\begin{table}%t4
%\centering
\par
\caption{{\em Chandra} ACIS--S spectral fitting results when the thermal 
emission model (Model~1) and the photoionized gas model (Model~2) are applied 
to the spectrum of the inner 10$''$. The last column refers to the 
spectrum of the extended hot gas halo instead. Fluxes are given in units of 
$10^{-13}$~erg~cm$^{-2}$ s$^{-1}$, luminosities in units of 
$10^{43}$~erg~s$^{-1}$; both are corrected for absorption. 
$^*$ denotes a fixed parameter.}
\label{chares}
\begin{tabular}{llll}
\par
\hline\hline 
\par
&  {Model 1} &  {Model 2} &  {Hot Gas} \\
& Inner $10''$ & Inner $10''$ &  {Halo} \\
\hline
\par
\bf{Apec(1)} & & & \\ 
$kT$ [keV] & $\rm 7.8^{+7.5}_{-2.8}$ & -- & -- \\
$f~_{0.3 - 10\: {\rm keV}}$ & $\rm 1.60^{+0.20}_{-0.17}$ & -- & -- \\   
\hline
\par
\bf{Apec(2)} & & & \\ 
$kT$ [keV] & $\rm 0.80^{+0.04}_{-0.05}$ & $0.81\pm0.05$ & -- \\
$f~_{0.3 - 10\: {\rm keV}}$ & $0.37\pm0.06$ & $\rm 0.33^{+0.03}_{-0.05}$ &  -- \\   
\hline
\par
\bf{Apec(3)} & & & \\
$kT$ [keV] & -- & -- & $0.38\pm0.04$ \\   
$f~_{0.3 - 10\: {\rm keV}}$ & -- & -- & $0.30\pm0.04$ \\   
\hline
\par
\bf{Power-law(1)} & & & \\
$N{\rm H}$ [$10^{22}$~cm$^{-2}$] & $41\pm6$ & $39\pm5$ & -- \\
$\Gamma$ & $1.9^*$ & $1.9^*$ & -- \\  
$f~_{0.3 - 10 \:{\rm keV}}$ & $\rm 53^{+12}_{-9}$ & $\rm 53^{+10}_{-9}$ & -- \\   
\hline
\par
\bf{Power-law(2)} & & & \\
$N{\rm H}$ [$10^{20}$~cm$^{-2}$] & -- & $6.8^{+2.3}_{-2.0}$ & -- \\
$\Gamma$ & -- & $1.9^*$ & -- \\  
$f~_{0.3 - 10\: {\rm keV}}$ & -- & $1.7\pm0.2$ & -- \\   
\hline
\par
\bf{Fe K$\alpha$} & & & \\
$E$ & $6.34\pm0.04$ & $6.34\pm0.04$ & -- \\
$EW$ [eV] & $255\pm125$ & $242\pm120$ & -- \\     
$f~_{0.3 - 10\: {\rm keV}}$ & $0.72\pm0.35$ & $0.69\pm0.34$ & --  \\   
\hline
\par
\bf{Total} & & & \\
$f~_{0.3 - 10 \:{\rm keV}}$ & 55.4 & 55.9 & 0.3 \\ 
$L~_{0.3 - 10\: {\rm keV}}$ & 1.84 & 1.86 & 0.01 \\ 
\hline\noalign{\smallskip}
\par
$\chi^2/$d.o.f. & 65.0/75 & 62.0/75 & -- \\   
\hline
\end{tabular}
\end{table}