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TOI-3757 b: A Low-density Gas Giant Orbiting a Solar-metallicity M Dwarf

  • Authors: Shubham Kanodia, Jessica Libby-Roberts, Caleb I. Cañas, Joe P. Ninan, Suvrath Mahadevan, Gudmundur Stefansson, Andrea S. J. Lin, Sinclaire Jones, Andrew Monson, Brock A. Parker, Henry A. Kobulnicky, Tera N. Swaby, Luke Powers, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Jiayin Dong, Scott A. Diddams, Connor Fredrick, Arvind F. Gupta, Samuel Halverson, Fred Hearty, Sarah E. Logsdon, Andrew J. Metcalf, Michael W. McElwain, Caroline Morley, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Ryan C. Terrien, John Wisniewski, Jason T. Wright

Shubham Kanodia et al 2022 The Astronomical Journal 164 .

  • Provider: AAS Journals

Caption: Figure 10.

We show the planetary density of gas giants (R p > 4 R ) around M dwarfs (solid colors) as a function of stellar insolation and stellar metallicity, respectively. In panel (a) the markers are color coded by the equilibrium temperature, whereas panel (b) is color coded by planetary radius. Additionally, TOI-3757 b is highlighted with a green circle. In panel (a), we show that TOI-3757 b does not receive an unusually large amount of incident flux from its host star, compared to other similar gas giants. In panel (b), we show that the host star has the lowest metallicity of all known gas giants around M dwarfs, which could be a potential explanation of its density.

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