All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{3965f1.ps}\par\vspace*{3mm} \includegraphics[angle=-90,width=8.5cm,clip]{3965f2.ps} \end{figure}$ Figure 1: Light curves for PN (upper panel) and, for comparison, of the MOS 1 (lower panel) in the band [10-12] keV and the intensity filters we use.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3965f3.ps} \end{figure}$ Figure 2: XMM-Newton EPIC image of the cluster A3528 in the band [0.5-10.0] keV. The bright sources detected by the pipeline processing of the image are masked. Notice the high concentration of these X-ray emitting point sources in the region lying between the two clumps. None of these have an associated redshift.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3965f4.ps} \end{figure}$ Figure 3: XMM-Newton contour plots of the EPIC image of the cluster A3528 in the band [0.5-10.0] keV superposed on the DSS image, in the Bj band, of the same field of view. The contours are spaced by a factor of $\sim$ 1.4 between 1.7 and 579 cts/pixel.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{3965f5.ps} \end{figure}$ Figure 4: The regions used for the detection of the diffuse emission between the two clumps are here superimposed on the total EPIC raw image. The width of the strip is of 13.2 pixels $\approx$ 1.90 arcmin. The surface brightness profiles shown in Fig. 5 are extracted along these strips and are obtained by accumulating the counts in bins of 10 pixels ( $\approx$ 1.44 arcmin) each. The progression of the bins starts from north to south along the "clusters'' regions, while from west to east in the "bridge'' regions.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{3965f6bw.eps}\hspace*{4mm}... ...s}\hspace*{4mm} \includegraphics[width=6.4cm,clip]{3965f8b.ps}\par \end{figure}$ Figure 5: Left: adaptively smoothed exposure-corrected EPIC image of A3528 in the soft ([0.5-2.0] keV; top panel), medium ([2.0-4.5] keV, middle panel) and hard band ([4.5-8.0] keV, bottom panel). Right count rates in the regions defined in Fig. 4 and obtained in the soft ([0.5-2.0] keV; top panel), medium ([2.0-4.5] keV; middle panel) and hard ([4.5-8.0] keV; bottom panel) band. The error bars are the 1 $\sigma$ Poisson errors and the background shown as a dotted line is obtained by a median of the counts in the two last bins West and East of the three "bridge'' regions. Each bin has dimension $13.2\times 10$ pixels² ( $\approx$ $1.90\times 1.44$ arcmin²; see caption of Fig. 4).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3965f9.ps} \end{figure}$ Figure 6: Temperature map obtained by using 5 X-ray colours (0.4-0.8, 0.8-1.4, 1.4-2.0, 2.0-4.5, 4.5-8.0 keV) and estimating the expected count rate with XSPEC for a thermal MEKAL model, with fixed Galactic absorption ${N_{\rm H}}~$ and metallicity. The observed count rate is estimated in $4 \times 4$ original bins of $(8.7 \times 8.7)$ arcsec² with step in X and Y of 2 bins.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{3965f10.ps}\hspace*{5mm} \includegraphics[width=7.4cm,clip]{3965f11.ps}\end{figure}$ Figure 7: Temperature ( upper panels) and metal abundance ( lower panels) profiles for A3528-N and A3528-S. The dots show the best-fit results, while the squares are the deprojected values. The horizontal bars represent the width of the bins used to extract the counts and the dotted line indicates the temperature value from a spatially integrated fit. Uncertainties are at the 68% level for one interesting parameter ( $\Delta \chi ^{2}=1$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3965f12.ps}\hspace*{4mm} \includegraphics[width=8.5cm,clip]{3965f13.ps} \end{figure}$ Figure 8: EPIC temperature map (left) and abundance map (right).
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{3965f14.ps}\hspace*{1.2cm}... ...5f16.ps}\hspace*{7mm} \includegraphics[width=7cm,clip]{3965f17.ps} \end{figure}$ Figure 9: Gas temperature ( upper panels) and metal abundance ( lower panels) profiles measured in $90\deg-$ sectors for A3528-N ( left) and A3528-S ( right). Uncertainties are at the 68% level for one interesting parameter ( $\Delta \chi ^{2}=1$ ).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3965f18.eps} \end{figure}$ Figure 10: Isodensity distribution of the light in the A3528-N and A3528-S region, from the COSMOS/UKSTJ galaxy catalogue, over plotted onto the X-ray image. These contours have been calculated by summing the galaxy luminosities in bins of $2\times 2$ arcmin and then smoothing with a Gaussian of 3 pixels FWHM.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3965f19.ps} \end{figure}$ Figure 11: Mass profiles of A3528-N and A3528-S ( points: from hydrostatic equation applied to the spectral deprojected results; dashed lines: $1 \sigma$ range values obtained by assuming a King profile; dotted line $1 \sigma$ range values obtained by assuming a NFW profile).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3965f20.ps} \end{figure}$ Figure 12: Residuals above 2 in the X-ray brightness distribution. Given two regions, A and B, of (length, width) = (2 pixels $\approx 17$ arcsec $, 30^\circ )$ located symmetrically with respect to the center and with observed $C_{\rm A}$ and $C_{\rm B}$ counts respectively, the residuals are estimated as $\sigma = (C_{\rm A} - C_{\rm B}) / \sqrt {C_{\rm A} + C_{\rm B}}$ . An azimuthal scan with step of $30^\circ /3$ was done to smooth the map.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{3965f21.ps} \end{figure}$ Figure A.1: Joint fit of the two M1 (in black) and M2 (in red) spectra of A3528-N. Residuals are evident in the soft (0.5-2.0 keV) band.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.8cm,clip]{3965f22.ps}\hspa... ...ludegraphics[angle=-90,width=7.8cm,clip]{3965f25.ps} \vspace*{2mm} \end{figure}$ Figure A.2: MOS 1 data and folded model of the K iron line with free redshift and with fixed redshift at the optical value of 0.053 with the SASv5.3.3 in the upper panels and with SASv5.4.1 in the bottom panels.

In the text

$\begin{figure} \par\includegraphics[height=5.7cm,width=5.6cm,clip]{3965f26.ps}\h... ...*{3mm} \includegraphics[height=5.7cm,width=5.6cm,clip]{3965f27.ps} \end{figure}$ Figure C.1: Measured temperature as a function of different low energy cutoffs (the high energy cutoff is fixed at 8.0 keV because it had no effect on the measured temperature) for MOS1 (green), MOS2 (red) and PN singles (blue). Diamonds referred to fits with no background renormalization, triangles to fits with the renormalized background and squares to fits with the double subtraction. Uncertainties are at the 68% level for one interesting parameter ( $\Delta \chi ^{2}=1$ ).

In the text

$\begin{figure} \par\includegraphics[height=5.4cm,width=5.2cm,clip]{3965f28.ps}\h... ...*{3mm} \includegraphics[height=5.4cm,width=5.2cm,clip]{3965f29.ps} \end{figure}$ Figure C.2: Same symbols as in Fig. C.1 for radial profiles.

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.5cm,clip]{3965f1.ps}\par\vspace*{3mm} \includegraphics[angle=-90,width=8.5cm,clip]{3965f2.ps} \end{figure}$	Figure 1: Light curves for PN (upper panel) and, for comparison, of the MOS 1 (lower panel) in the band [10-12] keV and the intensity filters we use.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3965f3.ps} \end{figure}$	Figure 2: XMM-Newton EPIC image of the cluster A3528 in the band [0.5-10.0] keV. The bright sources detected by the pipeline processing of the image are masked. Notice the high concentration of these X-ray emitting point sources in the region lying between the two clumps. None of these have an associated redshift.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3965f4.ps} \end{figure}$	Figure 3: XMM-Newton contour plots of the EPIC image of the cluster A3528 in the band [0.5-10.0] keV superposed on the DSS image, in the Bj band, of the same field of view. The contours are spaced by a factor of $\sim$ 1.4 between 1.7 and 579 cts/pixel.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{3965f9.ps} \end{figure}$	Figure 6: Temperature map obtained by using 5 X-ray colours (0.4-0.8, 0.8-1.4, 1.4-2.0, 2.0-4.5, 4.5-8.0 keV) and estimating the expected count rate with XSPEC for a thermal MEKAL model, with fixed Galactic absorption ${N_{\rm H}}~$ and metallicity. The observed count rate is estimated in $4 \times 4$ original bins of $(8.7 \times 8.7)$ arcsec² with step in X and Y of 2 bins.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3965f12.ps}\hspace*{4mm} \includegraphics[width=8.5cm,clip]{3965f13.ps} \end{figure}$	Figure 8: EPIC temperature map (left) and abundance map (right).
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{3965f14.ps}\hspace{1.2cm}... ...5f16.ps}\hspace{7mm} \includegraphics[width=7cm,clip]{3965f17.ps} \end{figure}$	Figure 9: Gas temperature ( upper panels) and metal abundance ( lower panels) profiles measured in $90\deg-$ sectors for A3528-N ( left) and A3528-S ( right). Uncertainties are at the 68% level for one interesting parameter ( $\Delta \chi ^{2}=1$ ).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3965f18.eps} \end{figure}$	Figure 10: Isodensity distribution of the light in the A3528-N and A3528-S region, from the COSMOS/UKSTJ galaxy catalogue, over plotted onto the X-ray image. These contours have been calculated by summing the galaxy luminosities in bins of $2\times 2$ arcmin and then smoothing with a Gaussian of 3 pixels FWHM.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3965f19.ps} \end{figure}$	Figure 11: Mass profiles of A3528-N and A3528-S ( points: from hydrostatic equation applied to the spectral deprojected results; dashed lines: $1 \sigma$ range values obtained by assuming a King profile; dotted line $1 \sigma$ range values obtained by assuming a NFW profile).
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