Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3838.f01.eps}\end{figure}$ Figure 1: The effects of high background flaring: The usable fraction of data available after flare-screening is shown for all the datasets analysed.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{3838.f02.ps}\end{figure}$ Figure 2: A non-vignetted (4 $^\prime$ $^\prime$ ) exposure map is multiplied by a source-removed (4 $^\prime$ $^\prime$ ) mask map and rebinned to create a large-scale (1 $^\prime$ ) "area-times-exposure'' map (example is for PN).
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In the text

$\begin{figure} \par\includegraphics[width=5.7cm,clip]{3838.f03a.ps}\includegraph... ...,clip]{3838.f03b.ps}\includegraphics[width=5.7cm,clip]{3838.f03c.ps}\end{figure}$ Figure 3: Histogram distributions for the 72 clean observations of (from left to right) the observation revolution number, the Galactic hydrogen column, and the live exposure time (after cleaning for high background times) for M1 (thick line) and PN (filled region).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{3838.f04.ps}\end{figure}$ Figure 4: A 3D "imagecube'' of dimensions DETX, DETY and $N_{{\rm obs}}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{3838.f05.ps} .\end{figure}$ Figure 5: A 3D "clipcube'' of dimensions DETX, DETY and $N_{{\rm obs}}$ . In this example, for ${\rm DETX/DETY}=(1,1)$ , the value in image 1 is outside of the allowable range, and is to be clipped from the calculation of the mean value for ${\rm DETX/DETY}=(1,1)$
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In the text

$\begin{figure} \par\includegraphics[width=17.7cm,clip]{3838.f06.ps}\end{figure}$ Figure 6: The final $\sigma$ -clipped, averaged, and exposure-corrected background maps, for MOS1, full-frame mode. Energy band 0 (full-band), then bands 1-5 run from left to right. Rows 1-3 are for medium filter and show (row 1) the particle and photon combined (cim) maps, (row 2) the particle (cpaim) maps, and (row 3) the photon (cphim) maps. Rows 4-6 show the equivalent maps for thin filter. All 0-band maps are to the same level of scaling. All other maps are to a scaling 1/3 that of the 0-band maps. Note that at the very edges of the photon (and combined) map FOVs, there are sometimes a few pixels with unusually large or small values. This is due to extremely small exposure values in the original observation maps amplifying the noise.
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In the text

$\begin{figure} \par\includegraphics[width=17.7cm,clip]{3838.f07.ps}\end{figure}$ Figure 7: The final $\sigma$ -clipped, averaged, and exposure-corrected background maps, as for Fig. 6, but for MOS2, full-frame mode.
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In the text

$\begin{figure} \par\includegraphics[width=17.7cm,clip]{3838.f08.ps}\end{figure}$ Figure 8: The final $\sigma$ -clipped, averaged, and exposure-corrected background maps, as for Fig. 6, but for pn, full-frame mode.
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In the text

$\begin{figure} \par\includegraphics[width=17.7cm,clip]{3838.f09.ps}\end{figure}$ Figure 9: The final $\sigma$ -clipped, averaged, and exposure-corrected background maps, as for Fig. 6, but for pn, extended full-frame mode.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3838.f10.ps}\end{figure}$ Figure 10: (Thick line) the M1 0-band full-frame thin filter photon count rate distribution, and (filled region) the PN 0-band full-frame-extended thin filter photon count rate distribution
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In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{3838.f11.ps}\end{figure}$ Figure 11: Usage of BGrebinimage2SKY to rebin and sky-project a given low-resolution DETX/Y background map (top left, specifically the M1 thin-filter 0-band particle background map from Fig. 6) to the spatial binning and sky position of a user-created high-resolution sky image (top right). The resultant high-resolution sky background image is shown at the bottom. The dark areas in the background map are due mainly to CCD gaps.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=16.5cm,clip]{3838.f12.ps}\end{figure}$ Figure 12: Flux histograms of the detected and thereafter removed sources for each of the instrument/mode/filter combinations. (Top) Thin filter: MOS1, MOS2 and pn full-frame, pn full-frame extended. (Bottom) the same but for medium filter. All plots are to the same scale.
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In the text

$\begin{figure} \par\includegraphics[angle=90,width=15.5cm,clip]{3838.f13.eps}\end{figure}$ Figure 13: 4 $^\prime$ $^\prime$ resolution DETX/DETY (see Table 2) exposure maps for the background event files in each of the instrument/mode/filter combinations. (Top) Thin filter: MOS1, MOS2 and pn full-frame, pn full-frame extended. (Bottom) the same but for medium filter.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3838.f01.eps}\end{figure}$	Figure 1: The effects of high background flaring: The usable fraction of data available after flare-screening is shown for all the datasets analysed.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{3838.f02.ps}\end{figure}$	Figure 2: A non-vignetted (4 $^\prime$ $^\prime$ ) exposure map is multiplied by a source-removed (4 $^\prime$ $^\prime$ ) mask map and rebinned to create a large-scale (1 $^\prime$ ) "area-times-exposure'' map (example is for PN).
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$\begin{figure} \par\includegraphics[width=5.7cm,clip]{3838.f03a.ps}\includegraph... ...,clip]{3838.f03b.ps}\includegraphics[width=5.7cm,clip]{3838.f03c.ps}\end{figure}$	Figure 3: Histogram distributions for the 72 clean observations of (from left to right) the observation revolution number, the Galactic hydrogen column, and the live exposure time (after cleaning for high background times) for M1 (thick line) and PN (filled region).
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$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{3838.f04.ps}\end{figure}$	Figure 4: A 3D "imagecube'' of dimensions DETX, DETY and $N_{{\rm obs}}$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=18cm,clip]{3838.f05.ps} .\end{figure}$	Figure 5: A 3D "clipcube'' of dimensions DETX, DETY and $N_{{\rm obs}}$ . In this example, for ${\rm DETX/DETY}=(1,1)$ , the value in image 1 is outside of the allowable range, and is to be clipped from the calculation of the mean value for ${\rm DETX/DETY}=(1,1)$
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$\begin{figure} \par\includegraphics[width=17.7cm,clip]{3838.f07.ps}\end{figure}$	Figure 7: The final $\sigma$ -clipped, averaged, and exposure-corrected background maps, as for Fig. 6, but for MOS2, full-frame mode.
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$\begin{figure} \par\includegraphics[width=17.7cm,clip]{3838.f08.ps}\end{figure}$	Figure 8: The final $\sigma$ -clipped, averaged, and exposure-corrected background maps, as for Fig. 6, but for pn, full-frame mode.
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$\begin{figure} \par\includegraphics[width=17.7cm,clip]{3838.f09.ps}\end{figure}$	Figure 9: The final $\sigma$ -clipped, averaged, and exposure-corrected background maps, as for Fig. 6, but for pn, extended full-frame mode.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3838.f10.ps}\end{figure}$	Figure 10: (Thick line) the M1 0-band full-frame thin filter photon count rate distribution, and (filled region) the PN 0-band full-frame-extended thin filter photon count rate distribution
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$\begin{figure} \par\includegraphics[angle=-90,width=16.5cm,clip]{3838.f12.ps}\end{figure}$	Figure 12: Flux histograms of the detected and thereafter removed sources for each of the instrument/mode/filter combinations. (Top) Thin filter: MOS1, MOS2 and pn full-frame, pn full-frame extended. (Bottom) the same but for medium filter. All plots are to the same scale.
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$\begin{figure} \par\includegraphics[angle=90,width=15.5cm,clip]{3838.f13.eps}\end{figure}$	Figure 13: 4 $^\prime$ $^\prime$ resolution DETX/DETY (see Table 2) exposure maps for the background event files in each of the instrument/mode/filter combinations. (Top) Thin filter: MOS1, MOS2 and pn full-frame, pn full-frame extended. (Bottom) the same but for medium filter.
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