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\markboth{R.\ Trampedach}{Opacity Wish List}

\begin{document}

\title{A Modelers Opacity Wish List}
\author{Regner Trampedach$^{1,2,3}$
\affil{$^1$Space Science Institute, 4750 Walnut Street, Suite 205,
          Boulder, CO 80301 USA; \email{rtrampedach@SpaceScience.org}}
\affil{$^2$Stellar Astrophysics Centre, Dept.\ of Physics and Astronomy,
          Ny Munkegade 120, Aarhus University, DK--8000 Aarhus C, Denmark}
\affil{$^3$Laboratory for Atmospheric and Space Physics, University of Colorado Boulder, Boulder, USA}}

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\paperauthor{Regner Trampedach}{rtrampedach@SpaceScience.org}{}{Space Science Institute}{}{Boulder}{CO}{80301}{USA}

\begin{abstract}
At the Aug.\ 1--4, 2017 Workshop on Astrophysical Opacities, several attendees
voiced their interest in a list of absorption data, that are missing from or
inadequate in current models of astrophysical objects. This is a wish list
by modelers, meant as motivation and inspiration for experimentalists and
theoreticians alike.
\end{abstract}

\section{The Wish List}
Table \ref{TheTable} is the opacity wish list as I have compiled from the
responses I have received from both the workshop attendees and from several
1D and 3D stellar atmosphere groups. The first column lists the absorber
system, the second column lists the absorption mechanism: Rotational,
vibrational and electronic transitions in molecules, bound-bound (bb) and
bound-free (bf) electronic transitions in atoms/ions, and collision induced
absorption (CiA) from transient dipoles by pairs of passing particles. The
third and fourth columns list the requests for laboratory experiment and/or
theoretical calculations, and the last column lists the kind of objects for
which modeling will improve with updated atomic/molecular physics.



\begin{table}[!ht]
\caption{The opacity wish list.\label{TheTable}}
\smallskip
\begin{center}
\begin{minipage}{\textwidth}
\setlength{\footnotesep}{10pt}%  default = 14.14023pt
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{\small
\begin{tabular}{llccl}
\tableline
\noalign{\smallskip}
 Absorber           & Mechanism & Exp.& Calc.& For objects \\
\noalign{\smallskip}
\tableline
\noalign{\smallskip}
CH$_2$, C$_3$H      & Rot+vib+e &  X  &   X  & Cool star/C-star atm.       \\
CaOH, LaO, YO       & Rot+vib+e &  X  &   X  & Cool dwarf atm.             \\
~~ScO, TiS, ZrS     &                \multicolumn{4}{c}{---~|~|~---}       \\
%C$_2$H$_2$\footnote{Need higher vib-rot states, compared to {\protect\citet{SCAN-97}}.}
%                    & Rot+vib   &     &   X  & C-star atm.                 \\
%C$_3$\footnote{Need broader NIR features, compared to {\protect\citet{jorgensen:C3bands}}.}
%                    & Rot+vib   &     &   X  & C-star atm.                 \\
C$_2$H\footnote{No data are currently available for C$_2$H.}
                    & Rot+vib   &     &   X  & C-star atm.                 \\
N$_2$-H$_2$, N$_2$-He, N$_2$-Ne & CiA & & X  & M-dwarf atm.                \\
~~N$_2$-N$_2$, H$_2$-Ne         &    \multicolumn{4}{c}{---~|~|~---}       \\
H-H\footnote{This is a request for an update of the old \citet{doyle:H+H}
  result, and to match it to the red end of \citet{allard:NewQuasi-H2-Lya}'s
  Ly$\alpha$ satellites from {H-H} collisions.}
                    & CiA       &     &   X  & Cool dwarf atm.             \\
%HCN/HNC, NH$_3$     & Rot+vib   &  X  &   X  & 500--3000\,K plt/dwarf atm. \\
O, Fe-peak, Zn, Pb\footnote{Completeness is important for non-LTE calculations. Neutral atoms have highest priority.}
                    & bb, bf    &  X  &   X  & Stars in general \\
\noalign{\smallskip}
\tableline\
\end{tabular}
}
\end{minipage}
\end{center}
\end{table}

\subsection{Some Recent and Pending Calculations}

A new high-temperature (up to 1\,500\,K) line-list for acetylene (HCCH or
C$_2$H$_2$) has been published by \citet{lyulin:HiT-C2H2lineparms}, with
several experimental spectra cited. \citet{chubb:C2H2ExpCompilation}
performed a critical compilation of measured spectra and derived rovibrational
parameters for acetylene.

Calculations of the collision-induced-absorption has been carried out by
\citet{karman:N2-N2-CiA} 50--330\,$\mu$m and \citet{hartmann:N2-N2-CiA} at
2.05--2.3\,$\mu$m, but only for room-temperature and below. Experimental
spectra are cited in both papers.

The ExoMol \citep[][and elsewhere in these proceedings]{yurchenko:ExoMol}
team is very productive, and has already addressed a great number of
requests from the community, notably HCN/HNC by \citet{barber:HCN-HNC};  NH$_3$
by \citet{yurchenko:NH3}, with updates expected early 2018. In addition, an
ExoMol calculation of C$_2$H$_2$ is slated to be published by the
first half of 2018, and C$_3$ should be completed later that year.

\noindent 
\acknowledgements RT acknowledges funding from NASA grant NNX15AB24G.
Funding for the Stellar Astrophysics Centre is provided by The Danish National
Research Foundation (Grant DNRF106).

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