The Astronomical Journal (Jan 2023)

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

DOI
https://doi.org/10.3847/1538-3881/acf56e
Journal volume & issue
Vol. 166, no. 4
p. 163

Abstract

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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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