$\begin{figure} \par\mbox{\includegraphics[width=3.8cm,clip]{5882fig1.ps} \includegraphics[width=3.8cm,clip]{5882fig2.ps} } \end{figure}$ Figure 1: Images from a PN observation with the source holes removed prior to the ghosting procedure ( left) and after the ghosting procedure ( right). Although there are slight problems in the ghosting procedure in very source confused areas, no problems remain after stacking of several such filled event files.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,angle=180,clip]{5882fig3.ps}\end{figure}$ Figure 2: An image created from one of the final refilled event files for PN, thin filter, full-frame mode, between the energies of 7.8 keV and 8.2 keV. This shows the copper hole and the slight blurring of the edges of this feature due to the ghosting procedure.
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In the text

$\begin{figure} \par\mbox{\subfigure[MOS1 livetime histogram after cleaning, all ... ...servations]{ \includegraphics[width=.38\textwidth]{5882fig9.ps} }} \end{figure}$ Figure 3: Properties of all the files used to construct the MOS1 blank sky event files; a) histogram of livetimes, b) histogram of revolution numbers, c) fraction of time removed during cleaning, d) fraction of time removed per month, e) histogram of nH values in the direction of pointing for an observation and f) total livetime after cleaning per month.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=4.8cm]{5882fg10.ps} \includegrap... ...h=4.8cm]{5882fg20.ps} \includegraphics[width=4.8cm]{5882fg21.ps} } \end{figure}$ Figure 4: Flux histograms of the removed sources for each of the instrument-filter-mode combinations data sets, where M1 = MOS1, M2 = MOS2, F = full-frame mode, E = full-frame-extended mode, T = thin filter, M = medium filter and K = thick filter. The y-axis represents the number of sources removed from the data sets for a particular flux.
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In the text

$\begin{figure} \par\mbox{\hspace*{1.7cm}\subfigure[MOS1 thin filter, full-frame ... ...d-full-frame mode]{ \includegraphics[width=3.3cm]{5882fg35.ps} }} \end{figure}$ Figure 5: Images of the final unfilled event files for each instrument-filter-mode combination, between 0.3 keV and 12 keV for the PN and from between 0.2 keV and 12 keV for the MOS cameras. The PN event files for full-frame mode, with the medium or thin filters have been split into those events centred about the galactic centre, and those centred about the galactic anti-centre.
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In the text

$\begin{figure} \par\includegraphics[height=6.7cm, width=6.7cm, angle=270]{5882fg36.ps} \end{figure}$ Figure 6: Spectra plotted based on differences in count rate between 0.3 keV and 8 keV, for MOS1, in full-frame mode using the thin filter. Black shows the highest count rate, red is classed as the medium count rate spectrum, and green the lowest count rate spectrum.
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In the text

$\begin{figure} \par\includegraphics[height=7cm, width=7cm, angle=270]{5882fg37.p... ...\par\includegraphics[height=7cm, width=7cm, angle=270]{5882fg38.ps} \end{figure}$ Figure 7: MOS1 ( top) and PN ( bottom) (1.0-10 keV) spectra extracted from the full-frame, thin filter BG event files. The upper spectrum in each panel is extracted from the in-FOV region, while the lower spectrum shows the difference between the in-FOV spectrum and an extracted out-FOV spectrum, scaled to account for the difference in areas. Line features in the "difference'' spectra indicate the differences in distribution of fluorescent line emission across the detectors, as explained in the text.
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In the text

$\begin{figure} \par\includegraphics[height=7.8cm,width=7.8cm,angle=270]{5882fg39.ps}\end{figure}$ Figure 8: MOS1 background spectra based on events taken from different sky locations; centred on the galactic centre(black) and anti-centre(red), north(green) and south(blue) galactic poles.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=3.8cm,clip]{5882fig1.ps} \includegraphics[width=3.8cm,clip]{5882fig2.ps} } \end{figure}$	Figure 1: Images from a PN observation with the source holes removed prior to the ghosting procedure ( left) and after the ghosting procedure ( right). Although there are slight problems in the ghosting procedure in very source confused areas, no problems remain after stacking of several such filled event files.
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$\begin{figure} \par\includegraphics[width=7.4cm,angle=180,clip]{5882fig3.ps}\end{figure}$	Figure 2: An image created from one of the final refilled event files for PN, thin filter, full-frame mode, between the energies of 7.8 keV and 8.2 keV. This shows the copper hole and the slight blurring of the edges of this feature due to the ghosting procedure.
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$\begin{figure} \par\mbox{\subfigure[MOS1 livetime histogram after cleaning, all ... ...servations]{ \includegraphics[width=.38\textwidth]{5882fig9.ps} }} \end{figure}$	Figure 3: Properties of all the files used to construct the MOS1 blank sky event files; a) histogram of livetimes, b) histogram of revolution numbers, c) fraction of time removed during cleaning, d) fraction of time removed per month, e) histogram of nH values in the direction of pointing for an observation and f) total livetime after cleaning per month.
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$\begin{figure} \par\mbox{\includegraphics[width=4.8cm]{5882fg10.ps} \includegrap... ...h=4.8cm]{5882fg20.ps} \includegraphics[width=4.8cm]{5882fg21.ps} } \end{figure}$	Figure 4: Flux histograms of the removed sources for each of the instrument-filter-mode combinations data sets, where M1 = MOS1, M2 = MOS2, F = full-frame mode, E = full-frame-extended mode, T = thin filter, M = medium filter and K = thick filter. The y-axis represents the number of sources removed from the data sets for a particular flux.
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$\begin{figure} \par\mbox{\hspace*{1.7cm}\subfigure[MOS1 thin filter, full-frame ... ...d-full-frame mode]{ \includegraphics[width=3.3cm]{5882fg35.ps} }} \end{figure}$	Figure 5: Images of the final unfilled event files for each instrument-filter-mode combination, between 0.3 keV and 12 keV for the PN and from between 0.2 keV and 12 keV for the MOS cameras. The PN event files for full-frame mode, with the medium or thin filters have been split into those events centred about the galactic centre, and those centred about the galactic anti-centre.
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$\begin{figure} \par\includegraphics[height=6.7cm, width=6.7cm, angle=270]{5882fg36.ps} \end{figure}$	Figure 6: Spectra plotted based on differences in count rate between 0.3 keV and 8 keV, for MOS1, in full-frame mode using the thin filter. Black shows the highest count rate, red is classed as the medium count rate spectrum, and green the lowest count rate spectrum.
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$\begin{figure} \par\includegraphics[height=7.8cm,width=7.8cm,angle=270]{5882fg39.ps}\end{figure}$	Figure 8: MOS1 background spectra based on events taken from different sky locations; centred on the galactic centre(black) and anti-centre(red), north(green) and south(blue) galactic poles.
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