KELT-23Ab: A Hot Jupiter Transiting a Near-solar Twin Close to the TESS and JWST Continuous Viewing Zones
AuthorBeatty, Thomas G.
AffiliationUniv Arizona, Dept Astron
Univ Arizona, Steward Observ
planets and satellites: detection
planets and satellites: gaseous planets
techniques: radial velocities
MetadataShow full item record
PublisherIOP PUBLISHING LTD
CitationDaniel Johns et al 2019 AJ 158 78
RightsCopyright © 2019. The American Astronomical Society. All rights reserved.
Collection InformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at firstname.lastname@example.org.
AbstractWe announce the discovery of KELT-23Ab, a hot Jupiter transiting the relatively bright (V = 10.3) star BD+66 911 (TYC 4187-996-1), and characterize the system using follow-up photometry and spectroscopy. A global fit to the system yields host-star properties of T-eff = 5900 +/- 49 K, M* = 0.945(-0.054)(+0.060) M-circle dot, R* = 0.995 +/- 0.015 R-circle dot, L* = 1.082(-0.048)(+0.051) L-circle dot, log g* = 4.418(-0.025)(+0.026). (cgs), and [Fe/H] = -0.105 +/- 0.077. KELT-23Ab is a hot Jupiter with a mass of M-p = 0.938(-0.042)(+0.045). M-J, radius of R-p = 1.322 0.025 R-J, and density of rho(p) = 0.504(0.035)(+0.038) g cm(-3). Intense insolation flux from the star has likely caused KELT-23Ab to become inflated. The time of inferior conjunction is T-0 = 2458149.40776 +/- 0.00091 BJD(TDB) and the orbital period is P = 2.255353(-0.000030)(+0.000031) ON days. There is strong evidence that KELT-23A is a member of a long-period binary star system with a less luminous companion, and due to tidal interactions, the planet is likely to spiral into its host within roughly a gigayear. This system has one of the highest positive ecliptic latitudes of all transiting planet hosts known to date, placing it near the Transiting Planet Survey Satellite and James Webb Space Telescope continuous viewing zones. Thus we expect it to be an excellent candidate for long-term monitoring and follow up with these facilities.
VersionFinal published version
SponsorsOhio State University; Vanderbilt University; Lehigh University; Harvard Future Faculty Leaders Postdoctoral fellowship; NSF CAREER Grant [AST-1056524]; National Science Foundation [DGE-1343012, 1559487]; Space Telescope Science Institute [HST-HF2-51402.001-A]; NASA [NAS 5-26555, 80NSSC18K1009, NNX17AB94G]; National Aeronautics and Space Administration; FAPESP [2017/23731-1]; Carol and Ray Neag Undergraduate Research Fund; KELT follow-up collaboration