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

Creators: 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.

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Abstract

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 R_J and a mass of 0.37 ± 0.08 M_J 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.

Additional Information

© 2021 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2021 October 7. Received 2021 September 26; in original form 2021 July 21. Published: 22 December 2021. We are grateful to Coel Hellier for the insights regarding the WASP data. We also thank Elisabeth Newton, Robert Wells, Hongjing Yang, and Weicheng Zang for useful discussions. We also thank Elise Furlan for the contributions to the speckle data and Nadine Manset for scheduling the SPIRou observations. This work is partly supported by the National Science Foundation of China (Grant No. 11390372 and 11761131004 to SM and TG). This research uses data obtained through the Telescope Access Program (TAP), which has been funded by the TAP member institutes. This work is partly supported by JSPS KAKENHI Grant Numbers JP17H04574, JP18H05439, 20K14521, JST PRESTO Grant Number JPMJPR1775, and the Astrobiology Center of National Institutes of Natural Sciences (NINS) (Grant Number AB031010). This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. Some of the observations in the paper made use of the High-Resolution Imaging instrument 'Alopeke obtained under LLP GN-2021A-LP-105. 'Alopeke was funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Data were reduced using a software pipeline originally written by Elliott Horch and Mark Everett. 'Alopeke was mounted on the Gemini North telescope of the international Gemini Observatory, a program of NSF's OIR Lab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). Funding for the TESS mission is provided by NASA's Science Mission directorate. We acknowledge the use of TESS public data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work made use of tpfplotter by J. Lillo-Box (publicly available in www.github.com/jlillo/tpfplotter), which also made use of the python packages astropy, lightkurve, matplotlib and numpy. Data Availability: This paper includes photometric data collected by the TESS mission and ground instruments, which are publicly available in ExoFOP, at https://exofop.ipac.caltech.edu/tess/target.php?id = 387690507. All spectroscopy data underlying this paper are listed in the text. All of the high-resolution speckle imaging data are available at the NASA exoplanet Archive with no proprietary period.

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