\begin{table}
\caption{\label{tab5}The second part of Table~\ref{tab_intercal}.}
\small%\centerline
 {
\begin{tabular}{ccccccc|c c c|c}
\hline \hline
Mode & Grade & Source  & Model  & $N_{\rm H}$ & $\Gamma$ or/and &
$F_{{\rm Obs}}$ [0.3--10 keV] &  & {\it XMM-Newton} results & & {\it RXTE} results\\
    & & & & ($\times 10^{22}$ cm$^{-2}$) & $kT$ (keV) & ($\times 10^{-11}$
erg cm$^{-2}$ s$^{-1}$) & PN & MOS1 & MOS2 & \\
\hline
WT & 0--2 & 3C 273 & {\scriptsize WABS(POW} & 0.0179 fixed & $1.57 \pm 0.04$ &  & $1.646 \pm 0.011$ & $1.500 \pm 0.028$ & $1.533 \pm 0.025$ & $1.62\pm 0.03$ \\
&  &  &{\scriptsize+2*zBBODY}) &  & $0.050\pm 0.030$ &  & $0.074 \pm 0.003$ & $0.089 \pm 0.004$ & $0.072 \pm 0.004$ &  \\
&  &  & &  & $0.136\pm 0.060$ &  & $0.186 \pm 0.011$ & $0.304 \pm 0.015$ &
$0.266 \pm 0.014$ &  \\
&  &  & &  & & $16.1\pm 0.3$  & $14.7 \pm 0.1$ & $15.3 \pm 0.1$ & $15.3 \pm 0.14$ &  \\
&  &  & &  & & $10.2\pm 0.2$$^\dagger$  & $8.5 \pm 0.1$$^\dagger$ & $9.5 \pm
0.1$$^\dagger$ & $9.3 \pm 0.1$$^\dagger$ &  $10.2\pm 0.1$$^\dagger$ \\
WT & 0 &  & &  & $1.56\pm 0.04$ &  & & & &  \\
&  &  & &  & $0.046\pm 0.030$ &  & & &  &  \\
&  &  & &  & $0.129\pm 0.090$ &  & & & &  \\
&  &  & &  & & $\rm 16.5^{+0.3}_{-0.4}$  & & & &  \\
&  &  & &  & & $10.2\pm 0.2$$^\dagger$  & & & &  \\
\hline
\end{tabular}}
\medskip
$^*$ The abundance parameter was left as a free parameter. \\
$^{**}$ The spectra were extracted using a 40~arcsec radius circle  for both {\it Swift}-XRT and {\it XMM-Newton} data. Extended source ARFs were specially created to fit the XRT~spectra. \\
$^\dagger$ The values of the observed flux are given in the 2$-$10~keV energy range. \\
$^{c}$ The model is {\scriptsize CONST*TBABS(BBODYRAD+BBODYRAD)}  (see Beuermann et~al. \cite{Beue06}). All the parameters are fixed  ($N_{\rm H}=1.1$~$\times$ $10^{20}~{\rm cm}^{-2}$, $kT_1 = 62.8$~eV and $kT_2 = 32.3$~eV) except the constant factor. The lowest temperature black-body component has a minor impact in the XRT~energy range. It was introduced by Beuermann et~al. (\cite{Beue06}) to fit the EUVE data as well as the Chandra data. \\
$^\ddagger$ Values of the constant factor for the model described  in Beuermann et~al. (\cite{Beue06}).
\end{table}