Three Long-period Transiting Giant Planets from TESS*
Author:
Brahm RafaelORCID, Ulmer-Moll SolèneORCID, Hobson Melissa J.ORCID, Jordán AndrésORCID, Henning ThomasORCID, Trifonov TrifonORCID, Jones Matías I., Schlecker MartinORCID, Espinoza NestorORCID, Rojas Felipe I.ORCID, Torres PascalORCID, Sarkis PaulaORCID, Tala Marcelo, Eberhardt JanORCID, Kossakowski DianaORCID, Muñoz Diego J.ORCID, Hartman Joel D.ORCID, Boyle Gavin, Suc VincentORCID, Bouchy FrançoisORCID, Deline Adrien, Chaverot GuillaumeORCID, Grieves Nolan, Lendl MonikaORCID, Suarez OlgaORCID, Guillot TristanORCID, Triaud Amaury H. M. J.ORCID, Crouzet NicolasORCID, Dransfield GeorginaORCID, Cloutier RyanORCID, Barkaoui KhalidORCID, Schwarz Rick P.ORCID, Stockdale ChrisORCID, Harris MalloryORCID, Mireles IsmaelORCID, Evans PhilORCID, Mann Andrew W.ORCID, Ziegler Carl, Dragomir DianaORCID, Villanueva StevenORCID, Mordasini ChristophORCID, Ricker GeorgeORCID, Vanderspek RolandORCID, Latham David W.ORCID, Seager SaraORCID, Winn Joshua N.ORCID, Jenkins Jon M.ORCID, Vezie Michael, Youngblood AllisonORCID, Daylan TansuORCID, Collins Karen A.ORCID, Caldwell Douglas A.ORCID, Ciardi David R.ORCID, Palle EnricORCID, Murgas FelipeORCID
Abstract
Abstract
We report the discovery and orbital characterization of three new transiting warm giant planets. These systems were initially identified as presenting single-transit events in the light curves generated from the full-frame images of the Transiting Exoplanet Survey Satellite. Follow-up radial velocity measurements and additional light curves were used to determine the orbital periods and confirm the planetary nature of the candidates. The planets orbit slightly metal-rich late F- and early G-type stars. We find that TOI 4406b has a mass of M
P
= 0.30 ± 0.04 M
J, a radius of R
P
= 1.00 ± 0.02 R
J, and a low-eccentricity orbit (e = 0.15 ± 0.05) with a period of P = 30.08364 ±0.00005 days. TOI 2338b has a mass of M
P
= 5.98 ± 0.20 M
J, a radius of R
P
= 1.00 ± 0.01 R
J, and a highly eccentric orbit (e = 0.676 ± 0.002) with a period of P = 22.65398 ± 0.00002 days. Finally, TOI 2589b has a mass of M
P
= 3.50 ± 0.10 M
J, a radius of R
P
= 1.08 ± 0.03 R
J, and an eccentric orbit (e = 0.522 ± 0.006) with a period of P = 61.6277 ± 0.0002 days. TOI 4406b and TOI 2338b are enriched in metals compared to their host stars, while the structure of TOI 2589b is consistent with having similar metal enrichment to its host star.
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
2 articles.
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