\begin{table}%T4
\caption{Summary of the abundances derived in the programme stars. 
$N$, indicates the number of lines
utilized for a specific element if more than one line was used (we then
give the mean abundance together with its dispersion). 
[el/M] is the abundance 
ratio with respect to the mean derived [M/H] (see text and Table~\ref{t3}) and is only quoted for 
elements with $A\geq 30$.}
\label{t4}    
%\centerline
{ 
\begin{tabular}{cccccccccc}           
\hline\hline                      
       &   & IGI95-C1      &              &   & IGI95-C3      &                     &  
  &BMB-B~30       &                       \\     
\hline           
Element& $N$ & log $\epsilon$& $\rm{[el/M]}$& $N$ & log $\epsilon$& $\rm{[el/M]}$& 
$N$ & log $\epsilon$& $\rm{[el/M]}$ \\
\hline
Li&  & ${<}{-}0.50$     &       &   &$-1.00$      &      &   &$-0.80$      &           \\
Ca&  & --           &       &   &$5.85$       &      &   &$5.30$       &    \\
Ti& 3& $4.20\pm0.12$&       &  2&$4.70\pm0.05$&      &  4&$3.90\pm0.08$&           \\
V&  3& $3.10\pm0.15$&       &  3&$3.50\pm0.15$&      &   & --          &           \\
Cr& 2& $4.90\pm0.10$&       &   &$5.32$       &      &  2&$4.98\pm0.05$&       \\
Mn&  &  --          &       &   &  --         &      &  3&$4.39\pm0.05$&       \\
Fe&  & 6.85         &       &   &  --         &      &  3&$6.50\pm0.08$&       \\
Ni& 2& $5.50\pm0.10$&       &  2&$5.85\pm0.05$&      &   &$5.25$       &        \\
Zn&  & $4.00$       &$0.20$ &   &$4.10$       &$0.00$&   &$4.00$       &$0.40$ \\
Rb&  &${<}2.10$       &${<}0.50$&   &--           &      &   &$1.40$       &$0.00$ \\
Sr& 2&$3.00\pm0.17$ &$ 0.80$&  2&$3.35\pm0.05$&$0.90$&  2&$2.55\pm0.15$&$0.60$ \\
Y & 2&$2.05\pm0.03$ &$0.60$ &   &$2.55$       &$0.80$&  2&$1.65\pm0.02$&$0.40$ \\
Zr& 4&$2.30\pm0.09$ &$0.50$ &  5&$3.30\pm0.20$&$1.20$&  4&$2.00\pm0.04$&$0.40$ \\
Nb&  &${<}0.72$       &${<}0.10$&   &${<}1.20$      &${<}0.30$&  &${<}0.42$      &${<}0.00$\\
Ru& 2&$1.50\pm0.10$ &$0.50$ &   & --          &       &  &$1.45$       &${<}0.60$\\
Ba&  &$2.80$          &$1.50$ &   & $2.55$$^a$ &$0.80$ &  & $2.60$& $1.50$ \\
La& 5&$1.95\pm0.20$ &$1.60$ &   &$1.35$       &$0.70$ & 2&$1.50\pm0.15$&$1.40$ \\
Ce&  &${<}2.50$       &${<}1.70$&   & --          &       & 2&$1.60\pm0.20$&$1.00$ \\
Pr& 4&$1.10\pm0.04$ &$1.20$ &   & --          &       & 2&$0.80\pm0.08$&$1.10$ \\
Nd& 5&$2.50\pm0.12$ &$1.80$ &  2&$2.00\pm0.05$&$1.00$ & 4&$2.10\pm0.11$&$1.60$ \\
Sm& 2&$1.40\pm0.01$ &$1.20$ &  2&$1.50\pm0.10$&$0.90$ & 2&$1.05\pm0.05$&$0.95$ \\
Gd&  &${<}1.50$       &${<}1.20$&   &  --         &       &  &  --         &          \\
Hf&  &$1.00$          &$0.90$ &   &  --       &       &  & $1.10$      & $1.20$ \\
W &  &$1.20$          &$0.90$ &   &  --       &       &  & $0.50$      & $0.40$ \\
\hline                                   
\end{tabular}}
\medskip
$^a$ The Ba abundance derived in this star may be affected by 
the presence of Merrill-Sanford bands (see text).
\end{table}