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Published November 1, 2006 | Published
Journal Article Open

TrES-2: The First Transiting Planet in the Kepler Field


We announce the discovery of the second transiting hot Jupiter discovered by the Trans-atlantic Exoplanet Survey. The planet, which we dub TrES-2, orbits the nearby star GSC 03549-02811 every 2.47063 days. From high-resolution spectra, we determine that the star has T_eff = 5960 ± 100 K and log g = 4.4 ± 0.2, implying a spectral type of G0 V and a mass of 1.08^(+0.11)_(-0.05) M_☉. High-precision radial velocity measurements confirm a sinusoidal variation with the period and phase predicted by the photometry, and rule out the presence of line bisector variations that would indicate that the spectroscopic orbit is spurious. We estimate a planetary mass of 1.28^(+0.09)_(-0.04)M_Jup. We model B, r, R, and I photometric time series of the 1.4% deep transits and find a planetary radius of 1.24^(+0.09)_(-0.06) R_Jup. This planet lies within the field of view of the NASA Kepler mission, ensuring that hundreds of upcoming transits will be monitored with exquisite precision and permitting a host of unprecedented investigations.

Additional Information

© 2006 American Astronomical Society. Received 2006 August 21; accepted 2006 September 12; published 2006 October 16. Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among Caltech, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. We sincerely thank R. Brucato, M. Doyle, K. Dunscombe, R. Ellis, B. Gordon, J. Henning, L. Kroll, S. Kunsman, J. Mueller, H. Petrie, A. Pickles, N. Scoville, M. Sweet, R. Thicksten, G. van Idsinga, R. Wetzel, and D. Zieber for their assistance with the Sleuth instrument. We thank the referee, S. Gaudi, for his detailed comments that helped improve the Letter. We are indebted to S. Fernández Acosta, who accommodated the unscheduled transit observation at the IAC80, which is operated by the IAC in its Observatorio del Teide. This material is based on work supported by NASA under grants NNG 05GJ29G, NNG05GI57G, NNH 05AB88I, and NNG 04LG89G, issued through the Origins of Solar Systems Program. We acknowledge support from the NASA Kepler mission.

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