$\begin{figure} \par\includegraphics[width=8.2cm,clip]{ms0053f1.ps}\end{figure}$ Figure 1: EPIC pn+MOS1+MOS2 light curves of the background-subtracted count rate in the 0.8-10 keV band (top panel) and of the X-ray color 1.8-10 keV/0.8-1.5 keV (bottom panel). The extraction radius is 35 $^{\prime \prime }$ ; time bins are 3000 s. The dashed lines indicate the average values.
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In the text

$\begin{figure} \par\psfig{figure=ms0053f2a.ps,height=6.2cm,width=8.7cm,% bbllx=7... ...,% bbllx=384pt,bblly=17pt,bburx=570pt,bbury=704pt,angle=-90,clip=} \end{figure}$ Figure 2: EPIC pn unfolded spectrum of NGC 6251 described by a thermal component plus an absorbed power law. The lower panels show the data-to-model ratio for the pn, MOS1, and MOS2 cameras, respectively. The edge at 0.53 keV in the top panel is due to neutral oxygen in the absorbing material.
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In the text

$\begin{figure} { \psfig{figure=ms0053f4a.ps,height=4.cm,width=8cm,% bbllx=81pt,b... ... bbllx=81pt,bblly=20pt,bburx=590pt,bbury=720pt,angle=-90,clip=} } \end{figure}$ Figure 4: Top panel: EPIC pn data-to-model ratio from 2-10 keV of the best-fit continuum model for the EPIC pn data. Bottom panel: same as above but with a Gaussian line included. Energies are in the observer's frame.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{ms0053f1.ps}\end{figure}$	Figure 1: EPIC pn+MOS1+MOS2 light curves of the background-subtracted count rate in the 0.8-10 keV band (top panel) and of the X-ray color 1.8-10 keV/0.8-1.5 keV (bottom panel). The extraction radius is 35 $^{\prime \prime }$ ; time bins are 3000 s. The dashed lines indicate the average values.
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$\begin{figure} \par\psfig{figure=ms0053f2a.ps,height=6.2cm,width=8.7cm,% bbllx=7... ...,% bbllx=384pt,bblly=17pt,bburx=570pt,bbury=704pt,angle=-90,clip=} \end{figure}$	Figure 2: EPIC pn unfolded spectrum of NGC 6251 described by a thermal component plus an absorbed power law. The lower panels show the data-to-model ratio for the pn, MOS1, and MOS2 cameras, respectively. The edge at 0.53 keV in the top panel is due to neutral oxygen in the absorbing material.
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$\begin{figure} \par\psfig{figure=ms0053f3a.ps,height=6.2cm,width=8.7cm,% bbllx=7... ...,% bbllx=384pt,bblly=17pt,bburx=570pt,bbury=704pt,angle=-90,clip=} \end{figure}$	Figure 3: EPIC pn unfolded spectrum of NGC 6251 and data-to-model ratio. The spectral model is wabs(apec+apec+zwabs (powerlaw+zgauss)).
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$\begin{figure} { \psfig{figure=ms0053f4a.ps,height=4.cm,width=8cm,% bbllx=81pt,b... ... bbllx=81pt,bblly=20pt,bburx=590pt,bbury=720pt,angle=-90,clip=} } \end{figure}$	Figure 4: Top panel: EPIC pn data-to-model ratio from 2-10 keV of the best-fit continuum model for the EPIC pn data. Bottom panel: same as above but with a Gaussian line included. Energies are in the observer's frame.
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