TOI 4201 b and TOI 5344 b: Discovery of Two Transiting Giant Planets around M-dwarf Stars and Revised Parameters for Three Others
Author:
Hartman J. D.ORCID, Bakos G. Á.ORCID, Csubry Z., Howard A. W.ORCID, Isaacson H.ORCID, Giacalone S.ORCID, Chontos A.ORCID, Narita N.ORCID, Fukui A.ORCID, de Leon J. P.ORCID, Watanabe N.ORCID, Mori M.ORCID, Kagetani T.ORCID, Fukuda I.ORCID, Kawai Y.ORCID, Ikoma M.ORCID, Palle E.ORCID, Murgas F.ORCID, Esparza-Borges E.ORCID, Parviainen H.ORCID, Bouma L. G.ORCID, Cointepas M., Bonfils X.ORCID, Almenara J. M.ORCID, Collins Karen A.ORCID, Collins Kevin I.ORCID, Relles Howard M.ORCID, Barkaoui KhalidORCID, Schwarz Richard P.ORCID, Mourad GhachouiORCID, Timmermans Mathilde, Dransfield Georgina, Burdanov ArtemORCID, de Wit JulienORCID, Jehin EmmanuëlORCID, Triaud Amaury H. M. J.ORCID, Gillon MichaëlORCID, Benkhaldoun ZouhairORCID, Horne KeithORCID, Sefako RamotholoORCID, Jordán A.ORCID, Brahm R.ORCID, Suc V.ORCID, Howell Steve B.ORCID, Furlan E.ORCID, Schlieder J. E.ORCID, Ciardi D.ORCID, Barclay T.ORCID, Gonzales E. J.ORCID, Crossfield I.ORCID, Dressing C. D.ORCID, Goliguzova M.ORCID, Tatarnikov A.ORCID, Ricker George R.ORCID, Vanderspek RolandORCID, Latham David W.ORCID, Seager S.ORCID, Winn Joshua N.ORCID, Jenkins Jon M.ORCID, Striegel StephanieORCID, Shporer AviORCID, Vanderburg AndrewORCID, Levine Alan M.ORCID, Kostov Veselin B.ORCID, Watanabe DavidORCID
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.
Funder
NASA ∣ SMD ∣ Astrophysics Division MEXT ∣ Japan Society for the Promotion of Science MEXT ∣ JST ∣ Core Research for Evolutional Science and Technology ANID ∣ Fondo Nacional de Desarrollo Científico y Tecnológico
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics
Cited by
1 articles.
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