Volume 371, Number 1, May III 2001
|Page(s)||260 - 266|
|Published online||15 May 2001|
Search for spectroscopical signatures of transiting HD 209458b's exosphere*
ESO, Alonso de Cordova 3107, Santiago de Chile e-mail: firstname.lastname@example.org
2 Observatoire de Paris Meudon, 92195 Meudon Cedex, France e-mail: Athena.Coustenis@obspm.fr, Jean.Schneider@obspm.fr, Richard.Saint-Gilles@obspm.fr
3 Observatoire de Genève, Switzerland e-mail: email@example.com, firstname.lastname@example.org
Corresponding author: C. Moutou, email@example.com
Accepted: 18 January 2001
Following recent attempts to detect the exosphere of the extra-solar planet 51 Pegb in the infrared (Coustenis et al. [CITE], [CITE]; Rauer et al. [CITE]), we discuss here a search for optical spectroscopic signatures from a gaseous extended envelope (called exosphere) surrounding the planet HD 209458b. This planet has a demonstrated photometric transit (Charbonneau et al. [CITE]; Henry et al. [CITE]), thus offering an increased probability for the spectroscopic detection of such an envelope. Therefore it is the best known candidate for probing the exospheric composition of a giant planet, orbiting a Sun-like star at a short distance. The observations were performed with UVES at the VLT and cover most of the 328-669 nm range. We did not detect HD 209458b's exosphere at a level of 1% , a value close to the predictions. We discuss here the first results obtained and their limitations, as well as future prospective.
Key words: techniques: spectroscopic / stars: atmosphere / stars: planetary systems
© ESO, 2001
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