\begin{table}%t1
\caption{\label{abundance}LTE atmospheric abundances HD~49933 with error estimates based on the internal scatter from the number of analysed lines, $n$.}
%\centerline
 {\small \begin{tabular}{lcccccc}
\hline \hline
Ion &\multicolumn{4}{c}{HD~49933 -- this paper}& Bruntt et~al. (2008)  &  Sun \\                    
&$\log (N/N_{\rm tot})$ & $n$  &[$N_{\rm el}/N_{\rm H}$]$_{\rm AGS}$ &[$N_{\rm el}/N_{\rm H}$]$_{\rm GS}$ &[$N_{\rm el}/N_{\rm H}$]$_{\rm GS}$ &$\log (N/N_{\rm tot})$  \\
\hline    
\ion{C}{i}&$-3.74 \pm 0.10$ & 6 & $-$0.09 & $-$0.22 & $-$0.56 & $-$3.65\\			    %  & -0.17    
\ion{O}{i} &$-$3.55&1 &$-$0.17& $-$0.34 & $-$0.53 &$-$3.38\\	
\ion{Na}{i} &$-6.15 \pm 0.05$ & 5 & $-$0.28& $-$0.44 &$-$0.36 & $-$5.87\\ 
\ion{Mg}{i} &$-4.83 \pm 0.07$ & 4 &$-$0.32&$-$0.37 & &$-$4.51\\ 
\ion{Mg}{ii} &$-$4.73 &1 &$-$0.22&$-$0.27 & &$-$4.51\\
\ion{Al}{i} & $-$6.20: &  2 &$-$0.53&$-$0.63 &  & $-$5.67~ \\	\ion{Si}{i} & $-4.86 \pm 0.21$ & 20 & $-$0.33&$-$0.37 & $-$0.37 & $-$4.53\\ 
\ion{Si}{ii}&$-4.82 \pm 0.02$&6&$-$0.29&$-$0.33 & & $-$4.53~ \\	\ion{S}{i}& $-5.23 \pm 0.07$ & 2 &$-$0.33& $-$0.52 &$-$0.36 & $-$4.90\\ 
\ion{Ca}{i}&$-6.01\pm0.11$ & 26 &$-$0.28& $-$0.33 &$-$0.50 &$-$5.73\\ 
\ion{Ca}{ii}  &$- 6.01 \pm 0.09$ & 9 &$-$0.28&$-$0.33 &           & $-$5.73~ \\ 
\ion{Sc}{ii} &$- 9.24 \pm 0.12$ & 12 &$-$0.25&$-$0.37 &$-$0.45& $-$8.99 \\ 
\ion{Ti}{i} &$-7.54 \pm 0.07$ & 19 & $-$0.40&$-$0.52 & $-$0.52 & $-$7.14\\ 
\ion{Ti}{ii}  &$-7.42\pm0.12$ & 33 & $-$0.28&$-$0.40 &$-$0.41 & $-$7.14\\ 
\ion{V}{i}&$-8.50 \pm 0.13$ &4 & $-$0.46& $-$0.46 & & $-$8.04\\	\ion{V}{ii}&$-8.47 \pm 0.23$ & 5 &$-$0.43& $-$0.43 & & $-$8.04\\ 
\ion{Cr}{i} & $-6.82 \pm 0.17$ & 25 & $-$0.42&$-$0.45 &$-$0.63 & $-$6.40\\ 
\ion{Cr}{ii}  &  $- 6.61 \pm 0.17$ & 16 &$-$0.21& $-$0.24 & $-$0.43 & $-$6.40~ \\ 
\ion{Mn}{i} & $-7.33 \pm 0.14$ & 14 & $-$0.68& $-$0.68 &           &$-$6.65~ \\ 
\ion{Fe}{i} & $-5.04 \pm 0.06$ &158 & $-$0.45& $-$0.50 &$-$0.44 & $-$4.59\\ 
\ion{Fe}{ii}&$-5.03 \pm 0.08$ & 31 &$-$0.44&$-$0.49 &$-$0.44 & $-$4.59~ \\ 
\ion{Co}{i}& $-7.49\pm0.10$ &  3 & $-$0.37& $-$0.37 &           & $-$7.12~ \\			    %  &	-0.40
\ion{Ni}{i}   &$- 6.34 \pm 0.10$ & 41 &$-$0.53&$-$0.55 &$-$0.48 & $-$5.81 \\			    %  &	-0.57
\ion{Cu}{i}   & $-8.65 \pm 0.07$ &  2 & $-$0.82& $-$0.82 &       & $-$7.83 \\			    %  &	-0.86
\ion{Zn}{i}   & $-$8.12$\pm$0.06 &  2 &$-$0.66& $-$0.66 &           &$-$7.44\\			    %  &	-0.70
\ion{Sr}{i} &$-$9.65 &  1 &$-$0.53&$-$0.58 &  & $-$9.12 \\	\ion{Sr}{ii}  & $-9.50 \pm 0.04$ &  3 & $-$0.38& $-$0.43 &           & $-$9.12 \\			    %  &	-0.49
\ion{Y}{ii}   & $- 10.34 \pm 0.10$ &  5 & $-$0.51& $-$0.54 &           & $-$9.83 \\			    %  &	-0.64
\ion{Zr}{ii}  & $- 9.85 \pm 0.06$ &  5 & $-$0.40& $-$0.41 &           & $-$9.45 \\			    %  &	-0.45
\ion{Ba}{ii}  & $- 10.06 \pm 0.19$ &  5 & $-$0.19& $-$0.15 &           & $-$9.87\\			    %  &	-0.26
\ion{La}{ii} &$- 11.21 \pm 0.11$ &  5 & $-$0.30& $-$0.34 &           & ~$-$10.91~ \\			    %  & -0.34
\ion{Ce}{ii}  & ~$-10.73 \pm 0.10$ &  5 & $-$0.27& $-$0.27 &           & ~$-$10.46~ \\			    %  & -0.40
\ion{Nd}{ii}  & ~$-10.77 \pm 0.28$ &  8 & $-$0.18& $-$0.23 &           & ~$-$10.59~ \\			    %  & -0.11
\ion{Sm}{ii}  & ~$-11.09 \pm 0.16$ &  3 & $-$0.06& $-$0.06 &           & ~$-$11.03~ \\			    %  & -0.22
\ion{Eu}{ii}  & ~$-11.92 \pm 0.10$ &  2 & $-$0.40& $-$0.39 &           & ~$-$11.52~ \\			    %  & -0.68
\ion{Gd}{ii}  & ~$-11.16 \pm 0.09$ &  4 & $-$0.24& $-$0.24 &           & ~$-$10.92~ \\			    %  & -0.18
\ion{Dy}{ii}  & ~$-11.36 \pm 0.15$ &  2 & $-$0.46& $-$0.46 &           &$-$10.90\\ 
\hline								\Teff     &\multicolumn{4}{c}{6500~K}    & 6780~K    & 5777~K\\	\logg     &\multicolumn{4}{c}{4.00~}   & 4.24~   & 4.44\\	 
\hline		  
\end{tabular}}
\medskip
Fourth and fifth columns give HD~49933 abundances relative to the solar values from \citet{met05}~(AGS) and from \citet{sun_GS} (GS), respectively. The sixth column gives abundances derived
by Bruntt et~al. (2008) relative to GS. The last column gives the abundances of the solar atmosphere from \citet{met05}.
\end{table}