TESS Delivers Its First Earth-sized Planet and a Warm Sub-Neptune*

Dragomir, Diana; Teske, Johanna; Günther, Maximilian N.; Ségransan, D.; Burt, Jennifer; Huang, Chelsea X.; Vanderburg, Andrew; Matthews, Elisabeth C.; Dumusque, X.; Stassun, Keivan G.; Pepper, Joshua; Ricker, G.; Vanderspek, R.; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Beatty, Thomas G.; Bouchy, F.; Brown, Timothy M.; Butler, R. Paul; Ciardi, David R.; Crane, Jeffrey D.; Eastman, Jason D.; Fossati, L.; Francis, Jim; Fulton, Benjamin J.; Gaudi, B. Scott; Goeke, R.; James, D. J.; Klaus, Todd C.; Kuhn, Rudolf B.; Lovis, C.; Lund, Michael B.; McDermott, Scott; Paegert, Martin; Pepe, F.; Rodriguez, Joseph E.; Sha, Lizhou; Shectman, Stephen; Shporer, Avi; Siverd, Robert J.; Soto, Aylin Garciá; Stevens, Daniel J.; Twicken, Joseph D.; Udry, S.; Villanueva, Steven; Wang, Sharon X.; Wohler, Bill; Yao, Xinyu; Zhan, Zhuchang

doi:10.3847/2041-8213/ab12ed

Cited by 85 publications

(67 citation statements)

References 53 publications

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“…As expected, most of these confirmed exoplanet-hosting stars are in the thin disc (e.g. Jones et al 2018;Wang et al 2018;Dragomir et al 2019;Huber et al 2019). Esposito et al (2018) reported the existence of a hot Neptune orbiting an inactive G7 dwarf star, TOI 118, which we classify as a kinematic thick disc star.…”

Section: The Chemo-kinematics Of the Tess Objects Of Interestsupporting

confidence: 59%

Know thy star, know thy planet: chemo-kinematically characterizing TESS targets

Carrillo

Hawkins

Bowler

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The Transiting Exoplanet Survey Satellite (TESS ) has already begun to discover what will ultimately be thousands of exoplanets around nearby cool bright stars. These potential host stars must be well-understood to accurately characterize exoplanets at the individual and population levels. We present a catalogue of the chemo-kinematic properties of 2,218,434 stars in the TESS Candidate Target List using survey data from Gaia DR2, APOGEE, GALAH, RAVE, LAMOST, and photometrically-derived stellar properties from SkyMapper. We compute kinematic thin disc, thick disc, and halo membership probabilities for these stars and find that though the majority of TESS targets are in the thin disc, 4% of them reside in the thick disc and <1% of them are in the halo. The TESS Objects of Interest in our sample also display similar contributions from the thin disc, thick disc, and halo with a majority of them being in the thin disc. We also explore metallicity and [α/Fe] distributions for each Galactic component and show that each cross-matched survey exhibits metallicity and [α/Fe] distribution functions that peak from higher to lower metallicity and lower to higher [α/Fe] from the thin disc to the halo. This catalogue will be useful to explore planet occurrence rates, among other things, with respect to kinematics, componentmembership, metallicity, or [α/Fe].

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Section: The Chemo-kinematics Of the Tess Objects Of Interestsupporting

confidence: 59%

Know thy star, know thy planet: chemo-kinematically characterizing TESS targets

Carrillo

Hawkins

Bowler

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…We considered stars with P thick /P thin > 10 to be in the thick disk while stars in between (0.1 < P thick /P thin < 10) are ambiguous to judge. Up to now, TESS has detected five planet host stars located in the in-between region: TOI 118 (Esposito et al 2019), TOI 144 (Huang et al 2018b), TOI 172 (Rodriguez et al 2019), TOI 186 (Trifonov et al 2019;Dragomir et al 2019) andTOI 197 (Huber et al 2019). Table 4 lists their relative probabilities and none of them show clear-cut thick-disk probability.…”

Section: Thick-disk Characteristicsmentioning

confidence: 99%

LHS 1815b: The First Thick-disk Planet Detected by TESS

Gan

Shporer

Livingston

et al. 2020

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We report the first discovery of a thick-disk planet, LHS 1815b (TOI-704b, TIC 260004324), detected in the TESS survey. LHS 1815b transits a bright (V = 12.19 mag, K = 7.99 mag) and quiet M dwarf located 29.87 ± 0.02 pc away with a mass of 0.502 ± 0.015 M and a radius of 0.501 ± 0.030 R . We validate the planet by combining space and ground-based photometry, spectroscopy, and imaging. The planet has a radius of 1.088 ± 0.064 R ⊕ with a 3σ mass upper-limit of 8.7 M ⊕ . We analyze the galactic kinematics and orbit of the host star LHS 1815 and find that it has a large probability (P thick /P thin = 6482) to be in the thick disk 2 with a much higher expected maximal height (Z max = 1.8 kpc) above the Galactic plane compared with other TESS planet host stars. Future studies of the interior structure and atmospheric properties of planets in such systems using for example the upcoming James Webb Space Telescope (JWST), can investigate the differences in formation efficiency and evolution for planetary systems between different Galactic components (thick and thin disks, and halo).

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“…For the first time in human history, it is possible to find and characterize nearby rocky and potentially hab-et al 2007;Dressing & Charbonneau 2015) − systems that are especially amenable to spectroscopic observation due to their high transit frequency, low star-toplanet brightness contrasts, prolonged main sequence lifetimes, and abundance in both the solar neighborhood and the projected Transiting Exoplanet Survey Satellite (TESS) sample (Henry et al 2006;Barclay et al 2018). Indeed, TESS has already found small and Earthsized planets transiting cool stars (e.g., Vanderspek et al 2019;Dragomir et al 2019). Upcoming characterization efforts by the James Webb Space Telescope, groundbased 30-meter extremely large telescopes, and direct imaging missions will likely attempt to detect habitability indicators (e.g., N 2 , H 2 O v ) and/or biosignatures (O 2 , O 3 , CH 4 , N 2 O, CO 2 ; Sagan et al 1993) on these K-and M-dwarf systems.…”

Section: Introductionmentioning

confidence: 99%

Habitability and Spectroscopic Observability of Warm M-dwarf Exoplanets Evaluated with a 3D Chemistry-Climate Model

Chen

Wolf

Zhan

et al. 2019

ApJ

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Planets residing in circumstellar habitable zones (CHZs) offer our best opportunities to test hypotheses of life's potential pervasiveness and complexity. Constraining the precise boundaries of habitability and its observational discriminants is critical to maximizing our chances at remote life detection with future instruments. Conventionally, calculations of the inner edge of the habitable zone (IHZ) have been performed using both 1D radiative-convective and 3D general circulation models. However, these models lack interactive three-dimensional chemistry and do not resolve the mesosphere and lower thermosphere (MLT) region of the upper atmosphere. Here we employ a 3D high-top chemistry-climate model (CCM) to simulate the atmospheres of synchronously-rotating planets orbiting at the inner edge of habitable zones of K-and M-dwarf stars (between T eff = 2600 K and 4000 K). Specifically, we present the first simultaneous 3D investigation of climate, photochemistry, and circulation on moist and runaway greenhouse atmospheres. Simulations are conducted for planets with N 2 -O 2 -H 2 O v -CO 2dominated atmospheres around a range of stellar spectral types with self-consistent stellar spectral energy distribution (SED)-orbital period relationships. While our IHZ climate predictions are in good agreement with GCM studies, we find noteworthy departures in simulated ozone and HO x photochemistry. For instance, climates around inactive stars do not typically enter the classical moist greenhouse regime even with high ( 10 −3 mol mol −1 ) stratospheric water vapor mixing ratios, which suggests that planets around inactive M-stars may only experience minor water-loss over geologically significant timescales. In addition, we find much thinner ozone layers on potentially habitable moist greenhouse atmospheres, as ozone experiences rapid destruction via reaction with hydrogen oxide radicals. Using our CCM results as inputs, our simulated transmission spectra and secondary eclipse thermal emission spectra show that both water vapor and ozone features of these atmospheres could be detectable by instruments NIRSpec and MIRI LRS aboard the James Webb Space Telescope. Our work indicates that simultaneous constraints on the UV emission of low-mass stars and the orbital properties of their attending planets, in conjunction with coupled physical-chemical numerical modeling, will be critical to understanding the habitability and observational prospects of rocky exoplanets.

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TESS Delivers Its First Earth-sized Planet and a Warm Sub-Neptune*

Cited by 85 publications

References 53 publications

Know thy star, know thy planet: chemo-kinematically characterizing TESS targets

Know thy star, know thy planet: chemo-kinematically characterizing TESS targets

LHS 1815b: The First Thick-disk Planet Detected by TESS

Habitability and Spectroscopic Observability of Warm M-dwarf Exoplanets Evaluated with a 3D Chemistry-Climate Model

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