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HD 202772A b: A Transiting Hot Jupiter around a Bright, Mildly Evolved Star in a Visual Binary Discovered by TESS

Wang, Songhu and Fulton, Benjamin J. and Howard, Andrew W. and Petigura, Erik A. and Beichman, Charles A. and Christiansen, Jessie L. and Ciardi, David R. (2019) HD 202772A b: A Transiting Hot Jupiter around a Bright, Mildly Evolved Star in a Visual Binary Discovered by TESS. Astronomical Journal, 157 (2). Art. No. 51. ISSN 1538-3881. doi:10.3847/1538-3881/aaf1b7.

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We report the first confirmation of a hot Jupiter discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HD 202772A b. The transit signal was detected in the data from TESS Sector 1, and was confirmed to be of planetary origin through radial velocity (RV) measurements. HD 202772A b is orbiting a mildly evolved star with a period of 3.3 days. With an apparent magnitude of V = 8.3, the star is among the brightest and most massive known to host a hot Jupiter. Based on the 27 days of TESS photometry and RV data from the CHIRON, HARPS, and Tillinghast Reflector Echelle Spectrograph, the planet has a mass of 1.017^(+0.070)_(-0.068) M_J and radius of 1.545^(+0.052)_(-0.060) R_J, making it an inflated gas giant. HD 202772A b is a rare example of a transiting hot Jupiter around a quickly evolving star. It is also one of the most strongly irradiated hot Jupiters currently known.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Wang, Songhu0000-0002-7846-6981
Fulton, Benjamin J.0000-0003-3504-5316
Howard, Andrew W.0000-0001-8638-0320
Petigura, Erik A.0000-0003-0967-2893
Beichman, Charles A.0000-0002-5627-5471
Christiansen, Jessie L.0000-0002-8035-4778
Ciardi, David R.0000-0002-5741-3047
Additional Information:© 2019 The American Astronomical Society. Received 2018 October 3; revised 2018 November 13; accepted 2018 November 16; published 2019 January 14. We thank the anonymous referee for the insightful suggestions that greatly improved this manuscript. We thank Yanqin Wu, Smadar Naoz, Ian Crossfield, Lars A. Buchhave, Bonan Pu, Alexander P. Stephan, Sabarni Basu, Xi Zhang, Beibei Liu, and Jorge Lillo-Box for their insights. J.N.W. and S.W. thank the Heising-Simons Foundation for their generous support. M.N.G. acknowledges support from MITs Kavli Institute as a Torres postdoctoral fellow. S.M. and A.B.D. are supported by the National Science Foundation Graduate Research Fellowship Program under Grant Number DGE-1122492. R.B. acknowledges support from FONDECYT Postdoctoral Fellowship Project 3180246, and from the Millennium Institute of Astrophysics (MAS). G.L. acknowledges support from the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement Notice NNH13ZDA017C issued through the Science Mission Directorate. This research is based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere under ESO programme 0101.C-0232. This work makes use of observations from SMARTS and the LCO network. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Funding for the TESS mission is provided by NASA's Science Mission directorate. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This research has made use of the Exoplanet Follow-up Observation Program website and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). We made use of the Python programming language (Rossum 1995) and the open-source Python packages numpy (van der Walt et al. 2011), emcee (Foreman-Mackey et al. 2013), and celerite (Foreman-Mackey et al. 2017). Facilities: TESS - , CTIO:1.5 m (CHIRON) - , ESO:3.6 m (HARPS) - , Keck II (NIRC2) - , Keck I (HIRES) - , LCO:1.0 m (NRES) - , FLWO:1.5 m (TRES) - .
Group:Infrared Processing and Analysis Center (IPAC), Astronomy Department
Funding AgencyGrant Number
Heising-Simons FoundationUNSPECIFIED
Massachusetts Institute of Technology (MIT)UNSPECIFIED
NSF Graduate Research FellowshipDGE-1122492
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)3180246
Millennium Institute of Astrophysics (MAS)UNSPECIFIED
Subject Keywords:planetary systems – planets and satellites: detection – stars: individual (TIC 290131778-TOI 123-HD 202772 – techniques: radial velocities
Issue or Number:2
Record Number:CaltechAUTHORS:20190116-143250249
Persistent URL:
Official Citation:Songhu Wang et al 2019 AJ 157 51
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:92326
Deposited By: Tony Diaz
Deposited On:18 Jan 2019 04:49
Last Modified:16 Nov 2021 03:49

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