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1. CO2 in the atmosphere of Mars depleted in 13C

Author: Liuzzi, Giuliano, Villanueva, Geronimo L., Aoki, Shohei, Stone, Shane W., Faggi, Sara, Trompet, Loïc, Neary, Lori, Daerden, Frank, Viscardy, Sébastien, Masiello, Guido, Serio, Carmine, Thomas, Ian R., Patel, Manish R., Bellucci, Giancarlo, Lopez-Moreno, Jose-Juan, Ristic, Bojan, and Vandaele, Ann Carine
Published: 2024
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2. Ariel: Enabling planetary science across light-years

Author: Tinetti, Giovanna, Eccleston, Paul, Haswell, Carole, Lagage, Pierre-Olivier, Leconte, Jérémy, Lüftinger, Theresa, Micela, Giusi, Min, Michel, Pilbratt, Göran, Puig, Ludovic, Swain, Mark, Testi, Leonardo, Turrini, Diego, Vandenbussche, Bart, Osorio, Maria Rosa Zapatero, Aret, Anna, Beaulieu, Jean-Philippe, Buchhave, Lars, Ferus, Martin, Griffin, Matt, Guedel, Manuel, Hartogh, Paul, Machado, Pedro, Malaguti, Giuseppe, Pallé, Enric, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Szabó, Robert, Tan, Jonathan, Werner, Stephanie, Ratti, Francesco, Scharmberg, Carsten, Salvignol, Jean-Christophe, Boudin, Nathalie, Halain, Jean-Philippe, Haag, Martin, Crouzet, Pierre-Elie, Kohley, Ralf, Symonds, Kate, Renk, Florian, Caldwell, Andrew, Abreu, Manuel, Alonso, Gustavo, Amiaux, Jerome, Berthé, Michel, Bishop, Georgia, Bowles, Neil, Carmona, Manuel, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Désjonqueres, Lucile, Díaz, José J., Drummond, Rachel, Focardi, Mauro, Gómez, Jose M., Holmes, Warren, Krijger, Matthijs, Kovacs, Zsolt, Hunt, Tom, Machado, Richardo, Morgante, Gianluca, Ollivier, Marc, Ottensamer, Roland, Pace, Emanuele, Pagano, Teresa, Pascale, Enzo, Pearson, Chris, Pedersen, Søren Møller, Pniel, Moshe, Roose, Stéphane, Savini, Giorgio, Stamper, Richard, Szirovicza, Peter, Szoke, Janos, Tosh, Ian, Vilardell, Francesc, Barstow, Joanna, Borsato, Luca, Casewell, Sarah, Changeat, Quentin, Charnay, Benjamin, Civiš, Svatopluk, Foresto, Vincent Coudé du, Coustenis, Athena, Cowan, Nicolas, Danielski, Camilla, Demangeon, Olivier, Drossart, Pierre, Edwards, Billy N., Gilli, Gabriella, Encrenaz, Therese, Kiss, Csaba, Kokori, Anastasia, Ikoma, Masahiro, Morales, Juan Carlos, Mendonça, João, Moneti, Andrea, Mugnai, Lorenzo, Muñoz, Antonio García, Helled, Ravit, Kama, Mihkel, Miguel, Yamila, Nikolaou, Nikos, Pagano, Isabella, Panic, Olja, Rengel, Miriam, Rickman, Hans, Rocchetto, Marco, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Tsiaras, Angelos, Venot, Olivia, Vida, Krisztián, Waldmann, Ingo P., Yurchenko, Sergey, Szabó, Gyula, Zellem, Rob, Al-Refaie, Ahmed, Alvarez, Javier Perez, Anisman, Lara, Arhancet, Axel, Ateca, Jaume, Baeyens, Robin, Barnes, John R., Bell, Taylor, Benatti, Serena, Biazzo, Katia, Błęcka, Maria, Bonomo, Aldo Stefano, Bosch, José, Bossini, Diego, Bourgalais, Jeremy, Brienza, Daniele, Brucalassi, Anna, Bruno, Giovanni, Caines, Hamish, Calcutt, Simon, Campante, Tiago, Canestrari, Rodolfo, Cann, Nick, Casali, Giada, Casas, Albert, Cassone, Giuseppe, Cara, Christophe, Carone, Ludmila, Carrasco, Nathalie, Chioetto, Paolo, Cortecchia, Fausto, Czupalla, Markus, Chubb, Katy L., Ciaravella, Angela, Claret, Antonio, Claudi, Riccardo, Codella, Claudio, Comas, Maya Garcia, Cracchiolo, Gianluca, Cubillos, Patricio, Da Peppo, Vania, Decin, Leen, Dejabrun, Clemence, Delgado-Mena, Elisa, Di Giorgio, Anna, Diolaiti, Emiliano, Dorn, Caroline, Doublier, Vanessa, Doumayrou, Eric, Dransfield, Georgina, Dumaye, Luc, Dunford, Emma, Escobar, Antonio Jimenez, Van Eylen, Vincent, Farina, Maria, Fedele, Davide, Fernández, Alejandro, Fleury, Benjamin, Fonte, Sergio, Fontignie, Jean, Fossati, Luca, Funke, Bernd, Galy, Camille, Garai, Zoltán, García, Andrés, García-Rigo, Alberto, Garufi, Antonio, Sacco, Giuseppe Germano, Giacobbe, Paolo, Gómez, Alejandro, Gonzalez, Arturo, Gonzalez-Galindo, Francisco, Grassi, Davide, Griffith, Caitlin, Guarcello, Mario Giuseppe, Goujon, Audrey, Gressier, Amélie, Grzegorczyk, Aleksandra, Guillot, Tristan, Guilluy, Gloria, Hargrave, Peter, Hellin, Marie-Laure, Herrero, Enrique, Hills, Matt, Horeau, Benoit, Ito, Yuichi, Jessen, Niels Christian, Kabath, Petr, Kálmán, Szilárd, Kawashima, Yui, Kimura, Tadahiro, Knížek, Antonín, Kreidberg, Laura, Kruid, Ronald, Kruijssen, Diederik J. M., Kubelík, Petr, Lara, Luisa, Lebonnois, Sebastien, Lee, David, Lefevre, Maxence, Lichtenberg, Tim, Locci, Daniele, Lombini, Matteo, Lopez, Alejandro Sanchez, Lorenzani, Andrea, MacDonald, Ryan, Magrini, Laura, Maldonado, Jesus, Marcq, Emmanuel, Migliorini, Alessandra, Modirrousta-Galian, Darius, Molaverdikhani, Karan, Molinari, Sergio, Mollière, Paul, Moreau, Vincent, Morello, Giuseppe, Morinaud, Gilles, Morvan, Mario, Moses, Julianne I., Mouzali, Salima, Nakhjiri, Nariman, Naponiello, Luca, Narita, Norio, Nascimbeni, Valerio, Nikolaou, Athanasia, Noce, Vladimiro, Oliva, Fabrizio, Palladino, Pietro, Papageorgiou, Andreas, Parmentier, Vivien, Peres, Giovanni, Pérez, Javier, Perez-Hoyos, Santiago, Perger, Manuel, Pestellini, Cesare Cecchi, Petralia, Antonino, Philippon, Anne, Piccialli, Arianna, Pignatari, Marco, Piotto, Giampaolo, Podio, Linda, Polenta, Gianluca, Preti, Giampaolo, Pribulla, Theodor, Puertas, Manuel Lopez, Rainer, Monica, Reess, Jean-Michel, Rimmer, Paul, Robert, Séverine, Rosich, Albert, Rossi, Loic, Rust, Duncan, Saleh, Ayman, Sanna, Nicoletta, Schisano, Eugenio, Schreiber, Laura, Schwartz, Victor, Scippa, Antonio, Seli, Bálint, Shibata, Sho, Simpson, Caroline, Shorttle, Oliver, Skaf, N., Skup, Konrad, Sobiecki, Mateusz, Sousa, Sergio, Sozzetti, Alessandro, Šponer, Judit, Steiger, Lukas, Tanga, Paolo, Tackley, Paul, Taylor, Jake, Tecza, Matthias, Terenzi, Luca, Tremblin, Pascal, Tozzi, Andrea, Triaud, Amaury, Trompet, Loïc, Tsai, Shang-Min, Tsantaki, Maria, Valencia, Diana, Vandaele, Ann Carine, Van der Swaelmen, Mathieu, Vardan, Adibekyan, Vasisht, Gautam, Vazan, Allona, Del Vecchio, Ciro, Waltham, Dave, Wawer, Piotr, Widemann, Thomas, Wolkenberg, Paulina, Yip, Gordon Hou, Yung, Yuk, Zilinskas, Mantas, Zingales, Tiziano, and Zuppella, Paola
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Ariel, the Atmospheric Remote-sensing Infrared Exoplanet Large-survey, was adopted as the fourth medium-class mission in ESA's Cosmic Vision programme to be launched in 2029. During its 4-year mission, Ariel will study what exoplanets are made of, how they formed and how they evolve, by surveying a diverse sample of about 1000 extrasolar planets, simultaneously in visible and infrared wavelengths. It is the first mission dedicated to measuring the chemical composition and thermal structures of hundreds of transiting exoplanets, enabling planetary science far beyond the boundaries of the Solar System. The payload consists of an off-axis Cassegrain telescope (primary mirror 1100 mm x 730 mm ellipse) and two separate instruments (FGS and AIRS) covering simultaneously 0.5-7.8 micron spectral range. The satellite is best placed into an L2 orbit to maximise the thermal stability and the field of regard. The payload module is passively cooled via a series of V-Groove radiators; the detectors for the AIRS are the only items that require active cooling via an active Ne JT cooler. The Ariel payload is developed by a consortium of more than 50 institutes from 16 ESA countries, which include the UK, France, Italy, Belgium, Poland, Spain, Austria, Denmark, Ireland, Portugal, Czech Republic, Hungary, the Netherlands, Sweden, Norway, Estonia, and a NASA contribution., Comment: Ariel Definition Study Report, 147 pages. Reviewed by ESA Science Advisory Structure in November 2020. Original document available at: https://www.cosmos.esa.int/documents/1783156/3267291/Ariel_RedBook_Nov2020.pdf/
Published: 2021

3. Calibration of NOMAD on ESA's ExoMars Trace Gas Orbiter: Part 1 – The Solar Occultation channel

Author: Thomas, Ian R., Aoki, Shohei, Trompet, Loïc, Robert, Séverine, Depiesse, Cédric, Willame, Yannick, Erwin, Justin T., Vandaele, Ann Carine, Daerden, Frank, Mahieux, Arnaud, Neefs, Eddy, Ristic, Bojan, Hetey, Laszlo, Berkenbosch, Sophie, Clairquin, Roland, Beeckman, Bram, Patel, Manish R., Lopez-Moreno, Jose Juan, and Bellucci, Giancarlo
Published: 2022
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4. Calibration of the NOMAD-UVIS data

Author: Willame, Yannick, Depiesse, Cédric, Mason, Jonathon P., Thomas, Ian R., Patel, Manish R., Hathi, Brijen, Leese, Mark R., Bolsée, David, Wolff, Michael J., Trompet, Loïc, Vandaele, Ann Carine, Piccialli, Arianna, Aoki, Shohei, Ristic, Bojan, Neefs, Eddy, Beeckman, Bram, Berkenbosch, Sophie, Clairquin, Roland, Mahieux, Arnaud, Pereira, Nuno, Robert, Séverine, Viscardy, Sébastien, Wilquet, Valérie, Daerden, Frank, Lopez-Moreno, José Juan, and Bellucci, Giancarlo
Published: 2022
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5. Calibration of NOMAD on ESA's ExoMars Trace Gas Orbiter: Part 2 – The Limb, Nadir and Occultation (LNO) channel

Author: Thomas, Ian R., Aoki, Shohei, Trompet, Loïc, Robert, Séverine, Depiesse, Cédric, Willame, Yannick, Cruz-Mermy, Guillaume, Schmidt, Frédéric, Erwin, Justin T., Vandaele, Ann Carine, Daerden, Frank, Mahieux, Arnaud, Neefs, Eddy, Ristic, Bojan, Hetey, Laszlo, Berkenbosch, Sophie, Clairquin, Roland, Beeckman, Bram, Patel, Manish R., Lopez-Moreno, Jose Juan, and Bellucci, Giancarlo
Published: 2022
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6. Unexpected increase of the deuterium to hydrogen ratio in the Venus mesosphere.

Author: Mahieux, Arnaud, Viscardy, Sébastien, Yelle, Roger Vincent, Hiroki Karyu, Chamberlain, Sarah, Robert, Séverine, Piccialli, Arianna, Trompet, Loïc, Erwin, Justin Tyler, Ubukata, Soma, Hiromu Nakagawa, Shungo Koyama, Maggiolo, Romain, Pereira, Nuno, Cessateur, Gaël, Willame, Yannick, and Vandaele, Ann Carine
Abstract: This study analyzes H2O and HDO vertical profiles in the Venus mesosphere using Venus Express/Solar Occultation in the InfraRed data. The findings show increasing H2O and HDO volume mixing ratios with altitude, with the D/H ratio rising significantly from 0.025 at ~70 km to 0.24 at ~108 km. This indicates an increase from 162 to 1,519 times the Earth's ratio within 40 km. The study explores two hypotheses for these results: isotopic fractionation from photolysis of H2O over HDO or from phase change processes. The latter, involving condensation and evaporation of sulfuric acid aerosols, as suggested by previous authors [X. Zhang et al., Nat. Geosci. 3, 834-837 (2010)], aligns more closely with the rapid changes observed. Vertical transport computations for H2O, HDO, and aerosols show water vapor downwelling and aerosols upwelling. We propose a mechanism where aerosols form in the lower mesosphere due to temperatures below the water condensation threshold, leading to deuterium-enriched aerosols. These aerosols ascend, evaporate at higher temperatures, and release more HDO than H2O, which are then transported downward. Moreover, this cycle may explain the SO2 increase in the upper mesosphere observed above 80 km. The study highlights two crucial implications. First, altitude variation is critical to determining the Venus deuterium and hydrogen reservoirs. Second, the altitude-dependent increase of the D/H ratio affects H and D escape rates. The photolysis of H2O and HDO at higher altitudes releases more D, influencing long-term D/H evolution. These findings suggest that evolutionary models should incorporate altitude-dependent processes for accurate D/H fractionation predictions. [ABSTRACT FROM AUTHOR]
Published: 2024
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7. The Climatology of Mars Thermospheric Polar Warming at Aphelion

Author: Thiemann, Edward M. B., primary, Trompet, Loïc, additional, Bougher, Stephen W., additional, Yiğit, Erdal, additional, Gasperini, Federico, additional, Montabone, Luca, additional, Gonzalez‐Galindo, Francisco, additional, Eparvier, Francis G., additional, and Vandaele, Anne‐Carine, additional
Published: 2024
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8. Comprehensive investigation of Mars methane and organics with ExoMars/NOMAD

Author: Knutsen, Elise W., Villanueva, Geronimo L., Liuzzi, Giuliano, Crismani, Matteo M.J., Mumma, Michael J., Smith, Michael D., Vandaele, Ann Carine, Aoki, Shohei, Thomas, Ian R., Daerden, Frank, Viscardy, Sébastien, Erwin, Justin T., Trompet, Loic, Neary, Lori, Ristic, Bojan, Lopez-Valverde, Miguel Angel, Lopez-Moreno, Jose Juan, Patel, Manish R., Karatekin, Ozgur, and Bellucci, Giancarlo
Published: 2021
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9. On the plausibility of methane detections on Mars in the light of the ExoMars/TGO results

Author: Viscardy, Sébastien, Robert, Séverine, Erwin, Justin, Thomas, Ian R., Daerden, Frank, Neary, Lori, Piccialli, Arianna, Trompet, Loïc, Willame, Yannick, and Vandaele, Ann Carine
Abstract: As a potential biomarker, Martian methane has attracted attention through several reports of its detection over the last 20 years. However, the very existence of this gas has been continuously questioned, in particular, because the observed lifetime should be several orders of magnitude shorter than the 300 years predicted by photochemical models. Although several fast removal processes have been hypothesized to explain the observations, none of them has met a large consensus.It is in this context that the ESA-Roscomos ExoMars Trace Gas Orbiter (TGO) mission started its science operations in April 2018. ACS and NOMAD, two instruments onboard the TGO, have been collecting hundreds of highly sensitive measurements in solar occultation. No methane has been detected so far and an upper limit of 0.02 ppbv has been derived.The implications of this result on the methane problem on Mars will be addressed in this work.This upper limit is a strong constraint on the background level and, in turn, on the potential emission scenarios making the reported methane detections consistent with the TGO results. While several model studies aimed at identifying them, we will here adopt a probabilistic approach to the problem in order to question the plausibility of those detections and estimate the lifetime required to make them plausible from a probabilistic standpoint., The 28th IUGG General Assembly (IUGG2023) (Berlin 2023)
Published: 2023

10. Correlations between minor species in the Venus mesosphere from the SOIR/Venus Express spectrograph

Author: Mahieux, Arnaud, primary, Yangambi Libote, Aaron, additional, Robert, Séverine, additional, Piccialli, Ariana, additional, Trompet, Loïc, additional, and Vandaele, Ann Carine, additional
Published: 2023
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11. On the plausibility of methane detections on Mars

Author: Viscardy, Sébastien, primary, Robert, Séverine, additional, Erwin, Justin T., additional, Thomas, Ian R., additional, Daerden, Frank, additional, Neary, Lori, additional, Piccialli, Arianna, additional, Trompet, Loïc, additional, Willame, Yannick, additional, and Vandaele, Ann Carine, additional
Published: 2023
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12. Minor species in the Venus mesosphere from SOIR on board Venus Express: detection and upper limit profiles of H2CO, O3, NH3, HCN, N2O, NO2, and HO2

Author: Mahieux, Arnaud, primary, Robert, Séverine, additional, Mills, Frank, additional, Trompet, Loïc, additional, Aoki, Shohei, additional, Piccialli, Arianna, additional, Jessup, Kandis Lea, additional, and Vandaele, Ann Carine, additional
Published: 2022
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13. CO distributions retrieved from TGO NOMAD SO using multiple orders

Author: Yoshida, Nao, primary, Aoki, Shohei, additional, Vandaele, Ann Carine, additional, Nakagawa, Hiromu, additional, Thomas, Ian, additional, Erwin, Justin, additional, Daerden, Frank, additional, Trompet, Loïc, additional, Murata, Isao, additional, Terada, Naoki, additional, Neary, Lori, additional, Lopez-Valverde, Miguel, additional, Modak, Ashimananda, additional, Villanueva, Geronimo, additional, Liuzzi, Giuliano, additional, Kasaba, Yasumasa, additional, Patel, Manish, additional, Ristic, Bojan, additional, Bellucci, Giancarlo, additional, and López-Moreno, Jusé Juan, additional
Published: 2022
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14. Mesospheric and thermospheric carbon dioxide and temperature profiles from NOMAD-SO onboard TGO.

Author: Trompet, Loïc, primary, Vandaele, Ann Carine, additional, Thomas, Ian, additional, Aoki, Shohei, additional, Daerden, Frank, additional, Erwin, Justin, additional, Flimon, Zachary, additional, Neary, Lori, additional, Mahieux, Arnaud, additional, Robert, Séverine, additional, Villanueva, Geronimo, additional, Liuzzi, Giuliano, additional, Lopez-Valverde, Miguel Angel, additional, Brines, Adrian, additional, Bellucci, Giancarlo, additional, Lopez-Moreno, José Juan, additional, and Patel, Manish, additional
Published: 2022
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15. Two Martian years at Mars: Observations by NOMAD on ExoMars Trace Gas Orbiter

Author: Vandaele, Ann Carine, primary, Daerden, Frank, additional, Thomas, Ian R., additional, Depiesse, Cédric, additional, Erwin, Justin, additional, Flimon, Zachary, additional, Neary, Lori, additional, Piccialli, Arianna, additional, Ristic, Bojan, additional, Trompet, Loïc, additional, Viscardy, Sébastien, additional, Willame, Yannick, additional, Aoki, Shohei, additional, Gérard, Jean-Claude, additional, Villanueva, Geronimo, additional, Mason, Jon, additional, Patel, Manish, additional, Bellucci, Giancarlo, additional, Lopez-Valverde, Miguel, additional, and Lopez-Moreno, Jose Juan, additional
Published: 2022
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16. RoadMap to understand the role of dust in the atmosphere of Mars

Author: Vandaele, Ann Carine, primary, Merrison, Jon, additional, Wurm, Gerhard, additional, Munoz, Olga, additional, Jardiel, Teresa, additional, Lindqvist, Hannakaisa, additional, Wolff, Mike, additional, Neary, Lori, additional, Willame, Yannick, additional, Piccialli, Arianna, additional, Trompet, Loïc, additional, Flimon, Zachary, additional, Abesha, Andebo, additional, Becker, Tim, additional, Martikainen, Julia, additional, Gomez-Martin, Juan Carlos, additional, and Peiteado, Marco, additional
Published: 2022
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17. Ozone in the Martian atmosphere observed by TGO/NOMAD-UVIS solar occultations

Author: Piccialli, Arianna, primary, Vandaele, Ann Carine, additional, Willame, Yannick, additional, Määttänen, Anni, additional, Trompet, Loïc, additional, Erwin, Justin, additional, Daerden, Frank, additional, Neary, Lori, additional, Aoki, Shohei, additional, Viscardy, Sébastien, additional, Thomas, Ian, additional, Depiesse, Cedric, additional, Ristic, Bojan, additional, Mason, Jon, additional, Patel, Manish, additional, Wolff, Michael, additional, Khayat, Alain, additional, Bellucci, Giancarlo, additional, and Lopez-Moreno, Jose Juan, additional
Published: 2022
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18. Measuring the 13C/12C in the lower atmosphere of Mars with NOMAD/TGO: challenges and interpretation

Author: Liuzzi, Giuliano, primary, Villanueva, Geronimo, additional, Stone, Shane W., additional, Faggi, Sara, additional, Kofman, Vincent, additional, Aoki, Shohei, additional, Alday, Juan, additional, Trompet, Loïc, additional, and Vandaele, Ann Carine, additional
Published: 2022
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19. Mars water vapor vertical distributions from the troposphere to the mesosphere from NOMAD Solar Occultation for Martian Years 34 and 35

Author: Brines, Adrian, primary, Lopez Valverde, Miguel Ángel, additional, Stolzenbach, Aurélien, additional, Modak, Ashim, additional, Funke, Bernd, additional, Gonzalez Galindo, Francisco, additional, Lopez Moreno, Jose Juan, additional, Aoki, Shohei, additional, Vandaele, Ann Carine, additional, Daerden, Frank, additional, Thomas, Ian, additional, Erwin, Justin, additional, Trompet, Loïc, additional, Ristic, Bojan, additional, Villanueva, Gerónimo Luis, additional, Liuzzi, Giuliano, additional, Patel, Manish, additional, and Bellucci, Giancarlo, additional
Published: 2022
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20. GEM-Mars GCM products and tools available through the VESPA portal.

Author: Trompet, Loïc, primary, Daerden, Frank, additional, Neary, Lori, additional, Erwin, Justin, additional, Vandaele, Ann Carine, additional, and Erard, Stéphane, additional
Published: 2022
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21. Variations in Vertical CO/CO2 Profiles in the Martian Mesosphere and Lower Thermosphere Measured by the ExoMars TGO/NOMAD: Implications of Variations in Eddy Diffusion Coefficient

Author: Yoshida, Nao, Nakagawa, Hiromu, Aoki, Shohei, Erwin, Justin, Vandaele, Ann Carine, Daerden, Frank, Thomas, Ian, Trompet, Loïc, Koyama, Shungo, Terada, Naoki, Neary, Lori, Murata, Isao, Villanueva, Geronimo, Liuzzi, Giuliano, Lopez‐Valverde, Miguel Angel, Brines, Adrian, Modak, Ashimananda, Kasaba, Yasumasa, Ristic, Bojan, Bellucci, Giancarlo, López‐Moreno, José Juan, Patel, Manish, Ministerio de Ciencia e Innovación (España), European Commission, Belgian Science Policy Office, UK Space Agency, and Agenzia Spaziale Italiana
Subjects: Geophysics, Retrieval, Atmospheric composition, General Earth and Planetary Sciences, Mars, Eddy diffusion coefficient, Spectroscopy, Mesosphere
Abstract: This is an open access article under the terms of the Creative Commons Attribution License, which permits use, distribution and reproduction in any medium, provided the original work is properly cited., Using the Nadir and Occultation for MArs Discovery instrument aboard Trace Gas Orbiter, we derived the CO/CO2 profiles between 75 and 105 km altitude with the equivalent width technique. The derived CO/CO2 profiles showed significant seasonal variations in the southern hemisphere with decreases near perihelion and increases near aphelion. The estimation of the CO/CO2 profiles with a one-dimensional photochemical model shows that an altitude-dependent eddy diffusion coefficient better reproduces the observed profiles than a vertically uniform one. Our estimation suggests that the eddy diffusion coefficient in Ls = 240–270 is uniformly larger by a factor of ∼2 than that in Ls = 90–120 in the southern hemisphere, while they are comparable in the northern hemisphere. This fact demonstrates that the eddy diffusion coefficient is variable with season and latitude. © 2022. The Authors., The NOMAD experiment is led by the Royal Belgian Institute for Space Aeronomy (IASB-BIRA), 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 (BELSPO), with the financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493), by Spanish Ministry of Science and Innovation (MCIU) 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/V002295/1, ST/V005332/1, and ST/S00145x/1 and Italian Space Agency through Grant 2018-2-HH.0. This work was supported by the Belgian Fonds de la Recherche Scientifique–FNRS under Grant No. 30442502 (ET_HOME). 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 Astrofísica de Andalucía (SEV-2017-0709). US investigators were supported by the National Aeronautics and Space Administration. Canadian investigators were supported by the Canadian Space Agency. Y. N. is supported by The international Joint Graduate Program in Earth and Environmental Sciences, Tohoku University (GP-EES), and the Japanese Society for the Promotion of Science (JP21J13710). This work was supported by JSPS KAKENHI Grant Nos. 20H04605 and 19K03943.
Published: 2022

22. Variations in Vertical CO/CO 2 Profiles in the Martian Mesosphere and Lower Thermosphere Measured by the ExoMars TGO/NOMAD: Implications of Variations in Eddy Diffusion Coefficient

Author: Yoshida, Nao, primary, Nakagawa, Hiromu, additional, Aoki, Shohei, additional, Erwin, Justin, additional, Vandaele, Ann Carine, additional, Daerden, Frank, additional, Thomas, Ian, additional, Trompet, Loïc, additional, Koyama, Shungo, additional, Terada, Naoki, additional, Neary, Lori, additional, Murata, Isao, additional, Villanueva, Geronimo, additional, Liuzzi, Giuliano, additional, Lopez‐Valverde, Miguel Angel, additional, Brines, Adrian, additional, Modak, Ashimananda, additional, Kasaba, Yasumasa, additional, Ristic, Bojan, additional, Bellucci, Giancarlo, additional, López‐Moreno, José Juan, additional, and Patel, Manish, additional
Published: 2022
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23. Publisher Correction: No detection of methane on Mars from early ExoMars Trace Gas Orbiter observations

Author: Korablev, Oleg, Vandaele, Ann Carine, Montmessin, Franck, Fedorova, Anna A., Trokhimovskiy, Alexander, Forget, François, Lefèvre, Franck, Daerden, Frank, Thomas, Ian R., Trompet, Loïc, Erwin, Justin T., Aoki, Shohei, Robert, Séverine, Neary, Lori, Viscardy, Sébastien, Grigoriev, Alexey V., Ignatiev, Nikolay I., Shakun, Alexey, Patrakeev, Andrey, Belyaev, Denis A., Bertaux, Jean-Loup, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Ivanov, Yuriy S., Ristic, Bojan, Mason, Jon, Willame, Yannick, Depiesse, Cédric, Hetey, Laszlo, Berkenbosch, Sophie, Clairquin, Roland, Queirolo, Claudio, Beeckman, Bram, Neefs, Eddy, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, Jose-Juan, Wilson, Colin F., Etiope, Giuseppe, Zelenyi, Lev, Svedhem, Håkan, Vago, Jorge L., and The ACS and NOMAD Science Teams
Published: 2019
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24. Publisher Correction: Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

Author: Vandaele, Ann Carine, Korablev, Oleg, Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, Francesca, López-Valverde, Miguel, Villanueva, Geronimo, Liuzzi, Giuliano, Smith, Michael D., Erwin, Justin T., Trompet, Loïc, Fedorova, Anna A., Montmessin, Franck, Trokhimovskiy, Alexander, Belyaev, Denis A., Ignatiev, Nikolay I., Luginin, Mikhail, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Bertaux, Jean-Loup, Betsis, Daria, Bolsée, David, Clancy, R. Todd, Cloutis, Edward, Depiesse, Cédric, Funke, Bernd, Garcia-Comas, Maia, Gérard, Jean-Claude, Giuranna, Marco, Gonzalez-Galindo, Francisco, Grigoriev, Alexey V., Ivanov, Yuriy S., Kaminski, Jacek, Karatekin, Ozgur, Lefèvre, Franck, Lewis, Stephen, López-Puertas, Manuel, Mahieux, Arnaud, Maslov, Igor, Mason, Jon, Mumma, Michael J., Neary, Lori, Neefs, Eddy, Patrakeev, Andrey, Patsaev, Dmitry, Ristic, Bojan, Robert, Séverine, Schmidt, Frédéric, Shakun, Alexey, Teanby, Nicholas A., Viscardy, Sébastien, Willame, Yannick, Whiteway, James, Wilquet, Valérie, Wolff, Michael J., Bellucci, Giancarlo, Patel, Manish R., López-Moreno, Jose-Juan, Forget, François, Wilson, Colin F., Young, Roland, Svedhem, Håkan, Vago, Jorge L., Rodionov, Daniel, NOMAD Science Team, and ACS Science Team
Published: 2019
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25. SO2, SO3, OCS, H2S, and other trace gases in the Venus mesosphere from SOIR on board Venus Express: Detection and upper limit profiles

Author: Mahieux, Arnaud, primary, Robert, Séverine, additional, Mills, Frank, additional, Trompet, Loïc, additional, Aoki, Shohei, additional, Piccialli, Arianna, additional, Jessup, Kandis Lea, additional, and Vandaele, Ann Carine, additional
Published: 2022
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26. First Detection and Thermal Characterization of Terminator CO 2 Ice Clouds With ExoMars/NOMAD

Author: Liuzzi, Giuliano, primary, Villanueva, Geronimo L., additional, Trompet, Loïc, additional, Crismani, Matteo M. J., additional, Piccialli, Arianna, additional, Aoki, Shohei, additional, Lopez‐Valverde, Miguel Angel, additional, Stolzenbach, Aurélien, additional, Daerden, Frank, additional, Neary, Lori, additional, Smith, Michael D., additional, Patel, Manish R., additional, Lewis, Stephen R., additional, Clancy, R. Todd, additional, Thomas, Ian R., additional, Ristic, Bojan, additional, Bellucci, Giancarlo, additional, Lopez‐Moreno, Jose‐Juan, additional, and Vandaele, Ann Carine, additional
Published: 2021
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27. Martian water vapor vertical profiles from solar occultation measurements by NOMAD onboard TGO/ExoMars: H2O-Temperature retrievals with the IAA-KOPRA forward model

Author: Brines, Adrian, primary, Lopez-Valverde, Miguel Angel, additional, Stolzenbach, Aurélien, additional, Modak, Ashimananda, additional, Hill, Brittany, additional, Funke, Bernd, additional, González-Galindo, Francisco, additional, Lopez Moreno, Jose Juan, additional, Aoki, Shohei, additional, Vandaele, Ann Carine, additional, Daerden, Frank, additional, Thomas, Ian, additional, Erwin, Justin, additional, Trompet, Loïc, additional, Ristic, Bojan, additional, Villanueva, Gerónimo, additional, Liuzzi, Giuliano, additional, Patel, Manish, additional, and Bellucci, Giancarlo, additional
Published: 2021
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28. The Martian environment observed by NOMAD on ExoMars Trace Gas Orbiter

Author: Vandaele, Ann Carine, primary, Daerden, Frank, additional, Thomas, Ian R., additional, Aoki, Shohei, additional, Depiesse, Cédric, additional, Erwin, Justin, additional, Neary, Lori, additional, Piccialli, Arianna, additional, Ristic, Bojan, additional, Robert, Séverine, additional, Trompet, Loïc, additional, Viscardy, Sébastien, additional, Willame, Yannick, additional, Gérard, Jean-Claude, additional, Villanueva, Geronimo, additional, Mason, Jon, additional, Patel, Manish, additional, Bellucci, Giancarlo, additional, Lopez-Valverde, Miguel, additional, and Lopez-Moreno, Jose-Juan, additional
Published: 2021
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29. Probing the Atmospheric Cl Isotopic Ratio on Mars: Implications for Planetary Evolution and Atmospheric Chemistry

Author: Liuzzi, Giuliano, primary, Villanueva, Geronimo L., additional, Viscardy, Sebastien, additional, Mège, Daniel, additional, Crismani, Matteo M. J., additional, Aoki, Shohei, additional, Gurgurewicz, Joanna, additional, Tesson, Pierre‐Antoine, additional, Mumma, Michael J., additional, Smith, Michael D., additional, Faggi, Sara, additional, Kofman, Vincent, additional, Knutsen, Elise W., additional, Daerden, Frank, additional, Neary, Lori, additional, Schmidt, Frédéric, additional, Trompet, Loïc, additional, Erwin, Justin T., additional, Robert, Séverine, additional, Thomas, Ian R., additional, Ristic, Bojan, additional, Bellucci, Giancarlo, additional, Lopez‐Moreno, Jóse Juan, additional, Patel, Manish R., additional, and Vandaele, Ann Carine, additional
Published: 2021
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30. Variations in Vertical CO/CO2 Profiles in the Martian Mesosphere and Lower Thermosphere Measured by the ExoMars TGO/NOMAD: Implications of Variations in Eddy Diffusion Coefficient.

Author: Yoshida, Nao, Nakagawa, Hiromu, Aoki, Shohei, Erwin, Justin, Vandaele, Ann Carine, Daerden, Frank, Thomas, Ian, Trompet, Loïc, Koyama, Shungo, Terada, Naoki, Neary, Lori, Murata, Isao, Villanueva, Geronimo, Liuzzi, Giuliano, Lopez‐Valverde, Miguel Angel, Brines, Adrian, Modak, Ashimananda, Kasaba, Yasumasa, Ristic, Bojan, and Bellucci, Giancarlo
Subjects: DIFFUSION coefficients, MESOSPHERE, TRACE gases, THERMOSPHERE, MIDDLE atmosphere, EDDIES
Abstract: Using the Nadir and Occultation for MArs Discovery instrument aboard Trace Gas Orbiter, we derived the CO/CO2 profiles between 75 and 105 km altitude with the equivalent width technique. The derived CO/CO2 profiles showed significant seasonal variations in the southern hemisphere with decreases near perihelion and increases near aphelion. The estimation of the CO/CO2 profiles with a one‐dimensional photochemical model shows that an altitude‐dependent eddy diffusion coefficient better reproduces the observed profiles than a vertically uniform one. Our estimation suggests that the eddy diffusion coefficient in Ls = 240–270 is uniformly larger by a factor of ∼2 than that in Ls = 90–120 in the southern hemisphere, while they are comparable in the northern hemisphere. This fact demonstrates that the eddy diffusion coefficient is variable with season and latitude. Plain Language Summary: The eddy diffusion coefficient is widely used to parameterize the efficiency of vertical diffusion in the planetary atmosphere, whose variation characterizes the transportation of trace gas species. Additionally, it could vary their vertical distributions in the middle and upper atmosphere, which might cause an impact on the species escaping to space. However, the variability of the eddy diffusion coefficient in those altitude regions have been poorly understood. In this study, we focus on the estimation of variation in the eddy diffusion coefficient by analyzing the CO and CO2 measurements made by the ExoMars Trace Gas Orbiter. The observed CO/CO2 ratio between altitudes of 75 and 105 km shows a significant seasonal variation in the southern hemisphere. The observed CO/CO2 profiles are compared with the simulated profiles obtained with a one‐dimensional photochemical model assigning several shapes and intensity of eddy diffusion coefficient. The comparison shows that the eddy diffusion coefficient is not constant but variable depending on altitude, season, and latitude, which suggests that the efficiency of the vertical diffusion varies with season and latitude. This fact is useful to other 1D photochemical models to reproduce the seasonal and latitudinal variation of atmospheric composition. Key Points: The CO/CO2 profiles from 75 to 105 km measured by NOMAD aboard TGO are used to investigate variations in the eddy diffusion coefficientThe estimated CO/CO2 profiles agree well with the observed profiles if altitude‐dependent eddy diffusion coefficients are consideredOur results demonstrate a substantial seasonal variation in the eddy diffusion coefficient in the southern hemisphere [ABSTRACT FROM AUTHOR]
Published: 2022
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31. 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, Loïc, Robert, S., Neary, Lori, Viscardy, Sébastien, Clancy, Todd, Smith, Michael D., López-Valverde, Miguel, Hill, B., Ristic, Bojan, Patel, Manish R., Bellucci, Giancarlo, López-Moreno, Jose-Juan, Alonso-Rodrigo, G., Altieri, F., Bauduin, Sophie, and Bolsée, D.
Subjects: Sciences de la terre et du cosmos, Aéronomie, Télédétection, Système solaire, Sciences exactes et naturelles
Abstract: 0, info:eu-repo/semantics/published
Published: 2019

32. NOMAD on ExoMars Trace Gas Orbiter: One Martian year of observations

Author: Vandaele, Ann Carine, primary, Daerden, Frank, additional, Thomas, Ian R., additional, Aoki, Shohei, additional, Depiesse, Cédric, additional, Erwin, Justin, additional, Neary, Lori, additional, Piccialli, Arianna, additional, Ristic, Bojan, additional, Robert, Séverine, additional, Trompet, Loïc, additional, Viscardy, Sébastien, additional, Willame, Yannick, additional, Mason, Jon, additional, Patel, Manish, additional, Bellucci, Giancarlo, additional, and Lopez-Moreno, Jose-Juan, additional
Published: 2020
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33. Martian Atmosphere CO Vertical Profiles: Results from the First Year of TGO/NOMAD Science Operations

Author: Erwin, Justin, primary, Aoki, Shohei, additional, Thomas, Ian, additional, Trompet, Loïc, additional, Vandaele, Ann Carine, additional, Robert, Séverine, additional, Daerden, Frank, additional, Ristic, Bojan, additional, Lopez-Moreno, Jose Juan, additional, Bellucci, Giancarlo, additional, and Patel, Manish, additional
Published: 2020
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34. Update on CO2 and temperature profiles from NOMAD-SO on board ExoMars TGO

Author: Trompet, Loïc, primary, Vandaele, Ann Carine, additional, Aoki, Shohei, additional, Erwin, Justin, additional, Thomas, Ian, additional, Villanueva, Geronimo, additional, Liuzzi, Giulliano, additional, Crismani, Matteo, additional, Lopez-Valverde, Miguel Angel, additional, Hill, Brittany, additional, Piccialli, Arianna, additional, Daerden, Frank, additional, Ristic, Bojan, additional, Lopez-Moreno, Juan Jose, additional, Bellucci, Giancarlo, additional, and Patel, Manish, additional
Published: 2020
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35. First Detection and Thermal Characterization of Terminator CO2 Ice Clouds With ExoMars/NOMAD.

Author: Liuzzi, Giuliano, Villanueva, Geronimo L., Trompet, Loïc, Crismani, Matteo M. J., Piccialli, Arianna, Aoki, Shohei, Lopez‐Valverde, Miguel Angel, Stolzenbach, Aurélien, Daerden, Frank, Neary, Lori, Smith, Michael D., Patel, Manish R., Lewis, Stephen R., Clancy, R. Todd, Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Lopez‐Moreno, Jose‐Juan, and Vandaele, Ann Carine
Subjects: ICE clouds, TRACE gases, MARTIAN atmosphere, ICE nuclei, UPPER atmosphere, FREEZING points
Abstract: We present observations of terminator CO2 ice clouds events in three groups: Equatorial dawn, Equatorial dusk (both between 20°S and 20°N) and Southern midlatitudes at dawn (45°S and 55°S east of Hellas Basin) with ESA ExoMars Trace Gas Orbiter's Nadir and Occultation for MArs Discovery instrument. CO2 ice abundance is retrieved simultaneously with water ice, dust, and particle sizes, and rotational temperature and CO2 column profiles in 16 of 26 cases. Small particles (<0.5 μm) prevail at dusk, while water ice likely provides most source nuclei at dawn. Clouds east of Hellas are found to be dominantly nucleated on surface‐lifted dust. CO2 ice is sometimes detected in unsaturated air together with dust nuclei at dawn, suggesting ongoing sublimation. Depending on latitude and local time, the interplay between particle precipitation and the lifetime of temperature minima (i.e., cold pockets) determines CO2 ice properties. Plain Language Summary: The upper atmosphere of Mars is characterized by the seasonal presence of CO2 ice clouds. Their properties have been long studied, as well as their formation mechanisms in relation to the thermal structure of the atmosphere and its variability. In this study, we present the first observations of these clouds at the terminator (dawn and dusk) by the NOMAD spectrometer onboard the Exomars Trace Gas Orbiter. CO2 ice is detected simultaneously with dust, water ice and the temperature profile. Our results agree with previous findings in terms of how clouds are spatially distributed and their temporal occurrence. However, we also explore the sources of condensation nuclei for CO2 ice particles, showing that water ice is a possible source at dawn near the Equator. We also identify surface‐lifted dust below the CO2 ice clouds observed east of Hellas Basin, suggesting that, at that location, dust could provide nuclei for CO2 ice. CO2 ice is also sometimes detected at temperatures higher than the CO2 freezing point, suggesting ongoing sublimation. In this work we explore for the first time the composition of CO2 ice clouds, which is critical to advance our understanding of how CO2 ice clouds form in the mesosphere at Mars. Key Points: Twenty Six mesospheric CO2 ice clouds were detected with NOMAD SO in Mars Year 35, simultaneously with water ice, dust, and CO2 saturation ratiosEquatorial CO2 clouds are observed at 50–80 km altitude at dusk, and 40–60 km at dawn, when water ice likely provides condensation nucleiSix CO2 ice clouds are found east of Hellas basin; their formation is likely sourced by surface‐lifted dust at 40–65 km [ABSTRACT FROM AUTHOR]
Published: 2021
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36. Martian dust storm impact on atmospheric H2O and D/H observed by ExoMars Trace Gas Orbiter

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

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

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

38. The SPICAV-SOIR instrument probing the atmosphere of Venus: an overview

Author: Trompet, Loïc, Mahieux, Arnaud, Wilquet, Valérie, Robert, Séverine, Chamberlain, Sarah, Thomas, Ian, Vandaele, Ann Carine, Bertaux, Jean-Loup, Belgian Institute for Space Aeronomy / Institut d'Aéronomie Spatiale de Belgique (BIRA-IASB), Fonds National de la Recherche Scientifique [Bruxelles] (FNRS), 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.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: International audience; The Solar Occultation in the Infrared (SOIR) channel mounted on top of the SPICAV instrument of the ESA’s Venus Express mission has observed the atmosphere of Venus during more than eight years. This IR spectrometer (2.2-4.3 μm) with a high spectral resolution (0.12 cm-1) combined an echelle grating with an acousto-optic tunable filter for order selection. SOIR performed more than 1500 solar occultation measurements leading to about two millions spectra.The Royal Belgian Institute for Space Aeronomy (BIRA-IASB) was in charge of SOIR’s development and opera- tions as well as its data pipeline. BIRA-IASB carried out several studies on the composition of Venus mesosphere and lower thermosphere: carbon dioxide, carbon monoxide, hydrogen halide (HF, HCl, DF, DCl), sulfur dioxide, water (H2O, HDO) as well as sulphuric acid aerosols in the upper haze of Venus. Density and temperature profiles of the upper atmosphere of Venus (60 km to 170 km) at the terminator have been retrieved from SOIR’s spectra using different assumptions, wherein the hydrostatic equilibrium and the local thermodynamical equilibrium in the radiative transfer calculations. These results allow us to produce an Atmospheric model of Venus called Venus Atmosphere from SOIR measurements at the Terminator (VAST). Data obtained by SOIR will also contribute to update the Venus International Reference Atmosphere (VIRA).Recently, the treatment of the raw data to transmittance has been optimized, and a new dataset of spectra has been produced. All raw spectra (PSA level 2) as well as calibrated spectra (PSA level 3) have been delivered to ESA’s Planetary Science Archive (PDSPSA). Consequently the re-analysis of all spectra has been undergone.We will briefly present the improvements implemented in the data pipeline. We will also show a compilation of results obtained by the instrument considering the complete mission duration.
Published: 2016

39. Neutral composition of the Venus atmosphere measured by SPICAV/SOIR on board VENUS EXPRESS: A compendium

Author: Vandaele, Ann Carine, Mahieux, Arnaud, Wilquet, Valérie, Chamberlain, Sarah, Ristic, Bojan, Robert, Séverine, Thomas, Ian R., Trompet, Loïc, 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), Belgian Federal Science Policy Office and the European Space Agency, Belgian government (Planet TOPERS), HiResMIR International Scientific Coordination Network (GDRI), European Project: 606798,EC:FP7:SPA,FP7-SPACE-2013-1,EUROVENUS(2013), Cardon, Catherine, and European Unified Research on Observations of Venus using co-ordinated Space- and Earth-based facilities - EUROVENUS - - EC:FP7:SPA2013-10-01 - 2016-10-01 - 606798 - VALID
Subjects: [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]
Abstract: International audience; The Solar Occultation in the In-frared (SOIR) instrument on-board Venus Express is an infrared spectrometer covering the 2.2-4.3 µm spectral region. This instrument allows the detection of several key species of the Venus atmosphere, including CO2, CO, H2O/HDO, HCl, HF and SO2. From the CO2 density measurements, temperature is inferred giving information on the thermal structure of the atmosphere. Here we described the kind of data (profiles, latitudinal average, etc.) that have been obtained during the complete duration of the mission.
Published: 2016

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

Author: Vandaele, Ann Carine, Korablev, Oleg, Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, Francesca, López-Valverde, Miguel, Villanueva, Geronimo, Liuzzi, Giuliano, Smith, Michael D., Erwin, Justin T., Trompet, Loïc, Fedorova, Anna A., Montmessin, Franck, Trokhimovskiy, Alexander, Belyaev, Denis A., Ignatiev, Nikolay I., Luginin, Mikhail, Olsen, Kevin S., and Baggio, Lucio
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. High-resolution measurements of Martian atmospheric dust, water and semiheavy water, obtained by the ExoMars Trace Gas Orbiter during a global dust storm on Mars, are reported. [ABSTRACT FROM AUTHOR]
Published: 2019
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41. Variations in Vertical CO/CO2Profiles in the Martian Mesosphere and Lower Thermosphere Measured by the ExoMars TGO/NOMAD: Implications of Variations in Eddy Diffusion Coefficient

Author: Yoshida, Nao, Nakagawa, Hiromu, Aoki, Shohei, Erwin, Justin, Vandaele, Ann Carine, Daerden, Frank, Thomas, Ian, Trompet, Loïc, Koyama, Shungo, Terada, Naoki, Neary, Lori, Murata, Isao, Villanueva, Geronimo, Liuzzi, Giuliano, Lopez‐Valverde, Miguel Angel, Brines, Adrian, Modak, Ashimananda, Kasaba, Yasumasa, Ristic, Bojan, Bellucci, Giancarlo, López‐Moreno, José Juan, and Patel, Manish
Abstract: Using the Nadir and Occultation for MArs Discovery instrument aboard Trace Gas Orbiter, we derived the CO/CO2profiles between 75 and 105 km altitude with the equivalent width technique. The derived CO/CO2profiles showed significant seasonal variations in the southern hemisphere with decreases near perihelion and increases near aphelion. The estimation of the CO/CO2profiles with a one‐dimensional photochemical model shows that an altitude‐dependent eddy diffusion coefficient better reproduces the observed profiles than a vertically uniform one. Our estimation suggests that the eddy diffusion coefficient in Ls= 240–270 is uniformly larger by a factor of ∼2 than that in Ls= 90–120 in the southern hemisphere, while they are comparable in the northern hemisphere. This fact demonstrates that the eddy diffusion coefficient is variable with season and latitude. The eddy diffusion coefficient is widely used to parameterize the efficiency of vertical diffusion in the planetary atmosphere, whose variation characterizes the transportation of trace gas species. Additionally, it could vary their vertical distributions in the middle and upper atmosphere, which might cause an impact on the species escaping to space. However, the variability of the eddy diffusion coefficient in those altitude regions have been poorly understood. In this study, we focus on the estimation of variation in the eddy diffusion coefficient by analyzing the CO and CO2measurements made by the ExoMars Trace Gas Orbiter. The observed CO/CO2ratio between altitudes of 75 and 105 km shows a significant seasonal variation in the southern hemisphere. The observed CO/CO2profiles are compared with the simulated profiles obtained with a one‐dimensional photochemical model assigning several shapes and intensity of eddy diffusion coefficient. The comparison shows that the eddy diffusion coefficient is not constant but variable depending on altitude, season, and latitude, which suggests that the efficiency of the vertical diffusion varies with season and latitude. This fact is useful to other 1D photochemical models to reproduce the seasonal and latitudinal variation of atmospheric composition. The CO/CO2profiles from 75 to 105 km measured by NOMAD aboard TGO are used to investigate variations in the eddy diffusion coefficientThe estimated CO/CO2profiles agree well with the observed profiles if altitude‐dependent eddy diffusion coefficients are consideredOur results demonstrate a substantial seasonal variation in the eddy diffusion coefficient in the southern hemisphere The CO/CO2profiles from 75 to 105 km measured by NOMAD aboard TGO are used to investigate variations in the eddy diffusion coefficient The estimated CO/CO2profiles agree well with the observed profiles if altitude‐dependent eddy diffusion coefficients are considered Our results demonstrate a substantial seasonal variation in the eddy diffusion coefficient in the southern hemisphere
Published: 2022
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42. First Detection and Thermal Characterization of Terminator CO2Ice Clouds With ExoMars/NOMAD

Author: Liuzzi, Giuliano, Villanueva, Geronimo L., Trompet, Loïc, Crismani, Matteo M. J., Piccialli, Arianna, Aoki, Shohei, Lopez‐Valverde, Miguel Angel, Stolzenbach, Aurélien, Daerden, Frank, Neary, Lori, Smith, Michael D., Patel, Manish R., Lewis, Stephen R., Clancy, R. Todd, Thomas, Ian R., Ristic, Bojan, Bellucci, Giancarlo, Lopez‐Moreno, Jose‐Juan, and Vandaele, Ann Carine
Abstract: We present observations of terminator CO2ice clouds events in three groups: Equatorial dawn, Equatorial dusk (both between 20°S and 20°N) and Southern midlatitudes at dawn (45°S and 55°S east of Hellas Basin) with ESA ExoMars Trace Gas Orbiter's Nadir and Occultation for MArs Discovery instrument. CO2ice abundance is retrieved simultaneously with water ice, dust, and particle sizes, and rotational temperature and CO2column profiles in 16 of 26 cases. Small particles (<0.5 μm) prevail at dusk, while water ice likely provides most source nuclei at dawn. Clouds east of Hellas are found to be dominantly nucleated on surface‐lifted dust. CO2ice is sometimes detected in unsaturated air together with dust nuclei at dawn, suggesting ongoing sublimation. Depending on latitude and local time, the interplay between particle precipitation and the lifetime of temperature minima (i.e., cold pockets) determines CO2ice properties. The upper atmosphere of Mars is characterized by the seasonal presence of CO2ice clouds. Their properties have been long studied, as well as their formation mechanisms in relation to the thermal structure of the atmosphere and its variability. In this study, we present the first observations of these clouds at the terminator (dawn and dusk) by the NOMAD spectrometer onboard the Exomars Trace Gas Orbiter. CO2ice is detected simultaneously with dust, water ice and the temperature profile. Our results agree with previous findings in terms of how clouds are spatially distributed and their temporal occurrence. However, we also explore the sources of condensation nuclei for CO2ice particles, showing that water ice is a possible source at dawn near the Equator. We also identify surface‐lifted dust below the CO2ice clouds observed east of Hellas Basin, suggesting that, at that location, dust could provide nuclei for CO2ice. CO2ice is also sometimes detected at temperatures higher than the CO2freezing point, suggesting ongoing sublimation. In this work we explore for the first time the composition of CO2ice clouds, which is critical to advance our understanding of how CO2ice clouds form in the mesosphere at Mars. Twenty Six mesospheric CO2ice clouds were detected with NOMAD SO in Mars Year 35, simultaneously with water ice, dust, and CO2saturation ratiosEquatorial CO2clouds are observed at 50–80 km altitude at dusk, and 40–60 km at dawn, when water ice likely provides condensation nucleiSix CO2ice clouds are found east of Hellas basin; their formation is likely sourced by surface‐lifted dust at 40–65 km Twenty Six mesospheric CO2ice clouds were detected with NOMAD SO in Mars Year 35, simultaneously with water ice, dust, and CO2saturation ratios Equatorial CO2clouds are observed at 50–80 km altitude at dusk, and 40–60 km at dawn, when water ice likely provides condensation nuclei Six CO2ice clouds are found east of Hellas basin; their formation is likely sourced by surface‐lifted dust at 40–65 km
Published: 2021
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43. Impact of the 2018 Mars global dust storm on water vapour as observed by NOMAD on ExoMars Trace Gas Orbiter.

Author: Vandaele, Ann Carine, Daerden, Frank, Thomas, Ian R., Aoki, Shohei, Depiesse, Cedric, Erwin, Justin, Neary, Lori, Piccialli, Arianna, Ristic, Bojan, Robert, Severine, Trompet, Loïc, Viscardy, Sebastien, Willame, Yannick, Wilquet, Valerie, Altieri, Francesca, Smith, Michael, Villanueva, Geronimo, Lopez-Moreno, Jose-Juan, Bellucci, Giancarlo, and Patel, Manish R.
Published: 2019

44. Ozone vertical profiles from NOMAD-UVIS: a preliminary analysis.

Author: Piccialli, Arianna, Vandaele, Ann Carine, Willame, Yannick, Depiesse, Cedric, Trompet, Loïc, Neary, Lori, Viscardy, Sebastien, Daerden, Frank, Thomas, Ian R., Ristic, Bojan, Mason, Jon P., Patel, Manish R., Bellucci, Giancarlo, and Lopez-Moreno, Jose-Juan
Published: 2019

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

Author: Vandaele, Ann Carine, Korablev, Oleg, Daerden, Frank, Aoki, Shohei, Thomas, Ian R., Altieri, Francesca, López-Valverde, Miguel, Villanueva, Geronimo, Liuzzi, Giuliano, Smith, Michael D., Erwin, Justin T., Trompet, Loïc, Fedorova, Anna A., Montmessin, Franck, Trokhimovskiy, Alexander, Belyaev, Denis A., Ignatiev, Nikolay I., Luginin, Mikhail, Olsen, Kevin S., Baggio, Lucio, Alday, Juan, Bertaux, Jean-Loup, Betsis, Daria, Bolsée, David, Clancy, R. Todd, Cloutis, Edward, Depiesse, Cédric, Funke, Bernd, Garcia-Comas, Maia, Gérard, Jean-Claude, Giuranna, Marco, Gonzalez-Galindo, Francisco, Grigoriev, Alexey V., Ivanov, Yuriy S., Kaminski, Jacek, Karatekin, Ozgur, Lefèvre, Franck, Lewis, Stephen, López-Puertas, Manuel, Mahieux, Arnaud, Maslov, Igor, Mason, Jon, Mumma, Michael J., Neary, Lori, Neefs, Eddy, Patrakeev, Andrey, Patsaev, Dmitry, Ristic, Bojan, Robert, Séverine, Schmidt, Frédéric, Shakun, Alexey, Teanby, Nicholas A., Viscardy, Sébastien, Willame, Yannick, Whiteway, James, Wilquet, Valérie, Wolff, Michael J., Bellucci, Giancarlo, Patel, Manish R., López-Moreno, Jose-Juan, Forget, François, Wilson, Colin F., Svedhem, Håkan, Vago, Jorge L., and Rodionov, Daniel
Subjects: 13. Climate action, 520 Astronomy, 620 Engineering
Abstract: Global dust storms on Mars are rare but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere, primarily owing to solar heating of the dust. 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. 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, as well as a decrease in the water column at low latitudes. 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 crystals. 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.

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

Author: Korablev O, Vandaele AC, Montmessin F, Fedorova AA, Trokhimovskiy A, Forget F, Lefèvre F, Daerden F, Thomas IR, Trompet L, Erwin JT, Aoki S, Robert S, Neary L, Viscardy S, Grigoriev AV, Ignatiev NI, Shakun A, Patrakeev A, Belyaev DA, Bertaux JL, Olsen KS, Baggio L, Alday J, Ivanov YS, Ristic B, Mason J, Willame Y, Depiesse C, Hetey L, Berkenbosch S, Clairquin R, Queirolo C, Beeckman B, Neefs E, Patel MR, Bellucci G, López-Moreno JJ, Wilson CF, Etiope G, Zelenyi L, Svedhem H, and Vago JL
Abstract: The detection of methane on Mars has been interpreted as indicating that geochemical or biotic activities could persist on Mars today 1 . A number of different measurements of methane show evidence of transient, locally elevated methane concentrations and seasonal variations in background methane concentrations 2-5 . These measurements, however, are difficult to reconcile with our current understanding of the chemistry and physics of the Martian atmosphere 6,7 , which-given methane's lifetime of several centuries-predicts an even, well mixed distribution of methane 1,6,8 . 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 detections 2,4 . We suggest that reconciliation between the present findings and the background methane concentrations found in the Gale crater 4 would require an unknown process that can rapidly remove or sequester methane from the lower atmosphere before it spreads globally.
Published: 2019
Full Text: View/download PDF

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