\begin{table}%t3
\caption{\label{spectab} Spectral parameters for sufficiently bright sources.}
%\centerline
{
\begin{tabular}{clcccllccc}
\hline\hline
\multicolumn{1}{c}{1} & \multicolumn{1}{c}{2} & \multicolumn{1}{c}{3} &
\multicolumn{1}{c}{4} & \multicolumn{1}{c}{5} & \multicolumn{1}{c}{6} &
\multicolumn{1}{c}{7} & \multicolumn{1}{c}{8} & \multicolumn{1}{c}{9} & 
\multicolumn{1}{c}{10} \\
\hline
No. & \multicolumn{1}{c}{ID} & $\Gamma$ & $N_{\rm H}$ & $kT$ & 
\multicolumn{1}{c}{Abund.} & 
\multicolumn{1}{c}{Thermal} & $\chi^{2}$ & d.o.f. & No. \\
& & & [cm$^{-2}$] & [keV] & \multicolumn{1}{c}{(solar)} 
& \multicolumn{1}{c}{model} & & & \\
\hline
05 & 2E~0055.6--7241 & $\rm 2.59^{+0.16}_{-0.33}$ & $\rm 5.3^{+1.1}_{-0.8} 
\times 10^{21}$ & -- & \multicolumn{1}{c}{--} & -- & 41.4 & 51 & 2 \\
06 & XMMU~J005735.7--721932 & $\rm 1.42^{+0.25}_{-0.20}$ & $\rm 3.6^{+1.9}_{-1.5} 
\times 10^{21}$ & -- & \multicolumn{1}{c}{--} & -- & 84.6 & 63 & 4 \\
07 & AX~J0058--720          & $\rm 1.01^{+0.11}_{-0.11}$ & $\rm 3.4^{+5.9}_{-3.4} 
\times 10^{20}$ & -- & \multicolumn{1}{c}{--} & -- & 91.6 & 65 & 3 \\
08 & RX~J0057.8--7207       & $\rm 0.97^{+0.08}_{-0.07}$ & $\rm 3.0^{+0.8}_{-0.4} 
\times 10^{21}$ & -- & \multicolumn{1}{c}{--} & -- & 161.9 & 133 & 3 \\
10 & RX~J0059.3--7223       & $\rm 1.46^{+0.12}_{-0.13}$ & $\rm 1.8^{+0.7}_{-0.6} 
\times 10^{21}$ & -- & \multicolumn{1}{c}{--} & -- & 117.8 & 99 & 5 \\
11 & RX~J0100.2--7204       & $\rm 2.00^{+0.41}_{-0.26}$ & $\rm 1.7^{+0.9}_{-1.0} 
\times 10^{21}$ & -- & \multicolumn{1}{c}{--} & -- & 28.9 & 26 & 3 \\
14 & RX~J0101.3--7211       & $\rm 1.14^{+0.18}_{-0.13}$ & $\rm 3.3^{+2.4}_{-1.1} 
\times 10^{21}$ & $\rm 0.20^{+0.09}_{-0.06}$ & 
\multicolumn{1}{c}{$\rm 0.11^{+0.10}_{-0.11}$} & MEKAL 
& 82.6 & 56 & 2 \\
15 & RX~J0101.6--7204       & $\rm 1.73^{+0.15}_{-0.17}$ & $\rm 8.6^{+4.9}_{-5.6} 
\times 10^{20}$ & -- & \multicolumn{1}{c}{--} & -- & 68.0 & 58 & 6 \\
16 & AX~J0103--722          & $\rm 1.08_{-0.19}^{+0.12}$ & $\rm 1.9_{-1.7}^{+1.9} 
\times 10^{21}$ & $\rm 0.27_{-0.07}^{+0.08}$ & 
\multicolumn{1}{c}{$\rm 0.31_{-0.17}^{+0.43}$} & MEKAL 
& 172.7 & 155 & 3\\
17 & RX~J0103.6--7201 (Model 1) & $\rm 0.72_{-0.07}^{+0.06}$ & $\rm 1.7_{-0.9}^{+1.0} 
\times 10^{21}$ & $\rm 0.27_{-0.04}^{+0.03}$ & 
\multicolumn{1}{c}{$\rm 0.77_{-0.28}^{+0.17}$} & MEKAL 
& 295.1 & 240 & 3 \\
\noalign{\smallskip}
& \multicolumn{1}{r}{(Model 2)} & $\rm 0.71_{-0.06}^{+0.05}$ & $\rm 2.3_{-0.8}^{+0.8} \times 10^{21}$ & $\rm 0.32_{-0.05}^{+0.05}$ & $\rm 1.07_{-0.18}^{+0.57}$ (O) & VMEKAL & 272.9 & 238 & 3 \\
 & & & & & $\rm 1.61_{-0.66}^{+1.40}$ (Ne) & & & & \\
\hline
\end{tabular}}
\medskip
Notes to Col.~4:
Additional $N_{\rm H}$ to Galactic foreground $N_{\rm H, Gal}$ 
(see Eqs.~(\ref{power}) and~(\ref{powme})).  \\
Notes to Col.~9:
Degrees of freedom.  \\
Notes to Col.~10:
Number of used spectra.
\end{table}