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\begin{document}
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   \title{Calibration approach in the light of Gaia space mission}

   \subtitle{MARCS model based analysis of $\delta$ Eri}
   
   \author{V. Makaganiuk, A.J. Korn, U. Heiter and O. Kochukhov }

   \titlerunning{$\delta$ Eri RVS abundances}

   \institute{Department of Physics and Astronomy, Division of Astronomy and Space Physics, Uppsala University, Box 515, 75120 Uppsala, Sweden\\
              \email{Vitaly.Makaganiuk@fysast.uu.se} \\
              \email{Andreas.Korn@fysast.uu.se}      \\
              \email{Ulrike.Heiter@fysast.uu.se}     \\
              \email{Oleg.Kochukhov@fysast.uu.se}}

   \date{Received XX XX, 2010; accepted XX XX, 2010}

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  \abstract
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   {We investigate the possibility of using two spectral regions as independent and self-confirming information source for the derivation of fundamental parameters of the $\delta$ Eri star. It is also known that different stellar atmosphere models can introduce noticeable systematic effects in abundance derivation, so prior to the core analysis we have corrected a line list that was used in further analysis.}
  % aims heading (mandatory)
   {Compilation of a list of atomic lines with calibrated oscillator strengths for cool stellar models which to be used in future analysis of Gaia late-type stars. Judgement of the possible usage of optical region vs. infra-red in terms of deriving the information about fundamental stellar parameters and individual abundances of some chemical elements.}
  % methods heading (mandatory)
   {In order to minimize possible modelling effects we have calibrated \textit{gf} values of the spectral lines used in our analysis against the solar spectrum. For this purpose Spectroscopy Made Easy (SME) package along with MARCS model was utilized. The spectral synthesis method is underlying all our analysis process and calculations done under LTE assumption.}
  % results heading (mandatory)
   {It was found that that the results derived in the optical region of the spectrum fully confirm those, derived in the infra-red in spite of large quality difference between these regions. We also estimated the importance of the error in the initial parameters of the investigated object and their influence on the final result so it allowed us to conclude how accurately we can derive fundamental parameters and, particularly, abundances if the main tool for that is SME.}
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   {}

   \keywords{methods: data analysis -- techniques: spectroscopic -- stars: abundances}

   \maketitle

\section{Introduction}
\label{intro}
\input{intro}

\section{Fundamental parameters of \boldmath$\delta $\unboldmath \ Eri}
\label{para}
\input{para}

\section{Observations and some notes on data reduction}
\label{obs}
\input{obs}

\section{Preparation of the line list}
\label{linelist}
\input{linelist}

\newpage
\section{Analysis}
\label{ana}
\input{ana}

\section{Conclusions}
\label{conc}
\input{conc}

\begin{acknowledgements}
We thank \ldots\\
This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.\\
TNG\\
OPTICON\\
VM, AK and UH acknowledge support from the Swedish National Space Board.
\end{acknowledgements}

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\input{table_gfcorr_FeI_opt}

\end{document}
