\begin{table}%t3
\caption{\label{tab3}Spectral fits with an ionized absorber$^a$.}
%\begin{center}
{
\begin{tabular}{lccccc}
\hline
\hline
model & $N_{\rm H}^b$ 	& $z$ 	& $\xi^c$  	& $Z_{\rm Fe}^d$    	& 
$\chi^2$ (d.o.f.) \\ 
\hline
PL	& $0.26\pm0.05$	& 0~FIX  &  $\rm 0.21^{+0.50}_{-0.20}$  & 1FIX	& 
 134.7/143\\
BKNPL	&  $\rm 0.23^{+0.20}_{-0.10}$ & 0~FIX  & $<$0.8 &  1 FIX 		&  
 131.4/140\\
CUTOFFPL& $\rm 0.20^{+0.10}_{-0.06}$ & 0 FIX	& $<$1.0         & 1~FIX		& 
 126.5/142\\
\hline
PL	& $\rm 50^{+150}_{-25}$ & 3.27~FIX 	& $\rm 1800^{+2500}_{-1400}$ & $<$0.25&
 140.8/142\\
BKNPL	& $\rm 36^{+150}_{-24}$ &3.27~FIX& $\rm 1300^{+3700}_{-1100}$ & $<$0.25	&
 129.5/141\\
CUTOFFPL& $\rm 36^{+150}_{-24}$ & 3.27~FIX & $\rm 1700^{+3800}_{-1500}$ &  $<$0.3&
 127.6/141\\
\hline
\end{tabular}}
$^a$ Continuum fit values are indistinguishable from those in 
Table~\ref{tab2}.\\
$^b$ In $10^{22}$ cm$^{-2}$; $^c$ ionization parameter.
$^d$ Iron abundance in unit of the solar value.
%\end{center}
\par
\end{table}