TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert

Burt, Jennifer; Nielsen, L. D.; Quinn, Samuel N.; Mamajek, Eric E.; Matthews, Elisabeth C.; Zhou, George; Seidel, J. V.; Huang, Chelsea X.; Lopez, Eric; Soto, M. G.; Otegi, J. F.; Stassun, Keivan G.; Kreidberg, Laura; Collins, Karen A.; Eastman, Jason D.; Rodriguez, Joseph E.; Vanderburg, Andrew; Halverson, Samuel; Teske, Johanna; Wang, Sharon X.; Butler, R. Paul; Bouchy, F.; Dumusque, X.; Segransen, Damien; Shectman, Stephen; Crane, Jeffrey D.; Feng, Fabo; Montet, Benjamin T.; Feinstein, Adina D.; Beletski, Yuri; Flowers, Erin; Günther, Maximilian N.; Daylan, Tansu; Collins, Kevin I.; Conti, Dennis M.; Gan, Tianjun; Jensen, Eric L. N.; Kielkopf, John F.; Tan, T. G.; Helled, Ravit; Dorn, Caroline; Haldemann, Jonas; Lissauer, Jack J.; Ricker, G.; Vanderspek, R.; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Twicken, Joseph D.; Smith, Jeffrey C.; Tenenbaum, P.; Cartwright, Scott; Barclay, Thomas; Pepper, Joshua; Esquerdo, Gilbert A.; Fong, William

doi:10.3847/1538-3881/abac0c

Cited by 39 publications

(29 citation statements)

References 140 publications

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“…This is in line with other works (e.g. Burt et al 2020) and suggests additional light from other sources contaminates the SPOC aperture. We found the 2 background stars in the NGTS aperture contribute a negligible amount of third light and do not correct the NGTS transit depths.…”

Section: Orbital Geometry and Transit Propertiessupporting

confidence: 93%

TIC-320687387 B: a long-period eclipsing M-dwarf close to the hydrogen burning limit

Gill,

Ulmer-Moll,

Wheatley

et al. 2022

Preprint

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We are using precise radial velocities from CORALIE together with precision photometry from the Next Generation Transit Survey (NGTS) to follow up stars with single-transit events detected with the Transiting Exoplanet Survey Satellite (TESS). As part of this survey we identified a single transit on the star TIC-320687387, a bright (𝑇 = 11.6) G-dwarf observed by TESS in Sector 13 and 27. From subsequent monitoring of TIC-320687387 with CORALIE, NGTS, and Lesedi we determined that the companion, TIC-320687387 B, is a very low-mass star with a mass of 96.2± 1.9 2.0 𝑀 J and radius of 1.14± 0.02 0.02 𝑅 J placing it close to the hydrogen burning limit (∼ 80 𝑀 J ). TIC-320687387 B has a wide and eccentric orbit, with a period of 29.77381 days and an eccentricity of 0.366 ± 0.003. Eclipsing systems such as TIC-320687387 AB allow us to test stellar evolution models for low-mass stars, which in turn are needed to calculate accurate masses and radii for exoplanets orbiting single low-mass stars. The wide orbit of TIC-320687387 B makes it particularly valuable as its evolution can be assumed to be free from perturbations caused by tidal interactions with its G-type host star.

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Section: Orbital Geometry and Transit Propertiessupporting

confidence: 93%

TIC-320687387 B: a long-period eclipsing M-dwarf close to the hydrogen burning limit

Gill,

Ulmer-Moll,

Wheatley

et al. 2022

Preprint

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“…When handling crowded regions and faint sources like TOI 1227 (see Figure 1), the SPOC reduction of TESS data has been known to oversubtract the sky background (Burt et al 2020), leading to a deeper transit depth. This was a potential issue for data collected prior to Sector 27, after which SPOC applied a correction to their reduction.…”

Section: Mcmc Fit Of the Transitmentioning

confidence: 99%

TESS Hunt for Young and Maturing Exoplanets (THYME) VI: an 11 Myr giant planet transiting a very low-mass star in Lower Centaurus Crux

Mann,

Wood,

Schmidt

et al. 2021

Preprint

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Mature super-Earths and sub-Neptunes are predicted to be Jovian radius when younger than 10 Myr. Thus, we expect to find 5-15R ⊕ planets around young stars even if their older counterparts harbor none. We report the discovery and validation of TOI 1227 b, a 0.85 ± 0.05 R J (9.5R ⊕ ) planet transiting a very low-mass star (0.170 ± 0.015 M ) every 27.4 days. TOI 1227's kinematics and strong lithium absorption confirm it is a member of a previously discovered sub-group in the Lower Centaurus Crux OB association, which we designate the Musca group. We derive an age of 11±2 Myr for Musca, based on lithium, rotation, and the color-magnitude diagram of Musca members. The TESS data and ground-based followup show a deep (2.5%) transit. We use multiwavelength transit observations and radial velocities from the IGRINS spectrograph to validate the signal as planetary in nature, and we obtain an upper limit on the planet mass of 0.5 M J . Because such large planets are exceptionally rare around mature low-mass stars, we suggest that TOI 1227 b is still contracting and will eventually turn into one of the more common < 5R ⊕ planets.

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“…We used keplerspline from Vanderburg & Johnson (2014) to account for the long-term variability of the TESS lightcurves and averaged 10 model data points over the 30 minute Sectors 9 and 10 exposures, and 4 model data points over the 10 minute Sectors 36 and 37 exposures. We also fit a dilution term to the TESS lightcurves to account for poor background-subtraction (Burt et al 2020). In practice, fitting the dilution term means the transit depth is defined by the ground-based lightcurves.…”

Section: Transit-only Model With Exofastv2mentioning

confidence: 99%

TOI-3362b: A Proto Hot Jupiter Undergoing High-eccentricity Tidal Migration

Dong

Huang

Zhou

et al. 2021

ApJL

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High-eccentricity tidal migration is a possible way for giant planets to be placed in short-period orbits. If this happens often, one would expect to catch proto hot Jupiters on highly elliptical orbits undergoing high-eccentricity tidal migration. As of yet, few such systems have been discovered. Here, we introduce TOI-3362b (TIC-464300749b), an 18.1 day, 5 M Jup planet orbiting a main-sequence F-type star that is likely undergoing higheccentricity tidal migration. The orbital eccentricity is 0.815 -+ 0.032 0.023 . With a semimajor axis of 0.153 -+ 0.003 0.002 au, the planet's orbit is expected to shrink to a final orbital radius of 0.051 -+ 0.006 0.008 au after complete tidal circularization. Several mechanisms could explain the extreme value of the planet's eccentricity, such as planet-planet scattering and secular interactions. Such hypotheses can be tested with follow-up observations of the system, e.g., measuring the stellar obliquity and searching for companions in the system with precise, long-term radial-velocity observations. The variation in the planet's equilibrium temperature as it orbits the host star and the tidal heating at periapse make this planet an intriguing target for atmospheric modeling and observation. Because the planet's orbital period of 18.1 days is near the limit of TESS's period sensitivity, even a few such discoveries suggest that proto hot Jupiters may be quite common.

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TOI-824 b: A New Planet on the Lower Edge of the Hot Neptune Desert

Cited by 39 publications

References 140 publications

TIC-320687387 B: a long-period eclipsing M-dwarf close to the hydrogen burning limit

TIC-320687387 B: a long-period eclipsing M-dwarf close to the hydrogen burning limit

TESS Hunt for Young and Maturing Exoplanets (THYME) VI: an 11 Myr giant planet transiting a very low-mass star in Lower Centaurus Crux

TOI-3362b: A Proto Hot Jupiter Undergoing High-eccentricity Tidal Migration

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