TY - JOUR
T1 - Transiting exoplanets from the CoRoT space mission
T2 - XXI. CoRoT-19b: A low density planet orbiting an old inactive F9V-star
AU - Guenther, E. W.
AU - Díaz, R. F.
AU - Gazzano, J. C.
AU - Mazeh, T.
AU - Rouan, D.
AU - Gibson, N.
AU - Csizmadia, Sz
AU - Aigrain, S.
AU - Alonso, R.
AU - Almenara, J. M.
AU - Auvergne, M.
AU - Baglin, A.
AU - Barge, P.
AU - Bonomo, A. S.
AU - Bordé, P.
AU - Bouchy, F.
AU - Bruntt, H.
AU - Cabrera, J.
AU - Carone, L.
AU - Carpano, S.
AU - Cavarroc, C.
AU - Deeg, H. J.
AU - Deleuil, M.
AU - Dreizler, S.
AU - Dvorak, R.
AU - Erikson, A.
AU - Ferraz-Mello, S.
AU - Fridlund, M.
AU - Gandolfi, D.
AU - Gillon, M.
AU - Guillot, T.
AU - Hatzes, A.
AU - Havel, M.
AU - Hébrard, G.
AU - Jehin, E.
AU - Jorda, L.
AU - Lammer, H.
AU - Léger, A.
AU - Moutou, C.
AU - Nortmann, L.
AU - Ollivier, M.
AU - Ofir, A.
AU - Pasternacki, Th
AU - Pätzold, M.
AU - Parviainen, H.
AU - Queloz, D.
AU - Rauer, H.
AU - Samuel, B.
AU - Santerne, A.
AU - Schneider, J.
AU - Tal-Or, L.
AU - Tingley, B.
AU - Weingrill, J.
AU - Wuchterl, G.
N1 - Funding Information:
The French teams are grateful to CNES for its constant support and funding of A.B., J.M.A., and C.C. The German team thanks the DLR and the BMBF for the support under grants 50 OW 0204, and 50 OW 0603. The team at the IAC acknowledges support by grants ESP2007-65480-C02-02 and AYA2010-20982-C02-02 of the Spanish Ministerio de Ciencia e Innovación. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Foundation (SNF). M. Gillon and E. Jehin are FNRS Research Associates. MONET (MOnitoring NEtwork of Telescopes) is funded by the “Astronomie & Internet” program of the Alfred Krupp von Bohlen und Halbach Foundation, Essen, and operated by the Georg-August-Universität Göttingen, the McDonald Observatory of the University of Texas at Austin, and the South African Astronomical Observatory. The results are also partly based on observations performed with the FIES spectrograph at the Nordic Optical Telescope (NOT), under observing program P42-261. NOT is operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Additional data was obtained with the Sandiford spectrograph at the 2.1 m Otto Struve telescope at McDonald Observatory (Texas, USA), and the SOPHIE spectrograph at the Observatoire de Haute-Provence, France, under observing program PNP.08A.MOUT.
PY - 2012
Y1 - 2012
N2 - Context. Observations of transiting extrasolar planets are of key importance to our understanding of planets because their mass, radius, and mass density can be determined. These measurements indicate that planets of similar mass can have very different radii. For low-density planets, it is generally assumed that they are inflated owing to their proximity to the host-star. To determine the causes of this inflation, it is necessary to obtain a statistically significant sample of planets with precisely measured masses and radii. Aims. The CoRoT space mission allows us to achieve a very high photometric accuracy. By combining CoRoT data with high-precision radial velocity measurements, we derive precise planetary radii and masses. We report the discovery of CoRoT-19b, a gas-giant planet transiting an old, inactive F9V-type star with a period of four days. Methods. After excluding alternative physical configurations mimicking a planetary transit signal, we determine the radius and mass of the planet by combining CoRoT photometry with high-resolution spectroscopy obtained with the echelle spectrographs SOPHIE, HARPS, FIES, and SANDIFORD. To improve the precision of its ephemeris and the epoch, we observed additional transits with the TRAPPIST and Euler telescopes. Using HARPS spectra obtained during the transit, we then determine the projected angle between the spin of the star and the orbit of the planet. Results. We find that the host star of CoRoT-19b is an inactive F9V-type star close to the end of its main-sequence life. The host star has a mass M * = 1.21 ± 0.05 M ⊙ and radius R * = 1.65 ± 0.04 R ⊙. The planet has a mass of M P = 1.11 ± 0.06 M Jup and radius of R P = 1.29 ± 0.03 R Jup. The resulting bulk density is only ρ = 0.71 ± 0.06 g cm -3, which is much lower than that for Jupiter. Conclusions. The exoplanet CoRoT-19b is an example of a giant planet of almost the same mass as Jupiter but a ≈30% larger radius.
AB - Context. Observations of transiting extrasolar planets are of key importance to our understanding of planets because their mass, radius, and mass density can be determined. These measurements indicate that planets of similar mass can have very different radii. For low-density planets, it is generally assumed that they are inflated owing to their proximity to the host-star. To determine the causes of this inflation, it is necessary to obtain a statistically significant sample of planets with precisely measured masses and radii. Aims. The CoRoT space mission allows us to achieve a very high photometric accuracy. By combining CoRoT data with high-precision radial velocity measurements, we derive precise planetary radii and masses. We report the discovery of CoRoT-19b, a gas-giant planet transiting an old, inactive F9V-type star with a period of four days. Methods. After excluding alternative physical configurations mimicking a planetary transit signal, we determine the radius and mass of the planet by combining CoRoT photometry with high-resolution spectroscopy obtained with the echelle spectrographs SOPHIE, HARPS, FIES, and SANDIFORD. To improve the precision of its ephemeris and the epoch, we observed additional transits with the TRAPPIST and Euler telescopes. Using HARPS spectra obtained during the transit, we then determine the projected angle between the spin of the star and the orbit of the planet. Results. We find that the host star of CoRoT-19b is an inactive F9V-type star close to the end of its main-sequence life. The host star has a mass M * = 1.21 ± 0.05 M ⊙ and radius R * = 1.65 ± 0.04 R ⊙. The planet has a mass of M P = 1.11 ± 0.06 M Jup and radius of R P = 1.29 ± 0.03 R Jup. The resulting bulk density is only ρ = 0.71 ± 0.06 g cm -3, which is much lower than that for Jupiter. Conclusions. The exoplanet CoRoT-19b is an example of a giant planet of almost the same mass as Jupiter but a ≈30% larger radius.
KW - planetary systems
KW - techniques: photometric
KW - techniques: radial velocities
KW - techniques: spectroscopic
UR - http://www.scopus.com/inward/record.url?scp=84856183880&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/201117706
DO - 10.1051/0004-6361/201117706
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AN - SCOPUS:84856183880
SN - 0004-6361
VL - 537
JO - Astronomy and Astrophysics
JF - Astronomy and Astrophysics
M1 - A136
ER -