Search for spectroscopical signatures of transiting HD 209458b's exosphere

Details Search for spectroscopical signatures of transiting HD 209458b's exosphere Search for spectroscopical signatures of transiting HD 209458b's exosphere

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...371..260m&link_type=abstract

Astronomy and Astrophysics, v.371, p.260-266 (2001)

Astronomy and Astrophysics

Astrophysics

41

Techniques: Spectroscopic, Stars: Atmosphere, Stars: Planetary Systems

Scientific paper

Following recent attempts to detect the exosphere of the extra-solar planet 51 Pegb in the infrared (Coustenis et al. \cite{cou97}, \cite{cou98}; Rauer et al. \cite{rau00a}), 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{cha00a}; Henry et al. \cite{hen00}), 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. Based on public data from the UVES Commissioning at the ESO 8.2~m Kueyen telescope operated on Paranal Observatory, Chile.

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