\begin{table}%t1
%\centering
\par
\caption{The best model fits to the MOS spectra of the source 52, and the MOS and PN spectra of \object{PSR~J0751+1807} and \object{PSR~J1012+5307}.  For \object{PSR~J0751+1807} the interstellar absorption ($N_{\rm H}$) was fixed at $4 \times 10{\rm^{20}}$~cm$^{-2}$.  For \object{PSR~J1012+5307} the $N_{\rm H}$ was fixed at $7 \times 10{\rm^{19}}$~cm$^{-2}$.  For source 52, $z$ was fixed at 0.255.  All the errors shown are 1$\sigma$ confidence limits.  The fluxes and luminosities are given for the 0.2--10.0~keV band.}
\label{tab:src52specfits}
\begin{tabular}{llcccccccc}
\hline
\hline
 Object & Spectral & $N_{\rm H}$ (cm$^{-2}$) & $kT$ & Photon & Abundance &
 $\chi^{ 2}_{ \nu}$ & d.o.f. & Flux
 ($\times 10^{-13}$) & Luminosity\\ & model & ($\times$10${\rm^{22}}$) & (keV) & Index & & & & (${\rm ergs~ cm}^{-2}~{\rm
 s}^{-1}$) & (${\rm ergs~s}^{-1}$)\\
\hline 
{\bf \object{PSR~J0751+1807}}  & Power law & 0.04 & -- & $1.59\pm0.20$ & -- & 1.33 & 14 & 0.44 & $2.1\times 10^{31}$ \\
 & Bremsstrahlung & 0.04 & $12.36\pm12.31$ & -- & & 1.52 & 14 & & \\
 & Blackbody & 0.04  & $0.32\pm0.04$ & -- & & 2.21 & 14 & &\\
\hline
{\bf Source 52}   & Power law & $0.13\pm0.06$ & -- & $1.46\pm0.13$ & -- & 0.86 & 32 & 2.0 & $1.9\times 10^{43}$\\
 & Bremsstrahlung & $0.09\pm0.05$ & $17.31\pm10.42$ & -- & & 0.87 & 32 & &\\
 & Raymond Smith & $0.07\pm0.04$ & $17.63\pm12.78$ & -- & $0.16\pm1.20$ & 0.89 & 31 & &\\
\hline
{\bf \object{PSR~J1012+5307}} & Power law & 0.007 & -- & $1.78\pm0.36$ & -- & 1.27 & 9 & 1.2 & $3.9\times 10^{30}$\\
 & Bremsstrahlung & 0.007 & $1.95\pm1.45$ & -- & & 1.29 & 9 & &\\
 & Blackbody & 0.007  & $0.26\pm0.04$ & -- & & 1.37 & 9 & & \\
\hline
\end{tabular}
\end{table}