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\title{A SPECTROSCOPIC THERMOMETER: INDIVIDUAL VIBRATIONAL BAND SPECTROSCOPY WITH OH IN THE ATMOSPHERE OF WASP-33B}

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\author{\underline{\FirstName SERGEI N. \LastName YURCHENKO},
\underline{\FirstName J. \LastName TENNYSON},
\FirstName S. W.M. \LastName WRIGHT AND 
\FirstName  I. \LastName  WALDMANN}
\address{Department of Physics and Astronomy, University College London, Gower Street, WC1E 6BT London, United Kingdom}
\author{\FirstName M.  S. K. \LastName  NUGROHO}
\address{Astrobiology Center, NINS, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan}
\author{\FirstName M.  \LastName BROGI}
\address{Dipartimento di Fisica, Universit\`a degli Studi di Torino, via Pietro Giuria 1, I-10125, Torino, Italy}
\author{\FirstName N.P.  \LastName GIBSON}
\address{School of Physics, Trinity College Dublin, The University of Dublin, Dublin 2, Ireland}
\author{\FirstName E.J. W.  \LastName DE MOOIJ}
\address{Astrophysics Research Centre, Queen's University Belfast, Belfast BT7 1NN, UK}

 

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\fancyhead[C]{{\footnotesize \textit{HRMS, 28th Colloquium, Dijon, France,
  Aug. 28 - Sept. 1, 2023}}}
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Individual vibrational band spectroscopy presents an opportunity to examine exoplanet atmospheres in detail by distinguishing where the vibrational state populations of molecules differ from the current assumption of a Boltzmann distribution. Here, retrieving vibrational bands of OH in exoplanet atmospheres is explored using the hot Jupiter WASP-33b as an example.\footnote{S. O.M. Wright et al., \textit{Astron.}, In press (2023); \href{https://arxiv.org/abs/2305.11071}{arXiv:2305.11071}} We simulate low-resolution spectroscopic data for observations with the JWST's NIRSpec instrument and use high resolution observational data obtained from the Subaru InfraRed Doppler instrument (IRD). Vibrational band-specific OH cross section sets  are constructed and used in retrievals on the (simulated) low and (real) high resolution data. Low resolution observations are simulated for two  WASP-33b emission scenarios: under the assumption of local thermal equilibrium (LTE) and a toy non-LTE model for vibrational excitation of selected bands.\footnote{Sam O M Wright, Ingo Waldmann, and Sergei N Yurchenko, \href{http://dx.doi.org/10.1093/mnras/stac654}{Non-local thermal equilibrium spectra of atmospheric molecules for exoplanets}, \textit{Mon. Notices Royal Astron. Soc.}, \textbf{512}, 2911 (2022)}

We show that mixing ratios for individual bands can be retrieved with sufficient precision to allow the vibrational population distributions of the forward models to be reconstructed.  For high resolution, cross-correlation applications, we apply the individual vibrational band analysis to an IRD  spectrum of WASP-33b,\footnote{\href{http://dx.doi.org/10.3847/2041-8213/abec71}{S.K. Nugroho et al.}, \textit{Astrophys. J. Lett.}, \textbf{910}, L9 (2021)} applying an `un-peeling' technique. Individual detection significances for the two strongest bands are shown to be in line with Boltzmann distributed vibrational state populations consistent with the effective temperature of the WASP-33b atmosphere reported previously. We show the viability of this approach for analysing  the individual vibrational state populations behind observed and simulated spectra including reconstructing state population distributions.

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