TOI-530b: a giant planet transiting an M-dwarf detected by TESS

Gan, Tianjun; Lin, Zitao; Wang, Sharon Xuesong; Mao, Shude; Fouqué, Pascal; Fan, Jiahao; Bedell, Megan; Stassun, Keivan G.; Giacalone, Steven; Fukui, Akihiko; Murgas, Felipe; Ciardi, David R.; Howell, Steve B.; Collins, Karen A.; Shporer, Avi; Arnold, Luc; Barclay, Thomas; Charbonneau, David; Christiansen, Jessie; Crossfield, Ian J. M.; Dressing, Courtney D.; Elliott, Ashley; Esparza-Borges, Emma; Evans, Phil; Gnilka, Crystal L.; Gonzales, Erica J.; Howard, Andrew W.; Isogai, Keisuke; Kawauchi, Kiyoe; Kurita, Seiya; Liu, Beibei; Livingston, John H.; Matson, Rachel A.; Narita, Norio; Palle, Enric; Parviainen, Hannu; Rackham, Benjamin V.; Rodriguez, David R.; Rose, Mark; Rudat, Alexander; Schlieder, Joshua E.; Scott, Nicholas J.; Vezie, Michael; Ricker, George R.; Vanderspek, Roland; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.
Bibliographical reference

Monthly Notices of the Royal Astronomical Society

Advertised on:
3
2022
Number of authors
49
IAC number of authors
6
Citations
29
Refereed citations
28
Description
We report the discovery of TOI-530b, a transiting Saturn-like planet around an M0.5V dwarf, delivered by the Transiting Exoplanet Survey Satellite (TESS). The host star is located at a distance of 147.7 ± 0.6 pc with a radius of R* = 0.54 ± 0.03 R⊙ and a mass of M* = 0.53 ± 0.02 M⊙. We verify the planetary nature of the transit signals by combining ground-based multiwavelength photometry, high-resolution spectroscopy from SPIRou as well as high-angular-resolution imaging. With V = 15.4 mag, TOI-530b is orbiting one of the faintest stars accessible by ground-based spectroscopy. Our model reveals that TOI-530b has a radius of 0.83 ± 0.05 RJ and a mass of 0.37 ± 0.08 MJ on a 6.39-d orbit. TOI-530b is the sixth transiting giant planet hosted by an M-type star, which is predicted to be infrequent according to core accretion theory, making it a valuable object to further study the formation and migration history of similar planets. Furthermore, we identify a potential dearth of hot massive giant planets around M-dwarfs with separation distance smaller than 0.1 au and planet-to-star mass ratio between 2 × 10-3 and 10-2. We also find a possible correlation between hot giant planet formation and the metallicity of its parent M-dwarf. We discuss the potential formation channel of such systems.
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