Three short-period Jupiters from TESS

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dc.contributor.authorNielsen, L. D.
dc.contributor.authorBrahm, R.
dc.contributor.authorBouchy, F.
dc.contributor.authorEspinoza, N.
dc.contributor.authorTurner, O.
dc.contributor.authorRappaport, S.
dc.contributor.authorPearce, L.
dc.contributor.authorRicker, G.
dc.contributor.authorVanderspek, R.
dc.contributor.authorLatham, D. W.
dc.contributor.authorSeager, S.
dc.contributor.authorWinn, J. N.
dc.contributor.authorJenkins, J. M.
dc.contributor.authorActon, J. S.
dc.contributor.authorBakos, G.
dc.contributor.authorBarclay, T.
dc.contributor.authorBarkaoui, K.
dc.contributor.authorBhatti, W.
dc.contributor.authorBriceño, C.
dc.contributor.authorBryant, E. M.
dc.contributor.authorBurleigh, M. R.
dc.contributor.authorCiardi, D. R.
dc.contributor.authorCollins, K. A.
dc.contributor.authorCollins, K. I.
dc.contributor.authorCooke, B. F.
dc.contributor.authorCsubry, Z.
dc.contributor.authordos Santos, L. A.
dc.contributor.authorEigmüller, Ph.
dc.contributor.authorFausnaugh, M. M.
dc.contributor.authorGan, T.
dc.contributor.authorGillon, M.
dc.contributor.authorGoad, M. R.
dc.contributor.authorGuerrero, N.
dc.contributor.authorHagelberg, J.
dc.contributor.authorHart, R.
dc.contributor.authorHenning, T.
dc.contributor.authorHuang, C. X.
dc.contributor.authorJehin, E.
dc.contributor.authorJenkins, J. S.
dc.contributor.authorJordán, A.
dc.contributor.authorKielkopf, J. F.
dc.contributor.authorKossakowski, D.
dc.contributor.authorLavie, B.
dc.contributor.authorLaw, N.
dc.contributor.authorLendl, M.
dc.contributor.authorde Leon, J. P.
dc.contributor.authorLovis, C.
dc.contributor.authorMann, A. W.
dc.contributor.authorMarmier, M.
dc.contributor.authorMcCormac, J.
dc.contributor.authorMori, M.
dc.contributor.authorMoyano, M.
dc.contributor.authorNarita, N.
dc.contributor.authorOsip, D.
dc.contributor.authorOtegi, J. F.
dc.contributor.authorPepe, F.
dc.contributor.authorPozuelos, F. J.
dc.contributor.authorRaynard, L.
dc.contributor.authorRelles, H. M.
dc.contributor.authorSarkis, P.
dc.contributor.authorSégransan, D.
dc.contributor.authorSeidel, J. V.
dc.contributor.authorShporer, A.
dc.contributor.authorStalport, M.
dc.contributor.authorStockdale, C.
dc.contributor.authorSuc, V.
dc.contributor.authorTamura, M.
dc.contributor.authorTan, T. G.
dc.contributor.authorTilbrook, R. H.
dc.contributor.authorTing, E. B.
dc.contributor.authorTrifonov, T.
dc.contributor.authorUdry, S.
dc.contributor.authorVanderburg, A.
dc.contributor.authorWheatley, P. J.
dc.contributor.authorWingham, G.
dc.contributor.authorZhan, Z.
dc.contributor.authorZiegler, C.
dc.date.accessioned2020-10-21T17:27:15Z
dc.date.available2020-10-21T17:27:15Z
dc.date.issued2020-07-13
dc.description.abstractWe report the confirmation and mass determination of three hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HIP 65Ab (TOI-129, TIC-201248411) is an ultra-short-period Jupiter orbiting a bright (V = 11.1 mag) K4-dwarf every 0.98 days. It is a massive 3.213 ± 0.078 MJ planet in a grazing transit configuration with an impact parameter of b = 1.17₋₀.₀₈⁺⁰˙¹⁰. As a result the radius is poorly constrained, 2.03₋₀.₄₉⁺⁰˙⁶¹RJ. The planet’s distance to its host star is less than twice the separation at which it would be destroyed by Roche lobe overflow. It is expected to spiral into HIP 65A on a timescale ranging from 80 Myr to a few gigayears, assuming a reduced tidal dissipation quality factor of Qs′ = 107 − 109. We performed a full phase-curve analysis of the TESS data and detected both illumination- and ellipsoidal variations as well as Doppler boosting. HIP 65A is part of a binary stellar system, with HIP 65B separated by 269 AU (3.95 arcsec on sky). TOI-157b (TIC 140691463) is a typical hot Jupiter with a mass of 1.18 ± 0.13 MJ and a radius of 1.29 ± 0.02 RJ. It has a period of 2.08 days, which corresponds to a separation of just 0.03 AU. This makes TOI-157 an interesting system, as the host star is an evolved G9 sub-giant star (V = 12.7). TOI-169b (TIC 183120439) is a bloated Jupiter orbiting a V = 12.4 G-type star. It has a mass of 0.79 ±0.06 MJ and a radius of 1.09₋₀.₀₅⁺⁰˙⁰⁸RJ. Despite having the longest orbital period (P = 2.26 days) of the three planets, TOI-169b receives the most irradiation and is situated on the edge of the Neptune desert. All three host stars are metal rich with [Fe / H] ranging from 0.18 to 0.24.en_US
dc.description.sponsorshipWe thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to our planet search programmes. This work has been in particular carried out in the frame of the National Centre for Competence in Research ‘PlanetS’ supported by the Swiss National Science Foundation (SNSF). This publication makes use of The Data & Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA Explorer Program. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has made use of Aladin sky atlas developed at CDS, Strasbourg Observatory, France. This work makes use of observations from the LCOGT network. This work is partly supported by JSPS KAKENHI Grant Numbers JP15H02063, JP18H01265, JP18H05439, JP18H05442, and JST PRESTO Grant Number JPMJPR1775. The IRSF project is a collaboration between Nagoya University and the South African Astronomical Observatory (SAAO) supported by the Grants-in-Aid for Scientific Research on Priority Areas (A) (Nos. 10147207 and 10147214) and Optical & Near-Infrared Astronomy Inter-University Cooperation Program, from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan and the National Research Foundation (NRF) of South Africa. We thank Akihiko Fukui, Nobuhiko Kusakabe, Kumiko Morihana, Tetsuya Nagata, Takahiro Nagayama, Taku Nishiumi, and the staff of SAAO for their kind supports for IRSF SIRIUS observations and analyses. The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Fundation (SNF). MG and EJ are F.R.S.-FNRS Senior Research Associate. R.B. acknowledges support from FONDECYT Post-doctoral Fellowship Project 3180246, and from the Millennium Institute of Astrophysics (MAS). A.J. acknowledges support from FONDECYT project 1171208 and by the Ministry for the Economy, Development, and Tourism’s Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). JSJ acknowledge support by FONDECYT grant 1161218 and partial support from CONICYT project Basal AFB-170002. JVS and LAdS are supported by funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project Four Aces; grant agreement No 724427). L.A.P. is supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-1746060. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Science Foundation. Includes data collected under the NGTS project at the ESO La Silla Paranal Observatory. The NGTS facility is funded by the University of Warwick, the University of Leicester, Queen’s University Belfast, the University of Geneva, the Deutsches Zentrum für Luft- und Raumfahrt e.V. (DLR; under the ‘Großinvestition GI-NGTS’), the University of Cambridge and the UK Science and Technology Facilities Council (STFC; project references ST/M001962/1 and ST/S002642/1). Staff from the University of Warwick acknowledge support from STFC consolidated grant ST/P000495/1.en_US
dc.description.urihttps://www.aanda.org/articles/aa/abs/2020/07/aa37941-20/aa37941-20.htmlen_US
dc.format.extent16 pagesen_US
dc.genrejournal articlesen_US
dc.identifierdoi:10.13016/m22ddh-y2du
dc.identifier.citationNielsen, L. D.; Brahm, R.; Bouchy, F.; Espinoza, N.; Turner, O.; Rappaport, S.; Pearce, L.; Ricker, G.; Vanderspek, R.; Latham, D. W.; Seager, S.; Winn, J. N.; Jenkins, J. M.; Acton, J. S.; Bakos, G.; Barclay, T.; Barkaoui, K.; Bhatti, W.; Briceño, C.; Bryant, E. M.; Burleigh, M. R.; Ciardi, D. R.; Collins, K. A.; Collins, K. I.; Cooke, B. F.; Csubry, Z.; dos Santos, L. A.; Eigmüller, Ph.; Fausnaugh, M. M.; Gan, T.; Gillon, M.; Goad, M. R.; Guerrero, N.; Hagelberg, J.; Hart, R.; Henning, T.; Huang, C. X.; Jehin, E.; Jenkins, J. S.; Jordán, A.; Kielkopf, J. F.; Kossakowski, D.; Lavie, B.; Law, N.; Lendl, M.; de Leon, J. P.; Lovis, C.; Mann, A. W.; Marmier, M.; McCormac, J.; Mori, M.; Moyano, M.; Narita, N.; Osip, D.; Otegi, J. F.; Pepe, F.; Pozuelos, F. J.; Raynard, L.; Relles, H. M.; Sarkis, P.; Ségransan, D.; Seidel, J. V.; Shporer, A.; Stalport, M.; Stockdale, C.; Suc, V.; Tamura, M.; Tan, T. G.; Tilbrook, R. H.; Ting, E. B.; Trifonov, T.; Udry, S.; Vanderburg, A.; Wheatley, P. J.; Wingham, G.; Zhan, Z.; Ziegler, C.; Three short-period Jupiters from TESS; Astronomy & Astrophysics, Volume 639, July 2020, Article Number - A76; https://www.aanda.org/articles/aa/abs/2020/07/aa37941-20/aa37941-20.htmlen_US
dc.identifier.urihttps://doi.org/10.1051/0004-6361/202037941
dc.identifier.urihttp://hdl.handle.net/11603/19942
dc.language.isoen_USen_US
dc.publisherEDP Sciencesen_US
dc.relation.isAvailableAtThe University of Maryland, Baltimore County (UMBC)
dc.relation.ispartofUMBC Center for Space Sciences and Technology
dc.relation.ispartofUMBC Faculty Collection
dc.relation.ispartofUMBC Physics Department
dc.rightsThis item is likely protected under Title 17 of the U.S. Copyright Law. Unless on a Creative Commons license, for uses protected by Copyright Law, contact the copyright holder or the author.
dc.rightsPublic Domain Mark 1.0*
dc.rightsThis work was written as part of one of the author's official duties as an Employee of the United States Government and is therefore a work of the United States Government. In accordance with 17 U.S.C. 105, no copyright protection is available for such works under U.S. Law.
dc.rights.urihttp://creativecommons.org/publicdomain/mark/1.0/*
dc.titleThree short-period Jupiters from TESSen_US
dc.typeTexten_US

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