Kepler20: A Sunlike Star with Three SubNeptune Exoplanets and Two Earthsize Candidates
Abstract
We present the discovery of the Kepler20 planetary system, which we initially identified through the detection of five distinct periodic transit signals in the Kepler light curve of the host star 2MASS J19104752+4220194. From highresolution spectroscopy of the star, we find a stellar effective temperature T _{eff} = 5455 ± 100 K, a metallicity of [Fe/H] = 0.01 ± 0.04, and a surface gravity of log g = 4.4 ± 0.1. We combine these estimates with an estimate of the stellar density derived from the transit light curves to deduce a stellar mass of M _{sstarf} = 0.912 ± 0.034 M _{⊙} and a stellar radius of R _{sstarf} = 0.944^{+0.060} _{0.095} R _{⊙}. For three of the transit signals, we demonstrate that our results strongly disfavor the possibility that these result from astrophysical false positives. We accomplish this by first identifying the subset of stellar blends that reproduce the precise shape of the light curve and then using the constraints on the presence of additional stars from high angular resolution imaging, photometric colors, and the absence of a secondary component in our spectroscopic observations. We conclude that the planetary scenario is more likely than that of an astrophysical false positive by a factor of 2 × 10^{5} (Kepler20b), 1 × 10^{5} (Kepler20c), and 1.1 × 10^{3} (Kepler20d), sufficient to validate these objects as planetary companions. For Kepler20c and Kepler20d, the blend scenario is independently disfavored by the achromaticity of the transit: from Spitzer data gathered at 4.5 μm, we infer a ratio of the planetary to stellar radii of 0.075 ± 0.015 (Kepler20c) and 0.065 ± 0.011 (Kepler20d), 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 3.70 days and 1.91^{+0.12} _{0.21} R _{⊕} for Kepler20b, 10.85 days and 3.07^{+0.20} _{0.31} R _{⊕} for Kepler20c, and 77.61 days and 2.75^{+0.17} _{0.30} R _{⊕} for Kepler20d. From multiepoch radial velocities, we determine the masses of Kepler20b and Kepler20c to be 8.7 ± 2.2 M _{⊕} and 16.1 ± 3.5 M _{⊕}, respectively, and we place an upper limit on the mass of Kepler20d of 20.1 M _{⊕} (2σ).
 Publication:

The Astrophysical Journal
 Pub Date:
 April 2012
 DOI:
 10.1088/0004637X/749/1/15
 arXiv:
 arXiv:1112.4514
 Bibcode:
 2012ApJ...749...15G
 Keywords:

 eclipses;
 planetary systems;
 stars: individual: Kepler20 KIC 6850504 2MASS J19104752+4220194;
 Astrophysics  Earth and Planetary Astrophysics
 EPrint:
 accepted by ApJ, 58 pages, 12 figures revised Jan 2012 to correct table 2 and clarify planet parameter extraction