Masses, Radii, and Orbits of Small Kepler Planets: The Transition From Gaseous to Rocky Planets

@article{Marcy2014MassesRA,
  title={Masses, Radii, and Orbits of Small Kepler Planets: The Transition From Gaseous to Rocky Planets},
  author={G. Marcy and H. Isaacson and A. Howard and J. Rowe and J. Jenkins and S. Bryson and D. Latham and S. Howell and T. Gautier and N. Batalha and L. Rogers and D. Ciardi and D. Fischer and R. Gilliland and H. Kjeldsen and J. Christensen-Dalsgaard and D. Huber and W. Chaplin and S. Basu and L. Buchhave and S. Quinn and W. Borucki and D. Koch and R. Hunter and D. Caldwell and J. Cleve and R. Kolbl and L. Weiss and E. Petigura and S. Seager and T. Morton and J. Johnson and S. Ballard and C. Burke and W. Cochran and M. Endl and P. MacQueen and M. Everett and J. Lissauer and E. Ford and G. Torres and F. Fressin and T. Brown and J. Steffen and D. Charbonneau and G. Basri and D. Sasselov and J. Winn and R. Sanchis-Ojeda and J. Christiansen and E. Adams and C. Henze and A. Dupree and D. Fabrycky and J. Fortney and J. Tarter and M. Holman and P. Tenenbaum and A. Shporer and P. Lucas and W. Welsh and J. Orosz and T. Bedding and T. Campante and G. Davies and Y. Elsworth and R. Handberg and S. Hekker and C. Karoff and S. Kawaler and M. Lund and M. Lundkvist and T. Metcalfe and A. Miglio and V. S. Aguirre and D. Stello and T. White and A. Boss and E. Devore and A. Gould and A. Pr{\vs}a and E. Agol and T. Barclay and J. Coughlin and E. Brugamyer and F. Mullally and E. Quintana and M. Still and S. E. hompson and D. Morrison and J. Twicken and J. D'esert and J. Carter and J. Crepp and G. H'ebrard and A. Santerne and C. Moutou and C. Sobeck and D. Hudgins and M. R. Haas and P. Robertson and J. Lillo-box and D. Barrado},
  journal={Astrophysical Journal Supplement Series},
  year={2014},
  volume={210},
  pages={20}
}
We report on the masses, sizes, and orbits of the planets orbiting 22 Kepler stars. There are 49 planet candidates around these stars, including 42 detected through transits and 7 revealed by precise Doppler measurements of the host stars. Based on an analysis of the Kepler brightness measurements, along with high-resolution imaging and spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology, we establish low false-positive probabilities (FPPs) for all of the transiting planets… Expand
320 Citations
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