Author: "Pascal Bordé" / Topic: astrophysics - Searchworks@Jio Institute Digital Library Search Results

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1. 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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2. Planets, candidates, and binaries from the CoRoT/Exoplanet programme

Author: Eike W. Guenther, Alexandre Santerne, Ruth Titz-Weider, Tsevi Mazeh, J. Weingrill, Szilard Csizmadia, P. Guterman, A. P. Hatzes, Sascha Grziwa, A. S. Bonomo, Pascal Bordé, Brandon Tingley, Guillaume Hébrard, Aviv Ofir, Heike Rauer, Suzanne Aigrain, Hannu Parviainen, Juan Cabrera, J. M. Almenara, Magali Deleuil, François Bouchy, Anders Erikson, Roi Alonso, Rodrigo F. Díaz, Malcolm Fridlund, Daniel Rouan, Davide Gandolfi, Marc Ollivier, C. Moutou, Jean Schneider, Hans J. Deeg, Tristan Guillot, A. Léger, Martin Pätzold, 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 Oxford, Universidad de La Laguna [Tenerife - SP] (ULL), 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), INAF - Osservatorio Astrofisico di Torino (OATo), Istituto Nazionale di Astrofisica (INAF), ECLIPSE 2018, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Universidad de Buenos Aires [Buenos Aires] (UBA), DLR Institute of Planetary Research, German Aerospace Center (DLR), 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), Università degli studi di Torino = University of Turin (UNITO), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Thüringer Landessternwarte Tautenburg (TLS), 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), Rhenish Institute for Environmental Research (RIU), University of Cologne, Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), 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), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), European Space Agency (ESA)-European Space Agency (ESA), Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), University of Oxford [Oxford], Institut de Radioprotection et de Sûreté Nucléaire (IRSN), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Università degli studi di Torino (UNITO), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)
Subjects: instruments [space vehicles], Brown dwarf, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Binary number, FOS: Physical sciences, Astrophysics, 01 natural sciences, PARAMETERS, photometric [techniques], techniques: photometric, eclipsing [binaries], Planet, 0103 physical sciences, data analysis [methods], Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), space vehicles: instruments, 010303 astronomy & astrophysics, Physics, LIGHT CURVES, Earth and Planetary Astrophysics (astro-ph.EP), SPACE MISSION, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, binaries: eclipsing, Astronomy and Astrophysics, Orbital period, Light curve, EXOPLANETS, methods: data analysis, Exoplanet, Stars, Space and Planetary Science, Binaries: Eclipsing, Methods: Data analysis, Space vehicles: Instruments, Techniques: Photometric, stars: planetary systems - stars binaries: eclipsing - techniques: photometric - space vehicles: instrument - methods: data analysis , Astrophysics::Earth and Planetary Astrophysics, SYSTEM, Astrophysics - Earth and Planetary Astrophysics
Abstract: We provide the catalogue of all transit-like features, including false alarms, detected by the CoRoT exoplanet teams in the 177 454 light curves of the mission. All these detections have been re-analysed with the same softwares so that to ensure their homogeneous analysis. Although the vetting process involves some human evaluation, it also involves a simple binary flag system over basic tests: detection significance, presence of a secondary, difference between odd and even depths, colour dependence, V-shape transit, and duration of the transit. We also gathered the information from the large accompanying ground-based programme carried out on the planet candidates and checked how useful the flag system could have been at the vetting stage of the candidates. In total, we identified and separated 824 false alarms of various kind, 2269 eclipsing binaries among which 616 are contact binaries and 1653 are detached ones, 37 planets and brown dwarfs, and 557 planet candidates. For the planet candidates, the catalogue gives not only their transit parameters but also the products of their light curve modelling, together with a summary of the outcome of follow-up observations when carried out and their current status. Among the planet candidates whose nature remains unresolved, we estimate that 8 +/- 3 planets are still to be identified. We derived planet and brown dwarf occurrences and confirm disagreements with Kepler estimates: small-size planets with orbital period less than ten days are underabundant by a factor of three in the CoRoT fields whereas giant planets are overabundant by a factor of two. These preliminary results would however deserve further investigations using the recently released CoRoT light curves that are corrected of the various instrumental effects and a homogeneous analysis of the stellar populations observed by the two missions., Comment: Full tables will be provided online at CDS
Published: 2018
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3. Measuring stellar granulation during planet transits

Author: Anthony Caldas, Remo Collet, Pascal Bordé, Martin Asplund, Zazralt Magic, Jérémy Leconte, Franck Selsis, P. von Paris, Andrea Chiavassa, Université Côte d'Azur ( UCA ), ECLIPSE 2017, Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Interdisciplinaire Carnot de Bourgogne ( LICB ), Université de Bourgogne ( UB ) -Centre National de la Recherche Scientifique ( CNRS ), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interdisciplinaire Carnot de Bourgogne (LICB), and Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Gas giant, FOS: Physical sciences, Astrophysics, 01 natural sciences, Orbital inclination, photometric [techniques], techniques: photometric, Planet, 0103 physical sciences, Hot Jupiter, planet-star interactions, stars: activity, stars: atmospheres, Astrophysics::Solar and Stellar Astrophysics, Hot Neptune, Transit (astronomy), 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), atmospheres [stars], Earth and Planetary Astrophysics (astro-ph.EP), Physics, activity [stars], 010308 nuclear & particles physics, Astronomy and Astrophysics, Light curve, [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Exoplanet, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, radiative transfer, hydrodynamics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: Stellar activity and convection-related surface structures might cause bias in planet detection and characterization that use these transits. Surface convection simulations help to quantify the granulation signal. We used realistic three-dimensional radiative hydrodynamical simulations from the Stagger grid and synthetic images computed with the radiative transfer code Optim3D to model the transits of three prototype planets: a hot Jupiter, a hot Neptune, and a terrestrial planet. We computed intensity maps from RHD simulations of the Sun and a K-dwarf star at different wavelength bands from optical to far-infrared. We modeled the transit using synthetic stellar-disk images and emulated the temporal variation of the granulation intensity. We identified two types of granulation noise that act simultaneously during the planet transit: (i) the intrinsic change in the granulation pattern with timescales smaller than the usual planet transit, and (ii) the fact that the transiting planet occults isolated regions of the photosphere that differ in local surface brightness. Our modeling approach shows that the granulation pattern has a non-negligible effect on the light curve depth during the transit, and, consequentially on the determination of the radius of the planet transiting. The granulation noise appears to be correlated among the different wavelength ranges either in the visible or in the infrared regions. The granulation has to be considered as an intrinsic uncertainty (as a result of stellar variability) on the precise measurements of exoplanet transits of planets. The full characterization of the granulation is essential for determining the degree of uncertainty on the planet parameters. In this context, the use of 3D RHD simulations is important to measure the convection-related fluctuations., Accepted for publication in Section 10. Planets and planetary systems of Astronomy and Astrophysics
Published: 2017
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4. CoRoT-22 b: a validated 4.9 R exoplanet in 10-d orbit

Author: Davide Gandolfi, François Bouchy, T. Guillot, H. J. Deeg, Anders Erikson, Alexandre Santerne, J. Schneider, Helmut Lammer, J. M. Almenara, Brandon Tingley, C. Lovis, Eike W. Guenther, Heike Rauer, A. P. Hatzes, A. S. Bonomo, A. Baglin, Tsevi Mazeh, J. Cabrera, S. Carpano, Rudolf Dvorak, Guillaume Hébrard, Pierre Barge, Marc Ollivier, Michael Endl, C. Moutou, Günther Wuchterl, Aviv Ofir, Phillip J. MacQueen, Malcolm Fridlund, T. Pasternacki, Sylvio Ferraz-Mello, Pascal Bordé, Roi Alonso, Rodrigo F. Díaz, Martin Pätzold, William D. Cochran, D. Rouan, Szilard Csizmadia, Magali Deleuil, and Suzanne Aigrain
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, 01 natural sciences, Planet, Primary (astronomy), 0103 physical sciences, PLANETAS (SISTEMAS), Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Astronomy, Astronomy and Astrophysics, Planetary system, stars: planetary systems - techniques: photometry - techniques: radial velocities - techniques: spectroscopic, Light curve, Orbital period, Exoplanet, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics, Kepler-62c
Abstract: The CoRoT satellite has provided high-precision photometric light curves for more than 163 000 stars and found several hundreds of transiting systems compatible with a planetary scenario. If ground-based velocimetric observations are the best way to identify the actual planets among many possible configurations of eclipsing binary systems, recent transit surveys have shown that it is not always within reach of the radial-velocity detection limits. In this paper, we present a transiting exoplanet candidate discovered by CoRoT whose nature cannot be established from ground-based observations, and where extensive analyses are used to validate the planet scenario. They are based on observing constraints from radial-velocity spectroscopy, adaptive optics imaging and the CoRoT transit shape, as well as from priors on stellar populations, planet and multiple stellar systems frequency. We use the fully Bayesian approach developed in the PASTIS (Planet Analysis and Small Transit Investigation Software) analysis software, and conclude that the planet scenario is at least 1400 times more probable than any other false-positive scenario. The primary star is a metallic solar-like dwarf, with M-s = 1.099 +/- 0.049 M-circle dot and R-s = 1.136(-0.090)(+0.038) R-circle dot. The validated planet has a radius of R-p = 4.88(-0.39)(+0.17) R-circle plus and mass less than 49 M-circle plus. Its mean density is smaller than 2.56 g cm(-3) and orbital period is 9.7566 +/- 0.0012 d. This object, called CoRoT-22 b, adds to a large number of validated Kepler planets. These planets do not have a proper measurement of the mass but allow statistical characterization of exoplanets population.
Published: 2014

5. Transiting exoplanets from the CoRoT space mission: II. CoRoT-Exo-2b: A transiting planet around an active G star

Author: Annie Baglin, M. Ollivier, J. M. Almenara, C. Moutou, Martin Pätzold, Artie P. Hatzes, Suzanne Aigrain, Frederic Pont, Heike Rauer, Willy Benz, Roi Alonso, Malcolm Fridlund, Anders Erikson, Avi Shporer, R. de la Reza, G. Wuchterl, Rudolf Dvorak, Helmut Lammer, François Bouchy, Pierre Barge, Laurent Jorda, Tristan Guillot, Antoine Llebaria, Michel Mayor, Hans J. Deeg, Michaël Gillon, Pascal Bordé, Magali Deleuil, J. Schneider, B. Loeillet, Didier Queloz, Francesco Pepe, Tsevi Mazeh, Daniel Rouan, M. Barbieri, B. Stecklum, P. Gondoin, Petr Kabath, Guillaume Hébrard, Pierre Magain, Michel Auvergne, A. Léger, Stéphane 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 (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, 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), Instituto de Astrofísica de Canarias (IAC), University of Exeter, Physikalisches Institut, Universität Bern, 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), Observatório Nacional/MCTI, Institut für Astronomie, Universität Wien (IfA), Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Research and Scientific Support Department, ESA-ESTEC (RSSD), 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), Thüringer Landessternwarte, Tautenburg Observatory, Institut für Weltraumforschung, Österreichische Akademie der Wissenschaften (IWF), Institut d'Astrophysique, Géophysique et Océanographie, Université de Liège, Tel Aviv University (TAU), Rheinisches Institut für Umweltforschung an der Universität zu Köln (RIU), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, 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), European Southern Observatory (ESO), Observatoire de Paris - Site de Paris (OP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), School of Physics, Instituto de Astrofisica de Canarias (IAC), Physikalisches Institut [Bern], Universität Bern [Bern] (UNIBE), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), ON/MCT (ON/MCT, 20921-030, Rio de Janeiro, Brazil)), ON/MCT, DLR Institute of Planetary Research, German Aerospace Center (DLR), 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), Geneva Observatory, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), 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), Thüringer Landessternwarte Tautenburg (TLS), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), 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), Institute for Geophysics and Meteorology [Köln] (IGM), University of Cologne, 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), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Universität Bern [Bern], Université de Genève (UNIGE), European Space Agency (ESA)-European Space Agency (ESA), University of Geneva [Switzerland], Université Nice Sophia Antipolis (... - 2019) (UNS), School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Beaussier, Catherine, 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), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: photometry, FOS: Physical sciences, Context (language use), Exo-2b, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], CoRot, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), 010303 astronomy & astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy and Astrophysics, Galactic plane, Light curve, Exoplanet, Radial velocity, Stars, exoplanets, 13. Climate action, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], transit method, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Context. The CoRoT mission, a pioneer in exoplanet searches from space, has completed its first 150 days of continuous observations of ~12000 stars in the galactic plane. An analysis of the raw data identifies the most promising candidates and triggers the ground-based follow-up. Aims. We report on the discovery of the transiting planet CoRoT-Exo-2b, with a period of 1.743 days, and characterize its main parameters. Methods. We filter the CoRoT raw light curve of cosmic impacts, orbital residuals, and low frequency signals from the star. The folded light curve of 78 transits is fitted to a model to obtain the main parameters. Radial velocity data obtained with the SOPHIE, CORALIE and HARPS spectro-graphs are combined to characterize the system. The 2.5 min binned phase-folded light curve is affected by the effect of sucessive occultations of stellar active regions by the planet, and the dispersion in the out of transit part reaches a level of 1.09x10-4 in flux units. Results. We derive a radius for the planet of 1.465+-0.029 R_Jup and a mass of 3.31+-0.16 M_Jup, corresponding to a density of 1.31+-0.04 g/cm^3. The large radius of CoRoT-Exo-2b cannot be explained by current models of evolution of irradiated planets., A&A Letters (in press), 7 pages, 3 figures
Published: 2016
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6. The secondary eclipse of CoRoT-1b

Author: Roi Alonso, A. Léger, Tsevi Mazeh, François Bouchy, Laurent Jorda, Günther Wuchterl, Frederic Pont, Anders Erikson, Pierre Magain, Suzanne Aigrain, M. Pätzold, Magali Deleuil, Marc Ollivier, R. de la Reza, A. P. Hatzes, M. Fridlund, Antoine Llebaria, S. Chaintreuil, Hans J. Deeg, P. Gondoin, M. Barbieri, Pierre Barge, Helmut Lammer, A. Alapini, C. Moutou, Didier Queloz, Aldo S. Bonomo, M. Auvergne, Pascal Bordé, Jean Schneider, Heike Rauer, Tristan Guillot, D. Rouan, F. Fialho, A. Baglin, Rudolf Dvorak, 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, media_common.quotation_subject, Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, 7. Clean energy, symbols.namesake, Bond albedo, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Black-body radiation, Circular orbit, Eccentricity (behavior), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, media_common, Eclipse, Physics, Thermal equilibrium, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy and Astrophysics, CoRoT, secondary eclipse, exoplanets, 13. Climate action, Space and Planetary Science, transit method, symbols, CoRoT-1b, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: The transiting planet CoRoT-1b is thought to belong to the pM-class of planets, in which the thermal emission dominates in the optical wavelengths. We present a detection of its secondary eclipse in the CoRoT white channel data, whose response function goes from ~400 to ~1000 nm. We used two different filtering approaches, and several methods to evaluate the significance of a detection of the secondary eclipse. We detect a secondary eclipse centered within 20 min at the expected times for a circular orbit, with a depth of 0.016+/-0.006%. The center of the eclipse is translated in a 1-sigma upper limit to the planet's eccentricity of ecosomega, 6 pages, to appear in A&A, submitted 18 march 2009, accepted 7 July 2009
Published: 2016
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7. Planetary transit candidates in the CoRoT initial run: resolving their nature

Author: Eike W. Guenther, Günther Wuchterl, François Bouchy, Tsevi Mazeh, Magali Deleuil, S. Carpano, Francesco Pepe, C. Lovis, Martin Pätzold, Davide Gandolfi, J. M. Almenara, Suzanne Aigrain, Pierre Barge, Daniel Rouan, A. P. Hatzes, M. Fridlund, Laurent Jorda, C. Moutou, Antoine Llebaria, Michel Mayor, M. Auvergne, Pascal Bordé, Willy Benz, Jean Schneider, Heike Rauer, Marc Ollivier, Hans J. Deeg, G. Hebrard, Frederic Pont, M. Barbieri, A. Léger, Markus Rabus, P. Gondoin, R. de la Reza, Didier Queloz, B. Loeillet, Helmut Lammer, Petr Kabath, H. Bruntt, Tristan Guillot, Avi Shporer, A. Baglin, Rudolf Dvorak, Michaël Gillon, Anders Erikson, Pierre Magain, Roi Alonso, Stéphane Udry, 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, photometry, 010308 nuclear & particles physics, Giant planet, Astronomy, Astronomy and Astrophysics, Astrophysics, Planetary system, Light curve, follow-up observations, 01 natural sciences, CoRoT, Radial velocity, Stars, exoplanets, transit method, Space and Planetary Science, Planet, 0103 physical sciences, Binary star, transit candidates, Transit (astronomy), 010303 astronomy & astrophysics
Abstract: With the release of CoRoT lightcurves of the Initial Run IRa01, 50 transiting planetary candidates have been published in a companion paper. About twenty of them were identified as binary stars from the CoRoT lightcurve itself. Complementary observations were conducted for 29 candidates, including ground-based photometry and radial-velocity measurements. Two giant planets were identified and fully characterized. Nineteen binaries are recognized, from which 10 are background eclipsing binaries in the CoRoT mask or triple systems, diluted by the main CoRoT target. Eight cases remain of unclear origin, one of them still being a planetary candidate. Comparison with simulations shows that the actual threshold of confirmed planet detection in this field does not yet fulfill the expectations, and a number of reasons are invoked, like the ranking process based on lightcurve analyses, and the strategy and limits of follow-up observations for targets fainter than magnitude 15.
Published: 2016
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8. Transiting exoplanets from the CoRoT space mission Resolving the nature of transit candidates for the LRa03 and SRa03 fields

Author: Davide Gandolfi, François Bouchy, A. Baglin, Magali Deleuil, Günther Wuchterl, Rudolf Dvorak, Laurent Jorda, Alexandre Santerne, Jean Schneider, M. Auvergne, T Pasternacki, Hans J. Deeg, Roi Alonso, Pierre Barge, Rodrigo F. Díaz, A. P. Hatzes, Pascal Bordé, Eike W. Guenther, J. Weingrill, Aviv Ofir, Tristan Guillot, William D. Cochran, Ludmila Carone, J.-M. Almenara, Michael Endl, Aldo S. Bonomo, Szilard Csizmadia, D. Queloz, Helmut Lammer, S. Carpano, Tsevi Mazeh, A. Léger, C. Lovis, Brandon Tingley, Phillip J. MacQueen, Martin Pätzold, G. Hebrard, B. Samuel, T -O Lev, D. Rouan, Hannu Parviainen, Heike Rauer, Marc Ollivier, C. Moutou, M. Fridlund, Michaël Gillon, Anders Erikson, Suzanne Aigrain, C. Cavarroc, Juan Cabrera, 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: Physics, 010504 meteorology & atmospheric sciences, Field (physics), Astronomy, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Exoplanet, Cosmology, Stars, Spitzer Space Telescope, Space and Planetary Science, Planet, 0103 physical sciences, stars: planetary systems - techniques: photometry - techniques: radial velocities - techniques: spectroscopic, Transit (astronomy), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: CoRoT is a space telescope which aims at studying internal structure of stars and detecting extrasolar planets. We present here a list of transits detected in the light curves of stars observed by CoRoT in two fields in the anti-center direction: the LRa03 one observed during 148 days from 3 October 2009 to 1 March 2010 followed by the SRa03 one from the 5 March 2010 to the 29 March 2010 during 25 days. 5329 light curves for the LRa03 field and 4169 for the SRa03 field were analyzed by the detection team of CoRoT. Then some of the selected exoplanetary candidates have been followed up from the ground. In the LRa03 field, 19 exoplanet candidates have been found, 8 remain unsolved. No secured planet has been found yet. In the SRa03 field, there were 11 exoplanetary candidates among which 6 cases remain unsolved and 3 planets have been found: CoRoT-18b, CoRoT-19b, CoRoT-20b. © 2011 Springer Science+Business Media B.V.
Published: 2011
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9. Transiting exoplanets from the CoRoT space mission

Author: Amaury H. M. J. Triaud, Roi Alonso, Suzanne Aigrain, P. Gondoin, Didier Queloz, Michel Auvergne, Artie P. Hatzes, François Bouchy, Annie Baglin, Tristan Guillot, B. Loeillet, Pierre Magain, M. Ollivier, Helmut Lammer, Stéphane Udry, Rudolf Dvorak, Frederic Pont, G. Wuchterl, Michel Mayor, Laurent Jorda, R. de la Reza, J. Schneider, Malcolm Fridlund, Antoine Llebaria, C. Moutou, Pierre Barge, Magali Deleuil, Hans J. Deeg, Francesco Pepe, Martin Pätzold, Guillaume Hébrard, Heike Rauer, Pascal Bordé, A. Léger, Anders Erikson, Willy Benz, Daniel Rouan, 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), 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), Thüringer Landessternwarte, Tautenburg Observatory, 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), 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, Physikalisches Institut, Universität Bern, 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), Instituto de Astrofísica de Canarias (IAC), Observatório Nacional/MCTI, Institut für Astronomie, Universität Wien (IfA), Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), Research and Scientific Support Department, ESA-ESTEC (RSSD), 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), Institut d'Astrophysique, Géophysique et Océanographie, Université de Liège, Institut für Geophysik und Meteorologie, Universität zu Köln (IGM), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Thüringer Landessternwarte Tautenburg (TLS), School of Physics, Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Physikalisches Institut [Bern], Universität Bern [Bern], Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de Astrofisica de Canarias (IAC), ON/MCT (ON/MCT, 20921-030, Rio de Janeiro, Brazil)), ON/MCT, DLR Institute of Planetary Research, German Aerospace Center (DLR), Research and Scientific Support Department, ESTEC (RSSD), European Space Research and Technology Centre (ESTEC), European Space Agency (ESA)-European Space Agency (ESA), Geneva Observatory, University of Geneva [Switzerland], 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, 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), European Southern Observatory (ESO), Institute for Geophysics and Meteorology [Köln] (IGM), University of Cologne, Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université de Genève = University of Geneva (UNIGE), Universität Bern [Bern] (UNIBE), 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), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), Université Nice Sophia Antipolis (1965 - 2019) (UNS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Palaeontology - Institute of Geology, and Bergakademie Freiberg
Subjects: spectroscopy, photometry, FOS: Physical sciences, Exo-2b, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Space (mathematics), 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spectral analysis, Transit (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Exoplanet, CoRoT, Radial velocity, exoplanets, transit method, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: We report on the spectroscopic transit of the massive hot-Jupiter CoRoT-Exo-2b observed with the high-precision spectrographs SOPHIE and HARPS. By modeling the radial velocity anomaly occurring during the transit due to the Rossiter-McLaughlin (RM) effect, we determine the sky-projected angle between the stellar spin and the planetary orbital axis to be close to zero lambda=7.2+-4.5 deg, and we secure the planetary nature of CoRoT-Exo-2b. We discuss the influence of the stellar activity on the RM modeling. Spectral analysis of the parent star from HARPS spectra are presented., A&A Letters (in press), 5 pages, 2 figures
Published: 2008
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10. Inferring heat recirculation and albedo for exoplanetary atmospheres: Comparing optical phase curves and secondary eclipse data

Author: P. von Paris, Franck Selsis, Pascal Bordé, Pierre Gratier, ECLIPSE 2016, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and AMOR 2016
Subjects: 010504 meteorology & atmospheric sciences, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, 01 natural sciences, symbols.namesake, Planet, 0103 physical sciences, Thermal, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Scattering, Heat recirculation, Astronomy and Astrophysics, Thermal emission, Phase curve, Atmosphere of Earth, 13. Climate action, Space and Planetary Science, symbols, Astrophysics::Earth and Planetary Astrophysics, Doppler effect, Astrophysics - Earth and Planetary Astrophysics
Abstract: Basic atmospheric properties such as albedo and heat redistribution between day and nightside have been inferred for a number of planets using observations of secondary eclipses and thermal phase curves. Optical phase curves have not yet been used to constrain these atmospheric properties consistently. We re-model previously published phase curves of CoRoT-1b, TrES-2b and HAT-P-7b and infer albedos and recirculation efficiencies. These are then compared to previous estimates based on secondary eclipse data. We use a physically consistent model to construct optical phase curves. This model takes Lambertian reflection, thermal emission, ellipsoidal variations and Doppler boosting into account. CoRoT-1b shows a non-negligible scattering albedo (0.11, Comment: accepted for publication in Astronomy & Astrophysics on Dec 14th, main manuscript: 16 pages, 20 figures, 2 tables. Contains 5 Appendices
Published: 2015
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11. High‐Contrast Imaging from Space: Speckle Nulling in a Low‐Aberration Regime

Author: Wesley A. Traub and Pascal Bordé
Subjects: Diffraction, Wavefront, Physics, business.industry, Astrophysics (astro-ph), Fast Fourier transform, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Physics::Optics, Astronomy and Astrophysics, Speckle noise, Astrophysics, Image plane, Deformable mirror, law.invention, Speckle pattern, Optics, Space and Planetary Science, law, business, Coronagraph
Abstract: High-contrast imaging from space must overcome two major noise sources to successfully detect a terrestrial planet angularly close to its parent star: photon noise from diffracted star light, and speckle noise from star light scattered by instrumentally-generated wavefront perturbation. Coronagraphs tackle only the photon noise contribution by reducing diffracted star light at the location of a planet. Speckle noise should be addressed with adaptative-optics systems. Following the tracks of Malbet, Yu and Shao (1995), we develop in this paper two analytical methods for wavefront sensing and control that aims at creating dark holes, i.e. areas of the image plane cleared out of speckles, assuming an ideal coronagraph and small aberrations. The first method, speckle field nulling, is a fast FFT-based algorithm that requires the deformable-mirror influence functions to have identical shapes. The second method, speckle energy minimization, is more general and provides the optimal deformable mirror shape via matrix inversion. With a NxN deformable mirror, the size of matrix to be inverted is either N^2xN^2 in the general case, or only NxN if influence functions can be written as the tensor product of two one-dimensional functions. Moreover, speckle energy minimization makes it possible to trade off some of the dark hole area against an improved contrast. For both methods, complex wavefront aberrations (amplitude and phase) are measured using just three images taken with the science camera (no dedicated wavefront sensing channel is used), therefore there are no non-common path errors. We assess the theoretical performance of both methods with numerical simulations, and find that these speckle nulling techniques should be able to improve the contrast by several orders of magnitude., Comment: 31 pages, 8 figures, 1 table. Accepted for publication in ApJ (should appear in February 2006)
Published: 2006
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12. The diameter and evolutionary state of Procyon A

Author: Pascal Bordé, Janine Provost, Gabrielle Berthomieu, Pierre Kervella, Pierre Morel, F. Thévenin, European Southern Observatory, 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, Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)
Subjects: Physics, Oscillation, chemistry.chemical_element, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Mass ratio, Luminosity, chemistry, Space and Planetary Science, Angular diameter, Frequency separation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Parallax, Mass fraction, Astrophysics::Galaxy Astrophysics, Helium
Abstract: International audience; We report the angular diameter measurement obtained with the VINCI/VLTI instrument on the nearby star Procyon A (alpha CMi A, F5IV-V), at a relative precision of ± 0.9%. We obtain a uniform disk angular diameter in the K band of thetaUD = 5.376±0.047 mas and a limb darkened value of thetaLD = 5.448±0.053 mas. Together with the HIPPARCOS parallax, this gives a linear diameter of 2.048±0.025 D&sun;. We use this result in combination with spectroscopic, photometric and asteroseismic constraints to model this star with the CESAM code. One set of modeling parameters that reproduces the observations within their error bars are an age of 2314 Myr, an initial helium mass fraction Y_i=0.301 and an initial mass ratio of heavy elements to hydrogen (Z/X)i=0.0314. We also computed the adiabatic oscillation spectrum of our model of Procyon A, giving a mean large frequency separation of /line{Deltanu0}≈ 54.7 muHz. This value is in agreement with the seismic observations by Martic et al. (\cite{martic}, \cite{martic01}). The interferometric diameter and the asteroseismic large frequency spacing together suggest a mass closer to 1.4 M&sun; than to 1.5 M&sun;. We conclude that Procyon is currently ending its life on the main sequence, as its luminosity class indicates.
Published: 2003
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13. Transiting exoplanets from the CoRoT space mission: XXIV. CoRoT-25b and CoRoT-26b: two low-density giant planetas

Author: François Bouchy, Davide Gandolfi, Heike Rauer, Alexandre Santerne, J. M. Almenara, J. Weingrill, Juan Cabrera, A. P. Hatzes, Magali Deleuil, B. Samuel, Tristan Guillot, M. Auvergne, Sylvio Ferraz-Mello, B. Gardes, Brandon Tingley, T. Pasternacki, Günther Wuchterl, Roi Alonso, Rodrigo F. Díaz, S. Carpano, M. Fridlund, D. Queloz, Helmut Lammer, Suzanne Aigrain, Sz. Csizmadia, Hannu Parviainen, Daniel Rouan, A. Baglin, Aldo S. Bonomo, Rudolf Dvorak, Hans J. Deeg, Aviv Ofir, Michael Endl, Marc Ollivier, Jean Schneider, C. Moutou, Michaël Gillon, Anders Erikson, M. Havel, Patrick Gaulme, Phillip J. MacQueen, A. Léger, William D. Cochran, Pascal Bordé, Guillaume Hébrard, Lev Tal-Or, Eike W. Guenther, Martin Pätzold, Tsevi Mazeh, and Cilia Damiani
Subjects: Physics, Super-Earth, 010504 meteorology & atmospheric sciences, Giant planet, Astronomy and Astrophysics, Astrophysics, Planetary system, 01 natural sciences, Exoplanet, ESPECTROSCOPIA, planetary systems, photometric, radial velocities, techniques, spectroscopic, Radial velocity, planetary systems / techniques: photometric / techniques: radial velocities / techniques: spectroscopic, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, 010303 astronomy & astrophysics, Planetary mass, 0105 earth and related environmental sciences
Abstract: We report the discovery of two transiting exoplanets, CoRoT-25b and CoRoT-26b, both of low density, one of which is in the Saturn mass-regime. For each star, ground-based complementary observations through optical photometry and radial velocity measurements secured the planetary nature of the transiting body and allowed us to fully characterize them. For CoRoT-25b we found a planetary mass of 0.27 ± 0.04 M Jup , a radius of 1.08-0.10 +0.3 R Jup and hence a mean density of 0.15-0.06 +0.15 g cm-3 . The planet orbits an F9 main-sequence star in a 4.86-day period, that has a V magnitude of 15.0, solar metallicity, and an age of 4.5-2.0 +1.8 -Gyr. CoRoT-26b orbits a slightly evolved G5 star of 9.06 ± 1.5-Gyr age in a 4.20-day period that hassolar metallicity and a V magnitude of 15.8. With a mass of 0.52 ± 0.05 M Jup , a radius of 1.26-0.07 +0.13 R Jup , and a mean density of 0.28-0.07 +0.09 g cm-3 , it belongs to the low-mass hot-Jupiter population. Planetary evolution models allowed us to estimate a core mass of a few tens of Earth mass for the two planets with heavy-element mass fractions of 0.52-0.15 +0.08 and 0.26-0.08 +0.05 , respectively, assuming that a small fraction of the incoming flux is dissipated at the center of the planet. In addition, these models indicate that CoRoT-26b is anomalously large compared with what standard models could account for, indicating that dissipation from stellar heating could cause this size.
Published: 2013

14. Transiting exoplanets from the CoRoT space mission. XXIII. CoRoT-21b: a doomed large Jupiter around a faint subgiant star

Author: J. Weingrill, M. Fridlund, Michael Endl, Hannu Parviainen, Pascal Bordé, A. Léger, François Bouchy, Sascha Grziwa, Brandon Tingley, Günther Wuchterl, Guillaume Hébrard, Sz. Csizmadia, Didier Queloz, A. S. Bonomo, Suzanne Aigrain, A. Llebaria, Tsevi Mazeh, A. P. Hatzes, Helmut Lammer, Alexandre Santerne, Annie Baglin, D. Rouan, Magali Deleuil, Rudolf Dvorak, Davide Gandolfi, J. M. Almenara, Tristan Guillot, Sylvio Ferraz-Mello, Ruben Diaz, William D. Cochran, Roi Alonso, Marc Ollivier, Juan Cabrera, Jean Schneider, C. Cavarroc, Ludmila Carone, Phillip J. MacQueen, Aviv Ofir, T. Pasternacki, Martin Pätzold, Michaël Gillon, Anders Erikson, M. Auvergne, Heike Rauer, Pierre Barge, C. Moutou, Hans J. Deeg, Laurent Jorda, 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: 010504 meteorology & atmospheric sciences, planetary systems planet-star interactions extrasolar planets, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, Jupiter, Rings of Jupiter, Planet, planet-star interactions, 0103 physical sciences, Hot Jupiter, MECÂNICA CELESTE, Astrophysics::Solar and Stellar Astrophysics, planetary systems, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Stellar rotation, Giant planet, Astronomy, Astronomy and Astrophysics, planetary systems – planet-star interactions, Exoplanet, 13. Climate action, Space and Planetary Science, ddc:520, Astrophysics::Earth and Planetary Astrophysics, Jupiter mass
Abstract: CoRoT-21, a F8IV star of magnitude V = 16 mag, was observed by the space telescope CoRoT during the Long Run 01 (LRa01) in the first winter field (constellation Monoceros) from October 2007 to March 2008. Transits were discovered during the light curve processing. Radial velocity follow-up observations, however, were performed mainly by the 10-m Keck telescope in January 2010. The companion CoRoT-21b is a Jupiter-like planet of 2.26 ± 0.33 Jupiter masses and 1.30 ± 0.14 Jupiter radii in an circular orbit of semi-major axis 0.0417 ± 0.0011 AU and an orbital period of 2.72474 ± 0.00014 days. The planetary bulk density is (1.36 ± 0.48) × 103 kg m-3, very similar to the bulk density of Jupiter, and follows an M1/3 − R relation like Jupiter. The F8IV star is a sub-giant star of 1.29 ± 0.09 solar masses and 1.95 ± 0.2 solar radii. The star and the planet exchange extremetidal forces that will lead to orbital decay and extreme spin-up of the stellar rotation within 800 Myr if the stellar dissipation is Q∗/k2∗ ≤ 107. CoRoT-21, a F8IV star of magnitude V = 16 mag, was observed by the space telescope CoRoT during the Long Run 01 (LRa01) in the first winter field (constellation Monoceros) from October 2007 to March 2008. Transits were discovered during the light curve processing. Radial velocity follow-up observations, however, were performed mainly by the 10-m Keck telescope in January 2010. The companion CoRoT-21b is a Jupiter-like planet of 2.26 ± 0.33 Jupiter masses and 1.30 ± 0.14 Jupiter radii in an circular orbit of semi-major axis 0.0417 ± 0.0011 AU and an orbital period of 2.72474 ± 0.00014 days. The planetary bulk density is (1.36 ± 0.48) × 103 kg m-3, very similar to the bulk density of Jupiter, and follows an M1/3 - R relation like Jupiter. The F8IV star is a sub-giant star of 1.29 ± 0.09 solar masses and 1.95 ± 0.2 solar radii. The star and the planet exchange extremetidal forces that will lead to orbital decay and extreme spin-up of the stellar rotation within 800 Myr if the stellar dissipation is Q∗/k2∗ ≤ 107. The CoRoT space mission, launched on December 27th 2006, has been developed and is operated by CNES, with the contribution of Austria, Belgium, Brazil, ESA (RSSD and Science Programme), Germany and Spain.
Published: 2012
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15. 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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16. Transiting exoplanets from the CoRoT space mission. XXII. CoRoT-16b: a hot Jupiter with a hint of eccentricity around a faint solar-like star

Author: Sascha Grziwa, Günther Wuchterl, Brandon Tingley, A. Léger, François Bouchy, Sylvio Ferraz-Mello, Roi Alonso, Rodrigo F. Díaz, C. Lovis, T. Pasternacki, M. Fridlund, P. Guterman, M. Havel, A. P. Hatzes, Juan Cabrera, C. Cavarroc, Alexandre Santerne, Annie Baglin, Michael Endl, M. Auvergne, M. Tadeu dos Santos, J. Weingrill, William D. Cochran, J. M. Almenara, Heike Rauer, J. C. Gazzano, Lev Tal-Or, Hans J. Deeg, Michel Mayor, Guillaume Hébrard, Tristan Guillot, Rudolf Dvorak, Davide Gandolfi, Eike W. Guenther, Martin Pätzold, Pascal Bordé, Marc Ollivier, B. Samuel, Tsevi Mazeh, Jean Schneider, Helmut Lammer, Daniel Rouan, Sz. Csizmadia, Phillip J. MacQueen, H. Bruntt, Didier Queloz, Ludmila Carone, Magali Deleuil, Suzanne Aigrain, Aviv Ofir, C. Moutou, Aldo S. Bonomo, Michaël Gillon, Anders Erikson, Pierre Barge, S. Carpano, 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: media_common.quotation_subject, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, techniques: photometric, Planet, 0103 physical sciences, Hot Jupiter, techniques: radial velocities, Astrophysics::Solar and Stellar Astrophysics, Eccentricity (behavior), 010306 general physics, 010303 astronomy & astrophysics, planetary systems, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, Physics, [PHYS]Physics [physics], Astronomy, Astronomy and Astrophysics, Planetary system, PLANETAS, Exoplanet, Radial velocity, Orbit, 13. Climate action, Space and Planetary Science, ddc:520, High Energy Physics::Experiment, Satellite, Astrophysics::Earth and Planetary Astrophysics, stars: fundamental parameters, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], techniques: spectroscopic
Abstract: Aims. We report the discovery of CoRoT-16b, a low density hot jupiter that orbits a faint G5V star (mV = 15.63) in 5.3523 ± 0.0002 days with slight eccentricity. A fit of the data with no a priori assumptions on the orbit leads to an eccentricity of 0.33 ± 0.1. We discuss this value and also derive the mass and radius of the planet.Methods. We analyse the photometric transit curve of CoRoT-16 given by the CoRoT satellite, and radial velocity data from the HARPS and HIRES spectrometers. A combined analysis using a Markov chain Monte Carlo algorithm is used to get the system parameters.Results. CoRoT-16b is a 0.535 −0.083/+0.085 MJ, 1.17 −0.14/+0.16 RJ hot Jupiter with a density of 0.44 −0.14/+0.21 g cm-3. Despite its short orbital distance (0.0618 ± 0.0015 AU) and the age of the parent star (6.73 ± 2.8 Gyr), the planet orbit exhibits significantly non-zero eccentricity. This is very uncommon for this type of objects as tidal effects tend to circularise the orbit. This value is discussed taking into account the characteristics of the star and the observation accuracy. Aims: We report the discovery of CoRoT-16b, a low density hot jupiter that orbits a faint G5V star (mV = 15.63) in 5.3523 ± 0.0002 days with slight eccentricity. A fit of the data with no a priori assumptions on the orbit leads to an eccentricity of 0.33 ± 0.1. We discuss this value and also derive the mass and radius of the planet. Methods: We analyse the photometric transit curve of CoRoT-16 given by the CoRoT satellite, and radial velocity data from the HARPS and HIRES spectrometers. A combined analysis using a Markov chain Monte Carlo algorithm is used to get the system parameters. Results: CoRoT-16b is a 0.535 -0.083/+0.085 MJ, 1.17 -0.14/+0.16 RJ hot Jupiter with a density of 0.44 -0.14/+0.21 g cm-3. Despite its short orbital distance (0.0618 ± 0.0015 AU) and the age of the parent star (6.73 ± 2.8 Gyr), the planet orbit exhibits significantly non-zero eccentricity. This is very uncommon for this type of objects as tidal effects tend to circularise the orbit. This value is discussed taking into account the characteristics of the star and the observation accuracy. The CoRoT space mission, launched on December 27, 2006, has been developed and is operated by the CNES with the contribution of Austria, Belgium, Brasil, ESA, Germany, and Spain.Observations made with the HARPS spectrograph at ESO La Silla Observatory (HARPS programs 083.C-0186 and 184.C-0639) and the HIRES spectrograph at the Keck Observatory (NASA-Keck programs N035Hr, N143Hr and N095Hr).
Published: 2012
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17. Transiting exoplanets from the CoRoT space mission - XIX. CoRoT-23b: a dense hot Jupiter on an eccentric orbit

Author: Sz. Csizmadia, Aviv Ofir, Pierre Barge, C. Moutou, Michaël Gillon, M. Ollivier, Sylvio Ferraz-Mello, Roi Alonso, Rodrigo F. Díaz, B. Samuel, Tsevi Mazeh, Suzanne Aigrain, Jean Schneider, Alexandre Santerne, Heike Rauer, M. Havel, Anders Erikson, Helmut Lammer, G. Wuchterl, Aldo S. Bonomo, Didier Queloz, C. Cavarroc, Laurent Jorda, Antoine Llebaria, Daniel Rouan, Pascal Bordé, Davide Gandolfi, Rudolf Dvorak, Tristan Guillot, A. Léger, C. Lovis, Magali Deleuil, François Bouchy, Hannu Parviainen, Martin Pätzold, B. Tingley, M. Fridlund, Artie P. Hatzes, Annie Baglin, Guillaume Hébrard, Michel Auvergne, Juan Cabrera, Hans J. Deeg, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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 d'Astrophysique et de Géophysique [Liège], Université de Liège, Laboratoire des technologies de la microélectronique (LTM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln, Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), and Universität zu Köln = University of Cologne
Subjects: 010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], media_common.quotation_subject, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Orbital eccentricity, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, FOTOMETRIA, 01 natural sciences, techniques: spectroscopic – techniques: photometric – stars: fundamental parameters – planetary systems – techniques: radial velocities, Planet, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Eccentricity (behavior), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Subgiant, Astronomy and Astrophysics, Exoplanet, Radial velocity, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the detection of CoRoT-23b, a hot Jupiter transiting in front of its host star with a period of 3.6314 \pm 0.0001 days. This planet was discovered thanks to photometric data secured with the CoRoT satellite, combined with spectroscopic radial velocity (RV) measurements. A photometric search for possible background eclipsing binaries conducted at CFHT and OGS concluded with a very low risk of false positives. The usual techniques of combining RV and transit data simultaneously were used to derive stellar and planetary parameters. The planet has a mass of Mp = 2.8 \pm 0.3 MJup, a radius of Rpl = 1.05 \pm 0.13 RJup, a density of \approx 3 g cm-3. RV data also clearly reveal a non zero eccentricity of e = 0.16 \pm 0.02. The planet orbits a mature G0 main sequence star of V =15.5 mag, with a mass M\star = 1.14 \pm 0.08 M\odot, a radius R\star = 1. 61 \pm 0.18 R\odot and quasi-solar abundances. The age of the system is evaluated to be 7 Gyr, not far from the transition to subgiant, in agreement with the rather large stellar radius. The two features of a significant eccentricity of the orbit and of a fairly high density are fairly uncommon for a hot Jupiter. The high density is, however, consistent with a model of contraction of a planet at this mass, given the age of the system. On the other hand, at such an age, circularization is expected to be completed. In fact, we show that for this planetary mass and orbital distance, any initial eccentricity should not totally vanish after 7 Gyr, as long as the tidal quality factor Qp is more than a few 105, a value that is the lower bound of the usually expected range. Even if Corot-23b features a density and an eccentricity that are atypical of a hot Jupiter, it is thus not an enigmatic object., Astronomy & Astrophysics in press
Published: 2011
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18. Detection of small-size planetary candidates with CoRoT data

Author: Magali Deleuil, Pascal Bordé, P.-Y. Chabaud, Aldo S. Bonomo, Claire Moutou, 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), Sozzetti, A. and Lattanzi, M.~G. and Boss, and A.~P.
Subjects: Physics, Detection threshold, 010308 nuclear & particles physics, QC1-999, stars: late-type, Astronomy, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, methods: data analysis, Stars, techniques: photometric, Planet, Space and Planetary Science, 0103 physical sciences, Terrestrial planet, Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS
Abstract: With the discovery of CoRoT-7b, the first transiting super-Earth, the CoRoT space mission has shown the capability to detect short-period rocky planets around solar-like stars. By performing a blind test with real CoRoT light curves, we want to establish the detection threshold of small-size planets in CoRoT data. We investigate the main obstacles to the detection of transiting super-Earths in CoRoT data, notably the presence of short-time scale variability and hot pixels.
Published: 2011
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19. Transiting exoplanets from the CoRoT space mission.XVIII.CoRoT-18b: a massive hot Jupiter on a prograde, nearly aligned orbit

Author: M. Ollivier, C. Moutou, Suzanne Aigrain, Martin Pätzold, Pierre Barge, Michaël Gillon, M. Havel, Sz. Csizmadia, Juan Cabrera, G. Wuchterl, Hannu Parviainen, J. Schneider, Aviv Ofir, Helmut Lammer, Laurent Jorda, Annie Baglin, François Bouchy, B. Tingley, Alexandre Santerne, Ludmila Carone, Sylvio Ferraz-Mello, Thomas M. Evans, Davide Gandolfi, Roi Alonso, Rodrigo F. Díaz, E. W. Guenther, Anders Erikson, Artie P. Hatzes, Heike Rauer, Rudolf Dvorak, Tsevi Mazeh, S. Carpano, Didier Queloz, Guillaume Hébrard, Tristan Guillot, Aldo S. Bonomo, Malcolm Fridlund, Antoine Llebaria, Pascal Bordé, Hans J. Deeg, Neale P. Gibson, J. M. Almenara, Magali Deleuil, A. Léger, C. Cavarroc, Michel Auvergne, Daniel Rouan, 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), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Laboratoire des technologies de la microélectronique (LTM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln, Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), and Universität zu Köln = University of Cologne
Subjects: Rotation period, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Gyrochronology, 010303 astronomy & astrophysics, Stellar evolution, Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), Physics, 010308 nuclear & particles physics, planetary systems – techniques: spectroscopic – techniques: photometric – techniques: radial, Astronomy and Astrophysics, Exoplanet, Stars, 13. Climate action, Space and Planetary Science, Stellar physics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the detection of CoRoT-18b, a massive hot jupiter transiting in front of its host star with a period of 1.9000693 +/- 0.0000028 days. This planet was discovered thanks to photometric data secured with the CoRoT satellite combined with spectroscopic and photometric ground-based follow-up observations. The planet has a mass M_p = 3.47 +/- 0.38 M_Jup, a radius R_p = 1.31 +/- 0.18 R_Jup, and a density rho_p = 2.2 +/- 0.8 g/cm3. It orbits a G9V star with a mass M_* = 0.95 +/- 0.15 M_Sun, a radius R_* = 1.00 +/- 0.13 R_Sun, and a rotation period P_rot = 5.4 +/- 0.4 days. The age of the system remains uncertain, with stellar evolution models pointing either to a few tens Ma or several Ga, while gyrochronology and lithium abundance point towards ages of a few hundred Ma. This mismatch potentially points to a problem in our understanding of the evolution of young stars, with possibly significant implications for stellar physics and the interpretation of inferred sizes of exoplanets around young stars. We detected the Rossiter-McLaughlin anomaly in the CoRoT-18 system thanks to the spectroscopic observation of a transit. We measured the obliquity psi = 20 +/- 20 degrees (sky-projected value: lambda = -10 +/- 20 degrees), indicating that the planet orbits in the same way as the star is rotating and that this prograde orbit is nearly aligned with the stellar equator., 14 pages, 13 figures, 3 tables, A&A in press, final version
Published: 2011
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20. CoRoT LRa02_E2_0121: Neptune-size planet candidate turns into a hierarchical triple system with a giant primary

Author: Sylvio Ferraz-Mello, Tsevi Mazeh, Roi Alonso, Davide Gandolfi, A. Llebaria, Artie P. Hatzes, Aldo S. Bonomo, Magali Deleuil, Helmut Lammer, Pierre Barge, Laurent Jorda, Alexandre Santerne, M. Ollivier, Malcolm Fridlund, C. Moutou, Suzanne Aigrain, Martin Pätzold, G. Wuchterl, Y. Tsodikovich, Pascal Bordé, Anders Erikson, A. Léger, Rudolf Dvorak, Michaël Gillon, Hans J. Deeg, Lev Tal-Or, Didier Queloz, François Bouchy, E. W. Guenther, Tristan Guillot, Heike Rauer, Daniel Rouan, Michel Auvergne, 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), 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), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Laboratoire des technologies de la microélectronique (LTM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln, 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), Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), and Universität zu Köln = University of Cologne
Subjects: Triple system, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Binary number, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, techniques: photometric, Primary (astronomy), Neptune, Planet, 0103 physical sciences, MECÂNICA CELESTE, Astrophysics::Solar and Stellar Astrophysics, planetary systems, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Solar and Stellar Astrophysics (astro-ph.SR), Eclipse, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], techniques: radial velocities, binaries: eclipsing, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Orbit, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: This paper presents the case of CoRoT LRa02_E2_0121, which was initially classified as a Neptune-size transiting-planet candidate on a relatively wide orbit of 36.3 days. Follow-up observations were performed with UVES, Sandiford, SOPHIE and HARPS. These observations revealed a faint companion in the spectra. To find the true nature of the system we derived the radial velocities of the faint companion using TODMOR - a two-dimensional correlation technique, applied to the SOPHIE spectra. Modeling the lightcurve with EBAS we discovered a secondary eclipse with a depth of ~0.07%, indicating a diluted eclipsing binary. Combined MCMC modeling of the lightcurve and the radial velocities suggested that CoRoT LRa02_E2_0121 is a hierarchical triple system with an evolved G-type primary and an A-type:F-type grazing eclipsing binary. Such triple systems are difficult to discover., Comment: 7 pages, 5 figures
Published: 2011
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21. Exoplanet discoveries with the CoRoT space observatory

Author: Petr Kabath, David R. Ciardi, H. Ottacher, Hans J. Deeg, François Bouchy, Laurent Jorda, B. Samuel, A. P. Hatzes, Pascal Bordé, T. A. Lister, R. den Hartog, J. Weingrill, Pierre Barge, Willy Benz, M. Fridlund, C. Lovis, Magali Deleuil, Günther Wuchterl, Ludmila Carone, A. Llebaria, M. Steller, J. Hasiba, H. Bruntt, S. Carpano, A. Baglin, Rudolf Dvorak, M. Havel, A. Léger, Markus Rabus, Michel Mayor, Sylvio Ferraz-Mello, Eike W. Guenther, Roi Alonso, M. Hidas, Tsevi Mazeh, Stéphane Udry, Tristan Guillot, Daniel Rouan, Frederic Pont, Juan Cabrera, Aldo S. Bonomo, Brandon Tingley, Szilard Csizmadia, Jean Schneider, Avi Shporer, C. Moutou, Michaël Gillon, Anders Erikson, J.-C. Gazzano, Suzanne Aigrain, Martin Pätzold, Didier Queloz, Davide Gandolfi, Francesco Pepe, Alessandro Mura, Marc Ollivier, B. Stecklum, Rachel Street, Michel Auvergne, J. M. Almenara, G. Hebrard, Heike Rauer, P. Gondoin, Mauro Barbieri, Helmut Lammer, 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, Super-Earth, 010504 meteorology & atmospheric sciences, Brown dwarf, Astronomy, Astronomy and Astrophysics, Astrophysics, 7. Clean energy, 01 natural sciences, Exoplanet, CoRoT, Extrasolare Planten, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Hot Jupiter, Astrophysics::Solar and Stellar Astrophysics, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Transit (astronomy), 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Discoveries of exoplanets
Abstract: The CoRoT space observatory is a project which is led by the French space agency CNES and leading space research institutes in Austria, Brazil, Belgium, Germany and Spain and also the European Space Agency ESA. CoRoT observed since its launch in December 27, 2006 about 100 000 stars for the exoplanet channel, during 150 days uninterrupted high-precision photometry. Since the The CoRoT-team has several exoplanet candidates which are currently analyzed under its study, we report here the discoveries of nine exoplanets which were observed by CoRoT. Discovered exoplanets such as CoRoT-3b populate the brown dwarf desert and close the gap of measured physical properties between usual gas giants and very low mass stars. CoRoT discoveries extended the known range of planet masses down to about 4.8 Earth-masses (CoRoT-7b) and up to 21 Jupiter masses (CoRoT-3b), the radii to about 1.68 × 0.09 REarth (CoRoT-7b) and up to the most inflated hot Jupiter with 1.49 × 0.09 REarth found so far (CoRoT-1b), and the transiting exoplanet with the longest period of 95.274 days (CoRoT-9b). Giant exoplanets have been detected at low metallicity, rapidly rotating and active, spotted stars. Two CoRoT planets have host stars with the lowest content of heavy elements known to show a transit hinting towards a different planethost-star-metallicity relation then the one found by radial-velocity search programs. Finally the properties of the CoRoT-7b prove that rocky planets with a density close to Earth exist outside the Solar System. Finally the detection of the secondary transit of CoRoT-1b at a sensitivity level of 10-5 and the very clear detection of the "super-Earth" CoRoT-7b at 3.5 × 10-4 relative flux are promising evidence that the space observatory is being able to detect even smaller exoplanets with the size of the Earth. © 2010 Pleiades Publishing, Ltd.
Published: 2010
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22. Transiting exoplanets from the CoRoT space mission XIV. CoRoT-11b: a transiting massive 'hot-Jupiter' in a prograde orbit around a rapidly rotating F-type star

Author: Sz. Csizmadia, P. Eigmüller, Michael Endl, M. Fridlund, Suzanne Aigrain, François Bouchy, Annie Baglin, Artie P. Hatzes, M. Ollivier, H. Bruntt, William D. Cochran, Sylvio Ferraz-Mello, Tsevi Mazeh, Didier Queloz, B. Samuel, P. Gondoin, M. Havel, C. Moutou, Roi Alonso, G. Wuchterl, Petr Kabath, Tristan Guillot, Michaël Gillon, Aldo S. Bonomo, Hans J. Deeg, Martin Pätzold, Daniel Rouan, Antoine Llebaria, Neale P. Gibson, Jochen Eislöffel, S. Carpano, Rudolf Dvorak, Jean Schneider, J. C. Gazzano, Michel Mayor, Pascal Bordé, Pierre Barge, Heike Rauer, Helmut Lammer, Anders Erikson, M. Hartmann, A. Léger, Laurent Jorda, Magali Deleuil, Juan Cabrera, Phillip J. MacQueen, Ludmila Carone, E. W. Guenther, Guillaume Hébrard, B. Stecklum, Michel Auvergne, Stéphane Udry, Brandon Tingley, Francesco Pepe, Davide Gandolfi, 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: Dwarf star, planetary systems, techniques: photometric, techniques: radial velocities, techniques: spectroscopic, Astronomy and Astrophysics, Space and Planetary Science, Extrasolare Planeten, FOS: Physical sciences, Photometrie, Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Hot Jupiter, 010306 general physics, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), Physics, Orbital period, Radialgeschwindigkeit, Exoplanet, Radial velocity, Stars, 13. Climate action, Planetary mass, Astrophysics - Earth and Planetary Astrophysics
Abstract: The CoRoT exoplanet science team announces the discovery of CoRoT-11b, a fairly massive hot-Jupiter transiting a V=12.9 mag F6 dwarf star (M*=1.27 +/- 0.05 Msun, R*=1.37 +/- 0.03 Rsun, Teff=6440 +/- 120 K), with an orbital period of P=2.994329 +/- 0.000011 days and semi-major axis a=0.0436 +/- 0.005 AU. The detection of part of the radial velocity anomaly caused by the Rossiter-McLaughlin effect shows that the transit-like events detected by CoRoT are caused by a planet-sized transiting object in a prograde orbit. The relatively high projected rotational velocity of the star (vsini=40+/-5 km/s) places CoRoT-11 among the most rapidly rotating planet host stars discovered so far. With a planetary mass of mp=2.33+/-0.34 Mjup and radius rp=1.43+/-0.03 Rjup, the resulting mean density of CoRoT-11b (rho=0.99+/-0.15 g/cm^3) can be explained with a model for an inflated hydrogen-planet with a solar composition and a high level of energy dissipation in its interior., Comment: 15 pages, 13 figures, accepted for publication in A&A
Published: 2010
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23. A transiting giant planet with a temperature between 250 K and 430 K

Author: Daniel Rouan, Günther Wuchterl, Pierre Barge, C. Lovis, Magali Deleuil, Frederic Pont, Sylvio Ferraz-Mello, François Bouchy, J. M. Almenara, David R. Ciardi, Roi Alonso, Jean Schneider, S. Carpano, Stéphane Udry, Sz. Csizmadia, Avi Shporer, T. A. Lister, G. Hebrard, Brandon Tingley, A. Baglin, Ludmila Carone, Rudolf Dvorak, Hans J. Deeg, A. P. Hatzes, P. Gondoin, M. Hidas, R. den Hartog, M. Havel, Petr Kabath, J. Weingrill, M. Fridlund, Laurent Jorda, H. Bruntt, Michaël Gillon, Anders Erikson, Willy Benz, Juan Cabrera, Eike W. Guenther, J.-C. Gazzano, Tsevi Mazeh, Marc Ollivier, Suzanne Aigrain, A. Léger, Markus Rabus, D. Queloz, Mauro Barbieri, Helmut Lammer, B. Stecklum, Tristan Guillot, Aldo S. Bonomo, A. Llebaria, Rachel Street, Michel Mayor, Heike Rauer, C. Moutou, Martin Pätzold, M. Auvergne, Francesco Pepe, Davide Gandolfi, Pascal Bordé, B. Samuel, 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, Multidisciplinary, 010504 meteorology & atmospheric sciences, Giant planet, Astronomy, Astrophysics, 01 natural sciences, Exoplanet, 13. Climate action, Planet, extrasolare Planeten - Transitmethode - CoRoT 9b, 0103 physical sciences, Terrestrial planet, Astrophysics::Solar and Stellar Astrophysics, Kepler-62, Astrophysics::Earth and Planetary Astrophysics, Primary atmosphere, 010303 astronomy & astrophysics, Planetary mass, 0105 earth and related environmental sciences, Discoveries of exoplanets
Abstract: Of the over 400 known1 exoplanets, there are about 70 planets that transit their central star, a situation that permits the derivation of their basic parameters and facilitates investigations of their atmospheres. Some short-period planets2, including the first terrestrial exoplanet3,4 (CoRoT-7b), have been discovered using a space mission5 designed to find smaller and more distant planets than can be seen from the ground. Here we report transit observations of CoRoT-9b, which orbits with a period of 95.274 days on a low eccentricity of 0.11 ± 0.04 around a solar-like star. Its periastron distance of 0.36 astronomical units is by far the largest of all transiting planets, yielding a ‘temperate’ photospheric temperature estimated to be between 250 and 430 K. Unlike previously known transiting planets, the present size of CoRoT-9b should not have been affected by tidal heat dissipation processes. Indeed, the planet is found to be well described by standard evolution models6 with an inferred interior composition consistent with that of Jupiter and Saturn.
Published: 2010
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24. Transiting exoplanets from the CoRoT space mission. XI. CoRoT-8b: a hot and dense sub-Saturn around a K1 dwarf

Author: C. Moutou, J. Weingrill, Michaël Gillon, C. Lovis, Magali Deleuil, Pascal Bordé, Suzanne Aigrain, François Bouchy, Michel Mayor, Aldo S. Bonomo, Szilard Csizmadia, Alexandre Santerne, Ludmila Carone, Anders Erikson, Willy Benz, B. Samuel, Pierre Barge, Brandon Tingley, E. W. Guenther, P. Guterman, Juan Cabrera, Daniel Rouan, Tsevi Mazeh, S. Carpano, J. C. Gazzano, J. M. Almenara, Martin Pätzold, Francesco Pepe, Davide Gandolfi, Annie Baglin, M. Fridlund, Artie P. Hatzes, H. Bruntt, Guillaume Hébrard, Rudolf Dvorak, Marc Ollivier, Michel Auvergne, Stéphane Udry, Jean Schneider, Heike Rauer, Sylvio Ferraz-Mello, Roi Alonso, Didier Queloz, Tristan Guillot, Hans J. Deeg, Helmut Lammer, Laurent Jorda, A. Léger, M. Havel, 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: Physics, Orbital elements, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Extrasolare Planeten, FOS: Physical sciences, Astronomy and Astrophysics, Photometrie, Radius, Astrophysics, Radialgeschwindigkeit, 01 natural sciences, Exoplanet, Radial velocity, 13. Climate action, Space and Planetary Science, Neptune, Saturn, 0103 physical sciences, Transit (astronomy), Circular orbit, Detektion, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics - Earth and Planetary Astrophysics
Abstract: We report the discovery of CoRoT-8b, a dense small Saturn-class exoplanet that orbits a K1 dwarf in 6.2 days, and we derive its orbital parameters, mass, and radius. We analyzed two complementary data sets: the photometric transit curve of CoRoT-8b as measured by CoRoT and the radial velocity curve of CoRoT-8 as measured by the HARPS spectrometer. We find that CoRoT-8b is on a circular orbit with a semi-major axis of 0.063 +/- 0.001 AU. It has a radius of 0.57 +/- 0.02 RJ, a mass of 0.22 +/- 0.03 MJ, and therefore a mean density 1.6 +/- 0.1 g/cm^3. With 67 % of the size of Saturn and 72 % of its mass, CoRoT-8b has a density comparable to that of Neptune (1.76 g/cm^3). We estimate its content in heavy elements to be 47-63 Earth masses, and the mass of its hydrogen-helium envelope to be 7-23 Earth masses. At 0.063 AU, the thermal loss of hydrogen of CoRoT-8b should be no more than about 0.1 % over an assumed integrated lifetime of 3~Ga., Comment: 10 pages, 12 figures, accepted for publication in A&A
Published: 2010
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25. Transit timing analysis of CoRoT-1b

Author: Günther Wuchterl, Pascal Bordé, Eric Agol, Juan Cabrera, Eike W. Guenther, Davide Gandolfi, François Bouchy, Tristan Guillot, A. P. Hatzes, M. Fridlund, C. Lázaro, Laurent Jorda, Hans J. Deeg, Rudolf Dvorak, A. Llebaria, C. Moutou, Pierre Barge, Martin Pätzold, R. de la Reza, Marc Ollivier, D. Queloz, Helmut Lammer, Anders Erikson, Pierre Magain, A. Léger, Szilard Csizmadia, Stefan Renner, Heike Rauer, Jean Schneider, P Gondoin, Magali Deleuil, Suzanne Aigrain, Daniel Rouan, J. M. Almenara, Roi Alonso, Aldo S. Bonomo, 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, FOS: Physical sciences, Context (language use), Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, numerical methods, occultations, Transit (astronomy), 010303 astronomy & astrophysics, planetary systems, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Earth and Planetary Astrophysics (astro-ph.EP), Physics, photometric techniques, Astronomy and Astrophysics, Planetary system, Light curve, Orbital period, Earth mass, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Trojan, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: CoRoT, the pioneer space-based transit search, steadily provides thousands of high-precision light curves with continuous time sampling over periods of up to 5 months. The transits of a planet perturbed by an additional object are not strictly periodic. By studying the transit timing variations (TTVs), additional objects can be detected in the system. A transit timing analysis of CoRoT-1b is carried out to constrain the existence of additional planets in the system. We used data obtained by an improved version of the CoRoT data pipeline (version 2.0). Individual transits were fitted to determine the mid-transit times, and we analyzed the derived $O-C$ diagram. N-body integrations were used to place limits on secondary planets. No periodic timing variations with a period shorter than the observational window (55 days) are found. The presence of an Earth-mass Trojan is not likely. A planet of mass greater than $\sim 1$ Earth mass can be ruled out by the present data if the object is in a 2:1 (exterior) mean motion resonance with CoRoT-1b. Considering initially circular orbits: (i) super-Earths (less than 10 Earth-masses) are excluded for periods less than about 3.5 days, (ii) Saturn-like planets can be ruled out for periods less than about 5 days, (iii) Jupiter-like planets should have a minimum orbital period of about 6.5 days., 6 pages, accepted at A&A
Published: 2010
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26. Noise properties of the CoRoT data: a planet-finding perspective

Author: P. Gondoin, Helmut Lammer, M. Auvergne, Anders Erikson, Heike Rauer, M. Fridlund, Shay Zucker, P. Guterman, D. Rouan, Pierre Magain, A. Alapini, Francois Fressin, Suzanne Aigrain, Roi Alonso, Laurent Jorda, Rudolf Dvorak, Didier Queloz, Marc Ollivier, Antoine Llebaria, M. Barbieri, G. Wuchter, Pascal Bordé, Martin Pätzold, R. de la Reza, François Bouchy, Jean Schneider, Tsevi Mazeh, Pierre Barge, A. Léger, C. Moutou, Hans J. Deeg, Frederic Pont, Magali Deleuil, University of Exeter, Harvard-Smithsonian Center for Astrophysics, 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 (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, Tel Aviv University (TAU), 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 Thüringer Landessternwarte, Tautenburg Observatory
Subjects: noise, photometry, Population, transit search, FOS: Physical sciences, Astrophysics, Filter (large eddy simulation), Planet, Astrophysics::Solar and Stellar Astrophysics, education, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), education.field_of_study, Astronomy and Astrophysics, Planetary system, Light curve, CoRoT, Stars, Astrophysics - Solar and Stellar Astrophysics, exoplanets, Space and Planetary Science, transit method, Magnitude (astronomy), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Noise (radio), Astrophysics - Earth and Planetary Astrophysics
Abstract: In this short paper, we study the photometric precision of stellar light curves obtained by the CoRoT satellite in its planet finding channel, with a particular emphasis on the timescales characteristic of planetary transits. Together with other articles in the same issue of this journal, it forms an attempt to provide the building blocks for a statistical interpretation of the CoRoT planet and eclipsing binary catch to date. After pre-processing the light curves so as to minimise long-term variations and outliers, we measure the scatter of the light curves in the first three CoRoT runs lasting more than 1 month, using an iterative non-linear filter to isolate signal on the timescales of interest. The bevhaiour of the noise on 2h timescales is well-described a power-law with index 0.25 in R-magnitude, ranging from 0.1mmag at R=11.5 to 1mmag at R=16, which is close to the pre-launch specification, though still a factor 2-3 above the photon noise due to residual jitter noise and hot pixel events. There is evidence for a slight degradation of the performance over time. We find clear evidence for enhanced variability on hours timescales (at the level of 0.5 mmag) in stars identified as likely giants from their R-magnitude and B-V colour, which represent approximately 60 and 20% of the observed population in the direction of Aquila and Monoceros respectively. On the other hand, median correlated noise levels over 2h for dwarf stars are extremely low, reaching 0.05mmag at the bright end., Comment: 5 pages, 4 figures, accepted for publication in A&A
Published: 2009
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27. Modelling solar-like variability for the detection of Earth-like planetary transits II. Performance of the three-spot modelling, harmonic function fitting, iterative nonlinear filtering, and sliding boxcar filtering

Author: Suzanne Aigrain, Aldo S. Bonomo, Pascal Bordé, and A. F. Lanza
Subjects: Physics, Monte Carlo method, Astrophysics (astro-ph), Shot noise, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Filter (signal processing), Solar irradiance, Light curve, 01 natural sciences, Pulse shaping, Space and Planetary Science, 0103 physical sciences, Harmonic, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Algorithm
Abstract: We present a comparison of four methods of filtering solar-like variability to increase the efficiency of detection of Earth-like planetary transits by means of box-shaped transit finder algorithms. Two of these filtering methods are the harmonic fitting method and the iterative non-linear filter that, coupled respectively with the Box Least-Square (BLS) and Box Maximum-Likelihood algorithms, demonstrated the best performance during the first detection blind test organized inside the CoRoT consortium. The third method, the 3-spot model, is a simplified physical model of Sun-like variability and the fourth is a simple sliding boxcar filter. We apply a Monte Carlo approach by simulating a large number of 150-day light curves (as for CoRoT long runs) for different planetary radii, orbital periods, epochs of the first transit and standard deviations of the photon shot noise. Stellar variability is given by the Total Solar Irradiance variations as observed close to the maximum of solar cycle 23. After filtering solar variability, transits are searched for by means of the BLS algorithm. We find that the iterative non-linear filter is the best method to filter light curves of solar-like stars when a suitable window can be chosen. As the performance of this filter depends critically on the length of its window, we point out that the window must be as long as possible, according to the magnetic activity level of the star. We show an automatic method to choose the extension of the filter window from the power spectrum of the light curves. The iterative non-linear filter, when used with a suitable choice of its window, has a better performance than more complicated and computationally intensive methods of fitting solar-like variability, like the 200-harmonic fitting or the 3-spot model., Comment: accepted by A&A
Published: 2009

28. The CoRoT-7 planetary system: two orbiting super-Earths

Author: François Bouchy, Marc Ollivier, Davide Gandolfi, Pierre Barge, S. Ferraz Mello, Jean Schneider, C. Moutou, M. Fridlund, Michaël Gillon, Anders Erikson, Eike W. Guenther, Pierre Magain, Roi Alonso, A. P. Hatzes, Guillaume Hébrard, Stéphane Udry, Tristan Guillot, A. Baglin, Rudolf Dvorak, Willy Benz, Michel Mayor, Daniel Rouan, Didier Queloz, C. Lovis, Damien Ségransan, Günther Wuchterl, Hans J. Deeg, M. Auvergne, Francesco Pepe, M. Hartmann, Laurent Jorda, A. Léger, Helmut Lammer, Heike Rauer, Antoine Llebaria, Pascal Bordé, Martin Pätzold, Tsevi Mazeh, M. Barbieri, Magali Deleuil, 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: Rotation period, 010504 meteorology & atmospheric sciences, photometry, Astrophysics, 01 natural sciences, 7. Clean energy, Planet, Neptune, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Circular orbit, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Starspot, Astronomy, Astronomy and Astrophysics, Planetary system, Radial velocity, CoRoT, Amplitude, exoplanets, 13. Climate action, Space and Planetary Science, transit method, terrestrial planets, CoRoT-7, Astrophysics::Earth and Planetary Astrophysics, super-Earth
Abstract: We report on an intensive observational campaign carried out with HARPS at the 3.6 m telescope at La Silla on the star CoRoT-7. Additional simultaneous photometric measurements carried out with the Euler Swiss telescope have demonstrated that the observed radial velocity variations are dominated by rotational modulation from cool spots on the stellar surface. Several approaches were used to extract the radial velocity signal of the planet(s) from the stellar activity signal. First, a simple pre-whitening procedure was employed to find and subsequently remove periodic signals from the complex frequency structure of the radial velocity data. The dominant frequency in the power spectrum was found at 23 days, which corresponds to the rotation period of CoRoT-7. The 0.8535 day period of CoRoT-7b planetary candidate was detected with an amplitude of 3.3 m s −1 . Most other frequencies, some with amplitudes larger than the CoRoT-7b signal, are most likely associated with activity. A second approach used harmonic decomposition of the rotational period and up to the first three harmonics to filter out the activity signal from radial velocity variations caused by orbiting planets. After correcting the radial velocity data for activity, two periodic signals are detected: the CoRoT-7b transit period and a second one with a period of 3.69 days and an amplitude of 4 m s −1 . This second signal was also found in the pre-whitening analysis. We attribute the second signal to a second, more remote planet CoRoT-7c . The orbital solution of both planets is compatible with circular orbits. The mass of CoRoT-7b is 4.8 ± 0. 8( M⊕) and that of CoRoT-7c is 8.4 ± 0. 9( M⊕), assuming both planets are on coplanar orbits. We also investigated the false positive scenario of a blend by a faint stellar binary, and this may be rejected by the stability of the bisector on a nightly scale. According to their masses both planets belong to the super-Earth planet category. The average density of CoRoT-7b is ρ = 5.6 ± 1. 3gc m −3 , similar to the Earth. The CoRoT-7 planetary system provides us with the first insight into the physical nature of short period super-Earth planets recently detected by radial velocity surveys. These planets may be denser than Neptune and therefore likely made of rocks like the Earth, or a mix of water ice and rocks.
Published: 2009
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29. Transiting exoplanets from the CoRoT space mission I - CoRoT-Exo-1b: a low-density short-period planet around a G0V star

Author: J. M. Almenara, M. Ollivier, Michaël Gillon, Annie Baglin, Anders Erikson, Heike Rauer, Tsevi Mazeh, Pierre Magain, Suzanne Aigrain, Didier Queloz, Malcolm Fridlund, Antoine Llebaria, Pascal Bordé, Tristan Guillot, C. Moutou, B. Loeillet, Guillaume Hébrard, Martin Pätzold, R. de la Reza, J. Schneider, Rudolf Dvorak, Artie P. Hatzes, A. Léger, Pierre Barge, Daniel Rouan, G. Wuchterl, Frederic Pont, M. Barbieri, Avi Shporer, Magali Deleuil, P. Gondoin, Roi Alonso, Petr Kabath, Helmut Lammer, Laurent Jorda, Hans J. Deeg, François Bouchy, Michel Auvergne, 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 (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), DLR Institute of Planetary Research, German Aerospace Center (DLR), 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), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, School of Physics, University of Exeter, Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Instituto de Astrofisica de Canarias (IAC), 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), Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), ON/MCT (ON/MCT, 20921-030, Rio de Janeiro, Brazil)), ON/MCT, 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), Geneva Observatory, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), 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), Thüringer Landessternwarte Tautenburg (TLS), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), 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), European Southern Observatory (ESO), Institute for Geophysics and Meteorology [Köln] (IGM), University of Cologne, Observatoire de Paris - Site de Paris (OP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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 Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université de Genève (UNIGE), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), European Space Agency (ESA)-European Space Agency (ESA), University of Geneva [Switzerland], Université Nice Sophia Antipolis (... - 2019) (UNS), School of Physics and Astronomy [Tel Aviv], Tel Aviv University [Tel Aviv], Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - 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, Institute of Planetary Research, Deutsches Zentrum für Luft- und Raumfahrt (DLR), 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 Astronomique de l'Université de Genève, Instituto de Astrofísica de Canarias (IAC), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatório Nacional/MCTI, Institut für Astronomie, Universität Wien (IfA), Research and Scientific Support Department, ESA-ESTEC (RSSD), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Thüringer Landessternwarte, Tautenburg Observatory, Institut für Weltraumforschung, Österreichische Akademie der Wissenschaften (IWF), University of Liège, Tel Aviv University (TAU), Rheinisches Institut für Umweltforschung an der Universität zu Köln (RIU), 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), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Department of Palaeontology - Institute of Geology, Bergakademie Freiberg, PSL Research University (PSL)-PSL Research University (PSL), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), and Beaussier, Catherine
Subjects: transits, photometry, FOS: Physical sciences, Astrophysics, 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Planet, 0103 physical sciences, 010303 astronomy & astrophysics, Orbital elements, Physics, 010308 nuclear & particles physics, Astrophysics (astro-ph), Exo-1b, Astronomy and Astrophysics, Radius, Orbital period, Light curve, Exoplanet, CoRoT, Stars, exoplanets, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Planetary mass
Abstract: Context. The pioneer space mission for photometric planet searches, CoRoT, steadily monitors about 12,000 stars in each of its fields of view; it is able to detect transit candidates early in the processing of the data and before the end of a run. Aims. We report the detection of the first planet discovered by CoRoT and characterizing it with the help of follow-up observations. Methods. Raw data were filtered from outliers and residuals at the orbital period of the satellite. The orbital parameters and the radius of the planet were estimated by best fitting the phase folded light curve with 34 successive transits. Doppler measurements with the SOPHIE spectrograph permitted us to secure the detection and to estimate the planet mass. Results. The accuracy of the data is very high with a dispersion in the 2.17 min binned phase-folded light curve that does not exceed 3.10-4 in flux unit. The planet orbits a mildly metal-poor G0V star of magnitude V=13.6 in 1.5 days. The estimated mass and radius of the star are 0.95+-0.15Msun and 1.11+-0.05Rsun. We find the planet has a radius of 1.49+-0.08Rjup, a mass of 1.03+-0.12Mjup, and a particularly low mean density of 0.38 +-0.05g cm-3., A&A letters (in press) - 4 pages - 3 figures
Published: 2008
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30. Speckle noise reduction techniques for high-dynamic range imaging

Author: Pascal Bordé and Wesley A. Traub
Subjects: Physics, Wavefront, business.industry, Astrophysics (astro-ph), General Engineering, Astrophysics::Instrumentation and Methods for Astrophysics, Energy Engineering and Power Technology, FOS: Physical sciences, Physics::Optics, Speckle noise, Image plane, Astrophysics, Deformable mirror, law.invention, Speckle pattern, Optics, Computer Science::Graphics, High-dynamic-range imaging, law, business, Adaptive optics, Coronagraph
Abstract: High-dynamic range imaging from space in the visible, aiming in particular at the detection of terrestrial exoplanets, necessitates not only the use of a coronagraph, but also of adaptive optics to correct optical defects in real time. Indeed, these defects scatter light and give birth to speckles in the image plane. Speckles can be cancelled by driving a deformable mirror to measure and compensate wavefront aberrations. In a first approach, targeted speckle nulling, speckles are cancelled iteratively by starting with the brightest ones. This first method has demonstrated a contrast better than 1e9 in laboratory. In a second approach, zonal speckle nulling, the total energy of speckles is minimized in a given zone of the image plane. This second method has the advantage to tackle simultaneously all speckles from the targeted zone, but it still needs better experimental demonstration., 7 pages, 3 figures, in Optical techniques for direct imaging of exoplanets (a special issue of Comptes Rendus de Physique)
Published: 2007

31. Could we identify hot Ocean-Planets with CoRoT, Kepler and Doppler velocimetry?

Author: A. Léger, C. Moutou, François Bouchy, Marc Ollivier, Pierre Barge, F. Brachet, Pascal Bordé, Helmut Lammer, D. Despois, M. Decaudin, James F. Kasting, Franck Selsis, Jean-Mathias Grießmeier, David Ehrenreich, Christophe Sotin, Olivier Grasset, B. Chazelas, Dimitri Mawet, Magali Deleuil, Laboratoire de Planétologie et Géodynamique [UMR 6112] (LPG), Université d'Angers (UA)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire aquitain des sciences de l'univers (OASU), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: FOS: Physical sciences, Astrophysics, 01 natural sciences, Astrobiology, Physics::Geophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Kepler-47, [SDU.STU.PL]Sciences of the Universe [physics]/Earth Sciences/Planetology, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Kepler-62, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Astrophysics::Galaxy Astrophysics, Physics::Atmospheric and Oceanic Physics, Planetary migration, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Astronomy, Astronomy and Astrophysics, Planetary system, Habitability of orange dwarf systems, 13. Climate action, Space and Planetary Science, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Planetary mass
Abstract: Planets less massive than about 10 MEarth are expected to have no massive H-He atmosphere and a cometary composition (50% rocks, 50% water, by mass) provided they formed beyond the snowline of protoplanetary disks. Due to inward migration, such planets could be found at any distance between their formation site and the star. If migration stops within the habitable zone, this will produce a new kind of planets, called Ocean-Planets. Ocean-planets typically consist in a silicate core, surrounded by a thick ice mantle, itself covered by a 100 km deep ocean. The existence of ocean-planets raises important astrobiological questions: Can life originate on such body, in the absence of continent and ocean-silicate interfaces? What would be the nature of the atmosphere and the geochemical cycles ? In this work, we address the fate of Hot Ocean-Planets produced when migration ends at a closer distance. In this case the liquid/gas interface can disappear, and the hot H2O envelope is made of a supercritical fluid. Although we do not expect these bodies to harbor life, their detection and identification as water-rich planets would give us insight as to the abundance of hot and, by extrapolation, cool Ocean-Planets., 47 pages, 6 Fugures, regular paper. Submitted to Icarus
Published: 2007
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32. Speckle nulling for exoplanet detection with space-based coronagraphic telescopes

Author: Wesley A. Traub, Andreas Kuhnert, Pascal Bordé, Brian Kern, and John T. Trauger
Subjects: Physics, business.industry, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Speckle noise, Astrophysics, Deformable mirror, Exoplanet, law.invention, Telescope, Speckle pattern, Optics, law, Planet, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, business, Coronagraph, Noise (radio)
Abstract: To detect Earth-like planets in the visible with a coronagraphic telescope, two major noise sources have to be overcome: the photon noise of the diffracted star light, and the speckle noise due to the star light scattered by instrumental defects. Coronagraphs tackle only the photon noise contribution. In order to decrease the speckle noise below the planet level, an active control of the wave front is required. We have developed analytical methods to measure and correct the speckle noise behind a coronagraph with a deformable mirror. In this paper, we summarize these methods, present numerical simulations, and discuss preliminary experimental results obtained with the High-Contrast Imaging Testbed at NASA's Jet Propulsion Laboratory., 6 pages, 4 figures. This paper will be published in the proceedings of the conference Space Telescopes and Instrumentation I: Optical, Infrared, and Millimeter (SPIE 6265), part of SPIE's Astronomical Telescopes & Instrumentation, 24-31 May 2006, Orlando, FL
Published: 2006

33. Is Arcturus a well-understood K giant? Test of model atmospheres and potential companion detection by near-infrared interferometry

Author: S. T. Ridgway, Christoffel Waelkens, Tijl Verhoelst, Marc G. Lacasse, Kjell Eriksson, Leen Decin, P. A. Schuller, Pascal Bordé, Wesley A. Traub, Guy Perrin, Rafael Millan-Gabet, Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, 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, Harvard-Smithsonian Center for Astrophysics, Institute for Astronomy and Space Physics, and National Optical Astronomy Observatory, Tucson (NOAO)
Subjects: water-vapor, variables, FOS: Physical sciences, spectral irradiance calibration, Astrophysics, Star (graph theory), confirmation, Single star, Spherical model, Arcturus, instrument, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, atmospheres [stars], Physics, individual : arcturus [stars], Near-infrared spectroscopy, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, cool-star atmospheres, iota interferometer, interferometric [techniques], iso-sws calibration, long-period, Interferometry, Wavelength, Space and Planetary Science, radial-velocity, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], binaries : general [stars]
Abstract: We present near-IR interferometric measurements of the K1.5 giant Arcturus (alpha Bootis), obtained at the IOTA interferometer with the FLUOR instrument, in four narrow filters with central wavelengths ranging from 2.03 to 2.39 micron. These observations were expected to allow us to quantify the wavelength dependence of the diameter of a typical K giant. They are compared to predictions from both plane-parallel and spherical model atmospheres. Unexpectedly, neither can explain the observed visibilities. We show how these data suggest the presence of a companion, in accordance with the Hipparcos data on this star, and discuss this solution with respect to Arcturus' single star status., Comment: 15 pages, 14 figures, accepted for publication by Astronomy & Astrophysics
Published: 2005
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34. Speckle nulling with space-based coronagraphs

Author: Wesley A. Traub and Pascal Bordé
Subjects: Wavefront, business.industry, Computer science, Fast Fourier transform, Detector, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Speckle noise, Astrophysics, Deformable mirror, law.invention, Speckle pattern, Cardinal point, Optics, Space and Planetary Science, law, business, Coronagraph
Abstract: Following the tracks of Malbet, Yu, & Shao (1995} on dark hole algorithms, we present analytical methods to measure and correct the speckle noise behind an ideal coronagraph. We show that, in a low aberration regime, wavefront sensing can be accomplished with only three images, the next image being fully corrected (no iterative process needed). The only hardware required is the coronagraph deformable mirror and an imaging detector in the focal plane, thus there are no non-common path errors to correct. Our first method, speckle field nulling, is a fast FFT-based algorithm requiring the deformable mirror influence functions to have identical shapes. Our second method, speckle energy minimization is more general and based on matrix inversion. Numerical simulations show that these methods can improve the contrast by several orders of magnitude., 6 pages, 5 figures, to appear in the Proceedings of IAUC 200, Direct Imaging of Exoplanets: Science & Techniques, October 3-7, 2005, Nice, France
Published: 2005
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35. Catalog of reference stars for long baseline stellar interferometry

Author: Pascal Bordé, Guy Perrin, Vincent Coudé du Foresto, G. Chagnon, arXiv, Import, Wesley A. Traub, 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, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Physics, media_common.quotation_subject, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Function (mathematics), 01 natural sciences, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars, Interferometry, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Sky, 0103 physical sciences, Astronomical interferometer, Calibration, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Visibility, Baseline (configuration management), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common
Abstract: The calibration process of long baseline stellar interferometers requires the use of reference stars with accurately determined angular diameters. We present a catalog of 374 carefully chosen stars among the all-sky network of infrared sources provided by Cohen et al. 1999. The catalog benefits from a very good sky coverage and a median formal error on the angular diameters of only 1.2%. Besides, its groups together in a homogeneous handy set stellar coordinates, uniform and limb-darkened angular diameters, photometric measurements, and other parameters relevant to optical interferometry. In this paper, we describe the selection criteria applied to qualify stars as reference sources. Then, we discuss the catalog's statistical properties such as the sky coverage or the distributions of magnitudes and angular diameters. We study the number of available reference stars as a function of the baseline and the precision needed on the visibility measurements. Finally, we compare the angular diameters predicted in Cohen et al. 1999 with existing determinations in the literature, and find a very good agreement., Comment: Conference "Interferometry for Optical Astronomy II", SPIE 2002
Published: 2003
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36. Exoplanet detection capability of the COROT space mission

Author: A. Léger, Pascal Bordé, Daniel Rouan, 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), 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), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and arXiv, Import
Subjects: 010504 meteorology & atmospheric sciences, Stellar population, FOS: Physical sciences, Astrophysics, 01 natural sciences, Jupiter, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Observatory, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Galaxy, Exoplanet, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, Magnitude (astronomy), Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics
Abstract: COROT will be the first high precision photometric satellite to be launched with the aim of detecting exoplanets by the transit method. In this paper, we present the simulations we have carried out in order to assess the detection capability of COROT. Using the model of stellar population synthesis of the Galaxy developed at Besancon Observatory (Robin & Creze 1986) and a simple cross-correlation technique (Borde et al. 2001), we find that COROT has the capacity to detect numerous exoplanets, not only Jupiter and Uranus-class ones, but also hot terrestrial planets, if they exist. We show that small exoplanets should be mainly gathered around 14-15th magnitude K2-M2 dwarfs and giant exoplanets around 15-16th magnitude F7-G2 dwarfs. We study the effect of crowding and the impact of a high stellar variability noise that both reduce the detection capability of the instrument., 8 pages, 7 figures, accepted by A&A
Published: 2003

37. 10 um wavefront spatial filtering: first results with chalcogenide fibers

Author: Pierre-Ivan Raynal, Thanh Nguyen, Guy Perrin, Pascal Bordé, Christophe Daussy, Anne Amy-Klein, Alain Léger, Gwenael Maze, 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 de Physique des Lasers (LPL), Université Paris 13 (UP13)-Centre National de la Recherche Scientifique (CNRS), 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), Wesley A. Traub, 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), and arXiv, Import
Subjects: Chalcogenide, FOS: Physical sciences, Astrophysics, 01 natural sciences, 010309 optics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], chemistry.chemical_compound, Quality (physics), Optics, 0103 physical sciences, Calibration, 010303 astronomy & astrophysics, Physics, Wavefront, Spatial filter, MIDI, business.industry, Astrophysics (astro-ph), computer.file_format, Interferometry, chemistry, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Darwin (spacecraft), business, computer
Abstract: Wavefront cleaning by single-mode fibers has proved to be efficient in optical-infrared interferometry to improve calibration quality. For instance, the FLUOR instrument has demonstrated the capability of fluoride glass single-mode fibers in this respect in the K and L bands. New interferometric instruments developped for the mid-infrared require the same capability for the 8-12 um range. We have initiated a program to develop single-mode fibers in the prospect of the VLTI mid-infrared instrument MIDI and of the ESA/DARWIN and NASA/TPF missions that require excellent wavefront quality. In order to characterize the performances of chalcogenide fibers we are developping, we have set up an experiment to measure the far-field pattern radiated at 10 um. In this paper, we report the first and promising results obtained with this new component., Comment: Conference "Interferometry for Optical Astronomy II", SPIE 2002
Published: 2003
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38. Transiting exoplanets from the CoRoT space mission

Author: Jean Schneider, Sascha Grziwa, Laurent Jorda, C. Lovis, Sylvio Ferraz-Mello, A. S. Bonomo, Roi Alonso, Rodrigo F. Díaz, M. Tadeu dos Santos, Magali Deleuil, Michael Endl, D. Rouan, J. Weingrill, Suzanne Aigrain, M. Pätzold, François Bouchy, Thomas Fruth, A. P. Hatzes, C. Cavarroc, M. Fridlund, A. Léger, J. Cabrera, Hans J. Deeg, Tristan Guillot, D. Queloz, Helmut Lammer, Brandon Tingley, Sz. Csizmadia, Pierre Barge, William D. Cochran, Alexandre Santerne, Günther Wuchterl, C. Moutou, Pascal Bordé, J. M. Almenara, Eike W. Guenther, Stefania Carpano, A. Baglin, Rudolf Dvorak, Davide Gandolfi, M. Auvergne, Tsevi Mazeh, Aviv Ofir, G. Hebrard, T. Pasternacki, Ruth Titz-Weider, Heike Rauer, Phillip J. MacQueen, Michaël Gillon, Anders Erikson, Marc Ollivier, Departamento de Matemàtica, PUC RIO, Canada-France-Hawaii Telescope Corporation (CFHT), National Research Council of Canada (NRC)-Centre National de la Recherche Scientifique (CNRS)-University of Hawai'i [Honolulu] (UH), Instituto de Astrofisica de Canarias (IAC), Laboratoire d'Astrophysique de Marseille (LAM), 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), Thüringer Landessternwarte Tautenburg (TLS), School of Physics, 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), 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), Institut de Radioprotection et de Sûreté Nucléaire (IRSN), 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), Institute of Astronomy, University of Vienna [Vienna], DLR Institute of Planetary Research, German Aerospace Center (DLR), Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo = University of São Paulo (USP), 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), Department of Brain and Behavioural Sciences, Università degli Studi di Pavia = University of Pavia (UNIPV), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, 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), Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), 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), Rhenish Institute for Environmental Research (RIU), University of Cologne, DLR Institut für Planetenforschung, Deutsches Zentrum für Luft- und Raumfahrt [Berlin] (DLR), Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto = University of Porto, Laboratoire Univers et Théories (LUTH (UMR_8102)), and Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris
Subjects: Techniques: spectroscopic, FOS: Physical sciences, Astrophysics, Star (graph theory), Planetary systems, Techniques: photometric, Techniques: radial velocities, Astronomy and Astrophysics, Space and Planetary Science, Space (mathematics), spectroscopic [Techniques], planetary systems – techniques: photometric – techniques: radial velocities – techniques: spectroscopic, Planet, Low density, ComputingMilieux_MISCELLANEOUS, Earth and Planetary Astrophysics (astro-ph.EP), [PHYS]Physics [physics], Physics, Orbital elements, radial velocities [Techniques], photometric [Techniques], Planetary system, Light curve, ESPECTROSCOPIA, Exoplanet, 13. Climate action, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract: We present the discovery of a candidate multiply-transiting system, the first one found in the CoRoT mission. Two transit-like features with periods of 5.11 and 11.76d are detected in the CoRoT light curve, around a main sequence K1V star of r=15.1. If the features are due to transiting planets around the same star, these would correspond to objects of 3.7$\pm$0.4 and 5.0$\pm$0.5 R_earth respectively. Several radial velocities serve to provide an upper limit of 5.7 M_earth for the 5.11~d signal, and to tentatively measure a mass of 28$^{+11}_{-11}$ M_earth for the object transiting with a 11.76~d period. These measurements imply low density objects, with a significant gaseous envelope. The detailed analysis of the photometric and spectroscopic data serve to estimate the probability that the observations are caused by transiting Neptune-sized planets as $>$26$\times$ higher than a blend scenario involving only one transiting planet, and $>$900$\times$ higher than a scenario involving two blends and no planets. The radial velocities show a long term modulation that might be attributed to a 1.5 M_jup planet orbiting at 1.8~A.U. from the host, but more data are required to determine the precise orbital parameters of this companion., 13 pages, 13 figures, accepted to A&A, minor typos corrected
Published: 2014
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39. Exo-planet detection with the COROT space mission. I. A multi-transit detection criterion

Author: Pascal Bordé, Daniel Rouan, Alain Léger, Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), and arXiv, Import
Subjects: Physics, 010504 meteorology & atmospheric sciences, Stellar population, Detection threshold, Astrophysics (astro-ph), General Physics and Astronomy, Astronomy, FOS: Physical sciences, Astrophysics, Star (graph theory), Space (mathematics), 01 natural sciences, Galaxy, Exoplanet, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Transit (astronomy), Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: We present a detection criterion for exo-planets to be used with the space mission COROT. This criterion is based on the transit method, which suggests the observation of star dimming caused by partial occulations by planetary companions. When at least three transits are observed, we show that a cross-correlation technique can yield a detection threshold, thus enabling the evaluation of the number of possible detections, assuming a model for the stellar population in the Galaxy., Comment: 7 pages, 4 figures
Published: 2001

40. The Mass of CoRoT-7b

Author: Artie P. Hatzes, Malcolm Fridlund, Gil Nachmani, Tsevi Mazeh, Diana Valencia, Guillaume Hébrard, Ludmila Carone, Martin Pätzold, Stephane Udry, Francois Bouchy, Magali Deleuil, Claire Moutou, Pierre Barge, Pascal Bordé, Hans Deeg, Brandon Tingley, Rudolf Dvorak, Davide Gandolfi, Sylvio Ferraz-Mello, Günther Wuchterl, Eike Guenther, Tristan Guillot, Heike Rauer, Anders Erikson, Juan Cabrera, Szilard Csizmadia, Alain Léger, Helmut Lammer, Jörg Weingrill, Didier Queloz, Roi Alonso, Daniel Rouan, Jean Schneider, 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, 010504 meteorology & atmospheric sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Exoplanet, Radial velocity, Space and Planetary Science, Planet, 0103 physical sciences, ddc:520, Terrestrial planet, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences
Abstract: The mass of CoRoT-7b, the first transiting superearth exoplanet, is still a subject of debate. A wide range of masses have been reported in the literature ranging from as high as 8 M_Earth to as low as 2.3 M_Earth. Although most mass determinations give a density consistent with a rocky planet, the lower value permits a bulk composition that can be up to 50% water. We present an analysis of the CoRoT-7b radial velocity measurements that uses very few and simple assumptions in treating the activity signal. By only analyzing those radial velocity data for which multiple measurements were made in a given night we remove the activity related radial velocity contribution without any a priori model. We demonstrate that the contribution of activity to the final radial velocity curve is negligible and that the K-amplitude due to the planet is well constrained. This yields a mass of 7.42 +/- 1.21 M_Earth and a mean density of rho = 10.4 +/- 1.8 gm cm^-3. CoRoT-7b is similar in mass and radius to the second rocky planet to be discovered, Kepler-10b, and within the errors they have identical bulk densities - they are virtual twins. These bulk densities lie close to the density - radius relationship for terrestrial planets similar to what is seen for Mercury. CoRoT-7b and Kepler-10b may have an internal structure more like Mercury than the Earth.
Published: 2011
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