HD 202772A b: A Transiting Hot Jupiter around a Bright, Mildly Evolved Star in a Visual Binary Discovered by TESS

Wang, Songhu; Jones, M. I.; Shporer, Avi; Fulton, Benjamin J.; Paredes, Leonardo A.; Trifonov, T.; Kossakowski, D.; Eastman, Jason D.; Redfield, Seth; Günther, Maximilian N.; Kreidberg, Laura; Huang, Chelsea X.; Millholland, Sarah; Seligman, Darryl Z.; Fischer, Debra A.; Brahm, R.; Wang, Xianyu; Cruz, Bryndis; Henry, Todd J.; James, Hodari-Sadiki; Addison, Brett C.; Liang, En-Si; Davis, Allen B.; Tronsgaard, R.; Worku, Keduse; Brewer, John M.; Kürster, M.; Zhang, Hui; Beichman, Charles; Bieryla, Allyson; Brown, Timothy M.; Christiansen, Jessie L.; Ciardi, David R.; Collins, Karen A.; Esquerdo, Gilbert A.; Howard, Andrew W.; Isaacson, Howard; Latham, David W.; Mazeh, T.; Petigura, Erik A.; Quinn, Samuel N.; Shahaf, Sahar; Siverd, Robert J.; Rodler, F.; Reffert, S.; Zakhozhay, O. V.; Ricker, G.; Vanderspek, R.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Boyd, Patricia T.; Fürész, Gábor; Henze, Christopher E.; Levine, A.; Morris, Robert; Paegert, Martin; Stassun, Keivan G.; Ting, Eric B.; Vezie, Michael; Laughlin, Gregory

doi:10.3847/1538-3881/aaf1b7

Cited by 79 publications

(38 citation statements)

References 89 publications

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“…It will also overlap with the CVZs of the James Webb Space Telescope (JWST), providing key targets for detailed characterization. In about a hundred days of observations, TESS has already identified more than a hundred planet candidates, provided key observations to confirm several new planets, and provided new data on known transiting systems (Dragomir et al 2019;Gandolfi et al 2018;Huang et al 2018a;Nielsen et al 2019;Shporer et al 2019;Vanderspek et al 2019;Wang et al 2019;Quinn et al 2019;Rodriguez et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The L 98-59 System: Three Transiting, Terrestrial-size Planets Orbiting a Nearby M Dwarf

Kostov

Schlieder

Barclay

et al. 2019

Self Cite

109

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We report the Transiting Exoplanet Survey Satellite (TESS) discovery of three terrestrial-size planets transiting L 98-59 (TOI-175, TIC 307210830)-a bright M dwarf at a distance of 10.6 pc. Using the Gaia-measured distance and broadband photometry, we find that the host star is an M3 dwarf. Combined with the TESS transits from three sectors, the corresponding stellar parameters yield planet radii ranging from 0.8 R ⊕ to 1.6 R ⊕. All three planets have short orbital periods, ranging from 2.25 to 7.45 days with the outer pair just wide of a 2:1 period resonance. Diagnostic tests produced by the TESS Data Validation Report and the vetting package DAVE rule out common false-positive sources. These analyses, along with dedicated follow-up and the multiplicity of the system, lend confidence that the observed signals are caused by planets transiting L 98-59 and are not associated with other sources in the field. The L 98-59 system is interesting for a number of reasons: the host star is bright (V= 11.7 mag, K=7.1 mag) and the planets are prime targets for further follow-up observations including precision radial-velocity mass measurements and future transit spectroscopy with the James Webb Space Telescope; the near-resonant configuration makes the system a laboratory to study planetary system dynamical evolution; and three planets of relatively similar size in the same system present an opportunity to study terrestrial planets where other variables (age, metallicity, etc.) can be held constant. L 98-59 will be observed in four more TESS sectors, which will provide a wealth of information on the three currently known planets and have the potential to reveal additional planets in the system.

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Section: Introductionmentioning

confidence: 99%

The L 98-59 System: Three Transiting, Terrestrial-size Planets Orbiting a Nearby M Dwarf

Kostov

Schlieder

Barclay

et al. 2019

Self Cite

109

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“…TESS host stars are on average significantly brighter than typical Kepler hosts, facilitating groundbased measurements of planet masses with precisely characterized exoplanet hosts from asteroseismology. While some of the first exoplanets discovered with TESS orbit stars that have evolved off the main sequence (Brahm et al 2018;Nielsen et al 2019;Wang et al 2019), none of them were amenable to asteroseismology using TESS photometry. Here, we present the characterization of the HD 221416 (TESS Object of Interest 197, HIP 116158) system, the first discovery by TESS of a transiting exoplanet around a host star in which oscillations can be measured.…”

Section: Introductionmentioning

confidence: 99%

A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS

Huber

Chaplin

Chontos

et al. 2019

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We present the discovery of HD 221416 b, the first transiting planet identified by the Transiting Exoplanet Survey Satellite (TESS) for which asteroseismology of the host star is possible. HD 221416 b (HIP 116158, TOI-197) is a bright (V=8.2 mag), spectroscopically classified subgiant that oscillates with an average frequency of about 430 μHz and displays a clear signature of mixed modes. The oscillation amplitude confirms that the redder TESS bandpass compared to Kepler has a small effect on the oscillations, supporting the expected yield of thousands of solar-like oscillators with TESS 2 minute cadence observations. Asteroseismic modeling yields a robust determination of the host star radius (R å =2.943±0.064 R e), mass (M å =1.212±0.074 M e), and age (4.9±1.1 Gyr), and demonstrates that it has just started ascending the red-giant branch. Combining asteroseismology with transit modeling and radial-velocity observations, we show that the planet is a "hot Saturn" (R p =9.17±0.33 R ⊕) with an orbital period of ∼14.3 days, irradiance of F=343±24 F ⊕ , and moderate mass (M p =60.5±5.7 M ⊕) and density (ρ p =0.431±0.062 g cm −3). The properties of HD 221416 b show that the host-star metallicity-planet mass correlation found in sub-Saturns (4-8 R ⊕) does not extend to larger radii, indicating that planets in the transition between sub-Saturns and Jupiters follow a relatively narrow range of densities. With a density measured to ∼15%, HD 221416 b is one of the best characterized Saturn-size planets to date, augmenting the small number of known transiting planets around evolved stars and demonstrating the power of TESS to characterize exoplanets and their host stars using asteroseismology.

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“…The Transiting Exoplanet Survey Satellite is building upon this legacy by surveying most of the sky in roughly month-long sectors covering four 24 • × 24 • areas from the ecliptic poles to near the ecliptic plane (Ricker et al 2016). The mission will produce light curves for about 200,000 nearby late-type stars sampled at a 2 minute cadence to open a new era of stellar variability exploration (e.g., Dragomir et al 2019;Huang et al 2018;Ball et al 2018;Shen et al 2018;Wang et al 2019). The Characterizing Exoplanets Satellite will complement these surveys by providing a unique, large sample of high precision photometric monitoring of selected bright target stars (Broeg et al 2013;Gaidos et al 2017).…”

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confidence: 99%

Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation

Paxton¹,

Smolec²,

Schwab³

et al. 2019

ApJS

1,353

1,203

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We update the capabilities of the open-knowledge software instrument Modules for Experiments in Stellar Astrophysics (MESA). RSP is a new functionality in MESAstar that models the non-linear radial stellar pulsations that characterize RR Lyrae, Cepheids, and other classes of variable stars. We significantly enhance numerical energy conservation capabilities, including during mass changes. For example, this enables calculations through the He flash that conserve energy to better than 0.001%. To improve the modeling of rotating stars in MESA, we introduce a new approach to modifying the pressure and temperature equations of stellar structure, and a formulation of the projection effects of gravity darkening. A new scheme for tracking convective boundaries yields reliable values of the convective-core mass, and allows the natural emergence of adiabatic semiconvection regions during both core hydrogen-and helium-burning phases. We quantify the parallel performance of MESA on current generation multicore architectures and demonstrate improvements in the computational efficiency of radiative levitation. We report updates to the equation of state and nuclear reaction physics modules. We briefly discuss the current treatment of fallback in core-collapse supernova models and the thermodynamic evolution of supernova explosions. We close by discussing the new MESA Testhub software infrastructure to enhance source-code development.

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HD 202772A b: A Transiting Hot Jupiter around a Bright, Mildly Evolved Star in a Visual Binary Discovered by TESS

Cited by 79 publications

References 89 publications

The L 98-59 System: Three Transiting, Terrestrial-size Planets Orbiting a Nearby M Dwarf

The L 98-59 System: Three Transiting, Terrestrial-size Planets Orbiting a Nearby M Dwarf

A Hot Saturn Orbiting an Oscillating Late Subgiant Discovered by TESS

Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation

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