\begin{table}%t3 \caption{\label{t3}Abundances obtained for the target stars.} %\centerline { \par \begin{tabular}{lccccccccc} \hline\hline El. & 11583 & 12404 & 13415 & 16149 & 18646 & 8745 & 24938 & ${\rm \langle \log\epsilon (El)\rangle}$ & [El/H]\\ \hline HeI & $<$11.1 & 10.89 $\pm$ 0.07 & -- & -- & 10.90 $\pm$ 0.07 & 10.84 $\pm$ 0.07 & 10.99 $\pm$ 0.07 & 10.91 $\pm$ 0.03 & -- \\ OI & 7.56 $\pm$ 0.13& 7.84 $\pm$ 0.10& 7.82 $\pm$ 0.08& 7.73 $\pm$ 0.07& 7.86 $\pm$ 0.11& 7.83 $\pm$ 0.10& 7.87 $\pm$ 0.06& -- & -- \\ OI$_{\rm NLTE}$ & 7.41 $\pm$ 0.13& 7.70 $\pm$ 0.10& 7.68 $\pm$ 0.08& 7.56 $\pm$ 0.07& 7.72 $\pm$ 0.11& 7.68 $\pm$ 0.10& 7.70 $\pm$ 0.06& 7.67 $\pm$ 0.02 & --1.16 $\pm$ 0.03\\ NaI & 5.35 $\pm$ 0.10& 4.72 $\pm$ 0.04& 4.78 $\pm$ 0.05& 4.65 $\pm$ 0.03& 4.85 $\pm$ 0.03& 4.60 $\pm$ 0.04& 4.71 $\pm$ 0.02& -- & -- \\ NaI$_{\rm NLTE}$ & 5.15 $\pm$ 0.10& 4.52 $\pm$ 0.04& 4.58 $\pm$ 0.05& 4.45 $\pm$ 0.03& 4.65 $\pm$ 0.03& 4.40 $\pm$ 0.04& 4.51 $\pm$ 0.02& 4.52 $\pm$ 0.04 & --1.81 $\pm$ 0.04\\ SiII & 6.17 $\pm$ 0.13& 6.31 $\pm$ 0.10& 6.24 $\pm$ 0.10& 6.20 & 6.28 $\pm$ 0.12& 6.25 $\pm$ 0.09& 6.18 & 6.23 $\pm$ 0.02 & --1.32 $\pm$ 0.02\\ TiII & 3.61 $\pm$ 0.05& 3.74 $\pm$ 0.04& 3.64 $\pm$ 0.03& 3.58 $\pm$ 0.03& 3.71 $\pm$ 0.03& 3.60 $\pm$ 0.04& 3.60 & 3.64 $\pm$ 0.02 & --1.38 $\pm$ 0.02\\ CrII & 3.92 $\pm$ 0.05& 4.17 $\pm$ 0.06& 4.06 $\pm$ 0.02& 3.96 $\pm$ 0.04& 4.00 $\pm$ 0.02& 3.98 $\pm$ 0.04& 4.12 & 4.03 $\pm$ 0.03 & --1.64 $\pm$ 0.03\\ FeI & 5.83 $\pm$ 0.02& 6.14 $\pm$ 0.02& 5.97 $\pm$ 0.02& 5.82 $\pm$ 0.03& 6.08 $\pm$ 0.02& 5.91 $\pm$ 0.02& -- & 5.96 $\pm$ 0.05 & --1.54 $\pm$ 0.05\\ FeII & 5.81 $\pm$ 0.04& 6.01 $\pm$ 0.05& 5.95 $\pm$ 0.07& 5.92 $\pm$ 0.06& 5.95 $\pm$ 0.05& 5.89 $\pm$ 0.05& 5.94 $\pm$ 0.04& 5.92 $\pm$ 0.02 & --1.58 $\pm$ 0.02\\ BaII & 0.25 & -- & 0.45 & 0.55 & -- & -- & -- & 0.42 $\pm$ 0.09 & --1.71 $\pm$ 0.09\\ \hline \end{tabular}} \medskip \par In the two last columns we give the average abundances and the average abundances relative to the Sun. In the calculation of the average abundances of O and Na we rejected the star \#11583 because its O and Na contents deviate from the general trend (see text). For \#11583 we give an upper limit for the He abundance, which is useful for the discussion, see Sect.~6. Errors for He abundance were obtained as described in Sect.~6. \end{table}