Journal
ASTRONOMY & ASTROPHYSICS
Volume 651, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/202140732
Keywords
planets and satellites: atmospheres; techniques: spectroscopic; planets and satellites: individual: WASP-33b
Categories
Funding
- Max-Planck-Gesellschaft (MPG)
- Consejo Superior de Investigaciones Cientificas (CSIC)
- Ministerio de Economia y Competitividad (MINECO)
- European Regional Development Fund (ERDF) [FICTS-2011-02, ICTS-2017-07-CAHA-4, CAHA16-CE-3978]
- Instituto de Astrofisica de Andalucia
- Deutsche Forschungsgemeinschaft through the Major Research Instrumentation Programme [FOR2544]
- Deutsche Forschungsgemeinschaft through the priority program [SPP 1992]
- Exploring the Diversity of Extrasolar Planets [RE 1664/16-1]
- Blue Planets around Red Stars [RE 1664/21-1]
- Agencia Estatal de Investigacion of the Ministerio de Ciencia, Innovacion y Universidades
- ERDF [PID2019-109522GB-C5[1:4]/AEI/, PID2019-110689RB-I00/AEI/]
- Centre of Excellence Severo Ochoa award [SEV-2015-0548]
- Centre of Excellence Maria de Maeztu award [SEV-2015-0548]
- Instituto de Astrofisica de Andalucia [SEV-2017-0709]
- Centro de Astrobiologia [MDM-2017-0737]
- European Research Council under the European Union's Horizon 2020 research and innovation program [832428]
- Generalitat de Catalunya/CERCA programme
- [CA 1795/3]
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The study identified characteristics of TiO and Fe in the dayside emission spectrum of the ultra-hot Jupiter WASP-33b, with the detection of Fe showing higher significance compared to TiO. The model spectra require different temperature profiles to match the observations.
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 4.9 sigma 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 5.7 sigma and 4.5 sigma, respectively. By combining all observations, we obtain a significance level of 7.3- for Fe. We find the TiO signal at Kp = 248:0+2:0 2:5 km s 1, which is in disagreement with the Fe detection at Kp = 225:0+4:0 3:5 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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