%%
%% Sample TeX file for the HRMS Dijon 2023 abstracts
%%
%% Lines (or parts of) beginning with at least one '%' are comments
%% and are silently ignored by LaTeX
%%
%% Codings beginning with \ are LaTeX macros, or commands.
%% They are used to tell the LaTeX parser how to format the document.
%% All the macros below are mandatory.
%%
%% Various informations about latex may be found at
%%
%%   http://en.wikibooks.org/wiki/LaTeX
%%
%% *-----------------------------------------------------------------------------------------*
\documentclass[11pt]{article}

\usepackage{hrms}  %% Page settings, style ... for the HRMS abstract book.

%% *-----------------------------------------------------------------------------------------*

\title{SEMICLASSICAL ESTIMATES OF PRESSURE-INDUCED LINE-WIDTHS FOR INFRARED ABSORPTION BY EXOMOLECULES}

%% Note that \author and \address macros must be paired.
%% The names of authors must also appear IN CAPITALS.
%% The name(s) of author(s) presenting the work is(are) usually underlined.

\author{\underline{\FirstName K. \LastName STEHLIN}$^*$,
  \underline{\FirstName J. \LastName BULDYREVA}$^*$,
  \underline{\FirstName S.N. \LastName YURCHENKO}$^{*,**}$,
  \underline{\FirstName J.~\LastName TENNYSON}$^{**}$}
\address{Institut UTINAM, UMR CNRS 6213, Universit\'{e} de Franche-Comt\'{e}, 16 route de Gray, 25030 Besan\c{c}on cedex, France ($^*$); Department of Physics and Astronomy, University College London, Gower Street, WC1E 6BT London, United Kingdom ($^{**}$)}

%% Place below other \usepackage{ ... }, if you need other packages.
%% See http://www.tug.org/texlive/doc.html for a description of available packages.

%% The macros below will change the page head and foot.
%% Please, do not modify the content of the \fancyhead macro nor the \fancyfoot line.
\usepackage{fancyhdr}
\pagestyle{fancy}
\fancyhead[C]{{\footnotesize \textit{HRMS, 28th Colloquium, Dijon, France,
  Aug. 28 - Sept. 1, 2023}}}
\fancyfoot[C]{}
\renewcommand{\headrulewidth}{0.6pt}
\renewcommand{\footrulewidth}{0.6pt}

%% The hyperref package allows to include hyperlinks in a document.
%% See the instructions for abstract submission for more details.
%% WARNING: Make sure that this package comes LAST since it re-defines many LaTeX macros.
\usepackage[colorlinks=true,urlcolor=blue,linkcolor=blue,citecolor=blue]{hyperref}
\voffset -.65 cm

%% *-----------------------------------------------------------------------------------------*

\category {8,1}
\begin{document}

\maketitle  %% This will also build the list of author(s) and addresse(s).

%% Index macro(s): see the abstract samples and the instructions
%% Remove the %% to account for the index item(s)
%% \index{Item1}
%% \index{Item2}

Molecules and molecular ions found or expected in exoplanetary atmospheres are generally poorly characterized from the viewpoint of their spectroscopic line-shape parameters; in many cases, there are no data at all. From the experimental point of view, this fact is due to elevated temperatures and high fluxes of stellar radiation irreproducible in laboratory conditions. From the theoretical point of view, potential energy surfaces for required molecular pairs are unavailable and advanced (computationally expensive) calculations can not be performed.

As account for and completeness of such data are crucial for reliable simulations of radiative transfer in the atmospheres of exoplanets [1],
we employ a simple semi-classical expression [2] to generate rotationally-independent estimates of pressure-broadened linewiths for (vib)rotational transitions. 
A wide range of absorbers and perturbation including He, Ar, H$_2$, N$_2$, O$_2$, CO, NO, CO$_2$, H$_2$O, CH$_4$, NH$_3$ and self-perturbation are considered. The leading long-range interaction term, molecular masses and kinetic diameters as well as temperature are used as input parameters, allowing   tables
% (see Figure)
of pressure-broadening coefficients $\gamma (T_{\rm ref})$ at the reference temperature $T_{\rm ref}$=296~K to be produced. Values  $\gamma (T)$ for other temperatures $T$ can be readily obtained using the power law $\gamma (T)=\gamma (T_{\rm ref}) (T_{\rm ref}/T)^{0.5}$. In some cases kinetic diameters were unavailable but Lennard-Jones parameters $\sigma$ could be found and were used instead. For most cases none of them were found, and the required kinetic diameters were estimated by a semi-empirical formula [3] from the molecular polarizabilities.

These theoretical estimates provide data on collision pairs which are so far completely missing in spectroscopic databases. They should prove useful for  remote sensing of exoplanetary atmospheres.

SY acknowledges the mobility grant provided by the Region Bourgogne-Franche-Comt\'e for his visit to
Besancon.
%\vspace{3mm}
%\centerline{\psfig{figure=Figure.eps,width=9cm}}
\vspace{0.5cm}\\
\begin{small}
\mbox{[1]}  J.J. Fortney et al., \href{https://arxiv.org/abs/1905.07064}{arXiv:1905.07064} (2019).\\
\mbox{[2]} J. Buldyreva et al., \textit{RASTI}, \textbf{1}, 43 (2022), \href{https://doi.org/10.1093/rasti/rzac004}{doi:10.1093/rasti/rzac004}.\\
\mbox{[3]} B.I. Loukhovitski and A.S. Sharipov, \textit{J. Phys. Chem. A}, \textbf{125}, 5117 (2021), \href{https://doi.org/10.1021/acs.jpca.1c02201}{doi:10.1021/acs.jpca.1c02201}.
\end{small}

\end{document}
