A&A 470, 721-726 (2007)
The HARPS search for southern extra-solar planets
1 European Southern Observatory, Casilla 19001, Santiago 19, Chile
2 Observatoire de Genève, Université de Genève, 51 Ch. des Maillettes, 1290 Sauverny, Switzerland
3 Physikalisches Institut Universität Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
4 Institut d'Astrophysique de Paris, UMR7095, Université Pierre & Marie Curie, 98bis Bd Arago, 75014 Paris, France
5 Laboratoire d'Astrophysique de Marseille, Traverse du Siphon, 13376 Marseille 12, France
6 Centro de Astronomia e Astrofísica da Universidade de Lisboa, Observatório Astronómico de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal
7 Centro de Geofísica de Évora, Rua Romão Ramalho 59, 7002-554 Évora, Portugal
(Received 26 February 2007 / Accepted 11 April 2007 )
Context. The HARPS high-resolution high-accuracy spectrograph was made available to the astronomical community in the second half of 2003. Since then, we have been using this instrument for monitoring radial velocities of a large sample of Solar-type stars (1400 stars) in order to search for their possible low-mass companions.
Aims. Amongst the goals of our survey, one is to significantly increase the number of detected extra-solar planets in a volume-limited sample to improve our knowledge of their orbital elements distributions and thus obtain better constraints for planet-formation models.
Methods.Radial-velocities were obtained from high-resolution HARPS spectra via the cross-correlation method. We then searched for Keplerian signals in the obtained radial-velocity data sets. Finally, companions orbiting our sample stars were characterised using the fitted orbital parameters.
Results. In this paper, we present the HARPS radial-velocity data and orbital solutions for 3 Solar-type stars: HD 100777 , HD 190647 , and HD 221287 . The radial-velocity data of HD 100777 is best explained by the presence of a 1.16 planetary companion on a 384-day eccentric orbit (e = 0.36). The orbital fit obtained for the slightly evolved star HD 190647 reveals the presence of a long-period (P = 1038 d) 1.9 planetary companion on a moderately eccentric orbit (e = 0.18). HD 221287 is hosting a 3.1 planet on a 456-day orbit. The shape of this orbit is not very well-constrained because of our non-optimal temporal coverage and because of the presence of abnormally large residuals. We find clues that these large residuals result from spectral line-profile variations probably induced by processes related to stellar activity.
Key words: stars: individual: HD 100777 -- stars: individual: HD 190647 -- stars: individual: HD 221287 -- stars: planetary systems -- techniques: radial velocities
© ESO 2007