\begin{table}%t5
  \caption{\label{table:model}Best-fit values of the parameters obtained fitting the emission features with relativistic smeared lines (diskline in XSPEC). The Fe-K$\alpha$ 
feature is modelled with one diskline component.}
%\centerline
{\begin{tabular}{l c c c }          
\hline\hline                       
Aver. spectrum&
Spectrum 1+3&
Spectrum 2\\
\hline \noalign{\smallskip}                       
$N_{\rm H}$  (10$^{22}$ cm$^{-2}$)&  
$0.735 \pm 0.004$&
0.735 (fixed)  &
0.735 (fixed)
\\
&\\
$kT_{\rm BB}$ (keV)         &
$1.797^{\rm +0.016}_{-0.007}$&
$1.780^{\rm +0.023}_{-0.009}$&
$1.818^{\rm +0.013}_{-0.010}$\\
 $N_{\rm BB}$ (10$^{-1}$) &
$1.048^{\rm +0.004}_{-0.013}$&
$0.924^{\rm +0.013}_{-0.017}$&
$1.126^{\rm +0.007}_{-0.009}$\\
&\\
$kT_{\rm DIS~KBB}$ (keV)         &
$1.049^{\rm +0.028}_{-0.014}$&
$1.08^{\rm +0.03}_{-0.02}$&
$1.05 \pm 0.02$\\
$N_{\rm DIS~KBB}$  &
$207^{\rm +9}_{-20}$&
$213^{\rm +14}_{-18}$&
$190^{\rm +5}_{-12} $\\
&\\
$E_{1~{\rm keV}}$ (keV) &
$1.052^{\rm +0.006}_{-0.009}$&
 $1.030^{\rm +0.009}_{-0.016}$  &
 $1.062^{\rm +0.004}_{-0.009}$  \\
$\sigma_{1~{\rm keV}}$ (eV) &
$85^{\rm +13}_{-7}$   &
$120^{\rm +20}_{-8}$  &
$66^{\rm +10}_{-7}$  \\
$I_{1~{\rm keV}}$  & 
$24^{\rm +4}_{-2}$   &
$42^{\rm +8}_{-4}$   &
$17.0^{\rm +2.1}_{-1.4}$   \\
Equiv. width (eV) & 
$22 \pm 2$  &
$32 \pm 2$  &
$17 \pm 2$  \\
&&\\
$\beta$  emiss. index& 
$-2.1 \pm 0.2               $ &
$-2.10^{\rm +0.12}_{-0.23} $ &
$-2.10^{\rm +0.11}_{-0.16}$ \\
$R_{\rm in}$ ($R_{\rm g}$) & 
$6.2^{\rm +19.1}_{-0.2}$ &
$6.6^{\rm +12.2}_{-0.6}$ &
$10^{\rm +14}_{-4}$ \\
$R_{\rm out}$ ($R_{\rm g}$) & 
$1980^{\rm +2900}_{-710}$&
1980 (fixed)&
1980 (fixed)
 \\
$\theta$ (degrees)   &
$41.4^{\rm +1.0}_{-2.1}$  &
41.4 (fixed)&
41.4 (fixed)\\
&\\
$E_{{\rm S} \; {\rm XVI}}$ (keV) &
2.62 (fixed)  &
2.62 (fixed)  &
2.62 (fixed)  \\
%($10^{-3}$ ph cm$^{-2}$ s$^{-1}$)
$I_{{\rm S} \; {\rm XVI}}$   &
$2.2^{\rm +0.5}_{-0.9}$  &
$3.4^{\rm +0.9}_{-1.0}$  &
$0.9 \pm 0.6$  \\
Equiv. width (eV) & 
$5 \pm 3$  &
$8^{\rm +4}_{-3} $  &
$2^{\rm +3}_{-2} $  \\
&\\
$E_{{\rm Ar \; XVIII}}$ (keV) &
$3.29 \pm 0.03$  &
$3.32 \pm 0.02$  &
$3.28^{\rm +0.02}_{-0.04}$  \\
$I_{{\rm Ar} \; {\rm XVIII}}$    &
$3.5^{\rm +0.5}_{-0.6}$ & 
$3.8^{\rm +0.9}_{-1.1}$  &
$2.7^{\rm +0.6}_{-0.8} $  \\
Equiv. width (eV) & 
$11 \pm 4$  &
$12 \pm 4 $  &
$9 \pm 4$  \\
&\\
$E_{{\rm Ca} \; {\rm XIX}}$ (keV) &
$3.89 \pm 0.03$ &
$3.89^{\rm +0.03}_{-0.04}$ &
$3.90 \pm 0.03$ \\
$I_{{\rm Ca} \; {\rm XIX}}$  & 
$3.6^{\rm +0.5}_{-0.7}$   &
$3.5 \pm 0.9$   &
$3.2 \pm 0.7$   \\
Equiv. width (eV) & 
$15 \pm 4$  &
$15 \pm 5$  &
$13 \pm 5$  \\
&\\
$E_{{\rm Fe} \; {\rm XXV}}$ (keV) &
$6.76 \pm 0.02$ &
$6.74 \pm 0.04$ &
$6.78 \pm 0.03$ \\
$I_{{\rm Fe} \; {\rm XXV}}$  & 
$5.7^{\rm +0.5}_{-0.6}$   &
$5.5 \pm 0.8$   &
$5.8^{\rm +0.7}_{-0.8}$   \\
Equiv. width (eV) & 
$61 \pm 9$  &
$64 \pm 11$  &
$59 \pm 11$  \\
&\\
$\chi_{\rm red}^2({\rm d.o.f.})$ &
$1.47(268)$  &
$1.24(271)$  &
$1.30(271)$  \\\noalign{\smallskip}
 \hline                                            
\end{tabular}}
\par
Note.    Uncertainties are  at the  90\% 
confidence
    level for a single parameter.   
The parameters are defined as in XSPEC. The continuum emission is fitted with 
a {\tt blackbody} plus a multicolored disk blackbody, {\tt diskbb}. 
The four broad emission features are modelled adopting {\tt diskline} 
components.  All components are subject to interstellar absorption. 
The intensity of the lines are in units of 10$^{-3}$~ph~cm$^{-2}$ s$^{-1}$.
\end{table}