\begin{table}%t2
\caption{Absolute coronal abundances of CN~Leo$ ^1$.}\label{abund} 
\small%\centerline
{
\begin{tabular}{ccccccccc}
\hline\hline
&C  & N & O & Ne & Mg & Si & S &Fe\\
\hline
XSPEC    &1.49 $\pm$ 0.24 & 1.28 $\pm$ 0.21 & 0.62 $\pm$ 0.08 & 1.20 $\pm$ 0.16 & 0.85 $\pm$ 0.17 & 0.78 $\pm$ 0.33& 1.41 $\pm$ 0.27  & 0.59 $\pm$ 0.07\\
$\it DEM$ method 1 &1.27 $\pm$ 0.13 & 1.03 $\pm$ 0.13 & 0.66 $\pm$ 0.03 & 1.22 $\pm$ 0.11 & 0.92 $\pm$ 0.16 &n.a.&n.a  & 0.56 $\pm$ 0.04\\
$\it DEM$ method 2 &1.18 $\pm$ 0.12 & 0.97 $\pm$ 0.12 & 0.63 $\pm$ 0.03 & 1.17 $\pm$ 0.11 & 0.85 $\pm$ 0.15 &n.a.&n.a  & 0.55 $\pm$ 0.04\\
\hline
\end{tabular}}
\medskip
$ ^1$ Abundances are derived from the RGS and EPIC data as fitted with a~three~component temperature model as described in Sect.~\ref{xspec}. Methods~1 and~2 use a~differential emission measure method as described in Sect.~\ref{emissionmeasure}. The given errors
are the statistical 1$\sigma$~standard deviations.
\end{table}