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Volume 491, Number 3, December I 2008
Page(s) 883 - 888
Section Planets and planetary systems
DOI https://doi.org/10.1051/0004-6361:200810241
Published online 03 October 2008

A&A 491, 883-888 (2008)
DOI: 10.1051/0004-6361:200810241

Extrasolar planets and brown dwarfs around A–F type stars

V. A planetary system found with HARPS around the F6IV–V star HD 60532
M. Desort1, A.-M. Lagrange1, F. Galland1, H. Beust1, S. Udry2, M. Mayor2, and G. Lo Curto3

1  Laboratoire d'Astrophysique de Grenoble, UMR 5571 CNRS, Université Joseph Fourier, BP 53, 38041 Grenoble Cedex 9, France
    e-mail: morgan.desort@obs.ujf-grenoble.fr
2  Observatoire de Genève, Université de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland
3  European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago, Chile

Received 22 May 2008 / Accepted 22 September 2008

Aims. In the framework of the search for extrasolar planets and brown dwarfs around early-type stars, we present the results obtained for the F-type main-sequence star HD 60532 (F6V) with HARPS.
Methods. Using 147 spectra obtained with HARPS at La Silla on a time baseline of two years, we studied the radial velocities of this star.
Results. HD 60532 radial velocities are periodically variable, and the variations have a Keplerian origin. This star is surrounded by a planetary system of two planets with minimum masses of 1 and 2.5 $M_{\rm Jup}$ and orbital separations of 0.76 and 1.58 AU, respectively. We also detect high-frequency, small-amplitude (10 m s-1 peak-to-peak) pulsations. Dynamical studies of the system point toward a possible 3:1 mean-motion resonance that should be confirmed within the next decade.

Key words: techniques: radial velocities -- stars: early-type -- stars: planetary systems -- stars: individual: HD 60532 -- stars: oscillations

© ESO 2008