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On the Frequency of Gas Giant Planets in the Metal-Poor Regime

Published online by Cambridge University Press:  09 March 2010

A. Sozzetti ,
D. W. Latham ,
G. Torres ,
B. W. Carney ,
J. B. Laird ,
R. P. Stefanik ,
A. P. Boss  and
S. Korzennik
A. Sozzetti
Affiliation:
INAF- Astronomical Observatory of Torino, I-10025 Pino Torinese (TO), Italy email: [email protected]
D. W. Latham
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
G. Torres
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
B. W. Carney
Affiliation:
University of North Carolina at Chapel Hill, Chapel Hill, NC 27599, USA
J. B. Laird
Affiliation:
Bowling Green State University, Bowling Green, OH 43403, USA
R. P. Stefanik
Affiliation:
INAF- Astronomical Observatory of Torino, I-10025 Pino Torinese (TO), Italy email: [email protected]
A. P. Boss
Affiliation:
Carnegie Institution of Washington, Washington DC 20015, USA
S. Korzennik
Affiliation:
Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
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Abstract

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We present an analysis of three years of precision radial velocity measurements of 160 metal-poor stars observed with Keck/HIRES. We report on variability and long-term velocity trends for each star in our sample. We identify several long-term, low-amplitude radial-velocity variables worthy of follow-up with direct imaging techniques. We place lower limits on the detectable companion mass as a function of orbital period. None of the stars in our sample exhibits radial-velocity variations compatible with the presence of Jovian planets with periods shorter than the survey duration (3 yr). The resulting average frequency of gas giants orbiting metal-poor dwarfs with −2.0≤[Fe/H]≤ −0.6 is fp < 0.67%. By combining our dataset with the Fischer & Valenti (2005) uniform sample, we confirm that the likelihood of a star to harbor a planet more massive than Jupiter within 2 AU is a steeply rising function of the host's metallicity. However, the data for stars with −1.0≤[Fe/H]≤ 0.0 are compatible, in a statistical sense, with a constant occurrence rate fp≃1%. Our results usefully inform theoretical studies of the process of giant planet formation across two orders of magnitude in metallicity.

Keywords

planetary systems: formation — stars: abundances — stars: statistics — techniques: radial velocities
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S265: Chemical Abundances in the Universe: Connecting First Stars to Planets , August 2009 , pp. 416 - 419
Copyright
Copyright © International Astronomical Union 2010

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