David G. Koch
NASA Exoplanet Science Institute
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Astrophysical Journal Supplement Series | 2011
Francois Fressin; Guillermo Torres; J.-M. Desert; David Charbonneau; Natalie M. Batalha; Jonathan J. Fortney; Jason F. Rowe; Christopher Allen; William J. Borucki; Timothy M. Brown; Stephen T. Bryson; David R. Ciardi; William D. Cochran; Drake Deming; Edward W. Dunham; Daniel C. Fabrycky; Thomas N. Gautier; Ronald L. Gilliland; Christopher E. Henze; Matthew J. Holman; Steve B. Howell; Jon M. Jenkins; Karen Kinemuchi; Heather A. Knutson; David G. Koch; David W. Latham; Jack J. Lissauer; Geoffrey W. Marcy; Darin Ragozzine; Dimitar D. Sasselov
The Kepler mission has recently announced the discovery of Kepler-10 b, the smallest exoplanet discovered to date and the first rocky planet found by the spacecraft. A second, 45 day period transit-like signal present in the photometry from the first eight months of data could not be confirmed as being caused by a planet at the time of that announcement. Here we apply the light curve modeling technique known as BLENDER to explore the possibility that the signal might be due to an astrophysical false positive (blend). To aid in this analysis we report the observation of two transits with the Spitzer Space Telescope at 4.5 μm. When combined, they yield a transit depth of 344 ± 85 ppm that is consistent with the depth in the Kepler passband (376 ± 9 ppm, ignoring limb darkening), which rules out blends with an eclipsing binary of a significantly different color than the target. Using these observations along with other constraints from high-resolution imaging and spectroscopy, we are able to exclude the vast majority of possible false positives. We assess the likelihood of the remaining blends, and arrive conservatively at a false alarm rate of 1.6 × 10^(–5) that is small enough to validate the candidate as a planet (designated Kepler-10 c) with a very high level of confidence. The radius of this object is measured to be R_p = 2.227^(+0.052)_(–0.057) R_⊕ (in which the error includes the uncertainty in the stellar properties), but currently available radial-velocity measurements only place an upper limit on its mass of about 20 M_⊕. Kepler-10 c represents another example (with Kepler-9 d and Kepler-11 g) of statistical validation of a transiting exoplanet, as opposed to the usual confirmation that can take place when the Doppler signal is detected or transit timing variations are measured. It is anticipated that many of Keplers smaller candidates will receive a similar treatment since dynamical confirmation may be difficult or impractical with the sensitivity of current instrumentation.
Archive | 2006
William J. Borucki; David G. Koch; Gibor Basri; Timothy M. Brown; Douglas A. Caldwell; Edna DeVore; Edward W. Dunham; Thomas N. Gautier; John C. Geary; Ronald L. Gilliland; Alan Gould; Steven B. Howell; Jon M. Jenkins
Archive | 2001
William J. Borucki; David G. Koch; Jon M. Jenkins
Archive | 1995
Laurance R. Doyle; Jon M. Jenkins; Hans J. Deeg; E. L. Martín; Jakob P. Schneider; Michel Chevreton; E. V. Paleologou; Won Boo Lee; Edward W. Dunham; David G. Koch; E. J. Blue; D. Toublanc; Zoran Ninkov; Christiaan L. Sterken
Archive | 2006
Natalie M. Batalha; William J. Borucki; Douglas A. Caldwell; Hema Chandrasekaran; Thomas N. Gautier; Jon M. Jenkins; David G. Koch
Archive | 2001
Jon M. Jenkins; Douglas A. Caldwell; William J. Borucki; David G. Koch
Archive | 1998
Douglas A. Caldwell; William J. Borucki; Jon M. Jenkins; David G. Koch; Zoran Ninkov
Archive | 1995
William J. Borucki; David G. Koch
Archive | 1993
William J. Borucki; David G. Koch; Edward W. Dunham; Peter Rex Davis; Silvano P. Colombano; Arno F. Granados; C. H. Ford; Phuong N. Pham; Laurance R. Doyle; William Dale Heacox; Harold J. Reitsema; Alan W. Delamere; Martin J. Duncan; L. Robinson
Archive | 2011
Eric B. Ford; Daniel C. Fabrycky; Matthew J. Holman; Jack J. Lissauer; Althea V. Moorhead; Robert C. Morehead; Darin Ragozzine; Jason H. Steffen; David G. Koch