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:10.3847/1538-3881/ad09c2

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 RoyChristian Schwab, Ryan C. Terrien

^*Corresponding author for this work

School of Mathematical and Physical Sciences

Research output: Contribution to journal › Article › peer-review

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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^+0.17g 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⁺¹⁷M_⊕ (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.

Original language	English
Article number	4
Pages (from-to)	1-14
Number of pages	14
Journal	Astronomical Journal
Volume	167
Issue number	1
DOIs	https://doi.org/10.3847/1538-3881/ad09c2
Publication status	Published - 1 Jan 2024

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© 2023. The Author(s). Published by the American Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

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Han, T., Robertson, P., Kanodia, S., Cañas, C., Lin, A. S. J., Stefánsson, G., Libby-Roberts, J. E., Larsen, A., Kobulnicky, H. A., Mahadevan, S., Bender, C. F., Cochran, W. D., Endl, M., Everett, M. E., Gupta, A. F., Halverson, S., Hearty, F., Monson, A., Ninan, J. P., ... Terrien, R. C. (2024). TOI-5344 b: A Saturn-like planet orbiting a super-solar metallicity M0 dwarf. Astronomical Journal, 167(1), 1-14. Article 4. https://doi.org/10.3847/1538-3881/ad09c2

@article{34bd339cb0e648fe96adcc83f658d571,

title = "TOI-5344 b: A Saturn-like planet orbiting a super-solar metallicity M0 dwarf",

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+0.17g cm−3) with a planetary radius of 9.7 ± 0.5 R⊕ (0.87 ± 0.04 RJup) and a planetary mass of 135−18+17M⊕ (0.42−0.06+0.05 MJup ). 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.",

author = "Te Han and Paul Robertson and Shubham Kanodia and Caleb Ca{\~n}as and Lin, \{Andrea S. J.\} and Gumundur Stef{\'a}nsson and Libby-Roberts, \{Jessica E.\} and Alexander Larsen and Kobulnicky, \{Henry A.\} and Suvrath Mahadevan and Bender, \{Chad F.\} and Cochran, \{William D.\} and Michael Endl and Everett, \{Mark E.\} and Gupta, \{Arvind F.\} and Samuel Halverson and Fred Hearty and Andrew Monson and Ninan, \{Joe P.\} and Arpita Roy and Christian Schwab and Terrien, \{Ryan C.\}",

note = "{\textcopyright} 2023. The Author(s). Published by the American Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher. ",

year = "2024",

month = jan,

day = "1",

doi = "10.3847/1538-3881/ad09c2",

language = "English",

volume = "167",

pages = "1--14",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "American Astronomical Society",

number = "1",

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Han, T, Robertson, P, Kanodia, S, Cañas, C, Lin, ASJ, Stefánsson, G, Libby-Roberts, JE, Larsen, A, Kobulnicky, HA, Mahadevan, S, Bender, CF, Cochran, WD, Endl, M, Everett, ME, Gupta, AF, Halverson, S, Hearty, F, Monson, A, Ninan, JP, Roy, A, Schwab, C & Terrien, RC 2024, 'TOI-5344 b: A Saturn-like planet orbiting a super-solar metallicity M0 dwarf', Astronomical Journal, vol. 167, no. 1, 4, pp. 1-14. https://doi.org/10.3847/1538-3881/ad09c2

TY - JOUR

T1 - TOI-5344 b

T2 - A Saturn-like planet orbiting a super-solar metallicity M0 dwarf

AU - Han, Te

AU - Robertson, Paul

AU - Kanodia, Shubham

AU - Cañas, Caleb

AU - Lin, Andrea S. J.

AU - Stefánsson, Gumundur

AU - Libby-Roberts, Jessica E.

AU - Larsen, Alexander

AU - Kobulnicky, Henry A.

AU - Mahadevan, Suvrath

AU - Bender, Chad F.

AU - Cochran, William D.

AU - Endl, Michael

AU - Everett, Mark E.

AU - Gupta, Arvind F.

AU - Halverson, Samuel

AU - Hearty, Fred

AU - Monson, Andrew

AU - Ninan, Joe P.

AU - Roy, Arpita

AU - Schwab, Christian

AU - Terrien, Ryan C.

N1 - © 2023. The Author(s). Published by the American Astronomical Society. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

PY - 2024/1/1

Y1 - 2024/1/1

N2 - 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+0.17g cm−3) with a planetary radius of 9.7 ± 0.5 R⊕ (0.87 ± 0.04 RJup) and a planetary mass of 135−18+17M⊕ (0.42−0.06+0.05 MJup ). 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.

AB - 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+0.17g cm−3) with a planetary radius of 9.7 ± 0.5 R⊕ (0.87 ± 0.04 RJup) and a planetary mass of 135−18+17M⊕ (0.42−0.06+0.05 MJup ). 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.

UR - https://www.scopus.com/pages/publications/85180078521

U2 - 10.3847/1538-3881/ad09c2

DO - 10.3847/1538-3881/ad09c2

M3 - Article

AN - SCOPUS:85180078521

SN - 0004-6256

VL - 167

SP - 1

EP - 14

JO - Astronomical Journal

JF - Astronomical Journal

IS - 1

M1 - 4

ER -

TOI-5344 b: A Saturn-like planet orbiting a super-solar metallicity M0 dwarf

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