TESS unveils the phase curve of WASP-33b

Essen, C. von; Mallonn, M.; Borre, Camilla C.; Antoci, V.; Stassun, Keivan G.; Khalafinejad, S.; Tautvaišienė, G.

doi:10.1051/0004-6361/202037905

Cited by 53 publications

(55 citation statements)

References 92 publications

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“…To produce a S/N peak in this range, our model tends to favor the presence of TiO on the night hemisphere or close to the terminator regions. However, the nightside atmosphere has a significantly lower average temperature than the dayside (von Essen et al 2020). Hence, the nightside atmosphere is unlikely to possess a temperature inversion and we do not expect that the TiO emission originates from the nightside hemisphere.…”

Section: Tio Depleted Hot Spot Regionmentioning

confidence: 91%

“…General circulation models predict a confined region with enhanced temperature, namely the hot spot, as a general feature in UHJ atmospheres (e.g., Komacek et al 2017;Parmentier et al 2018;Arcangeli et al 2019). With an average dayside temperature of T day ∼ 3000 K (Zhang et al 2018;von Essen et al 2020), TiO is expected to be largely dissociated in the hot spot region. Consequently, the molecule will be more concentrated toward the terminator region of the planet.…”

Section: Tio Depleted Hot Spot Regionmentioning

confidence: 99%

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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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Section: Tio Depleted Hot Spot Regionmentioning

confidence: 91%

Section: Tio Depleted Hot Spot Regionmentioning

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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“…A&A proofs: manuscript no. W33-Ha dition to the thermal emission spectra, phase curve observations have been performed for several UHJs, including WASP-33b (Zhang et al 2018;von Essen et al 2020), WASP-121b (Daylan et al 2019;Bourrier et al 2020b), and KELT-9b (Wong et al 2020;Mansfield et al 2020). These observations suggest that these UHJs have relatively low day-night temperature contrasts and relatively high heat transport efficiencies.…”

Section: Introductionmentioning

confidence: 99%

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

Yan

Wyttenbach

Casasayas-Barris

et al. 2020

A&A

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Ultra-hot Jupiters (UHJs) are highly irradiated giant exoplanets with extremely high day-side temperatures, which lead to thermal dissociation of most of the molecular species. It is expected that the neutral hydrogen atom is one of the main species in the upper atmospheres of ultra-hot Jupiters. Neutral hydrogen has been detected in several UHJs by observing its Balmer line absorption. Here, we report four transit observations of the ultra-hot Jupiter WASP-33b, performed with the CARMENES and HARPS-North spectrographs, and the detection of the Hα, Hβ, and Hγ lines in the planetary transmission spectrum. The combined Hα transmission spectrum of the four transits has an absorption depth of 0.99±0.05 %, which corresponds to an effective radius of 1.31±0.01 R p. The strong Hα absorption indicates that the line probes the high-altitude thermosphere. We further fitted the three Balmer lines using the PAWN model, assuming that the atmosphere is hydrodynamic and in LTE. We retrieved a thermosphere temperature 12200 +1300 −1000 K and a mass-loss rateṀ = 10 11.8 +0.6 −0.5 g s −1. The retrieved large mass-loss rate is compatible with the "Balmer-driven" atmospheric escape scenario, in which the stellar Balmer continua radiation in the near-ultraviolet is substantially absorbed by the excited hydrogen atoms in the planetary thermosphere.

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“…Though many of these planets have had their phase curves observed in the near-infrared (NIR), until recently, there were only 15 hot Jupiters around bright stars with optical phase-curve data-all from Kepler (Angerhausen et al 2015;Esteves et al 2015). The TESS mission has dramatically changed this picture, and there are now 13 additional systems with published results (Shporer et al 2019;Bourrier et al 2020;von Essen et al 2020;Wong et al 2020aWong et al , 2020cWong et al , 2020d, with many more on the way as TESS completes its 2 yr primary mission.…”

Section: Introductionmentioning

confidence: 99%

The TESS Phase Curve of KELT-1b Suggests a High Dayside Albedo

Beatty

Wong

Fetherolf

et al. 2020

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We measured the optical phase curve of the transiting brown dwarf KELT-1b (TOI 1476) using data from the TESS spacecraft. We found that KELT-1b shows significant phase variation in the TESS bandpass, with a relatively large phase amplitude of -+ 234 44 43 ppm and a secondary eclipse depth of -+371 49 47 ppm. We also measured a marginal eastward offset in the dayside hot spot of 18°.3±7°. 4 relative to the substellar point. We detected a strong phase-curve signal attributed to ellipsoidal distortion of the host star with an amplitude of 399±19 ppm. Our results are roughly consistent with the Spitzer phase curves of KELT-1b, but the TESS eclipse depth is deeper than expected. Our cloud-free 1D models of KELT-1b's dayside emission are unable to fit the full combined eclipse spectrum. Instead, the large TESS eclipse depth suggests that KELT-1b may have a significant dayside geometric albedo of A g ∼0.5 in the TESS bandpass, which would agree with the tentative trend between equilibrium temperature and geometric albedo recently suggested by Wong et al. We posit that if KELT-1b has a high dayside albedo, it is likely due to silicate clouds that form on KELT-1b's nightside and are subsequently transported onto the western side of KELT-1b's dayside hemisphere before breaking up.

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TESS unveils the phase curve of WASP-33b

Cited by 53 publications

References 92 publications

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

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

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

The TESS Phase Curve of KELT-1b Suggests a High Dayside Albedo

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