Volume 654, October 2021
|Number of page(s)||13|
|Section||Planets and planetary systems|
|Published online||13 October 2021|
The obliquity and atmosphere of the ultra-hot Jupiter TOI-1431b (MASCARA-5b): A misaligned orbit and no signs of atomic or molecular absorptions
Instituto de Astrofísica de Canarias,
Vía Láctea s/n,
2 Departamento de Astrofísica, Universidad de La Laguna, 38200 San Cristobal de La Laguna, Spain
3 Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands
4 National Space Institute, Technical University of Denmark, Elektrovej, 2800 Kgs. Lyngby, Denmark
5 INAF – Osservatorio Astronomico di Padova, Vicolo dell’Osservatorio 5, 35122 Padova, Italy
6 Institut für Astrophysik, Georg-August-Universität, Friedrich-Hund-Platz 1, 37077 Göttingen, Germany
7 INAF – Osservatorio Astrofisico di Catania, Via Santa Sofia 78, 95123 Catania, Italy
8 Department of Physics and Astronomy, Università degli Studi di Padova, Vicolo dell’Osservatorio 3, 35122 Padova, Italy
9 University of Southern Queensland, Centre for Astrophysics, USQ Toowoomba, West Street, QLD 4350, Australia
10 INAF – Osservatorio Astrofisico di Torino, via Osservatorio 20, 10025 Pino Torinese, Italy
11 INAF – Osservatorio Astronomico di Brera, Via E. Bianchi 46, 23807 Merate, Italy
12 Yale University, 52 Hillhouse Avenue, New Haven, CT 06511, USA
13 Fundación Galileo Galilei - INAF, Rambla José Ana Fernandez Pérez 7, 38712 Breña Baja, TF, Spain
Accepted: 12 April 2021
Ultra-hot Jupiters are defined as giant planets with equilibrium temperatures larger than 2000 K. Most of them are found orbiting bright A-F type stars, making them extremely suitable objects to study their atmospheres using high-resolution spectroscopy. Recent studies show a variety of atoms and molecules detected in the atmospheres of this type of planets. Here we present our analysis of the newly discovered ultra-hot Jupiter TOI-1431 b/MASCARA-5 b, using two transit observations with the HARPS-N spectrograph and one transit observation with the EXPRES spectrograph. Analysis of the Rossiter-McLaughlin effect shows that the planet is in a polar orbit, with a projected obliquity λ = −155−10+20 degrees. Combining the nights and applying both cross-correlation methods and transmission spectroscopy, we find no evidences of Ca I, Fe I, Fe II, Mg I, Na I, V I, TiO, VO or Hα in the atmosphere of the planet. Our most likely explanation for the lack of atmospheric features is the large surface gravity of the planet.
Key words: planets and satellites: individual: TOI-1431b / planets and satellites: individual: MASCARA-5b / planets and satellites: atmospheres / techniques: spectroscopic
© ESO 2021
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