Jerome A. Orosz, William F. Welsh, Joshua A. Carter, Erik Brugamyer, Lars A. Buchhave, William D. Cochran, Michael Endl, Eric B. Ford, Phillip MacQueen, Donald R. Short, Guillermo Torres, Gur Windmiller, Eric Agol, Thomas Barclay, Douglas A. Caldwell, Bruce D. Clarke, Laurance R. Doyle, Daniel C. Fabrycky, John C. Geary, Nader Haghighipour, Matthew J. Holman, Khadeejah A. Ibrahim, Jon M. Jenkins, Karen Kinemuchi, Jie Li, Jack J. Lissauer, Andrej Prsa, Darin Ragozzine, Avi Shporer, Martin Still, Richard A. Wade
We discuss the discovery and characterization of the circumbinary planet Kepler-38b. The stellar binary is single-lined, with a period of 18.8 days, and consists of a moderately evolved main-sequence star (M_A = 0.949 +/- 0.059 solar masses and R_A = 1.757 +/- 0.034 solar radii) paired with a low-mass star (M_B = 0.249 +/- 0.010 solar masses and R_B = 0.2724 +/- 0.0053 solar radii) in a mildly eccentric (e=0.103) orbit. A total of eight transits due to a circumbinary planet crossing the primary star were identified in the Kepler light curve (using Kepler Quarters 1 through 11), from which a planetary period of 105.595 +/- 0.053 days can be established. A photometric dynamical model fit to the radial velocity curve and Kepler light curve yields a planetary radius of 4.35 +/- 0.11 Earth radii, or 1.12 +/- 0.03 Neptune radii. Since the planet is not sufficiently massive to observably alter the orbit of the binary from Keplerian motion, we can only place an upper limit on the mass of the planet of 122 Earth masses (7.11 Neptune masses or 0.384 Jupiter masses) at 95% confidence. This upper limit should decrease as more Kepler data become available.
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http://arxiv.org/abs/1208.3712
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