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

Cochran, William D. and Fabrycky, Daniel C. and Torres, Guillermo and Fressin, Francois and Desert, Jean Michel and Ragozzine, Darin and Sasselov, Dimitar and Fortney, Jonathan J. and Rowe, Jason F. and Brugamyer, Erik J. and Bryson, Stephen T. and Carter, Joshua A. and Ciardi, David R. and Howell, Steve B. and Steffen, Jason H. and Borucki, William J. and Koch, David G. and Winn, Joshua N. and Welsh, William F. and Uddin, Kamal and Tenenbaum, Peter and Still, M. and Seager, Sara and Quinn, Samuel N. and Mullally, F. and Miller, Neil and Marcy, Geoffrey W. and MacQueen, Phillip J. and Lucas, Phillip and Lissauer, Jack J. and Latham, David W. and Knutson, Heather and Kinemuchi, K. and Johnson, John A. and Jenkins, Jon M. and Isaacson, Howard and Howard, Andrew and Horch, Elliott and Holman, Matthew J. and Henze, Christopher E. and Haas, Michael R. and Gilliland, Ronald L. and Gautier, Thomas N. and Ford, Eric B. and Fischer, Debra A. and Everett, Mark and Endl, Michael and Demory, Brice Oliver and Deming, Drake and Charbonneau, David and Caldwell, Douglas and Buchhave, Lars and Brown, Timothy M. and Batalha, Natalie (2011) 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. Astrophysical Journal, Supplement Series, 197 (1). pp. 7-25. ISSN 0067-0049

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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 ⊕, an' 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.

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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Access to published version in accordance with the copyright policy of the publisher.
Faculty / Department / School: No Faculty
Date Deposited: 18 Jun 2017 23:02
Last Modified: 27 Jun 2017 01:19
Uncontrolled Keywords: planetary systems; stars; Kepler-18; KIC 8644288; 2MASS J19521906+4444467; photometry; spectroscopy
Fields of Research : 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems
02 Physical Sciences > 0201 Astronomical and Space Sciences > 020102 Astronomical and Space Instrumentation
Socio-Economic Objective: E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences
Identification Number or DOI: 10.1088/0067-0049/197/1/7

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