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Two new HATNet hot Jupiters around A stars, and the first glimpse at the occurrence rate of hot Jupiters from TESS*
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dc.contributor.author | Zhou, G. | |
dc.contributor.author | Huang, C. X. | |
dc.contributor.author | Bakos, G. Á. | |
dc.contributor.author | Hartman, J. D. | |
dc.contributor.author | Latham, David W. | |
dc.contributor.author | Quinn, S. N. | |
dc.contributor.author | Collins, K. A. | |
dc.contributor.author | Winn, J. N. | |
dc.contributor.author | Wong, I. | |
dc.contributor.author | Kovács, G. | |
dc.contributor.author | Csubry, Z. | |
dc.contributor.author | Bhatti, W. | |
dc.contributor.author | Penev, K. | |
dc.contributor.author | Bieryla, A. | |
dc.contributor.author | Esquerdo, G. A. | |
dc.contributor.author | Berlind, P. | |
dc.contributor.author | Calkins, M. L. | |
dc.contributor.author | de Val-Borro, M. | |
dc.contributor.author | Noyes, R. W. | |
dc.contributor.author | Lázár, J. | |
dc.contributor.author | Papp, I. | |
dc.contributor.author | Sári, P. | |
dc.contributor.author | Kovács, T. | |
dc.contributor.author | Buchhave, Lars A. | |
dc.contributor.author | Szklenar, T. | |
dc.contributor.author | Béky, B. | |
dc.contributor.author | Johnson, M. C. | |
dc.contributor.author | Cochran, W. D. | |
dc.contributor.author | Kniazev, A. Y. | |
dc.contributor.author | Stassun, K. G. | |
dc.contributor.author | Fulton, B. J. | |
dc.contributor.author | Shporer, A. | |
dc.contributor.author | Espinoza, N. | |
dc.contributor.author | Bayliss, D. | |
dc.contributor.author | Everett, M. | |
dc.contributor.author | Howell, S. B. | |
dc.contributor.author | Hellier, C. | |
dc.contributor.author | Anderson, D. R. | |
dc.contributor.author | Cameron, A. Collier | |
dc.contributor.author | West, R. G. | |
dc.contributor.author | Brown, D. J. A. | |
dc.contributor.author | Schanche, N. | |
dc.contributor.author | Barkaoui, K. | |
dc.contributor.author | Pozuelos, F. | |
dc.contributor.author | Gillon, M. | |
dc.contributor.author | Jehin, E. | |
dc.contributor.author | Benkhaldoun, Z. | |
dc.contributor.author | Daassou, A. | |
dc.contributor.author | Ricker, G. | |
dc.contributor.author | Vanderspek, R. | |
dc.contributor.author | Seager, S. | |
dc.contributor.author | Jenkins, J.M. | |
dc.contributor.author | Lissauer, Jack J. | |
dc.contributor.author | Armstrong, J.D. | |
dc.contributor.author | Collins, K. I. | |
dc.contributor.author | Gan, T. | |
dc.contributor.author | Hart, R. | |
dc.contributor.author | Horne, K. | |
dc.contributor.author | Kielkopf, J. F. | |
dc.contributor.author | Nielsen, L.D. | |
dc.contributor.author | Nishiumi, T. | |
dc.contributor.author | Narita, N. | |
dc.contributor.author | Palle, E. | |
dc.contributor.author | Relles, H.M. | |
dc.contributor.author | Sefako, R. | |
dc.contributor.author | Tan, T.G. | |
dc.contributor.author | Davies, M. | |
dc.contributor.author | Goeke, Robert F. | |
dc.contributor.author | Guerrero, N. | |
dc.contributor.author | Haworth, K. | |
dc.contributor.author | Villanueva, S. | |
dc.date.accessioned | 2019-08-02T14:30:06Z | |
dc.date.available | 2019-08-02T14:30:06Z | |
dc.date.issued | 2019-10 | |
dc.identifier | 260363600 | |
dc.identifier | 61de1a8f-2bb6-4fbc-b773-17a827f458de | |
dc.identifier | 85075253842 | |
dc.identifier | 000485726200002 | |
dc.identifier.citation | Zhou , G , Huang , C X , Bakos , G Á , Hartman , J D , Latham , D W , Quinn , S N , Collins , K A , Winn , J N , Wong , I , Kovács , G , Csubry , Z , Bhatti , W , Penev , K , Bieryla , A , Esquerdo , G A , Berlind , P , Calkins , M L , de Val-Borro , M , Noyes , R W , Lázár , J , Papp , I , Sári , P , Kovács , T , Buchhave , L A , Szklenar , T , Béky , B , Johnson , M C , Cochran , W D , Kniazev , A Y , Stassun , K G , Fulton , B J , Shporer , A , Espinoza , N , Bayliss , D , Everett , M , Howell , S B , Hellier , C , Anderson , D R , Cameron , A C , West , R G , Brown , D J A , Schanche , N , Barkaoui , K , Pozuelos , F , Gillon , M , Jehin , E , Benkhaldoun , Z , Daassou , A , Ricker , G , Vanderspek , R , Seager , S , Jenkins , J M , Lissauer , J J , Armstrong , J D , Collins , K I , Gan , T , Hart , R , Horne , K , Kielkopf , J F , Nielsen , L D , Nishiumi , T , Narita , N , Palle , E , Relles , H M , Sefako , R , Tan , T G , Davies , M , Goeke , R F , Guerrero , N , Haworth , K & 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 , vol. 158 , no. 4 , 141 , pp. 1-24 . https://doi.org/10.3847/1538-3881/ab36b5 | en |
dc.identifier.issn | 0004-6256 | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/1906.00462v2 | |
dc.identifier.other | ORCID: /0000-0002-8863-7828/work/61978774 | |
dc.identifier.uri | https://hdl.handle.net/10023/18238 | |
dc.description.abstract | 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 3.58+0.58/-0.58 M Jup and a radius of 1.676+0.051/-0.033 R Jup and resides in a prograde 4.79 day orbit. HAT-P-70 b has a radius of 1.87+0.15/-0.10 R Jup and a mass constraint of <6.78 (3σ) 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. | |
dc.format.extent | 24 | |
dc.format.extent | 2078450 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astronomical Journal | en |
dc.subject | P;anetary systems | en |
dc.subject | Stars: individual (HAT-P-69,HAT-P-70, TIC379929661, TIC399870368) | en |
dc.subject | Techniques: photometric | en |
dc.subject | Techniques: spectroscopic | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | NDAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Two new HATNet hot Jupiters around A stars, and the first glimpse at the occurrence rate of hot Jupiters from TESS* | en |
dc.type | Journal article | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.identifier.doi | 10.3847/1538-3881/ab36b5 | |
dc.description.status | Peer reviewed | en |
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