\begin{table}%T4
\caption{Chemical abundances of the secondary star in  {Nova Scorpii~1994}.} 
\label{tbl4} 
\small%\centerline
{        
\begin{tabular}{lccccccc}     % 7 columns 
\hline
\hline\noalign{\smallskip}
Element & $[{\rm X}/{\rm
H}]_{\rm LTE}^{a,b}$ & $\sigma$ & $\Delta_\sigma^{c}$ &
$\Delta_{T_{\rm eff}}$ & $\Delta_{\log g}$ & $\Delta_{\rm tot}$ &  $n_{\rm lines}^{d}$\\   
\noalign{\smallskip}
\hline     
\noalign{\smallskip}
O$^{e}$  &  0.91 & 0.07 & 0.04 & 0     &  0.07 & 0.09 & 3  \\
Na           &  0.31 & 0.37 & 0.18 & 0.19  &  0    & 0.26 & 4  \\
Mg           &  0.48 & 0.29 & 0.09 & 0.10  & --0.03 & 0.15 & 10 \\
Al           &  0.05 & 0.15 & 0.15 & 0.1   &  0    & 0.18 & 1  \\
Si           &  0.58 & 0.21 & 0.06 & 0.05  &  0.01 & 0.08 & 12 \\
S            &  0.66 & 0.18 & 0.09 & --0.04 &  0.06 & 0.12 & 4  \\
Ca           & --0.02 & 0.17 & 0.07 & 0.12  &  0.01 & 0.14 & 7  \\
Ti           &  0.27 & 0.11 & 0.07 & 0.2   &  0.05 & 0.22 & 2  \\
Fe~          & --0.11 & 0.11 & 0.03 & 0.09  &  0.01 & 0.10 & 9  \\
Ni           &  0    & 0.10 & 0.06 & 0.2   &  0.05 & 0.21 & 5  \\
Li$^{f}$ &  2.13 & 0.15 & 0.15 & 0.15  &  0    & 0.21 & 1  \\ 
\hline
\end{tabular}}
\smallskip
$^{a}$ The solar element abundances were adopted from Grevesse
et~al. (\cite{Grevesse1996}) and Ecuvillon et~al. (\cite{Ecuvillon2006}):
$\log \epsilon({\rm O })_{\odot}=8.74$, 
$\log \epsilon({\rm Na})_{\odot}=6.33$,
$\log \epsilon({\rm Mg})_{\odot}=7.58$,  
$\log \epsilon({\rm Al})_{\odot}=6.47$,  
$\log \epsilon({\rm Si})_{\odot}=7.55$,  
$\log \epsilon({\rm S })_{\odot}=7.21$,  
$\log \epsilon({\rm Ca})_{\odot}=6.36$,  
$\log \epsilon({\rm Ti})_{\odot}=4.99$,  
$\log \epsilon({\rm Fe})_{\odot}=7.50$,  
$\log \epsilon({\rm Ni})_{\odot}=6.25$.\\
$^{b}$ Element abundances (calculated assuming LTE) are
${\rm [X/H]}= \log [N({\rm X})/N({\rm H})]_{\rm star} - \log
[N({\rm X})/N({\rm H})]_{\rm Sun}$, where $N({\rm X})$ is
the number density of atoms. Uncertainties, $\Delta_{\rm tot}$, are at
1$\sigma$ level and take into account the error in the
stellar parameters and the dispersion of the measurements.\\
$^{c}$ The errors from the dispersion of the best
fits to different features, see text.\\
$^{d}$ Number of features analysed for each element.\\
$^{e}$ LTE abundance of oxygen, see text.\\
$^{f}$ \mbox{Li}~abundance is expressed as: \[\log
\epsilon({\rm Li})_{\rm NLTE} = \log
[N({\rm Li})/N({\rm H})]_{\rm NLTE} + 12.\]
\end{table}