EDP Sciences
Free Access
Volume 443, Number 1, November III 2005
Page(s) 337 - 345
Section Planets and planetary systems
DOI https://doi.org/10.1051/0004-6361:20052938
Published online 21 October 2005

A&A 443, 337-345 (2005)
DOI: 10.1051/0004-6361:20052938

Extrasolar planets and brown dwarfs around A-F type stars

I. Performances of radial velocity measurements, first analyses of variations
F. Galland1, 2, A.-M. Lagrange1, S. Udry2, A. Chelli1, F. Pepe2, D. Queloz2, J.-L. Beuzit1 and M. Mayor2

1  Laboratoire d'Astrophysique de l'Observatoire de Grenoble, Université Joseph Fourier, BP 53, 38041 Grenoble, France
    e-mail: Franck.Galland@obs.ujf-grenoble.fr
2  Observatoire de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland

(Received 25 February 2005 / Accepted 23 August 2005 )

We present the performances of a radial velocity measurement method that we developed for A-F type stars. These perfomances are evaluated through an extensive set of simulations, together with actual radial velocity observations of such stars using the ELODIE and HARPS spectrographs. We report the case of stars constant in radial velocity, the example of a binary detection on HD 48097 (an A2V star, with $v\sin{i}$ equal to 90 km s$^{\rm -1}$) and a confirmation of the existence of a 3.9  $M_{\rm Jup}$ planet orbiting around HD 120136 (Tau Boo). The instability strip problem is also discussed. We show that with this method, it is in principle possible to detect planets and brown dwarfs around A-F type stars, thus allowing further study of the impact of stellar masses on planetary system formation over a wider range of stellar masses than is currently done.

Key words: techniques: radial velocities -- stars: binaries: spectroscopic -- stars: low-mass, brown dwarfs -- stars: planetary systems

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© ESO 2005

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