All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{7930-01.ps} \end{figure}$ Figure 1: Filter wheel closed spectra for the MOS1 ( upper) and MOS2 ( lower) detectors. The MOS2 data have been scaled by a factor of 1.5 in order to separate the spectra for clarity. The spectra are comprised of a general continuum from the QPB and the FX lines of Al, Si, Au, and other elements. The energy binning for the data is a constant 15 eV.
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In the text

$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{7930-02.ps} }\end{figure}$ Figure 2: Images in detector coordinates of the FWC data for the MOS1 ( upper row) and MOS2 ( lower row) detectors. The data are from ( left to right) the 0.35-1.25, 1.25-2.0, 2.0-4.0, and 4.0-8.0 keV bands, and have been binned into $25''\times 25''$ pixels. The 1.25-2.0 band is most affected by the FX contamination, and it is likely that there is some difference between the spatial distributions between FWC and open data due to the different source geometry. Note that all of the bands show at least somewhat different structure. The circles indicate the FOV regions of the instruments outside of which the detectors are always shielded from cosmic X-rays.
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In the text

$\begin{figure} \par {\includegraphics[width=12.35cm,clip]{7930-03.ps} } \end{figure}$ Figure 3: Top panel: QPB count rate in the 0.3-10.0 keV band from the out-of-FOV corners of the detectors from KS07 (their Fig. 6) for the individual CCDs from both MOS instruments. The MOS1 data are shown in black, the MOS2 data are shown in blue, and time periods of anomalous CCD background behavior are shown in red. Bottom panel: QPB (2.5-5.0 keV)/(0.4-0.8 keV) hardness from the out-of-FOV corners of the detectors from KS07 (their Fig. 7) for the individual CCDs from both MOS instruments. The MOS1 data are shown in black, the MOS2 data are shown in blue, and time periods of anomalous CCD background behavior are shown in red. The plot limits are 0-0.075 counts s^-1 chip^-1 for the count-rate plots and 0-7.5 for the ratio plots. The data are linearly scaled in both cases.
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In the text

$\begin{figure} \par {\includegraphics[width=15.5cm,clip]{7930-04.ps} }\end{figure}$ Figure 4: Image in detector coordinates of the SP data for the MOS1 ( upper row) and MOS2 ( lower row) detectors. From left to right the data are from the 0.35-0.8 keV, 0.8-1.25 keV, 1.25-2.0 keV, 2.0-4.0 keV, and 4.0-8.0 keV bands. In the plots blue and green indicate lower intensities while red and white indicate higher intensities. The data are linearly scaled. For better statistics, data are from the observations using all filters have been combined as there is little difference between the distributions for the thin, medium, and thick filter observations separately. Note that the distributions are not flat across the detectors nor are they symmetrically vignetted like cosmic X-rays. As well, the distributions are not the same for different energies.
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In the text

$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{7930-05.ps} } \end{figure}$ Figure 5: Sample light curves and light-curve histograms from two observations with different amounts of SP contamination. The top two panels show the light-curve histogram and light curve for the data from ObsID 0202130101 while the bottom two panels show the same for ObsID 0049150101.
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In the text

$\begin{figure} \par {\includegraphics[width=8.5cm,clip]{7930-06.ps} } \end{figure}$ Figure 6: Spectra from two of the four XMM-Newton EPIC MOS observations of the Hubble Deep Field North (ObsID 0202130101 in black and ObsID 0049150101 in red). The black data points and curve show the spectrum from the contaminated observation while the red data points and curve show an uncontaminated spectrum. The uncontaminated spectrum agreed well with the two other observations of this direction. The additional curves show the fitted model contributions to the fits where all components besides the SWCX emission were fit simultaneously for the two spectra.
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In the text

$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{7930-07.ps} }\end{figure}$ Figure 7: All-sky maps in the $\frac{1}{4}$ keV ( upper), $\frac{3}{4}$ keV ( middle), and 1.5 keV ( lower) bands from Snowden et al. (1997) in an Aitoff-Hammer projection with the Galactic center at the center with longitude increasing to the left. Red and white indicate higher intensities while purple and blue indicate lower intensities.
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In the text

$\begin{figure} \par {\includegraphics[width=7.6cm,clip]{7930-08.ps} }\end{figure}$ Figure 8: Temporal filtering results for the MOS1 Abell 1795 cluster observation with ObsID 0097820101. The upper panel plots the light curve histogram for the 2.5-12.0 keV band from the FOV, the middle panel displays the 2.5-12.0 keV band FOV light curve, and the lower panel displays 2.5-12.0 keV band light curve from the unexposed corners of the instrument. The histogram is derived from the smoothed light curve. In the upper panel, the blue vertical lines show the range for the Gaussian fit, the green curve shows the Gaussian fit, while the red vertical lines show the upper and lower bounds for filtering the data. In the bottom two panels green points indicate accepted data while black points indicate data excluded by the filtering algorithm. The high count rate excursions are produced by soft protons rather than a particle background flare as the latter case would produce a similar increase in the corner data.
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In the text

$\begin{figure} \par {\includegraphics[width=8cm,clip]{7930-09.ps} }\end{figure}$ Figure 9: Spectra from two annuli from the Abell 1795 analysis, 1'-2' ( upper panel) and 10'-15' ( lower panel). In each panel the upper spectrum is the total spectrum while the lower spectrum is the modeled QPB spectrum. The data have not been normalized for solid angle, otherwise the 1'-2' spectrum would be relatively brighter by about two orders of magnitude.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=15.7cm,clip]{7930-10.ps} }\end{figure}$ Figure 10: Spectral fit to the data from Abell 1795. MOS1 and MOS2 spectra are shown for all ten annuli, as well as the ROSAT spectral energy distribution. The lower panel shows the ratio of the data to the model and demonstrates that the fit is reasonably good over the full dynamic range.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-11.ps} }\end{figure}$ Figure 11: Comparison of results for the A1795 temperature radial profile from Chandra (square, Vikhlinin et al. 2005), and XMM-Newton analysis from Nevalainen et al. (2005) (circle) and this analysis (cross). The radii for the XMM-Newton points have been slightly offset in the plot for clarity.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-12.ps} }\end{figure}$ Figure 12: Comparison of results for the temperature radial profiles for various clusters in their $\sim$ 1'-5' annuli from Chandra (Vikhlinin et al. 2005) and XMM-Newton (this analysis).
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In the text

$\begin{figure} \par {\includegraphics[width=7.5cm,clip]{7930-13.ps} }\end{figure}$ Figure 13: Comparison of results for the Abell 1795 ( top panel) and Abell 2204 ( bottom panel) temperature radial profiles from analysis including (cross) and not including (square) the effect of PSF smearing (crosstalk between adjacent annuli). The radii have been slightly offset in the plot for clarity.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-14.ps} }\end{figure}$ Figure 14: Ratio of the fitted temperatures for a selection of clusters analyzed using SAS V7.1 and the calibration files of 2007 September versus the calibration used for the cluster catalog. The horizontal line is set at a ratio of 1.0.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6.7cm,clip]{7930-15.ps} \end{figure}$ Figure 15: Comparison of temperature radial profile results for the two observations of Abell 1835 ( upper panel), Sérsic 159-3 ( middle panel), and Perseus ( lower panel). The radii have been slightly offset in the plot for clarity. For the Sérsic 159-3 plot the CIE results of de Plaa et al. (2006). In all panels the box and cross symbols represent the results of this paper while in the middle panel the circle symbols represent the de Plaa et al. (2006) results.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6.7cm,clip]{7930-16.ps} \end{figure}$ Figure 16: The two plots display the comparison results from using Anders & Grevesse (1989) and Lodders (2003) abundances for the fitted values of the abundance ( upper panel) and temperature ( lower panel). In the upper plot the line is the best-fit scale factor of 1.44 while in the lower plot the line shows the one-to-one relationship. In both plots the filled circles indicate data from the outer annuli.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=7cm,clip]{7930-17.ps} \end{figure}$ Figure 17: Comparison of the fitted values for the annuli iron abundances and emission temperatures using Anders & Grevesse (1989) and Lodders (2003) model abundances while allowing all abundances to vary. The upper panel shows the correlation between the fitted values for the iron abundance for the two abundance models. The solid line is the best-fit correlation of 1.47 while the dashed line shows the 1.44 correlation of the single abundance normalization. The lower panel shows the fitted values for the temperatures where (open circle) abundances starting with Anders & Grevesse (1989) values were allowed to vary independently, (filled circle) Anders & Grevesse (1989) values were allowed to vary only with a single scale factor, and (filled triangle) Lodders (2003) values were allowed to vary only with a single scale factor.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-18.ps} }\end{figure}$ Figure 18: Scaled temperature radial profiles for all of the analyzed clusters.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-19.ps} }\end{figure}$ Figure 19: Abundance radial profiles for all of the analyzed clusters.
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In the text

$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-20.ps} }\end{figure}$ Figure 20: Scaled flux radial profiles for all of the analyzed clusters.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-21.ps} \end{figure}$ Figure 21: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-22.ps} \end{figure}$ Figure 22: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-23.ps} \end{figure}$ Figure 23: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-24.ps} \end{figure}$ Figure 24: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-25.ps} \end{figure}$ Figure 25: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-26.ps} \end{figure}$ Figure 26: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-27.ps} \end{figure}$ Figure 27: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-28.ps} \end{figure}$ Figure 28: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-29.ps} \end{figure}$ Figure 29: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-30.ps} \end{figure}$ Figure 30: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-31.ps} \end{figure}$ Figure 31: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-32.ps} \end{figure}$ Figure 32: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-33.ps} \end{figure}$ Figure 33: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-34.ps} \end{figure}$ Figure 34: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-35.ps} \end{figure}$ Figure 35: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-36.ps} \end{figure}$ Figure 36: Soft ( left) and hard ( right) band images of the clusters.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-37.ps} \end{figure}$ Figure 37: Soft ( left) and hard ( right) band images of the clusters.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-38.ps} \end{figure}$ Figure 38: Soft ( left) and hard ( right) band images of the clusters.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-39.ps} \end{figure}$ Figure 39: Soft ( left) and hard ( right) band images of the clusters.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-40.ps} \end{figure}$ Figure 40: Soft ( left) and hard ( right) band images of the clusters.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-41.ps} \end{figure}$ Figure 41: Soft ( left) and hard ( right) band images of the clusters.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-42.ps} \end{figure}$ Figure 42: Soft ( left) and hard ( right) band images of the clusters.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{7930-01.ps} \end{figure}$	Figure 1: Filter wheel closed spectra for the MOS1 ( upper) and MOS2 ( lower) detectors. The MOS2 data have been scaled by a factor of 1.5 in order to separate the spectra for clarity. The spectra are comprised of a general continuum from the QPB and the FX lines of Al, Si, Au, and other elements. The energy binning for the data is a constant 15 eV.
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$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{7930-05.ps} } \end{figure}$	Figure 5: Sample light curves and light-curve histograms from two observations with different amounts of SP contamination. The top two panels show the light-curve histogram and light curve for the data from ObsID 0202130101 while the bottom two panels show the same for ObsID 0049150101.
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$\begin{figure} \par {\includegraphics[width=7.8cm,clip]{7930-07.ps} }\end{figure}$	Figure 7: All-sky maps in the $\frac{1}{4}$ keV ( upper), $\frac{3}{4}$ keV ( middle), and 1.5 keV ( lower) bands from Snowden et al. (1997) in an Aitoff-Hammer projection with the Galactic center at the center with longitude increasing to the left. Red and white indicate higher intensities while purple and blue indicate lower intensities.
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$\begin{figure} \par {\includegraphics[width=8cm,clip]{7930-09.ps} }\end{figure}$	Figure 9: Spectra from two annuli from the Abell 1795 analysis, 1'-2' ( upper panel) and 10'-15' ( lower panel). In each panel the upper spectrum is the total spectrum while the lower spectrum is the modeled QPB spectrum. The data have not been normalized for solid angle, otherwise the 1'-2' spectrum would be relatively brighter by about two orders of magnitude.
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$\begin{figure} \par {\includegraphics[angle=-90,width=15.7cm,clip]{7930-10.ps} }\end{figure}$	Figure 10: Spectral fit to the data from Abell 1795. MOS1 and MOS2 spectra are shown for all ten annuli, as well as the ROSAT spectral energy distribution. The lower panel shows the ratio of the data to the model and demonstrates that the fit is reasonably good over the full dynamic range.
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$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-11.ps} }\end{figure}$	Figure 11: Comparison of results for the A1795 temperature radial profile from Chandra (square, Vikhlinin et al. 2005), and XMM-Newton analysis from Nevalainen et al. (2005) (circle) and this analysis (cross). The radii for the XMM-Newton points have been slightly offset in the plot for clarity.
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$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-12.ps} }\end{figure}$	Figure 12: Comparison of results for the temperature radial profiles for various clusters in their $\sim$ 1'-5' annuli from Chandra (Vikhlinin et al. 2005) and XMM-Newton (this analysis).
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$\begin{figure} \par {\includegraphics[width=7.5cm,clip]{7930-13.ps} }\end{figure}$	Figure 13: Comparison of results for the Abell 1795 ( top panel) and Abell 2204 ( bottom panel) temperature radial profiles from analysis including (cross) and not including (square) the effect of PSF smearing (crosstalk between adjacent annuli). The radii have been slightly offset in the plot for clarity.
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$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-14.ps} }\end{figure}$	Figure 14: Ratio of the fitted temperatures for a selection of clusters analyzed using SAS V7.1 and the calibration files of 2007 September versus the calibration used for the cluster catalog. The horizontal line is set at a ratio of 1.0.
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$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-18.ps} }\end{figure}$	Figure 18: Scaled temperature radial profiles for all of the analyzed clusters.
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$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-19.ps} }\end{figure}$	Figure 19: Abundance radial profiles for all of the analyzed clusters.
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$\begin{figure} \par {\includegraphics[angle=-90,width=8cm,clip]{7930-20.ps} }\end{figure}$	Figure 20: Scaled flux radial profiles for all of the analyzed clusters.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-21.ps} \end{figure}$	Figure 21: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-22.ps} \end{figure}$	Figure 22: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-23.ps} \end{figure}$	Figure 23: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-24.ps} \end{figure}$	Figure 24: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-25.ps} \end{figure}$	Figure 25: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-26.ps} \end{figure}$	Figure 26: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-27.ps} \end{figure}$	Figure 27: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-28.ps} \end{figure}$	Figure 28: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-29.ps} \end{figure}$	Figure 29: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-30.ps} \end{figure}$	Figure 30: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-31.ps} \end{figure}$	Figure 31: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-32.ps} \end{figure}$	Figure 32: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-33.ps} \end{figure}$	Figure 33: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-34.ps} \end{figure}$	Figure 34: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=-90,width=5.5in]{7930-35.ps} \end{figure}$	Figure 35: Cluster temperature, abundance, and flux radial profiles. The name of the cluster, fitted redshift, and values for the temperature ( $T_{\rm N}$ ) and flux ( $T_{\rm N}$ ) used for the normalization of the data are provided in the abundance panel.
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$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-36.ps} \end{figure}$	Figure 36: Soft ( left) and hard ( right) band images of the clusters.
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$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-37.ps} \end{figure}$	Figure 37: Soft ( left) and hard ( right) band images of the clusters.
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$\begin{figure} \par\includegraphics[angle=0,width=6.5in]{7930-38.ps} \end{figure}$	Figure 38: Soft ( left) and hard ( right) band images of the clusters.
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