Detection of a Low-eccentricity and Super-massive Planet to the Subgiant HD 38801

Creators: Harakawa, Hiroki; Sato, Bun'ei; Fischer, Debra A.; Ida, Shigeru; Omiya, Masashi; Johnson, John A.; Marcy, Geoffrey W.; Toyota, Eri; Hori, Yasunori; Howard, Andrew W.

Abstract

We report the detection of a large mass planet orbiting around the K0 metal-rich subgiant HD38801 (V = 8.26) by precise radial velocity (RV) measurements from the Subaru Telescope and the Keck Telescope. The star has a mass of 1.36 M_☉ and a metallicity of [Fe/H] = +0.26. The RV variations are consistent with a circular orbit with a period of 696.0 days and a velocity semiamplitude of 200.0 m s^(–1), which yield a minimum mass for the companion of 10.7 M JUP and a semimajor axis of 1.71 AU. Such super-massive objects with very low eccentricities and periods of hundreds of days are uncommon among the ensemble of known exoplanets.

Additional Information

© 2010 American Astronomical Society. Received 2009 September 12; accepted 2010 April 10; published 2010 April 29. We extend our gratitude to Akito Tajitsu and Tae-Soo Pyo for their great expertise and support of HDS observations from the Subaru Telescope. We also gratefully acknowledge the efforts and dedication of all Keck Observatory staff. This research has made use of the Simbad database, operated at CDS, Strasbourg, France. We thank all Hawaiian people for their hospitality and native Hawaiian ancestry on whose sacred mountain of Mauna Kea we are privileged to be guests. Without their generous supports, we would not be able to publish our new planet. Based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. 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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