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Atmospheric signatures by transit of HD209458 with VLT/UVES

Published online by Cambridge University Press:  02 May 2006

Athena Coustenis ,
N. Iro ,
C. Moutou ,
M. Mayor  and
D. Queloz
Athena Coustenis
Affiliation:
LESIA – Observatoire de Paris-Meudon, 5, place Jules Jannsen, FRANCE email: [email protected]
N. Iro
Affiliation:
LESIA – Observatoire de Paris-Meudon, 5, place Jules Jannsen, FRANCE email: [email protected] Department of Physics – University of Florida, USA email: [email protected]
C. Moutou
Affiliation:
LAM – Marseille, FRANCE email: [email protected]
M. Mayor
Affiliation:
Observatoire de Genève, SWITZERLAND email: [email protected],[email protected]
D. Queloz
Affiliation:
Observatoire de Genève, SWITZERLAND email: [email protected],[email protected]
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Abstract

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In our search for clues as to the nature of the exosphere of HD209458 (Moutou et al., 2001 ; Moutou et al., 2003, Iro et al., 2004), we have acquired VLT/UVES data during an ambitious observational campaign performed in June-September 2002 and covering 6 transits of the exoplanet. The resolving power was R=100000 in the 0.475-0.68 micron range. We search for ions and neutral molecules (such as H2O+, CO+, CH+, etc) originating in the planets exosphere and located in the evaporated material around the planet, occulting its primary star. We present in this paper a tentative search in the spectral regions where features of sodium or H$_2$O$^+$ can be present.

Keywords

Exoplanetstransitsexosphereatmospheretechniques: spectroscopic(stars:) planetary systemsline: identification
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Colloquium C200: Direct Imaging of Exoplanets: Science & Techniques , October 2005 , pp. 171 - 174
Copyright
© 2006 International Astronomical Union