Kepler input catalog: photometric calibration and stellar classification
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In this paper, the authors describe the photometric calibration and stellar classification methods used by the Stellar Classification Project to produce the Kepler Input Catalog (KIC) and derive atmospheric extinction corrections from hourly observations of secondary standard fields within the Kepler field of view.Abstract:
We describe the photometric calibration and stellar classification methods used by the Stellar Classification Project to produce the Kepler Input Catalog (KIC). The KIC is a catalog containing photometric and physical data for sources in the Kepler mission field of view; it is used by the mission to select optimal targets. Four of the visible-light (g, r, i, z) magnitudes used in the KIC are tied to Sloan Digital Sky Survey magnitudes; the fifth (D51) is an AB magnitude calibrated to be consistent with Castelli & Kurucz (CK) model atmosphere fluxes. We derived atmospheric extinction corrections from hourly observations of secondary standard fields within the Kepler field of view. For these filters and extinction estimates, repeatability of absolute photometry for stars brighter than magnitude 15 is typically 2%. We estimated stellar parameters {T eff, log (g), log (Z), E B – V } using Bayesian posterior probability maximization to match observed colors to CK stellar atmosphere models. We applied Bayesian priors describing the distribution of solar-neighborhood stars in the color-magnitude diagram, in log (Z), and in height above the galactic plane. Several comparisons with samples of stars classified by other means indicate that for 4500 K ≤T eff ≤ 6500 K, our classifications are reliable within about ±200 K and 0.4 dex in log (g) for dwarfs, with somewhat larger log (g) uncertainties for giants. It is difficult to assess the reliability of our log (Z) estimates, but there is reason to suspect that it is poor, particularly at extreme T eff. Comparisons between the CK models and observed colors are generally satisfactory with some exceptions, notably for stars cooler than 4500 K. Of great importance for the Kepler mission, for T eff ≤ 5400 K, comparison with asteroseismic results shows that the distinction between main-sequence stars and giants is reliable with about 98% confidence. Larger errors in log (g) occur for warmer stars, for which our filter set provides inadequate gravity diagnostics. The KIC is available through the MAST data archive.read more
Citations
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Journal ArticleDOI
Planetary Candidates Observed by Kepler. III. Analysis of the First 16 Months of Data
Natalie M. Batalha,Natalie M. Batalha,Jason F. Rowe,Stephen T. Bryson,Thomas Barclay,Christopher J. Burke,Douglas A. Caldwell,Jessie L. Christiansen,Fergal Mullally,Susan E. Thompson,Timothy M. Brown,Andrea K. Dupree,Daniel C. Fabrycky,Eric B. Ford,Jonathan J. Fortney,Ronald L. Gilliland,Howard Isaacson,David W. Latham,Geoffrey W. Marcy,Samuel N. Quinn,Samuel N. Quinn,Darin Ragozzine,Avi Shporer,William J. Borucki,David R. Ciardi,Thomas N. Gautier,Michael R. Haas,Jon M. Jenkins,David G. Koch,Jack J. Lissauer,William Rapin,Gibor Basri,Alan P. Boss,Lars A. Buchhave,Joshua A. Carter,David Charbonneau,Joergen Christensen-Dalsgaard,Bruce D. Clarke,William D. Cochran,Brice-Olivier Demory,Jean-Michel Desert,Edna DeVore,Laurance R. Doyle,Gilbert A. Esquerdo,Mark E. Everett,Francois Fressin,John C. Geary,Forrest R. Girouard,Alan Gould,Jennifer R. Hall,Matthew J. Holman,Andrew W. Howard,Steve B. Howell,Khadeejah A. Ibrahim,Karen Kinemuchi,Hans Kjeldsen,Todd C. Klaus,Jie Li,Philip W. Lucas,Søren Meibom,Robert L. Morris,Andrej Prsa,Elisa V. Quintana,Dwight T. Sanderfer,Dimitar Sasselov,Shawn Seader,Jeffrey C. Smith,Jason H. Steffen,Martin Still,Martin C. Stumpe,Jill Tarter,Peter Tenenbaum,Guillermo Torres,Joseph D. Twicken,Kamal Uddin,Jeffrey Van Cleve,Lucianne M. Walkowicz,William F. Welsh +77 more
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Journal ArticleDOI
Planet Occurrence within 0.25 AU of Solar-Type Stars from Kepler
Andrew W. Howard,Geoffrey W. Marcy,Stephen T. Bryson,Jon M. Jenkins,Jason F. Rowe,Natalie M. Batalha,William J. Borucki,David G. Koch,Edward W. Dunham,Thomas N. Gautier,Jeffrey Van Cleve,William D. Cochran,David W. Latham,Jack J. Lissauer,Guillermo Torres,Timothy M. Brown,Ronald L. Gilliland,Lars A. Buchhave,Douglas A. Caldwell,Jørgen Christensen-Dalsgaard,Jørgen Christensen-Dalsgaard,David R. Ciardi,Francois Fressin,Michael R. Haas,Steve B. Howell,Hans Kjeldsen,Sara Seager,Leslie A. Rogers,Dimitar Sasselov,Jason H. Steffen,Gibor Basri,David Charbonneau,Jessie L. Christiansen,B. D. Clarke,Andrea K. Dupree,Daniel C. Fabrycky,Debra A. Fischer,Eric B. Ford,Jonathan J. Fortney,Jill Tarter,Forrest R. Girouard,Matthew J. Holman,John Asher Johnson,Todd C. Klaus,P. Machalek,Althea V. Moorhead,Robert C. Morehead,Darin Ragozzine,Peter Tenenbaum,Joseph D. Twicken,Samuel N. Quinn,Howard Isaacson,Avi Shporer,Avi Shporer,Philip W. Lucas,Lucianne M. Walkowicz,William F. Welsh,Alan P. Boss,Edna DeVore,Alan Gould,Jeffrey C. Smith,Robert L. Morris,Andrej Prsa,Timothy D. Morton,Martin Still,Susan E. Thompson,Fergal Mullally,Michael Endl,Phillip J. MacQueen +68 more
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Journal ArticleDOI
The false positive rate of kepler and the occurrence of planets
Francois Fressin,Guillermo Torres,David Charbonneau,Stephen T. Bryson,Jessie L. Christiansen,Courtney D. Dressing,Jon M. Jenkins,Lucianne M. Walkowicz,Natalie M. Batalha +8 more
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The Occurrence of Potentially Habitable Planets Orbiting M Dwarfs Estimated from the Full Kepler Dataset and an Empirical Measurement of the Detection Sensitivity
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Journal ArticleDOI
Architecture and Dynamics of Kepler's Candidate Multiple Transiting Planet Systems
Jack J. Lissauer,Darin Ragozzine,Daniel C. Fabrycky,Jason H. Steffen,Eric B. Ford,Jon M. Jenkins,Avi Shporer,Avi Shporer,Matthew J. Holman,Jason F. Rowe,Elisa V. Quintana,Natalie M. Batalha,William J. Borucki,Stephen T. Bryson,Douglas A. Caldwell,Joshua A. Carter,David R. Ciardi,Edward W. Dunham,Jonathan J. Fortney,Thomas N. Gautier,Steve B. Howell,David G. Koch,David W. Latham,Geoffrey W. Marcy,Robert C. Morehead,Dimitar Sasselov +25 more
TL;DR: In this article, the authors characterize the dynamical properties of these candidate multi-planet systems and find that virtually all candidate systems are stable, as tested by numerical integrations that assume a nominal mass-radius relationship.
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