The N2K Consortium. I. A Hot Saturn Planet Orbiting HD 88133

Creators: Fischer, Debra A.; Laughlin, Greg; Butler, Paul; Marcy, Geoff; Johnson, John; Henry, Greg; Valenti, Jeff; Vogt, Steve; Ammons, Mark; Robinson, Sara; Spear, Greg; Strader, Jay; Driscoll, Peter; Fuller, Abby; Johnson, Teresa; Manrao, Elizabeth; McCarthy, Chris; Muñoz, Melesio; Tah, K. L.; Wright, Jason; Ida, Shigeru; Sato, Bun'ei; Toyota, Eri; Minniti, Dante

Abstract

The N2K ("next 2000") consortium is carrying out a distributed observing campaign with the Keck, Magellan, and Subaru telescopes, as well as the automatic photometric telescopes of Fairborn Observatory, in order to search for short-period gas giant planets around metal-rich stars. We have established a reservoir of more than 14,000 main-sequence and subgiant stars closer than 110 pc, brighter than V = 10.5, and with 0.4 < B - V < 1.2. Because the fraction of stars with planets is a sensitive function of stellar metallicity, a broadband photometric calibration has been developed to identify a subset of 2000 stars with [Fe/H] > 0.1 dex for this survey. We outline the strategy and report the detection of a planet orbiting the metal-rich G5 IV star HD 88133 with a period of 3.41 days, semivelocity amplitude K = 35.7 m s^(-1), and M sin i = 0.29M_J. Photometric observations reveal that HD 88133 is constant on the 3.415 day radial velocity period to a limit of 0.0005 mag. Despite a transit probability of 19.5%, our photometry rules out the shallow transits predicted by the large stellar radius.

Additional Information

© 2005 American Astronomical Society. Received 2004 September 7; accepted 2004 October 12. 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. We gratefully acknowledge the dedication and support of the Keck Observatory staff. We thank the NOAO and NASA telescope assignment committees for generous allocations of telescope time. We thank the Michaelson Science Center for travel support and support through the KDPA program. G.W. H. acknowledges support from NASA grant NCC5-511 and NSF grant HRD-9706268. We acknowledge support by NASA grant NAG5-75005 (to G. W. M.), NSF grant AST-9988358, NASA grant NAG5-4445 (to S. S. V.), and NASA grant NNG04GKi9G (to G. L.). D. M. is supported by FONDAP 15010003. We are grateful to Sun Microsystems for ongoing support. We thank the anonymous referee for helpful comments. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. The authors extend thanks to those of native Hawaiian 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.

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