PLANET HUNTERS. VII. DISCOVERY OF A NEW LOW-MASS, LOW-DENSITY PLANET (PH3 C) ORBITING KEPLER-289 WITH MASS MEASUREMENTS OF TWO ADDITIONAL PLANETS (PH3 B AND D)
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Schmitt-2014-PLANET HUNTERS. VII.pdf
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Author(s)
Schmitt, Joseph R.
Agol, Eric
Deck, Katherine M.
Rogers, Leslie A.
Gazak, J. Zachary
Fischer, Debra A.
Wang, Ji
Holman, Matthew J.
Jek, Kian J.
Margossian, Charles
Date Issued
October 2014
Journal
The Astrophysical Journal
Publisher
IOP Publishing
Citation
Schmitt, Joseph R., Eric Agol, Katherine M. Deck, Leslie A. Rogers, J. Zachary Gazak, Debra A. Fischer, Ji Wang, et al. “PLANET HUNTERS. VII. DISCOVERY OF A NEW LOW-MASS, LOW-DENSITY PLANET (PH3 C) ORBITING KEPLER-289 WITH MASS MEASUREMENTS OF TWO ADDITIONAL PLANETS (PH3 B AND D).” The Astrophysical Journal 795, no. 2 (October 28, 2014): 167. © 2014 The American Astronomical Society
Version
Final published version
Abstract
We report the discovery of one newly confirmed planet (P = 66.06 days, R [subscript P] = 2.68 ± 0.17 R [subscript ⊕]) and mass determinations of two previously validated Kepler planets, Kepler-289 b (P = 34.55 days, R [subscript P] = 2.15 ± 0.10 R [subscript ⊕]) and Kepler-289-c (P = 125.85 days, R [subscript P] = 11.59 ± 0.10 R [subscript ⊕]), through their transit timing variations (TTVs). We also exclude the possibility that these three planets reside in a 1:2:4 Laplace resonance. The outer planet has very deep (~1.3%), high signal-to-noise transits, which puts extremely tight constraints on its host star's stellar properties via Kepler's Third Law. The star PH3 is a young (~1 Gyr as determined by isochrones and gyrochronology), Sun-like star with M [subscript *] = 1.08 ± 0.02 M [subscript ☉], R [subscript *] = 1.00 ± 0.02 R [subscript ☉], and T [subscript eff] = 5990 ± 38 K. The middle planet's large TTV amplitude (~5 hr) resulted either in non-detections or inaccurate detections in previous searches. A strong chopping signal, a shorter period sinusoid in the TTVs, allows us to break the mass-eccentricity degeneracy and uniquely determine the masses of the inner, middle, and outer planets to be M = 7.3 ± 6.8 M [subscript ⊕], 4.0 ± 0.9M [subscript ⊕], and M = 132 ± 17 M [subscript ⊕], which we designate PH3 b, c, and d, respectively. Furthermore, the middle planet, PH3 c, has a relatively low density, ρ = 1.2 ± 0.3 g cm[superscript –3] for a planet of its mass, requiring a substantial H/He atmosphere of 2.1[+0.8 over -0.3]% by mass, and joins a growing population of low-mass, low-density planets.
MIT Department
Massachusetts Institute of Technology. Department of Physics
MIT Kavli Institute for Astrophysics and Space Research
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DOI of Published Version
https://doi.org/10.1088/0004-637x/795/2/167
