\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}