Extrasolar planets and brown dwarfs around A–F type stars

Free access article

This article has an erratum: [erratum]

Issue		A&A Volume 491, Number 3, December I 2008


Page(s)		883 - 888
Section		Planets and planetary systems
DOI		http://dx.doi.org/10.1051/0004-6361:200810241
Published online		03 October 2008

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

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

Abstract
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

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