HAT-P-14b: A 2.2 M_J Exoplanet Transiting a Bright F Star

Creators: Torres, G.; Bakos, G. Á.; Hartman, J.; Kovács, Géza; Noyes, R. W.; Latham, D. W.; Fischer, D. A.; Johnson, J. A.; Marcy, G. W.; Howard, A. W.; Sasselov, D. D.; Kipping, D.; Sipőcz, B.; Stefanik, R. P.; Esquerdo, G. A.; Everett, M. E.; Lázár, J.; Papp, I.; Sári, P.

Abstract

We report the discovery of HAT-P-14b, a fairly massive transiting extrasolar planet orbiting the moderately bright star GSC 3086-00152 (V = 9.98), with a period of P = 4.627669 ± 0.000005 days. The transit is close to grazing (impact parameter 0.891^(+0.007)_(–0.008)) and has a duration of 0.0912 ± 0.0017 days, with a reference epoch of mid-transit of T_c = 2,454, 875.28938 ± 0.00047 (BJD). The orbit is slightly eccentric (e = 0.107 ± 0.013), and the orientation is such that occultations are unlikely to occur. The host star is a slightly evolved mid-F dwarf with a mass of 1.386 ± 0.045 M_☉, a radius of 1.468 ± 0.054 R_☉, effective temperature 6600 ± 90 K, and a slightly metal-rich composition corresponding to [Fe/H] = +0.11 ± 0.08. The planet has a mass of 2.232 ± 0.059 M_J and a radius of 1.150 ± 0.052 R_J, implying a mean density of 1.82 ± 0.24 g cm^(–3). Its radius is well reproduced by theoretical models for the 1.3 Gyr age of the system if the planet has a heavy-element fraction of about 50 M_⊕ (7% of its total mass). The brightness, near-grazing orientation, and other properties of HAT-P-14 make it a favorable transiting system to look for changes in the orbital elements or transit timing variations induced by a possible second planet, and also to place meaningful constraints on the presence of sub-Earth mass or Earth-mass exomoons, by monitoring it for transit duration variations.

Additional Information

© 2010 American Astronomical Society. Received 2010 February 11; accepted 2010 March 30; published 2010 April 29. 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. HATNet operations have been funded by NASA grants NNG04GN74G and NNX08AF23G, and SAO IR&D grants. G.T. acknowledges partial support from NASA grant NNX09AF59G. G.Á.B. and J.A.J. were supported by Postdoctoral Fellowships of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). We acknowledge partial support also from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 (D.W.L., PI). G.K. thanks the Hungarian Scientific Research Foundation (OTKA) for support through grant K-81373. G.Á.B. thanks Gábor Kovács for his help in system management of the HATNet computers while the data analysis was carried out. We are grateful to the anonymous referee for helpful suggestions. This research has benefited from Keck telescope time allocations granted through NOAO (programs A264Hr, A146Hr) and NASA (N049Hr, N018Hr). This research has also made use of the SIMBAD database and the VizieR catalogue access tool, both operated at CDS, Strasbourg, France, of NASA's Astrophysics Data System Abstract Service, and of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the NSF.

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