Hostname: page-component-54dcc4c588-dbm8p Total loading time: 0 Render date: 2025-10-06T23:56:06.966Z Has data issue: false hasContentIssue false
  • English
  • Français

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: athena.coustenis@obspm.fr
N. Iro
Affiliation:
LESIA – Observatoire de Paris-Meudon, 5, place Jules Jannsen, FRANCE email: athena.coustenis@obspm.fr Department of Physics – University of Florida, USA email: iro@phys.ufl.edu
C. Moutou
Affiliation:
LAM – Marseille, FRANCE email: claire.moutou@oamp.fr
M. Mayor
Affiliation:
Observatoire de Genève, SWITZERLAND email: Michel.Mayor@obs.unige.ch,Didier.Queloz@obs.unige.ch
D. Queloz
Affiliation:
Observatoire de Genève, SWITZERLAND email: Michel.Mayor@obs.unige.ch,Didier.Queloz@obs.unige.ch
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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