\begin{table}%t2
\caption{\label{tab-fits}Spectral fit results.}
%%%\centerline
\par 
{
\begin{tabular}{lllllll}
\hline\hline\noalign{\smallskip}
\multicolumn{1}{l}{Source} &
\multicolumn{1}{c}{$\gamma$} &
\multicolumn{1}{c}{{\it kT}} &
\multicolumn{1}{c}{\nh} &
\multicolumn{1}{c}{SM$^4$} &
\multicolumn{1}{c}{Flux$^5$} &
\multicolumn{1}{c}{Luminosity$^6$} \\
\multicolumn{1}{l}{XMMU~J05...} &
\multicolumn{1}{c}{} &
\multicolumn{1}{c}{[keV]} &
\multicolumn{1}{c}{[\oexpo{21}cm$^{-2}$]} &
\multicolumn{1}{c}{} &
\multicolumn{1}{c}{[erg cm$^{-2}$ s$^{-1}$}] &
\multicolumn{1}{c}{[erg s$^{-1}$]} \\
\noalign{\smallskip}\hline\noalign{\smallskip}
 2924.3-655724 & &$ 0.68\pm0.08 $         & $<$0.1              & MK & 6.6\expo{-14} &\\
 2940.5-655318 & $\rm 2.33^{+0.13}_{-0.20}$ & & $\rm 1.3^{+0.2}_{-0.4}$ & PL & 9.6\expo{-14} &\\
 2947.4-655639 &$1.31 \pm 0.17 $        & &$2.6 \pm 1.0 $       & PL & 2.2\expo{-13} & 7.7\expo{34}\\
 3011.2-655122 &$1.07 \pm 0.06 $        & &$6.9 \pm 0.3 $       & PL & 1.2\expo{-12} & 3.9\expo{35}\\
 3034.9-655653 & & 0.7 fixed              & $\rm 1.9^{+0.8}_{-0.6}$ & MK & 1.9\expo{-14} & 1.2\expo{34}\\
\noalign{\smallskip}
 3041.0-660532 & $\rm 1.40^{+0.14}_{-0.11}$ & & $\rm 2.7^{+0.9}_{-0.7}$ & PL & 2.9\expo{-13} &\\
 3049.9-655522 & $\rm 2.00^{+0.20}_{-0.21}$ & & $\rm 1.4^{+0.5}_{-0.5}$ & PL & 5.1\expo{-14} &\\
 3056.2-654809$^1$ & & $\rm 0.049^{+0.006}_{-0.012}$ & $<$0.3           & BB & 4.2\expo{-14} & 1.3\expo{34}\\
 3102.5-660649$^2$ & $\rm 1.81^{+0.09}_{-0.07}$ & & $<$0.1          & PL & 2.3\expo{-13} &\\
 3113.3-660705 & $\rm 1.67^{+0.12}_{-0.13}$ &$ 0.10\pm0.02$ & $\rm 6.9^{+0.7}_{-1.3}$ / $\rm 97^{+3}_{-7}$ & MC & 7.0\expo{-12} & 4.6\expo{37}\\
\noalign{\smallskip}
 3137.2-660131 & & $0.66\pm0.16$          & $<$1.0              & MK & 1.6\expo{-14} &\\
 3150.9-655616 & $\rm 1.92^{+0.14}_{-0.07}$ & & $\rm 5.3^{+0.9}_{-0.7}$ & PL & 1.6\expo{-13} &\\
 3153.8-660217 & $\rm 2.07^{+0.20}_{-0.17}$ & & $2.8\pm0.6$ 	& PL & 1.0\expo{-13} &\\
 3153.9-654959 & $\rm 1.88^{+0.30}_{-0.26}$ & & $\rm 3.8^{+1.8}_{-1.2}$ & PL & 1.1\expo{-13} &\\
 3157.1-660233 & $\rm 1.62^{+0.14}_{-0.17}$ & & $\rm 3.8^{+1.0}_{-1.2}$ & PL & 1.4\expo{-13} &\\
\noalign{\smallskip}
 3226.2-655352 & & $0.68\pm0.06$          & $\rm 2.1^{+0.9}_{-0.6}$ & MK & 5.5\expo{-14} & 3.6\expo{34}\\
 3230.2-655735$^3$ & $\rm 2.23^{+0.20}_{-0.13}$ & & $\rm 0.7^{+0.3}_{-0.5}$ & PL & 6.3\expo{-14} &\\
 3232.4-655139 & $\rm 1.18^{+0.25}_{-0.29}$ & & $\rm 2.5^{+2.2}_{-1.5}$ & PL & 1.2\expo{-13} & 4.1\expo{34}\\
 3236.7-655551 & $\rm 2.02^{+0.19}_{-0.16}$ & & $\rm 1.3^{+0.5}_{-0.4}$ & PL & 1.1\expo{-13} &\\
 3243.9-660258 & & $0.52\pm0.18  $        & $<$0.4              & MK & 1.0\expo{-14} &\\
\hline
\end{tabular}}
\smallskip
$^1$ Spectral fit to pn spectrum only.\\
$^2$ The low absorption indicates a low energy excess which is probably caused by contamination from \exo.\\
$^3$ Located in arc structure caused by single reflected photons from nearby bright SNR which 
     probably causes contamination.\\
$^4$ Spectral model; MC: multi-component (see text), PL: power-law, BB: blackbody, MK: thermal emission from plasma in
     collisional equilibrium \citep[Mewe-Kaastra,][]{1985AetAS...62..197M}.\\
$^5$ 0.2--10 keV, determined from the pn spectrum except for \exo\ (MOS1) which is
     located on a CCD gap in the pn.\\
$^6$ 0.2--10 keV, intrinsic luminosity with \nh\ set to 0 for sources located in the LMC assuming 
     a distance of 50~kpc.
\end{table}