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The California Planet Survey. I. Four New Giant Exoplanets

Howard, Andrew W. and Johnson, John Asher and Marcy, Geoffrey W. and Fischer, Debra A. and Wright, Jason T. and Bernat, David and Henry, Gregory W. and Peek, Kathryn M. G. and Isaacson, Howard and Apps, Kevin and Endl, Michael and Cochran, William D. and Valenti, Jeff A. and Anderson, Jay and Piskunov, Nikolai E. (2010) The California Planet Survey. I. Four New Giant Exoplanets. Astrophysical Journal, 721 (2). pp. 1467-1481. ISSN 0004-637X.

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We present precise Doppler measurements of four stars obtained during the past decade at Keck Observatory by the California Planet Survey (CPS). These stars, namely, HD 34445, HD 126614, HD 13931, and Gl 179, all show evidence for a single planet in Keplerian motion. We also present Doppler measurements from the Hobby-Eberly Telescope (HET) for two of the stars, HD 34445 and Gl 179, that confirm the Keck detections and significantly refine the orbital parameters. These planets add to the statistical properties of giant planets orbiting near or beyond the ice line, and merit follow-up by astrometry, imaging, and space-borne spectroscopy. Their orbital parameters span wide ranges of planetary minimum mass (M sin i = 0.38-1.9 M_(Jup)), orbital period (P = 2.87-11.5 yr), semimajor axis (a = 2.1-5.2 AU), and eccentricity (e = 0.02-0.41). HD 34445 b (P = 2.87 yr, M sin i = 0.79 M_(Jup), e = 0.27) is a massive planet orbiting an old, G-type star. We announce a planet, HD 126614 Ab, and an M dwarf, HD 126614 B, orbiting the metal-rich star HD 126614 (which we now refer to as HD 126614 A). The planet, HD 126614 Ab, has minimum mass M sin i = 0.38 M_(Jup) and orbits the stellar primary with period P = 3.41 yr and orbital separation a = 2.3 AU. The faint M dwarf companion, HD 126614 B, is separated from the stellar primary by 489 mas (33 AU) and was discovered with direct observations using adaptive optics and the PHARO camera at Palomar Observatory. The stellar primary in this new system, HD 126614 A, has the highest measured metallicity ([Fe/H] = +0.56) of any known planet-bearing star. HD 13931 b (P = 11.5 yr, M sin i = 1.88 M_(Jup), e = 0.02) is a Jupiter analog orbiting a near solar twin. Gl 179 b (P = 6.3 yr, M sin i = 0.82 M Jup, e = 0.21) is a massive planet orbiting a faint M dwarf. The high metallicity of Gl 179 is consistent with the planet-metallicity correlation among M dwarfs, as documented recently by Johnson & Apps.

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Howard, Andrew W.0000-0001-8638-0320
Marcy, Geoffrey W.0000-0002-2909-0113
Wright, Jason T.0000-0001-6160-5888
Isaacson, Howard0000-0002-0531-1073
Additional Information:© 2010 The American Astronomical Society. Received 2009 May 28; accepted 2010 July 13; published 2010 September 10. Based on observations obtained at the W. M. Keck Observatory, which is operated jointly by the University of California and the California Institute of Technology. Keck time has been granted by both NASA and the University of California. Two of the planets announced here are also based on observations obtained with the Hobby-Eberly Telescope, which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. We thank the many observers who contributed to the velocities reported here. We gratefully acknowledge the efforts and dedication of the Keck Observatory staff, especially Grant Hill and Scott Dahm for support of HIRES and Greg Wirth for support of remote observing. We are grateful to the time assignment committees of the University of California, NASA, and NOAO for their generous allocations of observing time. Without their long-term commitment to radial velocity monitoring, these longperiod planets would likely remain unknown. We acknowledge R. Paul Butler and S. S. Vogt for many years of contributing to the data presented here. A.W.H. gratefully acknowledges support from a Townes Post-doctoral Fellowship at the U. C. Berkeley Space Sciences Laboratory. J.A.J. is an NSF Astronomy and Astrophysics Postdoctoral Fellow and acknowledges support form NSF grant AST-0702821. G.W.M. acknowledges NASA grant NNX06AH52G. J.T.W. received support from NSF grant AST-0504874. M.E. and W.D.C acknowledge support from NASA grants NNX07AL70G and NNX09AB30G issued through the Origins of Solar Systems Program. Automated Astronomy at Tennessee State University has been supported by NASA and NSF as well as Tennessee State University and the State of Tennessee through its Centers of Excellence program. This work made use of the SIMBAD database (operated at CDS, Strasbourg, France), NASA’s Astrophysics Data System Bibliographic Services, and the NASA Star and Exoplanet Database (NStED). Finally, the authors wish to extend special thanks to those of Hawai‘ian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous hospitality, the Keck observations presented herein would not have been possible.
Funding AgencyGrant Number
UC Berkeley Space Sciences Laboratory Townes Postdoctoral FellowshipUNSPECIFIED
Subject Keywords:binaries: visual; planetary systems; stars: individual (HD 34445, HD 126614, HD 24496, HD 13931, G1 179); techniques: high angular resolution; techniques: photometric; techniques: radial velocities
Classification Code:PACS: 97.82.-j; 97.10.Wn; 95.85.Kr; 97.20.Jg
Record Number:CaltechAUTHORS:20101029-093212671
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Official Citation:Andrew W. Howard et al 2010 ApJ 721 1467 doi: 10.1088/0004-637X/721/2/1467
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:20594
Deposited By: Ruth Sustaita
Deposited On:29 Oct 2010 20:42
Last Modified:16 Nov 2017 17:52

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