\begin{table}%t4
\caption{\label{abundance}LTE atmospheric abundances in programme stars with the error
estimates based on the internal scattering from the number of analysed lines, $n$.}
%\centerline
{
\begin{tabular}{l|cc|cc|cc|c}
\hline
\hline
Ion &\multicolumn{2}{|c|}{HD~145788} &\multicolumn{2}{c|}{21~Peg} &\multicolumn{2}{c|}{$\pi$~Cet} &  Sun (*) \\                                  %HD66318&
    &$\log (N/N_{\rm tot})$ & $n$  &$\log (N/N_{\rm tot})$ & $n$ &$\log (N/N_{\rm tot})$ & $n$ &$\log (N/N_{\rm tot})$  \\       %& $\log (N/N_{\rm tot})$ 
\hline
\ion{He}{i }  & ~~$-$1.10 $\pm$ 0.05 &  4 & ~~$-$1.09 $\pm$ 0.03 &  7 & ~~$-$0.97 $\pm$ 0.04 &  6 & ~~$-$1.12~ \\                            %  & 0.95 for 5876 and 6678       
%\ion{C}{i}    & ~~$-$3.43 $\pm$ 0.12 &  5 & ~~$-$3.71 $\pm$ 0.17 & 12 &                   &    & ~~$-$3.65~ \\			    % & 	
\ion{C}{i}    & ~~$-$3.60 $\pm$ 0.14 &  5 & ~~$-$3.66 $\pm$ 0.14 &  9 &                    &    & ~~$-$3.65~ \\			    % & using NIST for all lines	
\ion{C}{ii}   & ~~$-$3.63:         &  2 & ~~$-$3.65 $\pm$ 0.05 &  4 & ~~$-$3.58 $\pm$ 0.07 &  7 & ~~$-$3.65~ \\			    % & 	
\ion{N}{i}    &                    &    & ~~$-$3.95 $\pm$ 0.12 &  4 & ~~$-$4.03 $\pm$ 0.13 & 10 & ~~$-$4.26~ \\			    % & 	
\ion{N}{ii}   &                    &    & ~~$-$3.90:         &  1 & ~~$-$3.74 $\pm$ 0.07 &  9 & ~~$-$4.26~ \\			    % & 	
\ion{O}{i}    & ~~$-$3.12 $\pm$ 0.09 &  7 & ~~$-$3.28 $\pm$ 0.11 & 18 & ~~$-$3.06 $\pm$ 0.14 &  9 & ~~$-$3.38~ \\			    % & ~$-$4.6 
\ion{O}{ii}   &                    &    &                    &    & ~~$-$3.04:         &  2 & ~~$-$3.38~ \\			    % & ~$-$4.6 
\ion{Ne}{i}   &                    &    & ~~$-$3.76 $\pm$ 0.05 &  7 & ~~$-$3.66 $\pm$ 0.09 & 20 & ~~$-$4.20~ \\			    % & ~$-$4.6 
\ion{Na}{i}   &                    &    & ~~$-$5.60:         &  1 & ~~$-$5.23 $\pm$ 0.07 &  3 & ~~$-$5.87~ \\			    %  &	  
\ion{Mg}{i}   & ~~$-$4.17 $\pm$ 0.24 &  5 & ~~$-$4.42 $\pm$ 0.12 &  5 & ~~$-$4.27:         &  2 & ~~$-$4.51~ \\			    %  &	  
\ion{Mg}{ii}  & ~~$-$4.29 $\pm$ 0.06 &  4 & ~~$-$4.56 $\pm$ 0.03 &  7 & ~~$-$4.47 $\pm$ 0.16 & 10 & ~~$-$4.51~ \\			    %  & ~$-$4.95
\ion{Al}{i }  & ~~$-$5.70:         &  2 & ~~$-$5.89:         &  2 & ~~$-$5.57:         &  2 & ~~$-$5.67~ \\			    %  &	  
\ion{Al}{ii}  & ~~$-$5.11 $\pm$ 0.10 &  3 & ~~$-$5.70 $\pm$ 0.10 &  4 & ~~$-$5.73 $\pm$ 0.27 &  8 & ~~$-$5.67~ \\			    %  &	  
\ion{Al}{iii} &                    &    &                    &    & ~~$-$5.30 $\pm$ 0.02 &  3 & ~~$-$5.67~ \\			    %  &	  
\ion{Si}{i}   & ~~$-$4.75:         &  1 & ~~$-$4.95:         &  1 & ~~$-$4.80:         &  1 & ~~$-$4.53~ \\			    %  & using BL loggf for 3905 	  
\ion{Si}{ii}  & ~~$-$4.27 $\pm$ 0.14 & 11 & ~~$-$4.49 $\pm$ 0.13 & 22 & ~~$-$4.41 $\pm$ 0.20 & 31 & ~~$-$4.53~ \\			    %  & ~$-$2.8 
\ion{Si}{iii} &                    &    & ~~$-$4.26 $\pm$ 0.18 &  2 & ~~$-$4.16:         &  2 & ~~$-$4.53~ \\			    %  & ~$-$2.8 
\ion{P}{ii}   &                    &    & ~~$-$6.37 $\pm$ 0.06 &  3 & ~~$-$6.38 $\pm$ 0.19 &  9 & ~~$-$6.68~ \\			    %  & ~$-$2.8 
\ion{P}{iii}  &                    &    &                    &    & ~~$-$6.19:         &  1 & ~~$-$6.68~ \\			    %  & ~$-$2.8 
\ion{S}{ii}   & ~~$-$4.36:         &  2 & ~~$-$4.86 $\pm$ 0.13 & 26 & ~~$-$4.78 $\pm$ 0.16 & 31 & ~~$-$4.90~ \\			    %  & ~$-$2.8 
\ion{Cl}{ii}  &                    &    &                    &    & ~~$-$6.95:         &  2 & ~~$-$6.54~ \\			    %  & ~$-$2.8 
\ion{Ar}{i}   &                    &    &                    &    & ~~$-$4.86 $\pm$ 0.24:&  2 & ~~$-$5.86~ \\			    %  &	  
\ion{Ar}{ii}  &                    &    &                    &    & ~~$-$5.24 $\pm$ 0.19 &  6 & ~~$-$5.86~ \\			    %  & ~$-$2.8 
\ion{Ca}{i}   & ~~$-$5.46 $\pm$ 0.11 &  5 & ~~$-$5.84 $\pm$ 0.11 &  3 &                    &    & ~~$-$5.73~ \\			    %  &	  
\ion{Ca}{ii}  & ~~$-$5.54 $\pm$ 0.16 &  6 & ~~$-$5.98 $\pm$ 0.08 &  5 & ~~$-$5.77:         &  2 & ~~$-$5.73~ \\			    %  & ~$-$6.4 
\ion{Sc}{ii}  & ~~$-$8.90 $\pm$ 0.03 &  5 & ~~$-$9.37 $\pm$ 0.10 &  7 & ~~$-$9.31:         &  1 & ~~$-$8.99~ \\			    %  &	  
\ion{Ti}{ii}  & ~~$-$6.80 $\pm$ 0.15 & 47 & ~~$-$7.23 $\pm$ 0.09 & 59 & ~~$-$7.42 $\pm$ 0.08 & 11 & ~~$-$7.14~ \\			    %  & ~$-$5.15
\ion{V}{ii}   & ~~$-$7.55 $\pm$ 0.20 &  4 & ~~$-$7.98 $\pm$ 0.06 &  9 &                    &    & ~~$-$8.04~ \\			    %  &				  
\ion{Cr}{i}   & ~~$-$6.15 $\pm$ 0.09 &  4 & ~~$-$6.29 $\pm$ 0.09 &  5 &                    &    & ~~$-$6.40~ \\			    %  &	  
\ion{Cr}{ii}  & ~~$-$5.86 $\pm$ 0.11 & 31 & ~~$-$6.20 $\pm$ 0.10 & 68 & ~~$-$6.41 $\pm$ 0.10 & 21 & ~~$-$6.40~ \\			    %  & ~$-$3.8 
\ion{Mn}{i}   & ~~$-$6.43:         &  2 & ~~$-$6.54 $\pm$ 0.21 &  5 &                    &    & ~~$-$6.65~ \\			    %  &	  
\ion{Mn}{ii}  & ~~$-$6.15 $\pm$ 0.08 &  4 & ~~$-$6.51 $\pm$ 0.17 & 19 & ~~$-$6.50 $\pm$ 0.09 &  3 & ~~$-$6.65~ \\			    %  & ~$-$6.85
\ion{Fe}{i}   & ~~$-$4.23 $\pm$ 0.16 & 88 & ~~$-$4.52 $\pm$ 0.13 &108 & ~~$-$4.53 $\pm$ 0.22 &  7 & ~~$-$4.59~ \\			    %  &	  
\ion{Fe}{ii}  & ~~$-$4.13 $\pm$ 0.15 &147 & ~~$-$4.50 $\pm$ 0.12 &406 & ~~$-$4.58 $\pm$ 0.14 &186 & ~~$-$4.59~ \\			    %  & ~$-$3.05
\ion{Fe}{iii} &                    &    & ~~$-$4.60 $\pm$ 0.06 &  3 & ~~$-$4.52 $\pm$ 0.10 &  4 & ~~$-$4.59~ \\			    %  & ~$-$3.05
\ion{Co}{ii}  &                    &    & ~~$-$6.75 $\pm$ 0.18 &  3 & ~~$-$6.93:         &  1 & ~~$-$7.12~ \\			    %  &	  
\ion{Ni}{i}   & ~~$-$5.32 $\pm$ 0.13 &  8 & ~~$-$5.71 $\pm$ 0.05 & 10 &                    &    & ~~$-$5.81~ \\			    %  &	  
\ion{Ni}{ii}  & ~~$-$5.12 $\pm$ 0.05 &  3 & ~~$-$5.61 $\pm$ 0.09 & 23 & ~~$-$5.76 $\pm$ 0.19 & 17 & ~~$-$5.81~ \\			    %  &	  
\ion{Zn}{i}   &                    &    & ~~$-$6.86:         &  1 &                    &    & ~~$-$7.44~ \\			    %  &	  
\ion{Sr}{ii}  & ~~$-$8.45:         &  2 & ~~$-$9.10:         &  2 & ~~$-$9.15:         &  2 & ~~$-$9.12~ \\			    %  &	  
\ion{Y}{ii}   & ~~$-$9.06:         &  1 & ~~$-$9.76 $\pm$ 0.15 &  4 &                    &    & ~~$-$9.83~ \\			    %  &	  
\ion{Zr}{ii}  & ~~$-$8.75 $\pm$ 0.32 &  3 & ~~$-$9.48 $\pm$ 0.28 &  4 &                    &    & ~~$-$9.45~ \\			    %  &	  
\ion{Ba}{ii}  & ~~$-$8.96 $\pm$ 0.11 &  3 & ~~$-$9.19 $\pm$ 0.06 &  3 &                    &    & ~~$-$9.87~ \\			    %  &	  
%\ion{Pr}{iii} & ~~$-$9.71 $\pm$ 0.09 &  2 & ~~$-$9.71 $\pm$ 0.09 &  2& ~~$-$9.71 $\pm$ 0.09 &  2 & ~$-$11.33~ \\			    % & ~$-$8.3 
\ion{Nd}{iii} &                    &    & ~$-$10.09 $\pm$ 0.07 &  3 &                    &    & ~$-$10.59~ \\			    % & ~$-$7.0 
\hline											     % 
\Teff     &\multicolumn{2}{|c|}{9750~K}   &\multicolumn{2}{c|}{10~400~K}   &\multicolumn{2}{c|}{12~800~K}   & 5777~K  \\				%   &	 9200 
\logg     &\multicolumn{2}{|c|}{3.7~~~~~} &\multicolumn{2}{c|}{3.55~~~~}  &\multicolumn{2}{c|}{3.75~~~~} & 4.44~~~~\\				   %   &    4.50 
\hline						 \end{tabular}}
\smallskip
\par
Internal scattering was not estimated when $n<3$, in which case
the derived abundance if flagged with a colon (:). (*) The abundances of the solar atmosphere
calculated by \citet{met05}. 
\end{table}