Bibcode
Hartman, J. D.; Bakos, G. Á.; Csubry, Z.; Howard, A. W.; Isaacson, H.; Giacalone, S.; Chontos, A.; Narita, N.; Fukui, A.; de Leon, J. P.; Watanabe, N.; Mori, M.; Kagetani, T.; Fukuda, I.; Kawai, Y.; Ikoma, M.; Palle, E.; Murgas, F.; Esparza-Borges, E.; Parviainen, H.; Bouma, L. G.; Cointepas, M.; Bonfils, X.; Almenara, J. M.; Collins, Karen A.; Collins, Kevin I.; Relles, Howard M.; Barkaoui, Khalid; Schwarz, Richard P.; Mourad, Ghachoui; Timmermans, Mathilde; Dransfield, Georgina; Burdanov, Artem; de Wit, Julien; Jehin, Emmanuël; Triaud, Amaury H. M. J.; Gillon, Michaël; Benkhaldoun, Zouhair; Horne, Keith; Sefako, Ramotholo; Jordán, A.; Brahm, R.; Suc, V.; Howell, Steve B.; Furlan, E.; Schlieder, J. E.; Ciardi, D.; Barclay, T.; Gonzales, E. J.; Crossfield, I.; Dressing, C. D.; Goliguzova, M.; Tatarnikov, A.; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, S.; Winn, Joshua N.; Jenkins, Jon M.; Striegel, Stephanie; Shporer, Avi; Vanderburg, Andrew; Levine, Alan M.; Kostov, Veselin B.; Watanabe, David
Bibliographical reference
The Astronomical Journal
Advertised on:
10
2023
Citations
11
Refereed citations
10
Description
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.
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Enric
Pallé Bago