Issue |
A&A
Volume 470, Number 2, August I 2007
|
|
---|---|---|
Page(s) | 721 - 726 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361:20077361 | |
Published online | 10 May 2007 |
The HARPS search for southern extra-solar planets*,**
IX. Exoplanets orbiting HD 100777, HD 190647, and HD 221287
1
European Southern Observatory, Casilla 19001, Santiago 19, Chile e-mail: dnaef@eso.org
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 MJup
planetary companion on a 384-day eccentric orbit (). The orbital fit obtained for the slightly evolved star
HD 190647 reveals the presence of a long-period (
d) 1.9 MJup planetary
companion on a moderately eccentric orbit (
). HD 221287 is hosting a 3.1 MJup
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
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