TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from the Transiting Exoplanet Survey Satellite

Creators: Brahm, Rafael; Nielsen, Louise D.; Wittenmyer, Robert A.; Wang, Songhu; Rodriguez, Joseph E.; Espinoza, Néstor; Jones, Matías I.; Jordán, Andrés; Henning, Thomas; Hobson, Melissa; Kossakowski, Diana; Rojas, Felipe; Sarkis, Paula; Schlecker, Martin; Trifonov, Trifon; Shahaf, Sahar; Ricker, George; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Addison, Brett C.; Bakos, Gáspár Á.; Bhatti, Waqas; Bayliss, Daniel; Berlind, Perry; Bieryla, Allyson; Bouchy, Francois; Bowler, Brendan P.; Briceño, César; Brown, Timothy M.; Bryant, Edward M.; Caldwell, Douglas A.; Charbonneau, David; Collins, Karen A.; Davis, Allen B.; Esquerdo, Gilbert A.; Fulton, Benjamin J.; Guerrero, Natalia M.; Henze, Christopher E.; Hogan, Aleisha; Horner, Jonathan; Huang, Chelsea X.; Irwin, Jonathan; Kane, Stephen R.; Kielkopf, John; Mann, Andrew W.; Mazeh, Tsevi; McCormac, James; McCully, Curtis; Mengel, Matthew W.; Mireles, Ismael; Okumura, Jack; Plavchan, Peter; Quinn, Samuel N.; Rabus, Markus; Saesen, Sophie; Schlieder, Joshua E.; Ségransan, Damien; Shiao, Bernie; Shporer, Avi; Siverd, Robert J.; Stassun, Keivan G.; Suc, Vincent; Tan, Thiam-Guan; Torres, Pascal; Tinney, Chris G.; Udry, Stephane; Vanzi, Leonardo; Vezie, Michael; Vines, Jose I.; Vuckovic, Maja; Wright, Duncan J.; Yahalomi, Daniel A.; Zapata, Abner; Zhang, Hui; Ziegler, Carl

Abstract

We present the discovery of two new 10 day period giant planets from the Transiting Exoplanet Survey Satellite mission, whose masses were precisely determined using a wide diversity of ground-based facilities. TOI-481 b and TOI-892 b have similar radii (0.99 ± 0.01 R_J and 1.07 ± 0.02 R_J, respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53 ± 0.03 M_J versus 0.95 ± 0.07 M_J, respectively). Both planets orbit metal-rich stars ([Fe/H] = +0.26 ± 0.05 dex and [Fe/H] = +0.24 ± 0.05 for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a M⋆ = 1.14 ± 0.02 M_⊙, R⋆ = 1.66 ± 0.02 R_⊙ G-type star (T_(eff) = 5735 ± 72 K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892 on the other hand, is a F-type dwarf star (T_(eff) = 6261 ± 80 K), which has a mass of M⋆ = 1.28 ± 0.03 M_⊙ and a radius of R⋆ = 1.39 ± 0.02 R_⊙. TOI-481 b and TOI-892 b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters.

Additional Information

© 2020 The American Astronomical Society. Received 2020 August 4; revised 2020 September 10; accepted 2020 September 17; published 2020 October 29. We acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the exoplanet follow-up observation program website, 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). 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. R.B. acknowledges support from FONDECYT Post-doctoral Fellowship Project 3180246, and from ANID - Millennium Science Initiative—ICN12_009. A.J. acknowledges support from FONDECYT project 1171208, and from ANID—Millennium Science Initiative—ICN12_009. J.I.V. acknowledges support of CONICYT-PFCHA/Doctorado Nacional-21191829. This work was supported by the DFG Research Unit FOR2544 "Blue Planets around Red Stars," project no. RE 2694/4-1. We thank Paul Eigenthaler, Angela Hempel, Maren Hempel, Sam Kim, and Régis Lachaume for their technical assistance during the observations at the MPG 2.2 m Telescope. We thank the Swiss National Science Foundation (SNSF) and the Geneva University for their continuous support to our planet search programs. 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). Minerva-Australis is supported by Australian Research Council LIEF Grant LE160100001, Discovery Grant DP180100972, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. This research was supported by grant No. 2016069 of the United States-Israel Binational Science Foundation (BSF) The MEarth Team gratefully acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering (awarded to D.C.). This material is based upon work supported by the National Science Foundation under grants AST-0807690, AST-1109468, AST-1004488 (Alan T. Waterman Award), and AST-1616624, and upon work supported by the National Aeronautics and Space Administration under grant No. 80NSSC18K0476 issued through the XRP Program. This work is made possible by a grant from the John Templeton Foundation. The opinions expressed in this publication are those of the authors and do not necessarily reflect the views of the John Templeton Foundation. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors, and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the Minerva-Australis facility at Mt. Kent is situated. R.B. acknowledges support from CORFO project N°14ENI2-26865. Facilities: Astrometry: Gaia (Gaia Collaboration et al. 2016, 2018). Imaging: SOAR (HRCam; Tokovinin 2018). Spectroscopy: CTIO1.5m (CHIRON; Tokovinin et al. 2013), MPG2.2m (FEROS; Kaufer et al. 1999), Euler1.2m (CORALIE; Mayor et al. 2003), Tillinghast1.5m (TRES) (Fűrész 2008), Minerva-Australis (Addison et al. 2019), NRES (Siverd et al. 2018), Photometry: CHAT:0.7m, MEarth-South (Irwin et al. 2015), NGTS (Wheatley et al. 2018), TESS (Ricker et al. 2015). Software: juliet (Espinoza et al. 2019b), CERES (Jordán et al. 2014; Brahm et al. 2017a), ZASPE (Brahm et al. 2015, 2017b), radvel (Fulton et al. 2018) emcee (Foreman-Mackey et al. 2013), MultiNest (Feroz et al. 2009), batman (Kreidberg et al. 2015), SPC (Buchhave et al. 2012), SpecMatch (Yee et al. 2017).

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