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

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 Hab...

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Bibliographic Details
Published in:The Astronomical journal 2024-01, Vol.167 (1), p.4
Main Authors: Han, Te, Robertson, Paul, Kanodia, Shubham, Cañas, Caleb, Lin, Andrea S. J., Stefánsson, Gumundur, Libby-Roberts, Jessica E., Larsen, Alexander, Kobulnicky, Henry A., Mahadevan, Suvrath, Bender, Chad F., Cochran, William D., Endl, Michael, Everett, Mark E., Gupta, Arvind F., Halverson, Samuel, Hearty, Fred, Monson, Andrew, Ninan, Joe P., Roy, Arpita, Schwab, Christian, Terrien, Ryan C.
Format: Article
Language:English
Subjects:
Astronautics (General)
Buttes
Circumstellar habitable zone
Deposition
Dwarf stars
Exoplanet systems
Extrasolar gaseous giant planets
Extrasolar planets
M dwarf stars
Metallicity
Orbits
Photometry
Planet detection
Planetary mass
Planets
Radial velocity
Red dwarf stars
Saturn
Transit
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Summary: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 +0.17 −0.15 g cm−3) with a planetary radius of 9.7 ± 0.5 R⊕ (0.87 ± 0.04 RJup) and a planetary mass of 135+17 −18 M⊕ (0.42+0.05 −0.06 MJup). It has an orbital period of 3.792622+0.000010 −0.000010 days and an orbital eccentricity of 0.06 +0.07 −0.04 . 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.
ISSN:0004-6256
1538-3881
DOI:10.3847/1538-3881/ad09c2