TOI 4201 b and TOI 5344 b: Discovery of Two Transiting Giant Planets around M-dwarf Stars and Revised Parameters for Three Others
Kostov, Veselin B.; Vanderburg, Andrew; Triaud, Amaury H. M. J.; Latham, David W.; Narita, N.; Palle, E.; Howell, Steve B.; Horne, Keith; Collins, Karen A.; Watanabe, David; Ricker, George R.; Vanderspek, Roland; Winn, Joshua N.; Jenkins, Jon M.; Bonfils, X.; Seager, S.; Barkaoui, Khalid; Dransfield, Georgina; Shporer, Avi; Collins, Kevin I.; Gillon, Michaël; de Wit, Julien; Levine, Alan M.; Bouma, L. G.; Jehin, Emmanuël; Relles, Howard M.; Sefako, Ramotholo; Almenara, J. M.; Esparza-Borges, E.; Murgas, F.; Fukui, A.; Parviainen, H.; Watanabe, N.; Mori, M.; de Leon, J. P.; Isaacson, H.; Furlan, E.; Chontos, A.; Giacalone, S.; Schwarz, Richard P.; Barclay, T.; Striegel, Stephanie; Jordán, A.; Schlieder, J. E.; Dressing, C. D.; Benkhaldoun, Zouhair; Bakos, G. Á.; Hartman, J. D.; Brahm, R.; Csubry, Z.; Howard, A. W.; Suc, V.; Timmermans, Mathilde; Burdanov, Artem; Gonzales, E. J.; Kagetani, T.; Ikoma, M.; Cointepas, M.; Crossfield, I.; Ciardi, D.; Kawai, Y.; Fukuda, I.; Tatarnikov, A.; Mourad, Ghachoui; Goliguzova, M.
United States, Japan, Spain, France, Switzerland, Belgium, Morocco, United Kingdom, South Africa, Chile, Russia
Abstract
We present the discovery from the TESS mission of two giant planets transiting M-dwarf stars: TOI 4201 b and TOI 5344 b. We also provide precise radial velocity measurements and updated system parameters for three other M dwarfs with transiting giant planets: TOI 519, TOI 3629, and TOI 3714. We measure planetary masses of 0.525 ± 0.064 M J, 0.243 ± 0.020 M J, 0.689 ± 0.030 M J, 2.57 ± 0.15 M J, and 0.412±0.040 M J for TOI 519 b, TOI 3629 b, TOI 3714 b, TOI 4201 b, and TOI 5344 b, respectively. The corresponding stellar masses are 0.372 ± 0.018 M ☉, 0.635 ± 0.032 M ☉, 0.522 ± 0.028 M ☉, 0.626 ± 0.033 M ☉, and 0.612 ± 0.034 M ☉. All five hosts have supersolar metallicities, providing further support for recent findings that, like for solar-type stars, close-in giant planets are preferentially found around metal-rich M-dwarf host stars. Finally, we describe a procedure for accounting for systematic errors in stellar evolution models when those models are included directly in fitting a transiting planet system.