TESS delivers five new hot giant planets orbiting bright stars from the full-frame images

Rodriguez, Joseph E. and Quinn, Samuel N. and Zhou, George ORCID: https://orcid.org/0000-0002-4891-3517 and Vanderburg, Andrew and Nielsen, Louise D. and Wittenmyer, Robert A. and Brahm, Rafael and Reed, Phillip A. and Huang, Chelsea X. ORCID: https://orcid.org/0000-0003-0918-7484 and Vach, Sydney and Ciardi, David R. and Oelkers, Ryan J. and Stassun, Keivan G. and Hellier, Coel and Gaudi, B. Scott and Eastman, Jason D. and Collins, Karen A. and Bieryla, Allyson and Christian, Sam and Latham, David W. and Carleo, Ilaria and Wright, Duncan J. and Matthews, Elisabeth and Gonzales, Erica J. and Ziegler, Carl and Dressing, Courtney D. and Howell, Steve B. and Tan, Thiam-Guan and Wittrock, Justin and Plavchan, Peter and McLeod, Kim K. and Baker, David and Wang, Gavin and Radford, Don J. and Schwarz, Richard P. and Esposito, Massimiliano and Ricker, George R. and Vanderspek, Roland K. and Seager, Sara and Winn, Joshua N. and Jenkins, Jon M. and Addison, Brett ORCID: https://orcid.org/0000-0003-3216-0626 and Anderson, D. R. and Barclay, Thomas and Beatty, Thomas G. and Berlind, Perry and Bouchy, Francois and Bowen, Michael and Bowler, Brendan P. and Brasseur, C. E. and Briceno, Cesar and Caldwell, Douglas A. and Calkins, Michael L. and Cartwright, Scott and Chaturvedi, Priyanka and Chaverot, Guillaume and Chimaladinne, Sudhish and Christiansen, Jessie L. and Collins, Kevin I. and Crossfield, Ian J. M. and Eastridge, Kevin and Espinoza, Nestor and Esquerdo, Gilbert A. and Feliz, Dax L. and Fenske, Tyler and Fong, William and Gan, Tianjun and Giacalone, Steven and Gill, Holden and Gordon, Lindsey and Granados, A. and Grieves, Nolan and Guenther, Eike W. and Guerrero, Natalia and Henning, Thomas and Henze, Christopher E. and Hesse, Katharine and Hobson, Melissa J. and Horner, Jonathan and James, David J. and Jensen, Eric L. N. and Jimenez, Mary and Jordan, Andres and Kane, Stephen R. and Kielkopf, John and Kim, Kingsley and Kuhn, Rudolf B. and Latouf, Natasha and Law, Nicholas M. and Levine, Alan M. and Lund, Michael B. and Mann, Andrew W. and Mao, Shude and Matson, Rachel A. and Mengel, Matthew W. ORCID: https://orcid.org/0000-0002-7830-6822 and Mink, Jessica and Newman, Patrick and O'Dwyer, Tanner and Okumura, Jack and Palle, Enric and Pepper, Joshua and Quintana, Elisa V. and Sarkis, Paula and Savel, Arjun B. and Schlieder, Joshua E. and Schnaible, Chloe and Shporer, Avi and Sefako, Ramotholo and Seidel, Julia V. and Siverd, Robert J. and Skinner, Brett and Stalport, Manu and Stevens, Daniel J. and Stibbard, Caitlin and Tinney, C. G. and West, R. G. and Yahalomi, Daniel A. and Zhang, Hui (2021) TESS delivers five new hot giant planets orbiting bright stars from the full-frame images. The Astronomical Journal, 161 (4):194. ISSN 0004-6256

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We present the discovery and characterization of five hot and warm Jupiters—TOI-628 b (TIC 281408474; HD 288842), TOI-640 b (TIC 147977348), TOI-1333 b (TIC 395171208, BD+47 3521A), TOI-1478 b (TIC 409794137), and TOI-1601 b (TIC 139375960)—based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The five planets were identified from the full-frame images and were confirmed through a series of photometric and spectroscopic follow-up observations by the TESS Follow-up Observing Program Working Group. The planets are all Jovian size (RP = 1.01-1.77 RJ) and have masses that range from 0.85 to 6.33 MJ. The host stars of these systems have F and G spectral types (5595 ≤ Teff ≤ 6460 K) and are all relatively bright (9.5 < V < 10.8, 8.2 < K < 9.3), making them well suited for future detailed characterization efforts. Three of the systems in our sample (TOI-640 b, TOI-1333 b, and TOI-1601 b) orbit subgiant host stars ( $\mathrm{log}$ g < 4.1). TOI-640 b is one of only three known hot Jupiters to have a highly inflated radius (RP > 1.7 RJ, possibly a result of its host star's evolution) and resides on an orbit with a period longer than 5 days. TOI-628 b is the most massive, hot Jupiter discovered to date by TESS with a measured mass of ${6.31}_{-0.30}^{+0.28}$ MJ and a statistically significant, nonzero orbital eccentricity of e = ${0.074}_{-0.022}^{+0.021}$ . This planet would not have had enough time to circularize through tidal forces from our analysis, suggesting that it might be remnant eccentricity from its migration. The longest-period planet in this sample, TOI-1478 b (P = 10.18 days), is a warm Jupiter in a circular orbit around a near-solar analog. NASA's TESS mission is continuing to increase the sample of well-characterized hot and warm Jupiters, complementing its primary mission goals.

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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: © 2021. The American Astronomical Society. Submitted version deposited in accordance with the copyright policy of the publisher.
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Date Deposited: 11 Aug 2021 07:12
Last Modified: 07 Feb 2022 05:03
Uncontrolled Keywords: exoplanet astronomy; exoplanet migration; exoplanet detection; methods; exoplanets; transits; radial velocity; direct imaging; 486; 2205; 489; 498; 1711; 1332; 387; astrophysics; solar and stellar astrophysics
Fields of Research (2008): 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems
Fields of Research (2020): 51 PHYSICAL SCIENCES > 5101 Astronomical sciences > 510109 Stellar astronomy and planetary systems
Socio-Economic Objectives (2008): E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences
Socio-Economic Objectives (2020): 28 EXPANDING KNOWLEDGE > 2801 Expanding knowledge > 280120 Expanding knowledge in the physical sciences
Identification Number or DOI: https://doi.org/10.3847/1538-3881/abe38a
URI: http://eprints.usq.edu.au/id/eprint/42816

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