RT Journal Article
T1 Atmospheric characterization of the ultra-hot Jupiter WASP-33b Detection of Ti and V emission lines and retrieval of a broadened line profile
A1 Cont, David
A1 Montes Gutiérrez, David
A1 Sánchez López, Alejandro
AB Ultra-hot Jupiters are highly irradiated gas giant exoplanets on close-in orbits around their host stars. The dayside atmospheres of these objects strongly emit thermal radiation due to their elevated temperatures, making them prime targets for characterization by emission spectroscopy. We analyzed high-resolution spectra from CARMENES, HARPS-N, and ESPaDOnS taken over eight observation nights to study the emission spectrum of WASP-33b and draw conclusions about its atmosphere. By applying the cross-correlation technique, we detected the spectral signatures of Ti I, V I, and a tentative signal of Ti II for the first time via emission spectroscopy. These detections are an important finding because of the fundamental role of Ti- and V-bearing species in the planetary energy balance. Moreover, we assessed and confirm the presence of OH, Fe I, and Si I from previous studies. The spectral lines are all detected in emission, which unambiguously proves the presence of an inverted temperature profile in the planetary atmosphere. By performing retrievals on the emission lines of all the detected species, we determined a relatively weak atmospheric thermal inversion extending from approximately 3400 to 4000 K. We infer a supersolar metallicity close to 1.5 dex in the planetary atmosphere, and find that its emission signature undergoes significant line broadening with a Gaussian full width at half maximum of about 4.5 km s^(−1) . Also, we find that the atmospheric temperature profile retrieved at orbital phases far from the secondary eclipse is about 300 to 700 K cooler than that measured close to the secondary eclipse, which is consistent with different day- and nightside temperatures. Moreover, retrievals performed on the emission lines of the individual chemical species lead to consistent results, which gives additional confidence to our retrieval method. Increasing the number of species included in the retrieval and expanding the set of retrieved atmospheric parameters will further advance our understanding of exoplanet atmospheres.
PB EDP Sciencies
SN 0004-6361
YR 2022
FD 2022
LK https://hdl.handle.net/20.500.14352/73276
UL https://hdl.handle.net/20.500.14352/73276
LA eng
NO © D. Cont et al. 2022. Artículo firmado por 20 autores. The authors thank the referee for very useful comments and suggestions. CARMENES is an instrument at the Centro Astronómico Hispano en Andalucía (CAHA) at Calar Alto (Almería, Spain), operated jointly by the Junta de Andalucía and the Instituto de Astrofísica de Andalucía (CSIC). CARMENES was funded by the Max-Planck-Gesellschaft (MPG), the Consejo Superior de Investigaciones Científicas (CSIC), the Ministerio de Economía y Competitividad (MINECO) and the European Regional Development Fund (ERDF) through projects FICTS-2011-02, ICTS-2017-07-CAHA-4, and CAHA16-CE-3978, and the members of the CARMENES Consortium (Max-Planck-Institut für Astronomie, Instituto de Astrofísica de Andalucía, Landessternwarte Königstuhl, Institut de Ciències de l’Espai, Institut für Astrophysik Göttingen, Universidad Complutense de Madrid, Thüringer Landessternwarte Tautenburg, Instituto de Astrofísica de Canarias, Hamburger Sternwarte, Centro de Astrobiología and Centro Astronómico Hispano-Alemán), with additional contributions by the MINECO, the Deutsche Forschungsgemeinschaft (DFG) through the Major Research Instrumentation Programme and Research Unit FOR2544 “Blue Planets around Red Stars”, the Klaus Tschira Stiftung, the states of Baden-Württemberg and Niedersachsen, and by the Junta de Andalucía. We acknowledge financial support from the DFG through Research Unit FOR2544 “Blue Planets around Red Stars” (RE 1664/21-1); the Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación and the ERDF “A way of making Europe” through projects PID2019-109522GB-C5[1:4], PID2019- 110689RB-I00, and the Centre of Excellence “Severo Ochoa” and “María de Maeztu” awards to the Instituto de Astrofísica de Canarias (CEX2019-000920-S), Instituto de Astrofísica de Andalucía (SEV-2017-0709), and Centro de Astrobiología (MDM-2017-0737); the European Research Council under the European Union’s Horizon 2020 research and innovation program under grant agreements Nos. 832428-Origins and 694513, and under the Marie Skłodowska-Curie grant agreement No. 895525; and the Generalitat de Catalunya/CERCA programme.
NO Max-Planck-Gesellschaft (MPG)
NO Consejo Superior de Investigaciones Científicas (CSIC)
NO Ministerio de Economía y Competitividad (MINECO)
NO European Regional Development Fund (ERDF)
NO Max-Planck-Institut für Astronomie
NO Instituto de Astrofísica de Andalucía
NO Landessternwarte Königstuhl
NO Institut de Ciències de l’Espai
NO Institut für Astrophysik Göttingen
NO Universidad Complutense de Madrid (UCM)
NO Thüringer Landessternwarte Tautenburg
NO Instituto de Astrofísica de Canarias
NO Hamburger Sternwarte
NO Centro de Astrobiología
NO Deutsche Forschungsgemeinschaft (DFG) through the Major Research Instrumentation Programme and Research Unit FOR2544 “Blue Planets around Red Stars”
NO Klaus Tschira Stiftung
NO States of Baden-Württemberg and Niedersachsen
NO Junta de Andalucía
NO Agencia Estatal de Investigación of the Ministerio de Ciencia e Innovación
NO ERDF “A way of making Europe”
NO Centre of Excellence “Severo Ochoa” and “María de Maeztu” awards to the Instituto de Astrofísica de Canarias
NO Instituto de Astrofísica de Andalucía
NO Centro de Astrobiología
NO European Research Council under the European Union’s Horizon 2020
NO Marie Skłodowska-Curie
NO Generalitat de Catalunya/CERCA
NO Centro Astronómico Hispano-Alemán
DS Docta Complutense
RD 13 may 2025