Thomas N. Gautier III, David Charbonneau, Jason F. Rowe, Geoffrey W. Marcy, Howard Isaacson, Guillermo Torres, Francois Fressin, Leslie A. Rogers, Jean-Michel Désert, Lars A. Buchhave, David W. Latham, Samuel N. Quinn, David R. Ciardi, Daniel C. Fabrycky, Eric B. Ford, Ronald L. Gilliland, Lucianne M. Walkowicz, Stephen T. Bryson, William D. Cochran, Michael Endl, Debra A. Fischer, Steve B. Howel, Elliott P. Horch, Thomas Barclay, Natalie Batalha, William J. Borucki, Jessie L. Christiansen, John C. Geary, Christopher E. Henze, Matthew J. Holman, Khadeejah Ibrahim, Jon M. Jenkins, Karen Kinemuchi, David G. Koch, Jack J. Lissauer, Dwight T. Sanderfer, Dimitar D. Sasselov, Sara Seager, Kathryn Silverio, Jeffrey C. Smith, Martin Still, Martin C. Stumpe, Peter Tenenbaum, Jeffrey Van Cleve
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).
View original:
http://arxiv.org/abs/1112.4514
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