\begin{table}%t2
\caption{\label{table:fit}EPIC--RGS spectral fits to the persistent emission.}
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\par
\par
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\begin{tabular}{lccc}
\hline\hline\noalign{\smallskip}
Par/component & OBS 1 & OBS 2 & Average value\\ 
\hline
 {\it absorber} & & & \\ 
$N_{\rm H}$ ~ ($10^{25} ~ {\rm m}^{-2}$) &  $ 3.65  \pm 0.05  $  &  $ 3.68  \pm 0.04  $   &  $ 3.67  \pm 0.03  $ \\ 
$kT$        ~     ($10^{-4}$ keV)         &  $ 7.07  \pm 0.10  $  &  $ 7.22  \pm 0.09  $   &  $ 7.15  \pm 0.07  $ \\ 
O          &  $ 1.471 \pm 0.008 $  &  $ 1.403 \pm 0.008 $   &  $ 1.437 \pm 0.006 $ \\ 
Ne         &  $ 2.72  \pm 0.04  $  &  $ 2.64  \pm 0.04  $   &  $ 2.68  \pm 0.03  $ \\ 
Mg         &  $ 0.81  \pm 0.09  $  &  $ 0.80  \pm 0.09  $   &  $ 0.80  \pm 0.06  $ \\ 
Fe         &  $ 1.90  \pm 0.03  $  &  $ 2.01  \pm 0.02  $   &  $ 1.98  \pm 0.02  $ \\ 
\hline                                        
{\it blackbody} & & & \\ 
 flux (10$^{-13}$ W m$^{-2}$) & 0.65 $\pm$ 0.10 & 0.55 $\pm$ 0.03 & 0.56 $\pm$ 0.03 \\ 
 $kT_{\rm bb}$ (keV)  &  $ 0.170 \pm 0.002 $      &  $ 0.167 \pm 0.002  $      &  $ 0.168 \pm 0.001 $ \\ 
\hline
{\it C1 comptonization}       & & & \\ 
 flux (10$^{-13}$ W m$^{-2}$) & 7.8 $\pm$ 0.3 & 7.7 $\pm$ 0.3 & 7.75 $\pm$ 0.21 \\ 
 $kT_{\rm s} $ \hspace{0.22cm}(keV)    &  $ 0.25  \pm 0.02  $      &  $ 0.24 \pm 0.01       $   &  $ 0.24  \pm 0.01  $ \\ 
 $kT_{\rm e} $ \hspace{0.22cm}(keV)    &  $ 2.07  \pm 0.05  $      &  $ 2.38 \pm 0.06       $   &  $ 2.20  \pm 0.04  $ \\ 
 $ \tau $        &  $ 11.0  \pm 0.6   $      &  $ 9.3  \pm 0.4        $   &  $ 9.8  \pm 0.3   $ \\   
\hline
{\it C2 comptonization}       & & & \\ 
 flux (10$^{-13}$ W m$^{-2}$) & 0.9 $\pm$ 0.1 & 0.6 $\pm$ 0.1 & 0.75 $\pm$ 0.07 \\ 
 $kT_{\rm s} $ \hspace{0.22cm}(keV)    &  $ 0.50  \pm 0.01    $    &  $ 0.54  \pm 0.01    $     &  $ 0.52  \pm 0.01  $ \\ 
 $kT_{\rm e} $ \hspace{0.22cm}(keV)    &  $ 9.4   \pm 0.8     $    &  $ 4.6   \pm 0.5     $     &  $ 5.9   \pm 0.4   $ \\ 
 $ \tau $        &  $\leq$0.5 &  $\leq$0.7   &  -- \\ 
\hline
% pn-rgs-1-2 N.
$C_{\rm stat}$ / d.o.f. & $2451 / 1705$ & $2579 / 1710$ & -- \\
\hline
\end{tabular}
\tablefoot{Abundances are relative to the protosolar values of \cite{Lodders}. Fluxes are derived in the 0.3--10~keV band. We also report the weighted averages between the two observations. See also Fig.~\ref{fig:epic_rgs_fit}.}
\end{table}