\begin{table}%t1
%\centering
\par
  \caption {\label{tab1}Spectral fit to the Suzaku XIS time-averaged spectrum.}
    \begin{tabular}{ccccccccc}
    \hline\hline
    \noalign{\smallskip}
Data & $\Gamma$ & \nH & $N_{\rm H,W}$ & $\xi$ &
$E_{\rm FeK}$ & $\sigma$ & $I_{\rm FeK}$ & $\chi^2$/d.o.f. \\
& & \psqcm & \psqcm
& erg\thinspace s$^{-1}$\thinspace cm
&keV & keV & \phpspsqcm & \\ 
\hline
Total & $\rm 1.40^{+0.05}_{-0.04}$ & $5.4^{+2.8}_{-3.0}\times 10^{20}$
& $2.1^{+0.3}_{-0.2}\times 10^{22}$ & $\rm 34^{+5}_{-4}$ & $\rm 6.36^{+0.04}_{-0.04}$ & $\rm 0.09^{+0.05}_{-0.05}$ & $6.4^{+2.2}_{-1.8}\times 10^{-6}$ & 406.0/407 \\ 
\hline
\end{tabular}
\tablefoot {The spectrum was obtained by combining the XIS0 and XIS3
  data. The model consists of a power law with a Gaussian for the Fe
  K$\alpha$~line, modified by warm and cold absorption. The cold
  absorption column is denoted by \nH, which is in excess of the
  Galactic column of $1.85\times 10^{20}$~\psqcm. Tim Kallman's XSTAR
  grid tables (``grid~25'') with the turbulent velocity of 200~km~s$^{-1}$ is adopted for the warm absorber modelling.}
\end{table}