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2. The EChO science case

Author

Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Isaak, Kate, Linder, Martin, Lovis, Christophe, Micela, Giusi, Ollivier, Marc, Puig, Ludovic, Ribas, Ignasi, Snellen, Ignas, Allard, Bruce Swinyard. France, Barstow, Joanna, Cho, James, Coustenis, Athena, Cockell, Charles, Correia, Alexandre, Decin, Leen, de Kok, Remco, Deroo, Pieter, Encrenaz, Therese, Forget, Francois, Glasse, Alistair, Griffith, Caitlin, Guillot, Tristan, Koskinen, Tommi, Lammer, Helmut, Leconte, Jeremy, Maxted, Pierre, Mueller-Wodarg, Ingo, Nelson, Richard, North, Chris, Pallé, Enric, Pagano, Isabella, Piccioni, Guseppe, Pinfield, David, Selsis, Franck, Sozzetti, Alessandro, Stixrude, Lars, Tennyson, Jonathan, Turrini, Diego, Beaulieu, Mariarosa Zapatero-Osorio. Jean-Philippe, Grodent, Denis, Guedel, Manuel, Luz, David, Nørgaard-Nielsen, Hans Ulrik, Ray, Tom, Rickman, Hans, Selig, Avri, Banaszkiewicz, Mark Swain. Marek, Barlow, Mike, Bowles, Neil, Branduardi-Raymont, Graziella, Foresto, Vincent Coudé du, Gerard, Jean-Claude, Gizon, Laurent, Hornstrup, Allan, Jarchow, Christopher, Kerschbaum, Franz, Kovacs, Géza, Lagage, Pierre-Olivier, Lim, Tanya, Lopez-Morales, Mercedes, Malaguti, Giuseppe, Pace, Emanuele, Pascale, Enzo, Vandenbussche, Bart, Wright, Gillian, Adriani, Gonzalo Ramos Zapata. Alberto, Azzollini, Ruymán, Balado, Ana, Bryson, Ian, Burston, Raymond, Colomé, Josep, Crook, Martin, Di Giorgio, Anna, Griffin, Matt, Hoogeveen, Ruud, Ottensamer, Roland, Irshad, Ranah, Middleton, Kevin, Morgante, Gianluca, Pinsard, Frederic, Rataj, Mirek, Reess, Jean-Michel, Savini, Giorgio, Schrader, Jan-Rutger, Stamper, Richard, Abe, Berend Winter. L., Abreu, M., Achilleos, N., Ade, P., Adybekian, V., Affer, L., Agnor, C., Agundez, M., Alard, C., Alcala, J., Prieto, C. Allende, Floriano, F. J. Alonso, Altieri, F., Iglesias, C. A. Alvarez, Amado, P., Andersen, A., Aylward, A., Baffa, C., Bakos, G., Ballerini, P., Banaszkiewicz, M., Barber, R. J., Barrado, D., Barton, E. J., Batista, V., Bellucci, G., Avilés, J. A. Belmonte, Berry, D., Bézard, B., Biondi, D., Błęcka, M., Boisse, I., Bonfond, B., Bordé, P., Börner, P., Bouy, H., Brown, L., Buchhave, L., Budaj, J., Bulgarelli, A., Burleigh, M., Cabral, A., Capria, M. T., Cassan, A., Cavarroc, C., Cecchi-Pestellini, C., Cerulli, R., Chadney, J., Chamberlain, S., Charnoz, S., Jessen, N. Christian, Ciaravella, A., Claret, A., Claudi, R., Coates, A., Cole, R., Collura, A., Cordier, D., Covino, E., Danielski, C., Damasso, M., Deeg, H. J., Delgado-Mena, E., Del Vecchio, C., Demangeon, O., De Sio, A., De Wit, J., Dobrijévic, M., Doel, P., Dominic, C., Dorfi, E., Eales, S., Eiroa, C., Contreras, M. Espinoza, Esposito, M., Eymet, V., Fabrizio, N., Fernández, M., Castella, B. Femenía, Figueira, P., Filacchione, G., Fletcher, L., Focardi, M., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gambicorti, L., Gaulme, P., López, R. J. García, Garcia-Piquer, A., Gear, W., Gerard, J. -C., Gesa, L., Giani, E., Gianotti, F., Gillon, M., Giro, E., Giuranna, M., Gomez, H., Gomez-Leal, I., Hernandez, J. Gonzalez, Merino, B. González, Graczyk, R., Grassi, D., Guardia, J., Guio, P., Gustin, J., Hargrave, P., Haigh, J., Hébrard, E., Heiter, U., Heredero, R. L., Herrero, E., Hersant, F., Heyrovsky, D., Hollis, M., Hubert, B., Hueso, R., Israelian, G., Iro, N., Irwin, P., Jacquemoud, S., Jones, G., Jones, H., Justtanont, K., Kehoe, T., Kerschbaum, F., Kerins, E., Kervella, P., Kipping, D., Koskinen, T., Krupp, N., Lahav, O., Laken, B., Lanza, N., Lellouch, E., Leto, G., Goldaracena, J. Licandro, Lithgow-Bertelloni, C., Liu, S. J., Cicero, U. Lo, Lodieu, N., Lognonné, P., Lopez-Puertas, M., Lopez-Valverde, M. A., Rasmussen, I. Lundgaard, Luntzer, A., Machado, P., MacTavish, C., Maggio, A., Maillard, J. -P., Magnes, W., Maldonado, J., Mall, U., Marquette, J. -B., Mauskopf, P., Massi, F., Maurin, A. -S., Medvedev, A., Michaut, C., Miles-Paez, P., Montalto, M., Rodríguez, P. Montañés, Monteiro, M., Montes, D., Morais, H., Morales, J. C., Morales-Calderón, M., Morello, G., Martín, A. Moro, Moses, J., Bedon, A. Moya, Alcaino, F. Murgas, Oliva, E., Orton, G., Palla, F., Pancrazzi, M., Pantin, E., Parmentier, V., Parviainen, H., Ramírez, K. Y. Peña, Peralta, J., Perez-Hoyos, S., Petrov, R., Pezzuto, S., Pietrzak, R., Pilat-Lohinger, E., Piskunov, N., Prinja, R., Prisinzano, L., Polichtchouk, I., Poretti, E., Radioti, A., Ramos, A. A., Rank-Lüftinger, T., Read, P., Readorn, K., López, R. Rebolo, Rebordão, J., Rengel, M., Rezac, L., Rocchetto, M., Rodler, F., Béjar, V. J. Sánchez, Lavega, A. Sanchez, Sanromá, E., Santos, N., Forcada, J. Sanz, Scandariato, G., Schmider, F. -X., Scholz, A., Scuderi, S., Sethenadh, J., Shore, S., Showman, A., Sicardy, B., Sitek, P., Smith, A., Soret, L., Sousa, S., Stiepen, A., Stolarski, M., Strazzulla, G., Tabernero, H. M, Tanga, P., Tecsa, M., Temple, J., Terenzi, L., Tessenyi, M., Testi, L., Thompson, S., Thrastarson, H., Tingley, B. W., Trifoglio, M., Torres, J. Martín, Tozzi, A., Turrini, D., Varley, R., Vakili, F., de Val-Borro, M., Valdivieso, M. L., Venot, O., Villaver, E., Vinatier, S., Viti, S., Waldmann, I., Waltham, D., Ward-Thompson, D., Waters, R., Watkins, C., Watson, D., Wawer, P., Wawrzaszk, A., White, G., Widemann, T., Winek, W., Wiśniowski, T., Yelle, R., Yung, Y., and Yurchenko, S. N.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The discovery of almost 2000 exoplanets has revealed an unexpectedly diverse planet population. Observations to date have shown that our Solar System is certainly not representative of the general population of planets in our Milky Way. The key science questions that urgently need addressing are therefore: What are exoplanets made of? Why are planets as they are? What causes the exceptional diversity observed as compared to the Solar System? EChO (Exoplanet Characterisation Observatory) has been designed as a dedicated survey mission for transit and eclipse spectroscopy capable of observing a large and diverse planet sample within its four-year mission lifetime. EChO can target the atmospheres of super-Earths, Neptune-like, and Jupiter-like planets, in the very hot to temperate zones (planet temperatures of 300K-3000K) of F to M-type host stars. Over the next ten years, several new ground- and space-based transit surveys will come on-line (e.g. NGTS, CHEOPS, TESS, PLATO), which will specifically focus on finding bright, nearby systems. The current rapid rate of discovery would allow the target list to be further optimised in the years prior to EChO's launch and enable the atmospheric characterisation of hundreds of planets. Placing the satellite at L2 provides a cold and stable thermal environment, as well as a large field of regard to allow efficient time-critical observation of targets randomly distributed over the sky. A 1m class telescope is sufficiently large to achieve the necessary spectro-photometric precision. The spectral coverage (0.5-11 micron, goal 16 micron) and SNR to be achieved by EChO, thanks to its high stability and dedicated design, would enable a very accurate measurement of the atmospheric composition and structure of hundreds of exoplanets., Comment: 50 pages, 30 figures. Experimental Astronomy

Published
2015
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3. Toward a numerical deshaker for PFS

Author

Schmidt, F., Shatalina, I., Kowalski, M., Gac, N., Saggin, B., and Giuranna, M.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The Planetary Fourier Spectrometer (PFS) onboard Mars Express (MEx) is the instrument with the highest spectral resolution observing Mars from orbit since January 2004. It permits studying the atmospheric structure, major and minor compounds. The present time version of the calibration is limited by the effects of mechanical vibration, currently not corrected. We proposed here a new approach to correct for the vibrations based on semi-blind deconvolution of the measurements. This new approach shows that a correction can be done efficiently with 85% reduction of the artefacts, in a equivalent manner to the stacking of 10 spectra. Our strategy is not fully automatic due to the dependence on some regularisation parameters. It may be applied on the complete PFS dataset, correcting the large-scale perturbation due to microvibrations for each spectrum independently. This approach is validated on actual PFS data of Short Wavelength Channel (SWC), perturbed by microvibrations. A coherence check can be performed and also validate our approach. Unfortunately, the coherence check can be done only on the first 310 orbits of MEx only, until the laser line has been switch off. More generally, this work may apply to numerically "deshake" Fourier Transform Spectrometer (FTS), widely used in space experiments or in the laboratory., Comment: 18 pages, 8 figures, submitted to Planetary and Space Science

Published
2013
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6. Mars Express investigations of Phobos and Deimos

Author

Witasse, O., Duxbury, T., Chicarro, A., Altobelli, N., Andert, T., Aronica, A., Barabash, S., Bertaux, J.-L., Bibring, J.-P., Cardesin-Moinelo, A., Cichetti, A., Companys, V., Dehant, V., Denis, M., Formisano, V., Futaana, Y., Giuranna, M., Gondet, B., Heather, D., Hoffmann, H., Holmström, M., Manaud, N., Martin, P., Matz, K.-D., Montmessin, F., Morley, T., Mueller, M., Neukum, G., Oberst, J., Orosei, R., Pätzold, M., Picardi, G., Pischel, R., Plaut, J.J., Reberac, A., Pardo Voss, P., Roatsch, T., Rosenblatt, P., Remus, S., Schmedemann, N., Willner, K., and Zegers, T.

Published
2014
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8. NOMAD, an Integrated Suite of Three Spectrometers for the ExoMars Trace Gas Mission: Technical Description, Science Objectives and Expected Performance

Author

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

Published
2018
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9. The EChO science case

Author

Tinetti, Giovanna, primary, Drossart, Pierre, additional, Eccleston, Paul, additional, Hartogh, Paul, additional, Isaak, Kate, additional, Linder, Martin, additional, Lovis, Christophe, additional, Micela, Giusi, additional, Ollivier, Marc, additional, Puig, Ludovic, additional, Ribas, Ignasi, additional, Snellen, Ignas, additional, Swinyard, Bruce, additional, Allard, France, additional, Barstow, Joanna, additional, Cho, James, additional, Coustenis, Athena, additional, Cockell, Charles, additional, Correia, Alexandre, additional, Decin, Leen, additional, de Kok, Remco, additional, Deroo, Pieter, additional, Encrenaz, Therese, additional, Forget, Francois, additional, Glasse, Alistair, additional, Griffith, Caitlin, additional, Guillot, Tristan, additional, Koskinen, Tommi, additional, Lammer, Helmut, additional, Leconte, Jeremy, additional, Maxted, Pierre, additional, Mueller-Wodarg, Ingo, additional, Nelson, Richard, additional, North, Chris, additional, Pallé, Enric, additional, Pagano, Isabella, additional, Piccioni, Guseppe, additional, Pinfield, David, additional, Selsis, Franck, additional, Sozzetti, Alessandro, additional, Stixrude, Lars, additional, Tennyson, Jonathan, additional, Turrini, Diego, additional, Zapatero-Osorio, Mariarosa, additional, Beaulieu, Jean-Philippe, additional, Grodent, Denis, additional, Guedel, Manuel, additional, Luz, David, additional, Nørgaard-Nielsen, Hans Ulrik, additional, Ray, Tom, additional, Rickman, Hans, additional, Selig, Avri, additional, Swain, Mark, additional, Banaszkiewicz, Marek, additional, Barlow, Mike, additional, Bowles, Neil, additional, Branduardi-Raymont, Graziella, additional, du Foresto, Vincent Coudé, additional, Gerard, Jean-Claude, additional, Gizon, Laurent, additional, Hornstrup, Allan, additional, Jarchow, Christopher, additional, Kerschbaum, Franz, additional, Kovacs, Géza, additional, Lagage, Pierre-Olivier, additional, Lim, Tanya, additional, Lopez-Morales, Mercedes, additional, Malaguti, Giuseppe, additional, Pace, Emanuele, additional, Pascale, Enzo, additional, Vandenbussche, Bart, additional, Wright, Gillian, additional, Ramos Zapata, Gonzalo, additional, Adriani, Alberto, additional, Azzollini, Ruymán, additional, Balado, Ana, additional, Bryson, Ian, additional, Burston, Raymond, additional, Colomé, Josep, additional, Crook, Martin, additional, Di Giorgio, Anna, additional, Griffin, Matt, additional, Hoogeveen, Ruud, additional, Ottensamer, Roland, additional, Irshad, Ranah, additional, Middleton, Kevin, additional, Morgante, Gianluca, additional, Pinsard, Frederic, additional, Rataj, Mirek, additional, Reess, Jean-Michel, additional, Savini, Giorgio, additional, Schrader, Jan-Rutger, additional, Stamper, Richard, additional, Winter, Berend, additional, Abe, L., additional, Abreu, M., additional, Achilleos, N., additional, Ade, P., additional, Adybekian, V., additional, Affer, L., additional, Agnor, C., additional, Agundez, M., additional, Alard, C., additional, Alcala, J., additional, Prieto, C. Allende, additional, Alonso Floriano, F. J., additional, Altieri, F., additional, Alvarez Iglesias, C. A., additional, Amado, P., additional, Andersen, A., additional, Aylward, A., additional, Baffa, C., additional, Bakos, G., additional, Ballerini, P., additional, Banaszkiewicz, M., additional, Barber, R. J., additional, Barrado, D., additional, Barton, E. J., additional, Batista, V., additional, Bellucci, G., additional, Belmonte Avilés, J. A., additional, Berry, D., additional, Bézard, B., additional, Biondi, D., additional, Błęcka, M., additional, Boisse, I., additional, Bonfond, B., additional, Bordé, P., additional, Börner, P., additional, Bouy, H., additional, Brown, L., additional, Buchhave, L., additional, Budaj, J., additional, Bulgarelli, A., additional, Burleigh, M., additional, Cabral, A., additional, Capria, M. T., additional, Cassan, A., additional, Cavarroc, C., additional, Cecchi-Pestellini, C., additional, Cerulli, R., additional, Chadney, J., additional, Chamberlain, S., additional, Christian Jessen, N., additional, Ciaravella, A., additional, Claret, A., additional, Claudi, R., additional, Coates, A., additional, Cole, R., additional, Collur, A., additional, Cordier, D., additional, Covino, E., additional, Danielski, C., additional, Damasso, M., additional, Deeg, H. J., additional, Delgado-Mena, E., additional, Del Vecchio, C., additional, Demangeon, O., additional, De Sio, A., additional, De Wit, J., additional, Dobrijévi, M., additional, Doel, P., additional, Dominic, C., additional, Dorfi, E., additional, Eales, S., additional, Eiroa, C., additional, Espinoza Contreras, M., additional, Esposito, M., additional, Eymet, V., additional, Fabrizio, N., additional, Fernández, M., additional, Femenía Castella, B., additional, Figueira, P., additional, Filacchione, G., additional, Fletcher, L., additional, Focardi, M., additional, Fossey, S., additional, Fouqué, P., additional, Frith, J., additional, Galand, M., additional, Gambicorti, L., additional, Gaulme, P., additional, García López, R. J., additional, Garcia-Piquer, A., additional, Gear, W., additional, Gerard, J. -C., additional, Gesa, L., additional, Giani, E., additional, Gianotti, F., additional, Gillon, M., additional, Giro, E., additional, Giuranna, M., additional, Gomez, H., additional, Gomez-Leal, I., additional, Gonzalez Hernandez, J., additional, GonzÁlez Merino, B., additional, Graczyk, R., additional, Grassi, D., additional, Guardia, J., additional, Guio, P., additional, Gustin, J., additional, Hargrave, P., additional, Haigh, J., additional, Hébrard, E., additional, Heiter, U., additional, Heredero, R. L., additional, Herrero, E., additional, Hersant, F., additional, Heyrovsky, D., additional, Hollis, M., additional, Hubert, B., additional, Hueso, R., additional, Israelian, G., additional, Iro, N., additional, Irwin, P., additional, Jacquemoud, S., additional, Jones, G., additional, Jones, H., additional, Justtanont, K., additional, Kehoe, T., additional, Kerschbaum, F., additional, Kerins, E., additional, Kervell, P., additional, Kipping, D., additional, Koskinen, T., additional, Krupp, N., additional, Lahav, O., additional, Laken, B., additional, Lanza, N., additional, Lellouch, E., additional, Leto, G., additional, Goldaracena, J. Licandro, additional, Bertelloni, C. Lithgow, additional, Liu, S. J., additional, Cicero, U. Lo, additional, Lodieu, N., additional, Lognonné, P., additional, Puertas, M. Lopez, additional, Valverde, M. A. Lopez, additional, Rasmussen, I. Lundgaard, additional, Luntzer, A., additional, Machado, P., additional, Tavish, C. Mac, additional, Maggio, A., additional, Maillard, J. P., additional, Magnes, W., additional, Maldonado, J., additional, Mall, U., additional, Marquette, J. B., additional, Mauskopf, P., additional, Massi, F., additional, Maurin, A. S., additional, Medvedev, A., additional, Michaut, C., additional, Paez, P. Miles, additional, Montalto, M., additional, Rodríguez, P. Montañés, additional, Monteiro, M., additional, Montes, D., additional, Morais, H., additional, Morale, J. C., additional, Morales-Calderón, M., additional, Morello, G., additional, Martín, A. Moro, additional, Moses, J., additional, Bedon, A. Moya, additional, Alcaino, F. Murgas, additional, Oliva, E., additional, Orton, G., additional, Palla, F., additional, Pancrazzi, M., additional, Pantin, E., additional, Parmentier, V., additional, Parviainen, H., additional, Ramirez, Y. Pena, additional, Peralta, J., additional, Perez-Hoyos, S., additional, Petrov, R., additional, Pezzuto, S., additional, Pietrzak, R., additional, Pilat-Lohinger, E., additional, Piskunov, N., additional, Prinja, R., additional, Prisinzano, L., additional, Polichtchouk, I., additional, Poretti, E., additional, Radioti, A., additional, Ramos, A., additional, Rank-Luftinger, T., additional, Read, P., additional, Readorn, K., additional, Lopez, R. Rebolo, additional, Rebordao, J., additional, Rengel, M., additional, Rezac, L., additional, Rocchetto, M., additional, Rodler, F., additional, Bejar, J. Sanchez, additional, Sanchez Lavega, A., additional, Sanroma, E., additional, Santos, N., additional, Forcada, J. Sanz, additional, Scandariato, G., additional, Schmider, F.- X., additional, Scholz, A., additional, Scuderi, S., additional, Sethenadh, J., additional, Shore, S., additional, Showman, A., additional, Sicardy, B., additional, Sitek, P., additional, Smith, A., additional, Soret, L., additional, Sousa, S., additional, Stiepen, A., additional, Stolarski, M., additional, Strazzulla, G., additional, Tabernero, H. M., additional, Tanga, P., additional, Tecsa, M., additional, Temple, J., additional, Terenzi, L., additional, Tessenyi, M., additional, Testi, L., additional, Thompson, S., additional, Thrastarson, H., additional, Tingley, B. W., additional, Trifoglio, M., additional, Torres, J. Martin, additional, Tozzi, A., additional, Turrini, D., additional, Varley, R., additional, Vakili, F., additional, de Val-Borro, M., additional, Valdivieso, M. L., additional, Venot, O., additional, Villaver, E., additional, Vinatier, S., additional, Viti, S., additional, Waldmann, I., additional, Waltham, D., additional, Ward-Thompson, D., additional, Waters, R., additional, Watkins, C., additional, Watson, D., additional, Wawer, P., additional, Wawrzaszk, A., additional, White, G., additional, Widemann, T., additional, Winek, W., additional, Wi.niowski, T., additional, Yelle, R., additional, Yung, Y., additional, and Yurchenko, S. N., additional

Published
2015
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11. 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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13. 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

14. AOST: Fourier spectrometer for studying mars and phobos

Author

Korablev, O. I., Grigor’ev, A. V., Moshkin, B. E., Zasova, L. V., Montmessin, F., Gvozdev, A. B., Shashkin, V. N., Patsaev, D. V., Makarov, V. S., Maksimenko, S. V., Ignatiev, N. I., Fedorova, A. A., Arnold, G., Shakun, A. V., Terentiev, A. I., Zharkov, A. V., Mayorov, B. S., Nikol’sky, Yu. V., Khatuntsev, I. V., Bellucci, G., Giuranna, M., Kuz’min, R. O., and Rodin, A. V.

Published
2012
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16. PFS/MEX observations of the condensing CO.sub.2 south polar cap of Mars

Author

Giuranna, M., Grassi, D., Formisano, V., Montabone, L., Forget, F., and Zasova, L.

Subjects
Mars (Planet) -- Analysis, Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2008.05.019 Byline: M. Giuranna (a)(b), D. Grassi (a), V. Formisano (a), L. Montabone (c)(d), F. Forget (d), L. Zasova (a)(e) Keywords: Mars; polar caps; Mars; climate; Ices Abstract: The condensing CO.sub.2 south polar cap of Mars and the mechanisms of the CO.sub.2 ice accumulation have been studied through the analysis of spectra acquired by the Planetary Fourier Spectrometer (PFS) during the first two years of ESA's Mars Express (MEX) mission. This dataset spans more than half a martian year, from Ls[approximately equal to]330[degrees] to Ls[approximately equal to]194[degrees], and includes the southern fall season which is found to be extremely important for the study of the residual south polar cap asymmetry. The cap expands symmetrically and with constant speed during the fall season. The maximum extension occurs sometime in the 80[degrees]-90[degrees]Ls range, when the cap edges are as low as -40[degrees] latitude. Inside Hellas and Argyre basins, frost can be stable at lower latitudes due to the higher pressure values, causing the seasonal cap to be asymmetric. Within the seasonal range considered in this paper, the cap edge recession rate is approximately half the rate at which the cap edge expanded. The longitudinal asymmetries reduce during the cap retreat, and disappear around Ls[approximately equal to]145[degrees]. Two different mechanisms are responsible for CO.sub.2 ice accumulation during the fall season, especially in the 50[degrees]-70[degrees]Ls range. Here, CO.sub.2 condensation in the atmosphere, and thus precipitation, is allowed exclusively in the western hemisphere, and particularly in the longitudinal corridor of the perennial cap. In the eastern hemisphere, the cap consists mainly of CO.sub.2 frost deposits, as a consequence of direct vapor deposition. The differences in the nature of the surface ice deposits are the main cause for the residual south polar cap asymmetry. Results from selected PFS orbits have also been compared with the results provided by the martian general circulation model (GCM) of the Laboratoire de Meteorologie dynamique (LMD) in Paris, with the aim of putting the observations in the context of the global circulation. This first attempt of cross-validation between PFS measurements and the LMD GCM on the one hand confirms the interpretation of the observations, and on the other hand shows that the climate modeling during the southern polar night on Mars is extremely sensitive to the dynamical forcing. Author Affiliation: (a) Istituto di Fisica dello Spazio Interplanetario INAF-IFSI, Via del Fosso del Cavaliere 100, 00133 Roma, Italy (b) Centro Interdipartimentale di Studi e Attivita Spaziali CISAS - 'G. Colombo,' University of Padova, Via Venezia 15, 35131 Padova, Italy (c) Department of Physics & Astronomy, The Open University, Walton Hall, Milton Keynes MK7 6AA, United Kingdom (d) Laboratoire de Meteorologie Dynamique du CNRS, Universite Paris 6, BP99, 75252, Paris Cedex 05, France (e) Space Research Institute of Russian Academy of Sciences (IKI), Profsojuznaja 84/32, 117810 Moscow, Russia Article History: Received 20 November 2007; Revised 4 April 2008

Published
2008

17. Investigation of water vapor on Mars with PFS/SW of Mars Express

Author

Tschimmel, M., Ignatiev, N.I., Titov, D.V., Lellouch, E., Fouchet, T., Giuranna, M., and Formisano, V.

Subjects
Mars (Planet), Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2008.01.018 Byline: M. Tschimmel (a), N.I. Ignatiev (b), D.V. Titov (a)(b), E. Lellouch (c), T. Fouchet (c)(d), M. Giuranna (e), V. Formisano (e) Keywords: Mars; Mars; atmosphere; Abundances; atmospheres; Atmospheres; structure; Infrared observations Abstract: New insight into the seasonal, diurnal and spatial distribution of water vapor on Mars has been obtained from analyzing the spectra of the short-wavelength channel (SW) of the Planetary Fourier Spectrometer (PFS) onboard Mars Express. The processed dataset, recorded between January 2004 and April 2005, covers the seasons from L.sub.S=331[degrees] of Mars Year 26 to L.sub.S=196[degrees] of the following year. In this period the mean column density around vernal equinox was 8.2 pr. [mu]m. The maximum values during northern summer were about 65 pr. [mu]m, located around 75[degrees] N latitude with a longitudinally inhomogeneous distribution. Regarding the atmospheric transport, the majority of polar water vapor remains in the north polar region while only about a quarter is transported southward. Geographically there are two water vapor maxima visible, over Arabia Terra and the Tharsis plateau, that are most likely caused both by atmosphere-ground interaction and by atmospheric circulation. A comparison with other instruments generally shows a good agreement, only the SPICAM results are systematically lower. Compared to the results from the PFS long-wavelength channel the results of this work are slightly higher. A strong discrepancy is visible northward of about 50[degrees] N during the northern summer that is possibly explained by a non-uniform vertical H.sub.2O mixing. In particular, a confinement of the water to the lower few kilometers yields a much better agreement between the retrieved column densities of the two PFS channels. Author Affiliation: (a) Max Planck Institute for Solar System Research, 37191 Katlenburg-Lindau, Germany (b) Space Research Institute (IKI RAN), Moscow 117997, Russia (c) Observatoire de Paris, LESIA, Meudon 92195, France (d) Universite Pierre et Marie Curie - Paris 6, UMR 8109, Paris 75005, France (e) Istituto di Fisica dello Spazio Interplanetario INAF-IFSI, 00133 Rome, Italy Article History: Received 3 July 2007; Revised 15 January 2008

Published
2008

18. Results of measurements with the Planetary Fourier Spectrometer onboard Mars Express: Clouds and dust at the end of southern summer. A comparison with OMEGA images

Author

Zasova, L. V., Formisano, V., Moroz, V. I., Bibring, J. -P., Grassi, D., Ignatiev, N. I., Giuranna, M., Bellucci, G., Altieri, F., Blecka, M., Gnedykh, V. N., Grigoriev, A. V., Lellouch, E., Mattana, A., Maturilli, A., Moshkin, B. E., Nikolsky, Yu. V., Patsaev, D. V., Piccioni, G., Ratai, M., Saggin, B., Fonti, S., Khatuntsev, I. V., Hirsh, H., and Ekonomov, A. P.

Published
2006
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19. Albedo and photometric study of Mars with the Planetary Fourier Spectrometer on-board the Mars Express mission

Author

Esposito, F., Giuranna, M., Maturilli, A., Palomba, E., Colangeli, L., and Formisano, V.

Subjects
Mars (Planet) -- Observations, Photometry -- Usage, Mars (Planet) -- Atmosphere, Mars (Planet) -- Environmental aspects, Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2006.08.028 Byline: F. Esposito (a), M. Giuranna (b), A. Maturilli (b), E. Palomba (b), L. Colangeli (a), V. Formisano (b) Keywords: Mars; surface; Photometry; Infrared observations Abstract: The Short Wavelength Channel of the Planetary Fourier Spectrometer (PFS) covers the 8333-1750 cm.sup.-1 (1.2-5.7 [mu]m) spectral range, that is well suited to study the reflectance properties of the martian soil. These properties vary with time due to the dust dynamics in the martian environment. Wind can blow off dust exposing soil and fresh rocks and can support grain mobility inducing local dust settling. We have analyzed PFS data from January 2004 to April 2005. A detailed photometric study of the radiance acquired from the planet has been performed in order to compare correctly measurements obtained at different viewing geometries and to produce a mosaic image of the planet. The results show good agreement with data from the Thermal Emission Spectrometer (on-board NASA Mars Global Surveyor orbiter), although some variations are observed. Some albedo changes could be due to small to medium scale dust storms. A very accurate estimation of the limb-darkening parameter has been computed from the analyzed data. The obtained values are compared with a surface roughness and a thermal inertia map in order to assess the relation between the limb-darkening parameter and the physical properties of surface. Author Affiliation: (a) INAF - Osservatorio Astronomico di Capodimonte (INAF-OAC), Via Moiariello 16, 80131 Napoli, Italy (b) INAF - Istituto di Fisica dello Spazio Interplanetario INAF-IFSI, Via del Fosso del Cavaliere 100, 00133 Roma, Italy Article History: Received 2 February 2006; Revised 25 August 2006

Published
2007

22. Observations of non-LTE emission at 4-5 microns with the planetary Fourier spectrometer abord the Mars Express mission

Author

Formisano, V., Maturilli, A., Giuranna, M., D'Aversa, E., and Lopez-Valverde, M.A.

Subjects
Astronomy, Earth sciences
Abstract

To link to full-text access for this article, visit this link: http://dx.doi.org/10.1016/j.icarus.2005.12.022 Byline: V. Formisano (a), A. Maturilli (a), M. Giuranna (a), E. D'Aversa (a), M.A. Lopez-Valverde (b) Keywords: Mars; Mars; atmosphere; Atmospheres; composition Abstract: We report on PFS-MEX (Planetary Fourier Spectrometer on board Mars Express) limb observations of the non-Local Thermodynamic Equilibrium emission by CO and CO.sub.2 isotopic molecules. The CO emission is observed peaking at altitudes lower than the CO.sub.2 emission peak. Two orbits have been considered, which explore latitudes from 75 to 15[degrees] N, located in local time at 11:30 and 06:40, and with L.sub.s=138[degrees] and 168[degrees], respectively. In general in the season considered (northern summer) the emission intensity increases going to lower latitudes. The peak emission height is also decreasing with decreasing latitude. The CO.sub.2 isotopic molecules are emitting radiance out of proportion with respect to the normal isotopic abundance, which surely indicates a strong contribution from a large number of much weaker CO.sub.2 bands, a result that will demand careful theoretical modeling. By comparison with Hitran data base we can identify, among the emitting bands, the second hot band for the 626 and 636 molecule, while for the 628 and 627 emission from the third hot bands are very possible. Other minor bands or lines are also observed in emission for the first time in Mars. In one of the two orbits considered, the orbit 1234 of MEX, we also observe at altitudes 80-85 km scattered radiation, with indication of CO.sub.2 ice aerosols as scattering centers. At the same altitude the Pathfinder descending measurements show a temperature that allows CO.sub.2 condensation. Pathfinder measurements were at 03:00 local time, while our observations are for orbit 1234 showing CO.sub.2 ice signature at 11:30 local time. These non-LTE limb emissions, with their unprecedented spectral resolution in this portion of the near infrared and their sensitivity and geographical coverage, will represent in our opinion an excellent data set for testing current theoretical models of the martian upper atmosphere. Author Affiliation: (a) Istituto di Fisica dello Spazio Interplanetario IFSI-INAF, Via del Fosso del Cavaliere 100, 00113 Roma, Italy (b) Instituto de Astrofisica de Andalucia (CSIC), Apdo. 3004, 18080 Granada, Spain Article History: Received 23 May 2005; Revised 20 December 2005

Published
2006

23. The planetary fourier spectrometer (PFS) onboard the European Venus Express mission

Author

Formisano, V., Angrilli, F., Arnold, G., Atreya, S., Baines, K.H., Bellucci, G., Bezard, B., Billebaud, F., Biondi, D., Blecka, M.I., Colangeli, L., Comolli, L., Crisp, D., D’Amore, M., Encrenaz, T., Ekonomov, A., Esposito, F., Fiorenza, C., Fonti, S., Giuranna, M., Grassi, D., Grieger, B., Grigoriev, A., Helbert, J., Hirsch, H., Ignatiev, N., Jurewicz, A., Khatuntsev, I., Lebonnois, S., Lellouch, E., Mattana, A., Maturilli, A., Mencarelli, E., Michalska, M., Lopez Moreno, J., Moshkin, B., Nespoli, F., Nikolsky, Yu., Nuccilli, F., Orleanski, P., Palomba, E., Piccioni, G., Rataj, M., Rinaldi, G., Rossi, M., Saggin, B., Stam, D., Titov, D., Visconti, G., and Zasova, L.

Published
2006
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24. 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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26. The Planetary Fourier Spectrometer (PFS) onboard the European Mars Express mission

Author

Formisano, V., Angrilli, F., Arnold, G., Atreya, S., Bianchini, G., Biondi, D., Blanco, A., Blecka, M.I., Coradini, A., Colangeli, L., Ekonomov, A., Esposito, F., Fonti, S., Giuranna, M., Grassi, D., Gnedykh, V., Grigoriev, A., Hansen, G., Hirsh, H., Khatuntsev, I., Kiselev, A., Ignatiev, N., Jurewicz, A., Lellouch, E., Lopez Moreno, J., Marten, A., Mattana, A., Maturilli, A., Mencarelli, E., Michalska, M., Moroz, V., Moshkin, B., Nespoli, F., Nikolsky, Y., Orfei, R., Orleanski, P., Orofino, V., Palomba, E., Patsaev, D., Piccioni, G., Rataj, M., Rodrigo, R., Rodriguez, J., Rossi, M., Saggin, B., Titov, D., and Zasova, L.

Published
2005
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36. 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

37. 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

38. 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

39. NOMAD, an integrated suite of three spectrometers for the ExoMars trace gas mission: Technical description, science objectivs and expected performance

Author

Vandaele, Ann Carine, Lopez-Moreno, J.-J., Patel, M.R., Bellucci, G., Daerden, F., Ristic, B., Robert, Séverine, Thomas, I.R., Wilquet, Valérie, Allen, M., Alonso-Rodrigo, G., Altieri, F., Aoki, S, Bolsée, D., Clancy, T., Cloutis, E., Depiesse, Cédric, Drummond, Rachel, Fedorova, A., Formisano, V., Funke, Bernd, Gonzalez-Galindo, F., Geminale, A., Gérard, J.-C., Giuranna, M., Hetey, L., Ignatiev, N., Kaminski, J., Karatekin, Ozgur, Kasaba, Y., Leese, M., Lefèvre, F., Lewis, S. R., Lopez-Puertas, Manuel, Lopez-Valverde, M.A., Mahieux, Arnaud, Mason, James, McConnell, John, Mumma, M., Neary, L., Neefs, Eddy, Renotte, E., Gómez-Rodriguez, Julio, Sindoni, G., Smith, M., Stiepen, A., Trokhimovsky, A., Vander Auwera, Jean, Villanueva, G., Viscardy, Sébastien, Whiteway, J.A., Willame, Yannick, Wolff, M., and NOMAD, Team

Subjects
Spectroscopie [électromagnétisme, optique, acoustique], Chimie, Physique atomique et moléculaire
Abstract

info:eu-repo/semantics/published

Published
2018

40. Mesospheric CO 2 ice clouds on Mars observed by Planetary Fourier Spectrometer onboard Mars Express

Author

Sato, Y., Giuranna, M., Wolkenberg, P., Aoki, Shohei, Sato, Takao M., Nakagawa, Hiromu, and Kasaba, Yasumasa

Subjects
010504 meteorology & atmospheric sciences, Planetary Fourier Spectrometer, Imaging spectrometer, Mars, Astrophysics, 01 natural sciences, Atmospheric radiative transfer codes, 0103 physical sciences, Spectral resolution, 010303 astronomy & astrophysics, Spectroscopy, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences, Remote sensing, Ice cloud, Infrared observations, Ice crystals, Astronomy and Astrophysics, Mars Exploration Program, Atmosphere of Mars, Mars, atmosphere, 13. Climate action, Space and Planetary Science, Mars, climate, Astrophysics::Earth and Planetary Astrophysics, Geology
Abstract

Accepted: 2017-10-30, 資料番号: SA1170353000

Published
2018
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41. Ground-based infrared mapping of H2O2 on Mars near opposition

Author

Encrenaz, T., primary, Greathouse, T. K., additional, Aoki, S., additional, Daerden, F., additional, Giuranna, M., additional, Forget, F., additional, Lefèvre, F., additional, Montmessin, F., additional, Fouchet, T., additional, Bézard, B., additional, Atreya, S. K., additional, DeWitt, C., additional, Richter, M. J., additional, Neary, L., additional, and Viscardy, S., additional

Published
2019
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42. Mesospheric CO2 ice clouds on Mars observed by Planetary Fourier Spectrometer onboard Mars Express

Author

Aoki, Shohei, Sato, Y., Giuranna, M., Wolkenberg, P., Sato, Takao M., Nakagawa, Hiromu, Kasaba, Yasumasa, 青木, 翔平, 佐藤, 隆雄, 中川, 広務, 笠羽, 康正, Aoki, Shohei, Sato, Y., Giuranna, M., Wolkenberg, P., Sato, Takao M., Nakagawa, Hiromu, Kasaba, Yasumasa, 青木, 翔平, 佐藤, 隆雄, 中川, 広務, and 笠羽, 康正

Abstract

Accepted: 2017-10-30

Published
2018

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

Author

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

Abstract

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

Published
2018

44. Comet Siding Spring's influence on the Mars' ionosphere

Author

Witasse, Olivier, Sánchez-Cano, B., Molina-Cuberos, Gregorio, Blelly, Pierre-Louis, Lester, M., Leblanc, François, Modolo, Ronan, Chaufray, Jean-Yves, Gronoff, Guillaume, Espley, Jared, Costa, M., Giuranna, M., European Space Research and Technology Centre (ESTEC), European Space Agency (ESA), Department of Physics and Astronomy [Leicester], University of Leicester, Department of Electromagnetism and Electronics [Murcia], Universidad de Murcia, 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), HELIOS - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), NASA Langley Research Center [Hampton] (LaRC), GSFC Planetary Magnetospheres Laboratory, NASA Goddard Space Flight Center (GSFC), Istituto Nazionale di Astrofisica (INAF), Agence Spatiale Européenne = European Space Agency (ESA), 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), and 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)

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

International audience; On October 19th 2014, Mars experienced a close encounter with Comet C/2013 A1 (Siding Spring), at a distance of ~138,000 km. The coma washed over Mars and the planet passed directly through the cometary debris stream, producing significant effects in Mars' upper atmosphere. We present here an overview of ionospheric measurements performed during the comet encounter with Mars Express, MAVEN, and Mars Reconnaissance Orbiter. We discuss the comet's influence on the ionosphere through different processes that work at different altitudes: magnetospheric disturbances, impact of cometary pickup ions, and deposition of cometary dust.

Published
2017

45. Mars Express recent findings and future plans

Author

Titov, D.V., Bibring, Jean-Pierre, Cardesin Moinelo, A., Duxbury, T., Forget, Francois, Giuranna, M., Gonzalez-Galindo, F., Holmström, M, Jaumann, R., Määttänen, Anni, Martin, Patrick, Montmessin, Franck, Orosei, R., Pätzold, M, Plaut, J. J., and Mex Sgs Team, Team

Subjects
Planetengeologie, animal diseases, Physics::Space Physics, Mars, Astrophysics::Earth and Planetary Astrophysics, Physics::Geophysics
Abstract

Mars Express remains one of ESA's most scientifically productive missions whose publication record now exceeds 1000 papers. Characterization of geological processes on a local-to-regional scale by HRSC, OMEGA and partner experiments on NASA spacecraft has allowed constraining land-forming processes in space and time. Recent results suggest episodic geological activity as well as the presence of large bodies of liquid water in several provinces (e.g. Eridania Planum, Terra Chimeria) in the early and middle Amazonian epoch and formation of vast sedimentary plains north of the Hellas basin. Mars Express observations and experimental teams provided an essential contribution to the selection of the Mars-2020 landing sites. More than a decade-long record of atmospheric parameters such as temperature, dust loading, water vapor and ozone abundance, water ice and CO2 clouds distribution, collected by SPICAM, PFS and OMEGA spectrometers as well as subsequent modeling have provided key contributions to our understanding of the martian climate. The ASPERA-3 observations of ion escape covering a complete solar cycle have revealed important dependencies of the atmospheric erosion rate on parameters of the solar wind and EUV flux. Structure of the ionosphere sounded by the MARSIS radar and the MaRS radio science experiment was found to be significantly affected by the solar activity, the crustal magnetic field, as well as by the influx of meteorite and cometary dust. MARSIS and ASPERA-3 observations suggest that the sunlit ionosphere over the regions with strong crustal fields is denser and extends to higher altitudes as compared to the regions with no crustal anomalies. The ionospheric plasma expands to higher altitudes where it contacts with the solar wind plasma. Reconnection of solar magnetic field lines carried by the solar wind with field lines of crustal origin opens channels through which the ionospheric plasma escapes to space, producing strong and narrow cavities in the density. The situation is very different on the night side where the ionosphere has a patchy structure. Such patchy ionizations are observed in the regions where crustal field lines have a dominant vertical component. Through these patches the ionospheric plasma from the dayside penetrates and supplies the nightside ionosphere. Mars Express has fully accomplished its objectives set for 2015-2016. The mission provides unique observation capabilities amongst the flotilla of spacecraft investigating Mars. The mission has been confirmed till the end of 2018. The science case for the mission extension until the end of 2020 has been submitted. The observation program proposed for 2019-2020 includes both augmenting the coverage and extending long-time series, as well as new elements and potentially new opportunities for discoveries. It will be boosted by collaboration and synergies with NASA's MAVEN, ESA-Roscosmos ExoMars-2016 Trace Gas Orbiter and other missions. The talk will give the mission status, review the recent science highlights, and outline future plans.

Published
2017

47. Stringent upper limit of CH4 on Mars based on SOFIA/EXES observations

Author

Aoki, S., primary, Richter, M.J., additional, DeWitt, C., additional, Boogert, A., additional, Encrenaz, T., additional, Sagawa, H., additional, Nakagawa, H., additional, Vandaele, A. C., additional, Giuranna, M., additional, Greathouse, T. K., additional, Fouchet, T., additional, Geminale, A., additional, Sindoni, G., additional, McKelvey, M., additional, Case, M., additional, and Kasaba, Y., additional

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

Author

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

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

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

Published
2016

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

Author

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

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

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

Published
2015

50. The MARS EXPRESS Limbs Observations Database

Author

Gondet, Brigitte, Bibring, Jean-Pierre, Montmessin, Franck, Lefèvre, Franck, Lacombe, Gaetan, Giuranna, M., Aronica, A., Hoffmann, H., 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), 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), STRATO - LATMOS, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), DLR Institute of Planetary Research, German Aerospace Center (DLR), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES)

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

International audience; The capability to orient Mars Express makes it possible to implement a great diversity of observations modes, in particular nadir and limb (fig 1). During day and night limb's observations, 4 out of 7 MEX instruments (the spectrometers: SPICAM[1], OMEGA [2], PFS [3] and the high-resolution camera HRSC [4]) work together to provide spectra (.12 µm to 45 µm) of the Martian atmosphere (dust and clouds detached layers, day and night emissions), at each altitude step, with the associated image.. Fig 1 : Mars Express pointing modes relevant for limb observations by remote sensing instruments. Until now, the data reduction of observations of the limb from each Mars Express instrument had been done separately. Examples of the potential of each data set are given in Figures 2,3,4,5). We present here a database which makes it possible to retrieve the limb observations from different Mars Express instruments relevant for a given location and time frame. The limb database is now accessible to the scientific community via the ESA/PSA website (www.rssd.esa.int/PSA). Fig 2: detached layer observed by HRSC

Published
2015

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