\begin{table}%t3
\par
\caption {\label{xmmtab} Summary of the spectral results.
The EPIC-pn/ACIS-S net counts are derived in a circle of radius $r_{\rm ext}$, given in
the third column. 
}
%\centerline
 { \begin{tabular}{ccccccccccc}
\hline 
\hline
\noalign{\smallskip}
Source  &  $N_{\rm H_{gal}}$ & $r_{\rm ext}$ 
  & cts & ${\it kT}_{\rm mekal}$ & $\Gamma$ & $N_{\rm H_{int}}$  &
  $\chi^{2}/\rm d.o.f.$ & $L_{\rm mekal
 (0.5{-}2.0)}$ & $L_{\rm po(2.0{-}10)}$ & $L_{\rm LMXBs}^{***}$ \\
 &  cm$^{-2}$ & $\arcsec$ & pn/ACIS-S & keV & & cm$^{-2}$ & & erg~s$^{-1}$ & erg~s$^{-1}$ & 
 erg~s$^{-1}$\\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
NGC~2954       & $3.43 \times 10^{20}$ & 30  & $132 \pm 19$  &  --  &  $1.9\pm 0.3$ & -- & $10.36/12$  & -- & $3.2 \times 10^{39}$  & $1.1 \times 10^{40}$  \\
NGC~2954       & $3.43 \times  10^{20}$ & 30  & $132 \pm 19$  &  0.54  & 1.9$^{*}$  & -- & $8.10/11$  &  ${5.4 \times 10^{38}}^{**}$ & $2.5 \times 10^{39}$  & $1.1 \times 10^{40}$\\
\noalign{\smallskip}
NGC~7052            & $13.6 \times 10^{20}$  &  50  &  $719\pm 30$ &  $0.48\pm0.06$  &  1.4$^{+0.4}_{-0.8}$ &  & $47/48$ & $1.4 \times 10^{41}$ &  $5.3 \times 10^{40}$ & 
$4.5 \times 10^{40}$ \\
NGC~7052            & $13.6 \times 10^{20}$  &  50  &  $719\pm 30$ &  
$0.48\pm 0.06$  &  1.9$^{*}$ & $9^{+1.1}_{-0.7} \times 10^{21}$ & $46/48$ & $1 \times 10^{41}$ &  
$5 \times 10^{40}$ & $4.5 \times 10^{40}$ \\
\noalign{\smallskip}
\noalign{\smallskip}
NGC~7785             &  $5.24 \times 10^{20}$  &  120  & 
$3340 \pm 87$  &  $0.56 \pm 0.02$  & $2.0 \pm 0.3$  & -- & $263/254$ & $8 \times 10^{40}$ &  
$2.0  \times 10^{40}$  & $3.0 \times 10^{40}$ \\
\hline
\end{tabular}}
\par
\smallskip
$^{\rm *}$ { Fixed;
$^{\rm **}$ note that this is not a statistically
significant component. We use it to derive an upper limit of 
$L_{\rm X}  \le 1.5 \times 10^{39}$~erg~s$^{-1}$  for the plasma component (see text for details);} 
 $^{\rm ***}$   { $L_{\rm (2.0{-}10)}$ expected from LMXBs,
calculated using the relation in Kim \& Fabbiano (\cite{Kim04}),
taking into account the appropriate $K$-band luminosity and energy range.} 
\end{table}