TOI-3714 b and TOI-3629 b: Two Gas Giants Transiting M Dwarfs Confirmed with the Habitable-zone Planet Finder and NEID

Cañas, Caleb I.; Kanodia, Shubham; Bender, Chad F.; Mahadevan, Suvrath; Stefánsson, Guðmundur; Cochran, William D.; Lin, Andrea S. J.; Hwang, Hsiang-Chih; Powers, Luke; Monson, Andrew; Green, Elizabeth M.; Parker, Brock A.; Swaby, Tera N.; Kobulnicky, Henry A.; Wisniewski, John P.; Gupta, Arvind F.; Everett, Mark E.; Jones, Sinclaire; Anjakos, Benjamin; Beard, Corey; Blake, Cullen H.; Diddams, Scott A.; Dong, Zehao; Fredrick, Connor; Hakemiamjad, Elnaz; Hebb, Leslie; Libby-Roberts, Jessica E.; Logsdon, Sarah E.; McElwain, Michael; Metcalf, Andrew J.; Ninan, Joe P.; Rajagopal, Jayadev; Ramsey, Lawrence W.; Robertson, Paul; Roy, Arpita; Ruhle, Jacob; Schwab, Christian; Terrien, Ryan C.; Wright, Jason T.

doi:10.3847/1538-3881/ac7804

Cited by 27 publications

(33 citation statements)

References 230 publications

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“…There is a small but growing number of these planets (∼ 11, Fig. 1; hereafter the GGM-D sample) confirmed by NASA's TESS mission (Ricker et al 2015): TOI-1728 b (Kanodia et al 2020), TOI-1899 b (Cañas et al 2020), TOI-442 b (Dreizler et al 2020), TOI-674 b (Murgas et al 2021), TOI-532 b (Kanodia et al 2021), TOI-737 b, TOI-552 b (Jordán et al 2022), TOI-3629 b, TOI-3714 b (Cañas et al 2022), TOI-3757 b (Kanodia et al 2022), and TOI-530 b (Gan et al 2022); all with close-in orbits, thus making them perfect bodies to study tidal evolution around M-dwarf hosts.…”

Section: Introductionmentioning

confidence: 97%

Tidally induced migration of TESS gas giants orbiting M dwarfs

Alvarado-Montes

2022

Monthly Notices of the Royal Astronomical Society

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According to core-accretion formation models, the conditions under which gas giants will form around M dwarfs are very restrictive. Also, the correlation of the occurrence of these planets with the metallicity of host stars is still unknown due to the intrinsic faintness of M dwarfs in the optical and some intricacies in their spectra. Interestingly, NASA’s TESS mission has started to create a growing sample of these systems, with ten observed planets located in close-in orbits: contrary to what is expected for low stellar masses. Tidal interactions with the host star will play a key role in determining the fate of these planets, so by using the measured physical and orbital characteristics of these M-dwarf systems we numerically analyse the exchange of rotational and orbital angular momentum, while constraining the energy dissipation in each system to calculate whether host stars are spun up or spun down, depending on the relationship between the gain and loss of angular momentum by the stellar rotation. We also study the coupled orbital and physical evolution of their gas giant companion and calculate orbital circularization time-scales, as well as the time needed to undergo orbital decay from their current orbital position to the Roche limit. The thorough study of tidal processes occurring over short and long time-scales in star-planet systems like those studied here, can help constrain tidal dissipation rates inside the star and planet, complement tidal theories, and improve estimations of unconstrained properties of exoplanetary systems.

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Section: Introductionmentioning

confidence: 97%

Tidally induced migration of TESS gas giants orbiting M dwarfs

Alvarado-Montes

2022

Monthly Notices of the Royal Astronomical Society

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“…While gas giants are predicted to be rare and hard to form under the core-accretion framework (Laughlin et al 2004;Ida & Lin 2005), they do exist around M dwarfs, as has been evinced by recent discoveries from transiting surveys, especially TESS (Johnson et al 2012;Hartman et al 2015;Bayliss et al 2018;Cañas et al 2020Cañas et al , 2022Jordán et al 2022;Kanodia et al 2022). In addition to transit discoveries, there have been RV-only detections of gas giants around M dwarfs, e.g., Johnson et al (2010) (2022).…”

Section: Discussionmentioning

confidence: 99%

“…New discoveries from the Transiting Exoplanet Survey Satellite (TESS; Ricker et al 2014) have helped find numerous gas giants around M dwarfs despite their rarity (e.g., Cañas et al 2020Cañas et al , 2022Jordán et al 2022;Kanodia et al 2022), by Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.…”

Section: Introductionmentioning

confidence: 99%

TOI-5205b: A Short-period Jovian Planet Transiting a Mid-M Dwarf

Kanodia

Mahadevan

Libby-Roberts

et al. 2023

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We present the discovery of TOI-5205b, a transiting Jovian planet orbiting a solar metallicity M4V star, which was discovered using Transiting Exoplanet Survey Satellite photometry and then confirmed using a combination of precise radial velocities, ground-based photometry, spectra, and speckle imaging. TOI-5205b has one of the highest mass ratios for M-dwarf planets, with a mass ratio of almost 0.3%, as it orbits a host star that is just 0.392 ± 0.015 M ⊙. Its planetary radius is 1.03 ± 0.03 R J, while the mass is 1.08 ± 0.06 M J. Additionally, the large size of the planet orbiting a small star results in a transit depth of ∼7%, making it one of the deepest transits of a confirmed exoplanet orbiting a main-sequence star. The large transit depth makes TOI-5205b a compelling target to probe its atmospheric properties, as a means of tracing the potential formation pathways. While there have been radial-velocity-only discoveries of giant planets around mid-M dwarfs, this is the first transiting Jupiter with a mass measurement discovered around such a low-mass host star. The high mass of TOI-5205b stretches conventional theories of planet formation and disk scaling relations that cannot easily recreate the conditions required to form such planets.

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“…In mass-radius space (Figure 4, top panel), TOI-3235 b joins a small cluster of ten giant planets with 0.8 R J R p 1.2 R J and 0.3 M J M p 1.5 M J . Most of these planets (HATS-6 b, Hartman et al 2015;HATS-74 b and HATS-75 b, Jordán et al 2022;Kepler-45 b, Johnson et al 2012; TOI-530 b, Gan et al 2022; TOI-3714 b, Canas et al 2022;WASP-80 b, Triaud et al 2013) are hosted by early M dwarfs with M å 0.5 M ☉ . The sole other exception, aside from TOI-3235 b itself, is TOI-5205 b, a Jupiter-sized planet transiting a 0.392 M ☉ star (Kanodia et al 2023).…”

Section: Discussionmentioning

confidence: 99%

TOI-3235 b: A Transiting Giant Planet around an M4 Dwarf Star

Jordán

Bryant

Brahm

et al. 2023

ApJL

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We present the discovery of TOI-3235 b, a short-period Jupiter orbiting an M dwarf with a stellar mass close to the critical mass at which stars transition from partially to fully convective. TOI-3235 b was first identified as a candidate from TESS photometry and confirmed with radial velocities from ESPRESSO and ground-based photometry from HATSouth, MEarth-South, TRAPPIST-South, LCOGT, and ExTrA. We find that the planet has a mass of 0.665 ± 0.025 M J and a radius of 1.017 ± 0.044 R J. It orbits close to its host star, with an orbital period of 2.5926 days but has an equilibrium temperature of ≈ 604 K, well below the expected threshold for radius inflation of hot Jupiters. The host star has a mass of 0.3939 ± 0.0030 M ☉, a radius of 0.3697 ± 0.0018 R ☉, an effective temperature of 3389 K, and a J-band magnitude of 11.706 ± 0.025. Current planet formation models do not predict the existence of gas giants such as TOI-3235 b around such low-mass stars. With a high transmission spectroscopy metric, TOI-3235 b is one of the best-suited giants orbiting M dwarfs for atmospheric characterization.

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TOI-3714 b and TOI-3629 b: Two Gas Giants Transiting M Dwarfs Confirmed with the Habitable-zone Planet Finder and NEID

Cited by 27 publications

References 230 publications

Tidally induced migration of TESS gas giants orbiting M dwarfs

Tidally induced migration of TESS gas giants orbiting M dwarfs

TOI-5205b: A Short-period Jovian Planet Transiting a Mid-M Dwarf

TOI-3235 b: A Transiting Giant Planet around an M4 Dwarf Star

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