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

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

doi:10.3847/1538-3881/ac7c20

Cited by 17 publications

(13 citation statements)

References 163 publications

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“…However, similar to TOI-3757 b (Kanodia et al 2022), we see that this periodic signal is likely an artifact from the photometry reduction of the FFI. The signal is seen a few adjoining pixels in an 8 × 8 grid centered on the centroid for TOI-5205, which suggests that the signal is not astrophysical in origin.…”

Section: A32 Rotation Period Estimatessupporting

confidence: 54%

“…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%

“…Despite the enhanced detection signatures, the sample of confirmed transiting gas giants with precise mass measurements around M dwarfs consists of only <10 planets. All of these transiting gas giants around M dwarfs orbit early-M host stars, most of which are also metal-rich stars (Gan et al 2022;Kanodia et al 2022). These trends agree with the mass budget argument, which necessitates massive stars (and disks) with high dust content to form the 10 M ⊕ cores (Pollack et al 1996) in a timely manner before the disk dissipates.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: A32 Rotation Period Estimatessupporting

confidence: 54%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Kanodia

Mahadevan

Libby-Roberts

et al. 2023

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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: 90%

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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The GAPS programme at TNG

Maldonado¹,

Petralia²,

Mantovan³

et al. 2023

A&A

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Context. Massive substellar companions orbiting active low-mass stars are rare. They, however, offer an excellent opportunity to study the main mechanisms involved in the formation and evolution of substellar objects. Aims. We aim to unravel the physical nature of the transit signal observed by the TESS space mission on the active M dwarf TOI-5375. Methods. We analysed the available TESS photometric data as well as high-resolution (R ~ 115 000) HARPS-N spectra. We combined these data to characterise the star TOI-5375 and to disentangle signals related to stellar activity from the companion transit signal in the light-curve data. We ran a Markov chain Monte Carlo analysis to derive the orbital solution and applied state-of-the-art Gaussian process regression to deal with the stellar activity signal. Results. We reveal the presence of a companion in the boundary between the brown dwarfs and the very-low-mass stars orbiting around the star TOI-5375. The best-fit model corresponds to a companion with an orbital period of 1.721564 ± 10−6 d, a mass of 77 ± 8 MJ, and a radius of 0.99 ± 0.16 RJ. Conclusions. We derive a rotation period for the host star of 1.9692 ± 0.0004 d, and we conclude that the star is very close to synchronising its rotation with the orbital period of the companion.

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

Cited by 17 publications

References 163 publications

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

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

Tidally induced migration of TESS gas giants orbiting M dwarfs

The GAPS programme at TNG

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