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1. The PLATO field selection process I. Identification and content of the long-pointing fields

Author: V. Nascimbeni, G. Piotto, A. Börner, M. Montalto, P. M. Marrese, J. Cabrera, S. Marinoni, C. Aerts, G. Altavilla, S. Benatti, R. Claudi, M. Deleuil, S. Desidera, M. Fabrizio, L. Gizon, M. J. Goupil, V. Granata, A. M. Heras, D. Magrin, L. Malavolta, J. M. Mas-Hesse, S. Ortolani, I. Pagano, D. Pollacco, L. Prisinzano, R. Ragazzoni, G. Ramsay, H. Rauer, S. Udry, 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), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: planets and satellites: detection, Astronomy, FOS: Physical sciences, astronomical databases: miscellaneous, Astrophysics, Field (computer science), Task (project management), techniques: photometric, Planet, Selection (linguistics), planetary systems, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astronomy and Astrophysics, Identification (information), Stars, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Terrestrial planet, Satellite, stars: fundamental parameters, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, catalogs, Astrophysics - Earth and Planetary Astrophysics
Abstract: PLATO (PLAnetary Transits and Oscillations of stars) is an ESA M-class satellite planned for launch by end 2026 and dedicated to the wide-field search of transiting planets around bright and nearby stars, with a strong focus on discovering habitable rocky planets hosted by solar-like stars. The choice of the fields to be pointed at is a crucial task since it has a direct impact on the scientific return of the mission. In this paper we describe and discuss the formal requirements and the key scientific prioritization criteria that have to be taken into account in the Long-duration Observation Phase (LOP) field selection, and apply a quantitative metric to guide us in this complex optimization process. We identify two provisional LOP fields, one for each hemisphere (LOPS1, LOPN1), and discuss their properties and stellar content. While additional fine-tuning shall be applied to LOP selection before the definitive choice (to be made two years before launch), we expect their position will not move by more than a few degrees with respect to what is proposed in this paper., Comment: 17 pages, 10 figures, 3 tables, A&A in press (accepted: October 26, 2021). Some typos corrected. Author list corrected
Published: 2022
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2. Modeling the structure of irradiated ocean planets - implications for mass-radius relationships

Author: Olivier Mousis, Emmanuel Marcq, Artyom Aguichine, M. Deleuil, 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), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, Planet, [SDU]Sciences of the Universe [physics], Radius, Irradiation, Astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract: Water-rich planets should be ubiquitous in the universe. Among the current exoplanet populations, many of those worlds are subject to important irradiation from their host star. As a consequence, water-rich worlds display supercritical water layer surrounded by an extended steam atmosphere making them good candidates for matching the observed mass-radius distribution of sub-Neptunes [1]. Here we describe a model that computes a realistic structure for water-rich planets by combining an interior model with an updated equation of state (EoS) for water, and an atmospheric model that takes into account radiative transfer. Our model has been applied to the GJ 9827 system as a test case and indicates Earth- or Venus-like interiors for planets b and c, respectively. Planet d could be an irradiated ocean planet with a water mass fraction of ∼20 ± 10%. We also provide mass-radius relationships for water-rich planets and their analytical expression. This allows one to directly retrieve a wide range of planetary compositions, without the requirement to run the model. The possible existence of such planets is discussed in light of atmospheric loss processes, suggesting that some sub-Neptunes are the outcome of planets that lost their H/He reservoirs. Figure 1. Mass-radius relationships produced by our model (green, yellow and red thick lines) [2], compared to mass-radius relationships of planets with only condensed phases and no atmosphere (black, grey and light blue thin lines) [3,4]. A few planets of the solar system, the GJ-9827 system and the TOI-178 system are shown as well [5,6]. [1] Mousis, O., Deleuil, M., Aguichine, A., et al. 2020, ApJL, 896, L22.[2] Aguichine, A., Mousis, O., Deleuil, M., et al. 2021, accepted in ApJ.[3] Zeng, L., Sasselov, D. D., & Jacobsen, S. B. 2016, ApJ, 819, 127.[4] Brugger, B., Mousis, O., Deleuil, M., et al. 2017, ApJ, 850, 93.[5] Kosiarek, M. R., Berardo, D. A., Crossfield, I. J. M., et al. 2021, AJ, 161, 47.[6] Leleu, A., Alibert, Y., Hara, N. C., et al. 2021, A&A, 649, A26.
Published: 2021
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3. Discovery and characterization of the exoplanets WASP-148b and c

Author: Jose-Manuel Almenara, K. Lam, Coel Hellier, Jorge Prieto-Arranz, Barry Smalley, Olivier Demangeon, Pierre F. L. Maxted, M. Martin-Lagarde, Flavien Kiefer, S. C. C. Barros, G. Boué, Carole A. Haswell, T. Lopez, Richard G. West, P. A. Wilson, D. Verilhac, Don Pollacco, D. J. A. Brown, Alexandre Santerne, P. Boumis, Jacques Laskar, Oliver Turner, Enric Palle, H. P. Osborn, James McCormac, Alexandre C. M. Correia, Aldo S. Bonomo, Peter J. Wheatley, Guillaume Hébrard, Didier Queloz, M. Deleuil, Ulrich Kolb, Louise D. Nielsen, Isabelle Boisse, Rodrigo F. Díaz, Stéphane Udry, A. Collier Cameron, A. Lecavelier des Etangs, François Bouchy, David R. Anderson, Amanda P. Doyle, S. Dalal, 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Departamento de Fisica [Aveiro], Universidade de Aveiro, University of St Andrews [Scotland], 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), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Inflammatory Bowel Disease Center,, Cedars-Sinai Medical Center, Université Paris-Sud - Paris 11 (UP11), Laboratoire de Génie de la Conception (LGeco), Institut National des Sciences Appliquées - Strasbourg (INSA Strasbourg), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA), Institute of Physical Chemistry, Johannes Gutenberg - Universität Mainz = Johannes Gutenberg University (JGU), University of Toronto, Institut National de la Santé et de la Recherche Médicale (INSERM), University of Warwick [Coventry], Department of Geosciences and Natural Resource Management [Copenhagen] (IGN), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, The University of Sydney, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Johannes Gutenberg - Universität Mainz (JGU), University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Université de Genève (UNIGE), Universidade do Porto, Queloz, Didier [0000-0002-3012-0316], and Apollo - University of Cambridge Repository
Subjects: Orbital plane, FOS: Physical sciences, Astrophysics, 01 natural sciences, spectroscopic [Techniques], techniques: photometric, Planet, QB460, 0103 physical sciences, Hot Jupiter, techniques: radial velocities, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, QA, 010303 astronomy & astrophysics, planetary systems, QB600, QC, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, radial velocities [Techniques], 010308 nuclear & particles physics, photometric [Techniques], Astronomy and Astrophysics, DAS, Planetary system, Light curve, Orbital period, Exoplanet, Radial velocity, Planetary systems, QC Physics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery and characterization of WASP-148, a new extrasolar system that includes at least two giant planets. The host star is a slowly rotating inactive late-G dwarf with a V=12 magnitude. The planet WASP-148b is a hot Jupiter of 0.72 R_Jup and 0.29 M_Jup that transits its host with an orbital period of 8.80 days. We found the planetary candidate with the SuperWASP photometric survey, then characterized it with the SOPHIE spectrograph. Our radial velocity measurements subsequently revealed a second planet in the system, WASP-148c, with an orbital period of 34.5 days and a minimum mass of 0.40 M_Jup. No transits of this outer planet were detected. The orbits of both planets are eccentric and fall near the 4:1 mean-motion resonances. This configuration is stable on long timescales, but induces dynamical interactions so that the orbits differ slightly from purely Keplerian orbits. In particular, WASP-148b shows transit-timing variations of typically 15 minutes, making it the first interacting system with transit-timing variations that is detected on ground-based light curves. We establish that the mutual inclination of the orbital plane of the two planets cannot be higher than 35 degrees, and the true mass of WASP-148c is below 0.60 M_Jup. We present photometric and spectroscopic observations of this system that cover a time span of ten years. We also provide their Keplerian and Newtonian analyses; these analyses should be significantly improved through future TESS~observations., 16 pages, 10 figures, 7 tables, A&A in press
Published: 2021
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4. CHEOPS precision phase curve of the Super-Earth 55 Cancri e

Author: Luca Fossati, M. Fridlund, Giampaolo Piotto, M. Beck, D. L. Pollacco, G. Olofsson, M. Deleuil, K. G. Isaak, Alexis Brandeker, P. Guterman, A. Lecavelier des Etangs, Nicolas Billot, Heike Rauer, Michaël Gillon, Anders Erikson, N. C. Santos, Laetitia Delrez, Andrew Collier Cameron, T. G. Wilson, Wolfgang Baumjohann, D. Segransan, Yann Alibert, C. Lovis, Kevin Heng, C. Broeg, Gisbert Peter, B. Ulmer, Manuel Guedel, B. O. Demory, Sergio Hoyer, Monika Lendl, Mahmoudreza Oshagh, Melvyn B. Davies, Brett M. Morris, J. Cabrera, Roberto Ragazzoni, Gy. M. Szabó, D. Queloz, Vincent Bourrier, S. G. Sousa, A. García Muñoz, Davide Gandolfi, Jacques Laskar, Willy Benz, S. Charnoz, Francisco J. Pozuelos, T. Bárczy, Nicola Rando, Thomas Beck, D. De Miguel Ferreras, David Ehrenreich, Pierre F. L. Maxted, G. Anglada Escudé, S. C. C. Barros, H. G. Floren, A. Deline, László L. Kiss, A. Bekkelien, M. Steller, D. Futyan, G. Scandariato, A. M. Smith, S. Sulis, I. Pagano, O. D. S. Demangeon, I. Ribas, M. Lieder, A. E. Simon, X. Bonfils, Andrea Fortier, Maria Bergomi, Roland Ottensamer, V. Nascimbeni, Demetrio Magrin, N. Thomas, David Barrado, Enric Palle, A. Pizarro Rubio, Roi Alonso, Stéphane Udry, N. A. Walton, Valérie Van Grootel, Cavendish Laboratory, University of Cambridge [UK] (CAM), Stockholm University, Institut für Festkörper- und Materialphysik, Technische Universität Dresden, Technische Universität Dresden = Dresden University of Technology (TU Dresden), 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), Center for Space and Habitability (CSH), University of Bern, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Swiss Space Office, Swiss National Science Foundation, European Commission, Fundação para a Ciência e a Tecnologia (Portugal), Queloz, Didier [0000-0002-3012-0316], Walton, Nicholas [0000-0003-3983-8778], and Apollo - University of Cambridge Repository
Subjects: Atmospheres, 010504 meteorology & atmospheric sciences, 55 Cnc, individual: 55 Cnc e [Planets and satellites], Astrophysics, 01 natural sciences, techniques: photometric, Spitzer Space Telescope, Planet, QB460, Methods, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Observational, Instrumentation, QC, planets and satellites: individual: 55 Cnc e, Eclipse, QB, Earth and Planetary Astrophysics (astro-ph.EP), Physics, planets and satellites: atmospheres, Super-Earth, 520 Astronomy, Planets and Satellites, Exoplanet, instrumentation: photometers, Amplitude, atmospheres [Planets and satellites], Astrophysics::Earth and Planetary Astrophysics, methods: observational, individual: 55 Cnc [Stars], FOS: Physical sciences, Individual, Photometric, Photometry (optics), stars: individual: 55 Cnc, 0103 physical sciences, observational [Methods], invidual: 55 Cnc [Stars], QB600, 0105 earth and related environmental sciences, MCC, Photometers, Stars: invidual: 55 Cnc, photometric [Techniques], Astronomy and Astrophysics, DAS, Phase curve, 620 Engineering, Stars, Techniques, photometers [Instrumentation], QC Physics, 13. Climate action, Space and Planetary Science, Instrumentation: photometers, Methods: observational, Planets and satellites: atmospheres, Planets and satellites: individual: 55 Cnc e, Stars: individual: 55 Cnc, Techniques: photometric, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 55 Cnc e, Astrophysics - Earth and Planetary Astrophysics
Abstract: Morris, B. M. et al., [Context] 55 Cnc e is a transiting super-Earth (radius 1.88 R⊕ and mass 8 M⊕) orbiting a G8V host star on a 17-h orbit. Spitzer observations of the planet's phase curve at 4.5 μm revealed a time-varying occultation depth, and MOST optical observations are consistent with a time-varying phase curve amplitude and phase offset of maximum light. Both broadband and high-resolution spectroscopic analyses are consistent with either a high mean molecular weight atmosphere or no atmosphere for planet e. A long-term photometric monitoring campaign on an independent optical telescope is needed to probe the variability in this system. [Aims] We seek to measure the phase variations of 55 Cnc e with a broadband optical filter with the 30 cm effective aperture space telescope CHEOPS and explore how the precision photometry narrows down the range of possible scenarios. [Methods] We observed 55 Cnc for 1.6 orbital phases in March of 2020. We designed a phase curve detrending toolkit for CHEOPS photometry which allowed us to study the underlying flux variations in the 55 Cnc system. [Results] We detected a phase variation with a full-amplitude of 72 ± 7 ppm, but did not detect a significant secondary eclipse of the planet. The shape of the phase variation resembles that of a piecewise-Lambertian; however, the non-detection of the planetary secondary eclipse, and the large amplitude of the variations exclude reflection from the planetary surface as a possible origin of the observed phase variations. They are also likely incompatible with magnetospheric interactions between the star and planet, but may imply that circumplanetary or circumstellar material modulate the flux of the system. [Conclusions] This year, further precision photometry of 55 Cnc from CHEOPS will measure variations in the phase curve amplitude and shape over time., Centre of Competence in Research (NCCR) supported by the Swiss National Science Foundation (SNSF). CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The Swiss participation to CHEOPS has been supported by the Swiss Space Office (SSO) in the framework of the Prodex programme and the Activités Nationales Complémentaires (ANC), the Universities of Bern and Geneva as well as of the NCCR PlanetS and the Swiss National Science Foundation. This work benefited from support from the Swiss National Science Foundation (PP00P2-163967 and PP00P2-190080). This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement No 724427). This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987. S.C.C.B. and S.G.S. acknowledge support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004, IF/00028/2014/CP1215/CT0002. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). X.B., S.C., D.G., M.F. and J.L. acknowledge their roles as ESA-appointed CHEOPS science team members. A.C.C. and T.W. acknowledge support from STFC consolidated grant number ST/R000824/1. This project was supported by the CNES. S.H. gratefully acknowledges CNES funding through the grant 837319. P.M. acknowledges support from STFC consolidated grant number ST/M001040/1. K.G.I. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme.
Published: 2021
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5. Spi-OPS: Spitzer and CHEOPS confirm the near-polar orbit of MASCARA-1 b and reveal a hint of dayside reflection

Author: T. Bárczy, Willy Benz, Sz. Csizmadia, Sergio Hoyer, David Ehrenreich, Nicholas A. Walton, Carina M. Persson, T. G. Wilson, Anders Erikson, Kevin Heng, H. Parviainen, M. Deleuil, Michaël Gillon, Yann Alibert, Ignasi Ribas, Olivier Demangeon, Don Pollacco, Demetrio Magrin, Juan Cabrera, Gy. M. Szabó, F. Ratti, Gaetano Scandariato, Luca Fossati, Mahmoudreza Oshagh, A. Bonfanti, Giampaolo Piotto, Nicolas Billot, G. Anglada Escudé, Alexis Brandeker, Gisbert Peter, Roberto Ragazzoni, Matthew J. Hooton, Heike Rauer, X. Bonfils, Nicola Rando, Malcolm Fridlund, Antoine Simon, C. Lovis, László L. Kiss, Göran Olofsson, Roi Alonso, Stéphane Udry, Enric Palle, S. G. Sousa, Andrea Fortier, M.-D. Busch, C. Broeg, Nuno C. Santos, David Barrado, Damien Ségransan, Roland Ottensamer, M. Steller, A. Luntzer, A. Deline, B. Ulmer, B. O. Demory, Brett M. Morris, Thomas Beck, Nicolas Thomas, Valerio Nascimbeni, Pierre F. L. Maxted, S. C. C. Barros, Sébastien Charnoz, Wolfgang Baumjohann, Isabella Pagano, Valérie Van Grootel, D. Futyan, Jacques Laskar, K. Jones, A. Lecavelier des Etangs, Mathias Beck, Alexis M. S. Smith, Laetitia Delrez, Vincent Bourrier, A. Collier Cameron, Melvyn B. Davies, Manuel Güdel, Kate Gudrun Isaak, Monika Lendl, Davide Gandolfi, Jacopo Farinato, S. Sulis, Didier Queloz, D. Kitzmann, Sébastien Salmon, Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, 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), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, 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), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Swiss National Science Foundation, Science and Technology Facilities Council (UK), Fundação para a Ciência e a Tecnologia (Portugal), European Research Council, European Commission, National Aeronautics and Space Administration (US), Ministerio de Economía y Competitividad (España), Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Space Agency, and Generalitat de Catalunya
Subjects: Astrophysics, 01 natural sciences, Geometric albedo, QB460, Planets and satellites: atmospheres, QB Astronomy, 610 Medicine & health, 010303 astronomy & astrophysics, QC, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 520 Astronomy, 3rd-DAS, techniques photometric, symbols, atmospheres [Planets and satellites], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, FOS: Physical sciences, individual: MASCARA-1 b [Planets and satellites], Photometry (optics), symbols.namesake, Bond albedo, planets and satellites individual, 0103 physical sciences, Hot Jupiter, planets and satellites physical evolution, MASCARA-1 b, Gravity darkening, Instrumentation and Methods for Astrophysics (astro-ph.IM), QB600, physical evolution [Planets and satellites], MCC, 010308 nuclear & particles physics, Stellar rotation, photometric [Techniques], Planets and satellites: individual: MASCARA-1 b, Astronomy and Astrophysics, 620 Engineering, Light curve, Stars, QC Physics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], planets and satellites atmospheres, Planets and satellites: physical evolution, Techniques: photometric, 570 Life sciences, biology, Astrophysics - Earth and Planetary Astrophysics
Abstract: M. J. Hooton et al., [Context] The light curves of tidally locked hot Jupiters transiting fast-rotating, early-type stars are a rich source of information about both the planet and star, with full-phase coverage enabling a detailed atmospheric characterisation of the planet. Although it is possible to determine the true spin–orbit angle Ψ – a notoriously difficult parameter to measure – from any transit asymmetry resulting from gravity darkening induced by the stellar rotation, the correlations that exist between the transit parameters have led to large disagreements in published values of Ψ for some systems., [Aims] We aimed to study these phenomena in the light curves of the ultra-hot Jupiter MASCARA-1 b, which is characteristically similar to well-studied contemporaries such as KELT-9 b and WASP-33 b., [Methods] We obtained optical CHaracterising ExOPlanet Satellite (CHEOPS) transit and occultation light curves of MASCARA-1 b, and analysed them jointly with a Spitzer/IRAC 4.5 μm full-phase curve to model the asymmetric transits, occultations, and phase-dependent flux modulation. For the latter, we employed a novel physics-driven approach to jointly fit the phase modulation by generating a single 2D temperature map and integrating it over the two bandpasses as a function of phase to account for the differing planet–star flux contrasts. The reflected light component was modelled using the general ab initio solution for a semi-infinite atmosphere., [Results] When fitting the CHEOPS and Spitzer transits together, the degeneracies are greatly diminished and return results consistent with previously published Doppler tomography. Placing priors informed by the tomography achieves even better precision, allowing a determination of Ψ = 72.1−2.4+2.5 deg. From the occultations and phase variations, we derived dayside and nightside temperatures of 3062−68+66 K and 1720 ± 330 K, respectively.Our retrieval suggests that the dayside emission spectrum closely follows that of a blackbody. As the CHEOPS occultation is too deep to be attributed to blackbody flux alone, we could separately derive geometric albedo Ag = 0.171−0.068+0.066 and spherical albedo As = 0.266−0.100+0.097 from the CHEOPS data, and Bond albedoAB = 0.057−0.101+0.083 from the Spitzer phase curve.Although small, the Ag and As indicate that MASCARA-1 b is more reflective than most other ultra-hot Jupiters, where H− absorption is expected to dominate., [Conclusions] Where possible, priors informed by Doppler tomography should be used when fitting transits of fast-rotating stars, though multi-colour photometry may also unlock an accurate measurement of Ψ. Our approach to modelling the phase variations at different wavelengths provides a template for how to separate thermal emission from reflected light in spectrally resolved James Webb Space Telescope phase curve data., Y.A. acknowledge the support of the Swiss National Fund under grant 200020_172746. S.H. gratefully acknowledges CNES funding through the grant 837319. D.K. acknowledges partial financial support from the Center for Space and Habitability (CSH), the PlanetS National Center of Competence in Research (NCCR), and the Swiss National Science Foundation and the Swiss-based MERAC Foundation. A.C.C. and T.G.W. acknowledge support from STFC consolidated grant number ST/M001296/1. P.M. acknowledges support from STFC research grant number ST/M001040/1. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). S.S. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 833925, project STAREX). A.Br. was supported by the SNSA. This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalizacão by these grants: UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017 and POCI-01-0145-FEDER- 032113, PTDC/FIS-AST/28953/2017 and POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 and POCI-01-0145-FEDER-028987, O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia Maria de Maeztu-Centro de Astrobiologí a (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. X.B., S.C., D.G., M.F., and J.L. acknowledge their roles as ESA-appointed CHEOPS science team members. This project was supported by the CNES. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES. grant agreement no. 724427). D.E. acknowledges financial support from the Swiss National Science Foundation for project 200021_200726. C.M.P. and M.F. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). D.G. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 ‘Gaseousor rocky? Unveiling the nature of small worlds’. M.G. is an F.R.S.-FNRS Senior Research Associate. KGI is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. Acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B-C33, as well as the support of the Generalitat de Catalunya/CERCA programme. S.G.S. acknowledges support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). This project has been supported by the Hungarian National Research, Development and Innovation Office (NKFIH) grants GINOP-2.3.2-15-2016-00003, K-119517, K-125015, and the City of Szombathely under Agreement No. 67.177-21/2016., , , ,
Published: 2021
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6. CHEOPS observations of the HD 108236 planetary system

Author: D. Segransan, Oscar Barragán, K. G. Isaak, I. Pagano, Monika Lendl, O. D. S. Demangeon, M. Beck, E. Hernandez, Thomas Beck, Luca Fossati, Sergio Hoyer, J. Cabrera, V. Van Eylen, I. Ribas, V. Nascimbeni, Giampaolo Piotto, Willy Benz, T. Kuntzer, L. Borsato, Vardan Adibekyan, Mario Salatti, T. Bandy, A. E. Simon, Heike Rauer, M. Steller, Matteo Munari, Jacopo Farinato, Gisbert Peter, Roi Alonso, Valérie Van Grootel, Luca Marafatto, J. Asquier, T. Bárczy, Alexander J. Mustill, B. Chazelas, Stéphane Udry, C. Corral Van Damme, Virginie Cessa, P. Guterman, Nicola Rando, Malcolm Fridlund, L. Delrez, Gy. M. Szabó, Anders Erikson, Alexis Brandeker, Harald Michaelis, D. Futyan, Nuno C. Santos, David Barrado, Enric Palle, Roberto Ragazzoni, Maria Bergomi, T. G. Wilson, S. Salmon, C. Broeg, M. Sordet, D. L. Pollacco, R. Rohlfs, N. A. Walton, M. J. Hooton, Didier Queloz, Davide Gandolfi, M. Gillon, Jacques Laskar, Valentina Viotto, Roland Ottensamer, B. O. Demory, A. Collier Cameron, Melvyn B. Davies, H. Ottacher, Pierre F. L. Maxted, S. C. C. Barros, Carina M. Persson, C. Lovis, Kevin Heng, L. Malvasio, Francois Wildi, X. Bonfils, M. Deleuil, M. Tschentscher, A. Lecavelier des Etangs, Hugh P. Osborn, Andrea Fortier, Daniele Piazza, László L. Kiss, S. G. Sousa, Martin Rieder, F. Ratti, G. Scandariato, S. Charnoz, A. García Muñoz, J. Hasiba, A. M. Smith, Ingo Walter, M.-D. Busch, G. Olofsson, F. Safa, David Ehrenreich, A. Bonfanti, Yann Alibert, G. Lacedelli, Nicolas Billot, A. Bekkelien, Wolfgang Baumjohann, Manuel Guedel, D. Wolter, Demetrio Magrin, N. Thomas, A. Tuson, Ministerio de Ciencia, Innovación y Universidades (España), Université de Liège, Fundação para a Ciência e a Tecnologia (Portugal), Swiss Space Office, Autoridade de Gestão do Programa Operacional Competitividade e Internacionalização (Portugal), European Commission, Swedish National Space Agency, Centre National D'Etudes Spatiales (France), Agenzia Spaziale Italiana, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Bonfanti, A. [0000-0002-1916-5935], Cameron, A. [0000-0002-8863-7828], Santos, N. [0000-0003-4422-2919], Mustill, A. J. [0000-0002-2086-3642], Swiss Space Office (SSO), La Silla Observatory, Austrian Research Promotion Agency (FFG), European Research Council (ERC), Swiss National Science Foundation (SNSF), Agencia Estatal de Investigación (AEI), Generalitat de Catalunya, European Space Agency (ESA), Fundacao para a Ciencia e a Tecnologia (FCT), Belgian Federal Science Policy Office (BELSPO), Hungarian National Research, Development and Innovation Office (NKFIH), Istituto Nazionale di Astrofisica (INAF), Swedish National Infrastructure for Computing (SNIC), Science & Technology Facilities Council, University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Space Research Institute, Austrian Academy of Sciences, Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: planets and satellites: detection, Outer planets, Fundamental Parameters, 010504 meteorology & atmospheric sciences, Stellar mass, Astrophysics::High Energy Astrophysical Phenomena, Institut für Planetenforschung, fundamental parameters [Planets and satellites], FOS: Physical sciences, Astrophysics, Ephemerides, Ephemeris, Planets and satellites: Detection, Planets and satellites: Fundamental parameters, Stars: Fundamental parameters, 01 natural sciences, 7. Clean energy, fundamental parameters [Stars], Planet, 0103 physical sciences, QB Astronomy, planets and satellites: fundamental parameters, 010303 astronomy & astrophysics, QC, QB, 0105 earth and related environmental sciences, Condensed Matter::Quantum Gases, Earth and Planetary Astrophysics (astro-ph.EP), Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], DAS, Astronomy and Astrophysics, Planets and Satellites, Planetary system, Orbital period, Light curve, Stars, Photometry (astronomy), detection [Planets and satellites], Detection, QC Physics, 13. Climate action, Space and Planetary Science, Condensed Matter::Strongly Correlated Electrons, stars: fundamental parameters, Optik, Kalibrierung und Validierung, QB799, Astrophysics - Earth and Planetary Astrophysics
Abstract: Bonfati, A. et al. (Fermi-LAT Collaboration), [Context] The detection of a super-Earth and three mini-Neptunes transiting the bright (V = 9.2 mag) star HD 108236 (also known as TOI-1233) was recently reported on the basis of TESS and ground-based light curves. [Aims] We perform a first characterisation of the HD 108236 planetary system through high-precision CHEOPS photometry and improve the transit ephemerides and system parameters. [Methods] We characterise the host star through spectroscopic analysis and derive the radius with the infrared flux method. We constrain the stellar mass and age by combining the results obtained from two sets of stellar evolutionary tracks. We analyse the available TESS light curves and one CHEOPS transit light curve for each known planet in the system. [Results] We find that HD 108236 is a Sun-like star with R? = 0.877 ± 0.008 R? , M? = 0.869-0.048+0.050 M? , and an age of 6.7-5.1+4.0 Gyr. We report the serendipitous detection of an additional planet, HD 108236 f, in one of the CHEOPS light curves. For this planet, the combined analysis of the TESS and CHEOPS light curves leads to a tentative orbital period of about 29.5 days. From the light curve analysis, we obtain radii of 1.615 ± 0.051, 2.071 ± 0.052, 2.539-0.065+0.062, 3.083 ± 0.052, and 2.017-0.057+0.052 R? for planets HD 108236 b to HD 108236 f, respectively. These values are in agreement with previous TESS-based estimates, but with an improved precision of about a factor of two. We perform a stability analysis of the system, concluding that the planetary orbits most likely have eccentricities smaller than 0.1. We also employ a planetary atmospheric evolution framework to constrain the masses of the five planets, concluding that HD 108236 b and HD 108236 c should have an Earth-like density, while the outer planets should host a low mean molecular weight envelope. [Conclusions] The detection of the fifth planet makes HD 108236 the third system brighter than V = 10 mag to host more than four transiting planets. The longer time span enables us to significantly improve the orbital ephemerides such that the uncertainty on the transit times will be of the order of minutes for the years to come. A comparison of the results obtained from the TESS and CHEOPS light curves indicates that for a V - 9 mag solar-like star and a transit signal of -500 ppm, one CHEOPS transit light curve ensures the same level of photometric precision as eight TESS transits combined, although this conclusion depends on the length and position of the gaps in the light curve., National Science Foundation. Based on observations made with the ESO 3.6 m telescope at the La Silla Observatory under program ID 1102.C-0923. M.Le acknowledges support from the Austrian Research Promotion Agency (FFG) under project 859 724 “GRAPPA”. A.D. and D.E. acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project Four Aces; grant agreement No 724427). M.J.H. acknowledges the support of the Swiss National Fund under grant 200020172746. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). The Spanish scientific participation in CHEOPS has been supported by the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87676-C5-1-R, PGC2018-098153-B-C31, PGC2018-098153-B-C33, and MDM-2017-0737 Unidad de Excelencia María de Maeztu-Centro de Astrobiología (INTA-CSIC), as well as by the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. This work was supported by Fundação para a Ciência e a Tecnologia (FCT) through national funds and by Fundo Europeu de Desenvolvimento Regional (FEDER) via COMPETE2020 - Programa Operacional Competitividade e Internacional-ização through the research grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987. S.C.C.B. and S.G.S. acknowledge support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004, IF/00028/2014/CP1215/CT0002. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. M.G. is F.R.S.-FNRS Senior Research Associate. S.Sa has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 833925, project STAREX). G.M.S. acknowledges funding from the Hungarian National Research, Development and Innovation Office (NKFIH) grant GINOP-2.3.2-15-2016-00003 and K-119517. For Italy, CHEOPS actvities have been supported by the Italian Space Agency, under the programs: ASI-INAF n. 2013-016-R.0 and ASI-INAF n. 2019-29-HH.0. L.B., G.P., I.P., G.S., and V.N. acknowledge the funding support from Italian Space Agency (ASI) regulated by “Accordo ASI-INAF n. 2013-016-R.0 del 9 luglio 2013 e integrazione del 9 luglio 2015”. G.La acknowledges support by CARIPARO Foundation, according to the agreement CARIPARO-Università degli Studi di Padova (Pratica n. 2018/0098). A.Mu acknowledges support from the Swedish National Space Agency (grant 120/19 C). The dynamical simulations were enabled by resources provided by the Swedish National Infrastructure for Computing (SNIC) at Lunarc partially funded by the Swedish Research Council through grant agreement no. 2016-07213. Simulations in this paper made use of the REBOUND code which is freely available at http://github.com/hannorein/rebound. S.Ho acknowledges CNES funding through the grant 837 319. K.G.I. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. X.B., S.C., D.G., M.F., and J.L. acknowledge their roles as ESA-appointed CHEOPS science team members. A.B. acknowledges B. Akinsanmi, G. Bruno, M. Günther, R. Luque, F.J. Pozuelos Romero, and L.M. Serrano for the very fruitful discussions. We acknowledge T. Daylan for his help in planning the CHEOPS observations.
Published: 2021
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7. A self-consistent thermodynamic approach to compute the interiors of irradiated ocean planets

Author: Olivier Mousis, Emmanuel Marcq, Artyom Aguichine, and M. Deleuil
Subjects: Physics, Planet, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Irradiation, Self consistent
Abstract: Planetary interior models rely on the thermodynamic properties of the used materials. Equations of states (EOSs) are key ingredients to compute internal structures, as they link the pressure and density profiles, and leave a unique solution satisfying all equations describing the interior of the planet. Often, when thermodynamic data are lacking, the formulation of EOSs allow extrapolation in both pressure and temperature. The effect of temperature on EOSs is often minor, implying that models of isothermal planets provide consistent results. This approach meets limitations in the case of fluids (liquids, gases and supercritical fluids), whose properties are very sensitive to variations in temperature. Here we propose a way to compute the relevant thermodynamic parameters in supercritical water from the most recent EOSs, in order to compute the internal structures of irradiated ocean planets, coupled with a 1D convective-radiative atmospheric model. Our results allow a better understanding of the diversity of observed sub-Neptunes, linking their internal structure to formation conditions.
Published: 2020
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8. The hot dayside and asymmetric transit of WASP-189 b seen by CHEOPS

Author: H. Ottacher, T. Kuntzer, M. Steller, Xavier Bonfils, A. García Muñoz, Don Pollacco, Ingo Walter, Gaetano Scandariato, A. Deline, Ignasi Ribas, J. Hasiba, T. Bandy, Bruno Chazelas, Yann Alibert, Luca Marafatto, Maria Bergomi, E. Hernandez, Michaël Gillon, Anders Erikson, O. Demangeon, Valerio Nascimbeni, Heike Rauer, N. Thomas, Virginie Cessa, G. Olofsson, F. Safa, R. Rohlfs, N. A. Walton, C. Broeg, Didier Queloz, C. Corral Van Damme, D. Futyan, Nicola Rando, Malcolm Fridlund, Federico Biondi, Roi Alonso, David Ehrenreich, T. Lüftinger, Stéphane Udry, László L. Kiss, K. G. Isaak, Wolfgang Baumjohann, Alexis M. S. Smith, Monika Lendl, D. Wolter, A. E. Simon, Thomas Beck, L. Malvasio, Nuno C. Santos, David Barrado, Demetrio Magrin, J. Asquier, V. Singh, Enric Palle, Damien Ségransan, Pierre F. L. Maxted, Roland Ottensamer, Gisbert Peter, M.-D. Busch, S. C. C. Barros, D. Kitzmann, Willy Benz, S. Hoyer, B. M. Morris, C. Lovis, Kevin Heng, Isabella Pagano, S. Salmon, Davide Gandolfi, Jacopo Farinato, Gy. M. Szabó, Sébastien Charnoz, Giampaolo Piotto, A. Bekkelien, Andrea Fortier, M. Sordet, A. Bonfanti, Nicolas Billot, Luca Fossati, Jacques Laskar, Francois Wildi, Szilard Csizmadia, Martin Rieder, M. Tschentscher, Valérie Van Grootel, Valentina Viotto, Vincent Bourrier, Roberto Ragazzoni, M. Beck, M. J. Hooton, F. Ratti, T. G. Wilson, T. Bárczy, L. Delrez, Daniele Piazza, A. Collier Cameron, Melvyn B. Davies, S. G. Sousa, B. O. Demory, Juan Cabrera, Alexis Brandeker, P. Guterman, M. Deleuil, A. Lecavelier des Etangs, Harald Michaelis, Matteo Munari, Swiss Space Office, University of Bern, Swiss National Science Foundation, Austrian Research Promotion Agency, German Research Foundation, European Commission, Ministerio de Ciencia e Innovación (España), Consejo Superior de Investigaciones Científicas (España), Generalitat de Catalunya, Fundação para a Ciência e a Tecnologia (Portugal), Fédération Wallonie-Bruxelles, Hungarian Scientific Research Fund, Agenzia Spaziale Italiana, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Wilson, T. G. [0000-0001-8749-1962], Cameron, A. [0000-0002-8863-7828], Fridlund, M. [0000-0002-0855-8426], Cabrera, J. [0000-0001-6653-5487], Barros, S. [0000-0003-2434-3625], Santos, N. [0000-0003-4422-2919], Piotto, G. [0000-0002-9937-6387], Austrian Research Promotion Agency (FFG), Deutsche Forschungsgemeinschaft (DFG), European Research Council (ERC), Swiss National Science Foundation (SNSF), Agencia Estatal de Investigación (AEI), Fundação para a Ciência e a Tecnologia (FCT), National Research Development and Innovation Office, Hungarian (NKFIH), Agenzia Spaziale Italiana (ASI), European Space Agency (ESA), Fundacao para a Ciencia e a Tecnologia (FCT), Belgian Federal Science Policy Office (BELSPO), Istituto Nazionale di Astrofisica (INAF), University of St Andrews. School of Physics and Astronomy, University of St Andrews. St Andrews Centre for Exoplanet Science, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Space Sciences, Technologies and Astrophysics Research Institute (STAR), Université de Liège, Physikalisches Institut [Bern], Universität Bern [Bern], Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), European Research Council (ERC) under European Union, European Commission (EU), Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, European Space Agency, FEDER through COMPETE2020 Programa Operacional Competitividade e Internacionalizacao, Hungarian National Research, and Centre National D'etudes Spatiales
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics, atmospheres -planets and satellites, 01 natural sciences, 7. Clean energy, Occultation, Planet, Planets and satellites: atmospheres, QB Astronomy, photometric -planets and satellites, individual, 010303 astronomy & astrophysics, QC, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 16. Peace & justice, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, individual: WASP- 189 b [Planets and satellites], atmospheres [Planets and satellites], Astrophysics - Instrumentation and Methods for Astrophysics, Extrasolare Planeten und Atmosphären, Weltrauminstrumente, FOS: Physical sciences, WASP-189 b, Photometry (optics), 0103 physical sciences, Hot Jupiter, individual: WASP-189 b [Planets and satellites], Planets and satellites: individual: WASP-189 b, Techniques: photometric, Gravity darkening, planetary systems, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, abundance pattern, photometric [Techniques], Astronomy and Astrophysics, DAS, Light curve, Stars, QC Physics, Space and Planetary Science, exoplanet occultation, Planetare Sensorsysteme, techniques, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics, QB799
Abstract: Full author list: Lendl, M., Csizmadia, S., Deline, A., Fossati, L., Kitzmann, D., Heng, K., Hoyer, S., Salmon, S., Benz, W., Broeg, C., Ehrenreich, D., Fortier, A., Queloz, D., Bonfanti, A., Brandeker, A., Collier Cameron, A., Delrez, L.a,g,l, Garcia Muñoz, A.m, Hooton, M.J.f, Maxted, P.F.L.i, Morris, B.M., Van Grootel, V., Wilson, T.G., Alibert, Y., Alonso, R., Asquier, J., Bandy, T.f, Bárczy, T.q, Barrado, D.r, Barros, S.C.C.s,t, Baumjohann, W.b, Beck, M., Beck, T., Bekkelien, A., Bergomi, M., Billot, N., Biondi, F., Bonfils, X., Bourrier, V., Busch, M.-D., Cabrera, J., Cessa, V., Charnoz, S., Chazelas, B., Corral Van Damme, C., Davies, M.B., Deleuil, M., Demangeon, O.D.S., Demory, B.-O., Erikson, A., Farinato, J., Fridlund, M., Futyan, D., Gandolfi, D., Gillon, M.l, Guterman, P., Hasiba, J., Hernandez, E., Isaak, K., Kiss, L., Kuntzer, T., Lecavelier Des Etangs, A., Lüftinger, T., Laskar, J., Lovis, C., Magrin, D., Malvasio, L., Marafatto, L., Michaelis, H., Munari, M., Nascimbeni, V., Olofsson, G., Ottacher, H., Ottensamer, R., Pagano, I., Pallé, E., Peter, G., Piazza, D., Piotto, G., Pollacco, D., Ratti, F., Rauer, H., Ragazzoni, R., Rando, N., Ribas, I., Rieder, M., Rohlfs, R., Safa, F., Santos, N.C., Scandariato, G., Ségransan, D., Simon, A.E., Singh, V., Smith, A.M.S., Sordet, M., Sousa, S.G., Steller, M., Szabó, G.M., Thomas, N., Tschentscher, M., Udry, S., Viotto, V., Walter, I., Walton, N.A., Wildi, F., Wolter, D., The CHEOPS space mission dedicated to exoplanet follow-up was launched in December 2019, equipped with the capacity to perform photometric measurements at the 20 ppm level. As CHEOPS carries out its observations in a broad optical passband, it can provide insights into the reflected light from exoplanets and constrain the short-wavelength thermal emission for the hottest of planets by observing occultations and phase curves. Here, we report the first CHEOPS observation of an occultation, namely, that of the hot Jupiter WASP-189 b, a MP ≈ 2MJ planet orbiting an A-type star. We detected the occultation of WASP-189 b at high significance in individual measurements and derived an occultation depth of dF = 87.9 ± 4.3 ppm based on four occultations. We compared these measurements to model predictions and we find that they are consistent with an unreflective atmosphere heated to a temperature of 3435 ± 27 K, when assuming inefficient heat redistribution. Furthermore, we present two transits of WASP-189 b observed by CHEOPS. These transits have an asymmetric shape that we attribute to gravity darkening of the host star caused by its high rotation rate. We used these measurements to refine the planetary parameters, finding a ~25% deeper transit compared to the discovery paper and updating the radius of WASP-189 b to 1.619 ± 0.021RJ. We further measured the projected orbital obliquity to be λ = 86.4-4.4+2.9°, a value that is in good agreement with a previous measurement from spectroscopic observations, and derived a true obliquity of ψ = 85.4 ± 4.3°. Finally, we provide reference values for the photometric precision attained by the CHEOPS satellite: for the V = 6.6 mag star, and using a 1-h binning, we obtain a residual RMS between 10 and 17 ppm on the individual light curves, and 5.7 ppm when combining the four visits., with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The Swiss participation to CHEOPS has been supported by the Swiss Space Office (SSO) in the framework of the Prodex Programme and the Activités Nationales Complémentaires (ANC), the Universities of Bern and Geneva as well as well as of the NCCR PlanetS and the Swiss National Science Foundation. M.L.E. acknowledges support from the Austrian Research Promotion Agency (FFG) under project 859724 “GRAPPA”. Sz. Cs. thanks DFG Research Unit 2440: ‘Matter Under Planetary Interior Conditions: High Pressure, Planetary, and Plasma Physics’ for support. Sz. Cs. acknowledges support by DFG grants RA 714/14-1 within the DFG Schwerpunkt SPP 1992: “Exploring the Diversity of Extrasolar Planets”. A.D.E. and D.E.H. acknowledge support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES; grant agreement no. 724427). M.J.H. acknowledges the support of the Swiss National Fund under grant 200020_172746. The Spanish scientific participation in CHEOPS has been supported by the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, ESP2017-87676-C5-1-R, PGC2018-098153-B-C31, PGC2018-098153-B-C33, and MDM-2017-0737 Unidad de Excelencia María de Maeztu–Centro de Astrobiología (INTA-CSIC), as well as by the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. This work was supported by FCT – Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 – Programa Operacional Competitividade e Internacionalização by these grants: UID/FIS/04434/2019; UIDB/04434/2020; UIDP/04434/2020; PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113; PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953; PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987. S.C.C.B. and S.G.S. acknowledge support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004, IF/00028/2014/CP1215/CT0002. O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through Fundação para a Ciência e Tecnologia (FCT). The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Program, and by the University of Liege through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. M.G. is F.R.S.-FNRS Senior Research Associate. S.S. has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 833925, project STAREX). Gy.S. acknowledges funding from the Hungarian National Research, Development and Innovation Office (NKFIH) grant GINOP-2.3.2-15-2016-00003 and K-119517. For Italy, CHEOPS activities have been supported by the Italian Space Agency, under the programs: ASI-INAF n. 2013-016-R.0 and ASI-INAF n. 2019-29-HH.0. The team at LAM acknowledges CNES funding for the development of the CHEOPS DRP, including grants 124378 for O.D. and 837319 for S.H. X.B., S.C., D.G., M.F. and J.L. acknowledge their role as an ESA-appointed CHEOPS science team members.
Published: 2020
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9. Transiting exoplanets from the CoRoT space mission

Author: D. Rouan, Davide Gandolfi, Aldo S. Bonomo, François Bouchy, S. C. C. Barros, Eike W. Guenther, Anders Erikson, Heike Rauer, O. L. Creevey, M. Pätzold, M. Fridlund, Tsevi Mazeh, Suzanne Aigrain, Jean Schneider, Hans J. Deeg, Günther Wuchterl, A. Baglin, Peter Klagyivik, Sz. Csizmadia, Sascha Grziwa, M. Deleuil, Hannu Parviainen, A. P. Hatzes, Guillaume Hébrard, J. Cabrera, Marc Ollivier, Pascal Bordé, J. M. Almenara, Cilia Damiani, T. Guillot, Alexandre Santerne, Sylvio Ferraz-Mello, Roi Alonso, Rodrigo F. Díaz, 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), Istituto di Fisica dello Spazio Interplanetario (INAF), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Thüringer Landessternwarte Tautenburg (TLS), Department of Brain and Behavioural Sciences, Università degli Studi di Pavia = University of Pavia (UNIPV), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), 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), School of Physics, University of Exeter, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Universidade do Porto = University of Porto, DLR Institute of Planetary Research, German Aerospace Center (DLR), Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo = University of São Paulo (USP), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Tel Aviv] (TAU), Raymond and Beverly Sackler Faculty of Exact Sciences [Tel Aviv] (TAU), Tel Aviv University (TAU)-Tel Aviv University (TAU), 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), Institute for Geophysics and Meteorology [Köln] (IGM), University of Cologne, Laboratoire Univers et Théories (LUTH (UMR_8102)), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)
Subjects: Extrasolare Planeten und Atmosphären, Metallicity, Population, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, planetary systems / stars: fundamental parameters / stars: individual: CoRoT-30 / stars: individual: CoRoT-31, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, education, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Stars: fundamental parameters, Stars: individual: CoRoT-30, Stars: individual: CoRoT-31, [PHYS]Physics [physics], Physics, education.field_of_study, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Planetary system, Exoplanet, Radial velocity, Photometry (astronomy), Planetary systems, [SDU]Sciences of the Universe [physics], 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Planetary mass
Abstract: Aims. We report the discovery as well as the orbital and physical characterizations of two new transiting giant exoplanets, CoRoT-30 b and CoRoT-31 b, with the CoRoT space telescope. Methods. We analyzed two complementary data sets: photometric transit light curves measured by CoRoT, and radial velocity curves measured by the HARPS spectrometer. To derive the absolute masses and radii of the planets, we modeled the stars from available magnitudes and spectra. Results. We find that CoRoT-30 b is a warm Jupiter on a close-to-circular 9.06-day orbit around a G3V star with a semi-major axis of about 0.08 AU. It has a radius of 1.01 ± 0.08 RJ, a mass of 2.90 ± 0.22 MJ, and therefore a mean density of 3.45 ± 0.65 g cm−3. The hot Jupiter CoRoT-31 b is on a close-to-circular 4.63-day orbit around a G2 IV star with a semi-major axis of about 0.05 AU. It has a radius of 1.46 ± 0.30 RJ, a mass of 0.84 ± 0.34 MJ, and therefore a mean density of 0.33 ± 0.18 g cm−3. Conclusions. Neither system seems to support the claim that stars hosting planets are more depleted in lithium. The radii of both planets are close to that of Jupiter, but they differ in mass; CoRoT-30 b is ten times denser than CoRoT-31 b. The core of CoRoT-30 b would weigh between 15 and 75 Earth masses, whereas relatively weak constraints favor no core for CoRoT-31 b. In terms of evolution, the characteristics of CoRoT-31 b appear to be compatible with the high-eccentricity migration scenario, which is not the case for CoRoT-30 b. The angular momentum of CoRoT-31 b is currently too low for the planet to evolve toward synchronization of its orbital revolution with stellar rotation, and the planet will slowly spiral-in while its host star becomes a red giant. CoRoT-30 b is not synchronized either: it looses angular momentum owing to stellar winds and is expected reach steady state in about 2 Gyr. CoRoT-30 and 31, as a pair, are a truly remarkable example of diversity in systems with hot Jupiters.
Published: 2020
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10. HD219666b: A hot-Neptune from TESS Sector 1

Author: V. Van Eylen, J. N. Winn, Teriyuki Hirano, M. Esposito, D. L. Pollacco, Ignasi Ribas, J. de León, M. Tala-Pinto, David Nespral, H. J. Deeg, P. Figueira, S. Hojjatpanah, O. D. S. Demangeon, Grzegorz Nowak, M. Hjorth, John H. Livingston, Hugh P. Osborn, Farzana Meru, François Bouchy, William D. Cochran, Alexis M. S. Smith, S. C. C. Barros, Davide Gandolfi, Edward M. Bryant, Anders Erikson, N. C. Santos, Louise D. Nielsen, Michael Endl, Norio Narita, Vardan Adibekyan, Sascha Grziwa, K. W. F. Lam, D. Hidalgo, P. G. Beck, Duncan A. Brown, Peter J. Wheatley, Carina M. Persson, Mikkel N. Lund, Xavier Dumusque, Savita Mathur, A. P. Hatzes, Judith Korth, Anders Bo Justesen, Szilard Csizmadia, J. Prieto-Arranz, Fei Dai, J. Cabrera, Francesca Faedi, Rafael Luque, Emil Knudstrup, E. Delgado Mena, M. Pätzold, M. Fridlund, Oscar Barragán, Eike W. Guenther, J. Lillo-Box, Benjamin F. Cooke, Heike Rauer, Luca Fossati, Prajwal Niraula, S. Redfield, M. M. Musso, Patricio Cubillos, Roi Alonso, Rodrigo F. Díaz, Stéphane Udry, David Barrado, Enric Palle, A. S. Bonomo, P. Montanes Rodriguez, David J. Armstrong, Philipp Eigmüller, M. Deleuil, S. G. Sousa, D. Bayliss, A. Fukui, Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Dwarf star, 010504 meteorology & atmospheric sciences, fundamental parameters [Planets and satellites], FOS: Physical sciences, Astrophysics, Planets and satellites: individual: HD 219666 b, 01 natural sciences, fundamental parameters [Stars], Planet, 0103 physical sciences, Planets and satellites: detection, Planets and satellites: fundamental parameters, Stars: fundamental parameters, Techniques: photometric, Techniques: radial velocities, Hot Neptune, Spectroscopy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), radial velocities [Techniques], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], photometric [Techniques], Astronomy and Astrophysics, Radius, Light curve, Orbital period, Exoplanet, detection [Planets and satellites], Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], individual: HD 219666 b [Planets and satellites], Astrophysics - Earth and Planetary Astrophysics
Abstract: We report on the confirmation and mass determination of a transiting planet orbiting the old and inactive G7 dwarf star HD219666 (Mstar = 0.92 +/- 0.03 MSun, Rstar = 1.03 +/- 0.03 RSun, tau_star = 10 +/- 2 Gyr). With a mass of Mb = 16.6 +/- 1.3 MEarth, a radius of Rb = 4.71 +/- 0.17 REarth, and an orbital period of P ~ 6 days, HD219666b is a new member of a rare class of exoplanets: the hot-Neptunes. The Transiting Exoplanet Survey Satellite (TESS) observed HD219666 (also known as TOI-118) in its Sector 1 and the light curve shows four transit-like events, equally spaced in time. We confirmed the planetary nature of the candidate by gathering precise radial-velocity measurements with HARPS@ESO3.6m. We used the co-added HARPS spectrum to derive the host star fundamental parameters (Teff = 5527 +/- 65 K, log g = 4.40 +/- 0.11 (cgs), [Fe/H]= 0.04 +/- 0.04 dex, log R'HK = -5.07 +/- 0.03), as well as the abundances of many volatile and refractory elements. The host star brightness (V = 9.9) makes it suitable for further characterisation by means of in-transit spectroscopy. The determination of the planet orbital obliquity, along with the atmospheric metal-to-hydrogen content and thermal structure could provide us with important clues on the formation mechanisms of this class of objects., Comment: Accepted for publication in A&A
Published: 2019
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11. From thermal dissociation to condensation in the atmospheres of ultra hot Jupiters: WASP-121b in context

Author: M. Deleuil, Jean-Michel Desert, Jonathan J. Fortney, Jacob Arcangeli, Vivien Parmentier, Roxana Lupu, Michael R. Line, Laura Kreidberg, Megan Mansfield, Adam P. Showman, Channon Visscher, Jacob L. Bean, Mark S. Marley, 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), Department of Atmospheric, Oceanic and Planetary Physics [Oxford] (AOPP), University of Oxford [Oxford], University of Chicago, Harvard-Smithsonian Center for Astrophysics (CfA), Smithsonian Institution-Harvard University [Cambridge], Bay Area Environmental Research Institute (BAER), 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), University of California [Santa Cruz] (UCSC), University of California, 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), University of Oxford, Harvard University-Smithsonian Institution, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), University of California [Santa Cruz] (UC Santa Cruz), University of California (UC), and Low Energy Astrophysics (API, FNWI)
Subjects: 010504 meteorology & atmospheric sciences, Opacity, Gas giant, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, Planet, Ionization, 0103 physical sciences, Hot Jupiter, Emission spectrum, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, education.field_of_study, Astronomy and Astrophysics, Exoplanet, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: A new class of exoplanets has emerged: the ultra hot Jupiters, the hottest close-in gas giants. Most of them have weaker than expected spectral features in the $1.1-1.7\mu m$ bandpass probed by HST/WFC3 but stronger spectral features at longer wavelengths probed by Spitzer. This led previous authors to puzzling conclusions about the thermal structures and chemical abundances of these planets. Using the SPARC/MITgcm, we investigate how thermal dissociation, ionization, H$^-$ opacity and clouds shape the thermal structures and spectral properties of ultra hot Jupiters with a special focus on WASP-121b. We expand our findings to the whole population of ultra hot Jupiters through analytical quantification of the thermal dissociation and its influence on the strength of spectral features. We predict that most molecules are thermally dissociated and alkalies are ionized in the dayside photospheres of ultra hot Jupiters. This includes H$_{\rm 2}$O, TiO, VO, and H$_{\rm 2}$ but not CO, which has a stronger molecular bond. The vertical molecular gradient created by the dissociation significantly weakens the spectral features from water while the $4.5\mu m$ CO feature remain unchanged. The water band in the HST/WFC3 bandpass is further weakened by H$^-$ continuum opacity. Molecules are expected to recombine before reaching the limb, leading to order of magnitude variations of the chemical composition and cloud coverage between the limb and the dayside. Overall, molecular dissociation provides a qualitative understanding of the lack of strong spectral feature of water in the $1-2\mu m$ bandpass observed in most ultra hot Jupiters. Quantitatively, however, our model does not provide a satisfactory match to the WASP-121b emission spectrum. Together with WASP-33b and Kepler-33Ab, they seem the outliers among the population of ultra hot Jupiters in need of a more thorough understanding., Comment: Accepted in A&A
Published: 2018
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12. Extrasolar planets and brown dwarfs around AF-type stars. X.The SOPHIE northern sample. Combining the SOPHIE and HARPS surveys to compute the close giant planet mass-period distribution around AF-type stars

Author: R. da Silva, Nuno C. Santos, B. Loeillet, C. Lovis, D. Queloz, Damien Ségransan, A. Eggenberger, Guillaume Hébrard, François Bouchy, Anne-Marie Lagrange, G. Montagnier, J. P. Sivan, T. Forveille, J. L. Beuzit, K. Debondt, Isabelle Boisse, Rodrigo F. Díaz, Stéphane Udry, David Ehrenreich, Nicola Astudillo-Defru, C. Moutou, M. Deleuil, X. Bonfils, Luc Arnold, Francesco Pepe, Alfred Vidal-Madjar, Frederic Pont, F. Galland, N. Meunier, M. Desort, C. Perrier, X. Delfosse, Alexandre Santerne, S. Borgniet, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Universidad de Concepción [Chile], 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), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), Cavendish Laboratory, University of Cambridge [UK] (CAM), Universidade do Porto [Porto], Istituto Nazionale di Astrofisica (INAF), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Universidad de Concepción - University of Concepcion [Chile], Université de Genève = University of Geneva (UNIGE), Universidade do Porto = University of Porto, 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), and Universidade do Porto
Subjects: Stellar mass, Population, Brown dwarf, FOS: Physical sciences, Astrophysics, 01 natural sciences, 0103 physical sciences, education, 010303 astronomy & astrophysics, planetary systems, Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, 010308 nuclear & particles physics, Giant planet, Astronomy and Astrophysics, Planetary system, stars: early-type, Exoplanet, Radial velocity, stars: variables: general, Stars, 13. Climate action, Space and Planetary Science, echniques: radial velocities, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: The impact of the stellar mass on the giant planet properties is still to be fully understood. Main-Sequence (MS) stars more massive than the Sun remain relatively unexplored in radial velocity (RV) surveys, due to their characteristics that hinder classical RV measurements. Our aim is to characterize the close (up to 2.5 au) giant planet (GP) and brown dwarf (BD) population around AF MS stars and compare this population to stars with different masses. We used the SOPHIE spectrograph located on the 1.93m telescope at Observatoire de Haute-Provence to observe 125 northern, MS AF dwarfs. We used our dedicated SAFIR software to compute the RV and other spectroscopic observables. We characterized the detected sub-stellar companions and computed the GP and BD occurrence rates combining the present SOPHIE survey and a similar HARPS survey. We present new data on two known planetary systems around the F5-6V dwarfs HD16232 and HD113337. For the latter, we report an additional RV variation that might be induced by a second GP on a wider orbit. We also report the detection of fifteen binaries or massive sub-stellar companions with high-amplitude RV variations or long-term RV trends. Based on 225 targets observed with SOPHIE or HARPS, we constraint the BD frequency within 2-3 au around AF stars to be below 4 percents (1-sigma). For Jupiter-mass GP within 2-3 au (periods below 1000 days), we found the occurrence rate to be 3.7 (+3/-1) percents around AF stars with masses below 1.5 solar masses, and to be below 6 percents around AF stars with masses above 1.5 solar masses. For periods smaller than 10 days, we find the GP occurrence rate to be below 3 or 4.5 percents, respectively. Our results are compatible with the GP frequency reported around FGK dwarfs and are compatible with a possible increase of GP orbital periods with the stellar mass as predicted by formation models., Comment: 32 pages, 21 figures. Accepted to Astronomy & Astrophysics on August 30, 2018
Published: 2018
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13. Removing systematics from the CoRoT light curves: I. Magnitude-Dependent Zero Point

Author: T. Mazeh, P. Guterman, S. Aigrain, S. Zucker, N. Grinberg, A. Alapini, R. Alonso, M. Auvergne, M. Barbieri, P. Barge, P. Bordé, F. Bouchy, H. Deeg, R. De la Reza, M. Deleuil, R. Dvorak, A. Erikson, M. Fridlund, P. Gondoin, L. Jorda, H. Lammer, A. Léger, A. Llebaria, P. Magain, C. Moutou, M. Ollivier, M. Pätzold, F. Pont, D. Queloz, H. Rauer, D. Rouan, R. Sabo, J. Schneider, G. Wuchterl, Radcliffe Institute for Advanced Study, 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), University of Exeter, Tel Aviv University (TAU), 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), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), Instituto de Astrofisica de Canarias (IAC), Observatório Nacional/MCTI, Institut für Astronomie, Universität Wien (IfA), DLR Institut für Planetenerkundung, Research and Scientific Support Department, ESA-ESTEC (RSSD), Institut für Weltraumforschung, Österreichische Akademie der Wissenschaften (IWF), University of Liège, Rheinisches Institut für Umweltforschung an der Universität zu Köln (RIU), Observatoire Astronomique de l'Université de Genève, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Zentrum für Astronomie und Astrophysik, Technische Universität Berlin (TUB) (ZAA)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, photometry, Field (physics), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Zero-point energy, Astronomy and Astrophysics, Astrophysics, Function (mathematics), Light curve, Exoplanet, CoRoT, Apparent magnitude, exoplanets, transit method, Space and Planetary Science, Magnitude (astronomy), Outlier, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], systematic noise, Astrophysics - Earth and Planetary Astrophysics
Abstract: This paper presents an analysis that searched for systematic effects within the CoRoT exoplanet field light curves. The analysis identified a systematic effect that modified the zero point of most CoRoT exposures as a function of stellar magnitude. We could find this effect only after preparing a set of learning light curves that were relatively free of stellar and instrumental noise. Correcting for this effect, rejecting outliers that appear in almost every exposure, and applying SysRem, reduced the stellar RMS by about 20 %, without attenuating transit signals., Accepted for publication in Astronomy and Astrophysics
Published: 2016
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14. News of the CoRoT space mission and first results

Author: M. Deleuil, C. Moutou, and the CoRoT Exoplanet Science Team
Subjects: Physics, General Engineering, Astronomy, Astronomy and Astrophysics, Astrophysics, Parameter space, Space (mathematics), Orbital period, Exoplanet, Earth radius, Space and Planetary Science, Planet, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy)
Abstract: CoRoT is the first instrument aiming at detecting exoplanets from space, using the transit method. It has been built in order to explore the domain of planets with orbital period less than three months, and size down to about two Earth radii. Successfully launched on the 27th of December 2006, the instrument started its science observations by the beginning of February 2007. The first detections show the capability of the instrument to enlarge the parameter space and to explore the transition regime between gaseous giant and terrestrial planets. Five new transiting giant planets discovered by CoRoT are fully characterized at the time of writing.
Published: 2010
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15. Molecular hydrogen in the circumstellar disks of pre-main sequence stars

Author: C. Martin-Zaidi, Alfred Vidal-Madjar, Jean-Claude Bouret, P. D. Feldman, M. Deleuil, A. Lecavelier des Etangs, and Aki Roberge
Subjects: Physics, Hydrogen molecule, General Engineering, Astronomy, Astronomy and Astrophysics, Astrophysics, Circumstellar disk, Stars, Space and Planetary Science, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Emission spectrum, Astrophysics::Galaxy Astrophysics, Main sequence
Abstract: Circumstellar disks surrounding young forming stars, are likely the location where planets form. While the gaseous phase represents up to ~99% of the disk mass and control the dynamics, most of disk properties relies on dust analyses. The main constituent of the gaseous component, molecular hydrogen (H 2 ), remains nearly out of reach and the gas disk is probed through emission lines of minor tracers, such as CO. In this lecture, we will first recall how H 2 symmetric molecular structure makes its detection difficult. We will then review the most significant results achieved so far, thanks to new generation of ground and space-based telescopes, with a special emphasize given to Herbig Ae/be, which are pre-main sequence stars of intermediate mass. Though the first direct estimates of circumstellar disk mass have been reported, observation of H 2 is still challenging detection.
Published: 2010
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16. K2-19, The first K2 muti-planetary system showing TTVs

Author: M. Deleuil, K. W. F. Lam, P. Bendjoya, G. Hebrard, M. Tsantaki, D. Toublanc, Rodrigo F. Díaz, S. R. Walker, François Bouchy, O. D. S. Demangeon, A. S. Rajpurohit, S. C. C. Barros, D. L. Pollacco, L. Abe, J. Lillo-Box, A. Santerne, David Barrado, O. Suarez, Jessica Spake, J. C. Lachurié, Jason M. Kirk, J. McCormac, Hugh P. Osborn, Pascale Andre, A. S. Bonomo, B. Courcol, Isabelle Boisse, G. Bruno, J. Rey Cerda, P. Martinez, J. M. Almenara, Duncan A. Brown, David J. Armstrong, J. P. Rivet, and C. Moutou
Subjects: Radial velocity, Physics, Mean motion, Space and Planetary Science, Planet, Libration, Astronomy and Astrophysics, Transit (astronomy), Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Planetary system, Light curve, System dynamics
Abstract: In traditional transit timing variations (TTVs) analysis of multi-planetary systems, the individual TTVs are first derived from transit fitting and later modelled using n-body dynamic simulations to constrain planetary masses. We show that fitting simultaneously the transit light curves with the system dynamics (photo-dynamical model) increases the precision of the TTV measurements and helps constrain the system architecture. We exemplify the advantages of applying this photo-dynamical model to a multi-planetary system found in K2 data very close to 3:2 mean motion resonance, K2-19. In this case the period of the larger TTV variations (libration period) is much longer (>1.5 years) than the duration of the K2 observations (80 days). However, our method allows to detect the short period TTVs produced by the orbital conjunctions between the planets that in turn permits to uniquely characterise the system. Therefore, our method can be used to constrain the masses of near-resonant systems even when the full libration curve is not observed.
Published: 2016

17. III.5 Stellar classification in CoRoT faint stars fields

Author: J. C. Meunier, C. Moutou, CoRot Team, M. Deleuil, Frédéric Baudin, C. Damiani, 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), CoRot Team, and 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)
Subjects: Physics, Stars, Astronomy, [INFO]Computer Science [cs], Stellar classification, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], ComputingMilieux_MISCELLANEOUS
Abstract: International audience; no abstract
Published: 2016
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18. III.4 CoRoT planet host stars

Author: M. Fridlund, M. Deleuil, Giacomo Bruno, CoRoT team, Davide Gandolfi, CoRoT Cest Team, and Team Corot
Subjects: Physics, Stars, Planet, Astronomy, Host (network)
Published: 2016
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19. Detecting Earth-Uranus Class Planets with the Space Mission COROT

Author: A. Léger, C. Defaÿ, Pierre Barge, A. Baglin, M. Deleuil, D. Rouan, Pascal Bordé, J. Schneider, and A. Vuillemin
Subjects: Physics, Class (set theory), Planet, Uranus, Earth (chemistry), Astrophysics::Earth and Planetary Astrophysics, Space (mathematics), Astrobiology
Abstract: The space mission COROT can be considered as a DARWIN/TPF precursor, since it will contribute to the pre-DARWIN/TPF effort with its dedicated exoplanet program. COROT will survey more than 50 thousands stars, each one during five months, in order to detect transits of planets. Despite of the modest size of the telescope, the photon-noise limited performances may lead to the detection of several tens of “hot jupiters” and, more important, of a few planets of the Earth-Uranus class, i.e. with a size of typically 1.5 to 4 Earth radius. In the basic mode of operation (characterization of a planet by at least 3 detected transits), only planets with a short orbital period, and thus rather “hot” ones (T = 600K), should be discovered. However, one of the COROT's features is its capability to provide a wavelength dependent information, thanks to a prism in the optical path.
Published: 2004
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20. FUSE observations of H2 around the Herbig AeBe stars HD 100546 and HD 163296

Author: Alfred Vidal-Madjar, Roger Ferlet, F. Le Petit, Jean-Michel Desert, A. Roberge, Paul D. Feldman, Guillaume Hébrard, M. Deleuil, A. Lecavelier des Etangs, Jean-Claude Bouret, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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), Observatoire de Paris, and Université Paris sciences et lettres (PSL)
Subjects: Physics, stars: individual: HD 163296, Absorption spectroscopy, Astrophysics (astro-ph), Thin layer, FOS: Physical sciences, Astronomy and Astrophysics, stars: pre-main sequence, Astrophysics, circumstellar matter, Circumstellar disk, planetary systems: protoplanetary disks, Stars, [SDU]Sciences of the Universe [physics], Space and Planetary Science, stars: individual: HD 100546, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Absorption (electromagnetic radiation), Astrophysics::Galaxy Astrophysics
Abstract: We present the analysis of FUSE observations of two Herbig AeBe stars known to harbor young circumstellar disks: HD 100546 and HD 163296. In both cases we detect absorption lines from warm and dense H2. The thermalization of the rotational levels up to J~4 allows evaluation of the temperature, density and typical size of the absorbing layer. These quantities are consistent with absorption of the light of the central star by a thin layer of a circumstellar disk seen at an intermediate inclination., Comment: 5 pages, 4 figures, to be published in A&A
Published: 2003
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21. Far Ultraviolet Spectroscopic ExplorerObservations of Possible Infalling Planetesimals in the 51 Ophiuchi Circumstellar Disk

Author: Alfred Vidal-Madjar, A. Roberge, H. W. Moos, Roger Ferlet, Paul D. Feldman, A. Lecavelier des Etangs, J. C. Bouret, M. Deleuil, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Physics, Planetesimal, Absorption spectroscopy, Stars: Individual: Constellation Name: 51 Ophiuchi, Comets: General, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Redshift, chemistry.chemical_compound, Stars: Circumstellar Matter, chemistry, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Stars: Planetary Systems: Formation, Ionization, Astrophysics::Solar and Stellar Astrophysics, Beta Pictoris, Astrophysics::Earth and Planetary Astrophysics, Absorption (chemistry), Astrophysics::Galaxy Astrophysics, Carbon monoxide
Abstract: International audience; We present the first observations of the circumstellar (CS) disk system 51 Ophiuchi with the Far Ultraviolet Spectroscopic Explorer (FUSE). We detect several absorption lines arising from the unusual metastable atomic species N I (2D), N I (2P), and S II (2D). These levels lie 1.8-3.6 eV above the ground level and have radiative decay lifetimes of 2 days or less, indicating that the lines arise from warm CS gas. The high S/N FUSE spectra, obtained 6 days apart, also show time-variable absorption features arising from N I, N II, O I (1D), and Fe III, which are redshifted with respect to the stellar velocity. The resolved redshifted absorption extends over many tens of km s-1 (40 for N I, 100 for N II, 65 for O I (1D), and 84 for Fe III). We calculate column densities for all the variable infalling CS gasses, using the apparent optical depth method. The Fe III and N II infalling gasses must be produced through collisional ionization, and the ionization fraction of nitrogen suggests a gas temperature between 20,000 and 34,000 K. The infalling gas shows a peculiar, nonsolar composition, with nitrogen and iron more abundant than carbon. We also set upper limits on the line-of-sight column densities of H2 and CO. These observations strengthen the connection between 51 Oph and the older debris-disk system β Pictoris and indicate that there may be infalling planetesimals in the 51 Oph system.
Published: 2002
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22. [ITAL]FUSE[/ITAL] and [ITAL]Hubble Space Telescope[/ITAL]/STIS Observations of Hot and Cold Gas in the AB Aurigae System

Author: Bruce E. Woodgate, Roger Ferlet, J. C. Bouret, Paul D. Feldman, A. Boggess, M. Andre, Alfred Vidal-Madjar, A. Roberge, Carol A. Grady, Frederick C. Bruhweiler, M. Deleuil, and A. Lecavelier des Etangs
Subjects: Physics, Range (particle radiation), Mean kinetic temperature, Hydrogen, chemistry.chemical_element, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Spectral line, Redshift, chemistry, Space and Planetary Science, Ionization, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Absorption (electromagnetic radiation), Astrophysics::Galaxy Astrophysics, Space Telescope Imaging Spectrograph
Abstract: We present the first observations of a Herbig Ae star with a circumstellar disk by the Far Ultraviolet Spectroscopic Explorer (FUSE), as well as a simultaneous observation of the star obtained with the Hubble Space Telescope Space Telescope Imaging Spectrograph (STIS). The spectra of AB Aurigae show emission and absorption features arising from gasses that have a wide range in temperature, from hot OVI emission to cold molecular hydrogen and CO absorption. Emissions from the highly ionized species OVI and CIII present in the FUSE spectrum are redshifted, while absorption features arising from low-ionization species like OI, NI, and SiII are blueshifted and show characteristic stellar wind line-profiles. We find the total column density of molecular hydrogen toward AB Aur from the FUSE apectrum, N(H_2) = (6.8 +/- 0.5) x 10^19 cm^-2. The gas kinetic temperature of the molecular hydrogen derived from the ratio N(J=1)/N(J=0) is 65 +/- 4 K. The column density of the CO observed in the STIS spectrum is N(CO) = (7.1 +/- 0.5) x 10^13 cm^-2, giving a CO/H_2 ratio of (1.04 +/- 0.11) x 10^-6. We also use the STIS spectrum to find the column density of HI, permitting us to calculate the total column density of hydrogen atoms, the fractional abundance of H_2, and the gas-to-dust ratio.
Published: 2001
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23. Three irradiated and bloated hot Jupiters: WASP-76b, WASP-82b & WASP-90b

Author: R. G. West, C. Hellier, J.-M. Almenara, D. R. Anderson, S. C. C. Barros, F. Bouchy, D. J. A. Brown, A. Collier Cameron, M. Deleuil, L. Delrez, A. P. Doyle, F. Faedi, A. Fumel, M. Gillon, Y. Gómez Maqueo Chew, G. Hébrard, E. Jehin, M. Lendl, P. F. L. Maxted, F. Pepe, D. Pollacco, D. Queloz, D. Ségransan, B. Smalley, A. M. S. Smith, J. Southworth, A. H. M. J. Triaud, S. Udry, Instituto de Astrofisica de Canarias (IAC), Virologia, Laboratorio Nacional de Investigacao Veterinaria (LNIV), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), 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), University of St Andrews [Scotland], 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), Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Science & Technology Facilities Council, and University of St Andrews. School of Physics and Astronomy
Subjects: NDAS, individual: WASP-76 [Stars], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Photometry (optics), Planet, 0103 physical sciences, Hot Jupiter, QB Astronomy, Astrophysics::Solar and Stellar Astrophysics, individual: WASP-90 [Stars], Irradiation, 010303 astronomy & astrophysics, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, Planetary systems, Stars, QC Physics, 13. Climate action, Space and Planetary Science, TRAPPIST, Astrophysics::Earth and Planetary Astrophysics, individual: WASP-82 [Stars], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: International audience; We report on three new transiting hot Jupiter planets, discovered from the WASP surveys, which we combine with radial velocities from OHP/ SOPHIE and Euler/CORALIE and photometry from Euler and TRAPPIST. The planets WASP-76b, WASP-82b, and WASP-90b are all inflated, with radii of 1.7-1.8 R-Jup. All three orbit hot stars, of type F5-F7, with orbits of 1.8-3.9 d, and all three stars have evolved, post-main-sequence radii (1.7-2.2 R-circle dot). Thus the three planets fit a known trend of hot Jupiters that receive high levels of irradiation being highly inflated. We caution, though, about the presence of a selection effect, in that non-inflated planets around similar to 2 R-circle dot post-MS stars can often produce transits too shallow to be detected by the ground-based surveys that have found the majority of transiting hot Jupiters.
Published: 2013
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24. CoRoT 101186644: A transiting low-mass dense M-dwarf on an eccentric 20.7-day period orbit around a late F-star Discovered in the CoRoT lightcurves

Author: M. Fridlund, M. Deleuil, François Bouchy, Roi Alonso, G. Hebrard, Hans J. Deeg, Tsevi Mazeh, J. Cabrera, C. Moutou, Simchon Faigler, Lev Tal-Or, Brandon Tingley, A. Santerne, Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Physics, Period (periodic table), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astronomy and Astrophysics, Radius, Astrophysics, Star (graph theory), 01 natural sciences, Planetary systems - Stars: individual: CoRoT 101186644 - binaries: eclipsing - Techniques: photometric - Techniques: radial velocities, Stars, Orbit, Space and Planetary Science, Primary (astronomy), Planet, 0103 physical sciences, Low Mass, 010303 astronomy & astrophysics
Abstract: We present the study of the CoRoT transiting planet candidate 101186644, also named LRc01_E1_4780. Analysis of the CoRoT lightcurve and the HARPS spectroscopic follow-up observations of this faint (m$_V$ = 16) candidate revealed an eclipsing binary composed of a late F-type primary (T$_{eff}$ = 6090 {plusmn} 200 K) and a low-mass, dense late M-dwarf secondary on an eccentric (e = 0.4) orbit with a period of ~{}20.7 days. The M-dwarf has a mass of 0.096 {plusmn} 0.011 M$_{⊙}$, and a radius of 0.104$_{-0.006}$$^{+0.026}$ R$_{⊙}$, which possibly makes it the smallest and densest late M-dwarf reported so far. Unlike the claim that theoretical models predict radii that are 5-15% smaller than measured for low-mass stars, this one seems to have a radius that is consistent and might even be below the radius predicted by theoretical models. Based on observations made with the 1-m telescope at the Wise Observatory, Israel, the Swiss 1.2-m Leonhard Euler telescope at La Silla Observatory, Chile, the IAC-80 telescope at the Observatory del Teide, Canarias, Spain, and the 3.6-m telescope at La Silla Observatory (ESO), Chile (program 184.C-0639).
Published: 2013
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25. SOPHIE velocimetry of Kepler transit candidates: X KOI-142c: first radial velocity confirmation of a non-transiting exoplanet discovered by transit timing

Author: A. S. Bonomo, G. Montagnier, François Bouchy, G. Bruno, Rodrigo F. Díaz, J. M. Almenara, C. Moutou, A. Santerne, Cilia Damiani, M. Deleuil, G. Hebrard, and S. C. C. Barros
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Velocimetry, Orbital period, 01 natural sciences, Exoplanet, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Transit (astronomy), Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Planetary mass, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics
Abstract: The exoplanet KOI-142b (Kepler-88b) shows transit timing variations (TTVs) with a semi-amplitude of $\sim 12\,$ hours, earning the nickname of "king of transit variations". Only the transit of the planet b was detected in the Kepler data with an orbital period of $\sim 10.92\,$ days and a radius of $\sim 0.36$ R$_{\mathrm{Jup}}$. The TTVs together with the transit duration variations (TDVs) of KOI-142b were analysed by Nesvorny et al. (2013) who found a unique solution for a companion perturbing planet. The authors predicted an outer non-transiting companion, KOI-142c, with a mass of $0.626\pm 0.03$ M$_{\mathrm{Jup}}$ and a period of $22.3397^{+0.0021}_{-0.0018}\,$days, and hence close to the 2:1 mean-motion resonance with the inner transiting planet. We report independent confirmation of KOI-142c using radial velocity observations with the SOPHIE spectrograph at the Observatoire de Haute-Provence. We derive an orbital period of $22.10 \pm 0.25\,$days and a minimum planetary mass of $0.76^{+0.32}_{0.16}\,$ M$_{\mathrm{Jup}}$, both in good agreement with the predictions by previous transit timing analysis. Therefore, this is the first radial velocity confirmation of a non-transiting planet discovered with transit timing variations, providing an independent validation of the TTVs technique., Comment: 4 pages, 3 figures, A&A Accepted
Published: 2013
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26. K2-29 b/WASP-152 b: AN ALIGNED AND INFLATED HOT JUPITER IN A YOUNG VISUAL BINARY

Author: A. Santerne, G. Hébrard, J. Lillo-Box, D. J. Armstrong, S. C. C. Barros, O. Demangeon, D. Barrado, A. Debackere, M. Deleuil, E. Delgado Mena, M. Montalto, D. Pollacco, H. P. Osborn, S. G. Sousa, L. Abe, V. Adibekyan, J.-M. Almenara, P. André, G. Arlic, G. Barthe, P. Bendjoya, R. Behrend, I. Boisse, F. Bouchy, H. Boussier, M. Bretton, D. J. A. Brown, B. Carry, A. Cailleau, E. Conseil, G. Coulon, B. Courcol, B. Dauchet, J.-C. Dalouzy, M. Deldem, O. Desormières, P. Dubreuil, J.-M. Fehrenbach, S. Ferratfiat, R. Girelli, J. Gregorio, S. Jaecques, F. Kugel, J. Kirk, O. Labrevoir, J.-C. Lachurié, K. W. F. Lam, P. Le Guen, P. Martinez, L. P. A. Maurin, J. McCormac, J-B. Pioppa, U. Quadri, A. Rajpurohit, J. Rey, J.-P. Rivet, R. Roy, N. C. Santos, F. Signoret, L. Strabla, O. Suarez, D. Toublanc, M. Tsantaki, J.-M. Vienney, P. A. Wilson, M. Bachschmidt, F. Colas, O. Gerteis, P. Louis, J.-C. Mario, C. Marlot, J. Montier, V. Perroud, V. Pic, D. Romeuf, S. Ubaud, D. Verilhac, Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, 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), Virologia, Laboratorio Nacional de Investigacao Veterinaria (LNIV), Université Paris-Sud - Paris 11 (UP11), 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), 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, 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), 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), Instituto de Astrofisica de Canarias (IAC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Geneva Observatory, University of Geneva [Switzerland], CdR & CdL group, Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), 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 de Lille-Centre National de la Recherche Scientifique (CNRS), Observatoire Chante-Perdrix, School of Physics and Astronomy [Cardiff], Cardiff University, Hôpital Européen Georges Pompidou [APHP] (HEGP), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Hôpitaux Universitaires Paris Ouest - Hôpitaux Universitaires Île de France Ouest (HUPO), UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux (EPOC), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-École pratique des hautes études (EPHE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Département RadioChimie et Procédés (DRCP), CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Laval [Québec] (ULaval), 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, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), 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), Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables (CdR & CdL group), Universidade do Porto [Porto], Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), 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), 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), Université Côte d'Azur (UCA), 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), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy, Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-Hôpitaux Universitaires Paris Ouest - Hôpitaux Universitaires Île de France Ouest (HUPO), 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)-École pratique des hautes études (EPHE)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Université Laval, Departamento de Física e Astronomia [Porto], Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), 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), Centro de Astrofísica da Universidade do Porto ( CAUP ), 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 ), Université Paris-Sud - Paris 11 ( UP11 ), 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 ), LAEX, Depto. Astrofísica, Centro de Astrobiología, Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), 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 ), Instituto de Astrofisica de Canarias ( IAC ), Astrophysique Interactions Multi-échelles ( AIM - UMR 7158 - UMR E 9005 ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Paris Diderot - Paris 7 ( UPD7 ), Université Côte d'Azur ( UCA ), Observatoire de Haute-Provence ( OHP ), Institut Pythéas ( OSU PYTHEAS ), 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 ) -Aix Marseille Université ( AMU ) -Centre National de la Recherche Scientifique ( CNRS ), Institut de Mécanique Céleste et de Calcul des Ephémérides ( IMCCE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Lille-Centre National de la Recherche Scientifique ( CNRS ), School of Physis & Astronomy, Hôpital Européen Georges Pompidou [APHP] ( HEGP ), UMR 5805 Environnements et Paléoenvironnements Océaniques et Continentaux ( EPOC ), Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -École pratique des hautes études ( EPHE ) -Centre National de la Recherche Scientifique ( CNRS ), Département RadioChimie et Procédés ( DRCP ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Centre d'étude spatiale des rayonnements ( CESR ), Université Toulouse III - Paul Sabatier ( UPS ), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire Midi-Pyrénées ( OMP ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'études spatiales et d'instrumentation en astrophysique ( LESIA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Courbes de rotation d'astéroïdes, de comètes et d'étoiles variables ( CdR & CdL group ), 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université de Genève = University of Geneva (UNIGE), Environnements et Paléoenvironnements OCéaniques (EPOC), 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)-École Pratique des Hautes Études (EPHE), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Universidade do Porto, Centre National de la Recherche Scientifique (CNRS)-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, 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-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), Universidade do Porto-Universidade do Porto, Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées
Subjects: Physics, 010308 nuclear & particles physics, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Stellar rotation, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, 01 natural sciences, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, Magnitude (astronomy), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Visual binary
Abstract: International audience; In the present paper we report the discovery of a new hot Jupiter, K2-29 b, first detected by the Super-WASP observatory and then by the K2 space mission during its campaign 4. The planet has a period of 3.25 days, a mass of 0.73 +/- 0.04M(sic), and a radius of 1.19 +/- 0.02 R(sic). The host star is a relatively bright (V = 12.5) G7 dwarf with a nearby K5V companion. Based on stellar rotation and the abundance of lithium, we find that the system might be as young as similar to 450 Myr. The observation of the Rossiter-McLaughlin effect shows that the planet is aligned with respect to the stellar spin. Given the deep transit (20 mmag), the magnitude of the star and the presence of a nearby stellar companion, the planet is a good target for both space- and ground-based transmission spectroscopy, in particular in the near-infrared where both stars are relatively bright.
Published: 2016
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27. SOPHIE velocimetry of Kepler transit candidates VII. A false-positive rate of 35% for Kepler close-in giant candidates

Author: M. Deleuil, G. Hebrard, A. Santerne, J. M. Almenara, François Bouchy, N. C. Santos, C. Moutou, Rodrigo F. Díaz, A. S. Bonomo, 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), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Centre National de la Recherche Scientifique (CNRS), 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), Instituto de Astrofisica de Canarias (IAC), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, 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), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universidade do Porto, and Universidade do Porto [Porto]
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010504 meteorology & atmospheric sciences, Stellar population, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Brown dwarf, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Orbital period, 01 natural sciences, Exoplanet, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, Transit (astronomy), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics, 0105 earth and related environmental sciences
Abstract: The false-positive probability (FPP) of Kepler transiting candidates is a key value for statistical studies of candidate properties. A previous investigation of the stellar population in the Kepler field has provided an estimate for the FPP of less than 5% for most of the candidates. We report here the results of our radial velocity observations on a sample of 46 Kepler candidates with a transit depth greater than 0.4%, orbital period less than 25 days and host star brighter than Kepler magnitude 14.7. We used the SOPHIE spectrograph mounted on the 1.93-m telescope at the Observatoire de Haute-Provence to establish the nature of the transiting candidates. In this sample, we found five undiluted eclipsing binaries, two brown dwarfs, six diluted eclipsing binaries, and nine new transiting planets that complement the 11 already published planets. The remaining 13 candidates were not followed-up or remain unsolved due to photon noise limitation or lack of observations. From these results we computed the FPP for Kepler close-in giant candidates to be 34.8% \pm 6.5%. We aimed to investigate the variation of the FPP for giant candidates with the longer orbital periods and found that it should be constant for orbital periods between 10 and 200 days. This significant disagrees with the previous estimates. We discuss the reasons for this discrepancy and the possible extension of this work toward smaller planet candidates. Finally, taking the false-positive rate into account, we refined the occurrence rate of hot jupiters from the Kepler data., Accepted in A&A. 16 pages including 4 online material pages. 6 figures and 1 table
Published: 2012
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28. Transiting exoplanets from the CoRoT space mission.XX.CoRoT-20b: A very high density, high eccentricity transiting giant planet

Author: Davide Gandolfi, A. Santerne, M. Fridlund, Eike W. Guenther, Tsevi Mazeh, François Bouchy, M. Havel, C. Cavarroc, Hannu Parviainen, M. Deleuil, H. Bruntt, Stefania Carpano, G. Hebrard, Laurent Jorda, J. M. Almenara, A. Baglin, Adrián Rodríguez, H. J. Deeg, Rudolf Dvorak, J. Weingrill, Sylvio Ferraz-Mello, Suzanne Aigrain, A. P. Hatzes, Roi Alonso, A. Léger, Tristan Guillot, Pascal Bordé, J. Cabrera, Jean Schneider, Pierre Barge, Brandon Tingley, Günther Wuchterl, A. S. Bonomo, C. Moutou, M. Gillon, M. Auvergne, D. Rouan, D. Queloz, Helmut Lammer, Heike Rauer, Marc Ollivier, Anders Erikson, Lev Tal-Or, Sz. Csizmadia, Aviv Ofir, Cilia Damiani, 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, and 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)
Subjects: Orbital plane, 010504 meteorology & atmospheric sciences, media_common.quotation_subject, Angular velocity, Astrophysics, stars: planetary systems - stars: fundamental parameters - techniques: photometry - techniques: radial velocities - techniques: spectroscopy, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Eccentricity (behavior), Spin (physics), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, media_common, Physics, [PHYS]Physics [physics], Giant planet, Astronomy and Astrophysics, Radius, Orbital period, ESPECTROSCOPIA, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
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: 2012
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29. Transiting exoplanets from the CoRoT space mission. XVI. CoRoT-14b: an unusually dense very hot Jupiter

Author: Eike W. Guenther, Tsevi Mazeh, Günther Wuchterl, Michael Endl, François Bouchy, Laurent Jorda, Davide Gandolfi, Sz. Csizmadia, J. M. Almenara, A. P. Hatzes, J. Cabrera, M. Auvergne, Aviv Ofir, Heike Rauer, Brandon Tingley, Sylvio Ferraz-Mello, L. Carone, Anders Erikson, Roi Alonso, M. Pätzold, M. Fridlund, D. Rouan, C. Lovis, A. S. Bonomo, B. Samuel, A. Llebaria, H. J. Deeg, T. Guillot, M. Gillon, A. Léger, Phillip J. MacQueen, A. Shporer, Jean Schneider, Stefania Carpano, A. Baglin, Rudolf Dvorak, Pierre Barge, William D. Cochran, C. Moutou, Pascal Bordé, H. Bruntt, Francesco Pepe, Marc Ollivier, M. Deleuil, Suzanne Aigrain, G. Hebrard, D. Queloz, Helmut Lammer, J. C. Gazzano, 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, and 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)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Physics, COROT, Hot Jupiters, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Space (mathematics), 01 natural sciences, Exoplanet, Jupiter, Orbit, Space and Planetary Science, Planet, extrasolar planets, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Earth and Planetary Astrophysics
Abstract: In this paper, the CoRoT Exoplanet Science Team announces its 14th discovery. Herein, we discuss the observations and analyses that allowed us to derive the parameters of this system: a hot Jupiter with a mass of $7.6 \pm 0.6$ Jupiter masses orbiting a solar-type star (F9V) with a period of only 1.5 d, less than 5 stellar radii from its parent star. It is unusual for such a massive planet to have such a small orbit: only one other known exoplanet with a higher mass orbits with a shorter period., 7 pages, 10 figures, accepted to Astronomy and Astrophysics
Published: 2011
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30. Transiting exoplanets from the CoRoT space mission. X. CoRoT-10b: a giant planet in a 13.24 day eccentric orbit

Author: Pierre Barge, M. Pätzold, Marc Ollivier, M. Fridlund, A. P. Hatzes, François Bouchy, C. Moutou, J. Cabrera, Davide Gandolfi, A. F. Lanza, Willy Benz, A. S. Bonomo, Laurent Jorda, Pascal Bordé, D. Rouan, Sz. Csizmadia, Günther Wuchterl, M. Gillon, H. J. Deeg, A. Santerne, Sylvio Ferraz-Mello, Eike W. Guenther, Brandon Tingley, Roi Alonso, Tsevi Mazeh, Stéphane Udry, Stefania Carpano, A. Baglin, M. Havel, H. Bruntt, Rudolf Dvorak, Francesco Pepe, B. Samuel, M. Mayor, Jean Schneider, J. C. Gazzano, Antoine Llebaria, Anders Erikson, Suzanne Aigrain, A. Léger, Tristan Guillot, Andrew Collier Cameron, L. Carone, Heike Rauer, D. Queloz, Helmut Lammer, M. Auvergne, M. Deleuil, G. Hebrard, M. Barbieri, 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, and 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)
Subjects: 010504 meteorology & atmospheric sciences, Extrasolare Planeten, Orbital eccentricity, Photometrie, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Photometry (optics), Spitzer Space Telescope, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, Giant planet, Astronomy, Astronomy and Astrophysics, Radialgeschwindigkeit, Exoplanet, Radial velocity, Stars, 13. Climate action, Space and Planetary Science, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics
Abstract: The space telescope CoRoT searches for transiting extrasolar planets by continuously monitoring the optical flux of thousands of stars in several fields of view. We report the discovery of CoRoT-10b, a giant planet on a highly eccentric orbit (e=0.53 +/- 0.04) revolving in 13.24 days around a faint (V=15.22) metal-rich K1V star. We use CoRoT photometry, radial velocity observations taken with the HARPS spectrograph, and UVES spectra of the parent star to derive the orbital, stellar and planetary parameters. We derive a radius of the planet of 0.97 +/- 0.07 R_Jup and a mass of 2.75 +/- 0.16 M_Jup. The bulk density, rho_pl=3.70 +/- 0.83 g/cm^3, is ~2.8 that of Jupiter. The core of CoRoT-10b could contain up to 240 M_Earth of heavy elements. Moving along its eccentric orbit, the planet experiences a 10.6-fold variation in insolation. Owing to the long circularisation time, tau_circ > 7 Gyr, a resonant perturber is not required to excite and maintain the high eccentricity of CoRoT-10b.
Published: 2010
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31. The thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 microns

Author: H. J. Deeg, Jean Schneider, D. Queloz, François Bouchy, B. O. Demory, J. Harrington, J. J. Fortney, M. Gillon, D. Rouan, C. Moutou, Travis Barman, Pierre Magain, M. Fridlund, Neil Miller, Heike Rauer, Josefina Montalbán, A. A. Lanotte, M. Deleuil, A. Collier Cameron, Institut d'Astrophysique, Géophysique et Océanographie, Université de Liège, Lowell Observatory, Flagstaff, Department of Astronomy and Astrophysics, University of California, Observatoire Astronomique de l'Université de Genève, 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), Observatoire de Haute-Provence (OHP), Institut Pythéas (OSU PYTHEAS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE), School of Physics and Astronomy, University of St Andrews, Instituto de Astrofísica de Canarias (IAC), Research and Scientific Support Department, ESA-ESTEC (RSSD), Planetary Sciences Group, Department of Physics, University of Central Florida, Orlando, Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt (DLR), 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), Laboratoire Univers et Théories (LUTH (UMR_8102)), and Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: Orbital elements, Physics, Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astronomy and Astrophysics, Orbital eccentricity, Tidal heating, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Occultation, Omega, Space and Planetary Science, Planet, Roche limit, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Tidal circularization, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], binaries: eclipsing - planetary systems - stars: individual: CoRoT-2 - techniques: photometric, Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report measurements of the thermal emission of the young and massive planet CoRoT-2b at 4.5 and 8 microns with the Spitzer Infrared Array Camera (IRAC). Our measured occultation depths are 0.510 +- 0.042 % and 0.41 +- 0.11 % at 4.5 and 8 microns, respectively. In addition to the CoRoT optical measurements, these planet/star flux ratios indicate a poor heat distribution to the night side of the planet and are in better agreement with an atmosphere free of temperature inversion layer. Still, the presence of such an inversion is not definitely ruled out by the observations and a larger wavelength coverage is required to remove the current ambiguity. Our global analysis of CoRoT, Spitzer and ground-based data confirms the large mass and size of the planet with slightly revised values (Mp = 3.47 +- 0.22 Mjup, Rp = 1.466 +- 0.044 Rjup). We find a small but significant offset in the timing of the occultation when compared to a purely circular orbital solution, leading to e cos(omega) = -0.00291 +- 0.00063 where e is the orbital eccentricity and omega is the argument of periastron. Constraining the age of the system to be at most of a few hundreds of Myr and assuming that the non-zero orbital eccentricity is not due to a third undetected body, we model the coupled orbital-tidal evolution of the system with various tidal Q values, core sizes and initial orbital parameters. For log(Q_s') = 5 - 6, our modelling is able to explain the large radius of CoRoT-2b if log(Q_p'), 13 pages, 2 tables, 11 figures. Accepted for publication in Astronomy and Astrophysics
Published: 2009
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32. Photospheric activity and rotation of the planet-hosting star CoRoT-4a

Author: Pierre Barge, M. Deleuil, C. Moutou, G. Leto, Suzanne Aigrain, Giuseppe Cutispoto, A. F. Lanza, A. Collier Cameron, J. R. De Medeiros, S. Messina, A. Baglin, I. Pagano, M. Auvergne, A. S. Bonomo, Bernard Foing, INAF-Osservatorio Astrofisico di Catania (INAF-OACt), University of Exeter, 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), 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), School of Physics and Astronomy, University of St Andrews, Departamento de Física, Universidade Federal do Rio Grande do Norte, and ESA-ESTEC
Subjects: magnetic fields [Stars], FOS: Physical sciences, Astrophysics, Planet, Hot Jupiter, Differential rotation, Astrophysics::Solar and Stellar Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Earth and Planetary Astrophysics (astro-ph.EP), Physics, Sunspot, Stellar rotation, Astronomy and Astrophysics, Planetary system, Light curve, Orbital period, rotation [Stars], Planetary systems, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, late-type [Stars], Astrophysics::Earth and Planetary Astrophysics, individual: CoRoT-4a [Stars], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], activity [Stars], Astrophysics - Earth and Planetary Astrophysics
Abstract: The space experiment CoRoT has recently detected a transiting hot Jupiter in orbit around a moderately active F-type main-sequence star (CoRoT-Exo-4a). This planetary system is of particular interest because it has an orbital period of 9.202 days, the second longest one among the transiting planets known to date. We study the surface rotation and the activity of the host star during an uninterrupted sequence of optical observations of 58 days. Our approach is based on a maximum entropy spot modelling technique extensively tested by modelling the variation of the total solar irradiance. It assumes that stellar active regions consist of cool spots and bright faculae, analogous to sunspots and solar photospheric faculae, whose visibility is modulated by stellar rotation. The modelling of the light curve of CoRoT-Exo-4a reveals three main active longitudes with lifetimes between about 30 and 60 days that rotate quasi-synchronously with the orbital motion of the planet. The different rotation rates of the active longitudes are interpreted in terms of surface differential rotation and a lower limit of 0.057 \pm 0.015 is derived for its relative amplitude. The enhancement of activity observed close to the subplanetary longitude suggests a magnetic star-planet interaction, although the short duration of the time series prevents us from drawing definite conclusions., 8 pages, 6 figures, accepted by Astronomy & Astrophysics
Published: 2009
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33. Transiting exoplanets from the CoRoT space mission VI. CoRoT-Exo-3b: the first secure inhabitant of the brown-dwarf desert

Author: M. Deleuil, H. J. Deeg, R. Alonso, F. Bouchy, D. Rouan, M. Auvergne, A. Baglin, S. Aigrain, J. M. Almenara, M. Barbieri, P. Barge, H. Bruntt, P. Bordé, A. Collier Cameron, Sz. Csizmadia, R. De la Reza, R. Dvorak, A. Erikson, M. Fridlund, D. Gandolfi, M. Gillon, E. Guenther, T. Guillot, A. Hatzes, G. Hébrard, L. Jorda, H. Lammer, A. Léger, A. Llebaria, B. Loeillet, M. Mayor, T. Mazeh, C. Moutou, M. Ollivier, M. Pätzold, F. Pont, D. Queloz, H. Rauer, J. Schneider, A. Shporer, G. Wuchterl, S. Zucker, 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), 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 de Astrofísica de Canarias (IAC), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), 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, 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, School of Physics, University of Exeter, School of physics, University of New South Wales, Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy, University of St Andrews, Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Observatório Nacional/MCTI, Institut für Astronomie, Universität Wien (IfA), Research and Scientific Support Department, ESA-ESTEC (RSSD), Thüringer Landessternwarte, Tautenburg Observatory, Observatoire Astronomique de l'Université de Genève, Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut für Weltraumforschung, Österreichische Akademie der Wissenschaften (IWF), School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Rheinisches Institut für Umweltforschung an der Universität zu Köln (RIU), Laboratoire Univers et Théories (LUTH (UMR_8102)), and Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: photometry, Population, Brown dwarf, FOS: Physical sciences, Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Substellar object, education, 010303 astronomy & astrophysics, brown dwarf, Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Surface gravity, Light curve, Orbital period, Exoplanet, CoRoT, exoplanets, transit method, [SDU]Sciences of the Universe [physics], Space and Planetary Science, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Context. The CoRoT space mission routinely provides high-precision photometric measurements of thousands of stars that have been continuously observed for months. Aims. The discovery and characterization of the first very massive transiting planetary companion with a short orbital period is reported. Methods. A series of 34 transits was detected in the CoRoT light curve of an F3V star, observed from May to October 2007 for 152 days. The radius was accurately determined and the mass derived for this new transiting, thanks to the combined analysis of the light curve and complementary ground-based observations: high-precision radial-velocity measurements, on-off photometry, and high signal-to-noise spectroscopic observations. Results. CoRoT-Exo-3b has a radius of 1.01+-0.07 RJup and transits around its F3-type primary every 4.26 days in a synchronous orbit. Its mass of 21.66+-1.0 MJup, density of 26.4+-5.6 g cm^-3, and surface gravity of log g = 4.72 clearly distinguish it from the regular close-in planet population, making it the most intriguing transiting substellar object discovered so far. Conclusions. With the current data, the nature of CoRoT-Exo-3b is ambiguous, as it could either be a low-mass brown-dwarf or a member of a new class of "superplanets". Its discovery may help constrain the evolution of close-in planets and brown-dwarfs better. Finally, CoRoT-Exo-3b confirms the trend that massive transiting giant planets (M >= 4 MJup) are found preferentially around more massive stars than the Sun., 11 pages, 12 figures, accepted for A&A
Published: 2008
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34. Magnetic cycles of the planet-hosting star τ Bootis

Author: Moira Jardine, Gordon A. H. Walker, M. Deleuil, C. Moutou, Rim Fares, Andrew Collier Cameron, C. Catala, E. Shkolnik, J.-F. Donati, D. A. Bohlender, Laboratoire Astrophysique de Toulouse-Tarbes (LATT), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), 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), 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), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), 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), Centre National de la Recherche Scientifique (CNRS)-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, and University of St Andrews [Scotland]
Subjects: Rotation period, Equator, FOS: Physical sciences, Astrophysics, Rotation, 01 natural sciences, stars: individual: τ Boo, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Planet, 0103 physical sciences, stars: activity, stars: magnetic fields, Differential rotation, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics (astro-ph), Giant planet, Astronomy and Astrophysics, Zeeman–Doppler imaging, stars: imaging, Magnetic field, techniques: polarimetric, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics
Abstract: We have obtained new spectropolarimetric observations of the planet-hosting star tauBootis, using the ESPaDOnS and NARVAL spectropolarimeters at the Canada-France-Hawaii Telescope and Telescope Bernard-Lyot. With this data set, we are able to confirm the presence of a magnetic field at the surface of tauBoo and map its large-scale structure over the whole star. The overall polarity of the magnetic field has reversed with respect to our previous observation (obtained a year before), strongly suggesting that tauBoo is undergoing magnetic cycles similar to those of the Sun. This is the first time that a global magnetic polarity switch is observed in a star other than the Sun; we speculate that the magnetic cycle period of tauBoo is much shorter than that of the Sun. Our new data also allow us to confirm the presence of differential rotation from the latitudinal shearing that the magnetic structure is undergoing. The differential rotation surface shear that tauBoo experiences is found to be 6 to 10 times larger than that of the Sun. We propose that the short magnetic cycle period is due to the strong level of differential rotation. With a rotation period of 3.0 and 3.9 d at the equator and pole respectively, tauBoo appears as the first planet-hosting star whose rotation (at intermediate latitudes) is synchronised with the orbital motion of its giant planet (period 3.3 d). Assuming that this synchronisation is not coincidental, it suggests that the tidal effects induced by the giant planet can be strong enough to force the thin convective enveloppe (though not the whole star) into corotation and thus to play a role in the activity cycle of tauBoo., MNRAS, in press
Published: 2008
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35. Transiting exoplanets from the CoRoT space mission: V. CoRoT-Exo-4b: Stellar and planetary parameters

Author: C. Moutou, H. Bruntt, T. Guillot, A. Shporer, E. Guenther, S. Aigrain, J. M. Almenara, R. Alonso, M. Auvergne, A. Baglin, M. Barbieri, P. Barge, W. Benz, P. Bordé, F. Bouchy, H. J. Deeg, R. De la Reza, M. Deleuil, R. Dvorak, A. Erikson, M. Fridlund, M. Gillon, P. Gondoin, A. Hatzes, G. Hébrard, L. Jorda, P. Kabath, H. Lammer, A. Léger, A. Llebaria, B. Loeillet, P. Magain, M. Mayor, T. Mazeh, M. Ollivier, M. Pätzold, F. Pepe, F. Pont, D. Queloz, M. Rabus, H. Rauer, D. Rouan, J. Schneider, S. Udry, G. Wuchterl, 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, and 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)
Subjects: 010504 meteorology & atmospheric sciences, photometry, FOS: Physical sciences, Astrophysics, Star (graph theory), Space (mathematics), 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Circular orbit, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), Astronomy and Astrophysics, Radius, Exoplanet, CoRoT, Photometry (astronomy), exoplanets, 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], transit method, Satellite, Astrophysics::Earth and Planetary Astrophysics
Abstract: The CoRoT satellite has announced its fourth transiting planet (Aigrain et al. 2008) with space photometry. We describe and analyse complementary observations of this system performed to establish the planetary nature of the transiting body and to estimate the fundamental parameters of the planet and its parent star. We have analysed high precision radial-velocity data, ground-based photometry, and high signal-to-noise ratio spectroscopy. The parent star CoRoT-Exo-4 (2MASS 06484671-0040219) is a late F-type star of mass of 1.16 Msun and radius of 1.17 Rsun. The planet has a circular orbit with a period of 9.20205d. The planet radius is 1.19 Rjup and the mass is 0.72 Mjup. It is a gas-giant planet with a ''normal'' internal structure of mainly H and He. CoRoT-Exo-4b has the second longest period of the known transiting planets. It is an important discovery since it occupies an empty area in the mass-period diagram of transiting exoplanets., accepted in A&AL
Published: 2008
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36. Doppler search for exoplanet candidates and binary stars in a CoRoT field using a multi-fiber spectrograph. I. Global analysis and first results

Author: J. C. Bouret, M. Deleuil, A. Recio-Blanco, Frederic Pont, Frédéric Royer, P. de Laverny, François Bouchy, N. C. Santos, B. Loeillet, Pierre Barge, C. Moutou, 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, and 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)
Subjects: Physics, education.field_of_study, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Population, Astrophysics::Instrumentation and Methods for Astrophysics, Brown dwarf, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Exoplanet, Radial velocity, Stars, Space and Planetary Science, Planet, 0103 physical sciences, Binary star, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The discovery of the short-period giant exoplanet population, the so-called hot Jupiter population, and their link to brown dwarfs and low-mass stars challenges the conventional view of planet formation and evolution. We took advantage of the multi-fiber facilities GIRAFFE and FLAMES-UVES (VLT) to perform the first large radial velocity survey using a multi-fiber spectrograph, aiming at detecting planetary and brown dwarfs candidates and binaries. We observed during 5 consecutive half-nights 816 stars selected within one of the exoplanet field of the space mission CoRoT. We computed the radial velocities of these stars and shown that a systematic error of 30 m s$^{-1}$ has been reached over 5 consecutive nights. Over the whole sample the Doppler measurements allowed us to identify a sample of 50 binaries, 9 active or blended binary stars, 5 unsolved cases and 14 exoplanets and brown dwarf candidates. Further higher precision Doppler measurements are now necessary to confirm and better characterize these candidates. This study demonstrates the efficiency of such a multi-fiber approach for large radial velocity surveys in search for exoplanets as well as the follow-up of transiting exoplanet candidates of existing and future programs like the CoRoT space mission.
Published: 2008
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37. The CoRoT mission and its scientific objectives

Author: E. Michel, C. Catala, A. Baglin, M. Deleuil, Pierre Barge, M. Auvergne, and W. Weiss
Subjects: Physics, Pathfinder, Systems engineering, Satellite, Exoplanet, Remote sensing
Abstract: The CoRoT project, developed in the framework of the CNES small satellite programme with a wide european cooperation, has been set up in the early nineties, and will be launched in december 2006. It is dedicated to seismology and detection of rocky planets. In both domains it is a precursor and a pathfinder. Though the programmatic framework imposes quite strong limitations, it is possible to perform both a seismology and an exoplanet finder programme of prime scientific interest.We recall here the scientific specifications, written first in 1998 and upgraded till 2002, which have driven the concept of the instrument and its realisation.The knowledge on ultra‐high precision photometry from space acquired in building CoRoT, and its scientific results, will certainly be very helpful in the definition and preparation of the next generation missions.
Published: 2007
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38. KOI-200 b and KOI-889 b: Two transiting exoplanets detected and characterized withKepler, SOPHIE, and HARPS-N

Author: A. Santerne, C. Moutou, François Bouchy, A. S. Bonomo, G. Bruno, G. Montagnier, Rodrigo F. Díaz, J. M. Almenara, M. Deleuil, G. Hebrard, Cilia Damiani, Laboratoire d'Astrophysique de Marseille (LAM), and 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)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP), Rotation period, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Planetary system, 01 natural sciences, Kepler, Exoplanet, Photometry (optics), Radial velocity, Space and Planetary Science, Planet, 0103 physical sciences, 010303 astronomy & astrophysics, Spectrograph, Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the detection and characterization of the two new transiting, close-in, giant extrasolar planets KOI-200b and KOI-889b. They were first identified by the Kepler team as promising candidates from photometry of the Kepler satellite, then we established their planetary nature thanks to the radial velocity follow-up jointly secured with the spectrographs SOPHIE and HARPS-N. Combined analyses of the whole datasets allow the two planetary systems to be characterized. The planet KOI-200b has mass and radius of 0.68 +/- 0.09 M_Jup and 1.32 +/- 0.14 R_Jup; it orbits in 7.34 days a F8V host star with mass and radius of 1.40 (+0.14/-0.11) M_Sun and 1.51 +/- 0.14 R_Sun. KOI-889b is a massive planet with mass and radius of 9.9 +/- 0.5 M_Jup and 1.03 +/- 0.06 R_Jup; it orbits in 8.88 days an active G8V star with a rotation period of 19.2 +/- 0.3 days, and mass and radius of 0.88 +/- 0.06 M_Sun and 0.88 +/- 0.04 R_Sun. Both planets lie on eccentric orbits and are located just at the frontier between regimes where the tides can explain circularization and where tidal effects are negligible. The two planets are among the first ones detected and characterized thanks to observations secured with HARPS-N, the new spectrograph recently mounted at the Telescopio Nazionale Galileo. These results illustrate the benefits that could be obtained from joint studies using two spectrographs as SOPHIE and HARPS-N., Comment: 10 pages, 4 figures, 4 tables, accepted for publication in A&A
Published: 2013
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39. CHEOPS: A transit photometry mission for ESA's small mission programme

Author: G. Oloffson, Christopher Broeg, M. Steller, Giampaolo Piotto, E. Renotte, Willy Benz, Anton B. Ivanov, Andrea Fortier, Don Pollacco, Wolfgang Baumjohann, Michaël Gillon, N. Thomas, Cheops Team, Roberto Ragazzoni, Yann Alibert, Manuel Meyer, René Liseau, D. Queloz, M. Deleuil, David Ehrenreich, and I. Pagano
Subjects: Brightness, Computer science, media_common.quotation_subject, QC1-999, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Neptune, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Earth mass, Exoplanet, Radial velocity, Stars, Sky, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Ground based radial velocity (RV) searches continue to discover exoplanets below Neptune mass down to Earth mass. Furthermore, ground based transit searches now reach milli-mag photometric precision and can discover Neptune size planets around bright stars. These searches will find exoplanets around bright stars anywhere on the sky, their discoveries representing prime science targets for further study due to the proximity and brightness of their host stars. A mission for transit follow-up measurements of these prime targets is currently lacking. The first ESA S-class mission CHEOPS (CHaracterizing ExoPlanet Satellite) will fill this gap. It will perform ultra-high precision photometric monitoring of selected bright target stars almost anywhere on the sky with sufficient precision to detect Earth sized transits. It will be able to detect transits of RV-planets by photometric monitoring if the geometric configuration results in a transit. For Hot Neptunes discovered from the ground, CHEOPS will be able to improve the transit light curve so that the radius can be determined precisely. Because of the host stars' brightness, high precision RV measurements will be possible for all targets. All planets observed in transit by CHEOPS will be validated and their masses will be known. This will provide valuable data for constraining the mass-radius relation of exoplanets, especially in the Neptune-mass regime. During the planned 3.5 year mission, about 500 targets will be observed. There will be 20% of open time available for the community to develop new science programmes.
Published: 2013
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40. The CoRoT Exoplanet program: status & results

Author: C. Moutou, M. Deleuil, and P. Bordé
Subjects: education.field_of_study, Physics, QC1-999, Population, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Exoplanet, Planet, Quantitative Biology::Populations and Evolution, Computer Science::Programming Languages, Astrophysics::Solar and Stellar Astrophysics, Satellite, Astrophysics::Earth and Planetary Astrophysics, education
Abstract: The CoRoT satellite is the ﬁrst instrument hunting for planets from space. We will review the status of the CoRoT/Exoplanet program. We will then present the CoRoT exoplanetary systems and how they widen the range of properties of the close-in population and contribute to our understanding of the properties of planets.
Published: 2011
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