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Centro de Astrofísica da Universidade do Porto

The HARPS search for southern extrasolar planets
XXV. Results from the metal-poor sample

N. C. Santos, M. Mayor, X. Bonfils, X. Dumusque, F. Bouchy, P. Figueira, C. Lovis, C. Melo, F. Pepe, D. Queloz, D. Ségransan, S. G. Sousa, S. Udry

Abstract
Searching for extrasolar planets around stars of different metallicity may provide strong constraints to the models of planet formation and evolution. In this paper we present the overall results of a HARPS (a high-precision spectrograph mostly dedicated to deriving precise radial velocities) program to search for planets orbiting a sample of 104 metal-poor stars (selected [Fe/H] below -0.5). Radial velocity time series of each star are presented and searched for signals using several statistical diagnostics. Stars with detected signals are presented, including 3 attributed to the presence of previously announced giant planets orbiting the stars HD171028, HD181720, and HD190984. Several binary stars and at least one case of a coherent signal caused by activityrelated phenomena are presented. One very promising new, possible giant planet orbiting the star HD107094 is discussed, and the results are analyzed in light of the metallicity-giant planet correlation. We conclude that the frequency of giant planets orbiting metal-poor stars may be higher than previously thought, probably reflecting the higher precision of the HARPS survey. In the metallicity domain of our sample, we also find evidence that the frequency of planets is a steeply rising function of the stellar metal content, as found for higher metallicity stars.

Keywords
techniques: radial velocities – techniques: spectroscopic – planets and satellites: formation – planetary systems – stars: abundances

Notes
Based on observations collected at the La Silla Parana Observatory, ESO (Chile) with the HARPS spectrograph at the 3.6-m telescope (ESO runs ID 72.C-0488, 082.C-0212, and 085.C-0063).
See updated table at http://www.exoplanet.eu

Astronomy and Astrophysics
Volume 526, Page A112_1
February 2011

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