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dc.contributor.authorZhou, G.
dc.contributor.authorHuang, C. X.
dc.contributor.authorBakos, G. Á.
dc.contributor.authorHartman, J. D.
dc.contributor.authorLatham, David W.
dc.contributor.authorQuinn, S. N.
dc.contributor.authorCollins, K. A.
dc.contributor.authorWinn, J. N.
dc.contributor.authorWong, I.
dc.contributor.authorKovács, G.
dc.contributor.authorCsubry, Z.
dc.contributor.authorBhatti, W.
dc.contributor.authorPenev, K.
dc.contributor.authorBieryla, A.
dc.contributor.authorEsquerdo, G. A.
dc.contributor.authorBerlind, P.
dc.contributor.authorCalkins, M. L.
dc.contributor.authorde Val-Borro, M.
dc.contributor.authorNoyes, R. W.
dc.contributor.authorLázár, J.
dc.contributor.authorPapp, I.
dc.contributor.authorSári, P.
dc.contributor.authorKovács, T.
dc.contributor.authorBuchhave, Lars A.
dc.contributor.authorSzklenar, T.
dc.contributor.authorBéky, B.
dc.contributor.authorJohnson, M. C.
dc.contributor.authorCochran, W. D.
dc.contributor.authorKniazev, A. Y.
dc.contributor.authorStassun, K. G.
dc.contributor.authorFulton, B. J.
dc.contributor.authorShporer, A.
dc.contributor.authorEspinoza, N.
dc.contributor.authorBayliss, D.
dc.contributor.authorEverett, M.
dc.contributor.authorHowell, S. B.
dc.contributor.authorHellier, C.
dc.contributor.authorAnderson, D. R.
dc.contributor.authorCameron, A. Collier
dc.contributor.authorWest, R. G.
dc.contributor.authorBrown, D. J. A.
dc.contributor.authorSchanche, N.
dc.contributor.authorBarkaoui, K.
dc.contributor.authorPozuelos, F.
dc.contributor.authorGillon, M.
dc.contributor.authorJehin, E.
dc.contributor.authorBenkhaldoun, Z.
dc.contributor.authorDaassou, A.
dc.contributor.authorRicker, G.
dc.contributor.authorVanderspek, R.
dc.contributor.authorSeager, S.
dc.contributor.authorJenkins, J.M.
dc.contributor.authorLissauer, Jack J.
dc.contributor.authorArmstrong, J.D.
dc.contributor.authorCollins, K. I.
dc.contributor.authorGan, T.
dc.contributor.authorHart, R.
dc.contributor.authorHorne, K.
dc.contributor.authorKielkopf, J. F.
dc.contributor.authorNielsen, L.D.
dc.contributor.authorNishiumi, T.
dc.contributor.authorNarita, N.
dc.contributor.authorPalle, E.
dc.contributor.authorRelles, H.M.
dc.contributor.authorSefako, R.
dc.contributor.authorTan, T.G.
dc.contributor.authorDavies, M.
dc.contributor.authorGoeke, Robert F.
dc.contributor.authorGuerrero, N.
dc.contributor.authorHaworth, K.
dc.contributor.authorVillanueva, S.
dc.date.accessioned2019-08-02T14:30:06Z
dc.date.available2019-08-02T14:30:06Z
dc.date.issued2019-10
dc.identifier.citationZhou , 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/ab36b5en
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 260363600
dc.identifier.otherPURE UUID: 61de1a8f-2bb6-4fbc-b773-17a827f458de
dc.identifier.otherArXiv: http://arxiv.org/abs/1906.00462v2
dc.identifier.otherORCID: /0000-0002-8863-7828/work/61978774
dc.identifier.otherScopus: 85075253842
dc.identifier.otherWOS: 000485726200002
dc.identifier.urihttp://hdl.handle.net/10023/18238
dc.description.abstractWide-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.extent24
dc.language.isoeng
dc.relation.ispartofAstronomical Journalen
dc.rights© 2019 American Astronomical Society. This work has been made available online in accordance with the publisher's policies. This is the author created accepted version manuscript following peer review and as such may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.3847/1538-3881/ab36b5en
dc.subjectP;anetary systemsen
dc.subjectStars: individual (HAT-P-69,HAT-P-70, TIC379929661, TIC399870368)en
dc.subjectTechniques: photometricen
dc.subjectTechniques: spectroscopicen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleTwo new HATNet hot Jupiters around A stars, and the first glimpse at the occurrence rate of hot Jupiters from TESS*en
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.3847/1538-3881/ab36b5
dc.description.statusPeer revieweden


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