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\title{UPDATING THE CARBON DIOXIDE LINE LIST FOR THE HITEMP DATABASE}

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\author{\underline{\FirstName R.~J. \LastName HARGREAVES},
  \FirstName I.~E. \LastName GORDON, \FirstName L.~S. \LastName ROTHMAN}
\address{Center for Astrophysics $|$ Harvard and Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA}

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\author{\FirstName X. \LastName HUANG}
\address{NASA Ames Research Center, Moffett Field, CA 94035, USA; SETI Institute, 339 Bernado Avenue, Mountain View, CA 94043, USA }
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%\author{\FirstName L.~S. \LastName Rothman}
%\address{Center for Astrophysics $|$ Harvard and Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA}

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\fancyhead[C]{{\footnotesize \textit{HRMS, 28th Colloquium, Dijon, France,
  Aug. 28 - Sept. 1, 2023}}}
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\category {9,3}
\begin{document}

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The HITEMP database\footnote{Rothman, et al. {\it JQSRT\/}, {\bf 111}, 2139 (2010), \href{http://dx.doi.org/10.1016/j.jqsrt.2010.05.001}{doi:10.1016/j.jqsrt.2010.05.001}\label{refer1}} (\url{www.hitran.org/hitemp}) was established to model the radiative transfer of high temperature gaseous environments and provides accurate line-by-line molecular spectroscopic parameters for eight molecules: H$_{2}$O, CO$_{2}$, N$_{2}$O, CO, CH$_{4}$, NO, NO$_{2}$, and OH.  The addition and update of HITEMP line lists relies on the accuracy and completeness of state-of-the-art {\it ab initio} works. To account for molecular absorption at high temperatures, it is often necessary for these works to consider billions of individual transitions per isotopologue. This makes implementing full {\it ab initio}  line lists in line-by-line calculations impractical for applications such as calculating the radiative transfer of  stellar, brown dwarf, and exoplanetary atmospheres. When adding methane to the HITEMP database, a methodology\footnote{Hargreaves, et al. {\it ApJS\/}, {\bf 247}, 55 (2020), \href{http://dx.doi.org/10.3847/1538-4365/ab7a1a}{doi:10.3847/1538-4365/ab7a1a} \label{refer4}} was developed to convert the intensity contribution of numerous weak transitions into a relatively small number of ``effective'' lines, thereby substantially reducing the size of the line list while retaining the absorption contribution.

The recently-published AI-3000K infrared line list for hot carbon dioxide\footnote{Huang, et al. {\it JQSRT\/}, {\bf 392}, 111748 (2023), \href{http://dx.doi.org/10.1016/j.jms.2023.111748}{doi:10.1016/j.jms.2023.111748} \label{refer6}} contains over 36 billion transitions for the four most abundant CO$_{2}$ isotopologues, and has been shown to be accurate at high temperatures. AI-3000K provides an opportunity to extend the effective line approach developed for CH$_{4}$ in order to update the HITEMP line list of CO$_{2}$. This presentation will outline the development of the effective line methodology for CO$_{2}$, which reduces the total number of lines by 2 orders of magnitude. The CO$_{2}$ effective lines retain some quantum information that enables line broadening parameters to be applied to the HITEMP line list. The presentation will also include detailed validations against a series of high temperature experimental spectra.

%and will also include detailed validations against a series of high temperature experimental spectra.

%$^{\mbox{\scriptsize\ref{refer1}}}$$^,$\footnote{Hargreaves, et al. {\it JQSRT\/}, {\bf 232}, 35 (2019). \href{http://dx.doi.org/10.1016/j.jqsrt.2019.04.040}{doi:10.1016/j.jqsrt.2019.04.040} \label{refer}}$^,$\footnote{Hargreaves, et al. {\it ApJS\/}, {\bf 216}, 15 (2015). \href{http://dx.doi.org/10.1088/0067-0049/216/1/15}{doi:10.1088/0067-0049/216/1/15} \label{refer3}}$^,$\footnote{Hargreaves, et al. {\it ApJS\/}, {\bf 247}, 55 (2020), \href{http://dx.doi.org/10.3847/1538-4365/ab7a1a}{doi:10.3847/1538-4365/ab7a1a} \label{refer4}}

%Building on the technique that was used for CH$_{4}$ , 

%This enabled the CH4 line list to be practical to use while remaining capable of accurately modeling high temperature experimental spectra and astrophysical observations up to 2000 K. A major aspect of updating the HITRAN and HITEMP databases is comparing candidate line lists and validating against experimental works. A demonstration of these validations for H2O and CO2 will be presented, along with a summary of the most recent updates for HITEMP.

%AI-3000K Infrared line list for hot CO2\footnote{Huang, et al. {\it JQSRT\/}, {\bf 392}, 111748 (2023), \href{http://dx.doi.org/10.1016/j.jms.2023.111748}{doi:10.1016/j.jms.2023.111748} \label{refer6}}


%therefore contains substantially more transitions for each molecule than the corresponding molecule in HITRAN \footnote{Gordon, et al. {\it JQSRT\/}, {\bf 277}, 107949 (2022), \href{http://dx.doi.org/10.1016/j.jqsrt.2021.107949}{doi:10.1016/j.jqsrt.2021.107949} \label{refer5}}

%1.	Rothman, et al. (2010), JQSRT 111, 2139. (10.1016/j.jqsrt.2010.05.001) 
%2.	Hargreaves, et al. (2019), JQSRT 232, 35. (10.1016/j.jqsrt.2019.04.040) 
%3.	Li, et al. (2015), ApJS 216, 15. (10.1088/0067-0049/216/1/15)
%4.	Hargreaves, et al. (2020), ApJS 247, 55. (10.3847/1538-4365/ab7a1a) 
%5.	Gordon, et al. (2022), JQSRT 277, 107949. (10.1016/j.jqsrt.2021.107949) 





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