EDP Sciences
Free access
Issue A&A
Volume 446, Number 2, February I 2006
Page(s) 717 - 722
Section Planets and planetary systems
DOI http://dx.doi.org/10.1051/0004-6361:20054116

A&A 446, 717-722 (2006)
DOI: 10.1051/0004-6361:20054116

Elodie metallicity-biased search for transiting Hot Jupiters

I. Two Hot Jupiters orbiting the slightly evolved stars HD 118203 and HD 149143
R. Da Silva1, S. Udry1, F. Bouchy2, M. Mayor1, C. Moutou2, F. Pont1, D. Queloz1, N. C. Santos3, 1, D. Ségransan1 and S. Zucker1, 4

1  Geneva Observatory, 1290 Sauverny, Switzerland
    e-mail: Ronaldo.daSilva@obs.unige.ch
2  Observatoire de Marseille, France
3  Centro de Astronomia e Astrofísica da Universidade de Lisboa, Tapada da Ajuda, 1349-018 Lisboa, Portugal
4  The Weizmann Institute of Science, PO Box 26, Rehovot 76100, Israel

(Received 29 August 2005 / Accepted 22 September 2005)

We report the discovery of a new planet candidate orbiting the subgiant star HD 118203 with a period of P = 6.1335 days. The best Keplerian solution yields an eccentricity e = 0.31 and a minimum mass $m_2\sin{i}$ = 2.1 $M_{\rm Jup}$ for the planet. This star has been observed with the ELODIE fiber-fed spectrograph as one of the targets in our planet-search programme biased toward high-metallicity stars, on-going since March 2004 at the Haute-Provence Observatory. An analysis of the spectroscopic line profiles using line bisectors revealed no correlation between the radial velocities and the line-bisector orientations, indicating that the periodic radial-velocity signal is best explained by the presence of a planet-mass companion. A linear trend is observed in the residuals around the orbital solution that could be explained by the presence of a second companion in a longer-period orbit. We also present here our orbital solution for another slightly evolved star in our metal-rich sample, HD 149143 , recently proposed to host a 4-d period Hot Jupiter by the N2K consortium. Our solution yields a period P = 4.09 days, a marginally significant eccentricity e = 0.08 and a planetary minimum mass of 1.36 $M_{\rm Jup}$. We checked that the shape of the spectral lines does not vary for this star as well.

Key words: stars: individual: HD 118203 -- stars: individual: HD 149143 -- planetary systems -- techniques: radial velocities

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Editor-in-Chief: T. Forveille
Letters Editor-in-Chief: J. Alves
Managing Editor: N. Aghanim

ISSN: 0004-6361 ; e-ISSN: 1432-0746
Frequency: 12 volumes per year
Published by: EDP Sciences

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