EDP Sciences
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Volume 504, Number 2, September III 2009
Page(s) 617 - 623
Section Planets and planetary systems
DOI http://dx.doi.org/10.1051/0004-6361/200911658
Published online 15 July 2009
A&A 504, 617-623 (2009)
DOI: 10.1051/0004-6361/200911658

A planet around the evolved intermediate-mass star HD 110014

J. R. de Medeiros1, J. Setiawan2, A. P. Hatzes3, L. Pasquini4, L. Girardi5, S. Udry6, M. P. Döllinger4, and L. da Silva7

1  Departamento de Física, Universidade Federal do Rio Grande do Norte, Natal, Brazil
    e-mail: renan@dfte.ufrn.br
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

Received 13 January 2009 / 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 $M_{\odot}$, is slightly metal rich with [Fe/H] = 0.19 and a rotational velocity $V \sin i\ $ = 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 $835.48 \pm 6.04$ days. A Keplerian orbit, with an eccentricity $e = 0.462\pm 0.069$, yields a minimum mass $M \sin i$ = 11.09  $M_{{\rm Jup}}$. The analysis of the residuals shows evidence for a second RV variability with a period of 130 days and an amplitude of $\pm$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

© ESO 2009

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