Five Intermediate-Period Planets from the N2K Sample * **
© 2007. The American Astronomical Society. All rights reserved. Printed in U.S.A.
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Citation Debra A. Fischer et al 2007 ApJ 669 1336DOI 10.1086/521869
Debra A. Fischer
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Department of Physics and Astronomy, San Francisco State University, San Francisco, CA 94132
Steven S. Vogt
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UCO/Lick Observatory, University of California, Santa Cruz, CA 95064
Geoffrey W. Marcy
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Department of Astronomy, University of California, Berkeley, CA 94720
R. Paul Butler
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Department of Terrestrial Magnetism, Carnegie Institute of Washington DC, 5241 Broad Branch Road NW, Washington DC 20015-1305
Bun’ei Sato
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Tokyo Institute of Technology, 2-12-1 Okayama, Meguro-ku, Tokyo 152-8550, Japan
Gregory W. Henry
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Center of Excellence in Information Systems, Tennessee State University, 3500 John A. Merritt Boulevard, Box 9501, Nashville, TN 37209
Sarah Robinson
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UCO/Lick Observatory, University of California, Santa Cruz, CA 95064
Gregory Laughlin
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UCO/Lick Observatory, University of California, Santa Cruz, CA 95064
Shigeru Ida
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Tokyo Institute of Technology, 2-12-1 Okayama, Meguro-ku, Tokyo 152-8550, Japan
Eri Toyota
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Department of Earth and Planetary Sciences, Graduate School of Science, Kobe University, 1-1 Rokkodai, Nada, Kobe 657-8501, Japan
Masashi Omiya
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Department of Physics, Tokai University, 1117 Kitakaname, Hiratsuka, Kanagawa 259-1292, Japan
Peter Driscoll
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Department of Earth and Planetary Sciences, Johns Hopkins University, Baltimore, MD 21218
Genya Takeda
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Department of Physics and Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208
Jason T. Wright
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Department of Astronomy, University of California, Berkeley, CA 94720
John A. Johnson
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Department of Astronomy, University of California, Berkeley, CA 94720
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Dates
- Received 2007 March 31
- Accepted 2007 April 9
Abstract
We report the detection of five Jovian-mass planets orbiting high-metallicity stars. Four of these stars were first observed as part of the N2K program, and exhibited low rms velocity scatter after three consecutive observations. However, follow-up observations over the last 3 years now reveal the presence of longer period planets with orbital periods ranging from 21 days to a few years. HD 11506 is a G0 V star with a planet of M sin i = 4.74 MJup in a 3.85 yr orbit. HD 17156 is a G0 V star with a 3.12 MJup planet in a 21.2 day orbit. The eccentricity of this orbit is 0.67, one of the highest known for a planet with a relatively short period. The orbital period for this planet places it in a region of parameter space where relatively few planets have been detected. HD 125612 is a G3 V star with a planet of M sin i = 3.5 MJup in a 1.4 yr orbit. HD 170469 is a G5 IV star with a planet of M sin i = 0.67 MJup in a 3.13 year orbit. HD 231701 is an F8 V star with planet of 1.08 MJup in a 142 day orbit. All of these stars have supersolar metallicity. Three of the five stars were observed photometrically, but showed no evidence of brightness variability. A transit search conducted for HD 17156 was negative, but covered only 25% of the search space, and so is not conclusive.
Footnotes
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Based on observations obtained at the W. M. Keck Observatory, which is operated by the University of California and the California Institute of Technology. Keck time has been granted by NOAO and NASA.
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Based on observations obtained at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan.