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1. The Mid-Infrared Instrument for the James Webb Space Telescope, V: Predicted Performance of the MIRI Coronagraphs

Author: Boccaletti, A., Lagage, P. -O., Baudoz, P., Beichman, C., Bouchet, P., Cavarroc, C., Dubreuil, D., Glasse, Alistair, Glauser, A. M., Hines, D. C., Lajoie, C. -P., Lebreton, J., Perrin, M. D., Pueyo, L., Reess, J. M., Rieke, G. H., Ronayette, S., Rouan, D., Soummer, R., and Wright, G. S.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The imaging channel on the Mid-Infrared Instrument (MIRI) is equipped with four coronagraphs that provide high contrast imaging capabilities for studying faint point sources and extended emission that would otherwise be overwhelmed by a bright point-source in its vicinity. Such bright sources might include stars that are orbited by exoplanets and circumstellar material, mass-loss envelopes around post-main-sequence stars, the near-nuclear environments in active galaxies, and the host galaxies of distant quasars. This paper describes the coronagraphic observing modes of MIRI, as well as performance estimates based on measurements of the MIRI flight model during cryo-vacuum testing. A brief outline of coronagraphic operations is also provided. Finally, simulated MIRI coronagraphic observations of a few astronomical targets are presented for illustration.
Published: 2015
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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. Transiting exoplanets from the CoRoT space mission: XXVI. CoRoT-24: A transiting multi-planet system

Author: Alonso, R., Moutou, C., Endl, M., Almenara, J. M., Guenther, E. W., Deleuil, M., Hatzes, A., Aigrain, S., Auvergne, M., Baglin, A., Barge, P., Bonomo, A. S., Bordé, P., Bouchy, F., Cavarroc, C., Cabrera, J., Carpano, S., Csizmadia, Sz., Cochran, W. D., Deeg, H. J., Díaz, R. F., Dvorak, R., Erikson, A., Ferraz-Mello, S., Fridlund, M., Fruth, T., Gandolfi, D., Gillon, M., Grziwa, S., Guillot, T., Hébrard, G., Jorda, L., Léger, A., Lammer, H., Lovis, C., MacQueen, P. J., Mazeh, T., Ofir, A., Ollivier, M., Pasternacki, T., Patzold, M., Queloz, D., Rauer, H., Rouan, D., Santerne, A., Schneider, J., Santos, M. Tadeu dos, Tingley, B., Titz-Weider, R., Weingrill, J., and Wuchterl, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of a candidate multiply-transiting system, the first one found in the CoRoT mission. Two transit-like features with periods of 5.11 and 11.76d are detected in the CoRoT light curve, around a main sequence K1V star of r=15.1. If the features are due to transiting planets around the same star, these would correspond to objects of 3.7$\pm$0.4 and 5.0$\pm$0.5 R_earth respectively. Several radial velocities serve to provide an upper limit of 5.7 M_earth for the 5.11~d signal, and to tentatively measure a mass of 28$^{+11}_{-11}$ M_earth for the object transiting with a 11.76~d period. These measurements imply low density objects, with a significant gaseous envelope. The detailed analysis of the photometric and spectroscopic data serve to estimate the probability that the observations are caused by transiting Neptune-sized planets as $>$26$\times$ higher than a blend scenario involving only one transiting planet, and $>$900$\times$ higher than a scenario involving two blends and no planets. The radial velocities show a long term modulation that might be attributed to a 1.5 M_jup planet orbiting at 1.8~A.U. from the host, but more data are required to determine the precise orbital parameters of this companion., Comment: 13 pages, 13 figures, accepted to A&A, minor typos corrected
Published: 2014
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4. EChO - Exoplanet Characterisation Observatory

Author: Tinetti, G., Beaulieu, J. P., Henning, T., Meyer, M., Micela, G., Ribas, I., Stam, D., Swain, M., Krause, O., Ollivier, M., Pace, E., Swinyard, B., Aylward, A., van Boekel, R., Coradini, A., Encrenaz, T., Snellen, I., Zapatero-Osorio, M. R., Bouwman, J., Cho, J. Y-K., Foresto, V. Coudé du, Guillot, T., Lopez-Morales, M., Mueller-Wodarg, I., Palle, E., Selsis, F., Sozzetti, A., Ade, P. A. R., Achilleos, N., Adriani, A., Agnor, C. B., Afonso, C., Prieto, C. Allende, Bakos, G., Barber, R. J., Barlow, M., Bernath, P., Bezard, B., Bordé, P., Brown, L. R., Cassan, A., Cavarroc, C., Ciaravella, A., Cockell, C. O. U., Coustenis, A., Danielski, C., Decin, L., De Kok, R., Demangeon, O., Deroo, P., Doel, P., Drossart, P., Fletcher, L. N., Focardi, M., Forget, F., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gaulme, P., Hernández, J. I. González, Grasset, O., Grassi, D., Grenfell, J. L., Griffin, M. J., Griffith, C. A., Grözinger, U., Guedel, M., Guio, P., Hainaut, O., Hargreaves, R., Hauschildt, P. H., Heng, K., Heyrovsky, D., Hueso, R., Irwin, P., Kaltenegger, L., Kervella, P., Kipping, D., Koskinen, T. T., Kovács, G., La Barbera, A., Lammer, H., Lellouch, E., Leto, G., Morales, M. Lopez, Valverde, M. A. Lopez, Lopez-Puertas, M., Lovis, C., Maggio, A., Maillard, J. P., Prado, J. Maldonado, Marquette, J. B., Martin-Torres, F. J., Maxted, P., Miller, S., Molinari, S., Montes, D., Moro-Martin, A., Moses, J. I., Mousis, O., Tuong, N. Nguyen, Nelson, R., Orton, G. S., Pantin, E., Pascale, E., Pezzuto, S., Pinfield, D., Poretti, E., Prinja, R., Prisinzano, L., Rees, J. M., Reiners, A., Samuel, B., Sanchez-Lavega, A., Forcada, J. Sanz, Sasselov, D., Savini, G., Sicardy, B., Smith, A., Stixrude, L., Strazzulla, G., Tennyson, J., Tessenyi, M., Vasisht, G., Vinatier, S., Viti, S., Waldmann, I., White, G. J., Widemann, T., Wordsworth, R., Yelle, R., Yung, Y., and Yurchenko, S. N.
Subjects: Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: A dedicated mission to investigate exoplanetary atmospheres represents a major milestone in our quest to understand our place in the universe by placing our Solar System in context and by addressing the suitability of planets for the presence of life. EChO -the Exoplanet Characterisation Observatory- is a mission concept specifically geared for this purpose. EChO will provide simultaneous, multi-wavelength spectroscopic observations on a stable platform that will allow very long exposures. EChO will build on observations by Hubble, Spitzer and groundbased telescopes, which discovered the first molecules and atoms in exoplanetary atmospheres. EChO will simultaneously observe a broad enough spectral region -from the visible to the mid-IR- to constrain from one single spectrum the temperature structure of the atmosphere and the abundances of the major molecular species. The spectral range and resolution are tailored to separate bands belonging to up to 30 molecules to retrieve the composition and temperature structure of planetary atmospheres. The target list for EChO includes planets ranging from Jupiter-sized with equilibrium temperatures Teq up to 2000 K, to those of a few Earth masses, with Teq ~300 K. We have baselined a dispersive spectrograph design covering continuously the 0.4-16 micron spectral range in 6 channels (1 in the VIS, 5 in the IR), which allows the spectral resolution to be adapted from several tens to several hundreds, depending on the target brightness. The instrument will be mounted behind a 1.5 m class telescope, passively cooled to 50 K, with the instrument structure and optics passively cooled to ~45 K. EChO will be placed in a grand halo orbit around L2. We have also undertaken a first-order cost and development plan analysis and find that EChO is easily compatible with the ESA M-class mission framework., Comment: Accepted for publication in Experimental Astronomy, 23 pages, 15 figures
Published: 2011
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5. Transiting exoplanets from the CoRoT space mission XXI. CoRoT-19b: A low density planet orbiting an old inactive F9V-star

Author: Guenther, E. W., Diaz, R. F., Gazzano, J. -C., Mazeh, T., Rouan, D., Gibson, N., Csizmadia, Sz., Aigrain, S., Alonso, R., Almenara, J. M., Auvergne, M., Baglin, A., Barge, P., Bonomo, A. S., Borde, P., Bouchy, F., Bruntt, H., Cabrera, J., Carone, L., Carpano, S., Cavarroc, C., Deeg, H. J., Deleuil, M., Dreizler, S., Dvorak, R., Erikson, A., Ferraz-Mello, S., Fridlund, M., Gandolfi, D., Gillon, M., Guillot, T., Hatzes, A., Havel, M., Hebrard, G., Jehin, E., Jorda, L., Lammer, H., Leger, A., Moutou, C., Nortmann, L., Ollivier, M., Ofir, A., Pasternacki, Th., Paetzold, M., Parviainen, H., Queloz, D., Rauer, H., Samuel, B., Santerne, A., Schneider, J., Tal-Or, L., Tingley, B., Weingrill, J., and Wuchterl, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Observations of transiting extrasolar planets are of key importance to our understanding of planets because their mass, radius, and mass density can be determined. The CoRoT space mission allows us to achieve a very high photometric accuracy. By combining CoRoT data with high-precision radial velocity measurements, we derive precise planetary radii and masses. We report the discovery of CoRoT-19b, a gas-giant planet transiting an old, inactive F9V-type star with a period of four days. After excluding alternative physical configurations mimicking a planetary transit signal, we determine the radius and mass of the planet by combining CoRoT photometry with high-resolution spectroscopy obtained with the echelle spectrographs SOPHIE, HARPS, FIES, and SANDIFORD. To improve the precision of its ephemeris and the epoch, we observed additional transits with the TRAPPIST and Euler telescopes. Using HARPS spectra obtained during the transit, we then determine the projected angle between the spin of the star and the orbit of the planet. We find that the host star of CoRoT-19b is an inactive F9V-type star close to the end of its main-sequence life. The host star has a mass M*=1.21+/-0.05 Msun and radius R*=1.65+/-0.04 Rsun. The planet has a mass of Mp=1.11+/-0.06 Mjup and radius of Rp=1.29+/-0.03 Rjup. The resulting bulk density is only rho=0.71+/-0.06 gcm-3, which is much lower than that for Jupiter. The exoplanet CoRoT-19b is an example of a giant planet of almost the same mass as Jupiter but a 30% larger radius., Comment: 6 pages, 7 figures
Published: 2011
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6. Transiting exoplanets from the CoRoT space mission - XIX. CoRoT-23b: a dense hot Jupiter on an eccentric orbit

Author: Rouan, D., Parviainen, H., Moutou, C., Deleuil, M., Fridlund, M., Ofir, A., Havel, M., Aigrain, S., Alonso, R., Auvergne, M., Baglin, A., Barge, P., Bonomo, A., Bordé, P., Bouchy, F., Cabrera, J., Cavarroc, C., Csizmadia, Sz., Deeg, H., Diaz, R. F., Dvorak, R., Erikson, A., Ferraz-Mello, S., Gandolfi, D., Gillon, M., Guillot, T., Hatzes, A., Hébrard, G., Jorda, L., Léger, A., Llebaria, A., Lammer, H., Lovis, C., Mazeh, T., Ollivier, M., Pätzold, M., Queloz, D., Rauer, H., Samuel, B., Santerne, A., Schneider, J., Tingley, B., and Wuchterl, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the detection of CoRoT-23b, a hot Jupiter transiting in front of its host star with a period of 3.6314 \pm 0.0001 days. This planet was discovered thanks to photometric data secured with the CoRoT satellite, combined with spectroscopic radial velocity (RV) measurements. A photometric search for possible background eclipsing binaries conducted at CFHT and OGS concluded with a very low risk of false positives. The usual techniques of combining RV and transit data simultaneously were used to derive stellar and planetary parameters. The planet has a mass of Mp = 2.8 \pm 0.3 MJup, a radius of Rpl = 1.05 \pm 0.13 RJup, a density of \approx 3 g cm-3. RV data also clearly reveal a non zero eccentricity of e = 0.16 \pm 0.02. The planet orbits a mature G0 main sequence star of V =15.5 mag, with a mass M\star = 1.14 \pm 0.08 M\odot, a radius R\star = 1. 61 \pm 0.18 R\odot and quasi-solar abundances. The age of the system is evaluated to be 7 Gyr, not far from the transition to subgiant, in agreement with the rather large stellar radius. The two features of a significant eccentricity of the orbit and of a fairly high density are fairly uncommon for a hot Jupiter. The high density is, however, consistent with a model of contraction of a planet at this mass, given the age of the system. On the other hand, at such an age, circularization is expected to be completed. In fact, we show that for this planetary mass and orbital distance, any initial eccentricity should not totally vanish after 7 Gyr, as long as the tidal quality factor Qp is more than a few 105, a value that is the lower bound of the usually expected range. Even if Corot-23b features a density and an eccentricity that are atypical of a hot Jupiter, it is thus not an enigmatic object., Comment: Astronomy & Astrophysics in press
Published: 2011
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7. XX. CoRoT-20b: A very high density, high eccentricity transiting giant planet

Author: Deleuil, M., Bonomo, A. S., Ferraz-Mello, S., Erikson, A., Bouchy, F., Havel, M., Aigrain, S., Almenara, J. -M., Alonso, R., Auvergne, M., Baglin, A., Barge, P., Bordé, P., Bruntt, H., Cabrera, J., Carpano, S., Cavarroc, C., Csizmadia, Sz., Damiani, C., Deeg, H. J., Dvorak, R., Fridlund, M., Hébrard, G., Gandolfi, D., Gillon, M., Guenther, E., Guillot, T., Hatzes, A., Jorda, L., Léger, A., Lammer, H., Mazeh, T., Moutou, C., Ollivier, M., Ofir, A., Parviainen, H., Queloz, D., Rauer, H., Rodríguez, A., Rouan, D., Santerne, A., Schneider, J., Tal-Or, L., Tingley, B., Weingrill, J., and Wuchterl, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery by the CoRoT space mission of a new giant planet, CoRoT-20b. The planet has a mass of 4.24 +/- 0.23 MJ and a radius of 0.84 +/- 0.04 RJ. With a mean density of 8.87 +/- 1.10 g/cm^3, it is among the most compact planets known so far. Evolution models for the planet suggest a mass of heavy elements of the order of 800 ME if embedded in a central core, requiring a revision either of the planet formation models or of planet evolution and structure models. We note however that smaller amounts of heavy elements are expected from more realistic models in which they are mixed throughout the envelope. The planet orbits a G-type star with an orbital period of 9.24 days and an eccentricity of 0.56. The star's projected rotational velocity is vsini = 4.5 +/- 1.0 km/s, corresponding to a spin period of 11.5 +/- 3.1 days if its axis of rotation is perpendicular to the orbital plane. In the framework of Darwinian theories and neglecting stellar magnetic breaking, we calculate the tidal evolution of the system and show that CoRoT-20b is presently one of the very few Darwin-stable planets that is evolving towards a triple synchronous state with equality of the orbital, planetary and stellar spin periods., Comment: 10 pages, 10 figures
Published: 2011
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8. Transiting exoplanets from the CoRoT space mission. XVIII. CoRoT-18b: a massive hot jupiter on a prograde, nearly aligned orbit

Author: Hebrard, G., Evans, T. M., Alonso, R., Fridlund, M., Ofir, A., Aigrain, S., Guillot, T., Almenara, J. M., Auvergne, M., Baglin, A., Barge, P., Bonomo, A. S., Borde, P., Bouchy, F., Cabrera, J., Carone, L., Carpano, S., Cavarroc, C., Csizmadia, Sz., Deeg, H. J., Deleuil, M., Diaz, R. F., Dvorak, R., Erikson, A., Ferraz-Mello, S., Gandolfi, D., Gibson, N., Gillon, M., Guenther, E., Hatzes, A., Havel, M., Jorda, L., Lammer, H., Leger, A., Llebaria, A., Mazeh, T., Moutou, C., Ollivier, M., Parviainen, H., Patzold, M., Queloz, D., Rauer, H., Rouan, D., Santerne, A., Schneider, J., Tingley, B., and Wuchterl, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the detection of CoRoT-18b, a massive hot jupiter transiting in front of its host star with a period of 1.9000693 +/- 0.0000028 days. This planet was discovered thanks to photometric data secured with the CoRoT satellite combined with spectroscopic and photometric ground-based follow-up observations. The planet has a mass M_p = 3.47 +/- 0.38 M_Jup, a radius R_p = 1.31 +/- 0.18 R_Jup, and a density rho_p = 2.2 +/- 0.8 g/cm3. It orbits a G9V star with a mass M_* = 0.95 +/- 0.15 M_Sun, a radius R_* = 1.00 +/- 0.13 R_Sun, and a rotation period P_rot = 5.4 +/- 0.4 days. The age of the system remains uncertain, with stellar evolution models pointing either to a few tens Ma or several Ga, while gyrochronology and lithium abundance point towards ages of a few hundred Ma. This mismatch potentially points to a problem in our understanding of the evolution of young stars, with possibly significant implications for stellar physics and the interpretation of inferred sizes of exoplanets around young stars. We detected the Rossiter-McLaughlin anomaly in the CoRoT-18 system thanks to the spectroscopic observation of a transit. We measured the obliquity psi = 20 +/- 20 degrees (sky-projected value: lambda = -10 +/- 20 degrees), indicating that the planet orbits in the same way as the star is rotating and that this prograde orbit is nearly aligned with the stellar equator., Comment: 14 pages, 13 figures, 3 tables, A&A in press, final version
Published: 2011
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9. Transiting exoplanets from the CoRoT space mission XVII. The hot Jupiter CoRoT-17b: a very old planet

Author: Csizmadia, Sz., Moutou, C., Deleuil, M., Cabrera, J., Fridlund, M., Gandolfi, D., Aigrain, S., Alonso, R., Almenara, J. M., Auvergne, M., Baglin, A., Barge, P., Bonomo, A. S., Borde, P., Bouchy, F., Bruntt, H., Carone, L., Carpano, S., Cavarroc, C., Cochran, W., Deeg, H. J., Diaz, R. F., Dvorak, R., Endl, M., Erikson, A., Ferraz-Mello, S., Fruth, Th., Gazzano, J. C., Gillon, M., Guenther, E. W., Guillot, T., Hatzes, A., Havel, M., Hebrard, G., Jehin, E., Jorda, L., Leger, A., Llebaria, A., Lammer, H., Lovis, C., MacQueen, P. J., Mazeh, T., Ollivier, M., Paetzold, M., Queloz, D., Rauer, H., Rouan, D., Santerne, A., Schneider, J., Tingley, B., Titz-Weider, R., and Wuchterl, G.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We report on the discovery of a hot Jupiter-type exoplanet, CoRoT-17b, detected by the CoRoT satellite. It has a mass of $2.43\pm0.30$\Mjup and a radius of $1.02\pm0.07$\Rjup, while its mean density is $2.82\pm0.38$ g/cm$^3$. CoRoT-17b is in a circular orbit with a period of $3.7681\pm0.0003$ days. The host star is an old ($10.7\pm1.0$ Gyr) main-sequence star, which makes it an intriguing object for planetary evolution studies. The planet's internal composition is not well constrained and can range from pure H/He to one that can contain $\sim$380 earth masses of heavier elements., Comment: Published (A&A 531, A41, 2011)
Published: 2011
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10. The extreme physical properties of the CoRoT-7b super-Earth

Author: Léger, A., Grasset, O., Fegley, B., Codron, F., Albarede, A. F., Barge, P., Barnes, R., Cance, P., Carpy, S., Catalano, F., Cavarroc, C., Demangeon, O., Ferraz-Mello, S., Gabor, P., Griessmeier, J. -M., Leibacher, J., Libourel, G., Maurin, A-S., Raymond, S. N., Rouan, D., Samuel, B., Schaefer, L., Schneider, J., Schuller, P. A., Selsis, F., and Sotin, C.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The search for rocky exoplanets plays an important role in our quest for extra-terrestrial life. Here, we discuss the extreme physical properties possible for the first characterized rocky super-Earth, CoRoT-7b (R_pl = 1.58 \pm 0.10 R_Earth, Mpl = 6.9 \pm 1.2 M_Earth). It is extremely close to its star (a = 0.0171 AU = 4.48 R_st), with its spin and orbital rotation likely synchronized. The comparison of its location in the (Mpl, Rpl) plane with the predictions of planetary models for different compositions points to an Earth-like composition, even if the error bars of the measured quantities and the partial degeneracy of the models prevent a definitive conclusion. The proximity to its star provides an additional constraint on the model. It implies a high extreme-UV flux and particle wind, and the corresponding efficient erosion of the planetary atmosphere especially for volatile species including water. Consequently, we make the working hypothesis that the planet is rocky with no volatiles in its atmosphere, and derive the physical properties that result. As a consequence, the atmosphere is made of rocky vapours with a very low pressure (P \leq 1.5 Pa), no cloud can be sustained, and no thermalisation of the planetary is expected. The dayside is very hot (2474 \leq 71 K at the sub-stellar point) while the nightside is very cold (50 to 75 K). The sub-stellar point is as hot as the tungsten filament of an incandescent bulb, resulting in the melting and distillation of silicate rocks and the formation of a lava ocean. These possible features of CoRoT-7b could be common to many small and hot planets, including the recently discovered Kepler-10b. They define a new class of objects that we propose to name "Lava-ocean planets".
Published: 2011
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11. Optical performance of the JWST MIRI flight model: characterization of the point spread function at high-resolution

Author: Guillard, P., Rodet, T., Ronayette, S., Amiaux, J., Abergel, A., Moreau, V., Augueres, J. L., Bensalem, A., Orduna, T., Nehmé, C., Belu, A. R., Pantin, E., Lagage, P. O, Longval, Y., Glasse, A. C. H., Bouchet, P., Cavarroc, C., Dubreuil, D., and Kendrew, S.
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Mid Infra Red Instrument (MIRI) is one of the four instruments onboard the James Webb Space Telescope (JWST), providing imaging, coronagraphy and spectroscopy over the 5-28 microns band. To verify the optical performance of the instrument, extensive tests were performed at CEA on the flight model (FM) of the Mid-InfraRed IMager (MIRIM) at cryogenic temperatures and in the infrared. This paper reports on the point spread function (PSF) measurements at 5.6 microns, the shortest operating wavelength for imaging. At 5.6 microns the PSF is not Nyquist-sampled, so we use am original technique that combines a microscanning measurement strategy with a deconvolution algorithm to obtain an over-resolved MIRIM PSF. The microscanning consists in a sub-pixel scan of a point source on the focal plane. A data inversion method is used to reconstruct PSF images that are over-resolved by a factor of 7 compared to the native resolution of MIRI. We show that the FWHM of the high-resolution PSFs were 5-10% wider than that obtained with Zemax simulations. The main cause was identified as an out-of-specification tilt of the M4 mirror. After correction, two additional test campaigns were carried out, and we show that the shape of the PSF is conform to expectations. The FWHM of the PSFs are 0.18-0.20 arcsec, in agreement with simulations. 56.1-59.2% of the total encircled energy (normalized to a 5 arcsec radius) is contained within the first dark Airy ring, over the whole field of view. At longer wavelengths (7.7-25.5 microns), this percentage is 57-68%. MIRIM is thus compliant with the optical quality requirements. This characterization of the MIRIM PSF, as well as the deconvolution method presented here, are of particular importance, not only for the verification of the optical quality and the MIRI calibration, but also for scientific applications., Comment: 13 pages, submitted to SPIE Proceedings vol. 7731, Space Telescopes and Instrumentation 2010: Optical, Infrared, and Millimeter Wave
Published: 2010
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12. Comparison of coronagraphs for high contrast imaging in the context of Extremely Large Telescopes

Author: Martinez, P., Boccaletti, A., Kasper, M., Cavarroc, C., Yaitskova, N., Fusco, T., and Verinaud, C.
Subjects: Astrophysics
Abstract: We compare coronagraph concepts and investigate their behavior and suitability for planet finder projects with Extremely Large Telescopes (ELTs, 30-42 meters class telescopes). For this task, we analyze the impact of major error sources that occur in a coronagraphic telescope (central obscuration, secondary support, low-order segment aberrations, segment reflectivity variations, pointing errors) for phase, amplitude and interferometric type coronagraphs. This analysis is performed at two different levels of the detection process: under residual phase left uncorrected by an eXtreme Adaptive Optics system (XAO) for a large range of Strehl ratio and after a general and simple model of speckle calibration, assuming common phase aberrations between the XAO and the coronagraph (static phase aberrations of the instrument) and non-common phase aberrations downstream of the coronagraph (differential aberrations provided by the calibration unit). We derive critical parameters that each concept will have to cope with by order of importance. We evidence three coronagraph categories as function of the accessible angular separation and proposed optimal one in each case. Most of the time amplitude concepts appear more favorable and specifically, the Apodized Pupil Lyot Coronagraph gathers the adequate characteristics to be a baseline design for ELTs., Comment: 12 pages, 6 figures, Accepted for publication in A&A
Published: 2008
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13. Optimization of Apodized Pupil Lyot Coronagraph for ELTs

Author: Martinez, P., Boccaletti, A., Kasper, M., Baudoz, P., and Cavarroc, C.
Subjects: Astrophysics
Abstract: We study the optimization of the Apodized Pupil Lyot Coronagraph (APLC) in the context of exoplanet imaging with ground-based telescopes. The APLC combines an apodization in the pupil plane with a small Lyot mask in the focal plane of the instrument. It has been intensively studied in the literature from a theoretical point of view, and prototypes are currently being manufactured for several projects. This analysis is focused on the case of Extremely Large Telescopes, but is also relevant for other telescope designs. We define a criterion to optimize the APLC with respect to telescope characteristics like central obscuration, pupil shape, low order segment aberrations and reflectivity as function of the APLC apodizer function and mask diameter. Specifically, the method was applied to two possible designs of the future European-Extremely Large Telescope (E-ELT). Optimum configurations of the APLC were derived for different telescope characteristics. We show that the optimum configuration is a stronger function of central obscuration size than of other telescope parameters. We also show that APLC performance is quite insensitive to the central obscuration ratio when the APLC is operated in its optimum configuration, and demonstrate that APLC optimization based on throughput alone is not appropriate., Comment: 9 pages, 17 figures, accepted for publication in Astronomy & Astrophysics
Published: 2007
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14. Fundamental limitations on Earth-like planet detection with Extremely Large Telescopes

Author: Cavarroc, C., Boccaletti, A., Baudoz, P., Fusco, T., and Rouan, D.
Subjects: Astrophysics
Abstract: We analyse the fundamental limitations for the detection of extraterrestrial planets with Extremely Large Telescopes. For this task, a coronagraphic device combined to a very high order wavefront correction system is required but not sufficient to achieve the $10^{-10}$ contrast level needed for detecting an Earth-like planet. The stellar residuals left uncorrected by the wavefront correction system need to be calibrated and subtracted. In this paper, we consider a general model including the dynamic phase aberrations downstream the wavefront correction system, the static phase aberrations of the instrument and some differential aberrations provided by the calibration unit. A rather optimistic case of a filled circular pupil and of a perfect coronagraph is elsewhere assumed. As a result of the analytical study, the limitation mostly comes from the static aberrations. Using numerical simulations we confirm this result and evaluate the requirements in terms of phase aberrations to detect Earth-like planets on Extremely Large Telescopes., Comment: 8 pages, 8 figures, accepted in A&A
Published: 2005
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15. Target Acquisition for MIRI Coronagraphs

Author: Cavarroc, C., Boccaletti, A., Baudoz, P., Amiaux, J., and Regan, M.
Published: 2008
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16. Feasibility of the Four‐Quadrant Phase Mask in the Mid‐Infrared on the James Webb Space Telescope

Author: Baudoz, P., Boccaletti, A., Riaud, P., Cavarroc, C., Baudrand, J., Reess, J. M., and Rouan, D.
Published: 2006
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17. 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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18. EChO: Exoplanet characterisation observatory

Author: Tinetti, G., Beaulieu, J. P., Henning, T., Meyer, M., Micela, G., Ribas, I., Stam, D., Swain, M., Krause, O., Ollivier, M., Pace, E., Swinyard, B., Aylward, A., van Boekel, R., Coradini, A., Encrenaz, T., Snellen, I., Zapatero-Osorio, M. R., Bouwman, J., Cho, J. Y-K., Coudé de Foresto, V., Guillot, T., Lopez-Morales, M., Mueller-Wodarg, I., Palle, E., Selsis, F., Sozzetti, A., Ade, P. A. R., Achilleos, N., Adriani, A., Agnor, C. B., Afonso, C., Prieto, C. Allende, Bakos, G., Barber, R. J., Barlow, M., Batista, V., Bernath, P., Bézard, B., Bordé, P., Brown, L. R., Cassan, A., Cavarroc, C., Ciaravella, A., Cockell, C., Coustenis, A., Danielski, C., Decin, L., Kok, R. De, Demangeon, O., Deroo, P., Doel, P., Drossart, P., Fletcher, L. N., Focardi, M., Forget, F., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gaulme, P., Hernández, J. I. González, Grasset, O., Grassi, D., Grenfell, J. L., Griffin, M. J., Griffith, C. A., Grözinger, U., Guedel, M., Guio, P., Hainaut, O., Hargreaves, R., Hauschildt, P. H., Heng, K., Heyrovsky, D., Hueso, R., Irwin, P., Kaltenegger, L., Kervella, P., Kipping, D., Koskinen, T. T., Kovács, G., La Barbera, A., Lammer, H., Lellouch, E., Leto, G., Lopez Morales, M., Lopez Valverde, M. A., Lopez-Puertas, M., Lovis, C., Maggio, A., Maillard, J. P., Maldonado Prado, J., Marquette, J. B., Martin-Torres, F. J., Maxted, P., Miller, S., Molinari, S., Montes, D., Moro-Martin, A., Moses, J. I., Mousis, O., Nguyen Tuong, N., Nelson, R., Orton, G. S., Pantin, E., Pascale, E., Pezzuto, S., Pinfield, D., Poretti, E., Prinja, R., Prisinzano, L., Rees, J. M., Reiners, A., Samuel, B., Sánchez-Lavega, A., Forcada, J. Sanz, Sasselov, D., Savini, G., Sicardy, B., Smith, A., Stixrude, L., Strazzulla, G., Tennyson, J., Tessenyi, M., Vasisht, G., Vinatier, S., Viti, S., Waldmann, I., White, G. J., Widemann, T., Wordsworth, R., Yelle, R., Yung, Y., and Yurchenko, S. N.
Published: 2012
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19. Transiting exoplanets from the CoRoT space mission Resolving the nature of transit candidates for the LRa03 and SRa03 fields

Author: Cavarroc, C., Moutou, C., Gandolfi, D., Tingley, B., Ollivier, M., Aigrain, S., Alonso, R., Almenara, J.-M., Auvergne, M., Baglin, A., Barge, P., Bonomo, A. S., Bordé, P., Bouchy, F., Cabrera, J., Carpano, S., Carone, L., Cochran, W. D., Csizmadia, S., Deeg, H. J., Deleuil, M., Díaz, R. F., Dvorak, R., Endl, M., Erikson, A., Fridlund, M., Gillon, M., Guenther, E. W., Guillot, T., Hatzes, A., Hébrard, G., Jorda, L., Léger, A., Lammer, H., Lev, T.-O., Lovis, C., MacQueen, P. J., Mazeh, T., Ofir, A., Parviainen, H., Pasternacki, T., Pätzold, M., Queloz, D., Rauer, H., Rouan, D., Samuel, B., Santerne, A., Schneider, J., Weingrill, J., and Wuchterl, G.
Published: 2012
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20. Spectral and polarimetric characterization of gazeous and telluric planets with SEE COAST

Author: Keller C.-U., Pinfield D., Doel P., Cavarroc C., Hough J., Stam D., Galicher R., Tinetti G., Schneider J., Mawet D., Baudoz P., Boccaletti A., Beuzit J.-L., Udry S., Ferrari A., Martin E., Ménard F., and Sein E.
Subjects: Physics, QC1-999
Abstract: SEE COAST stands for Super Earth Explorer – Coronagraphic Off-Axis Space Telescope. The concept was initially proposed to ESA for Cosmic Vision. None of the direct detection exoplanet proposals were selected in 2007 and we are now pursuing our efforts to consolidate the astrophysical program and the technical developments for the next call for proposal. The prime objective of SEE COAST is to contribute to the understanding of the formation and evolution of planetary systems. Exploring the diversity of these objects is therefore the main driver to define the instrumentation. In the next decade the improvement of radial velocity instruments and obviously temporal coverage will provide us with a large numbers of long period giants as well as telluric planets, namely Super Earths. Obtaining the spectral and polarimetric signatures of these objects in the visible range to measure atmospheric parameters (molecular composition, clouds, soils, …) will be unique and with important scientific returns. A space mission complementary to near IR instruments like SPHERE, GPI, JWST and later ELTs for the full characterization of giants and Super Earths is a first secure step towards the longer term goal that is the characterization of telluric planets with mass and atmosphere comparable to that of the Earth. An overview of the astrophysical motivation and the trade-off that lead to a simple integrated concept of a space-based high contrast imaging instrument are given here.
Published: 2011
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21. XX. CoRoT-20b: A very high density, high eccentricity transiting giant planet

Author: Deleuil, M, Bonomo, A, Ferraz-Mello, S, Erikson, A, Bouchy, F, Havel, M, Aigrain, S, Almenara, J, Alonso, R, Auvergne, M, Baglin, A, Barge, P, Bordé, P, Bruntt, H, Cabrera, J, Carpano, S, Cavarroc, C, Csizmadia, S, Damiani, C, Deeg, H, Dvorak, R, Fridlund, M, Hébrard, G, Gandolfi, D, and Gillon, M
Abstract: We report the discovery by the CoRoT space mission of a new giant planet, CoRoT-20b. The planet has a mass of 4.24 +/- 0.23 MJ and a radius of 0.84 +/- 0.04 RJ. With a mean density of 8.87 +/- 1.10 g/cm^3, it is among the most compact planets known so far. Evolution models for the planet suggest a mass of heavy elements of the order of 800 ME if embedded in a central core, requiring a revision either of the planet formation models or of planet evolution and structure models. We note however that smaller amounts of heavy elements are expected from more realistic models in which they are mixed throughout the envelope. The planet orbits a G-type star with an orbital period of 9.24 days and an eccentricity of 0.56. The star's projected rotational velocity is vsini = 4.5 +/- 1.0 km/s, corresponding to a spin period of 11.5 +/- 3.1 days if its axis of rotation is perpendicular to the orbital plane. In the framework of Darwinian theories and neglecting stellar magnetic breaking, we calculate the tidal evolution of the system and show that CoRoT-20b is presently one of the very few Darwin-stable planets that is evolving towards a triple synchronous state with equality of the orbital, planetary and stellar spin periods.
Published: 2016
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22. The EChO science case

Author: Tinetti, G., Drossart, P., Eccleston, P., Hartogh, P., Isaak, K., Linder, M., Lovis, C., Micela, G., Olliver, M., Puig, L., Ribas, I., De Sio, A., Frith, J., Justtanot, K., Showman, A., Alard, C., Yurchenko, S. N., Parviainen, H., Fouqué, P., Oliva, E., Bordé, P., Balado, A., Varley, R., Di Giorgio, A., Griffin, M., Maillard, J. P., Maggio, A., Lellouch, E., Strazzulla, G., Villaver, E., Griffith, C., Stamper, R., Amado, P. J., Rezac, L., Laken, B., Hargrave, P., Orton, G., Thompson, S., Morales, J. C., Wright, G., Massi, F., Lundgaard Rasmussen, I., Altieri, F., Covino, E., Coustenis, A., Moses, J., Lithgow Bertelloni, C., Demangeon, O., Fletcher, L., Morales Calderón, M., Lo Cicero, U., López Puertas, M., Capria, M. T., Danielski, C., Luntzer, A., Bulgarelli, A., González Hernández, J., Jacquemoud, S., MacTavish, C., Mall, U., Christian Jessen, N., Sanromá, E., Femenía Castella, B., Rocchetto, M., Miles Paez, P., Allard, F., Aylward, A., Leconte, J., Palla, F., White, G., Malaguti, G., Cavarroc, C., Lammer, H., Leto, G., Batista, V., Adybekian, V., Readorn, K., Polichtchouk, I., Petrov, R., García Piquer, A., Pancrazzi, M., Gómez Leal, I., Israelian, G., Rebolo López, R., Peralta, J., Giro, E., Tecsa, M., Haigh, J., Moro Martín, A., Pezzuto, S., Piskunov, N., Agnor, C., Hollis, M., Radioti, A., De Kok, R., Gear, W., Eymet, V., Achilleos, N., Koskinen, T., Maurin, A. S., Rank Lüftinger, T., Barlow, M., Figueira, P., Affer, L., Viti, S., Machado, P., Vakili, F., Burston, R., González Merino, B., Dominic, C., Dorfi, E., Smith, A., Sitek, P., Sánchez Lavega, A., Kerschbaum, F., Hoogeeven, R., Ballerini, P., Filacchione, G., Rodler, F., Stixrude, L., Parmentier, V., Del Val Borro, M., Vandenbussche, B., Tingley, B. W., Deeg, H. J., Tabernero, H. M., Shore, S., Fossey, S., Alonso Floriano, F. J., Santos, N., Tozzi, A., Kipping, D., Maruquette, J. B., Trifoglio, M., Scandaratio, G., Scuderi, S., Hébrard, E., Lodieu, N., Forget, F., Gustin, J., Poretti, E., Murgas Alcaino, F., Sicardy, B., Stiepen, A., Hubert, B., Grodent, D., Magnes, W., Tennyson, J., Temple, J., Galand, M., Barton, E. J., Winter, B., Valdivieso, M. L., Cordier, D., Heredero, R. L., Barrado, D., Mueller Wodarg, I., Giani, E., Correira, A., Widemann, T., Ward Thompson, D., Montañés Rodríguez, P., Moya Bedon, A., Venot, O., Prinja, R., Pinfield, D., Waldmann, I., Morello, G., Lim, T., Pallé, E., Waters, R., Wawer, P., Lognonné, P., Pietrzak, R., Fernández Hernández, Maite, Winek, W., Andersen, A., Monteiro, M., Liu, S. J., Rengel, M., Tanga, P., Yelle, R., Barstow, J. K., Maldonado, J., Irshad, R., Nelson, R., Colomé, J., De Witt, J., Lanza, N., Glasse, A., Coudé du Foresto, V., Branduardi Raymont, G., Beaulieu, J. P., Claudi, R., García López, Ramón, Eales, S., López Valverde, M. A., Turrini, D., Vinatier, S., Crook, J., Damasso, M., Ramos Zapata, G., Kovács, G., Banaszkiewicz, M., Focardi, M., Mauskopf, P., Guedel, M., Rebordao, J., Stolarski, M., Adriani, A., Norgaard Nielsen, H. U., Selig, A., Peña Ramírez, K. Y., Schmider, F. X., Baffa, C., Piccioni, G., Pantin, E., Bowles, N., Hornstrup, A., Pilat Lohinger, E., Buchhave, L. A., Soret, L., Börne, P., López Morales, M., Medvedev, A., Gesa, L., Jones, H., Pérez Hoyos, S., Gerard, J. C., Bellucci, G., Morais, H., Álvarez Iglesias, C. A., Abe, L., Pinsard, F., Tessenyi, M., Blecka, M., Wawrzaszk, A., Middleton, K., Martín Torres, J., Cho, J., Berry, D., Rataj, M., Schrader, J. R., Scholz, A., Watkins, C., Abreu, M., Testi, L., Decin, L., Sánz Forcada, J., Sozzetti, A., Lagage, P. O., Ade, P., Alcala, J., Sousa, S., Espinoza Contreras, M., Swinyard, B., Dobrijévic, M., Sánchez Béjar, V. J., Krupp, N., Bakos, G., Chamberlain, S., Chadney, J., Brown, L., Iro, N., Montalto, M., Sethenadh, J., Bouy, H., Ottensamer, R., Kehoe, T., Doel, P., Delgado Mena, E., Read, P., Coates, A., Cecchi Pestellini, C., Guillot, T., Budaj, J., Selsis, F., Jarchow, C., Del Vecchio, C., Cassan, A., Burleigh, M. R., Pagano, I., Ray, T., Gambicorti, L., Biondi, D., Cerulli, R., Ciaravella, A., Watson, D., Deroo, P., Collura, A., Graczyk, R., North, C., Ramos, A. A., Waltham, D., Montes, D., Gianotti, F., Thrastarson, H., Cockell, C., Pace, E., Bryson, I., Gómez, H., Esposito, M., Azzollini, R., Allende Prieto, C., Gillon, M., Fabrizio, N., Rickman, H., Rees, J. M., Pascale, E., Luzzi, D., Bonford, B., Cole, R., Gizon, L., Licandro Goldaracena, J., Agundez, M., Lahav, O., Zapatero Osorio, M. R., Gaulme, P., Encrenaz, T., Heyrovsky, D., Guàrdia, J., Prisinzano, L., Terenzi, L., Swain, M., Grassi, D., Eiroa, C., Maxted, P., Kerins, E., Yung, Y., Irwin, P., Herrero, E., Guio, P., Boisse, I., Claret, A., Kervella, P., Heiter, U., Bézard, B., Cabral, A., Michaut, C., Giuranna, M., Hersant, F., Hueso, R., Savini, G., Snellen, I. A., Charnoz, S., Jones, G., Belmonte Avilés, J. A., Barber, R. J., Wisniowski, T., Morgante, G., University College of London [London] (UCL), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Laboratoire des technologies de la microélectronique (LTM), Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Dpto. de Organización de Empresas, Escuela Técnica Superior de Ingeniería Industrial de Barcelona, Universitat Politècnica de Catalunya [Barcelona] (UPC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Leicester], University of Leicester, U.S. Army Research Laboratory [Adelphi, MD] (ARL), United States Army (U.S. Army), Royal Observatory Edinburgh (ROE), University of Edinburgh, Departamento de Fisica [Aveiro], Universidade de Aveiro, SRON Netherlands Institute for Space Research (SRON), 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-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Planetary Sciences [Tucson], University of Arizona, Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Lunar and Planetary Laboratory [Tucson] (LPL), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), The Samuel Roberts Noble Foundation, Center for Human-Computer Interaction (HCI), Virginia Tech [Blacksburg], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), ECLIPSE 2015, 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)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [UCL London], Laboratoire de Physique Atmosphérique et Planétaire (LPAP), Université de Liège, Centro de Astronomia e Astrofísica da Universidade de Lisboa (CAAUL), Universidade de Lisboa = University of Lisbon (ULISBOA), Department of Physics and Astronomy [Uppsala], Uppsala University, Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), University of Stuttgart, Institute for Control Engineering of Machine Tools and Manufacturing Units (ISW), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford, Mullard Space Science Laboratory (MSSL), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut Curie [Paris], Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Centre for Behaviour and Evolution, Institute of Neuroscience, Newcastle University [Newcastle], foreign laboratories (FL), CERN [Genève], STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Estrutura de Missão para a Extensão da Plataforma Continental, Estrutura de Missão para a Extensão para a Extensão da Plataforma Continental, Centre for Planetary Sciences [UCL/Birkbeck] (CPS), Queen Mary University of London (QMUL), 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), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Computational Science and Engineering Department [Daresbury] (STFC), Science & Technologie Facilities Council, Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Calar Alto Observatory, Centro Astronómico Hispano-Alemán, Department of Geoscience, Nelson Mandela University [Port Elizabeth], African Earth Observatory Network - Earth Stewardship Science Research Institute (AEON-ESSRI), Animal Genetics, Teagasc - The Agriculture and Food Development Authority (Teagasc), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Instituto Nacional de Engenharia, Tecnologia e Inovacao (INETI), Université Pierre et Marie Curie - Paris 6 (UPMC), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Università di Salerno - Dipartimento di Matematica, Università degli Studi di Salerno = University of Salerno (UNISA), Department of Genetics, University of North Carolina [Chapel Hill] (UNC), University of North Carolina System (UNC)-University of North Carolina System (UNC)-Carolina Center for the Genome Sciences, Institut de Recerca i Tecnologia Agroalimentàries = Institute of Agrifood Research and Technology (IRTA), Univers, Transport, Interfaces, Nanostructures, Atmosphère et environnement, Molécules (UMR 6213) (UTINAM), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Department of Molecular Medicine, Università degli Studi di Padova = University of Padua (Unipd), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), ASP 2015, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (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 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-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)-Université de Bordeaux (UB), Institute for Astronomy [Vienna], University of Vienna [Vienna], Institut de génétique et microbiologie [Orsay] (IGM), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH = German Research Center for Artificial Intelligence (DFKI), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Dipartimento di Matematica 'Ulisse Dini', Università degli Studi di Firenze = University of Florence (UniFI), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Université de Rennes (UR), Imperial College London, Laboratoire Hippolyte Fizeau (FIZEAU), School of Physics and Astronomy [Cardiff], Cardiff University, Institut d'Astrophysique et de Géophysique [Liège], Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), University of Bradford, Instituto Universitario de Electroquimica, Universidad de Alicante, Centre de recherche en éducation de Nantes (CREN), Le Mans Université (UM)-Université de Nantes - UFR Lettres et Langages (UFRLL), Université de Nantes (UN)-Université de Nantes (UN), Departamento de Fisica Aplicada [Bilbao], Universidad del Pais Vasco / Euskal Herriko Unibertsitatea [Espagne] (UPV/EHU), NASA Goddard Space Flight Center (GSFC), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Los Alamos National Laboratory (LANL), Osserv Astrofis Catania, Ist Nazl Astrofis, Centre d'Etude de l'Energie Nucléaire (SCK-CEN), Institut de Physique du Globe de Paris (IPGP (UMR_7154)), Institut national des sciences de l'Univers (INSU - CNRS)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Consejo Super Invest Cient, Inst Astrofis Andalucia, ES-18080 Granada, Spain, Department of Rheumatology (LEIDEN - Rhumato), Leiden University Medical Center (LUMC), Universiteit Leiden-Universiteit Leiden, Department of Rheumatology (COIMBRA - Rhumato), Universidade de Coimbra [Coimbra], Centre Scientifique et Technique du Bâtiment (CSTB), INAF - Osservatorio Astrofisico di Arcetri (OAA), Université de Bordeaux (UB), Institut de Physique du Globe de Paris (IPGP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Institut de Physique du Globe de Paris (IPG Paris)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de physique des gaz et des plasmas (LPGP), Pontificia Universidad Católica de Chile (UC), Department of Computer Science [Verona] (UNIVR | DI), Università degli studi di Verona = University of Verona (UNIVR), IEB-UNIVERSITY OF BARCELONA, Departamento de Física e Astronomia [Porto] (DFA/FCUP), Faculdade de Ciências da Universidade do Porto (FCUP), Universidade do Porto = University of Porto-Universidade do Porto = University of Porto, Thüringer Landessternwarte Tautenburg (TLS), Bremer Institut für Produktion und Logistik GmbH (BIBA), Universität Bremen, INAF - Osservatorio Astrofisico di Catania (OACT), Plasmon Nano-optics, Institut de Ciencies Fotoniques [Castelldefels] (ICFO), Royal Holloway [University of London] (RHUL), Hong Kong Government Environmental Protection Department, Water Policy and Science Group, National Space Agencies, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Max Planck Institute for Solar System Research (MPS), European Space Agency (ESA), European Space Agency, Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'Énergie Atomique et aux Énergies Alternatives (CEA) - Grenoble-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), École normale supérieure - Paris (ENS Paris)-École normale supérieure - Paris (ENS Paris), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Samuel Roberts Noble Foundation, Inc., Universidade de Lisboa (ULISBOA), Polska Akademia Nauk (PAN), University of Oxford [Oxford], Max-Planck-Institut für Sonnensystemforschung (MPS), Institut Curie, University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Nelson Mandela Metropolitan University [Port Elizabeth, South Africa], AEON-ESSRI African Earth Observatory Network — Earth Stewardship Science Research Institute, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Instituto Nacional de Engenharia, Tecnologia e Inovacco (INETI), Physiologie de la reproduction et des comportements [Nouzilly] (PRC), Centre National de la Recherche Scientifique (CNRS)-Université de Tours-Institut Français du Cheval et de l'Equitation [Saumur]-Institut National de la Recherche Agronomique (INRA), Université Francois Rabelais [Tours], Institut Français du Cheval et de l'Equitation, Università degli Studi di Salerno (UNISA), IRTA, Laboratoire d'astrophysique de l'observatoire de Besançon (LAOB), Universita degli Studi di Padova, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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-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)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH (DFKI), Universidade do Porto [Porto], Università degli Studi di Firenze [Firenze], Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES), 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, Department of Earth Sciences, University College London, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-IPG PARIS-Université Paris Diderot - Paris 7 (UPD7)-Université de La Réunion (UR)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Centre interdisciplinaire de recherche, culture, éducation, formation, travail (CIRCEFT), Université Paris 8 Vincennes-Saint-Denis (UP8)-Université Paris-Est Créteil Val-de-Marne - Paris 12 (UPEC UP12), Centre National de la Recherche Scientifique (CNRS)-Université de La Réunion (UR)-Université Paris Diderot - Paris 7 (UPD7)-IPG PARIS-Institut national des sciences de l'Univers (INSU - CNRS), Station biologique, Centre National de la Recherche Scientifique (CNRS), Dipartimento di Informatica [Verona], Università degli Studi di Verona, Departamento de Física e Astronomia [Porto], UMR5116, Centre Émile Durkheim (CED), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS), Clinica Neurologica, Università degli Studi di Perugia (UNIPG), Rebordao, J. [0000-0002-7418-0345], Kerschbaum, F. [0000-0001-6320-0980], Abreu, M. [0000-0002-0716-9568], Tabernero, H. [0000-0002-8087-4298], López Puertas, M. [0000-0003-2941-7734], Jacquemoud, S. [0000-0002-1500-5256], Tennyson, J. [0000-0002-4994-5238], Focardi, M. [0000-0002-3806-4283], Leto, G. [0000-0002-0040-5011], Lodieu, N. [0000-0002-3612-8968], Tinetti, G. [0000-0001-6058-6654], Sanroma, E. [0000-0001-8859-7937], Poretti, E. [0000-0003-1200-0473], Deeg, H. [0000-0003-0047-4241], Grassi, D. [0000-0003-1653-3066], Piccioni, G. [0000-0002-7893-6808], Ribas, I. [0000-0002-6689-0312], Coates, A. [0000-0002-6185-3125], García Ramón, J. [0000-0002-8204-6832], Bouy, H. [0000-0002-7084-487X[, Lognonne, P. [0000-0002-1014-920X], Demangeon, O. [0000-0001-7918-0355], Morales, J. C. [0000-0003-0061-518X], Ray, T. [0000-0002-2110-1068], Guio, P. [0000-0002-1607-5862], Tanga, P. [0000-0002-2718-997X], Prisinzano, L. [0000-0002-8893-2210], Barstow, J. [0000-0003-3726-5419], Balado, A. [0000-0003-4268-2516], Lithgow Bertelloni, C. [0000-0003-0924-6587], Barton, E. [0000-0001-5945-9244], Delgado, M. E. [0000-0003-4434-2195], Affer, L. [0000-0001-5600-3778], Ciaravella, A. [0000-0002-3127-8078], Barrado Navascues, D. [0000-0002-5971-9242], Figueira, P. [0000-0001-8504-283X], Covino, E. [0000-0002-6187-6685], Venot, O. [0000-0003-2854-765X], Cabral, A. [0000-0002-9433-871X], Watson, D. [0000-0002-4465-8264], Morales Calderon, M. [0000-0001-9526-9499], Ward Thompson, D. [0000-0003-1140-2761], Rebolo, R. [0000-0003-3767-7085], López Valverde, M. A. [0000-0002-7989-4267], Gillon, M. [0000-0003-1462-7739], Morgante, G. [0000-0001-9234-7412], Zapatero Osorio, M. R. [0000-0001-5664-2852], Bulgarelli, A. [0000-0001-6347-0649], Pena Ramírez, K. [0000-0002-5855-401X], Galand, M. [0000-0001-5797-914X], Pancrazzi, M. [0000-0002-3789-2482], Malaguti, G. [0000-0001-9872-3378], Sánchez Lavega, A. [0000-0001-7234-7634], Waldmann, I. [0000-0002-4205-5267], Kovacs, G. [0000-0002-2365-2330], Guillot, T. [0000-0002-7188-8428], Turrini, D. [0000-0002-1923-7740], Altieri, F. [0000-0002-6338-8300], Bellucci, G. [0000-0003-0867-8679], Baffa, C. [0000-0002-4935-100X], Olivia, E. [0000-0002-9123-0412], Selsis, F. [0000-0001-9619-5356], Scuderi, Salvatore [0000-0002-8637-2109], Hersant, F. [0000-0002-2687-7500], Gear, W. [0000-0001-6789-6196], Damasso, M. [0000-0001-9984-4278], Tizzi, A. [0000-0002-6725-3825], Pinfield, D. [0000-0002-7804-4260], Kipping, D. [0000-0002-4365-7366], Maldonado, J. [0000-0002-4282-1072], Pace, E. [0000-0001-5870-1772], Burleigh, M. [0000-0003-0684-7803], Monteiro, M. [0000-0001-5644-0898], Pilat Lohinger, E. [0000-0002-5292-1923], Chadney, J. [0000-0002-5174-2114], Moro Martín, A. [0000-0001-9504-8426], Claret, A. [0000-0002-4045-8134], Gómez, H. [0000-0003-3398-0052], Maldonado, J. [0000-0002-2218-5689], Michaut, C. [0000-0002-2578-0117], Hornstrup, A. [0000-0002-3363-0936], Scholz, A. [0000-0001-8993-5053], Irwin, P. [0000-0002-6772-384X], Bezard, B. [0000-0002-5433-5661], López Heredero, R. [0000-0002-2197-8388], Sanz Forcada, J. [0000-0002-1600-7835], Danielski, C. [0000-0002-3729-2663], Sousa, S. [0000-0001-9047-2965], Medved, A. [0000-0003-2713-8977], Bakos, G. [0000-0001-7204-6727], Ade, P. [0000-0002-5127-0401], Vandenbussche, B. [0000-0002-1368-3109], Martín Torres, J. [0000-0001-6479-2236], Correira, A. [0000-0002-8946-8579], Haigh, J. [0000-0001-5504-4754], Scandariato, G. [0000-0003-2029-0626], Guedel, M. [0000-0001-9818-0588], Sánchez Bejar, V. [0000-0002-5086-4232], Rodríguez, P. [0000-0002-6855-9682], Piskunov, N. [0000-0001-5742-7767], Adibekyan, V. [0000-0002-0601-6199], Pérez Hoyos, S. [0000-0001-9797-4917], Kervella, P. [0000-0003-0626-1749], Pascale, E. [0000-0002-3242-8154], Claudi, R. [0000-0001-7707-5105], Filacchione, G. [0000-0001-9567-0055], Rickman, H. [0000-0002-9603-6619], Amado, P. J. [0000-0002-8388-6040], Maggio, A. [0000-0001-5154-6108], Agundez, M. [0000-0003-3248-3564], Montes, D. [0000-0002-7779-238X], Fletcher, L. [0000-0001-5834-9588], Stixrude, L. [0000-0003-3778-2432], Morais, M. H. [0000-0001-5333-2736], Hueso, R. [0000-0003-0169-123X], Yurchenko, S. [0000-0001-9286-9501], Rataj, M. [0000-0002-2978-9629], Pérez Hoyos, S. [0000-0002-2587-4682], Santos, N. [0000-0003-4422-2919], Peralta, J. [0000-0002-6823-1695], Budaj, J. [0000-0002-9125-7340], Barlow, M. [0000-0002-3875-1171], Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École des Ponts ParisTech (ENPC)-École polytechnique (X)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - 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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 ), Joseph Louis LAGRANGE ( LAGRANGE ), Université Nice Sophia Antipolis ( UNS ), Université Côte d'Azur ( UCA ) -Université Côte d'Azur ( UCA ) -Observatoire de la Côte d'Azur, Université Côte d'Azur ( UCA ) -Centre National de la Recherche Scientifique ( CNRS ), Lunar and Planetary Laboratory [Tucson], Space Research Institute of Austrian Academy of Sciences ( IWF ), Austrian Academy of Sciences ( OeAW ), Centre de Recherche Astrophysique de Lyon ( CRAL ), École normale supérieure - Lyon ( ENS Lyon ) -Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Center for Human-Computer Interaction ( HCI ), Istituto di Astrofisica e Planetologia Spaziali ( IAPS ), University of Hertfordshire [Hatfield] ( UH ), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - 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Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), Deutsches Forschungszentrum für Künstliche Intelligenz GmbH ( DFKI ), Consejo Nacional de Investigaciones Científicas y Técnicas ( CONICET ), Centro de Astrofísica da Universidade do Porto ( CAUP ), Institut Universitaire de France ( IUF ), Ministère de l'Éducation nationale, de l’Enseignement supérieur et de la Recherche ( M.E.N.E.S.R. ), Université de Rennes 1 ( UR1 ), Université de Rennes ( UNIV-RENNES ), Laboratoire Hippolyte Fizeau ( FIZEAU ), 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, Istituto di Fisica dello Spazio Interplanetario CNR (IFSI), Laboratoire de l'Accélérateur Linéaire ( LAL ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Centre de recherche en éducation de Nantes ( CREN ), Université de Nantes ( UN ), Universidad del Pais Vasco / Euskal Herriko Unibertsitatea ( UPV/EHU ), NASA Goddard Space Flight Center ( GSFC ), Onsala Space Observatory ( OSO ), Los Alamos National Laboratory ( LANL ), Centre d'Etude de l'Energie Nucléaire ( SCK-CEN ), Institut de Physique du Globe de Paris ( IPGP ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Instituto de Astrofísica de Andalucía ( IAA ), Consejo Superior de Investigaciones Científicas [Spain] ( CSIC ), Department of Rheumatology ( LEIDEN - Rhumato ), Department of Rheumatology ( COIMBRA - Rhumato ), Centre Scientifique et Technique du Bâtiment ( CSTB ), INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Centre interdisciplinaire de recherche, culture, éducation, formation, travail ( CIRCEFT ), Université Paris 8 Vincennes-Saint-Denis ( UP8 ) -Université Paris-Est Créteil Val-de-Marne - Paris 12 ( UPEC UP12 ), Institut national des sciences de l'Univers ( INSU - CNRS ) -IPG PARIS-Université Paris Diderot - Paris 7 ( UPD7 ) -Université de la Réunion ( UR ) -Centre National de la Recherche Scientifique ( CNRS ), Centre National de la Recherche Scientifique ( CNRS ), Laboratoire de physique des gaz et des plasmas ( LPGP ), Pontificia Universidad Católica de Chile, Thüringer Landessternwarte Tautenburg ( TLS ), BIBA Bremer Institut für Produktion und Logistik GmbH, Centre Émile Durkheim ( CED ), Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Sciences Po-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Catania ( OACT ), Institut de Ciencies Fotoniques [Castelldefels] ( ICFO ), Università di Perugia, Royal Holloway [University of London] ( RHUL ), and Low Energy Astrophysics (API, FNWI)
Subjects: Astrofísica, Solar System, Computer science, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], HOT-JUPITER ATMOSPHERES, 7. Clean energy, Space missions, law.invention, Astronomi, astrofysik och kosmologi, Planet, law, Observatory, Astronomy, Astrophysics and Cosmology, Transit (astronomy), Atmospheric science, Exoplanets, IR astronomy, Spectroscopy, Astronomy and Astrophysics, Space and Planetary Science, QC, QB, Eclipse, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Exoplanet, GIANT PLANETS, Physical Sciences, ENERGY-BALANCE, Astrophysics::Earth and Planetary Astrophysics, Population, MU-M, FOS: Physical sciences, F500, Astronomy & Astrophysics, Telescope, INFRARED-EMISSION-SPECTRUM, education, [ SDU.ASTR ] Sciences of the Universe [physics]/Astrophysics [astro-ph], EXTRASOLAR PLANET ATMOSPHERE, Science & Technology, Astronomy, EXOPLANET HD 189733B, HUBBLE-SPACE-TELESCOPE, Astronomía, TRANSMISSION SPECTROSCOPY, 0201 Astronomical And Space Sciences, 13. Climate action, WATER-VAPOR, astro-ph.EP, 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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23. XXVI. CoRoT-24: a transiting multiplanet system

Author: Alonso, R., Moutou, C., Endl, M., Almenara, J.-M., Guenther, E., Deleuil, M., Hatzes, A., Aigrain, S., Auvergne, M., Baglin, A., Barge, P., Bonomo, A., Bordé, P., Bouchy, F., Cavarroc, C., Cabrera, J., Carpano, S., Csizmadia, Sz., Cochran, W., Deeg, H., Díaz, R., Dvorak, R., Erikson, A., Ferraz-Mello, S., Fridlund, M., Fruth, T., Gandolfi, D., Gillon, M., Grziwa, S., Guillot, T., Hébrard, G., Jorda, L., Léger, A., Lammer, H., Lovis, C., MacQueen, P., Mazeh, T., Ofir, A., Ollivier, M., Pasternacki, T., Pätzold, M., Queloz, D., Rauer, H., Rouan, D., Santerne, A., Schneider, J., Tadeu Dos Santos, M., Tingley, B., Titz-Weider, R., Weingrill, J., Wuchterl, G., Departamento de Matemàtica, PUC RIO, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Instituto de Astrofisica de Canarias (IAC), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Thüringer Landessternwarte Tautenburg (TLS), School of Physics, University of Exeter, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Institut de Radioprotection et de Sûreté Nucléaire (IRSN), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institute of Astronomy, University of Vienna [Vienna], DLR Institute of Planetary Research, German Aerospace Center (DLR), Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo (USP), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Department of Brain and Behavioural Sciences, University of Pavia, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], Rhenish Institute for Environmental Research (RIU), University of Cologne, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: [PHYS]Physics [physics], planetary systems, photometric, radial velocities, spectroscopic, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: We present the discovery of a candidate multiply transiting system, the first one found in the CoRoT mission. Two transit-like features with periods of 5.11 and 11.76 d are detected in the CoRoT light curve around a main sequence K1V star of r = 15.1. If the features are due to transiting planets around the same star, these would correspond to objects of 3.7 ± 0.4 and 5.0 ± 0.5 R⊕ , respectively. Several radial velocities serve to provide an upper limit of 5.7 M⊕ for the 5.11 d signal and to tentatively measure a mass of 28+11-11 M⊕ for the object transiting with a 11.76 d period. These measurements imply low density objects, with a significant gaseous envelope. The detailed analysis of the photometric and spectroscopic data serves to estimate the probability that the observations are caused by transiting Neptune-sized planets as much as over 26 times higher than a blend scenario involving only one transiting planet and as much as over 900 times higher than a scenario involving two blends and no planets. The radial velocities show a long-term modulation that might be attributed to a 1.5 MJup planet orbiting at 1.8 AU from the host, but more data are required to determine the precise orbital parameters of this companion. peerReviewed
Published: 2014
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24. EChO

Author: Tinetti, G, Beaulieu, JP, Henning, T, Meyer, M, Micela, G, Ribas, I, Stam, D, Swain, M, Krause, O, Ollivier, M, Pace, E, Swinyard, B, Aylward, A, van Boekel, R, Coradini, A, Encrenaz, T, Snellen, I, Zapatero-Osorio, MR, Bouwman, J, Cho, JY-K, du Foresto, VC, Guillot, T, Lopez-Morales, M, Mueller-Wodarg, I, Palle, E, Selsis, F, Sozzetti, A, Ade, PAR, Achilleos, N, Adriani, A, Agnor, CB, Afonso, C, Allende Prieto, C, Bakos, G, Barber, RJ, Barlow, M, Batista, V, Bernath, P, Bezard, B, Borde, P, Brown, LR, Cassan, A, Cavarroc, C, Ciaravella, A, Cockell, C, Coustenis, A, Danielski, C, Decin, L, De Kok, R, Demangeon, O, Deroo, P, Doel, P, Drossart, P, Fletcher, LN, Focardi, M, Forget, F, Fossey, S, Fouque, P, Frith, J, Galand, M, Gaulme, P, Gonzalez Hernandez, JI, Grasset, O, Grassi, D, Grenfell, JL, Griffin, MJ, Griffith, CA, Groezinger, U, Guedel, M, Guio, P, Hainaut, O, Hargreaves, R, Hauschildt, PH, Heng, K, Heyrovsky, D, Hueso, R, Irwin, P, Kaltenegger, L, Kervella, P, Kipping, D, Koskinen, TT, Kovacs, G, La Barbera, A, Lammer, H, Lellouch, E, Leto, G, Lopez Valverde, MA, Lopez-Puertas, M, Lovis, C, Maggio, A, Maillard, JP, Maldonado Prado, J, Marquette, JB, Martin-Torres, FJ, Maxted, P, Miller, S, Molinari, S, Montes, D, Moro-Martin, A, Moses, JI, Mousis, O, Nguyen Tuong, N, Nelson, R, Orton, GS, Pantin, E, Pascale, E, Pezzuto, S, Pinfield, D, Poretti, E, Prinja, R, Prisinzano, L, Rees, JM, Reiners, A, Samuel, B, Sanchez-Lavega, A, Sanz Forcada, J, Sasselov, D, Savini, G, Sicardy, B, Smith, A, Stixrude, L, Strazzulla, G, Tennyson, J, Tessenyi, M, Vasisht, G, Vinatier, S, Viti, S, Waldmann, I, White, GJ, Widemann, T, Wordsworth, R, Yelle, R, Yung, Y, and Yurchenko, SN
Subjects: Science & Technology, Exoplanets, EARTH-LIKE PLANETS, MU-M, Astronomy & Astrophysics, M-DWARFS, ATMOSPHERE, Space mission, EXOPLANET HD 209458B, 0201 Astronomical And Space Sciences, Physical Sciences, astro-ph.EP, UPSILON ANDROMEDAE B, TRANSMISSION SPECTRUM, PHASE CURVE, 189733B, TRANSITING EXTRASOLAR PLANET, Planetary atmospheres, astro-ph.IM
Published: 2012

25. Transiting exoplanets from the CoRoT space mission

Author: Guenther, E., Díaz, R., Gazzano, J.-C., Mazeh, T., Rouan, D., Gibson, N., Csizmadia, Sz., Aigrain, S., Alonso, R., Almenara, J., Auvergne, M., Baglin, A., Barge, P., Bonomo, A., Bordé, P., Bouchy, F., Bruntt, H., Cabrera, J., Carone, L., Carpano, S., Cavarroc, C., Deeg, H., Deleuil, M., Dreizler, S., Dvorak, R., Erikson, A., Ferraz-Mello, S., Fridlund, M., Gandolfi, D., Gillon, M., Guillot, T., Hatzes, A., Havel, M., Hébrard, G., Jehin, E., Jorda, L., Lammer, H., Léger, A., Moutou, C., Nortmann, L., Ollivier, M., Ofir, A., Pasternacki, Th., Pätzold, M., Parviainen, H., Queloz, D., Rauer, H., Samuel, B., Santerne, A., Schneider, J., Tal-Or, L., Tingley, B., Weingrill, J., Wuchterl, G., School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), School of Physics, University of Exeter, Departamento de Matemàtica, PUC RIO, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut de Recherche pour le Développement (IRD), Stellar Astrophysics Centre [Aarhus] (SAC), Aarhus University [Aarhus], Institut de Radioprotection et de Sûreté Nucléaire (IRSN), 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), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), ON/MCT (ON/MCT, 20921-030, Rio de Janeiro, Brazil)), ON/MCT, DLR Institute of Planetary Research, German Aerospace Center (DLR), Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo (USP), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Department of Brain and Behavioural Sciences, University of Pavia, Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Thüringer Landessternwarte Tautenburg (TLS), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Laboratoire des technologies de la microélectronique (LTM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Rhenish Institute for Environmental Research (RIU), University of Cologne, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut für Astrophysik [Göttingen], and Georg-August-University [Göttingen]
Subjects: [PHYS]Physics [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2012
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26. EChO

Author: Tinetti, G., Beaulieu, J. P., Henning, T., Meyer, M., Micela, G., Ribas, I., Stam, D., Swain, M., Krause, O., Ollivier, M., Pace, E., Swinyard, B., Aylward, A., van Boekel, R., Coradini, A., Encrenaz, T., Snellen, I., Zapatero-Osorio, M. R., Bouwman, J., Cho, J. Y-K., Coudé de Foresto, V., Guillot, T., Lopez-Morales, M., Mueller-Wodarg, I., Palle, E., Selsis, F., Sozzetti, A., Ade, P. A. R., Achilleos, N., Adriani, A., Agnor, C. B., Afonso, C., Prieto, C. Allende, Bakos, G., Barber, R. J., Barlow, M., Batista, V., Bernath, P., Bézard, B., Bordé, P., Brown, L. R., Cassan, A., Cavarroc, C., Ciaravella, A., Cockell, C., Coustenis, A., Danielski, C., Decin, L., Kok, R. De, Demangeon, O., Deroo, P., Doel, P., Drossart, P., Fletcher, L. N., Focardi, M., Forget, F., Fossey, S., Fouqué, P., Frith, J., Galand, M., Gaulme, P., Hernández, J. I. González, Grasset, O., Grassi, D., Grenfell, J. L., Griffin, M. J., Griffith, C. A., Grözinger, U., Guedel, M., Guio, P., Hainaut, O., Hargreaves, R., Hauschildt, P. H., Heng, Kevin, Heyrovsky, D., Hueso, R., Irwin, P., Kaltenegger, L., Kervella, P., Kipping, D., Koskinen, T. T., Kovács, G., La Barbera, A., Lammer, H., Lellouch, E., Leto, G., Lopez Morales, M., Lopez Valverde, M. A., Lopez-Puertas, M., Lovis, C., Maggio, A., Maillard, J. P., Maldonado Prado, J., Marquette, J. B., Martin-Torres, F. J., Maxted, P., Miller, S., Molinari, S., Montes, D., Moro-Martin, A., Moses, J. I., Mousis, O., Nguyen Tuong, N., Nelson, R., Orton, G. S., Pantin, E., Pascale, E., Pezzuto, S., Pinfield, D., Poretti, E., Prinja, R., Prisinzano, L., Rees, J. M., Reiners, A., Samuel, B., Sánchez-Lavega, A., Forcada, J. Sanz, Sasselov, D., Savini, G., Sicardy, B., Smith, A., Stixrude, L., Strazzulla, G., Tennyson, J., Tessenyi, M., Vasisht, G., Vinatier, S., Viti, S., Waldmann, I., White, G. J., Widemann, T., Wordsworth, R., Yelle, R., Yung, Y., and Yurchenko, S. N.
Subjects: 530 Physics, 520 Astronomy, Astrophysics::Earth and Planetary Astrophysics
Abstract: A dedicated mission to investigate exoplanetary atmospheres represents a major milestone in our quest to understand our place in the universe by placing our Solar System in context and by addressing the suitability of planets for the presence of life. EChO—the Exoplanet Characterisation Observatory—is a mission concept specifically geared for this purpose. EChO will provide simultaneous, multi-wavelength spectroscopic observations on a stable platform that will allow very long exposures. The use of passive cooling, few moving parts and well established technology gives a low-risk and potentially long-lived mission. EChO will build on observations by Hubble, Spitzer and ground-based telescopes, which discovered the first molecules and atoms in exoplanetary atmospheres. However, EChO’s configuration and specifications are designed to study a number of systems in a consistent manner that will eliminate the ambiguities affecting prior observations. EChO will simultaneously observe a broad enough spectral region—from the visible to the mid-infrared—to constrain from one single spectrum the temperature structure of the atmosphere, the abundances of the major carbon and oxygen bearing species, the expected photochemically-produced species and magnetospheric signatures. The spectral range and resolution are tailored to separate bands belonging to up to 30 molecules and retrieve the composition and temperature structure of planetary atmospheres. The target list for EChO includes planets ranging from Jupiter-sized with equilibrium temperatures T eq up to 2,000 K, to those of a few Earth masses, with T eq \u223c 300 K. The list will include planets with no Solar System analog, such as the recently discovered planets GJ1214b, whose density lies between that of terrestrial and gaseous planets, or the rocky-iron planet 55 Cnc e, with day-side temperature close to 3,000 K. As the number of detected exoplanets is growing rapidly each year, and the mass and radius of those detected steadily decreases, the target list will be constantly adjusted to include the most interesting systems. We have baselined a dispersive spectrograph design covering continuously the 0.4–16 μm spectral range in 6 channels (1 in the visible, 5 in the InfraRed), which allows the spectral resolution to be adapted from several tens to several hundreds, depending on the target brightness. The instrument will be mounted behind a 1.5 m class telescope, passively cooled to 50 K, with the instrument structure and optics passively cooled to \u223c45 K. EChO will be placed in a grand halo orbit around L2. This orbit, in combination with an optimised thermal shield design, provides a highly stable thermal environment and a high degree of visibility of the sky to observe repeatedly several tens of targets over the year. Both the baseline and alternative designs have been evaluated and no critical items with Technology Readiness Level (TRL) less than 4–5 have been identified. We have also undertaken a first-order cost and development plan analysis and find that EChO is easily compatible with the ESA M-class mission framework.
Published: 2012
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27. Exoplanets from the CoRoT space mission. XVII. The hot Jupiter CoRoT-17b: a very old planet

Author: Csizmadia, S, Moutou, C, Deleuil, M, Cabrera, J, Fridlund, M, Gandolfi, D, Aigrain, S, Alonso, R, Almenara, J, Auvergne, M, Baglin, A, Barge, P, Bonomo, A, Borde, P, Bouchy, F, Bruntt, H, Carone, L, Carpano, S, Cavarroc, C, Cochran, W.D., Deeg, H, Diaz, R, Dvorak, R, Endl, M, Erikson, A, Ferraz-Mello, S, Fruth, T, Gazzano, J-C, Gillon, M, Guenther, E., Guillot, T, Hatzes, A, Havel, M, Hebrard, G, Jehin, E, Jorda, L, Leger, A., Llebaria, A, Lammer, H, Lovis, C, MacQueen, P.J., Mazeh, T, Ollivier, M, Pätzold, M, Queloz, D, Rauer, H, Rouan, D, Santerne, A, Schneider, J., Tingley, B, Titz-Weider, R, and Wuchterl, G
Subjects: exoplanets, photometry, transit method, CoRoT-17, CoRoT
Published: 2011

28. The Mid-Infrared Instrument for theJames Webb Space Telescope, V: Predicted Performance of the MIRI Coronagraphs

Author: Boccaletti, A., primary, Lagage, P.-O., additional, Baudoz, P., additional, Beichman, C., additional, Bouchet, P., additional, Cavarroc, C., additional, Dubreuil, D., additional, Glasse, Alistair, additional, Glauser, A. M., additional, Hines, D. C., additional, Lajoie, C.-P., additional, Lebreton, J., additional, Perrin, M. D., additional, Pueyo, L., additional, Reess, J. M., additional, Rieke, G. H., additional, Ronayette, S., additional, Rouan, D., additional, Soummer, R., additional, and Wright, G. S., additional
Published: 2015
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29. Transiting exoplanets from the CoRoT space mission

Author: Alonso, R., Moutou, C., Endl, M., Almenara, J. -M, Guenther, E. W., Deleuil, M., Hatzes, A., Aigrain, S., Auvergne, M., Baglin, A., Barge, P., Bonomo, A. S., Borde, P., Bouchy, F., Cavarroc, C., Cabrera, J., Carpano, S., Csizmadia, Sz., Cochran, W. D., Deeg, H. J., Diaz, R. F., Dvorak, R., Erikson, A., Ferraz-Mello, S., Fridlund, M., Fruth, T., Gandolfi, D., Gillon, M., Grziwa, S., Guillot, T., Hebrard, G., Jorda, L., Leger, A., Lammer, H., Lovis, C., MacQueen, P. J., Mazeh, T., Ofir, A., Olivier, M., Pasternacki, T., Paetzold, M., Queloz, D., Rauer, H., Rouan, D., Santerne, A., Schneider, J., dos Santos, M. Tadeu, Tingley, B., Titz-Weider, R., Weingrill, J., Wuchterl, G., Alonso, R., Moutou, C., Endl, M., Almenara, J. -M, Guenther, E. W., Deleuil, M., Hatzes, A., Aigrain, S., Auvergne, M., Baglin, A., Barge, P., Bonomo, A. S., Borde, P., Bouchy, F., Cavarroc, C., Cabrera, J., Carpano, S., Csizmadia, Sz., Cochran, W. D., Deeg, H. J., Diaz, R. F., Dvorak, R., Erikson, A., Ferraz-Mello, S., Fridlund, M., Fruth, T., Gandolfi, D., Gillon, M., Grziwa, S., Guillot, T., Hebrard, G., Jorda, L., Leger, A., Lammer, H., Lovis, C., MacQueen, P. J., Mazeh, T., Ofir, A., Olivier, M., Pasternacki, T., Paetzold, M., Queloz, D., Rauer, H., Rouan, D., Santerne, A., Schneider, J., dos Santos, M. Tadeu, Tingley, B., Titz-Weider, R., Weingrill, J., and Wuchterl, G.
Abstract: We present the discovery of a candidate multiply transiting system, the first one found in the CoRoT mission. Two transit like features with periods of 5.11 and 11.76 d are detected in the CoRoT light curve around a main sequence K1V star of r = 15.1. If the features are due to transiting planets around the same star, these would correspond to objects of 3.7 +/- 0.4 and 5.0 +/- 0.5 R-circle plus, respectively. Several radial velocities serve to provide an upper limit of 5.7 M-circle plus for the 5.11 d signal and to tentatively measure a mass of 28(-11)(+11); M-circle plus for the object transiting with a 11.76 d period. These measurements imply low density objects, with a significant gaseous envelope. The detailed analysis of the photometric and spectroscopic data serves to estimate the probability that the observations are caused by transiting Neptune-sized planets as much as over 26 times higher than a blend scenario involving only one transiting planet and as much as over 900 times higher than a scenario involving two blends and no planets. The radial velocities show a long-term modulation that might be attributed to a 1.5 M-Jup planet orbiting at 1.8 AU from the host, but more data are required to determine the precise orbital parameters of this companion.
Published: 2014

30. Protostars and Planets with JWST-MIRI

Author: Dishoeck, E.F. van, Merín, B., Brandl, B., Böker, T., Greene, T., Meixner, M., Ressler, M., Rieke, G.H., Waelkens, C., Wright, G., Cavarroc, C., Boccaletti, A., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle Astronomie du LESIA, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: LPI Contribution No. 1286
Published: 2005

31. Transiting exoplanets from the CoRoT space mission

Author: Alonso, R., primary, Moutou, C., additional, Endl, M., additional, Almenara, J.-M., additional, Guenther, E. W., additional, Deleuil, M., additional, Hatzes, A., additional, Aigrain, S., additional, Auvergne, M., additional, Baglin, A., additional, Barge, P., additional, Bonomo, A. S., additional, Bordé, P., additional, Bouchy, F., additional, Cavarroc, C., additional, Cabrera, J., additional, Carpano, S., additional, Csizmadia, Sz., additional, Cochran, W. D., additional, Deeg, H. J., additional, Díaz, R. F., additional, Dvorak, R., additional, Erikson, A., additional, Ferraz-Mello, S., additional, Fridlund, M., additional, Fruth, T., additional, Gandolfi, D., additional, Gillon, M., additional, Grziwa, S., additional, Guillot, T., additional, Hébrard, G., additional, Jorda, L., additional, Léger, A., additional, Lammer, H., additional, Lovis, C., additional, MacQueen, P. J., additional, Mazeh, T., additional, Ofir, A., additional, Ollivier, M., additional, Pasternacki, T., additional, Pätzold, M., additional, Queloz, D., additional, Rauer, H., additional, Rouan, D., additional, Santerne, A., additional, Schneider, J., additional, Tadeu dos Santos, M., additional, Tingley, B., additional, Titz-Weider, R., additional, Weingrill, J., additional, and Wuchterl, G., additional
Published: 2014
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32. Optical performance of the JWST/MIRI flight model: characterization of the point spread function at high-resolution

Author: Oschmann, Jacobus M., Clampin, Mark C., MacEwen, Howard A., Guillard, P., Rodet, T., Ronayette, S., Amiaux, J., Abergel, A., Moreau, V., Augueres, J. L., Bensalem, A., Orduna, T., Nehmé, C., Belu, A. R., Pantin, E., Lagage, P.-O., Longval, Y., Glasse, A. C. H., Bouchet, P., Cavarroc, C., Dubreuil, D., Kendrew, S., Oschmann, Jacobus M., Clampin, Mark C., MacEwen, Howard A., Guillard, P., Rodet, T., Ronayette, S., Amiaux, J., Abergel, A., Moreau, V., Augueres, J. L., Bensalem, A., Orduna, T., Nehmé, C., Belu, A. R., Pantin, E., Lagage, P.-O., Longval, Y., Glasse, A. C. H., Bouchet, P., Cavarroc, C., Dubreuil, D., and Kendrew, S.
Abstract: The Mid Infra Red Instrument (MIRI) is one of the four instruments onboard the James Webb Space Telescope (JWST), providing imaging, coronagraphy and spectroscopy over the 5 - 28 µm band. To verify the optical performance of the instrument, extensive tests were performed at CEA on the flight model (FM) of the Mid-InfraRed IMager (MIRIM) at cryogenic temperatures and in the infrared. This paper reports on the point spread function (PSF) measurements at 5.6 µm, the shortest operating wavelength for imaging. At 5.6 µm, the PSF is not Nyquist-sampled, so we use am original technique that combines a microscanning measurement strategy with a deconvolution algorithm to obtain an over-resolved MIRIM PSF. The microscanning consists in a sub-pixel scan of a point source on the focal plane. A data inversion method is used to reconstruct PSF images that are over-resolved by a factor of 7 compared to the native resolution of MIRI. We show that the FWHM of the high-resolution PSFs were 5 - 10 % wider than that obtained with Zemax simulations. The main cause was identified as an out-of-specification tilt of the M4 mirror. After correction, two additional test campaigns were carried out, and we show that the shape of the PSF is conform to expectations. The FWHM of the PSFs are 0.18 - 0.20 arcsec, in agreement with simulations. 56.1 - 59.2% of the total encircled energy (normalized to a 5 arcsec radius) is contained within the first dark Airy ring, over the whole field of view. At longer wavelengths (7.7 - 25.5 µm), this percentage is 57 - 68 %. MIRIM is thus compliant with the optical quality requirements. This characterization of the MIRIM PSF, as well as the deconvolution method presented here, are of particular importance, not only for the verification of the optical quality and the MIRI calibration, but also for scientific applications.
Published: 2010

33. Transiting exoplanets from the CoRoT space mission

Author: Pätzold, M., primary, Endl, M., additional, Csizmadia, Sz., additional, Gandolfi, D., additional, Jorda, L., additional, Grziwa, S., additional, Carone, L., additional, Pasternacki, T., additional, Aigrain, S., additional, Almenara, J. M., additional, Alonso, R., additional, Auvergne, M., additional, Baglin, A., additional, Barge, P., additional, Bonomo, A. S., additional, Bordé, P., additional, Bouchy, F., additional, Cabrera, J., additional, Cavarroc, C., additional, Cochran, W. B., additional, Deleuil, M., additional, Deeg, H. J., additional, Díaz, R., additional, Dvorak, R., additional, Erikson, A., additional, Ferraz-Mello, S., additional, Fridlund, M., additional, Gillon, M., additional, Guillot, T., additional, Hatzes, A., additional, Hébrard, G., additional, Léger, A., additional, Llebaria, A., additional, Lammer, H., additional, MacQueen, P. J., additional, Mazeh, T., additional, Moutou, C., additional, Ofir, A., additional, Ollivier, M., additional, Parviainen, H., additional, Queloz, D., additional, Rauer, H., additional, Rouan, D., additional, Santerne, A., additional, Schneider, J., additional, Tingley, B., additional, Weingrill, J., additional, and Wuchterl, G., additional
Published: 2012
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34. EChO

Author: Tinetti, G., primary, Beaulieu, J. P., additional, Henning, T., additional, Meyer, M., additional, Micela, G., additional, Ribas, I., additional, Stam, D., additional, Swain, M., additional, Krause, O., additional, Ollivier, M., additional, Pace, E., additional, Swinyard, B., additional, Aylward, A., additional, van Boekel, R., additional, Coradini, A., additional, Encrenaz, T., additional, Snellen, I., additional, Zapatero-Osorio, M. R., additional, Bouwman, J., additional, Cho, J. Y-K., additional, Coudé de Foresto, V., additional, Guillot, T., additional, Lopez-Morales, M., additional, Mueller-Wodarg, I., additional, Palle, E., additional, Selsis, F., additional, Sozzetti, A., additional, Ade, P. A. R., additional, Achilleos, N., additional, Adriani, A., additional, Agnor, C. B., additional, Afonso, C., additional, Prieto, C. Allende, additional, Bakos, G., additional, Barber, R. J., additional, Barlow, M., additional, Batista, V., additional, Bernath, P., additional, Bézard, B., additional, Bordé, P., additional, Brown, L. R., additional, Cassan, A., additional, Cavarroc, C., additional, Ciaravella, A., additional, Cockell, C., additional, Coustenis, A., additional, Danielski, C., additional, Decin, L., additional, Kok, R. De, additional, Demangeon, O., additional, Deroo, P., additional, Doel, P., additional, Drossart, P., additional, Fletcher, L. N., additional, Focardi, M., additional, Forget, F., additional, Fossey, S., additional, Fouqué, P., additional, Frith, J., additional, Galand, M., additional, Gaulme, P., additional, Hernández, J. I. González, additional, Grasset, O., additional, Grassi, D., additional, Grenfell, J. L., additional, Griffin, M. J., additional, Griffith, C. A., additional, Grözinger, U., additional, Guedel, M., additional, Guio, P., additional, Hainaut, O., additional, Hargreaves, R., additional, Hauschildt, P. H., additional, Heng, K., additional, Heyrovsky, D., additional, Hueso, R., additional, Irwin, P., additional, Kaltenegger, L., additional, Kervella, P., additional, Kipping, D., additional, Koskinen, T. T., additional, Kovács, G., additional, La Barbera, A., additional, Lammer, H., additional, Lellouch, E., additional, Leto, G., additional, Lopez Morales, M., additional, Lopez Valverde, M. A., additional, Lopez-Puertas, M., additional, Lovis, C., additional, Maggio, A., additional, Maillard, J. P., additional, Maldonado Prado, J., additional, Marquette, J. B., additional, Martin-Torres, F. J., additional, Maxted, P., additional, Miller, S., additional, Molinari, S., additional, Montes, D., additional, Moro-Martin, A., additional, Moses, J. I., additional, Mousis, O., additional, Nguyen Tuong, N., additional, Nelson, R., additional, Orton, G. S., additional, Pantin, E., additional, Pascale, E., additional, Pezzuto, S., additional, Pinfield, D., additional, Poretti, E., additional, Prinja, R., additional, Prisinzano, L., additional, Rees, J. M., additional, Reiners, A., additional, Samuel, B., additional, Sánchez-Lavega, A., additional, Forcada, J. Sanz, additional, Sasselov, D., additional, Savini, G., additional, Sicardy, B., additional, Smith, A., additional, Stixrude, L., additional, Strazzulla, G., additional, Tennyson, J., additional, Tessenyi, M., additional, Vasisht, G., additional, Vinatier, S., additional, Viti, S., additional, Waldmann, I., additional, White, G. J., additional, Widemann, T., additional, Wordsworth, R., additional, Yelle, R., additional, Yung, Y., additional, and Yurchenko, S. N., additional
Published: 2012
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35. Transiting exoplanets from the CoRoT space mission

Author: Ollivier, M., primary, Gillon, M., additional, Santerne, A., additional, Wuchterl, G., additional, Havel, M., additional, Bruntt, H., additional, Bordé, P., additional, Pasternacki, T., additional, Endl, M., additional, Gandolfi, D., additional, Aigrain, S., additional, Almenara, J. M., additional, Alonso, R., additional, Auvergne, M., additional, Baglin, A., additional, Barge, P., additional, Bonomo, A. S., additional, Bouchy, F., additional, Cabrera, J., additional, Carone, L., additional, Carpano, S., additional, Cavarroc, C., additional, Cochran, W. D., additional, Csizmadia, Sz., additional, Deeg, H. J., additional, Deleuil, M., additional, Diaz, R. F., additional, Dvorak, R., additional, Erikson, A., additional, Ferraz-Mello, S., additional, Fridlund, M., additional, Gazzano, J.-C., additional, Grziwa, S., additional, Guenther, E., additional, Guillot, T., additional, Guterman, P., additional, Hatzes, A., additional, Hébrard, G., additional, Lammer, H., additional, Léger, A., additional, Lovis, C., additional, MacQueen, P. J., additional, Mayor, M., additional, Mazeh, T., additional, Moutou, C., additional, Ofir, A., additional, Pätzold, M., additional, Queloz, D., additional, Rauer, H., additional, Rouan, D., additional, Samuel, B., additional, Schneider, J., additional, Tadeu dos Santos, M., additional, Tal-Or, L., additional, Tingley, B., additional, and Weingrill, J., additional
Published: 2012
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36. Transiting exoplanets from the CoRoT space mission

Author: Deleuil, M., primary, Bonomo, A. S., additional, Ferraz-Mello, S., additional, Erikson, A., additional, Bouchy, F., additional, Havel, M., additional, Aigrain, S., additional, Almenara, J.-M., additional, Alonso, R., additional, Auvergne, M., additional, Baglin, A., additional, Barge, P., additional, Bordé, P., additional, Bruntt, H., additional, Cabrera, J., additional, Carpano, S., additional, Cavarroc, C., additional, Csizmadia, Sz., additional, Damiani, C., additional, Deeg, H. J., additional, Dvorak, R., additional, Fridlund, M., additional, Hébrard, G., additional, Gandolfi, D., additional, Gillon, M., additional, Guenther, E., additional, Guillot, T., additional, Hatzes, A., additional, Jorda, L., additional, Léger, A., additional, Lammer, H., additional, Mazeh, T., additional, Moutou, C., additional, Ollivier, M., additional, Ofir, A., additional, Parviainen, H., additional, Queloz, D., additional, Rauer, H., additional, Rodríguez, A., additional, Rouan, D., additional, Santerne, A., additional, Schneider, J., additional, Tal-Or, L., additional, Tingley, B., additional, Weingrill, J., additional, and Wuchterl, G., additional
Published: 2012
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37. Transiting exoplanets from the CoRoT space mission

Author: Rouan, D., primary, Parviainen, H., additional, Moutou, C., additional, Deleuil, M., additional, Fridlund, M., additional, Ofir, A., additional, Havel, M., additional, Aigrain, S., additional, Alonso, R., additional, Auvergne, M., additional, Baglin, A., additional, Barge, P., additional, Bonomo, A. S., additional, Bordé, P., additional, Bouchy, F., additional, Cabrera, J., additional, Cavarroc, C., additional, Csizmadia, Sz., additional, Deeg, H. J., additional, Diaz, R. F., additional, Dvorak, R., additional, Erikson, A., additional, Ferraz-Mello, S., additional, Gandolfi, D., additional, Gillon, M., additional, Guillot, T., additional, Hatzes, A., additional, Hébrard, G., additional, Jorda, L., additional, Léger, A., additional, Llebaria, A., additional, Lammer, H., additional, Lovis, C., additional, Mazeh, T., additional, Ollivier, M., additional, Pätzold, M., additional, Queloz, D., additional, Rauer, H., additional, Samuel, B., additional, Santerne, A., additional, Schneider, J., additional, Tingley, B., additional, and Wuchterl, G., additional
Published: 2012
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38. Transiting exoplanets from the CoRoT space mission Resolving the nature of transit candidates for the LRa03 and SRa03 fields

Author: Cavarroc, C., primary, Moutou, C., additional, Gandolfi, D., additional, Tingley, B., additional, Ollivier, M., additional, Aigrain, S., additional, Alonso, R., additional, Almenara, J.-M., additional, Auvergne, M., additional, Baglin, A., additional, Barge, P., additional, Bonomo, A. S., additional, Bordé, P., additional, Bouchy, F., additional, Cabrera, J., additional, Carpano, S., additional, Carone, L., additional, Cochran, W. D., additional, Csizmadia, S., additional, Deeg, H. J., additional, Deleuil, M., additional, Díaz, R. F., additional, Dvorak, R., additional, Endl, M., additional, Erikson, A., additional, Fridlund, M., additional, Gillon, M., additional, Guenther, E. W., additional, Guillot, T., additional, Hatzes, A., additional, Hébrard, G., additional, Jorda, L., additional, Léger, A., additional, Lammer, H., additional, Lev, T.-O., additional, Lovis, C., additional, MacQueen, P. J., additional, Mazeh, T., additional, Ofir, A., additional, Parviainen, H., additional, Pasternacki, T., additional, Pätzold, M., additional, Queloz, D., additional, Rauer, H., additional, Rouan, D., additional, Samuel, B., additional, Santerne, A., additional, Schneider, J., additional, Weingrill, J., additional, and Wuchterl, G., additional
Published: 2011
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39. THE ORBITAL PHASES AND SECONDARY TRANSITS OF KEPLER-10b. A PHYSICAL INTERPRETATION BASED ON THE LAVA-OCEAN PLANET MODEL

Author: Rouan, D., primary, Deeg, H. J., additional, Demangeon, O., additional, Samuel, B., additional, Cavarroc, C., additional, Fegley, B., additional, and Léger, A., additional
Published: 2011
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40. Transiting exoplanets from the CoRoT space mission

Author: Hébrard, G., primary, Evans, T. M., additional, Alonso, R., additional, Fridlund, M., additional, Ofir, A., additional, Aigrain, S., additional, Guillot, T., additional, Almenara, J. M., additional, Auvergne, M., additional, Baglin, A., additional, Barge, P., additional, Bonomo, A. S., additional, Bordé, P., additional, Bouchy, F., additional, Cabrera, J., additional, Carone, L., additional, Carpano, S., additional, Cavarroc, C., additional, Csizmadia, Sz., additional, Deeg, H. J., additional, Deleuil, M., additional, Díaz, R. F., additional, Dvorak, R., additional, Erikson, A., additional, Ferraz-Mello, S., additional, Gandolfi, D., additional, Gibson, N., additional, Gillon, M., additional, Guenther, E., additional, Hatzes, A., additional, Havel, M., additional, Jorda, L., additional, Lammer, H., additional, Léger, A., additional, Llebaria, A., additional, Mazeh, T., additional, Moutou, C., additional, Ollivier, M., additional, Parviainen, H., additional, Pätzold, M., additional, Queloz, D., additional, Rauer, H., additional, Rouan, D., additional, Santerne, A., additional, Schneider, J., additional, Tingley, B., additional, and Wuchterl, G., additional
Published: 2011
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41. Transiting exoplanets from the CoRoT space mission

Author: Csizmadia, Sz., primary, Moutou, C., additional, Deleuil, M., additional, Cabrera, J., additional, Fridlund, M., additional, Gandolfi, D., additional, Aigrain, S., additional, Alonso, R., additional, Almenara, J.-M., additional, Auvergne, M., additional, Baglin, A., additional, Barge, P., additional, Bonomo, A. S., additional, Bordé, P., additional, Bouchy, F., additional, Bruntt, H., additional, Carone, L., additional, Carpano, S., additional, Cavarroc, C., additional, Cochran, W., additional, Deeg, H. J., additional, Díaz, R. F., additional, Dvorak, R., additional, Endl, M., additional, Erikson, A., additional, Ferraz-Mello, S., additional, Fruth, Th., additional, Gazzano, J.-C., additional, Gillon, M., additional, Guenther, E. W., additional, Guillot, T., additional, Hatzes, A., additional, Havel, M., additional, Hébrard, G., additional, Jehin, E., additional, Jorda, L., additional, Léger, A., additional, Llebaria, A., additional, Lammer, H., additional, Lovis, C., additional, MacQueen, P. J., additional, Mazeh, T., additional, Ollivier, M., additional, Pätzold, M., additional, Queloz, D., additional, Rauer, H., additional, Rouan, D., additional, Santerne, A., additional, Schneider, J., additional, Tingley, B., additional, Titz-Weider, R., additional, and Wuchterl, G., additional
Published: 2011
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42. The extreme physical properties of the CoRoT-7b super-Earth

Author: Léger, A., primary, Grasset, O., additional, Fegley, B., additional, Codron, F., additional, Albarede, A.F., additional, Barge, P., additional, Barnes, R., additional, Cance, P., additional, Carpy, S., additional, Catalano, F., additional, Cavarroc, C., additional, Demangeon, O., additional, Ferraz-Mello, S., additional, Gabor, P., additional, Grießmeier, J.-M., additional, Leibacher, J., additional, Libourel, G., additional, Maurin, A.-S., additional, Raymond, S.N., additional, Rouan, D., additional, Samuel, B., additional, Schaefer, L., additional, Schneider, J., additional, Schuller, P.A., additional, Selsis, F., additional, and Sotin, C., additional
Published: 2011
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43. Spectral and polarimetric characterization of gazeous and telluric planets with SEE COAST

Author: Boccaletti, A., primary, Baudoz, P., additional, Mawet, D., additional, Schneider, J., additional, Tinetti, G., additional, Galicher, R., additional, Stam, D., additional, Cavarroc, C., additional, Hough, J., additional, Doel, P., additional, Pinfield, D., additional, Keller, C.-U., additional, Beuzit, J.-L., additional, Udry, S., additional, Ferrari, A., additional, Martin, E., additional, Ménard, F., additional, and Sein, E., additional
Published: 2011
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44. Sex and PRNP Genotype Determination in Preimplantation Caprine Embryos

Author: Guignot, F, primary, Perreau, C, additional, Cavarroc, C, additional, Touzé, J-L, additional, Pougnard, J-L, additional, Dupont, F, additional, Beckers, J-F, additional, Rémy, B, additional, Babilliot, J-M, additional, Bed’Hom, B, additional, Lamorinière, JM, additional, Mermillod, P, additional, and Baril, G, additional
Published: 2010
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45. Optical performance of the JWST/MIRI flight model: characterization of the point spread function at high resolution

Author: Guillard, P., primary, Rodet, T., additional, Ronayette, S., additional, Amiaux, J., additional, Abergel, A., additional, Moreau, V., additional, Augueres, J. L., additional, Bensalem, A., additional, Orduna, T., additional, Nehmé, C., additional, Belu, A. R., additional, Pantin, E., additional, Lagage, P.-O., additional, Longval, Y., additional, Glasse, A. C. H., additional, Bouchet, P., additional, Cavarroc, C., additional, Dubreuil, D., additional, and Kendrew, S., additional
Published: 2010
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46. Performance verification of the MIRI imager flight model at CEA

Author: Ronayette, S., primary, Cavarroc, C., additional, Kendrew, S., additional, Amiaux, J., additional, Auguères, J.-L., additional, Bouzat, M., additional, Guillard, P., additional, Moreau, V., additional, Pantin, E., additional, Bouchet, P., additional, Bensalem, A., additional, Orduna, T., additional, Lagage, P.-O., additional, Nehme, C., additional, Belu, A., additional, Glasse, A., additional, Baudoz, P., additional, and Dubreuil, D., additional
Published: 2010
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47. Comparison of coronagraphs for high-contrast imaging in the context of extremely large telescopes

Author: Martinez, P., primary, Boccaletti, A., additional, Kasper, M., additional, Cavarroc, C., additional, Yaitskova, N., additional, Fusco, T., additional, and Vérinaud, C., additional
Published: 2008
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48. Development approach and first infrared test results of JWST/Mid Infra Red Imager Optical Bench

Author: Amiaux, J., primary, Alouadi, F., additional, Augueres, J. L., additional, Bouchet, P., additional, Bouzat, M., additional, Cavarroc, C., additional, Cloue, C., additional, De Antoni, P., additional, Desforges, D., additional, Donati, A., additional, Dubreuil, D., additional, Eppelle, D., additional, Gougnaud, F., additional, Hervieu, B., additional, Lagage, P. O., additional, Leboeuf, D., additional, Le Mer, I., additional, Lussignol, Y., additional, Mattei, P., additional, Meigner, F., additional, Moreau, V., additional, Pantin, E., additional, Perrin, P., additional, Ronayette, S., additional, Tauzin, G., additional, Poupar, S., additional, Wright, D., additional, Glasse, A., additional, Wright, G., additional, Mazy, E., additional, Plesseria, J. Y., additional, Renotte, E., additional, Ray, T., additional, Abergel, A., additional, Guillard, P., additional, Longval, Y., additional, Ressler, M., additional, Reess, J. M., additional, Hofferbert, R., additional, Krause, O., additional, Justtanont, K., additional, and Olofsson, G., additional
Published: 2008
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49. Optimization of apodized pupil Lyot coronagraph for ELTs

Author: Martinez, P., primary, Boccaletti, A., additional, Kasper, M., additional, Baudoz, P., additional, and Cavarroc, C., additional
Published: 2007
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50. Feasibility of the Four‐Quadrant Phase Mask in the Mid‐Infrared on theJames Webb Space Telescope

Author: Baudoz, P., primary, Boccaletti, A., additional, Riaud, P., additional, Cavarroc, C., additional, Baudrand, J., additional, Reess, J. M., additional, and Rouan, D., additional
Published: 2006
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