Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

Hoeijmakers, H. J.; Seidel, J. V.; Pino, L.; Kitzmann, Daniel; Sindel, Jan Philip; Ehrenreich, D.; Oza, A.; Bourrier, V.; Allart, R.; Gebek, Andrea; Lovis, C.; Yurchenko, Sergei N.; Astudillo-Defru, N.; Bayliss, Daniel; Cegla, H. M.; Lavie, B.; Lendl, M.; Melo, C.; Murgas, F.; Nascimbeni, V.; Pepe, F.; Ségransan, D.; Udry, S.; Wyttenbach, A.; Heng, Kevin

doi:10.1051/0004-6361/202038365

Cited by 152 publications

(159 citation statements)

References 108 publications

(46 reference statements)

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“…We also confirm the presence of Fe ii in the planetary atmosphere ( Fig. 17), which has been previously debated (Ben-Yami et al 2020;Hoeijmakers et al 2020). A net blueshift is present for all the detections.…”

Section: -supporting

confidence: 85%

Atmospheric Rossiter–McLaughlin effect and transmission spectroscopy of WASP-121b with ESPRESSO

Borsa

Allart

Casasayas-Barris

et al. 2020

A&A

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124

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Context. Ultra-hot Jupiters are excellent laboratories for the study of exoplanetary atmospheres. WASP-121b is one of the most studied; many recent analyses of its atmosphere report interesting features at different wavelength ranges. Aims. In this paper we analyze one transit of WASP-121b acquired with the high-resolution spectrograph ESPRESSO at VLT in one-telescope mode, and one partial transit taken during the commissioning of the instrument in four-telescope mode. Methods. We take advantage of the very high S/N data and of the extreme stability of the spectrograph to investigate the anomalous in-transit radial velocity curve and study the transmission spectrum of the planet. We pay particular attention to the removal of instrumental effects, and stellar and telluric contamination. The transmission spectrum is investigated through single-line absorption and cross-correlation with theoretical model templates. Results. By analyzing the in-transit radial velocities we were able to infer the presence of the atmospheric Rossiter-McLaughlin effect. We measured the height of the planetary atmospheric layer that correlates with the stellar mask (mainly Fe) to be 1.052±0.015 R p and we also confirmed the blueshift of the planetary atmosphere. By examining the planetary absorption signal on the stellar cross-correlation functions we confirmed the presence of a temporal variation of its blueshift during transit, which could be investigated spectrum-by-spectrum thanks to the quality of our ESPRESSO data. We detected significant absorption in the transmission spectrum for Na, H, K, Li, Ca ii, and Mg, and we certified their planetary nature by using the 2D tomographic technique. Particularly remarkable is the detection of Li, with a line contrast of ∼0.2% detected at the 6σ level. With the cross-correlation technique we confirmed the presence of Fe i, Fe ii, Cr i, and V i. Hα and Ca ii are present up to very high altitudes in the atmosphere (∼1.44 R p and ∼2 R p , respectively), and also extend beyond the transit-equivalent Roche lobe radius of the planet. These layers of the atmosphere have a large line broadening that is not compatible with being caused by the tidally locked rotation of the planet alone, and could arise from vertical winds or high-altitude jets in the evaporating atmosphere.

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Section: -supporting

confidence: 85%

Atmospheric Rossiter–McLaughlin effect and transmission spectroscopy of WASP-121b with ESPRESSO

Borsa

Allart

Casasayas-Barris

et al. 2020

A&A

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124

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“…Besides, the search for VO remains elusive at high spectral resolution (Merritt et al 2020). On the other hand, as various atoms and ions have been discovered in UHJs with an inverted atmosphere, atomic species have become promising candidates for causing and maintaining temperature inversions (Lothringer et al 2018;Hoeijmakers et al 2020b).…”

Section: Introductionmentioning

confidence: 99%

Silicon in the dayside atmospheres of two ultra-hot Jupiters

Cont

Yan

Reiners

et al. 2022

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Atmospheres of highly irradiated gas giant planets host a large variety of atomic and ionic species. Here we observe the thermal emission spectra of the two ultra-hot Jupiters WASP-33b and KELT-20b/MASCARA-2b in the near-infrared wavelength range with CARMENES. Via high-resolution Doppler spectroscopy, we searched for neutral silicon (Si) in their dayside atmospheres. We detect the Si spectral signature of both planets via cross-correlation with model spectra. Detection levels of 4.8σ and 5.4σ, respectively, are observed when assuming a solar atmospheric composition. This is the first detection of Si in exoplanet atmospheres. The presence of Si is an important finding due to its fundamental role in cloud formation and, hence, for the planetary energy balance. Since the spectral lines are detected in emission, our results also confirm the presence of an inverted temperature profile in the dayside atmospheres of both planets.

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“…The first CHEOPS science paper by Lendl et al (2020) presents WASP-189b with an global dayside temperature of ≈3400 K for a non-reflective atmosphere with inefficient heat redistribution. Also WASP-121b shows less extreme temperatures than KELT-9b such that the presence of neutral atoms such as Mg, Na, Ca, Cr, Fe, and also Ni and V have been inferred from observations of the terminator regions (Hoeijmakers et al 2020). However, Hoeijmakers et al (2020) did not detect Ti and TiO on WASP-121b which may be an indication for cloud-depleted Ti abundances at the cold evening terminator similar to WASP-18b or HAT-P-7b (Helling et al 2019a,b).…”

Section: Introductionmentioning

confidence: 99%

“…Also WASP-121b shows less extreme temperatures than KELT-9b such that the presence of neutral atoms such as Mg, Na, Ca, Cr, Fe, and also Ni and V have been inferred from observations of the terminator regions (Hoeijmakers et al 2020). However, Hoeijmakers et al (2020) did not detect Ti and TiO on WASP-121b which may be an indication for cloud-depleted Ti abundances at the cold evening terminator similar to WASP-18b or HAT-P-7b (Helling et al 2019a,b). Gibson et al (2020) detect Fe I in WASP-121b applying VLT/UVES transit observations.…”

Section: Introductionmentioning

confidence: 99%

Cloud property trends in hot and ultra-hot giant gas planets (WASP-43b, WASP-103b, WASP-121b, HAT-P-7b, and WASP-18b)

Helling

Lewis

Samra

et al. 2021

A&A

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Context. Ultra-hot Jupiters are the hottest exoplanets that have been discovered so far. Observations begin to provide insight into the composition of their extended atmospheres and their chemical day/night asymmetries. Both are strongly affected by cloud formation. Aims. We explore trends in cloud properties for a sample of five giant gas planets: the hot gas giant WASP-43b and the four ultra-hot Jupiters (UHJs) WASP-18b, HAT-P-7b, WASP-103b, and WASP-121b. This provides a reference frame for cloud properties for the JWST targets WASP-43b and WASP-121b. We further explore chemically inert tracers to observe geometrical asymmetries of UHJs and if the location of the inner boundary of a 3D global circulation model (3D GCM) matters for the clouds that form. Methods. A homogeneous set of 3D GCM results was used as input for a kinetic cloud formation code to evaluate the cloud opacity and gas parameters such as C/O, mean molecular weight, and degree of ionisation. We cast our results in terms of integrated quantities to enable a global comparison between the sample planets. Results. The large day/night temperature differences of UHJs cause the following chemical asymmetries: cloud-free days but cloudy nights, atomic versus molecular gases and their different mean molecular weights, deep thermal ionospheres versus low-ionised atmospheres, and undepleted versus enhanced C/O. WASP-18b, as the heaviest planet in the sample, has the lowest global C/O. Conclusions. The global climate may be considered as similar amongst UHJs, but different to that of hot gas giants. The local weather, however, is individual for each planet since the local thermodynamic conditions, and hence the local cloud and gas properties, differ. The morning and the evening terminator of UHJs will carry signatures of their strong chemical asymmetry such that ingress and egress asymmetries can be expected. An increased C/O ratio is a clear sign of cloud formation, making cloud modelling a necessity when utilising C/O (or other mineral ratios) as a tracer for planet formation. The changing geometrical extension of the atmosphere from the day to the nightside may be probed through chemically inert species such as helium. Ultra-hot Jupiters are likely to develop deep atmospheric ionospheres which may impact the atmosphere dynamics through magneto-hydrodynamic processes.

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Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS)

Cited by 152 publications

References 108 publications

Atmospheric Rossiter–McLaughlin effect and transmission spectroscopy of WASP-121b with ESPRESSO

Atmospheric Rossiter–McLaughlin effect and transmission spectroscopy of WASP-121b with ESPRESSO

Silicon in the dayside atmospheres of two ultra-hot Jupiters

Cloud property trends in hot and ultra-hot giant gas planets (WASP-43b, WASP-103b, WASP-121b, HAT-P-7b, and WASP-18b)

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