Transiting exoplanets from the CoRoT space mission. III. The spectroscopic transit of CoRoT-Exo-2b with SOPHIE and HARPS

Bibcode
2008A&A...482L..25B
DOI
10.1051/0004-6361:200809433
Bouchy, F.; Queloz, D.; Deleuil, M.; Loeillet, B.; Hatzes, A. P.; Aigrain, S.; Alonso, R.; Auvergne, M.; Baglin, A.; Barge, P.; Benz, W.; Bordé, P.; Deeg, H. J.; de La Reza, R.; Dvorak, R.; Erikson, A.; Fridlund, M.; Gondoin, P.; Guillot, T.; Hébrard, G.; Jorda, L.; Lammer, H.; Léger, A.; Llebaria, A.; Magain, P.; Mayor, M.; Moutou, C.; Ollivier, M.; Pätzold, M.; Pepe, F.; Pont, F.; Rauer, H.; Rouan, D.; Schneider, J.; Triaud, A. H. M. J.; Udry, S.; Wuchterl, G.
Referencia bibliográfica

Astronomy and Astrophysics, Volume 482, Issue 3, 2008, pp.L25-L28

Fecha de publicación:
5
2008
Revista
Astronomy and Astrophysics
Número de autores
37
Número de autores del IAC
1
Número de citas
113
Número de citas referidas
90
Descripción
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 λ = 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. Observations made with SOPHIE spectrograph at Observatoire de Haute Provence, France (PNP.07A.MOUT) and HARPS spectrograph at ESO La Silla Observatory (079.C-0127(F)). The CoRoT space mission, launched on December 27th 2006, has been developed and is operated by CNES, with the contribution of Austria, Belgium, Brasil, ESA, Germany, and Spain.
Proyectos relacionados
Helio y Astroseismología
Sismología Solar y Estelar y Búsqueda de Exoplanetas
Los objetivos principales de este proyecto son: 1) estudiar la estructura y la dinámica del interior solar, 2) ampliar este estudio a otros tipos de estrellas y 3) buqueda de planetas extrasolares utilizando métodos fotométricos y su caracterización con información complementaria (espectrometría). Para alcanzar el primer objetivo, utilizamos la
Savita
Mathur
En ejecución
Tipo
Con árbitro
Física estelar e interestelar (FEEI)
Técnicas

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