TOI 4201 b and TOI 5344 b: Discovery of Two Transiting Giant Planets around M-dwarf Stars and Revised Parameters for Three Others
J. D. Hartman, G. Á. Bakos, Z. Csubry, Andrew W. Howard, Howard Isaacson, Steven Giacalone, Ashley Chontos, Norio Narita, Akihiko Fukui, Jerome de Leon, Noriharu Watanabe, M. Mori, Taiki Kagetani, Izuru Fukuda, Y. Kawai, Masahiro Ikoma, Ε. Πάλλη, F. Murgas, E. Esparza-Borges, H. Parviainen, Luke G. Bouma, Marion Cointepas, X. Bonfıls, J. M. Almenara, Karen A. Collins, Kevin I. Collins, Howard M. Relles, Khalid Barkaoui, Richard P. Schwarz, Mourad Ghachoui, Mathilde Timmermans, Georgina Dransfield, Artem Burdanov, Julien de Wit, Emmanuël Jehin, A. H. M. J. Triaud, M. Gillon, Z. Benkhaldoun, K. Horne, Ramotholo Sefako, Andrés Jordán, Rafael Brahm, V. Suc, Steve B. Howell, Elise Furlan, Joshua E. Schlieder, David R. Ciardi, Thomas Barclay, Erica J. Gonzales, Ian J. M. Crossfield, Courtney D. Dressing, Maria V. Goliguzova, А. М. Татарников, G. Ricker, R. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Stephanie Striegel, Avi Shporer, Andrew Vanderburg, Alan M. Levine, Veselin B. Kostov, David Watanabe
Abstract
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.