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

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arxiv 1401.4195 v1 pith:ZG4OPCCF submitted 2014-01-16 astro-ph.EP

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

Geoffrey W. Marcy , Howard Isaacson , Andrew W. Howard , Jason F. Rowe , Jon M. Jenkins , Stephen T. Bryson , David W. Latham , Steve B. Howell
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Thomas N. Gautier III Natalie M. Batalha Leslie A. Rogers David Ciardi Debra A. Fischer Ronald L. Gilliland Hans Kjeldsen J{\o}rgen Christensen-Dalsgaard Daniel Huber William J. Chaplin Sarbani Basu Lars A. Buchhave Samuel N. Quinn William J. Borucki David G. Koch Roger Hunter Douglas A. Caldwell Jeffrey Van Cleve Rea Kolbl Lauren M. Weiss Erik Petigura Sara Seager Timothy Morton John Asher Johnson Sarah Ballard Chris Burke William D. Cochran Michael Endl Phillip MacQueen Mark E. Everett Jack J. Lissauer Eric B. Ford Guillermo Torres Francois Fressin Timothy M. Brown Jason H. Steffen David Charbonneau Gibor S. Basri Dimitar D. Sasselov Joshua Winn Roberto Sanchis-Ojeda Jessie Christiansen Elisabeth Adams Christopher Henze Andrea Dupree Daniel C. Fabrycky Jonathan J. Fortney Jill Tarter Matthew J. Holman Peter Tenenbaum Avi Shporer Philip W. Lucas William F. Welsh Jerome A. Orosz T. R. Bedding T. L. Campante G. R. Davies Y. Elsworth R. Handberg S. Hekker C. Karoff S. D. Kawaler M. N. Lund M. Lundkvist T. S. Metcalfe A. Miglio V. Silva Aguirre D. Stello T. R. White Alan Boss Edna Devore Alan Gould Andrej Prsa Eric Agol Thomas Barclay Jeff Coughlin Erik Brugamyer Fergal Mullally Elisa V. Quintana Martin Still Susan E. hompson David Morrison Joseph D. Twicken Jean-Michel D\'esert Josh Carter Justin R. Crepp Guillaume H\'ebrard Alexandre Santerne Claire Moutou Charlie Sobeck Douglas Hudgins Michael R. Haas Paul Robertson Jorge Lillo-Box David Barrado
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classification astro-ph.EP
keywords planetsmassesrockystarsdopplerkeplermeasurementscomposition
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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 for all of the transiting planets (41 of 42 have a false-positive probability under 1%), and we constrain their sizes and masses. Most of the transiting planets are smaller than 3X the size of Earth. For 16 planets, the Doppler signal was securely detected, providing a direct measurement of the planet's mass. For the other 26 planets we provide either marginal mass measurements or upper limits to their masses and densities; in many cases we can rule out a rocky composition. We identify 6 planets with densities above 5 g/cc, suggesting a mostly rocky interior for them. Indeed, the only planets that are compatible with a purely rocky composition are smaller than ~2 R_earth. Larger planets evidently contain a larger fraction of low-density material (H, He, and H2O).

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