Kepler-20: A Sun-like Star with Three Sub-Neptune Exoplanets and Two Earth-size Candidates
Creators: name: Gautier, Thomas N.
name: Charbonneau, David
name: Rowe, Jason F.
name: Marcy, Geoffrey W.
name: Isaacson, Howard
name: Torres, Guillermo
name: Fressin, Francois
name: Rogers, Leslie A.
name: Désert, Jean-Michel
name: Buchhave, Lars A.
name: Latham, David W.
name: Quinn, Samuel N.
name: Ciardi, David R.
name: Fabrycky, Daniel C.
name: Ford, Eric B.
name: Gilliland, Ronald L.
name: Walkowicz, Lucianne M.
name: Bryson, Stephen T.
name: Cochran, William D.
name: Endl, Michael
name: Fischer, Debra A.
name: Howel, Steve B.
name: Horch, Elliott P.
name: Barclay, Thomas
name: Batalha, Natalie
name: Borucki, William J.
name: Christiansen, Jessie L.
name: Geary, John C.
name: Henze, Christopher E.
name: Holman, Matthew J.
name: Ibrahim, Khadeejah
name: Jenkins, Jon M.
name: Kinemuchi, Karen
name: Koch, David G.
name: Lissauer, Jack J.
name: Sanderfer, Dwight T.
name: Sasselov, Dimitar D.
name: Seager, Sara
name: Silverio, Kathryn
name: Smith, Jeffrey C.
name: Still, Martin
name: Stumpe, Martin C.
name: Tenenbaum, Peter
name: Van Cleve, Jeffrey
Publisher: name: arXiv
Year: 2011
Subjects: subject: Earth and Planetary Astrophysics (astro-ph.EP)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We present the discovery of the Kepler-20 planetary system, which we initially identified through the detection of five distinct periodic transit signals in the Kepler light curve of the host star 2MASSJ19104752+4220194. We find a stellar effective temperature Teff=5455+-100K, a metallicity of [Fe/H]=0.01+-0.04, and a surface gravity of log(g)=4.4+-0.1. Combined with an estimate of the stellar density from the transit light curves we deduce a stellar mass of Mstar=0.912+-0.034 Msun and a stellar radius of Rstar=0.944^{+0.060}_{-0.095} Rsun. For three of the transit signals, our results strongly disfavor the possibility that these result from astrophysical false positives. We conclude that the planetary scenario is more likely than that of an astrophysical false positive by a factor of 2e5 (Kepler-20b), 1e5 (Kepler-20c), and 1.1e3 (Kepler-20d), sufficient to validate these objects as planetary companions. For Kepler-20c and Kepler-20d, the blend scenario is independently disfavored by the achromaticity of the transit: From Spitzer data gathered at 4.5um, we infer a ratio of the planetary to stellar radii of 0.075+-0.015 (Kepler-20c) and 0.065+-0.011 (Kepler-20d), consistent with each of the depths measured in the Kepler optical bandpass. We determine the orbital periods and physical radii of the three confirmed planets to be 3.70d and 1.91^{+0.12}_{-0.21} Rearth for Kepler-20b, 10.85 d and 3.07^{+0.20}_{-0.31} Rearth for Kepelr-20c, and 77.61 d and 2.75^{+0.17}_{-0.30} Rearth for Kepler-20d. From multi-epoch radial velocities, we determine the masses of Kepler-20b and Kepler-20c to be 8.7\+-2.2 Mearth and 16.1+-3.5 Mearth, respectively, and we place an upper limit on the mass of Kepler-20d of 20.1 Mearth (2 sigma).
description: accepted by ApJ, 58 pages, 12 figures revised Jan 2012 to correct table 2 and clarify planet parameter extraction