Old, Rich, and Eccentric: Two Jovian Planets Orbiting Evolved Metal-Rich Stars

Creators: Peek, Kathryn M. G.; Johnson, John Asher; Fischer, Debra A.; Marcy, Geoffrey W.; Henry, Gregory W.; Howard, Andrew W.; Wright, Jason T.; Lowe, Thomas B.; Reffert, Sabine; Schwab, Christian; Williams, Peter K. G.; Isaacson, Howard; Giguere, Matthew J.

Abstract

We present radial velocity measurements of two stars observed as part of the Lick Subgiants Planet Search and the Keck N2K survey. Variations in the radial velocities of both stars reveal the presence of Jupiter-mass exoplanets in highly eccentric orbits. HD 16175 is a G0 subgiant from the Lick Subgiants Planet Search, orbited by a planet having a minimum mass of 4.4 MJup, in an eccentric (e = 0.59), 2.71 yr orbit. HD 96167 is a G5 subgiant from the N2K ("Next 2000") program at Keck Observatory, orbited by a planet having a minimum mass of 0.68 MJup, in an eccentric (e = 0.71), 1.366 yr orbit. Both stars are relatively massive (M⋆ = 1.3 M⊙) and are very metal rich ([Fe/H] > +0.3). We describe our methods for measuring the stars' radial velocity variations and photometric stability.

Additional Information

© 2009 Astronomical Society of the Pacific. Received 2009 March 20; accepted 2009 April 16; published 2009 May 16. We are indebted to the many observers who collected spectra of these stars. For HD 16175, we thank the observers Kelsey Clubb, Julia Kregenow, Joshua Peek, Karin Sandstrom, and Julien Spronck. For HD 96167, we thank the observers Gaspar Bakos, R. Paul Butler, Chris McCarthy, Guillermo Torres, Steven S. Vogt, and Joshua Winn. We gratefully acknowledge the dedication and support of the Lick and Keck Observatory staffs, in particular Tony Misch for support with the Hamilton Spectrograph and Grant Hill and Scott Dahm for support with HIRES. JAJ is an NSF Astronomy and Astrophysics Postdoctoral Fellow with support from the NSF grant AST-0702821. DAF acknowledges research support from NASA grant NNX08AF42G. GWH acknowledges that 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. We thank the NASA Exoplanet Science Institute (NExScI) for support through the KPDA program. We thank the NASA, NOAO, and UCO/Lick telescope assignment committees for allocations of telescope time. The authors extend thanks to those of Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their kind hospitality, the Keck observations presented here would not have been possible. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA's Astrophysics Data System Bibliographic Services. Based on observations obtained at the Lick Observatory, which is operated by the University of California, and on observations obtained at theW. M. Keck Observatory, which is operated as a scientific partnership with the University of California, the California Institute of Technology, and the National Aeronautics and Space Administration. Keck Observatory was made possible by the generous financial support of theW. M. Keck Foundation. Keck time has been granted by both NASA and the University of California.

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