HAT-P-6b: A Hot Jupiter Transiting a Bright F Star*

R. W. Noyes; G. Á. Bakos; G. Torres; A. Pál; Géza Kovács; D. W. Latham; J. M. Fernández; D. A. Fischer; R. P. Butler; G. W. Marcy; B. Sipőcz; G. A. Esquerdo; Gábor Kovács; D. D. Sasselov; B. Sato; R. Stefanik; M. Holman; J. Lázár; I. Papp; P. Sári

doi:10.1086/527358

HAT-P-6b: A Hot Jupiter Transiting a Bright F Star^*

R. W. Noyes¹, G. Á. Bakos^1,2, G. Torres¹, A. Pál^1,3, Géza Kovács⁴, D. W. Latham¹, J. M. Fernández¹, D. A. Fischer⁵, R. P. Butler⁶, G. W. Marcy⁷, B. Sipőcz^1,3, G. A. Esquerdo¹, Gábor Kovács¹, D. D. Sasselov¹, B. Sato⁸, R. Stefanik¹, M. Holman¹, J. Lázár⁹, I. Papp⁹, and P. Sári⁹

Published 2008 January 8 • © 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A.
The Astrophysical Journal, Volume 673, Number 1 Citation R. W. Noyes et al 2008 ApJ 673 L79 DOI 10.1086/527358

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Author affiliations

¹ Harvard-Smithsonian Center for Astrophysics, Cambridge, MA

² Hubble Fellow

³ Department of Astronomy, Eötvös Loránd University, Budapest, Hungary

⁴ Konkoly Observatory, Budapest, Hungary

⁵ Department of Physics and Astronomy, San Francisco State University, San Francisco, CA

⁶ Department of Terrestrial Magnetism, Carnegie Institute of Washington, DC

⁷ Department of Astronomy, University of California, Berkeley, CA

⁸ Tokyo Institute of Technology, Tokyo, Japan

⁹ Hungarian Astronomical Association, Budapest, Hungary

Dates

Received 2007 October 13
Accepted 2007 November 29
Published 2008 January 8

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Abstract

In the ongoing HATNet survey we have detected a giant planet, with radius 1.33 ± 0.06 R_Jup and mass 1.06 ± 0.12 M_Jup, transiting the bright (V = 10.5) star GSC 03239–00992. The planet is in a circular orbit with period 3.852985 ± 0.000005 days and midtransit epoch 2,454,035.67575 ± 0.00028 (HJD). The parent star is a late F star with mass 1.29 ± 0.06 M_☉, radius 1.46 ± 0.06 R_☉, T_eff ∼ 6570 ± 80 K , [ Fe/H ] = − 0.13 ± 0.08, and age ~2.3^{+ 0.5}_−0.7 Gyr. With this radius and mass, HAT-P-6b has somewhat larger radius than theoretically expected. We describe the observations and their analysis to determine physical properties of the HAT-P-6 system, and briefly discuss some implications of this finding.

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Footnotes

*
Based in part 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 in part granted by NASA (run N162Hr) and NOAO (run A285Hr).

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