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

Songhu Wang, Matias Jones, Avi Shporer, Benjamin J. Fulton, Leonardo A. Paredes, Trifon Trifonov, Diana Kossakowski, Jason Eastman, Seth Redfield, Maximilian N. Günther, Laura Kreidberg, Chelsea X. Huang, Sarah Millholland, Darryl Seligman, Debra Fischer, Rafael Brahm, Xian Yu Wang, Bryndis Cruz, Todd Henry, Hodari Sadiki JamesBrett Addison, En Si Liang, Allen B. Davis, René Tronsgaard, Keduse Worku, John M. Brewer, Martin Kürster, Hui Zhang, Charles A. Beichman, Allyson Bieryla, Timothy M. Brown, Jessie L. Christiansen, David R. Ciardi, Karen A. Collins, Gilbert A. Esquerdo, Andrew W. Howard, Howard Isaacson, David W. Latham, Tsevi Mazeh, Erik A. Petigura, Samuel N. Quinn, Sahar Shahaf, Robert J. Siverd, Florian Rodler, Sabine Reffert, Olga Zakhozhay, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Patricia T. Boyd, Gábor Frész, Christopher Henze, Alen M. Levine, Robert Morris, Martin Paegert, Keivan G. Stassun, Eric B. Ting, Michael Vezie, Gregory Laughlin

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63 Citas (Scopus)

Resumen

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 and radius of , 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.

Idioma originalInglés
Número de artículo51
PublicaciónAstronomical Journal
Volumen157
N.º2
DOI
EstadoPublicada - feb. 2019
Publicado de forma externa

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