Abstract
Abstract
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
⊕
(0.42
−
0.06
+
0.05
M
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.
Funder
National Aeronautics and Space Administration
National Science Foundation
NASA ∣ NASA Astrobiology Institute
Heising-Simons Foundation
Publisher
American Astronomical Society
Subject
Space and Planetary Science,Astronomy and Astrophysics