TOI 564 b and TOI 905 b: Grazing and Fully Transiting Hot Jupiters Discovered by TESS
Allen B. Davis, Songhu Wang, Matias Jones, Jason D. Eastman, Maximilian N. Günther, Keivan G. Stassun, Brett C. Addison, Karen A. Collins, Samuel N. Quinn, David W. Latham, Trifon Trifonov, Sahar Shahaf, Tsevi Mazeh, Stephen R. Kane, Norio Narita, Xian-Yu Wang, Thiam-Guan Tan, David R. Ciardi, Andrei Tokovinin, Carl Ziegler, René Tronsgaard, Sarah Millholland, Bryndis Cruz, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, Kevin I. Collins, Dennis M. Conti, Felipe Murgas, Phil Evans, Pablo Lewin, Don J. Radford, Leonardo A. Paredes, Todd J. Henry, James Hodari-Sadiki, Michael B. Lund, Jessie L. Christiansen, Nicholas M. Law, Andrew W. Mann, César Briceño, Hannu Parviainen, Enric Palle, Noriharu Watanabe, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Akshata Krishnamurthy, Natalie M. Batalha, Jennifer Burt, Knicole D. Colón, Scott Dynes, Douglas A. Caldwell, Robert Morris, Christopher E. Henze, Debra A. Fischer
Abstract
Abstract We report the discovery and confirmation of two new hot Jupiters discovered by the Transiting Exoplanet Survey Satellite (TESS): TOI 564 b and TOI 905 b. The transits of these two planets were initially observed by TESS with orbital periods of 1.651 and 3.739 days, respectively. We conducted follow-up observations of each system from the ground, including photometry in multiple filters, speckle interferometry, and radial velocity measurements. For TOI 564 b, our global fitting revealed a classical hot Jupiter with a mass of M J and a radius of R J . Also a classical hot Jupiter, TOI 905 b has a mass of M J and radius of R J . Both planets orbit Sun-like, moderately bright, mid-G dwarf stars with V ∼ 11. While TOI 905 b fully transits its star, we found that TOI 564 b has a very high transit impact parameter of , making it one of only ∼20 known systems to exhibit a grazing transit and one of the brightest host stars among them. Therefore, TOI 564 b is one of the most attractive systems to search for additional nontransiting, smaller planets by exploiting the sensitivity of grazing transits to small changes in inclination and transit duration over a timescale of several years.