The Astronomical Journal (Jan 2023)

TOI-5344 b: A Saturn-like Planet Orbiting a Super-solar Metallicity M0 Dwarf

  • Te Han,
  • Paul Robertson,
  • Shubham Kanodia,
  • Caleb Cañas,
  • Andrea S. J. Lin,
  • Gumundur Stefánsson,
  • Jessica E. Libby-Roberts,
  • Alexander Larsen,
  • Henry A. Kobulnicky,
  • Suvrath Mahadevan,
  • Chad F. Bender,
  • William D. Cochran,
  • Michael Endl,
  • Mark E. Everett,
  • Arvind F. Gupta,
  • Samuel Halverson,
  • Fred Hearty,
  • Andrew Monson,
  • Joe P. Ninan,
  • Arpita Roy,
  • Christian Schwab,
  • Ryan C. Terrien

DOI
https://doi.org/10.3847/1538-3881/ad09c2
Journal volume & issue
Vol. 167, no. 1
p. 4

Abstract

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We confirm the planetary nature of TOI-5344 b as a transiting giant exoplanet around an M0-dwarf star. TOI-5344 b was discovered with the Transiting Exoplanet Survey Satellite photometry and confirmed with ground-based photometry (the Red Buttes Observatory 0.6 m telescope), radial velocity (the Habitable-zone Planet Finder), and speckle imaging (the NN-Explore Exoplanet Stellar Speckle Imager). TOI-5344 b is a Saturn-like giant planet ( ρ = 0.80 ${}_{-0.15}^{+0.17}$ g cm ^−3 ) with a planetary radius of 9.7 ± 0.5 R _⊕ (0.87 ± 0.04 R _Jup ) and a planetary mass of ${135}_{-18}^{+17}\ {M}_{\oplus }$ (0.42 ${}_{-0.06}^{+0.05}\ {M}_{\mathrm{Jup}}$ ). It has an orbital period of ${3.792622}_{-0.000010}^{+0.000010}$ days and an orbital eccentricity of ${0.06}_{-0.04}^{+0.07}$ . We measure a high metallicity for TOI-5344 of [Fe/H] = 0.48 ± 0.12, where the high metallicity is consistent with expectations from formation through core accretion. We compare the metallicity of the M-dwarf hosts of giant exoplanets to that of M-dwarf hosts of nongiants (≲8 R _⊕ ). While the two populations appear to show different metallicity distributions, quantitative tests are prohibited by various sample caveats.

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