\begin{table}%t6
\caption{\label{table:5}Results of the $\chi^2$ fits to our source count distributions with a model with three power-laws.}
\par
\small%\centerline
 {
\begin{tabular}{c c c c c c c c }         
\hline\hline
Energy band &  ${\rm \Gamma_b}$     &  ${\rm \Gamma_i}$  &  ${\rm \Gamma_f}$ & $S_{\rm b}^{\rm b}$ & $S_{\rm b}^{\rm f}$ &$K$ & F-test \\
 (keV)   &  &  & & (${\rm 10^{-14}~cgs}$) &  (${\rm 10^{-14}~cgs}$) & (${\rm deg^2}$)  & prob. (\%)\\
 (1) & (2) & (3) & (4) & (5) & (6) & (7) & (8)\\
\hline 
0.5--1 & $\rm 2.34_{-0.02}^{+0.02}$ & $\rm 1.91_{-0.03}^{+0.02}$ & $\rm 1.56_{-0.06}^{+0.06}$ & $\rm 0.97_{-0.07}^{+0.06}$ & $\rm 0.31_{-0.02}^{+0.04}$  &$\rm 57.6_{-3.7}^{+4.9}$ & $\>$99.99  \\
1--2 & $\rm 2.51_{-0.02}^{+0.02}$ & $\rm 2.28_{-0.04}^{+0.04}$ & $\rm 1.74_{-0.03}^{+0.03}$ & $\rm 1.21_{-0.20}^{+0.15}$ & $\rm 0.52_{-0.01}^{+0.04}$ & $\rm 47.9_{-7.6}^{+12.4}$ & $\>$99.99  \\
2--4.5 & $\rm 2.72_{-0.03}^{+0.03}$ & $\rm 2.39_{-0.03}^{+0.04}$ & $\rm 1.93_{-0.22}^{+0.13}$ & $\rm 2.2_{-0.16}^{+0.19}$ & $\rm 0.72_{-0.08}^{+0.06}$  &$4\rm 0.4_{-5.9}^{+5.9}$ & $\>$97.3 \\
4.5--10& $\rm 2.72_{-0.03}^{+0.03}$ & --  & -- & -- & -- & $\rm 270.7_{-16.2}^{+17.2}$ \\
0.5--2 & $\rm 2.44_{-0.02}^{+0.03}$ & $\rm 2.10_{-0.04}^{+0.03}$ & $\rm 1.61_{-0.02}^{+0.03}$ & $\rm 2.42_{-0.22}^{+0.19}$ & $\rm 0.80_{-0.06}^{+0.04}$  &$\rm 46.0_{-4.0}^{+6.1}$ & $\>$99.99  \\
2--10 & $\rm 2.69_{-0.03}^{+0.02}$ & $\rm 2.40_{-0.04}^{+0.01}$ & $\rm 0.96_{-0.51}^{+0.40}$ & $\rm 4.09_{-0.69}^{+0.22}$ & $\rm 1.24_{-0.13}^{+0.04}$  &$\rm 60.2_{-3.4}^{+6.9}$ & $\>$94.3 \\
\hline                                   
\end{tabular}}
\medskip
 (1) Energy band definition (in keV). (2), (3) and (4) Power-law slopes at the 
brightest, intermediate and fainter fluxes respectively. 
(5)~and (6)~Flux breaks (in units of ${\rm 10^{-14}~erg~cm^{-2}~s^{-1}}$) at bright 
and faint fluxes. (7)~Normalisation of the model in each band. (8)~F-test significance of 
improvement of the quality of the fit with respect to a broken power-law model.
Errors are 1$\sigma$~uncertainty.
\end{table}