Radial-Velocity Variability of G-Type Giants: First Three Years of the Okayama Planet Search Program

Details Radial-Velocity Variability of G-Type Giants: First Three Years of the Okayama Planet Search Program Radial-Velocity Variability of G-Type Giants: First Three Years of the Okayama Planet Search Program

Feb 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005pasj...57...97s&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.57, No.1, pp. 97-107

Astronomy and Astrophysics

Astronomy

30

Stars: Late-Type, Stars: Planetary Systems, Techniques: Radial Velocities

Scientific paper

We report on the radial-velocity variability of G-type giants based on the results of precise Doppler measurements of 57 stars that were observed for the first 3 years of the Okayama Planet Search Program. This program aims to search for planets around intermediate-mass stars in their evolved stages as late-G giants. We found that most of the targets with B - V < 1.0 have radial-velocity scatters of σ ˜ 10 m s-1, with the most stable reaching levels of 6-8 m s-1, while those with B - V > 1.0 typically show σ ˜ 20 m s-1. In total, about 60% of the targets are stable in radial velocity to a level of σ < 15 m s-1 over 1-3 years, and about 90% have σ < 30 m s-1. We found that 4 stars (HD 30557, HD 34559, HD 68077, and HD 85444) show significant long-term radial-velocity trends, suggesting that they are probably orbited by unseen stellar or substellar companions. Three stars (HD 79181, HD 104985, and HD 141680) show periodic radial-velocity variations. HD 104985 is the first planet-harboring star discovered from our survey. The properties of the variations in these 3 stars have been, and will be, extensively discussed in separate papers. Relatively large, but not apparently periodic, radial-velocity variations of σ > 30 m s-1 are found in 4 stars (HD 41597, HD 134190, HD 161178, and HD 176598). For most of the stars without showing any significant periodicity, we can exclude companions with K > 50 m s-1, or m2sin i > 1.8 MJ (a/AU)1/2(M* /M&sun;)1/2 for orbital radii a ≲ 1-2 AU.

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