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Title: KELT-19Ab: A P ∼ 4.6-day Hot Jupiter Transiting a Likely Am Star with a Distant Stellar Companion
Authors: Siverd, RJ
Collins, KA
Zhou, G
Quinn, SN
Gaudi, BS
Stassun, KG
Johnson, MC
Bieryla, A
Latham, DW
Ciardi, DR
Rodriguez, JE
Penev, K
Pinsonneault, M
Pepper, J
Eastman, JD
Relles, H
Kielkopf, JF
Gregorio, J
Oberst, TE
Aldi, GF
Esquerdo, GA
Calkins, ML
Berlind, P
Dressing, CD
Patel, R
Stevens, DJ
Beatty, TG
Lund, MB
Labadie-Bartz, J
Kuhn, RB
Colón, KD
James, D
Yao, X
Johnson, JA
Wright, JT
McCrady, N
Wittenmyer, RA
Johnson, SA
Sliski, DH
Jensen, ELN
Cohen, DH
McLeod, KK
Penny, MT
Joner, MD
Stephens, DC
Villanueva, S
Zambelli, R
Stockdale, C
Evans, P
Tan, TG
Curtis, IA
Reed, PA
Trueblood, M
Trueblood, P
First Published: 22-Dec-2017
Publisher: American Astronomical Society, IOP Publishing
Citation: Astronomical Journal, 2018, 155 (1)
Abstract: We present the discovery of the giant planet KELT-19Ab, which transits the moderately bright (V ∼ 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 ≳4.1 MJ (3s), and a clear Doppler tomography signal, which indicates a retrograde projected spin-orbit misalignment of λ = -179.7-3.8+3.7degrees. Global modeling indicates that the Teff= 7500 ±110 K host star has M M = 1.62+0.20-0.25and R = 1.83 0.10 R. The planet has a radius of RP = 1.91 0.11 RJ and receives a stellar insolation flux of ∼ 3.2 10 erg s-1cm-2, leading to an inferred equilibrium temperature of Teq ∼ 1935 K assuming zero albedo and complete heat redistribution. With a v I sin 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 »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.
DOI Link: 10.3847/1538-3881/aa9e4d
ISSN: 0004-6256
Version: Publisher Version
Status: Peer-reviewed
Type: Journal Article
Rights: Copyright © 2018, American Astronomical Society, IOP Publishing. Deposited with reference to the publisher’s open access archiving policy. (
Appears in Collections:Published Articles, Dept. of Physics and Astronomy

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