An Eccentric Massive Jupiter Orbiting a Subgiant on a 9.5-day Period Discovered in the Transiting Exoplanet Survey Satellite Full Frame Images
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Rodriguez_2019_AJ_157_191.pdf
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Published version
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1.9 MB
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Author(s)
Rodriguez, Joseph E.
Quinn, Samuel N.
Huang, Chelsea X.
Vanderburg, Andrew
Penev, Kaloyan
Brahm, Rafael
Jordán, Andrés
Ikwut-Ukwa, Mma
Tsirulik, Shelly
Latham, David W.
Date Issued
April 2019
Journal
Astronomical Journal
Publisher
American Astronomical Society
Citation
Rodriguez, Joseph A. et al. "An Eccentric Massive Jupiter Orbiting a Subgiant on a 9.5-day Period Discovered in the Transiting Exoplanet Survey Satellite Full Frame Images." Astronomical Journal 157, 5 (April 2019): 191 © 2019 American Astronomical Society
Version
Final published version
Abstract
We report the discovery of TOI-172 b from the Transiting Exoplanet Survey Satellite (TESS) mission, a massive hot Jupiter transiting a slightly evolved G star with a 9.48-day orbital period. This is the first planet to be confirmed from analysis of only the TESS full frame images, because the host star was not chosen as a two-minute cadence target. From a global analysis of the TESS photometry and follow-up observations carried out by the TESS Follow-up Observing Program Working Group, TOI-172 (TIC 29857954) is a slightly evolved star with an effective temperature of T eff = 5645 ± 50 K, a mass of M ∗ = 1.128-0.061+0.065 M o, radius of R ∗ = 1.777-0.044+0.047 R o, a surface gravity of log g ∗ = 3.993-0.028+0.027, and an age of 7.4-1.5+1.6. Its planetary companion (TOI-172 b) has a radius of R P = 0.965-0.029+0.032 R J, a mass of M P = 5.42-0.20+0.22 M J, and is on an eccentric orbit (e = 0.3806-0.0090+0.0093 ). TOI-172 b is one of the few known massive giant planets on a highly eccentric short-period orbit. Future study of the atmosphere of this planet and its system architecture offer opportunities to understand the formation and evolution of similar systems.
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/10.3847/1538-3881/ab11d9
