Davis, Allen B. and Wang, Songhu and Jones, Matias and Eastman, Jason D. and Günther, Maximilian N. and Stassun, Keivan G. and Addison, Brett C. and Collins, Karen A. and Quinn, Samuel N. and Latham, David W. and Trifonov, Trifon and Shahaf, Sahar and Mazeh, Tsevi and Kane, Stephen R. and Narita, Norio and Wang, Xian-Yu and Tan, Thiam-Guan and Ciardi, David R. and Tokovinin, Andrei and Ziegler, Carl and Tronsgaard, René and Millholland, Sarah and Cruz, Bryndis and Berlind, Perry and Calkins, Michael L. and Esquerdo, Gilbert A. and Collins, Kevin I. and Conti, Dennis M. and Murgas, Felipe and Evans, Phil and Lewin, Pablo and Radford, Don J. and Paredes, Leonardo A. and Henry, Todd J. and Hodari-Sadiki, James and Lund, Michael B. and Christiansen, Jessie L. and Law, Nicholas M. and Mann, Andrew W. and Briceño, César and Parviainen, Hannu and Palle, Enric and Watanabe, Noriharu and Ricker, George R. and Vanderspek, Roland and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Krishnamurthy, Akshata and Batalha, Natalie M. and Burt, Jennifer and Colón, Knicole D. and Dynes, Scott and Caldwell, Douglas A. and Morris, Robert and Henze, Christopher E. and Fischer, Debra A. (2020) TOI 564 b and TOI 905 b: Grazing and Fully Transiting Hot Jupiters Discovered by TESS. Astronomical Journal, 160 (5). Art. No. 229. ISSN 1538-3881. doi:10.3847/1538-3881/aba49d. https://resolver.caltech.edu/CaltechAUTHORS:20201102-083736294
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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 1.463^(+0.10)_(−0.096) M_J and a radius of 1.02^(+0.71)_(−0.29) RJ. Also a classical hot Jupiter, TOI 905 b has a mass of 0.667^(+0.042)_(−0.041) M_J and radius of 1.171^(+0.053)_(−0.051) 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 0.994^(+0.083)_(−0.049), 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.
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| Additional Information: | © 2020 The American Astronomical Society. Received 2019 December 20; revised 2020 June 26; accepted 2020 June 29; published 2020 October 29. A.B.D. is supported by the National Science Foundation Graduate Research Fellowship Program under grant No. DGE-1122492. S.W. thanks the Heising-Simons Foundation for its generous support as a 51 Pegasi b fellow. M.N.G. acknowledges support from MITs Kavli Institute as a Torres postdoctoral fellow. C.Z. is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the Dunlap family and the University of Toronto. Work by J.N.W. was partly supported by the Heising-Simons Foundation. This work is partly supported by JSPS KAKENHI grant Nos. JP18H01265 and JP18H05439 and JST PRESTO grant No. JPMJPR1775. H.P. and E.P. acknowledge funding from the Spanish Ministry of Economics and Competitiveness through project PGC2018-098153-B-C31. Funding for the TESS mission is provided by the National Aeronautics and Space Administration's (NASA) Science Mission directorate. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and the TESS Science Processing Operations Center. 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 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). Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA. This work makes use of observations from SMARTS and the LCOGT network. This work is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO program 0103.C-0548. This work is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez, operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. Software: numpy (van der Walt et al. 2011), pandas (Reback et al. 2020), emcee (Foreman-Mackey et al. 2013, 2018), celerite (Foreman-Mackey et al. 2017a, 2017b), EXOFAST (v2; Eastman et al. 2013; Eastman 2017; Eastman et al. 2019), Tapir software package (Jensen 2013), AstroImageJ (Collins et al. 2017), ARES2 (v2; Sousa et al. 2015), MOOG code (Sneden 1973). Facilities: TESS - , CTIO:1.5 m (CHIRON) - , FLWO:1.5 m (TRES) - , ESO:3.6 m (HARPS) - , LCOGT - , Sanchez (MuSCAT2) - , SOAR (HRCam) - , Hale (PHARO). - | ||||||||||||||||||||||
| Group: | Infrared Processing and Analysis Center (IPAC) | ||||||||||||||||||||||
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| Subject Keywords: | Exoplanet astronomy; Exoplanet detection methods; Radial velocity; Transit photometry; Extrasolar gas giants; Hot Jupiters | ||||||||||||||||||||||
| Issue or Number: | 5 | ||||||||||||||||||||||
| Classification Code: | Unified Astronomy Thesaurus concepts: Exoplanet astronomy (486); Exoplanet detection methods (489); Radial velocity (1332); Transit photometry (1709); Extrasolar gas giants (509); Hot Jupiters (753) | ||||||||||||||||||||||
| DOI: | 10.3847/1538-3881/aba49d | ||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20201102-083736294 | ||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20201102-083736294 | ||||||||||||||||||||||
| Official Citation: | Allen B. Davis et al 2020 AJ 160 229 | ||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||
| ID Code: | 106375 | ||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||
| Deposited By: | Tony Diaz | ||||||||||||||||||||||
| Deposited On: | 04 Nov 2020 19:05 | ||||||||||||||||||||||
| Last Modified: | 16 Nov 2021 18:53 |
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