TESS Discovery of a Transiting Super-Earth in the pi Mensae System

Huang, Chelsea X.; Burt, Jennifer; Vanderburg, Andrew; Günther, Maximilian N.; Shporer, Avi; Dittmann, Jason; Winn, Joshua N.; Wittenmyer, R. A.; Sha, Lizhou; Kane, Stephen R.; Ricker, G.; Vanderspek, R.; Latham, David W.; Seager, Sara; Jenkins, Jon M.; Caldwell, Douglas A.; Collins, Karen A.; Guerrero, Natalia; Smith, Jeffrey C.; Quinn, Samuel N.; Udry, S.; Pepe, F.; Bouchy, F.; Ségransan, D.; Lovis, C.; Ehrenreich, D.; Marmier, M.; Mayor, M.; Wohler, Bill; Haworth, Kari; Morgan, E.; Fausnaugh, Michael; Ciardi, David R.; Christiansen, Jessie L.; Charbonneau, David; Dragomir, Diana; Deming, Drake; Glidden, Ana; Levine, Alan M.; McCullough, P. R.; Yu, Li; Narita, Norio; Nguyen, Tam T.; Morton, Tim; Pepper, Joshua; Pál, András; Rodriguez, Joseph E.; Stassun, Keivan G.; Torres, Guillermo; Sozzetti, A.; Doty, J.; Christensen‐Dalsgaard, J.; Laughlin, Gregory; Clampin, Mark; Bean, Jacob L.; Buchhave, Lars A.; Bakos, G. Á.; Sato, Bun’ei; Ida, Shigeru; Kaltenegger, Lisa; Πάλλη, Ε.; Sasselov, Dimitar; Butler, R. Paul; Lissauer, Jack J.; Ge, Jian; Rinehart, Stephen A.

doi:10.3847/2041-8213/aaef91

Cited by 178 publications

(141 citation statements)

References 37 publications

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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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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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“…The other three targets were not included in the set of stars observed in short-cadence mode by the mission, so only ∼ 30 min integrations from the Full Frame Images (FFIs) are available for these objects. Of these, HATS-72 was bright enough to have a light curve produced from the FFI observations by the TESS Quick Look Pipeline (QLP; Huang et al 2018) at MIT. We made use of the detrended light curve for HATS-72 produced by this pipeline.…”

Section: Tessmentioning

confidence: 99%

HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b: Four Warm Giant Planets Transiting K Dwarfs*

Hartman

Jordán

Bakos

et al. 2020

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site is operated in conjunction with MPIA, and the station at Siding Spring Observatory (SSO) is operated jointly with ANU. Based in part on observations made with the MPG 2.2 m Telescope at the ESO Observatory in La Silla. Based on observations collected at the European Southern Observatory. This paper includes data gathered with the 6.5 meter Magellan Telescopes at Las Campanas Observatory, Chile. ABSTRACTWe report the discovery of four transiting giant planets around K dwarfs. The planets HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b have masses of 0.369 +0.031 −0.021 M J , 0.243 +0.022 −0.030 M J , 0.353 +0.038 −0.027 M J and 0.1254 ± 0.0039 M J , respectively, and radii of 1.117 ± 0.014 R J , 0.800 ± 0.015 R J , 0.765 ± 0.013 R J , and 0.7224 ± 0.0032 R J , respectively. The planets orbit close to their host stars with orbital periods of 3.9228 d, 3.1317 d, 4.1480 d and 7.3279 d, respectively. The hosts are main sequence K dwarfs with masses of 0.674 +0.016 −0.012 M , 0.7279 ± 0.0066 M , 0.7133 ± 0.0075 M , and 0.7311 ± 0.0028, and with V -band magnitudes of V = 14.829 ± 0.010, 14.35 ± 0.11, 14.998 ± 0.040 and 12.469 ± 0.010. The Super-Neptune HATS-72b (a.k.a. WASP-191b and TOI 294.01) was independently identified as a transiting planet candidate by the HATSouth, WASP and TESS surveys, and we present a combined analysis of all of the data gathered by each of these projects (and their follow-up programs). An exceptionally precise mass is measured for HATS-72b thanks to high-precision radial velocity (RV) measurements obtained with VLT/ESPRESSO, FEROS, HARPS and Magellan/PFS. We also incorporate TESS observations of the warm Saturn-hosting systems HATS-47 (a.k.a. TOI 1073.01), HATS-48A and HATS-49. HATS-47 was independently identified as a candidate by the TESS team, while the other two systems were not previously identified from the TESS data. The RV orbital variations are measured for these systems using Magellan/PFS. HATS-48A has a resolved 5. 4 neighbor in Gaia DR2, which is a common-proper-motion binary star companion to HATS-48A with a mass of 0.22 M and a current projected physical separation of ∼1,400 au.

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“…The Transiting Exoplanet Survey Satellite (TESS ; Ricker et al 2015) is well suited to address these questions by discovering more systems like WASP-47 and Kepler-730. By observing most of the sky, TESS is expected to find thousands of hot Jupiters (Sullivan et al 2015), while also having good enough photometric precision to find smaller planets around the same stars (see, e.g., Huang et al 2018), especially those with short orbital periods.…”

Section: Introductionmentioning

confidence: 99%

TESS Spots a Hot Jupiter with an Inner Transiting Neptune

Huang

Quinn

Vanderburg

et al. 2020

ApJL

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2Hot Jupiters are rarely accompanied by other planets within a factor of a few in orbital distance. Previously, only two such systems have been found. Here, we report the discovery of a third system using data from the Transiting Exoplanet Survey Satellite (TESS ). The host star, TOI-1130, is an 11th magnitude K-dwarf in Gaia G band. It has two transiting planets: a Neptune-sized planet (3.65 ± 0.10 R ⊕ ) with a 4.1-day period, and a hot Jupiter (1.50 +0.27 −0.22 R J ) with an 8.4-day period. Precise radial-velocity observations show that the mass of the hot Jupiter is 0.974 +0.043 −0.044 M J . For the inner Neptune, the data provide only an upper limit on the mass of 0.17 M J (3σ). Nevertheless, we are confident the inner planet is real, based on follow-up ground-based photometry and adaptive optics imaging that rule out other plausible sources of the TESS transit signal. The unusual planetary architecture of and the brightness of the host star make TOI-1130 a good test case for planet formation theories, and an attractive target for future spectroscopic observations.

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TESS Discovery of a Transiting Super-Earth in the pi Mensae System

Cited by 178 publications

References 37 publications

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

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

HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b: Four Warm Giant Planets Transiting K Dwarfs*

TESS Spots a Hot Jupiter with an Inner Transiting Neptune

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