All Figures

$\begin{figure} \par\includegraphics[width=12cm,clip]{7990f1.ps}\end{figure}$ Figure 1: X-ray contours superimposed on the Digitalized Sky Survey image of A3128. North is up, West is to the right. The thick contours highlight the large scale features in the X-ray morphology, the thin contours highlight the features at small spatial scales. The contour spacing is arbitrary.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{7990f2a.ps}\includegraphics[angle=-90,width=8cm,clip]{7990f2b.ps}\end{figure}$ Figure 2: The spectrum of the NE ( left panel) and SW ( right panel) X-ray peak extracted from circular region with a radius of 1.5 $^{\prime }$ . The continuous line represents the best fit model. The EPIC/pn and the coadded EPIC/MOS spectra are indicated. The position of the Fe K line in the spectrum from the NE peak shows that the emitting cluster is at a redshift of z=0.44.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7990f3.ps} \end{figure}$ Figure 3: Spectrum of the galaxy associated with the radio source SUMSS J033057-522811 in the centre of the NE X-ray peak. On the y-axis we plot arbitrary count units (ADU). Lines, used for redshift determination, are shown with arrows.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{7990f4.ps} \end{figure}$ Figure 4: Combined R-band image of the galaxy associated with the radio source SUMSS J033057-522811 in the centre of the NE X-ray peak. The total exposure time is 360 s. Note the arc to the Southwest of the galaxy. The scale of 1 $^{\prime }$ is indicated on the image.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{7990f5a.ps}\includegraphics[... ...th=7cm,clip]{7990f5c.ps}\includegraphics[width=7cm,clip]{7990f5d.ps}\end{figure}$ Figure 5: Top left: the projected emission measure per arcminute, in units of 10⁶⁴ cm^-3 arcmin^-2, integrated along the line of sight, after the emission of the background cluster was subtracted. Top right: temperature map derived from spectral fitting in units of keV. Bottom left: map of the pressure derived from the best fit temperature and emission measure, assuming a length scale along our line of sight of 1 Mpc. The units are 10^-12 dyne cm^-2. Bottom right: map of the entropy derived from the best fit temperature and emission measure, assuming a length scale along our line of sight of 1 Mpc. The units are keV cm². The white and black circles indicate the high surface brightness low entropy region and the region at the centre of the galaxy distribution, respectively. These we use for subsequent spectral analysis. The X-ray isophotes from the wavelet decomposed image are overplotted.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=6cm,clip=t,angle=0.]{7990f6a.ps}... ...990f6b.ps}\includegraphics[width=6cm,clip=t,angle=0.]{7990f6c.ps} } \end{figure}$ Figure 6: Left panel: density map of the ICM. Central panel: map of the entropy of the ICM. Right panel: the pressure map of the ICM. The thermodynamic properties are calculated using volume estimates for the spectral extraction regions described in Henry et al. (2004) and Mahdavi et al. (2005). The volumes are calculated assuming two centres, one at the SW X-ray peak, and one at the X-ray bright low entropy region at the possible centre of the gravitational potential of A3128.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7990f1.ps}\end{figure}$	Figure 1: X-ray contours superimposed on the Digitalized Sky Survey image of A3128. North is up, West is to the right. The thick contours highlight the large scale features in the X-ray morphology, the thin contours highlight the features at small spatial scales. The contour spacing is arbitrary.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{7990f2a.ps}\includegraphics[angle=-90,width=8cm,clip]{7990f2b.ps}\end{figure}$	Figure 2: The spectrum of the NE ( left panel) and SW ( right panel) X-ray peak extracted from circular region with a radius of 1.5 $^{\prime }$ . The continuous line represents the best fit model. The EPIC/pn and the coadded EPIC/MOS spectra are indicated. The position of the Fe K line in the spectrum from the NE peak shows that the emitting cluster is at a redshift of z=0.44.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7990f3.ps} \end{figure}$	Figure 3: Spectrum of the galaxy associated with the radio source SUMSS J033057-522811 in the centre of the NE X-ray peak. On the y-axis we plot arbitrary count units (ADU). Lines, used for redshift determination, are shown with arrows.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{7990f4.ps} \end{figure}$	Figure 4: Combined R-band image of the galaxy associated with the radio source SUMSS J033057-522811 in the centre of the NE X-ray peak. The total exposure time is 360 s. Note the arc to the Southwest of the galaxy. The scale of 1 $^{\prime }$ is indicated on the image.
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