Zhou, G, Huang, CX, Bakos, GÁ, Hartman, JD, Latham, DW, Quinn, SN, Collins, KA, Winn, JN, Wong, I, Kovács, G, Csubry, Z, Bhatti, W, Penev, K, Bieryla, A, Esquerdo, GA, Berlind, P, Calkins, ML, Val-Borro, MD, Noyes, RW, Lázár, J, Papp, I, Sári, P, Kovács, T, Buchhave, LA, Szklenar, T, Béky, B, Johnson, MC, Cochran, WD, Kniazev, AY, Stassun, KG, Fulton, BJ, Shporer, A, Espinoza, N, Bayliss, D, Everett, M, Howell, SB, Hellier, C, Anderson, DR, Cameron, AC, West, RG, Brown, DJA, Schanche, N, Barkaoui, K, Pozuelos, F, Gillon, M, Jehin, E, Benkhaldoun, Z, Daassou, A, Ricker, G, Vanderspek, R, Seager, S, Jenkins, JM, Lissauer, JJ, Armstrong, JD, Collins, KI, Gan, T, Hart, R, Horne, K, Kielkopf, JF, Nielsen, LD, Nishiumi, T, Narita, N, Palle, E, Relles, HM, Sefako, R, Tan, TG, Davies, M, Goeke, RF, Guerrero, N, Haworth, K and Villanueva, S (2019) Two New HATNet Hot Jupiters around A Stars and the First Glimpse at the Occurrence Rate of Hot Jupiters from TESS. Astronomical Journal, 158. 141 - 141. ISSN 0004-6256

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Wide-field surveys for transiting planets are well suited to searching diverse stellar populations, enabling a better understanding of the link between the properties of planets and their parent stars. We report the discovery of HAT-P-69 b (TOI 625.01) and HAT-P-70 b (TOI 624.01), two new hot Jupiters around A stars from the Hungarian-made Automated Telescope Network (HATNet) survey that have also been observed by the Transiting Exoplanet Survey Satellite. HAT-P-69 b has a mass of M Jup and a radius of R Jup and resides in a prograde 4.79 day orbit. HAT-P-70 b has a radius of R Jup and a mass constraint of M Jup and resides in a retrograde 2.74 day orbit. We use the confirmation of these planets around relatively massive stars as an opportunity to explore the occurrence rate of hot Jupiters as a function of stellar mass. We define a sample of 47,126 main-sequence stars brighter than T mag = 10 that yields 31 giant planet candidates, including 18 confirmed planets, 3 candidates, and 10 false positives. We find a net hot Jupiter occurrence rate of 0.41 ± 0.10% within this sample, consistent with the rate measured by Kepler for FGK stars. When divided into stellar mass bins, we find the occurrence rate to be 0.71 ± 0.31% for G stars, 0.43 ± 0.15% for F stars, and 0.26 ± 0.11% for A stars. Thus, at this point, we cannot discern any statistically significant trend in the occurrence of hot Jupiters with stellar mass.

Item Type: Article
Additional Information: This is the final published version of the article (version of record). It first appeared online via IOP Publishing Ltd. at https://doi.org/10.3847/1538-3881/ab36b5 - please refer to any applicable terms of use of the publisher.
Uncontrolled Keywords: planetary systems – stars: individual (HAT-P-69,HAT-P-70, TIC379929661, TIC399870368) – techniques: photometric – techniques: spectroscopic
Subjects: Q Science > QB Astronomy
Divisions: Faculty of Natural Sciences > School of Chemical and Physical Sciences
Depositing User: Symplectic
Date Deposited: 27 Sep 2019 13:00
Last Modified: 23 Mar 2021 11:13
URI: https://eprints.keele.ac.uk/id/eprint/6895

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