The CORALIE survey for southern extra-solar planets

Free access article

Issue		A&A Volume 480, Number 3, March IV 2008


Page(s)		L33 - L36
Section		Letters
DOI		http://dx.doi.org/10.1051/0004-6361:20078737
Published online		14 February 2008

A&A 480, L33-L36 (2008)
DOI: 10.1051/0004-6361:20078737

Letter

XV. Discovery of two eccentric planets orbiting HD 4113 and HD 156846

O. Tamuz^{1, 2}, D. Ségransan¹, S. Udry¹, M. Mayor¹, A. Eggenberger^{3, 1}, D. Naef⁴, F. Pepe¹, D. Queloz¹, N. C. Santos⁵, B.-O. Demory¹, P. Figuera¹, M. Marmier¹, and G. Montagnier^{1, 3}

¹ Observatoire astronomique de l'Université de Genève, 51 Ch. des Maillettes, Sauverny, 1290 Versoix, Switzerland
e-mail: Damien.Segransan@obs.unige.ch
² School of Physics and Astronomy, Raymond and Beverly Sackler Faculty of Exact Sciences, Tel Aviv University, Tel Aviv, Israel
³ Laboratoire d'Astrophysique de Grenoble, BP 53, 38041 Grenoble Cedex, France
⁴ European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile
⁵ Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, 4150-762 Porto, Portugal

(Received 26 September 2007 / Accepted 30 October 2007)

Abstract
We report the detection of two very eccentric planets orbiting HD 4113 and HD 156846 with the CORALIE Echelle spectrograph mounted on the 1.2-m Euler Swiss telescope at La Silla. The first planet, HD 4113 b, has minimum mass of $m\sin{i}=1.6$ $\pm$ $0.2~M_{\rm Jup}$ , a period of P=526.59 $\pm$ 0.21 days and an eccentricity of e=0.903 $\pm$ 0.02. It orbits a metal rich G5V star at a=1.28 AU, which displays an additional radial velocity drift of 28 m s^-1 yr^-1 observed during 8 years. The combination of the radial-velocity data and the non-detection of any main sequence stellar companion in our high contrast images, taken at the VLT with NACO/SDI, characterizes the companion as a probable brown dwarf or as a faint white dwarf. The second planet, HD 156846 b , has minimum mass of $m\sin{i}=10.45$ $\pm$ $0.05~M_{\rm Jup}$ , a period of P=359.51 $\pm$ 0.09 days, an eccentricity of e=0.847 $\pm$ 0.002 and is located at a=1.0 AU from its parent star. HD 156846 is a metal rich G0 dwarf and is also the primary of a wide binary system (a>250 AU, P>4000 years). Its stellar companion, IDS 17147-1914 B , is a M4 dwarf. The very high eccentricities of both planets can be explained by Kozai oscillations induced by the presence of a third object.

Key words: stars: planetary systems -- techniques: radial velocities -- methods: observational -- stars: low-mass, brown dwarfs

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