\begin{table}%t3
%\centering
\par
\caption {\label{tab:pnspecall}The joint best-fit spectral parameter for the 2-$T$ fit with individually varying metal abundances for the 4 pn spectra. The notation ``$M/M_\odot$'' indicates the ratio between the \bcep\ coronal abundance and the solar photospheric abundance. The notation ``$M/M_{\rm phot}$'' indicates the ratio between the coronal abundance of \bcep\ determined here and the photospheric abundance of \bcep\ determined by \citet{mba+2006}. In all cases, the solar photospheric abundances of \citet{gs98} were used. The indicated uncertainties are~90\% errors derived from a $\Delta \chi^2$ analysis. For all heavy elements not explicitly indicated, the abundances are equal to the value for~Fe.}
\begin{tabular}{cl}
\hline\hline
$N({\rm H})$ & $2.50 \pm 0.01 \times 10^{20}$ cm$^{-2}$\\
$T_1$ & $0.24\pm0.01 $ keV\\
$T_2$ & $0.63\pm0.03 $ keV\\
$E\!M_1$ & $1.1\pm0.2$ $10^{54}$ cm$^{-3}$ \\
$E\!M_2$ & $1.3\pm0.3$ $10^{53}$ cm$^{-3}$ \\ 
O/O$_\odot$ & $0.12\pm0.02 $\\
Ne/Ne$_\odot$ & $0.18\pm0.03$ \\
Si/Si$_\odot$ & $0.31\pm0.06 $\\
Fe/Fe$_\odot$ & $0.33\pm0.04$\\ 
O/O$_{\rm phot}$ & 0.28\\
Si/Si$_{\rm phot}$ & 0.86\\
Fe/Fe$_{\rm phot}$ & 0.60\\
\hline
\end{tabular}
\end{table}