The obliquity and atmosphere of the ultra-hot Jupiter TOI-1431b (MASCARA-5b): A misaligned orbit and no signs of atomic or molecular absorptions

M. Stangret*, E. Pallé, N. Casasayas-Barris, M. Oshagh, A. Bello-Arufe, R. Luque, V. Nascimbeni, F. Yan, J. Orell-Miquel, D. Sicilia, L. Malavolta, B. C. Addison, L. A. Buchhave, A. S. Bonomo, F. Borsa, S. H.C. Cabot, M. Cecconi, D. A. Fischer, A. Harutyunyan, J. M. MendonçaG. Nowak, H. Parviainen, A. Sozzetti, R. Tronsgaard

*Corresponding author for this work

Research output: Contribution to journalJournal articlepeer-review

Abstract

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.

Original languageEnglish
Article numberA73
JournalAstronomy and Astrophysics
Volume654
Number of pages13
ISSN0004-6361
DOIs
Publication statusPublished - 2021

Keywords

  • Planets and satellites: atmospheres
  • Planets and satellites: individual: MASCARA-5b
  • Planets and satellites: individual: TOI-1431b
  • Techniques: spectroscopic

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