Transmission spectroscopy of the ultra-hot Jupiter MASCARA-4 b

Zhang, Yapeng; Snellen, I. A. G.; Wyttenbach, A.; Nielsen, L. D.; Lendl, M.; Casasayas-Barris, N.; Chaverot, Guillaume; Kesseli, Aurora Y.; Pepe, F.; Psaridi, Angelica; Seidel, J. V.; Udry, S.; Ulmer-Moll, S.

doi:10.1051/0004-6361/202244203

Cited by 15 publications

(23 citation statements)

References 110 publications

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“…The simulations ran for a total of 2000 plane-tary days. Our GCM assumes hydrostatic equilibrium, which is a valid assumption for the opacity sources included in the high-resolution spectra we calculate from these models (Zhang et al 2022).…”

Section: Gcmmentioning

confidence: 99%

Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b

Beltz

Rauscher

Kempton

et al. 2022

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Ultrahot Jupiters are ideal candidates to explore with high-resolution emission spectra. Detailed theoretical studies are necessary to investigate the range of spectra that we can expect to see from these objects throughout their orbit, because of the extreme temperature and chemical longitudinal gradients that exist across their dayside and nightside regions. Using previously published 3D general circulation models of WASP-76b with different treatments of magnetic drag, we postprocess the 3D atmospheres to generate high-resolution emission spectra for two wavelength ranges, throughout the planet’s orbit. We find that the high-resolution emission spectra vary strongly as a function of phase, at times showing emission features, absorption features, or both, which are a direct result of the 3D structure of the planet. At phases exhibiting both emission and absorption features, the Doppler shift differs in direction between the two spectral features, making them differentiable, instead of canceling each other out. Through the use of cross correlation, we find different patterns in net Doppler shift for models with different treatments of drag: the nightside spectra show opposite signs in their Doppler shift, while the dayside phases display a reversal in the trend of net shift with phase. Finally, we caution researchers against using a single spectral template throughout the planet’s orbit; this can bias the corresponding net Doppler shift returned, as it can pick up on a bright region on the edge of the planet disk that is highly redshifted or blueshifted.

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Section: Gcmmentioning

confidence: 99%

Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b

Beltz

Rauscher

Kempton

et al. 2022

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“…Day-to-night wind flow in KELT-9b was also reported by Pai and Bello-Arufe et al (2022) based on the Doppler shift of Fe ii lines seen in transmission compared to the stellar systemic velocity. While Fe i traces gas motions in the gravitationally bound part of the atmosphere of a planet, Fe ii is likely tracing the dynamics of the evaporating exosphere (Zhang et al 2022). Therefore, a full analysis combining highspectral-resolution phase curves and transmission spectroscopy of UHJs has the potential to illuminate the physical processes leading to mass loss in this class of exoplanets.…”

Section: Implications For Wind Dynamics Measured In Transmission Spec...mentioning

confidence: 99%

The GAPS Programme at TNG

Pino

Brogi

Désert

et al. 2022

A&A

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Aims. We present a novel method for studying the thermal emission of exoplanets as a function of orbital phase at very high spectral resolution, and use it to investigate the climate of the ultra-hot Jupiter KELT-9b. Methods. We combine three nights of HARPS-N and two nights of CARMENES optical spectra, covering orbital phases between quadratures (0.25 < ϕ < 0.75), when the planet shows its day-side hemisphere with different geometries. We co-add the signal of thousands of Fe i lines through cross-correlation, which we map to a likelihood function. We investigate the phase-dependence of two separate observable quantities, namely (i) the line depths of Fe i and (ii) their Doppler shifts, introducing a new method that exploits the very high spectral resolution of our observations. Results. We confirm a previous detection of Fe i emission, and demonstrate a precision of 0.5 km s −1 on the orbital properties of KELT-9b when combining all nights of observations. By studying the phase-resolved Doppler shift of Fe i lines, we detect an anomaly in the planet's orbital radial velocity well-fitted with a slightly eccentric orbital solution (e = 0.016 ± 0.003, ω = 150 +13 • −11 , 5σ preference). However, we argue that this anomaly is caused by atmospheric circulation patterns, and can be explained if neutral iron gas is advected by day-to-night atmospheric wind flows of the order of a few km s −1 . We additionally show that the Fe i emission line depths are symmetric around the substellar point within 10 • (2σ), possibly indicating the lack of a large hot-spot offset at the altitude probed by neutral iron emission lines. Finally, we do not obtain a significant preference for models with a strong phase-dependence of the Fe i emission line strength. We show that these results are qualitatively compatible with predictions from general circulation models (GCMs) for ultra-hot Jupiter planets. Conclusions. Very high-resolution spectroscopy phase curves are of sufficient sensitivity to reveal a phase dependence in both the line depths and their Doppler shifts throughout the orbit. They constitute an under-exploited treasure trove of information that is highly complementary to space-based phase curves obtained with HST and JWST, and open a new window onto the still poorly understood climate and atmospheric structure of the hottest planets known to date.

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“…3.2.1. Template Spectra Zhang et al (2022) reported excess absorption by Hα, Hβ, Na I D1&D2, and Ca II H&K, and strong lines of Mg, Fe, and Fe+, and detected the species Mg, Ca, Cr, Fe, and Fe+ using the cross-correlation technique. Given its high equilibrium temperature, we suspected that this planet might also bear heavier species, as found in the atmospheres KELT-9 b, WASP-121 b and WASP-76 b (Hoeijmakers et al 2019;Azevedo Silva et al 2022).…”

Section: Survey Of Atoms and Molecules Using The Crosscorrelation Tec...mentioning

confidence: 99%

“…MASCARA-4 b is an UHJ with a mass of 1.675 ± 0.241 M Jup , a radius of 1.515 ± 0.044 R Jup , and an equilibrium temperature T eq of 2250 ± 62 K with an orbital period of ∼2.82406 days (Dorval et al 2020;Zhang et al 2022). Thus, it is an ideal target for atmospheric characterization given its large atmospheric scale heights and TSM (Kempton et al 2018).…”

Section: Introductionmentioning

confidence: 99%

“…Thus, it is an ideal target for atmospheric characterization given its large atmospheric scale heights and TSM (Kempton et al 2018). Recently, Zhang et al (2022) explored the chemical species in the atmosphere of this planet using the Echelle Spectrograph for Rocky Exoplanets and Stable Spectroscopic Observations (ESPRESSO; Pepe et al 2021) mounted on the Very Large Telescope (VLT), and they resolved excess absorption about Hα, Hβ, Na I D1&D2, and Ca II H&K, and detected Mg, Ca, Cr, Fe, and Fe+ by the cross-correlation analysis.…”

Section: Introductionmentioning

confidence: 99%

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Detection of Rubidium and Samarium in the Atmosphere of the Ultrahot Jupiter MASCARA-4b

Jiang

Wang

Zhao

et al. 2023

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Ultrahot Jupiters (UHJs) possess the most extreme environments among various types of exoplanets, making them ideal laboratories to study the chemical composition and kinetics properties of exoplanet atmosphere with high-resolution spectroscopy. It has the advantage of resolving the tiny Doppler shift and weak signal from exoplanet atmosphere and has helped to detect dozens of heavy elements in UHJs including KELT-9b, WASP-76b, and WASP-121b. MASCARA-4b is a 2.8 days UHJ with an equilibrium temperature of ∼2250 K, which is expected to contain heavy elements detectable with the Very Large Telescope (VLT). In this letter, we present a survey of atoms/ions in the atmosphere of the MASCARA-4b, using the two VLT/ESPRESSO transits data. Cross-correlation analyses are performed on the obtained transmission spectra at each exposure with the template spectra generated by petitRADTRANS for atoms/ions from element Li to U. We confirm the previous detection of Mg, Ca, Cr, and Fe, and report the detection of Rb, Sm, Ti+, and Ba+ with peak signal-to-noise ratios (S/Ns) > 5. We report a tentative detection of Sc+, with peak S/Ns ∼ 6 but deviating from the estimated position. The most interesting discovery is the first-time detection of elements Rb and Sm in an exoplanet. Rb is an alkaline element like Na and K, while Sm is the first lanthanide series element and is by far the heaviest one detected in exoplanets. Detailed modeling and acquiring more data are required to yield abundance ratios of the heavy elements and to understand better the common presence of them in UHJ’s atmospheres.

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Transmission spectroscopy of the ultra-hot Jupiter MASCARA-4 b

Cited by 15 publications

References 110 publications

Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b

Magnetic Drag and 3D Effects in Theoretical High-resolution Emission Spectra of Ultrahot Jupiters: the Case of WASP-76b

The GAPS Programme at TNG

Detection of Rubidium and Samarium in the Atmosphere of the Ultrahot Jupiter MASCARA-4b

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