Detection of the hydrogen Balmer lines in the ultra-hot Jupiter WASP-33b

Yan, F.; Wyttenbach, A.; Casasayas-Barris, N.; Reiners, A.; Πάλλη, Ε.; Henning, Th.; Mollière, P.; Czesla, S.; Nortmann, L.; Molaverdikhani, Karan; Chen, G.; Snellen, I. A. G.; Zechmeister, M.; Huang, Chenliang; Ribas, I.; Quirrenbach, A.; Caballero, J. A.; Amado, P. J.; Cont, D.; Khalafinejad, S.; Khaimova, J.; López‐Puertas, M.; Montes, D.; Nagel, E.; Oshagh, M.; Pedraz, S.; Stangret, M.

doi:10.1051/0004-6361/202039302

Cited by 43 publications

(60 citation statements)

References 91 publications

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“…D.1). To avoid detecting a Fe signal (Fe is present in the atmosphere of WASP-33b and KELT-20b; Nugroho et al 2020a;Cont et al 2021;Yan et al 2021b), the wavelength solution of the Fe model spectrum was shifted by a constant value of 500 Å. By shifting the wavelength axis, the Fe lines are no longer located at the right position.…”

Section: Appendix A: Parameters Of Planetary Systemsmentioning

confidence: 99%

“…The spectral features of Ca ii, Fe i, OH, TiO, and the hydrogen Balmer lines have been found at high spectral resolution (Nugroho et al 2017(Nugroho et al , 2020a(Nugroho et al , 2021Yan et al 2019Yan et al , 2021bCauley et al 2021;Borsa et al 2021b;Cont et al 2021), and AlO and FeH were tentatively detected (von Essen et al 2019;Kesseli et al 2020). KELT-20b/MASCARA-2b (Lund et al 2017;Talens et al 2018) is a UHJ with T eq ∼ 2300 K that orbits an A-type star without pulsations.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Appendix A: Parameters Of Planetary Systemsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Silicon in the dayside atmospheres of two ultra-hot Jupiters

Cont

Yan

Reiners

et al. 2022

A&A

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“…Recently, atomic hydrogen was found in the transmission spectra of UHJs (e.g., Yan & Henning 2018;Casasayas-Barris et al 2018;Jensen et al 2018;Cauley et al 2021;Yan et al 2021). Moreover, metals such as Fe, Mg, Na, Ca, Ti, or V and their ions were detected via transmission spectroscopy in the atmospheres of KELT-9b, KELT-20b, WASP-121b, WASP-12b, and WASP-33b (e.g., Fossati et al 2010;Hoeijmakers et al 2018;Casasayas-Barris et al 2019;Hoeijmakers et al 2019;Cauley et al 2019;Sing et al 2019;Yan et al 2019;Stangret et al 2020;Nugroho et al 2020b;Gibson et al 2020;Ben-Yami et al 2020;Hoeijmakers et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Detection of Fe and evidence for TiO in the dayside emission spectrum of WASP-33b

Cont

Yan

Reiners

et al. 2021

A&A

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Context. Theoretical studies predict the presence of thermal inversions in the atmosphere of highly irradiated gas giant planets. Recent observations have identified these inversion layers. However, the role of different chemical species in their formation remains unclear. Aims. We search for the signature of the thermal inversion agents TiO and Fe in the dayside emission spectrum of the ultra-hot Jupiter WASP-33b. Methods. The spectra were obtained with CARMENES and HARPS-N, covering different wavelength ranges. Telluric and stellar absorption lines were removed with SYSREM. We cross-correlated the residual spectra with model spectra to retrieve the signals from the planetary atmosphere. Results. We find evidence for TiO at a significance of 4.9σ with CARMENES. The strength of the TiO signal drops close to the secondary eclipse. No TiO signal is found with HARPS-N. An injection-recovery test suggests that the TiO signal is below the detection level at the wavelengths covered by HARPS-N. The emission signature of Fe is detected with both instruments at significance levels of 5.7σ and 4.5σ, respectively. By combining all observations, we obtain a significance level of 7.3σ for Fe. We find the TiO signal at Kp = 248.0−2.5+2.0 km s−1, which is in disagreement with the Fe detection at Kp = 225.0−3.5+4.0 km s−1. The Kp value for Fe is in agreement with prior investigations. The model spectra require different temperature profiles for TiO and Fe to match the observations. We observe a broader line profile for Fe than for TiO. Conclusions. Our results confirm the existence of a temperature inversion layer in the planetary atmosphere. The observed Kp offset and different strengths of broadening in the line profiles suggest the existence of a TiO-depleted hot spot in the planetary atmosphere.

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“…This includes the possible contributions of stellar activity (Rackham et al 2018;Cauley et al 2018;Salz et al 2018), stellar center-to-limb variations (CLVs) and the planet's Doppler shadow (Czesla et al 2015;Yan et al 2015Yan et al , 2017, stellar pulsations (Yan et al 2021;Cauley et al 2021), and changes in the transit chord due to orbital precession (Herman et al 2018;Johnson et al 2018;Watanabe et al 2020;Szabó et al 2020). For high-resolution transmission spectra these effects can alter the observed line profile morphologies, as well as the shape of light curves for individual atomic absorption lines.…”

Section: Introductionmentioning

confidence: 99%

“…Recently, a number of ultra-hot gas giants transiting rapidly rotating A-type stars have been the focus of de-tailed transmission spectroscopy campaigns due to their novel atmospheric chemistry and high signal-to-noise absorption signatures (Yan & Henning 2018;Hoeijmakers et al 2019;Cauley et al 2019;Casasayas-Barris et al 2019;Nugroho et al 2020;Hoeijmakers et al 2020;Stangret et al 2020;Rainer et al 2021;Yan et al 2021;Cauley et al 2021;Bello-Arufe et al 2021). Given the intense interest in these systems, and the likely discovery of more such objects in the TESS data, it is important to understand the magnitude and details of how gravity darkening can affect the observed transmission spectrum.…”

Section: Introductionmentioning

confidence: 99%

The Effects of Stellar Activity on Optical High-resolution Exoplanet Transmission Spectra

Cauley

Kuckein

Redfield

et al. 2018

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Chromospherically sensitive atomic lines display different spectra in stellar active regions, spots, and the photosphere, raising the possibility that exoplanet transmission spectra are contaminated by the contrast between various portions of the stellar disk. To explore this effect, we performed transit simulations of G and K-type stars for the spectral lines Ca II K at 3933Å, Na I 5890Å, H I 6563 A (Hα), and He I 10830Å. We find that strong facular emission and large coverage fractions can contribute a non-negligible amount to transmission spectra, especially for Hα, Ca II K, and Na I D, while spots and filaments are comparatively unimportant. The amount of contamination depends strongly on the location of the active regions and the intrinsic emission strength. In particular, active regions must be concentrated along the transit chord in order to produce a consistent in-transit signal. Mean absorption signatures in Na I and Hα for example, can reach ≈ 0.2% and 0.3%, respectively, for transits of active latitudes with line emission similar in strength to moderate solar flares. Transmission spectra of planets transiting active stars, such as HD 189733, are likely contaminated by the contrast effect, although the tight constraints on active region geometry and emission strength make it unlikely that consistent in-transit signatures are due entirely to the contrast effect. He I 10830Å is not strongly affected and absorption signatures are likely diluted, rather than enhanced, by stellar activity. He I 10830Å should thus be considered a priority for probing extended atmospheres, even in the case of active stars.

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Detection of the hydrogen Balmer lines in the ultra-hot Jupiter WASP-33b

Cited by 43 publications

References 91 publications

Silicon in the dayside atmospheres of two ultra-hot Jupiters

Silicon in the dayside atmospheres of two ultra-hot Jupiters

Detection of Fe and evidence for TiO in the dayside emission spectrum of WASP-33b

The Effects of Stellar Activity on Optical High-resolution Exoplanet Transmission Spectra

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