancy, R. T., additional, Smith, M., additional, Viscardy, S., additional, Erwin, J.T., additional, Thomas, I. R., additional, Villanueva, G., additional, Liuzzi, G., additional, Crismani, M., additional, Wolff, M., additional, Lewis, S. R., additional, Holmes, J. A., additional, Patel, M. R., additional, Giuranna, M., additional, Depiesse, C., additional, Piccialli, A., additional, Robert, S., additional, Trompet, L., additional, Willame, Y., additional, Ristic, B., additional, and Vandaele, A. C., additional
Published: 2020
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32. Virtual European Solar & Planetary Access (VESPA): A Planetary Science Virtual Observatory Cornerstone

Author: Erard, S., primary, Cecconi, B., additional, Le Sidaner, P., additional, Chauvin, C., additional, Rossi, A. P., additional, Minin, M., additional, Capria, T., additional, Ivanovski, S., additional, Schmitt, B., additional, Génot, V., additional, André, N., additional, Marmo, C., additional, Vandaele, A. C., additional, Trompet, L., additional, Scherf, M., additional, Hueso, R., additional, Määttänen, A., additional, Carry, B., additional, Achilleos, N., additional, Soucek, J., additional, Pisa, D., additional, Benson, K., additional, Fernique, P., additional, and Millour, E., additional
Published: 2020
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33. VESPA: Progress and Prospects

Author: Erard, Stéphane, Cecconi, Baptiste, Le Sidaner, Pierre, Chauvin, C., Rossi, Angelo Pio, Minin, M., Capria, Maria Teresa, Ivanovski, Stavro L., Schmitt, Bernard, Genot, Vincent, André, Nicolas, Marmo, Chiara, Vandaele, Ann-Carine, Trompet, L., Scherf, M., Hueso, R., Määttänen, Anni, Carry, Benoît, Achilleos, Nicholas, Soucek, J., Pisa, D., Benson, Kevin, Fernique, P., Millour, Ehouarn, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Physique des plasmas, 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Direction Informatique de l'Observatoire (DIO), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Jacobs University [Bremen], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Géosciences Paris Sud (GEOPS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Austrian Academy of Sciences (OeAW), Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University College of London [London] (UCL), Institute of Atmospheric Physics [Prague] (IAP), Czech Academy of Sciences [Prague] (CAS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-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-PSL), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL)
Subjects: [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], PADC
Abstract: International audience; We provide a summary of achievements of the VESPA activity in current Europlanet-2020 program, and prospects for a follow-up.
Published: 2019

34. 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

35. 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

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

Author: Belgian Science Policy Office, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Centre National de la Recherche Scientifique (France), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Russian Government, Agenzia Spaziale Italiana, European Space Agency, Korablev, O., Vandaele, Ann Carine, Montmessin, Franck, Fedorova, A. A., Trokhimovskiy, A., Forget, François, Lefèvre, F., Daerden, Frank, Thomas, Ian R., Trompet, L., Erwin, Justin T., Aoki, Shohei, Robert, S., Neary, L., Viscardy, S., Grigoriev, A.V., Ignatiev, N. I., Shakun, Alexey, Patrakeev, A., Belyaev, D.A., Bertaux, J.L., Olsen, K. S., Baggio, L., Alday, J., Ivanov, Y. S., Ristic, Bojan, Mason, J., Willame, Y., Depiesse, C., Hetey, L., Berkenbosch, S., Clairquin, R., Queirolo, C., Beeckman, B., Neefs, E., Patel, Manish R., Bellucci, Giancarlo, López-Moreno, José Juan, Wilson, C. F., Etiope, G., Zelenyi, Lev, Svedhem, H., Vago, J. L., Alonso-Rodrigo, G., Altieri, F., Anufreychik, K., Arnold, G., Bauduin, S., Bolsée, D., Funke, Bernd, García Comas, Maia, González-Galindo, F., López-Puertas, Manuel, López-Valverde, M. A., Martín-Torres, F. J., Vazquez, L., Zorzano, María Paz, Belgian Science Policy Office, Ministerio de Ciencia e Innovación (España), European Commission, UK Space Agency, Centre National de la Recherche Scientifique (France), Fonds de la Recherche Scientifique (Fédération Wallonie-Bruxelles), Roscosmos, Russian Government, Agenzia Spaziale Italiana, European Space Agency, Korablev, O., Vandaele, Ann Carine, Montmessin, Franck, Fedorova, A. A., Trokhimovskiy, A., Forget, François, Lefèvre, F., Daerden, Frank, Thomas, Ian R., Trompet, L., Erwin, Justin T., Aoki, Shohei, Robert, S., Neary, L., Viscardy, S., Grigoriev, A.V., Ignatiev, N. I., Shakun, Alexey, Patrakeev, A., Belyaev, D.A., Bertaux, J.L., Olsen, K. S., Baggio, L., Alday, J., Ivanov, Y. S., Ristic, Bojan, Mason, J., Willame, Y., Depiesse, C., Hetey, L., Berkenbosch, S., Clairquin, R., Queirolo, C., Beeckman, B., Neefs, E., Patel, Manish R., Bellucci, Giancarlo, López-Moreno, José Juan, Wilson, C. F., Etiope, G., Zelenyi, Lev, Svedhem, H., Vago, J. L., Alonso-Rodrigo, G., Altieri, F., Anufreychik, K., Arnold, G., Bauduin, S., Bolsée, D., Funke, Bernd, García Comas, Maia, González-Galindo, F., López-Puertas, Manuel, López-Valverde, M. A., Martín-Torres, F. J., Vazquez, L., and Zorzano, María Paz
Abstract: The detection of methane on Mars has been interpreted as indicating that geochemical or biotic activities could persist on Mars today1. A number of different measurements of methane show evidence of transient, locally elevated methane concentrations and seasonal variations in background methane concentrations2–5. These measurements, however, are difficult to reconcile with our current understanding of the chemistry and physics of the Martian atmosphere6,7, which—given methane’s lifetime of several centuries—predicts an even, well mixed distribution of methane1,6,8. Here we report highly sensitive measurements of the atmosphere of Mars in an attempt to detect methane, using the ACS and NOMAD instruments onboard the ESA-Roscosmos ExoMars Trace Gas Orbiter from April to August 2018. We did not detect any methane over a range of latitudes in both hemispheres, obtaining an upper limit for methane of about 0.05 parts per billion by volume, which is 10 to 100 times lower than previously reported positive detections2,4. We suggest that reconciliation between the present findings and the background methane concentrations found in the Gale crater4 would require an unknown process that can rapidly remove or sequester methane from the lower atmosphere before it spreads globally. © 2019, The Author(s), under exclusive licence to Springer Nature Limited.
Published: 2019

37. 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

38. Preliminary retrievals of CO2 column densities using the ﬁrst data of TGO/NOMAD

Author: European Planetary Science Congress 2018 (Berlin), Piccialli, A., Vandaele, Ann Carine, Thomas, Ian, Robert, Séverine, Aoki, Shohei, Trompet, L., Erwin, Justin T., Daerden, Frank, Neary, L., Viscardy, Sébastien, Ristic, Bojan, Karatekin, Ozgur, Smith, Michael D., Sindoni, G., Oliva, Fabrizio, Bauduin, Sophie, Wolkenberg, Paulina, Lopez-Moreno, J.-J., Bellucci, G., Patel, M.R., NOMAD, Team, European Planetary Science Congress 2018 (Berlin), Piccialli, A., Vandaele, Ann Carine, Thomas, Ian, Robert, Séverine, Aoki, Shohei, Trompet, L., Erwin, Justin T., Daerden, Frank, Neary, L., Viscardy, Sébastien, Ristic, Bojan, Karatekin, Ozgur, Smith, Michael D., Sindoni, G., Oliva, Fabrizio, Bauduin, Sophie, Wolkenberg, Paulina, Lopez-Moreno, J.-J., Bellucci, G., Patel, M.R., and NOMAD, Team
Abstract: info:eu-repo/semantics/nonPublished
Published: 2018

39. VESPA: A community-driven Virtual Observatory in Planetary Science

Author: Erard, S., primary, Cecconi, B., additional, Le Sidaner, P., additional, Rossi, A.P., additional, Capria, M.T., additional, Schmitt, B., additional, Génot, V., additional, André, N., additional, Vandaele, A.C., additional, Scherf, M., additional, Hueso, R., additional, Määttänen, A., additional, Thuillot, W., additional, Carry, B., additional, Achilleos, N., additional, Marmo, C., additional, Santolik, O., additional, Benson, K., additional, Fernique, P., additional, Beigbeder, L., additional, Millour, E., additional, Rousseau, B., additional, Andrieu, F., additional, Chauvin, C., additional, Minin, M., additional, Ivanoski, S., additional, Longobardo, A., additional, Bollard, P., additional, Albert, D., additional, Gangloff, M., additional, Jourdane, N., additional, Bouchemit, M., additional, Glorian, J.-M., additional, Trompet, L., additional, Al-Ubaidi, T., additional, Juaristi, J., additional, Desmars, J., additional, Guio, P., additional, Delaa, O., additional, Lagain, A., additional, Soucek, J., additional, and Pisa, D., additional
Published: 2018
Full Text: View/download PDF

40. 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
Full Text: View/download PDF

41. 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

42. 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

43. 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

44. PDS4 Archive developments for NOMAD/ExoMars TGO

Author: ESA’s Planetary GIS Workshop (5-7 May: ESAC, Madrid, Spain), Trompet, L., Mahieux, Arnaud, Depiesse, Cédric, Daerden, F., Berkenbosch, Sophie, Clairquin, Roland, Neefs, Eddy, Ristic, Bojan, Robert, Séverine, Thomas, I.R., Wilquet, Valérie, Vandaele, Ann Carine, Lopez-Moreno, J.-J., Patel, M.R., Bellucci, G., ESA’s Planetary GIS Workshop (5-7 May: ESAC, Madrid, Spain), Trompet, L., Mahieux, Arnaud, Depiesse, Cédric, Daerden, F., Berkenbosch, Sophie, Clairquin, Roland, Neefs, Eddy, Ristic, Bojan, Robert, Séverine, Thomas, I.R., Wilquet, Valérie, Vandaele, Ann Carine, Lopez-Moreno, J.-J., Patel, M.R., and Bellucci, G.
Abstract: info:eu-repo/semantics/nonPublished
Published: 2015

45. Contribution from SOIR/VEX to the updated Venus International Reference Atmosphere (VIRA)

Author: Vandaele, Ann Carine, Chamberlain, S, Mahieux, Arnaud, Ristic, Bojan, Robert, Séverine, Thomas, I.R., Trompet, L., Wilquet, Valérie, Belyaev, Denis, Fedorova, A., Korablev, O., Bertaux, Jean-Loup, Vandaele, Ann Carine, Chamberlain, S, Mahieux, Arnaud, Ristic, Bojan, Robert, Séverine, Thomas, I.R., Trompet, L., Wilquet, Valérie, Belyaev, Denis, Fedorova, A., Korablev, O., and Bertaux, Jean-Loup
Abstract: info:eu-repo/semantics/inPress
Published: 2015

46. PLANETARY DATA IN THE VIRTUAL OBSERVATORY: VESPA (VIRTUAL EUROPEAN SOLAR & PLANETARY ACCESS).

Author: Erard, S., Cecconi, B., Le Sidaner, P., Rossi, A. P., Tomasik, L., Ivanovski, S., Schmitt, B., André7, N., Trompet, L., Scherf, M., Hueso, R., Demleitner, M., Manaud, N., Taylor, M., Alexeev, I., Määttänen, A., Millour, E., Schmidt, F., Waldmann, I., and Fernique, P.
Subjects: OBSERVATORIES, ASTRONOMICAL catalogs, PLANETARY science, PLANETARY observations, SOLAR system, PYTHON programming language, METADATA
Published: 2021

47. VESPA: PROGRESS AND PROSPECTS.

Author: Erard, S., Cecconi, B., LeSidaner, P., Chauvin, C., Rossi, A. P., Minin, M., Capria, T., Ivanovski, S., Schmitt, B., Génot, V., André, N., Marmo, C., Vandaele, A. C., Trompet, L., Scherf, M., Hueso, R., Määttänen, A., Carry, B., Achilleos, N., and Soucek, J.
Subjects: ONLINE databases, SPATIAL data infrastructures, SPACE sciences
Published: 2019

48. MARTIAN ATMOSPHERIC VERTICAL PROFILES: RESULTS FROM THE FIRST YEAR OF TGO/NOMAD SCIENCE OPERATIONS.

Author: Erwin, J. T., Aoki, S., Thomas, I. R., Trompet, L., Vandaele, A. C., Robert, S., Daerden, F., Ristic, B., L Villanueva, G., Liuzzi, G., Lopez-Moreno, J. J., Bellucci, G., and Patel, M. R.
Subjects: MARTIAN atmosphere, SCIENCE conferences
Published: 2019

49. IASB-BIRA contribution to VESPA for planetary aeronomy studies

Author: Trompet, L., Vandaele, A. C., Geunes, Y., Mahieux, A., Wilquet, V., Chamberlain, S., Robert, S., Thomas, I., Erard, S., Baptiste Cecconi, Le Sidaner, P., Institut royal d'Aéronomie Spatiale de Belgique (IASB), 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), Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Direction Informatique de l'Observatoire (DIO), Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], PADC
Abstract: International audience; IASB-BIRA is contributing to VESPA activities by developing all necessary facilities to make accessible through the VESPA infrastructure: a) SOIR profiles of the atmosphere of Venus and b) the radiative transfer code ASIMUT for simulation or retrievals of spectra.

50. A Global and Seasonal Perspective of Martian Water Vapor from ExoMars/NOMAD

Author: Crismani, M. M. J., Villanueva, G. L., Liuzzi, G., Smith, M. D., Knutsen, E. W., Daerden, F., Neary, L., Mumma, M. J., Aoki, S., Trompet, L., Thomas, I.R., Ristic, B., Bellucci, G., Piccialli, A., Robert, S., Mahieux, A., Lopez Moreno, J‐J, Sindoni, G., Giuranna, M., Patel, M. R, Vandaele, A. C., Crismani, M. M. J., Villanueva, G. L., Liuzzi, G., Smith, M. D., Knutsen, E. W., Daerden, F., Neary, L., Mumma, M. J., Aoki, S., Trompet, L., Thomas, I.R., Ristic, B., Bellucci, G., Piccialli, A., Robert, S., Mahieux, A., Lopez Moreno, J‐J, Sindoni, G., Giuranna, M., Patel, M. R, and Vandaele, A. C.
Abstract: Slightly less than a Martian Year of nominal science (March 2018–January 2020) with the ExoMars Trace Gas Orbiter has furthered the ongoing investigation of dayside water vapor column abundance. These dayside observations span latitudes between 75°S and 75°N, and all longitudes, which can provide global snapshots of the total water column abundances. In addition to tracking the seasonal transport of water vapor between poles, geographic enhancements are noted, particularly in the southern hemisphere, both in Hellas Basin, and in other regions not obviously correlated to topography. We report consistent water vapor climatology with previous spacecraft observations, however, note a difference in total water vapor content is noted. Finally, we are unable to find evidence for substantial diurnal variation in the total dayside water vapor column.

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