Volume 504, Number 2, September III 2009
|Page(s)||617 - 623|
|Section||Planets and planetary systems|
|Published online||15 July 2009|
Departamento de Física, Universidade Federal do Rio Grande do Norte, Natal, Brazil e-mail: firstname.lastname@example.org
2 Max-Planck-Institut fur Astronomie, Königstuhl 17, 69117 Heidelberg, Germany
3 Thueringer Landessternwarte, Tautenburg, Germany
4 European Southern Observatory, Garching bei Munchen, Germany
5 Osservatorio Astronomico di Padova-INAF, Padova, Italy
6 Geneva Observatory, Geneva University, Geneva, Switzerland
7 Observatório Nacional, Rio de Janeiro, Brazil
Accepted: 10 July 2009
Context. We found evidence for a sub–stellar companion around the K giant star HD 110014. This cool evolved star, with a spectral type K2III and an estimated mass between 1.9 and 2.4 , is slightly metal rich with [Fe/H] = 0.19 and a rotational velocity = 2.0 km s-1.
Aims. To search for extrasolar planets around intermediate-mass stars and to improve our knowledge of the nature of radial velocity variations shown by G and K giant stars.
Methods. Based on radial velocity analysis, we found evidence for a substellar companion with a planetary mass and long orbital period. The Radial velocity variation of HD 110014 has been monitored from 2000 until 2007 with FEROS at 1.5 m ESO and at the 2.2 m MPG/ESO, HARPS at the 3.6 m ESO and Coralie at 1.2 m Leonard Euler swiss telescopes in La Silla observatory. The radial velocities were computed by using a cross-correlation technique. Line bisector, Hipparcos photometry and chromospheric lines were analyzed to exclude other root-causes for the radial velocity variability.
Results. We report the presence of an extrasolar planet around the giant star HD 110014, with an orbital period of days. A Keplerian orbit, with an eccentricity , yields a minimum mass = 11.09 . The analysis of the residuals shows evidence for a second RV variability with a period of 130 days and an amplitude of ±100 ms-1 . Its nature is not completely clear, but a second planet is a possible explanation.
Key words: stars: evolution / technique: radial velocities / stars: planetary systems / stars late-type
Based on observations collected at the 1.52-m ESO telescope (1999 to 2002), at the 2.2-m MPG/ESO telescope (2003 to 2007), at the 3.60 ESO telescope and at the Euler swiss telescope, at the La Silla Observatory, Chile.
© ESO, 2009
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