HAT-P-16b: A 4 M _J Planet Transiting a Bright Star on an Eccentric Orbit

• Published in: The Astrophysical Journal
• Main Authors: Buchhave, L. A., Bakos, G. Ã., Hartman, J. D., Torres, G., Kovács, A., Latham, D. W., Noyes, R. W., Esquerdo, G. A., Everett, M., Howard, A. W., Marcy, G. W., Fischer, D. A., Johnson, J. A., Andersen, J., Fűrész, G., Perumpilly, G., Sasselov, D. D., Stefanik, R. P., Béky, B., Lázár, J., Papp, I., Sári, P.
• Format: Article in Journal/Newspaper
• Language: unknown
• Published: American Astronomical Society 2010
• Subjects: planetary systems; stars: individual (HAT-P-16; GSC 2792-01700); techniques: photometric; techniques: spectroscopic; Norway; Observatorio; Iceland
• Online Access: https://doi.org/10.1088/0004-637X/720/2/1118

We report the discovery of HAT-P-16b, a transiting extrasolar planet orbiting the V = 10.8 mag F8 dwarf GSC 2792-01700, with a period P = 2.775960 ± 0.000003 days, transit epoch T_c = 2455027.59293 ± 0.00031 (BJD^(10)), and transit duration 0.1276 ± 0.0013 days. The host star has a mass of 1.22 ± 0.04 M ⊙, radius of 1.24 ± 0.05 R ⊙ , effective temperature 6158 ± 80 K, and metallicity [Fe/H] = +0.17 ± 0.08. The planetary companion has a mass of 4.193 ± 0.094 M _J and radius of 1.289 ± 0.066 R _J, yielding a mean density of 2.42 ± 0.35 g cm^(–3). Comparing these observed characteristics with recent theoretical models, we find that HAT-P-16b is consistent with a 1 Gyr H/He-dominated gas giant planet. HAT-P-16b resides in a sparsely populated region of the mass-radius diagram and has a non-zero eccentricity of e = 0.036 with a significance of 10σ. © 2010. The American Astronomical Society. All rights reserved. Received 2010 April 14; accepted 2010 July 5; published 2010 August 17. Based in part on observations made with the Nordic Optical Telescope, operated on the island of La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden, in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. 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 granted by NASA (N018Hr). HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR&D grants. The work of G.Ã.B. and J.A.J. were supported by the Postdoctoral Fellowship of the NSF Astronomy and Astrophysics Program (AST-0702843 and AST-0702821, respectively). G.T. acknowledges partial support from NASA grant NNX09AF59G.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. Based in part on ...