Kipping, D. M. and Hartman, J. and Bakos, G. Á. and Torres, G. and Latham, D. W. and Bayliss, D. and Kiss, L. L. and Sato, B. and Béky, B. and Kovács, Géza and Quinn, S. N. and Buchhave, L. A. and Andersen, J. and Marcy, G. W. and Howard, A. W. and Fischer, D. A. and Johnson, J. A. and Noyes, R. W. and Sasselov, D. D. and Stefanik, R. P. and Lázár, J. and Papp, I. and Sári, P. and Fűrész, G. (2011) HAT-P31bc:A Transiting, Eccentric, Hot Jupiter and a Long- Period, Massive Third Body. Astronomical Journal, 142 (3). Art. No. 95. ISSN 0004-6256 http://resolver.caltech.edu/CaltechAUTHORS:20110927-145207028
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We report the discovery of HAT-P-31b, a transiting exoplanet orbiting the V = 11.660 dwarf star GSC 2099-00908. HAT-P-31b is the first planet discovered with the Hungarian-made Automated Telescope (HAT) without any follow-up photometry, demonstrating the feasibility of a new mode of operation for the HATNet project. The 2.17 M_J , 1.1 R_J planet has a period of P_b = 5.0054 days and maintains an unusually high eccentricity of e_b = 0.2450 ± 0.0045, determined through Keck, FIbr-fed Échelle Spectrograph, and Subaru high-precision radial velocities (RVs). Detailed modeling of the RVs indicates an additional quadratic residual trend in the data detected to very high confidence. We interpret this trend as a long-period outer companion, HAT-P-31c, of minimum mass 3.4 M_J and period ≥2.8 years. Since current RVs span less than half an orbital period, we are unable to determine the properties of HAT-P-31c to high confidence. However, dynamical simulations of two possible configurations show that orbital stability is to be expected. Further, if HAT-P-31c has non-zero eccentricity, our simulations show that the eccentricity of HAT-P-31b is actively driven by the presence of c, making HAT-P-31 a potentially intriguing dynamical laboratory.
|Additional Information:||© 2011 The American Astronomical Society. Received 2011 June 6; accepted 2011 July 2; published 2011 August 16. 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 (N167Hr). Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. 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. HATNet operations have been funded by NASA grants NNG04GN74G, NNX08AF23G, and SAO IR&D grants. D.M.K. has been supported by Smithsonian Institution Restricted Endowment Funds. Work of G. Á. B. and J. Johnson 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-60750. L.L.K. is supported by the “Lendulet” Young Researchers Program of the Hungarian Academy of Sciences and the Hungarian OTKA grants K76816, K83790, and MB08C 81013. Tamás Szalai (University of Szeged) is acknowledged for his assistance during the ANU 2.3 m observations. This research has made use of Keck telescope time granted through NASA (N167Hr). This work is based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan, and 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. Thanks to G. Laughlin for useful advise on the Systemic Console, Dan Fabrycky and René Heller for useful comments, and special thanks to the anonymous referee for their helpful suggestions.|
|Subject Keywords:||planetary systems; stars: individual (HAT-P-31, GSC 2099-00908); techniques: photometric; techniques: spectroscopic|
|Classification Code:||PACS: 96.30.Kf; 96.12.De; 96.12.Bc|
|Official Citation:||HAT-P-31b,c: A Transiting, Eccentric, Hot Jupiter and a Long-period, Massive Third Body D. M. Kipping et al. 2011 The Astronomical Journal 142 95|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||27 Sep 2011 22:47|
|Last Modified:||26 Dec 2012 13:42|
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