\begin{table}%t1

\caption{Results of modeling the BeppoSAX-NFI and XMM-Newton spectra (last entry) with a combination of a disk black body model (Mitsuda et~al. 1984; Makishima et~al. 1986), Comptonization of soft photons in a hot plasma (Titarchuk 1991), and a narrow emission line.}{\label{tab1}}
%\centerline
 {\begin{tabular}{p{4.5cm}p{1cm}p{10cm}p{4.5cm}p{3.5cm}}
\hline
\hline
Observation date in 2000 & Exposure$^\ddag$ & Model Parameters$^\ast$ & 2--10 and 0.3--10 keV unabs. flux$^\dagger$ & $\chi^{2}_{\nu}$ (d.o.f.)\\
\hline
Mar. 13.19-13.85 & 21.4 ks& 
      \makebox[7cm][l]{$N_{\rm H}=8.8^{+0.6}_{-0.3}$}
      \makebox[7cm][l]{$kT_{\rm in}=1.9\pm0.1$,
          $R_{\rm in}^{2}\cos\theta=16.5^{+2.5}_{-1.0}$}
      \makebox[7cm][l]{$kT_{0}=0.48^{+0.03}_{-0.20}$,
          $kT_{\rm e}=\rm unconstrained$,
          $\tau<3$}
      \makebox[7cm][l]{$E_{\rm line}=6.82\pm0.06$,
          $EW=35$ eV, $f=(9.2\pm2.1)$ }
    & $3.9\times10^{-9}$ \hfill (79)  $5.9\times10^{-9}$ \hfill ~ 
    & 0.96 (70) \\\noalign{\medskip}
Mar. 16.71-17.48 & 34.4 ks & \makebox[7cm][l]{$N_{\rm H}=9.3^{+0.7}_{-0.3}$}
      \makebox[7cm][l]{$kT_{\rm in}=1.83\pm0.02$,
          $R_{\rm in}^{2}\cos\theta=14.4^{+1.8}_{-0.9}$}
      \makebox[7cm][l]{$kT_{0}=0.4\pm0.1$, $kT_{\rm e}=\rm unconstrained$,
          $\tau<0.2$}
      \makebox[7cm][l]{$E_{\rm line}=6.78^{+0.07}_{-0.05}$,
          $EW=41$ eV, $f=8.6^{+0.6}_{-2.1}$}
    & $3.0\times10^{-9}$\hfill  (82) $4.6\times10^{-9}$\hfill ~
    & 1.09 (73)\\\noalign{\medskip}
Mar. 27.63-28.45 & 36.6 ks & \makebox[7cm][l]{$N_{\rm H}=8.8^{\P}$}
      \makebox[7cm][l]{$kT_{\rm in}=1.87^{+0.02}_{-0.07}$,
          $R_{\rm in}^{2}\cos\theta=7.3^{+5.5}_{-0.6}$}
      \makebox[7cm][l]{$kT_{0}=0.41^{+0.04}_{-0.05}$, $kT_{\rm e}= \rm unconstrained$,
          $\tau=\rm unconstrained$}
      \makebox[7cm][l]{$E_{\rm line}=6.53^{+0.08}_{-0.07}$, $EW=33.2$ eV,
         $f=4.1^{+1.1}_{-1.0}$} 
    & $1.7\times10^{-9}$\hfill  (80) $2.6\times10^{-9}$ \hfill  ~
    & 1.04 (70)\\\noalign{\medskip}
Apr. 7.09-7.82 & 27.9 ks & \makebox[7cm][l]{$N_{\rm H}=8.8^{\P}$}
      \makebox[7cm][l]{$kT_{\rm in}=0.43\pm0.04$,
          $R_{\rm in}^{2}\cos\theta=340^{+280}_{-160}$}
      \makebox[7cm][l]{$kT_{0}=0.16^{+0.02}_{-0.01}$, $kT_{\rm e}=\rm unconstrained$,
          $\tau=\rm unconstrained$}
      \makebox[7cm][l]{$E_{\rm line}=6.75^{+0.03}_{-0.06}$, $EW=285$ eV,
         $f=1.31^{+0.19}_{-0.17}$}
    & $9.3\times10^{-11}$\hfill  (17)  $4.3\times10^{-10}$ \hfill ~
    & 1.00 (55)\\\noalign{\medskip}
Apr. 12.82-14.40 & 57.2 ks & \makebox[7cm][l]{$N_{\rm H}=8.8^{\P}$}
      \makebox[7cm][l]{$kT_{\rm in}=2.9\pm0.3$,
          $R_{\rm in}^{2}\cos\theta=0.20\pm0.04$}
      \makebox[7cm][l]{$kT_{0}<1.3$, $kT_{\rm e}=\rm unconstrained$,
          $\tau=\rm unconstrained$}
      \makebox[7cm][l]{$E_{\rm line}=6.56^{+0.09}_{-0.03}$, $EW=58.5$ eV,
         $f=2.3^{+0.4}_{-0.3}$}
    & $4.0\times10^{-10}$ \hfill (58) $7.1\times10^{-10}$ \hfill ~
    & 1.02 (64)\\\noalign{\medskip}
Sept. 21.39-21.63 & MOS\quad \mbox{16.7~ks},\quad EPIC-pn 7.6 ks &
      \makebox[7cm][l]{$N_{\rm H}=8.8^{\P}$}
      \makebox[7cm][l]{$kT_{\rm in}=0.3\pm0.1$,
         $R_{\rm in}^{2}\cos\theta=7.0^{+59}_{-0.6}\times10^{2}$}
      \makebox[7cm][l]{$kT_{0}=0.6\pm0.1$, $kT_{\rm e}=39^{+128}_{-7}$,
          $\tau=0.15^{+0.42}_{-0.10}$}
    & $8.7\times10^{-11}$\hfill  (1) $6.6\times10^{-10}$\hfill ~
    & 1.38 (139)\\
\hline
\end{tabular}}
\noindent
$^\ddag$ Net exposure time as it applies to the MECS data;\\
 $^\ast$
Parameters and units: $N_{\rm H}$: hydrogen column density in units of
10$^{22}$ cm$^{-2}$; $kT_{\rm in}$: temperature at inner disk radius in
keV; $R_{\rm in}^{2}\cos\theta$: $\theta$ is the disk inclination angle,
$R_{\rm in}$ is the disk inner radius in kilometers for a source at 10
kpc; $kT_{0}$: temperature of the Comptonized soft seed photons in
keV; $kT_{\rm e}$: temperature of the electron plasma in keV; $\tau$:
optical depth of the plasma; $E_{\rm line}$: centroid energy of Gaussian
line profile in keV; {\it EW}: equivalent width of the line; $f$: line flux
in $10^{-4}$ phot~s$^{-1}$ cm$^{-2}$.\\ $^\dagger$ Unabsorbed flux in
units of ergs~cm$^{-2}$~s$^{-1}$. The typical uncertainty in this
number is 10\% for 2--10 keV and a factor of 2 for 0.3--10~keV. The
number between parentheses refers to the fraction in percents of
detected photons coming from the blackbody component.\\ $^{\P}$ The
value was frozen.
\end{table}