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32 results on '"Réess, Jean-Michel"'

1. The SuperCam Infrared Spectrometer for the Perseverance Rover of the Mars2020 mission

Author

Fouchet, Thierry, Reess, Jean-Michel, Montmessin, Franck, Hassen-Khodja, Rafik, Nguyen-Tuong, Napoléon, Humeau, Olivier, Jacquinod, Sophie, Lapauw, Laurent, Parisot, Jérôme, Bonafous, Marion, Bernardi, Pernelle, Chapron, Frédéric, Jeanneau, Alexandre, Collin, Claude, Zeganadin, Didier, Nibert, Patricia, Abbaki, Sadok, Montaron, Christophe, Blanchard, Cyrille, Arslanyan, Vartan, Achelhi, Ourdya, Colon, Claudine, Royer, Clément, Hamm, Vincent, Bouzit, Mehdi, Poulet, François, Pilorget, Cédric, Mandon, Lucia, Forni, Olivier, Cousin, Agnès, Gasnault, Olivier, Pilleri, Paolo, Dubois, Bruno, Quantin, Cathy, Beck, Pierre, Beyssac, Olivier, Mouélic, Stéphane Le, Johnsson, Jeffrey R., McConnochie, Timothy H., Maurice, Sylvestre, and Wiens, Roger C.

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

We present the Infrared spectrometer of SuperCam Instrument Suite that enables the Mars 2020 Perseverance Rover to study remotely the Martian mineralogy within the Jezero crater. The SuperCam IR spectrometer is designed to acquire spectra in the 1.3-2.6 $\mu$m domain at a spectral resolution ranging from 5 to 20~nm. The field-of-view of 1.15 mrad, is coaligned with the boresights of the other remote-sensing techniques provided by SuperCam: laser-induced breakdown spectroscopy, remote time-resolved Raman and luminescence spectroscopies, and visible reflectance spectroscopy, and micro-imaging. The IR spectra can be acquired from the robotic-arm workspace to long-distances, in order to explore the mineralogical diversity of the Jezero crater, guide the Perseverance Rover in its sampling task, and to document the samples' environment. We present the design, the performance, the radiometric calibration, and the anticipated operations at the surface of Mars., Comment: Accepted for publication in Icarus

Published
2021
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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. Development of observation strategies from mission design to operations: illustration with Mars moons Explorer infrared spectrometer (MIRS)

Author

Sawyer, Eric, Barucci, Maria Antonietta, Rocard, Francis, Fornasier, Sonia, Doressoundiram, Alain, Piou, Véronique, Bernardi, Pernelle, Nakamura, Tomoki, Nakagawa, Hiromu, Iwata, Takahiro, Le Du, Michel, Reess, Jean-Michel, Jorda, Laurent, Nicolas, Théret, Pons, Nathalie, Donny, Christophe, Goulet, Sébastien, Jesus Martins Carriço, Inês De, and Canalias, Elisabet

Published
2023
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4. VUV test of a new polarimeter for spectropolarimetric measurements on board space missions

Author

Gal, Maelle Le, Pertenais, Martin, Ariste, Arturo Lopez, Neiner, Coralie, Champion, Norbert, Younes, Youssef, and Reess, Jean-Michel

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Optics
Abstract

High-resolution spectropolarimetry is a useful astronomical technique, in particular to study stellar magnetic fields. It has been extensively used in the past but mostly in the visible range. Space missions equipped with high-resolution spectropolarimeters working in the ultra-violet (UV) are now being studied. We propose a concept of a polarimeter working with temporal modulation and allowing to perform Stokes IQUV measurements over the full UV + Visible range. The purpose of this article is to describe the polarimeter concept, two prototypes and the bench developed to perform on ground testing to establish the performances of this new polarimeter.

Published
2019

5. The SuperCam infrared spectrometer for the perseverance rover of the Mars2020 mission

Author

Fouchet, Thierry, Reess, Jean-Michel, Montmessin, Franck, Hassen-Khodja, Rafik, Nguyen-Tuong, Napoléon, Humeau, Olivier, Jacquinod, Sophie, Lapauw, Laurent, Parisot, Jérôme, Bonafous, Marion, Bernardi, Pernelle, Chapron, Frédéric, Jeanneau, Alexandre, Collin, Claude, Zeganadin, Didier, Nibert, Patricia, Abbaki, Sadok, Montaron, Christophe, Blanchard, Cyrille, Arslanyan, Vartan, Achelhi, Ourdya, Colon, Claudine, Royer, Clément, Hamm, Vincent, Beuzit, Mehdi, Poulet, François, Pilorget, Cédric, Mandon, Lucia, Forni, Olivier, Cousin, Agnès, Gasnault, Olivier, Pilleri, Paolo, Dubois, Bruno, Quantin, Cathy, Beck, Pierre, Beyssac, Olivier, Le Mouélic, Stéphane, Johnsson, Jeffrey R., McConnochie, Timothy H., Maurice, Sylvestre, and Wiens, Roger C.

Published
2022
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6. Static spectropolarimeter concept adapted to space conditions and wide spectrum constraints

Author

Pertenais, Martin, Neiner, Coralie, Bernardi, Pernelle, Reess, Jean-Michel, and Petit, Pascal

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics, Physics - Optics, Physics - Space Physics
Abstract

The issues related to moving elements in space and instruments working in broader wavelength ranges lead to a need for robust polarimeters, efficient on a wide spectral domain, and adapted to space conditions. As part of the UVMag consortium, created to develop spectropolarimetric UV facilities in space, such as the Arago mission project, we present an innovative concept of static spectropolarimetry. We studied a static and polychromatic method for spectropolarimetry, applicable to stellar physics. Instead of modulating the polarization information temporally, as usually done in spectropolarimeters, the modulation is performed in a spatial direction, orthogonal to the spectral one. Thanks to the proportionality between phase retardance imposed by a birefringent material and its thickness, birefringent wedges can be used to create this spatial modulation. The light is then spectrally cross-dispersed, and a full-Stokes determination of the polarization over the whole spectrum can be obtained with a single-shot measurement. The use of Magnesium Fluoride wedges, for example, could lead to a compact, static polarimeter working at wavelengths from 0.115 mm up to 7 mm. We present the theory and simulations of this concept, as well as laboratory validation and a practical application to Arago., Comment: Article accepted for publication in Applied Optics on 20 July 2015

Published
2015
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7. 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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8. Could Jean-Dominique Cassini see the famous division in Saturn's rings?

Author

Lozi, Julien, Reess, Jean-Michel, Semery, Alain, Lhomé, Emilie, Jacquinod, Sophie, Combes, Michel, Bernardi, Pernelle, Andretta, Rémi, Motisi, Maxime, Bobis, Laurence, and Kaftan, Emilie

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

Nowadays, astronomers want to observe gaps in exozodiacal disks to confirm the presence of exoplanets, or even make actual images of these companions. Four hundred and fifty years ago, Jean-Dominique Cassini did a similar study on a closer object: Saturn. After joining the newly created Observatoire de Paris in 1671, he discovered 4 of Saturn's satellites (Iapetus, Rhea, Tethys and Dione), and also the gap in its rings. He made these discoveries observing through the best optics at the time, made in Italy by famous opticians like Giuseppe Campani or Eustachio Divini. But was he really able to observe this black line in Saturn's rings? That is what a team of optical scientists from Observatoire de Paris - LESIA with the help of Onera and Institut d'Optique tried to find out, analyzing the lenses used by Cassini, and still preserved in the collection of the observatory. The main difficulty was that even if the lenses have diameters between 84 and 239 mm, the focal lengths are between 6 and 50 m, more than the focal lengths of the primary mirrors of future ELTs. The analysis shows that the lenses have an exceptionally good quality, with a wavefront error of approximately 50 nm rms and 200 nm peak-to-valley, leading to Strehl ratios higher than 0.8. Taking into account the chromaticity of the glass, the wavefront quality and atmospheric turbulence, reconstructions of his observations tend to show that he was actually able to see the division named after him., Comment: 11 pages, 14 figures, proceedings of the SPIE conference Optics+Photonics, San Diego 2013

Published
2013
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9. SPICES: Spectro-Polarimetric Imaging and Characterization of Exoplanetary Systems

Author

Boccaletti, Anthony, Schneider, Jean, Traub, Wes, Lagage, Pierre-Olivier, Stam, Daphne, Gratton, Raffaele, Trauger, John, Cahoy, Kerri, Snik, Frans, Baudoz, Pierre, Galicher, Raphael, Reess, Jean-Michel, Mawet, Dimitri, Augereau, Jean-Charles, Patience, Jennifer, Kuchner, Marc, Wyatt, Mark, Pantin, Eric, Maire, Anne-Lise, Verinaud, Christophe, Ronayette, Samuel, Dubreuil, Didier, Min, Michiel, Rodenhuis, Michiel, Mesa, Dino, Belikov, Ruslan, Guyon, Olivier, Tamura, Motohide, Murakami, Naoshi, Beerer, Ingrid Mary, and team, the SPICES

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

SPICES (Spectro-Polarimetric Imaging and Characterization of Exoplanetary Systems) is a five-year M-class mission proposed to ESA Cosmic Vision. Its purpose is to image and characterize long-period extrasolar planets and circumstellar disks in the visible (450 - 900 nm) at a spectral resolution of about 40 using both spectroscopy and polarimetry. By 2020/22, present and near-term instruments will have found several tens of planets that SPICES will be able to observe and study in detail. Equipped with a 1.5 m telescope, SPICES can preferentially access exoplanets located at several AUs (0.5-10 AU) from nearby stars ($<$25 pc) with masses ranging from a few Jupiter masses to Super Earths ($\sim$2 Earth radii, $\sim$10 M$_{\oplus}$) as well as circumstellar disks as faint as a few times the zodiacal light in the Solar System.

Published
2012
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10. Current results of the PERSEE testbench: the cophasing control and the polychromatic null rate

Author

Lozi, Julien, Cassaing, Frederic, Duigou, Jean-Michel Le, Sorrente, Beatrice, Montri, Jospeh, Reess, Jean-Michel, Lhome, Emilie, Buey, Tristan, Henault, Francois, Marcotto, Aurelie, Girard, Paul, Barillot, Marc, Ollivier, Marc, and Foresto, Vincent Coude du

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Stabilizing a nulling interferometer at a nanometric level is the key issue to obtain deep null depths. The PERSEE breadboard has been designed to study and optimize the operation of a cophased nulling bench in the most realistic disturbing environment of a space mission. This presentation focuses on the current results of the PERSEE bench. In terms of metrology, we cophased at 0.33 nm rms for the piston and 80 mas rms for the tip/tilt (0.14% of the Airy disk). A Linear Quadratic Gaussian (LQG) control coupled with an unsupervised vibration identification allows us to maintain that level of correction, even with characteristic vibrations of nulling interferometry space missions. These performances, with an accurate design and alignment of the bench, currently lead to a polychromatic unpolarised null depth of 8.9E-6 stabilized at 3E-7 on the [1.65-2.45] \mum spectral band (37% bandwidth)., Comment: 17 pages, 10 figures, proceedings of the Optics+Photonics SPIE conference, San Diego, 2011

Published
2011
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11. PERSEE: Experimental results on the cophased nulling bench

Author

Lozi, Julien, Cassaing, Frédéric, Duigou, Jean-Michel Le, Houairi, Kamel, Sorrente, Béatrice, Montri, Joseph, Jacquinod, Sophie, Reess, Jean-Michel, Pham, Laurie, Lhomé, Emilie, Buey, Tristan, Hénault, François, Marcotto, Aurélie, Girard, Paul, Mauclert, Nicolas, Barillot, Marc, Foresto, Vincent Coudé du, and Ollivier, Marc

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Nulling interferometry is still a promising method to characterize spectra of exoplanets. One of the main issues is to cophase at a nanometric level each arm despite satellite disturbances. The bench PERSEE aims to prove the feasibility of that technique for spaceborne missions. After a short description of PERSEE, we will first present the results obtained in a simplified configuration: we have cophased down to 0.22 nm rms in optical path difference (OPD) and 60 mas rms in tip/tilt, and have obtained a monochromatic null of 3E-5 stabilized at 3E-6. The goal of 1 nm with additional typical satellite disturbances requires the use of an optimal control law; that is why we elaborated a dedicated Kalman filter. Simulations and experiments show a good rejection of disturbances. Performance of the bench should be enhanced by using a Kalman control law, and we should be able to reach the desired nanometric stability. Following, we will present the first results of the final polychromatic configuration, which includes an achromatic phase shifter, perturbators and optical delay lines. As a conclusion, we give the first more general lessons we have already learned from this experiment, both at system and component levels for a future space mission., Comment: 12 pages, 13 figures

Published
2010
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12. A chemical survey of exoplanets with ARIEL

Author

Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Heske, Astrid, Leconte, Jérémy, Micela, Giusi, Ollivier, Marc, Pilbratt, Göran, Puig, Ludovic, Turrini, Diego, Vandenbussche, Bart, Wolkenberg, Paulina, Beaulieu, Jean-Philippe, Buchave, Lars A., Ferus, Martin, Griffin, Matt, Guedel, Manuel, Justtanont, Kay, Lagage, Pierre-Olivier, Machado, Pedro, Malaguti, Giuseppe, Min, Michiel, Nørgaard-Nielsen, Hans Ulrik, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Swain, Mark, Szabo, Robert, Werner, Stephanie, Barstow, Joanna, Burleigh, Matt, Cho, James, du Foresto, Vincent Coudé, Coustenis, Athena, Decin, Leen, Encrenaz, Therese, Galand, Marina, Gillon, Michael, Helled, Ravit, Morales, Juan Carlos, Muñoz, Antonio García, Moneti, Andrea, Pagano, Isabella, Pascale, Enzo, Piccioni, Giuseppe, Pinfield, David, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Triaud, Amaury, Venot, Olivia, Waldmann, Ingo, Waltham, David, Wright, Gillian, Amiaux, Jerome, Auguères, Jean-Louis, Berthé, Michel, Bezawada, Naidu, Bishop, Georgia, Bowles, Neil, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Crouzet, Pierre-Elie, Da Peppo, Vania, Sanz, Isabel Escudero, Focardi, Mauro, Frericks, Martin, Hunt, Tom, Kohley, Ralf, Middleton, Kevin, Morgante, Gianluca, Ottensamer, Roland, Pace, Emanuele, Pearson, Chris, Stamper, Richard, Symonds, Kate, Rengel, Miriam, Renotte, Etienne, Ade, Peter, Affer, Laura, Alard, Christophe, Allard, Nicole, Altieri, Francesca, André, Yves, Arena, Claudio, Argyriou, Ioannis, Aylward, Alan, Baccani, Cristian, Bakos, Gaspar, Banaszkiewicz, Marek, Barlow, Mike, Batista, Virginie, Bellucci, Giancarlo, Benatti, Serena, Bernardi, Pernelle, Bézard, Bruno, Blecka, Maria, Bolmont, Emeline, Bonfond, Bertrand, Bonito, Rosaria, Bonomo, Aldo S., Brucato, John Robert, Brun, Allan Sacha, Bryson, Ian, Bujwan, Waldemar, Casewell, Sarah, Charnay, Bejamin, Pestellini, Cesare Cecchi, Chen, Guo, Ciaravella, Angela, Claudi, Riccardo, Clédassou, Rodolphe, Damasso, Mario, Damiano, Mario, Danielski, Camilla, Deroo, Pieter, Di Giorgio, Anna Maria, Dominik, Carsten, Doublier, Vanessa, Doyle, Simon, Doyon, René, Drummond, Benjamin, Duong, Bastien, Eales, Stephen, Edwards, Billy, Farina, Maria, Flaccomio, Ettore, Fletcher, Leigh, Forget, François, Fossey, Steve, Fränz, Markus, Fujii, Yuka, García-Piquer, Álvaro, Gear, Walter, Geoffray, Hervé, Gérard, Jean Claude, Gesa, Lluis, Gomez, H., Graczyk, Rafał, Griffith, Caitlin, Grodent, Denis, Guarcello, Mario Giuseppe, Gustin, Jacques, Hamano, Keiko, Hargrave, Peter, Hello, Yann, Heng, Kevin, Herrero, Enrique, Hornstrup, Allan, Hubert, Benoit, Ida, Shigeru, Ikoma, Masahiro, Iro, Nicolas, Irwin, Patrick, Jarchow, Christopher, Jaubert, Jean, Jones, Hugh, Julien, Queyrel, Kameda, Shingo, Kerschbaum, Franz, Kervella, Pierre, Koskinen, Tommi, Krijger, Matthijs, Krupp, Norbert, Lafarga, Marina, Landini, Federico, Lellouch, Emanuel, Leto, Giuseppe, Luntzer, A., Rank-Lüftinger, Theresa, Maggio, Antonio, Maldonado, Jesus, Maillard, Jean-Pierre, Mall, Urs, Marquette, Jean-Baptiste, Mathis, Stephane, Maxted, Pierre, Matsuo, Taro, Medvedev, Alexander, Miguel, Yamila, Minier, Vincent, Morello, Giuseppe, Mura, Alessandro, Narita, Norio, Nascimbeni, Valerio, Nguyen Tong, N., Noce, Vladimiro, Oliva, Fabrizio, Palle, Enric, Palmer, Paul, Pancrazzi, Maurizio, Papageorgiou, Andreas, Parmentier, Vivien, Perger, Manuel, Petralia, Antonino, Pezzuto, Stefano, Pierrehumbert, Ray, Pillitteri, Ignazio, Piotto, Giampaolo, Pisano, Giampaolo, Prisinzano, Loredana, Radioti, Aikaterini, Réess, Jean-Michel, Rezac, Ladislav, Rocchetto, Marco, Rosich, Albert, Sanna, Nicoletta, Santerne, Alexandre, Savini, Giorgio, Scandariato, Gaetano, Sicardy, Bruno, Sierra, Carles, Sindoni, Giuseppe, Skup, Konrad, Snellen, Ignas, Sobiecki, Mateusz, Soret, Lauriane, Sozzetti, Alessandro, Stiepen, A., Strugarek, Antoine, Taylor, Jake, Taylor, William, Terenzi, Luca, Tessenyi, Marcell, Tsiaras, Angelos, Tucker, C., Valencia, Diana, Vasisht, Gautam, Vazan, Allona, Vilardell, Francesc, Vinatier, Sabrine, Viti, Serena, Waters, Rens, Wawer, Piotr, Wawrzaszek, Anna, Whitworth, Anthony, Yung, Yuk L., Yurchenko, Sergey N., Osorio, María Rosa Zapatero, Zellem, Robert, Zingales, Tiziano, and Zwart, Frans

Published
2018
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13. The Venus Emissivity Mapper: implementation for flight on the NASA VERITAS mission

Author

Helbert, Jörn, primary, Pertenaïs, Martin, additional, Walter, Ingo, additional, Peter, Gisbert, additional, Säuberlich, Thomas, additional, Cacovean, Andrei, additional, Maturilli, Alessandro, additional, Alemanno, Giulia, additional, Zender, Bernd, additional, Arcos Carrasco, Carlos, additional, Dern, Patrick, additional, Pohl, Andreas, additional, Del Togno, Simone, additional, Rockstein, Steve, additional, Rosas-Ortiz, Yaquelin M., additional, Rufini Mastropasqua, Sergio, additional, Wendler, Dennis, additional, Westerdorff, Karsten, additional, Réess, Jean-Michel, additional, Pechevis, Eitan, additional, Carron, Jerome, additional, Buey, Tristan, additional, Widemann, Thomas, additional, Behnke, Thomas, additional, Wolff, Friederike, additional, Adeli, Solmaz, additional, D'Amore, Mario, additional, and Dyar, Melinda D., additional

Published
2022
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14. AIRS: ARIEL IR spectrometer status

Author

Martignac, Jérôme, primary, Amiaux, Jérôme, additional, Berthé, Michel, additional, Cara, Christophe, additional, Delisles, Cyrille, additional, Direk, Achrène, additional, Dumaye, Luc, additional, Fontignie, Jean, additional, Goestschy, Alain, additional, Horeau, Benoît, additional, Hurtado, Norma, additional, Huyn, Duc-Dat, additional, Kaszubiak, Grégory, additional, Lagage, Pierre-Olivier, additional, Le Mer, Isabelle, additional, Lortholary, Michel, additional, Moreau, Vincent, additional, Mouzali, Salima, additional, Mulet, Patrick, additional, Nico, François, additional, Pichon, Thibault, additional, Provost, Léna, additional, Renaud, Diana, additional, Schwartz, Victor, additional, Talvard, Michel, additional, Tourrette, Thierry, additional, Visticot, François, additional, Arhancet, Axel, additional, Bachet, Damien, additional, Berton, Nicolas, additional, Lacroix, Mickael, additional, Le Provost, Hervé, additional, Tellier, Olivier, additional, Philippon, Anne, additional, De Jabrun, Clémence, additional, Dubois, Jean-Pierre, additional, Langlet, François, additional, Le Claire, Dylan, additional, Lecomte, Benoît, additional, Ollivier, Marc, additional, Tosti, Stéphane, additional, Lapeyrère, Vincent, additional, Bonafous, Marion, additional, Parisot, Jérôme, additional, Réess, Jean-Michel, additional, Zegadanin, Didier, additional, Beaulieu, Jean-Philipe, additional, Batista, Virginie, additional, Drossart, Pierre, additional, Fahmy, Salma, additional, Jollet, Delphine, additional, Puig, Ludovic, additional, Tirolien, Thierry, additional, Danto, Pascale, additional, Hervet, Gilles, additional, Maisonnave, Oceane, additional, Eccleston, Paul, additional, Bishop, Georgia, additional, Drumond, Rachel, additional, Caldwell, Andrew, additional, Caldwell, Martin, additional, Desjonqueres, Lucile, additional, Whalley, Martin, additional, Pascale, Enzo, additional, Morgante, Gianluca, additional, Focardi, Mauro, additional, Pace, Emanuele, additional, and Di Giorgio, Anna-Maria, additional

Published
2022
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15. Observation opportunities for Mars atmosphere with the MIRS instrument aboard the Martian Moon eXploration mission

Author

Doressoundiram, Alain, Gautier, Thomas, Barucci, Maria, Aoki, Shohei, Lasue, Jérémie, Réess, Jean-Michel, Bernardi, Pernelle, Le Du, Michel, Sawyer, Eric, Iwata, Takahiro, Nakagawa, Hiromu, Nakamura, Tomoki, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institute of Space and Astronautical Science (ISAS), Japan Aerospace Exploration Agency [Sagamihara] (JAXA), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES), and Tohoku University [Sendai]

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

The Martian Moon eXploration mission (MMX), currently developed by the Japan Aerospace Exploration (JAXA) will aim at studying Mars satellites and return samples from Phobos to decipher the history of the Martian system. MMX mission is to be launched in September 2024 and arrive in Mars system on August 2025, will stay three years in Quasi Satellite Orbits (QSO) around Phobos, and will land for several hours on Phobos to collect at least 10g of Phobos regolith before returning to Earth. Among the mission instrument suite is the near-Infrared Spectrometer MIRS (MMX InfraRed Spectrometer) provided by CNES and built at LESIA-Paris Observatory in collaboration with four other French laboratories (LAB, LATMOS, LAM, IRAP-OMP) and in close collaboration with JAXA and MELCO. MIRS is an imaging spectrometer from 0.9 to 3.6 µm, with a spectral resolution better than 20 nm. The IFOV is 0.35 mrad and FOV of +/-1.65°. The SNR is higher than 100 up to 3.2 µm in a maximum integration time less than 2s. For Mars observation MIRS is expected to perform observations at 10 km spatial resolution, with a spectral radiometric absolute and relative accuracies of 10% and 1% respectively. Given MIRS spectral range, expected Signal-to-Noise ratio, and observation windows, a certain numbers of high priority targets have been set to achieve MMX goal of Constrain transport processes for dust and water near the Martian Surface, continuous observations of the mid-to low-latitude distributions of dust storms, ice clouds and water vapor in the Martian atmosphere (Barucci et al. 2021, Ogohara et al. 2021), summarized in Table 1. Simulated spectra of Martian atmosphere as observed by MIRS are provided in Figure 1. Table 1: List of MIRS main science targets for Mars observations (adapted from Barucci et al. 2021). Target Parameters Spectral range Ice cloud formation and evolution Water ice 1.5, 2 and 3 µm Dust clouds / storms formation and evolution Dust CO2 band @2.7 µm 0.9-3.6 µm continuum Water cycle H2O vapor 2.6 µm Atmospheric dynamics and composition Surface pressure CO2 band @ 2.0 µm CO 2.3 µm Limb observations for middle atmosphere O2 day-glow 1.27 µm Figure 1: Simulated MIRS spectra for typical Mars observation (from Barucci et al. 2021). Plain curves correspond to clear sky conditions, and the dashed ones include the effects of dust or water ice clouds. For gases, CO2, CO, and water vapor are calculated separately and reported in red, orange, and blue curves, respectively. MMX QSO around Phobos will result in a quasi-circular orbit around Mars with a period of ~7h, providing more than 3 hours window to Mars observation when Phobos observation is not possible. Several observation strategies, still in discussion, will be possible to maximize either temporal or spatial coverage of Mars and its atmosphere by MIRS. These strategies span from observations with a 30 minutes temporal resolution of a limited zone, to a complete coverage for low and mid latitude in a few orbits (Ogohara et al. 2021, Barucci et al. 2021). Limb observations may also be performed to obtain high vertical resolution observations of the Martian atmosphere. MIRS observations will provide further constraints on dust and water transport processes in the Martian atmosphere, by monitoring the distributions of dust content and storms, water ice clouds and water vapor. CO2 (and thus pressure) will be monitored through the CO2 2.0 µm band. Water vapor will be monitored on a daily basis using its 2.6 µm band (Maltagliati et al. 2008) and water ice clouds through their spectral features between 0.9 and 3.6 µm (Olsen et al. 2019). MIRS should also be able to detect CO 2.35 µm and O2 at 1.27 µm. MIRS spectra will also allow for estimations of the water adsorbed in the surface regolith. Finally, MIRS will be operated in close collaboration with the OROCHI (Optical Radiometer composed of Chromatic Imagers) and TENGOO (Telescopic Narrow Angle Camera) instruments. This will enable efficient monitoring and reactivity to investigate short lifespan events in Martian atmosphere. This will also render possible the investigation of CO2 clouds following the procedure proposed by Vincendon et al. 2011 for Mars Express observations. The reflectance spectrum from the light backscattered by atmospheric aerosols can be obtained by comparing successive observations of identical zones on Mars within a short time and with varying phase angles. Such a set of measurements permits to decorrelate the surface reflectance signal from the light scattered by the aerosols suspended in the atmosphere and gives information on the aerosols size and their composition properties averaged over the line of sight. Previous measurements showed a particle size distribution having an effective radius of 1.2±0.2 μm (Erard et al. 1994). The retrieved parameters include the scattering albedo, the phase function of the aerosols, the optical thickness, τ, of the atmosphere at the time of observation and the aerosols size distribution. In summary, MIRS observations, together with the ones from MSA, OROCHI and TENGOO, will help better understand the interdependencies of species and their roles in the Martian water, CO2 and dust cycles, thanks to long term monitoring of these key constituents of Mars atmosphere. References Barucci et al. 2021, MIRS an Imaging Spectrometer for the MMX mission, accepted for publication in Earth Planets and Space Erard, S., Mustard, J., Murchie, S., Bibring, J. P., Cerroni, P., & Coradini, A. (1994). Martian aerosols: Near-infrared spectral properties and effects on the observation of the surface. Icarus, 111(2), 317-337. Ogohara et al. 2021, The Mars system revealed by the Martian Moons eXploration mission, accepted for publication in Earth Planets and Space Vincendon et al. 2011, New near-IR observations of mesospheric CO2 and H2O clouds on Mars, JGR Planets 116, 0-02.

Published
2021

16. MIRS: an imaging spectrometer for MMX mission

Author

Bour, Aurélien, primary, Réess, Jean-Michel, additional, Bernardi, Pernelle, additional, Barucci, Maria Antonietta, additional, Castelnau, Matthieu, additional, Le Du, Michel, additional, Iwata, Takahiro, additional, Nakagawa, Hiromu, additional, Nakamura, Tomoki, additional, Doressoundiram, Alain, additional, and Fornasier, Sonia, additional

Published
2021
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17. Optical design and performance of the SuperCam instrument for the Perseverance rover

Author

Bernardi, Pernelle, primary, Parès, Laurent, additional, Newell, Raymond, additional, Nelson, Tony, additional, Gasnault, Olivier, additional, Réess, Jean-Michel, additional, Schridar, Vishnu, additional, Contijo, Ivair, additional, Reyes-Newell, Adriana, additional, Peterson, Glenn E., additional, Legett, Chip, additional, Dubois, Bruno, additional, and Robinson, Scott H., additional

Published
2021
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18. Thermal tests of birefringent plates in molecular adhesion for spatial ultra-violet polarimetry

Author

Le Gal, Maëlle, primary, Neiner, Coralie, additional, Louvel de Monceaux, Matthieu, additional, Nguyen-Tuong, Napoléon, additional, Parisot, Jérôme, additional, Collin, Claude, additional, Réess, Jean-Michel, additional, Bonafous, Marion, additional, Blanchard, Cyrille, additional, Pelleau, Aurélien, additional, Baudoz, Pierre, additional, Pertenais, Martin, additional, Costes, Vincent, additional, Brachet, Frank, additional, Locatelli, Elsa, additional, and Desmarres, Jean-Michel, additional

Published
2020
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23. Wedge filter imaging spectrometer

Author

Sémery, Alain, primary, Réess, Jean-Michel, additional, Lemarquis, Frédéric, additional, Drossart, Pierre, additional, Laubier, David, additional, and Bernardi, Pernelle, additional

Published
2017
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24. Final results of the PERSEE experiment

Author

Le Duigou, J.-M., primary, Lozi, J., primary, Cassaing, Frédéric, primary, Montri, J., primary, Lhomé, E., primary, Buey, T., primary, Hénault, F., primary, Girard, P., primary, Barillot, M., primary, Houairi, K., primary, Sorrente, B., primary, Jacquinod, S., primary, Réess, Jean-Michel, primary, Pham, L., primary, Marcotto, A., primary, Mauclert, N., primary, Coudé du Foresto, V., primary, and Ollivier, M., primary

Published
2017
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27. The science of EChO

Author

Tinetti , Giovanna, Cho , James Y.-K., Griffith , Caitlin A., Grasset , Olivier, Grenfell , Lee, Guillot , Tristan, Koskinen , Tommi T., Moses , Julianne I., Pinfield , David, Tennyson , Jonathan, Tessenyi , Marcell, Wordsworth , Robin, Aylward , Alan, Van Boekel , Roy, Coradini , Angioletta, Encrenaz , Therese, Snellen , Ignas, Zapatero-Osorio , Maria R., Bouwman , Jeroen, Du Foresto , Vincent Coudé, Lopez-Morales , Mercedes, Mueller-Wodarg , Ingo, Pallé , Enric, Selsis , Franck, Sozzetti , Alessandro, Beaulieu , Jean-Philippe, Henning , Thomas, Meyer , Michael, Micela , Giuseppina, Ribas , Ignasi, Stam , Daphne, Swain , Mark, Krause , Oliver, Ollivier , Marc, Pace , Emanuele, Swinyard , Bruce, Ade , Peter A. R., Achilleos , Nick, Adriani , Alberto, Agnor , Craig B., Afonso , Cristina, Prieto , Carlos Allende, Bakos , Gaspar, Barber , Robert J., Barlow , Michael, Bernath , Peter, Bézard , Bruno, Bordé , Pascal, Brown , Linda R., Cassan , Arnaud, Cavarroc , Céline, Ciaravella , Angela, Cockell , Charles, Coustenis , Athéna, Danielski , Camilla, Decin , Leen, De Kok , Remco, Demangeon , Olivier, Deroo , Pieter, Doel , Peter, Drossart , Pierre, Fletcher , Leigh N., Focardi , Matteo, Forget , Francois, Fossey , Steve, Fouqué , Pascal, Frith , James, Galand , Marina, Gaulme , Patrick, Hernández , Jonay I. González, Grassi , Davide, Griffin , Matt J., Grözinger , Ulrich, Guedel , Manuel, Guio , Pactrick, Hainaut , Olivier, Hargreaves , Robert, Hauschildt , Peter H., Heng , Kevin, Heyrovsky , David, Hueso , Ricardo, Irwin , Pat, Kaltenegger , Lisa, Kervella , Patrick, Kipping , David, Kovacs , Geza, Barbera , Antonino La, Lammer , Helmut, Lellouch , Emmanuel, Leto , Giuseppe, Morales , Mercedes Lopez, Valverde , Miguel A. Lopez, Lopez-Puertas , Manuel, Lovi , Christophe, Maggio , Antonio, Maillard , Jean-Pierre, Prado , Jesus Maldonado, Marquette , Jean-Baptiste, Martin-Torres , Francisco J., Maxted , Pierre, Miller , Steve, Molinari , Sergio, Montes , David, Moro-Martin , Amaya, Mousis , Olivier, Tuong , Napoléon Nguyen, Nelson , Richard, Orton , Glenn S., Pantin , Eric, Pascale , Enzo, Pezzuto , Stefano, Poretti , Ennio, Prinja , Raman, Prisinzano , Loredana, Réess , Jean-Michel, Reiners , Ansgar, Samuel , Benjamin, Forcada , Jorge Sanz, Sasselov , Dimitar, Savini , Giorgio, Sicardy , Bruno, Smith , Alan, Stixrude , Lars, Strazzulla , Giovanni, Vasisht , Gautam, Vinatier , Sandrine, Viti , Serena, Waldmann , Ingo, White , Glenn J., Widemann , Thomas, Yelle , Roger, Yung , Yuk, Yurchenko , Sergey, University College of London [London] ( UCL ), Lunar and Planetary Laboratory [Tucson], University of Arizona, Laboratoire de Planétologie et Géodynamique de Nantes ( LPGN ), Université de Nantes ( UN ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides ( CASSIOPEE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Department of Physics and Astronomy [UCL London], Laboratoire de Météorologie Dynamique (UMR 8539) ( LMD ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -École polytechnique ( X ) -École des Ponts ParisTech ( ENPC ) -Centre National de la Recherche Scientifique ( CNRS ) -Département des Géosciences - ENS Paris, École normale supérieure - Paris ( ENS Paris ) -École normale supérieure - Paris ( ENS Paris ), Istituto di Fisica dello Spazio Interplanetario ( INAF ), Consiglio Nazionale delle Ricerche [Roma] ( CNR ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Département d'Astrophysique (ex SAP) ( DAP ), Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Institut d'Astrophysique de Paris ( IAP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Max-Planck-Institut für Astronomie ( MPIA ), Liquides Ioniques et Interfaces Chargées ( LI2C ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -ESPCI ParisTech-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astronomico di Palermo ( OAPa ), Istituto Nazionale di Astrofisica ( INAF ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), SRON Netherlands Institute for Space Research ( SRON ), University of Calgary, 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 ), School of Physics and Astronomy [London], Queen Mary University of London ( QMUL ), Jet Propulsion Laboratory ( JPL ), NASA-California Institute of Technology ( CALTECH ), Astronomische Rechen-Institut [Heidelberg] ( ARI ), Universität Heidelberg [Heidelberg]-Zentrum für Astronomie der Universität Heidelberg, Planetary and Space Sciences Research Institute [Milton Keynes] ( PSSRI ), Centre for Earth, Planetary, Space and Astronomical Research [Milton Keynes] ( CEPSAR ), The Open University [Milton Keynes] ( OU ) -The Open University [Milton Keynes] ( OU ), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] ( AOPP ), University of Oxford [Oxford], Institut Pierre-Simon-Laplace ( IPSL ), École normale supérieure - Paris ( ENS Paris ) -Université de Versailles Saint-Quentin-en-Yvelines ( UVSQ ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Centre National d'Etudes Spatiales ( CNES ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Astrophysique de Toulouse-Tarbes ( LATT ), Université Paul Sabatier - Toulouse 3 ( UPS ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Blackett Laboratory, Imperial College London, Istituto di Fisica dello Spazio Interplanetaro ( IFSI ), Escuela Superior de Ingenieria, Universidad del País Vasco, Harvard-Smithsonian Center for Astrophysics ( CfA ), Harvard University [Cambridge]-Smithsonian Institution, Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), Department of Science and Technology Studies [London] ( STS ), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules ( UTINAM ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Franche-Comté ( UFC ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Institut Universitaire de France ( IUF ), Ministère de l'Éducation nationale, de l’Enseignement supérieur et de la Recherche ( M.E.N.E.S.R. ), Imperial College Healthcare NHS Trust, STFC Rutherford Appleton Laboratory ( RAL ), Science and Technology Facilities Council ( STFC ), Department of Physics and Astronomy [Milton Keynes], and The Open University [Milton Keynes] ( OU )

Subjects
[ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Instrumentation and Methods for Astrophysics, planets and satellites: formation, planets and satellites: general, Astrophysics::Earth and Planetary Astrophysics, planetary systems, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], planetary systems: formation
Abstract

International audience; The science of extra-solar planets is one of the most rapidly changing areas of astrophysics and since 1995 the number of planets known has increased by almost two orders of magnitude. A combination of ground-based surveys and dedicated space missions has resulted in 560-plus planets being detected, and over 1200 that await confirmation. NASA's Kepler mission has opened up the possibility of discovering Earth-like planets in the habitable zone around some of the 100,000 stars it is surveying during its 3 to 4-year lifetime. The new ESA's Gaia mission is expected to discover thousands of new planets around stars within 200 parsecs of the Sun. The key challenge now is moving on from discovery, important though that remains, to characterisation: what are these planets actually like, and why are they as they are? In the past ten years, we have learned how to obtain the first spectra of exoplanets using transit transmission and emission spectroscopy. With the high stability of Spitzer, Hubble, and large ground-based telescopes the spectra of bright close-in massive planets can be obtained and species like water vapour, methane, carbon monoxide and dioxide have been detected. With transit science came the first tangible remote sensing of these planetary bodies and so one can start to extrapolate from what has been learnt from Solar System probes to what one might plan to learn about their faraway siblings. As we learn more about the atmospheres, surfaces and near-surfaces of these remote bodies, we will begin to build up a clearer picture of their construction, history and suitability for life. The Exoplanet Characterisation Observatory, EChO, will be the first dedicated mission to investigate the physics and chemistry of Exoplanetary Atmospheres. By characterising spectroscopically more bodies in different environments we will take detailed planetology out of the Solar System and into the Galaxy as a whole. EChO has now been selected by the European Space Agency to be assessed as one of four M3 mission candidates.

Published
2010

28. The science of EChO

Author

Tinetti, Giovanna, primary, Cho, James Y-K., additional, Griffith, Caitlin A., additional, Grasset, Olivier, additional, Grenfell, Lee, additional, Guillot, Tristan, additional, Koskinen, Tommi T., additional, Moses, Julianne I., additional, Pinfield, David, additional, Tennyson, Jonathan, additional, Tessenyi, Marcell, additional, Wordsworth, Robin, additional, Aylward, Alan, additional, van Boekel, Roy, additional, Coradini, Angioletta, additional, Encrenaz, Therese, additional, Snellen, Ignas, additional, Zapatero-Osorio, Maria R., additional, Bouwman, Jeroen, additional, du Foresto, Vincent Coudé, additional, Lopez-Morales, Mercedes, additional, Mueller-Wodarg, Ingo, additional, Pallé, Enric, additional, Selsis, Franck, additional, Sozzetti, Alessandro, additional, Beaulieu, Jean-Philippe, additional, Henning, Thomas, additional, Meyer, Michael, additional, Micela, Giuseppina, additional, Ribas, Ignasi, additional, Stam, Daphne, additional, Swain, Mark, additional, Krause, Oliver, additional, Ollivier, Marc, additional, Pace, Emanuele, additional, Swinyard, Bruce, additional, Ade, Peter A.R., additional, Achilleos, Nick, additional, Adriani, Alberto, additional, Agnor, Craig B., additional, Afonso, Cristina, additional, Prieto, Carlos Allende, additional, Bakos, Gaspar, additional, Barber, Robert J., additional, Barlow, Michael, additional, Bernath, Peter, additional, Bézard, Bruno, additional, Bordé, Pascal, additional, Brown, Linda R., additional, Cassan, Arnaud, additional, Cavarroc, Céline, additional, Ciaravella, Angela, additional, Cockell, Charles, additional, Coustenis, Athéna, additional, Danielski, Camilla, additional, Decin, Leen, additional, De Kok, Remco, additional, Demangeon, Olivier, additional, Deroo, Pieter, additional, Doel, Peter, additional, Drossart, Pierre, additional, Fletcher, Leigh N., additional, Focardi, Matteo, additional, Forget, Francois, additional, Fossey, Steve, additional, Fouqué, Pascal, additional, Frith, James, additional, Galand, Marina, additional, Gaulme, Patrick, additional, Hernández, Jonay I. González, additional, Grassi, Davide, additional, Griffin, Matt J., additional, Grözinger, Ulrich, additional, Guedel, Manuel, additional, Guio, Pactrick, additional, Hainaut, Olivier, additional, Hargreaves, Robert, additional, Hauschildt, Peter H., additional, Heng, Kevin, additional, Heyrovsky, David, additional, Hueso, Ricardo, additional, Irwin, Pat, additional, Kaltenegger, Lisa, additional, Kervella, Patrick, additional, Kipping, David, additional, Kovacs, Geza, additional, Barbera, Antonino La, additional, Lammer, Helmut, additional, Lellouch, Emmanuel, additional, Leto, Giuseppe, additional, Morales, Mercedes Lopez, additional, Valverde, Miguel A. Lopez, additional, Lopez-Puertas, Manuel, additional, Lovi, Christophe, additional, Maggio, Antonio, additional, Maillard, Jean-Pierre, additional, Prado, Jesus Maldonado, additional, Marquette, Jean-Baptiste, additional, Martin-Torres, Francisco J., additional, Maxted, Pierre, additional, Miller, Steve, additional, Molinari, Sergio, additional, Montes, David, additional, Moro-Martin, Amaya, additional, Mousis, Olivier, additional, Tuong, Napoléon Nguyen, additional, Nelson, Richard, additional, Orton, Glenn S., additional, Pantin, Eric, additional, Pascale, Enzo, additional, Pezzuto, Stefano, additional, Poretti, Ennio, additional, Prinja, Raman, additional, Prisinzano, Loredana, additional, Réess, Jean-Michel, additional, Reiners, Ansgar, additional, Samuel, Benjamin, additional, Forcada, Jorge Sanz, additional, Sasselov, Dimitar, additional, Savini, Giorgio, additional, Sicardy, Bruno, additional, Smith, Alan, additional, Stixrude, Lars, additional, Strazzulla, Giovanni, additional, Vasisht, Gautam, additional, Vinatier, Sandrine, additional, Viti, Serena, additional, Waldmann, Ingo, additional, White, Glenn J., additional, Widemann, Thomas, additional, Yelle, Roger, additional, Yung, Yuk, additional, and Yurchenko, Sergey, additional

Published
2010
Full Text
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30. A chemical survey of exoplanets with ARIEL

Author

Tinetti, Giovanna, Drossart, Pierre, Eccleston, Paul, Hartogh, Paul, Heske, Astrid, Leconte, Jérémy, Micela, Giusi, Ollivier, Marc, Pilbratt, Göran, Puig, Ludovic, Turrini, Diego, Vandenbussche, Bart, Wolkenberg, Paulina, Beaulieu, Jean-Philippe, Buchave, Lars A., Ferus, Martin, Griffin, Matt, Guedel, Manuel, Justtanont, Kay, Lagage, Pierre-Olivier, Machado, Pedro, Malaguti, Giuseppe, Min, Michiel, Nørgaard-Nielsen, Hans Ulrik, Rataj, Mirek, Ray, Tom, Ribas, Ignasi, Swain, Mark, Szabo, Robert, Werner, Stephanie, Barstow, Joanna, Burleigh, Matt, Cho, James, Du Foresto, Vincent Coudé, Coustenis, Athena, Decin, Leen, Encrenaz, Therese, Galand, Marina, Gillon, Michael, Helled, Ravit, Morales, Juan Carlos, Muñoz, Antonio García, Moneti, Andrea, Pagano, Isabella, Pascale, Enzo, Piccioni, Giuseppe, Pinfield, David, Sarkar, Subhajit, Selsis, Franck, Tennyson, Jonathan, Triaud, Amaury, Venot, Olivia, Waldmann, Ingo, Waltham, David, Wright, Gillian, Amiaux, Jerome, Auguères, Jean-Louis, Berthé, Michel, Bezawada, Naidu, Bishop, Georgia, Bowles, Neil, Coffey, Deirdre, Colomé, Josep, Crook, Martin, Crouzet, Pierre-Elie, Da Peppo, Vania, Sanz, Isabel Escudero, Focardi, Mauro, Frericks, Martin, Hunt, Tom, Kohley, Ralf, Middleton, Kevin, Morgante, Gianluca, Ottensamer, Roland, Pace, Emanuele, Pearson, Chris, Stamper, Richard, Symonds, Kate, Rengel, Miriam, Renotte, Etienne, Ade, Peter, Affer, Laura, Alard, Christophe, Allard, Nicole, Altieri, Francesca, André, Yves, Arena, Claudio, Argyriou, Ioannis, Aylward, Alan, Baccani, Cristian, Bakos, Gaspar, Banaszkiewicz, Marek, Barlow, Mike, Batista, Virginie, Bellucci, Giancarlo, Benatti, Serena, Bernardi, Pernelle, Bézard, Bruno, Blecka, Maria, Bolmont, Emeline, Bonfond, Bertrand, Bonito, Rosaria, Bonomo, Aldo S., Brucato, John Robert, Brun, Allan Sacha, Bryson, Ian, Bujwan, Waldemar, Casewell, Sarah, Charnay, Bejamin, Pestellini, Cesare Cecchi, Chen, Guo, Ciaravella, Angela, Claudi, Riccardo, Clédassou, Rodolphe, Damasso, Mario, Damiano, Mario, Danielski, Camilla, Deroo, Pieter, Di Giorgio, Anna Maria, Dominik, Carsten, Doublier, Vanessa, Doyle, Simon, Doyon, René, Drummond, Benjamin, Duong, Bastien, Eales, Stephen, Edwards, Billy, Farina, Maria, Flaccomio, Ettore, Fletcher, Leigh, Forget, François, Fossey, Steve, Fränz, Markus, Fujii, Yuka, García-Piquer, Álvaro, Gear, Walter, Geoffray, Hervé, Gérard, Jean Claude, Gesa, Lluis, Gomez, H., Graczyk, Rafał, Griffith, Caitlin, Grodent, Denis, Guarcello, Mario Giuseppe, Gustin, Jacques, Hamano, Keiko, Hargrave, Peter, Hello, Yann, Heng, Kevin, Herrero, Enrique, Hornstrup, Allan, Hubert, Benoit, Ida, Shigeru, Ikoma, Masahiro, Iro, Nicolas, Irwin, Patrick, Jarchow, Christopher, Jaubert, Jean, Jones, Hugh, Julien, Queyrel, Kameda, Shingo, Kerschbaum, Franz, Kervella, Pierre, Koskinen, Tommi, Krijger, Matthijs, Krupp, Norbert, Lafarga, Marina, Landini, Federico, Lellouch, Emanuel, Leto, Giuseppe, Luntzer, A., Rank-Lüftinger, Theresa, Maggio, Antonio, Maldonado, Jesus, Maillard, Jean-Pierre, Mall, Urs, Marquette, Jean-Baptiste, Mathis, Stephane, Maxted, Pierre, Matsuo, Taro, Medvedev, Alexander, Miguel, Yamila, Minier, Vincent, Morello, Giuseppe, Mura, Alessandro, Narita, Norio, Nascimbeni, Valerio, Nguyen Tong, N., Noce, Vladimiro, Oliva, Fabrizio, Palle, Enric, Palmer, Paul, Pancrazzi, Maurizio, Papageorgiou, Andreas, Parmentier, Vivien, Perger, Manuel, Petralia, Antonino, Pezzuto, Stefano, Pierrehumbert, Ray, Pillitteri, Ignazio, Piotto, Giampaolo, Pisano, Giampaolo, Prisinzano, Loredana, Radioti, Aikaterini, Réess, Jean-Michel, Rezac, Ladislav, Rocchetto, Marco, Rosich, Albert, Sanna, Nicoletta, Santerne, Alexandre, Savini, Giorgio, Scandariato, Gaetano, Sicardy, Bruno, Sierra, Carles, Sindoni, Giuseppe, Skup, Konrad, Snellen, Ignas, Sobiecki, Mateusz, Soret, Lauriane, Sozzetti, Alessandro, Stiepen, A., Strugarek, Antoine, Taylor, Jake, Taylor, William, Terenzi, Luca, Tessenyi, Marcell, Tsiaras, Angelos, Tucker, C., Valencia, Diana, Vasisht, Gautam, Vazan, Allona, Vilardell, Francesc, Vinatier, Sabrine, Viti, Serena, Waters, Rens, Wawer, Piotr, Wawrzaszek, Anna, Whitworth, Anthony, Yung, Yuk L., Yurchenko, Sergey N., Osorio, María Rosa Zapatero, Zellem, Robert, Zingales, Tiziano, and Zwart, Frans

Subjects
13. Climate action, 530 Physics, 520 Astronomy, Astrophysics::Earth and Planetary Astrophysics, 500 Science, 7. Clean energy
Abstract

Thousands of exoplanets have now been discovered with a huge range of masses, sizes and orbits: from rocky Earth-like planets to large gas giants grazing the surface of their host star. However, the essential nature of these exoplanets remains largely mysterious: there is no known, discernible pattern linking the presence, size, or orbital parameters of a planet to the nature of its parent star. We have little idea whether the chemistry of a planet is linked to its formation environment, or whether the type of host star drives the physics and chemistry of the planet’s birth, and evolution. ARIEL was conceived to observe a large number (~1000) of transiting planets for statistical understanding, including gas giants, Neptunes, super-Earths and Earth-size planets around a range of host star types using transit spectroscopy in the 1.25–7.8 μm spectral range and multiple narrow-band photometry in the optical. ARIEL will focus on warm and hot planets to take advantage of their well-mixed atmospheres which should show minimal condensation and sequestration of high-Z materials compared to their colder Solar System siblings. Said warm and hot atmospheres are expected to be more representative of the planetary bulk composition. Observations of these warm/hot exoplanets, and in particular of their elemental composition (especially C, O, N, S, Si), will allow the understanding of the early stages of planetary and atmospheric formation during the nebular phase and the following few million years. ARIEL will thus provide a representative picture of the chemical nature of the exoplanets and relate this directly to the type and chemical environment of the host star. ARIEL is designed as a dedicated survey mission for combined-light spectroscopy, capable of observing a large and well-defined planet sample within its 4-year mission lifetime. Transit, eclipse and phase-curve spectroscopy methods, whereby the signal from the star and planet are differentiated using knowledge of the planetary ephemerides, allow us to measure atmospheric signals from the planet at levels of 10–100 part per million (ppm) relative to the star and, given the bright nature of targets, also allows more sophisticated techniques, such as eclipse mapping, to give a deeper insight into the nature of the atmosphere. These types of observations require a stable payload and satellite platform with broad, instantaneous wavelength coverage to detect many molecular species, probe the thermal structure, identify clouds and monitor the stellar activity. The wavelength range proposed covers all the expected major atmospheric gases from e.g. H₂O, CO₂, CH₄ NH₃, HCN, H₂S through to the more exotic metallic compounds, such as TiO, VO, and condensed species. Simulations of ARIEL performance in conducting exoplanet surveys have been performed – using conservative estimates of mission performance and a full model of all significant noise sources in the measurement – using a list of potential ARIEL targets that incorporates the latest available exoplanet statistics. The conclusion at the end of the Phase A study, is that ARIEL – in line with the stated mission objectives – will be able to observe about 1000 exoplanets depending on the details of the adopted survey strategy, thus confirming the feasibility of the main science objectives.

32. A dynamic upper atmosphere of Venus as revealed by VIRTIS on Venus Express.

Author

Drossart P, Piccioni G, Gérard JC, Lopez-Valverde MA, Sanchez-Lavega A, Zasova L, Hueso R, Taylor FW, Bézard B, Adriani A, Angrilli F, Arnold G, Baines KH, Bellucci G, Benkhoff J, Bibring JP, Blanco A, Blecka MI, Carlson RW, Coradini A, Di Lellis A, Encrenaz T, Erard S, Fonti S, Formisano V, Fouchet T, Garcia R, Haus R, Helbert J, Ignatiev NI, Irwin P, Langevin Y, Lebonnois S, Luz D, Marinangeli L, Orofino V, Rodin AV, Roos-Serote MC, Saggin B, Stam DM, Titov D, Visconti G, Zambelli M, Tsang C, Ammannito E, Barbis A, Berlin R, Bettanini C, Boccaccini A, Bonnello G, Bouyé M, Capaccioni F, Cardesin A, Carraro F, Cherubini G, Cosi M, Dami M, De Nino M, Del Vento D, Di Giampietro M, Donati A, Dupuis O, Espinasse S, Fabbri A, Fave A, Veltroni IF, Filacchione G, Garceran K, Ghomchi Y, Giustizi M, Gondet B, Hello Y, Henry F, Hofer S, Huntzinger G, Kachlicki J, Knoll R, Kouach D, Mazzoni A, Melchiorri R, Mondello G, Monti F, Neumann C, Nuccilli F, Parisot J, Pasqui C, Perferi S, Peter G, Piacentino A, Pompei C, Réess JM, Rivet JP, Romano A, Russ N, Santoni M, Scarpelli A, Sémery A, Soufflot A, Stefanovitch D, Suetta E, Tarchi F, Tonetti N, Tosi F, and Ulmer B

Abstract

The upper atmosphere of a planet is a transition region in which energy is transferred between the deeper atmosphere and outer space. Molecular emissions from the upper atmosphere (90-120 km altitude) of Venus can be used to investigate the energetics and to trace the circulation of this hitherto little-studied region. Previous spacecraft and ground-based observations of infrared emission from CO2, O2 and NO have established that photochemical and dynamic activity controls the structure of the upper atmosphere of Venus. These data, however, have left unresolved the precise altitude of the emission owing to a lack of data and of an adequate observing geometry. Here we report measurements of day-side CO2 non-local thermodynamic equilibrium emission at 4.3 microm, extending from 90 to 120 km altitude, and of night-side O2 emission extending from 95 to 100 km. The CO2 emission peak occurs at approximately 115 km and varies with solar zenith angle over a range of approximately 10 km. This confirms previous modelling, and permits the beginning of a systematic study of the variability of the emission. The O2 peak emission happens at 96 km +/- 1 km, which is consistent with three-body recombination of oxygen atoms transported from the day side by a global thermospheric sub-solar to anti-solar circulation, as previously predicted.

Published
2007
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