Kelt-19Ab: A P ~ 4.6-day Hot Jupiter Transiting a Likely Am Star with a Distant Stellar Companion


We present the discovery of the giant planet KELT-19Ab, which transits the moderately bright (V similar to 9.9) A8V star TYC 764-1494-1 with an orbital period of 4.61 days. We confirm the planetary nature of the companion via a combination of. radial velocities, which limit the mass to less than or similar to 4.1 M-J (3 sigma), and a clear Doppler tomography signal, which indicates a retrograde projected spin-orbit misalignment of lambda = -179.7(-3.7)(+3.8) degrees. Global modeling indicates that the T-eff=7500. 110 K host star has M-star = 1.62(-0.20)(+0.25) M-star and R-star = 1.83 +/- 0.10 R-circle dot. The planet has a radius of R-P = 1.91 +/- 0.11 R-J and receives a stellar insolation flux of similar to 3.2 x 10(9) erg s(-1) cm(-2), leading to an inferred equilibrium temperature of T-eq similar to 1935 K assuming zero albedo and complete heat redistribution. With a v sin I-* = 84.8 +/- 2.0 km s(-1), the host. is relatively slowly rotating compared to other stars with similar effective temperatures, and it appears to be enhanced in metallic elements but deficient in calcium, suggesting that it is likely an Am star. KELT-19A would be the first detection of an Am host of a transiting planet of which we are aware. Adaptive optics observations of the system reveal the existence of a companion with late-G9V/early-K1V spectral type at a projected separation of approximate to 160 au. Radial velocity measurements indicate that this companion is bound. Most Am stars are known to have stellar companions, which are often invoked to explain the relatively slow rotation of the primary. In this case, the stellar companion is unlikely to have caused the tidal braking of the primary. However, it may have emplaced the transiting planetary companion via the Kozai-Lidov mechanism.


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Outer planets, Extrasolar planets, Double stars, Spectroscopic imaging, Planets—Surfaces, Stars--Motion in line of sight

NSF CAREER Grant AST-1056524; National Science Foundation Graduate Research Fellowship under Grant No. DGE-1343012; NASA Hubble Fellowship grant HST-HF2-51402.001-A; NASA, under contract NAS 5-26555; National Aeronautics and Space Administration (EPSCOR grant NNX13AM97A); the Australian Research Council (LIEF grant LE140100050), and the National Science Foundation (grants 1516242 and 1608203).


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