\begin{table}%t2
\caption{\label{tab2}Emission lines detected in the \textit{Chandra} ACIS spectrum.}
\par
\small%\centerline
 {
\begin{tabular}{l c c c }
\hline\hline     
Energy                 & Intensity            & $P_{\rm F}$     & Tentative~IDs \\
\hline                
%&&&& \\[-8pt]
$\rm 0.76^{+0.02}_{-0.13}$   &$\rm 2.93^{+1.16}_{-1.02}$  &$>$$98.9 \%$ &OVII RRC, Fe XVII 3s-2p\\
$\rm 0.93^{+0.04}_{-0.02}$   &$\rm 2.51^{+0.85}_{-1.20}$  &$>$$99 \%$ &Ne IX rif\\			
$\rm 1.30^{+0.04}_{-0.02}$   &$1.41\pm0.46$ 	  &$>$$99.97 \%$ &Mg XI He$\alpha$\\
\hline  
\end{tabular}}
\medskip
$E_{\rm c}$ is the centroid line energy (keV) in the source rest frame; $F$~is the line flux in units of 10$^{-6}$~photons~cm$^{-2}$~s$^{-1}$; $P_{\rm F}$~is the significance of the fit improvement after including the Gaussian line in the model, based on the F-test.
\end{table}