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\title{NEW MEASUREMENTS OF H$_{2}$O BROADENED BY CO$_{2}$ LINE SHAPE PARAMETERS USING QUADRATIC SPEED-DEPENDENT VOIGT PROFILE}

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\author{\underline{\FirstName E. \LastName DUCREUX}$^{1,2,4}$, {\FirstName B. \LastName GROUIEZ}$^{1}$, {\FirstName L. \LastName R\'EGALIA}$^{1}$}
\address{$^{(1)}$Universit\'e de Reims Champagne-Ardenne, CNRS, GSMA, Reims, France}

\author{{\FirstName S. \LastName ROBERT}$^{2}$}
\address{$^{(2)}$Planetary Atmospheres, Royal Belgian Institute for Space Aeronomy, 3 Avenue Circulaire, 1180 Brussels, Belgium}

\author{{\FirstName R.R. \LastName GAMACHE}$^{3}$}
\address{$^{(3)}$Department of Environmental, Earth, and Atmospheric Sciences, University of Massachusetts Lowell, 1 University Avenue, Lowell, MA 01854, USA}

\author{{\FirstName M. \LastName LEP\`ERE}$^{4}$, {\FirstName B. \LastName VISPOEL}$^{4}$}
\address{$^{(4)}$Research Unit Lasers and Spectroscopies (LLS), Institute of Life, Earth and Environment (ILEE), University of Namur (UNamur), 61 rue de Bruxelles, Namur, B-5000, Belgium}

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% \author{{\FirstName L. \LastName RÉGALIA}}
% \address{Université de Reims Champagne-Ardenne, CNRS, GSMA UMR 7331, 51100 Reims}


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\fancyhead[C]{{\footnotesize \textit{HRMS, 28th Colloquium, Dijon, France,
  Aug. 28 - Sept. 1, 2023}}}
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\category {9}
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\index{High resolution infrared spectroscopy}
\index{Line shape parameters}
\index{Planetary atmospheres}
\index{Water vapor}
\index{Carbon dioxide}

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The main gas in the atmosphere of our closest planetary neighbors, Venus and Mars is CO$_{2}$. Since decades both planets have been regularly investigated by different probes and spacecrafts which carry a large amount of scientific instruments in constant improvement. Their accuracy is expected to be such that it is nowadays important to use the best line shape parameters to study their atmospheric spectra. 

A previous study was published in 2019\footnote{\href{https://doi.org/10.1016/j.jqsrt.2019.04.012}{doi:10.1016/j.jqsrt.2019.04.012}, L. R\'egalia, E. Cousin, R.R. Gamache, B. Vispoel, S. Robert and X. Thomas{\em , J. Quant. Spectrosc. Radiat. Transfer\/}, {\bf 231}, 126-135 (2019)} using a Voigt profile to measure the line parameters of water vapor in a CO$_{2}$-rich environment. In this work, we studied the influence of the line profile in the  determination of the line parameters. Hence, we recorded new spectra in Reims with our Bruker IFS125HR spectrometer combined with a 2-meters White cell at 2.7 $\mu$m. We analysed them using a multi-spectrum fitting procedure\footnote{\href{https://doi.org/10.1134/S102485601506010X}{doi:10.1134/S102485601506010X}, O.M. Lyulin{\em , Atmos Ocean Opt\/}, {\bf 28}, 487-495 (2015)} with Voigt and quadratic speed-dependent Voigt (qSDV)\footnote{\href{https://doi.org/10.1016/j.jqsrt.2013.05.034}{doi:10.1016/j.jqsrt.2013.05.034}, N.H. Ngo, D. Lisak, H. Tran and J.-M. Hartmann{\em , J. Quant. Spectrosc. Radiat. Transfer\/}, {\bf 129}, 89-100 (2013)}$^{,}$\footnote{\href{https://doi.org/10.1016/j.jqsrt.2013.06.015}{doi:10.1016/j.jqsrt.2013.06.015}, H. Tran, N.H. Ngo and J.-M. Hartmann{\em , J. Quant. Spectrosc. Radiat. Transfer\/}, {\bf 129}, 199-203 (2013)} profiles. The first gives us a characteristic w-shape residual, while the second profile can greatly reduce the residuals allowing more accurate line shape parameters, especially the CO$_{2}$ broadening and shift coefficients. The Voigt profile limits seem reached in our experiment as the speed dependence effects need to be taken into account.

Note that other spectral domains of atmospheric interest are being studied.

\vfill
Acknowledgments: This work was supported by the Programme National de Plan\'etologie (PNP) of CNRS-INSU co-funded by CNES. 

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