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HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star

Bakos, G. Á. and Kovács, G. and Torres, G. and Fischer, D. A. and Latham, D. W. and Noyes, R. W. and Sasselov, D. D. and Mazeh, T. and Shporer, A. and Butler, R. P. and Stefanik, R. P. and Fernández, J. M. and Sozzetti, A. and Pál, A. and Johnson, J. and Marcy, G. W. and Winn, J. N. and Sipőcz, B. and Lázár, J. and Papp, I. and Sári, P. (2007) HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star. Astrophysical Journal, 670 (1). pp. 826-832. ISSN 0004-637X. doi:10.1086/521866.

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We report the discovery of a massive (M_p = 9.04 ± 0.50 M_J) planet transiting the bright (V = 8.7) F8 star HD 147506, with an orbital period of 5.63341 ± 0.00013 days and an eccentricity of e = 0.520 ± 0.010. From the transit light curve we determine that the radius of the planet is R_p = 0.982^(+0.038)_(-0.105) R_J. HD 147506b (also coined HAT-P-2b) has a mass about 9 times the average mass of previously known transiting exoplanets and a density of ρp ≈ 12 g cm^(-3), greater than that of rocky planets like the Earth. Its mass and radius are marginally consistent with theories of structure of massive giant planets composed of pure H and He, and accounting for them may require a large (≳100 M_⊕) core. The high eccentricity causes a ninefold variation of insolation of the planet between peri- and apastron. Using follow-up photometry, we find that the center of transit is T_(mid) = 2,454,212.8559 ± 0.0007 (HJD) and the transit duration is 0.177 ± 0.002 days.

Item Type:Article
Related URLs:
URLURL TypeDescription
Bakos, G. Á.0000-0001-7204-6727
Torres, G.0000-0002-5286-0251
Fischer, D. A.0000-0003-2221-0861
Latham, D. W.0000-0001-9911-7388
Sasselov, D. D.0000-0001-7014-1771
Shporer, A.0000-0002-1836-3120
Johnson, J.0000-0001-9808-7172
Marcy, G. W.0000-0002-2909-0113
Winn, J. N.0000-0002-4265-047X
Additional Information:© 2007 American Astronomical Society. Received 2007 April 29; accepted 2007 July 20. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations fromthismountain. Keck time has been in part granted by NASA. Operation of the HATNet project is funded in part by NASA grant NNG04GN74G. Work by G.Á.B. was supported by NASA through Hubble Fellowship Grant HST-HF-01170.01-A. G. K. wishes to offer thanks for support from the Hungarian Scientific Research Foundation (OTKA) grant K-60750.We acknowledge partial support from the Kepler Mission under NASA Cooperative Agreement NCC2-1390 ( PI: D.W. L.). G. T. acknowledges partial support from NASA Origins grant NNG04LG89G. T. M. thanks the Israel Science Foundation for a support through grant 03/233. D.A. F. is a Cottrell Science Scholar of Research Corporation and acknowledges support from NASA grant NNG05G164G. We would like to thank Joel Hartman (CfA), Gil Esquerdo (CfA), and Ron Dantowitz and Marek Kozubal (Clay Center) for their efforts to observe HAT-P-2b in transit, and Howard Isaacson (San Francisco State University) for obtaining spectra at Lick Observatory. We wish to thank Amit Moran for his help in the observations with the Wise HAT telescope. We owe special thanks to the directors and staff of FLWO, SMA, and the Wise Observatory for supporting the operation of HATNet and WHAT. We would also like to thank the anonymous referee for the useful suggestions that improved this paper.
Funding AgencyGrant Number
NASA Hubble FellowshipHST-HF-01170.01-A
Hungarian Scientific Research Foundation (OTKA)K-60750
Israel Science Foundation03/233
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Record Number:CaltechAUTHORS:20130109-142201592
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Official Citation:HD 147506b: A Supermassive Planet in an Eccentric Orbit Transiting a Bright Star G. Á. Bakos et al. 2007 ApJ 670 826
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:36280
Deposited By: Ruth Sustaita
Deposited On:09 Jan 2013 22:48
Last Modified:09 Nov 2021 23:21

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