Kepler-18b,c, and d: a system of three planets confirmed by transit timing variations, light curve validation, Warm-Spitzer photometry, and radial velocity measurements

William D. Cochran, Daniel C. Fabrycky, Guillermo Torres, François Fressin, Jean-Michel Desert, Darin Ragozzine, Dimitar Sasselov, Jonathan J. Fortney, Jason F. Rowe, Erik J. Brugamyer, Stephen T. Bryson, Joshua A. Carter, David R. Ciardi, Steve B. Howell, Jason H. Steffen, William J. Borucki, David G. Koch, Joshua N. Winn, William F. Welsh, Kamal UddinPeter Tenenbaum, M. Still, Sara Seager, Samuel N. Quinn, F. Mullally, Niel Miller, Geoffrey W. Marcy, Phillip J. MacQueen, Phillip Lucas, Jack J. Lissauer, David W. Latham, Heather Knutson, K. Kinemuchi, John A. Johnson, Jon M. Jenkins, Howard Isaacson, Andrew Howard, Elliott Horch, Matthew J. Holman, Christopher E. Henze, Michael R. Haas, Ronald L. Gilliland, Thomas N. Gautier, Eric B. Ford, Debra A. Fischer, Mark Everett, Michael Endl, Brice-Oliver Demory, Drake Deming, David Charbonneau, Douglas Caldwell, Lars A. Buchhave, Timothy M. Brown, Natalie Batalha

124 Citationer (Scopus)

Abstract

We report the detection of three transiting planets around a Sun-like star, which we designate Kepler-18. The transit signals were detected in photometric data from the Kepler satellite, and were confirmed to arise from planets using a combination of large transit-timing variations (TTVs), radial velocity variations, Warm-Spitzer observations, and statistical analysis of false-positive probabilities. The Kepler-18 star has a mass of 0.97 M , a radius of 1.1 R , an effective temperature of 5345K, and an iron abundance of [Fe/H] = +0.19. The planets have orbital periods of approximately 3.5, 7.6, and 14.9 days. The innermost planet "b" is a "super-Earth" with a mass of 6.9 ± 3.4 M , a radius of 2.00 ± 0.10 R , and a mean density of 4.9 ± 2.4gcm3. The two outer planets "c" and "d" are both low-density Neptune-mass planets. Kepler-18c has a mass of 17.3 ± 1.9 M , a radius of 5.49 ± 0.26 R , and a mean density of 0.59 0.07gcm 3, while Kepler-18d has a mass of 16.4 ± 1.4 M , a radius of 6.98 ± 0.33 R and a mean density of 0.27 ± 0.03gcm3. Kepler-18c and Kepler-18d have orbital periods near a 2:1 mean-motion resonance, leading to large and readily detected TTVs.

OriginalsprogEngelsk
Artikelnummer7
TidsskriftAstrophysical Journal Supplement Series
Vol/bind197
Udgave nummer1
Antal sider19
ISSN0067-0049
DOI
StatusUdgivet - 1 nov. 2011

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