Global analysis of the TRAPPIST Ultra-Cool Dwarf Transit Survey

Lienhard, Florian; Queloz, D.; Gillon, M.; Burdanov, Artem; Delrez, Laetitia; Ducrot, Elsa; Handley, Will; Jehin, Emmanuël; Murray, C. A.; Triaud, A. H. M. J.; Gillen, Edward; Mortier, A.; Rackham, Benjamin V.

doi:10.1093/mnras/staa2054

Cited by 24 publications

(28 citation statements)

References 75 publications

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“…curve, which has already undergone detrending and systematics corrections by the SPOC pipeline. The presented recovery rates are, therefore, systematically higher than one might otherwise expect if the signals had been injected into the raw light curve (e.g., Lienhard et al 2020). Overall, this analysis highlights the difficulties associated with detecting longer-period planets using automated algorithms, and demonstrates a need for alternative detection methods such as citizen science.…”

Section: Limits On Additional Planetsmentioning

confidence: 76%

Planet Hunters TESS III: two transiting planets around the bright G dwarf HD 152843

Eisner

Nicholson

Barragán

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We report on the discovery and validation of a two-planet system around a bright (V = 8.85 mag) early G dwarf (1.43 R⊙ , 1.15 M⊙ , TOI 2319) using data from NASA’s Transiting Exoplanet Survey Satellite (TESS). Three transit events from two planets were detected by citizen scientists in the month-long TESS light curve (sector 25), as part of the Planet Hunters TESS project. Modelling of the transits yields an orbital period of $11.6264 _{ - 0.0025 } ^ { + 0.0022 }$ days and radius of $3.41 _{ - 0.12 } ^ { + 0.14 }$ R⊕ for the inner planet, and a period in the range 19.26–35 days and a radius of $5.83 _{ - 0.14 } ^ { + 0.14 }$ R⊕ for the outer planet, which was only seen to transit once. Each signal was independently statistically validated, taking into consideration the TESS light curve as well as the ground-based spectroscopic follow-up observations. Radial velocities from HARPS-N and EXPRES yield a tentative detection of planet b, whose mass we estimate to be $11.56 _{ - 6.14 } ^ { + 6.58 }$ M⊕, and allow us to place an upper limit of 27.5 M⊕ (99 per cent confidence) on the mass of planet c. Due to the brightness of the host star and the strong likelihood of an extended H/He atmosphere on both planets, this system offers excellent prospects for atmospheric characterisation and comparative planetology.

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Section: Limits On Additional Planetsmentioning

confidence: 76%

Planet Hunters TESS III: two transiting planets around the bright G dwarf HD 152843

Eisner

Nicholson

Barragán

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…It has been used in detrending photometric data (e.g. Carter & Winn 2009;Csizmadia et al 2015;Aigrain et al 2016;Pepper et al 2017;Luger et al 2017;Santerne et al 2018;Lienhard et al 2020;Nowak et al 2020;Leleu et al 2021), in disentangling planetary signals from stellar activity in radial velocity signals (e.g. Haywood et al 2014;Rajpaul et al 2015Rajpaul et al , 2016Faria et al 2016;Suárez Mascareño et al 2018;Barragán et al 2019;Damasso et al 2020;Ahrer et al 2021) and in transmission spectroscopy (e.g.…”

Section: Detrending With Gaussian Process Regressionmentioning

confidence: 99%

LRG-BEASTS: sodium absorption and Rayleigh scattering in the atmosphere of WASP-94A b using NTT/EFOSC2

Ahrer,

Wheatley,

Kirk

et al. 2022

Preprint

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We present an optical transmission spectrum for WASP-94A b, the first atmospheric characterisation of this highly-inflated hot Jupiter. The planet has a reported radius of 1.72 +0.06 −0.05 R Jup , a mass of only 0.456 +0.032 −0.036 M Jup , and an equilibrium temperature of 1508 ± 75 K. We observed the planet transit spectroscopically with the EFOSC2 instrument on the ESO New Technology Telescope (NTT) at La Silla, Chile: the first use of NTT/EFOSC2 for transmission spectroscopy. We achieved an average transitdepth precision of 128 ppm for bin widths of ∼ 200 Å. This high precision was achieved in part by linking Gaussian Process hyperparameters across all wavelength bins. The resulting transmission spectrum, spanning a wavelength range of 3800−7140 Å, exhibits a sodium absorption with a significance of 4.9𝜎, suggesting a relatively cloud-free atmosphere. The sodium signal may be broadened, with a best fitting width of 78 +67 −32 Å in contrast to the instrumental resolution of 27.2 ± 0.2 Å. We also detect a steep slope in the blue end of the transmission spectrum, indicating the presence of Rayleigh scattering in the atmosphere of WASP-94A b. Retrieval models show evidence for the observed slope to be super-Rayleigh and potential causes are discussed. Finally, we find narrow absorption cores in the CaII H&K lines of WASP-94A, suggesting the star is enshrouded in gas escaping the hot Jupiter.

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“…The second part of our analysis involves studying the dynamical evolution of this debris in three multi-planet, M-dwarf hosted systems (TRAPPIST-1, Proxima Centauri and TOI-700: Gillon et al 2016;Anglada-Escudé et al 2016;Gilbert et al 2020). In all cases we utilize the current published orbits and masses for the systems' planets as inputs for our numerical simulations (Anglada-Escudé et al 2016;Gillon et al 2017;Lienhard et al 2020;Damasso et al 2020;Kervella et al 2020;Suárez Mascareño et al 2020;Agol et al 2021). TRAPPIST-1 is an 0.0898 M M8V dwarf (Lienhard et al 2020) with three planets in the HZ (e, f and g).…”

Section: High-resolution Bombardment Models 221 Systems Of Interestmentioning

confidence: 99%

Habitable planet formation around low-mass stars: Rapid accretion, rapid debris removal and the essential contribution of external giants

Clement,

Quintana,

Quarles

2022

Preprint

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In recent years a paradigm shift has occurred in exoplanet science, wherein low-mass stars are increasingly viewed as a foundational pillar of the search for potentially habitable worlds in the solar neighborhood. However, the formation processes of this rapidly accumulating sample of planet systems are still poorly understood. Moreover, it is unclear whether tenuous primordial atmospheres around these Earth-analogs could have survived the intense epoch of heightened stellar activity that is typical for low-mass stars. We present new simulations of in-situ planet formation across the Mdwarf mass spectrum, and derive leftover debris populations of small bodies that might source delayed volatile delivery. We then follow the evolution of this debris with high-resolution models of real systems of habitable zone planets around low-mass stars such as TRAPPIST-1, Proxima Centauri and TOI-700. While debris in the radial vicinity of the habitable zone planets is removed rapidly, thus making delayed volatile delivery highly unlikely, we find that material ubiquitously scattered into an exo-asteroid belt region during the planet formation process represents a potentially lucrative reservoir of icy small bodies. Thus, the presence of external ∼Neptune-Saturn mass planets capable of dynamically perturbing these asteroids would be a sign that habitable zone worlds around low-mass stars might have avoided complete desiccation. However, we also find that such giant planets significantly limit the efficiency of asteroidal implantation during the planet formation process. In the coming decade, long-baseline radial velocity studies and Roman Space Telescope microlensing observations will undoubtedly further constrain this process.

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Global analysis of the TRAPPIST Ultra-Cool Dwarf Transit Survey

Cited by 24 publications

References 75 publications

Planet Hunters TESS III: two transiting planets around the bright G dwarf HD 152843

Planet Hunters TESS III: two transiting planets around the bright G dwarf HD 152843

LRG-BEASTS: sodium absorption and Rayleigh scattering in the atmosphere of WASP-94A b using NTT/EFOSC2

Habitable planet formation around low-mass stars: Rapid accretion, rapid debris removal and the essential contribution of external giants

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