All Figures

$\begin{figure} \par\includegraphics[width=5.4cm,clip]{3016fig1a.eps}\includegrap... ...p]{3016fig1b.eps}\includegraphics[width=5.4cm,clip]{3016fig1c.eps} \end{figure}$ Figure 1: Radio contours of the high resolution images of the head-tail radio galaxy J1331-3141 at 240 MHz ( left), 332 MHz ( centre) and 610 MHz ( right), overlaid on the DSS-1 optical frame. The rms noise is 0.80, 0.30 and 0.15 mJy b^-1 respectively. Contour levels are -2.4, 2.4, 4.8, 9.6, 19.2, 38.4, 76.8 mJy b^-1 at 240 MHz, -0.9, 0.9, 1.8, 3.6, 7.2, 14.4, 28.8, 57.6 mJy b^-1 at 332 MHz, -0.45, 0.45, 0.9, 1.8, 3.6, 7.2, 14.4, 28.8 mJy b^-1 at 610 MHz. The angular resolution is 17.4 $^{\prime \prime }\times 11.5$ $^{\prime \prime }$ in PA 11 $^{\circ }$ at 240 MHz, 15.0 $^{\prime \prime }\times 8.0$ $^{\prime \prime }$ in PA 26 $^{\circ }$ at 332 MHz and 7.3 $^{\prime \prime }\times 5.0$ $^{\prime \prime }$ in PA 7 $^{\circ }$ at 610 MHz.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3016fig2.ps} \end{figure}$ Figure 2: Low resolution image at 610 MHz of the central radio halo in A3562. The restoring beam is $30^{\prime \prime }\times 20^{\prime \prime }$ . Contour levels are -0.5, 0.25, 0.5, 1.0, 2.0, 4.0, 8.0, 16.0, 32.0, 64.0 mJy b^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3016fig3.ps} \end{figure}$ Figure 3: Low resolution image at 240 MHz of the central radio halo in A3562. The restoring beam is $41.9\hbox {$^{\prime \prime }$ }\times 35.1\hbox {$^{\prime \prime }$ }$ . Contour levels are -2.4, 2.4, 4.8, 9.6, 19.2, 38.4, 76.8, 153.6, 307.2, 614.4 mJy b^-1.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{3016fig4.eps} \end{figure}$ Figure 4: Low resolution image at 332 MHz of the region including the centre of A3562 and the extended radio galaxy J1332-3146a (on the right) overlaid on the optical DSS-1 frame. The restoring beam is $41.9^{\prime \prime }\times 35.1^{\prime \prime }$ . Contour levels are -1, 1, 2, 4, 8, 16, 32, 64, 128 mJy b^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3016fig5_new.ps} \end{figure}$ Figure 5: Color scale image of the spectral index distribution over the radio halo between 332 MHz and 1400 MHz, as computed from images with a restoring beam of $41.9^{\prime \prime }\times 35.1^{\prime \prime }$ , in PA 55 $^{\circ }$ . Overlaid are the GMRT 332 MHz radio contours at levels -1, 1, 2, 4, 8, 16, 32, 64, 128 mJy b^-1.
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In the text

$\begin{figure} \par\includegraphics[width=6.6cm,clip]{3016fig6.ps} \end{figure}$ Figure 6: Radio spectra of the halo source (filled dots) and of the head-tail J1333-3141 (triangles) in A3562. The 1.4 GHz flux density values are taken from V03. The 843 MHz value for the halo is from V00. For the head-tail, the 2.36 GHz flux density is taken from V00, and the 330 MHz, 4.86 GHz and 8.46 GHz values are from V03.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{3016fig7.ps} \end{figure}$ Figure 7: Color scale image of the spectral index distribution over the head-tail radio galaxy J1333-3141, between 332 MHz and 1380 MHz, as computed from images with a restoring beam of $15.0^{\prime \prime } \times 8.0^{\prime \prime }$ , in PA 26 $^{\circ }$ . Overlaid are the ATCA 1380 MHz radio contours at levels -0.5, 0.5, 1.0, 2.0, 4.0, 8.0, 16.0 mJy b^-1.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=7cm,clip]{3016fig8.ps} \end{figure}$ Figure 8: Energy spectrum of the radio halo in A3562 compared with the expectations from three models for the origin of the emitting electrons. The long dashed line represents the emission from a power law energy distribution of the emitting electrons; this model is normalized at the 332-1400 MHz emission. The short dashed line is a turbulent-acceleration model of electrons which are accelerated and emit in a region which is larger than the typical scale of variation of the magnetic field intensity (the slope of the model is similar to what is reported in Brunetti et al. 2004, Fig. 21). The solid line is obtained assuming that particles are accelerated with a fixed acceleration efficiency and emit in a region of constant magnetic field intensity.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=16cm,clip]{3016fig9.ps} \end{figure}$ Figure 9: VLA-1400 MHz contours of the radio emission from A3562 and SC 1329-313 superimposed on the XMM-Newton mosaic in the 0.8-2 keV band. The radio levels are -0.15, 0.15, 0.3, 0.6, 1.2, 2.4, 4.8, 9.6, 19.2, 38.4, 76.8 and 153.6 mJy b^-1. The restoring beam is ${\it FWHM}=41.9^{\prime \prime } \times 35.1^{\prime \prime }$ , in p.a. 55 $^{\circ }$ .
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.3cm,clip]{3016fig10.ps} \end{figure}$ Figure 10: VLA-1400 MHz image of the radio halo at the centre of A3562, overlaid on the XMM-Newton pseudo-entropy map of the cluster. Radio levels are 0.00015 $\times$ (-1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512, 1024) Jy b^-1 and the resolution is $41.9^{\prime \prime }\times 35.1^{\prime \prime }$ .
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.3cm,clip]{3016fig11.ps} \end{figure}$ Figure 11: VLA 1400 MHz image of the radio halo, overlaid on the pressure map of A3562. Radio levels are 0.00015 $\times$ (-1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512, 1024) Jy b^-1 and the resolution is $41.9^{\prime \prime }\times 35.1^{\prime \prime }$ .
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=7.8cm,clip]{3016fig12.ps} \end{figure}$ Figure 12: Grid used for the comparison of the radio and X-ray images of the cluster A3562. The size of each grid cell is 70 $^{\prime \prime }$ $\times$ 70 $^{\prime \prime }$ . The grid is overlaid on the Chandra X-ray surface brightness image. Contours represent the VLA-1400 MHz image of the halo, after subtraction of the central head-tail radio galaxy J1333-3141. Radio levels are 0.00015 $\times$ (-1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512, 1024) Jy b^-1. The angular resolution of the radio map is $41.9^{\prime \prime }\times 35.1^{\prime \prime }$ . The X-ray image has been obtained from the Chandra raw image (resolution 2 $^{\prime \prime } \times 2^{\prime \prime }$ ) after a smoothing with a box of 60 $^{\prime \prime }$ width.
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In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.4cm,clip]{3016fig13.ps} \end{figure}$ Figure 13: Relation between the radio flux density at 1.4 GHz and the Chandra X-ray flux for the cluster A3562. Data points represent the mean flux density in each cell of the grid constructed over the cluster region (Fig. 12). The error-bars are the rms of flux distribution. The filled dots indicate the values derived for the grid cells containing the weak filamentary structure of the radio halo extending toward South-West. The upper limits represent cells with no detected radio emission above the 1 $\sigma$ level. The dotted line is the radio 3 $\sigma$ level. The solid line is the best fit of the data including all the boxes. The long-dashed line is the best fit obtained excluding the western filament.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3016fig2.ps} \end{figure}$	Figure 2: Low resolution image at 610 MHz of the central radio halo in A3562. The restoring beam is $30^{\prime \prime }\times 20^{\prime \prime }$ . Contour levels are -0.5, 0.25, 0.5, 1.0, 2.0, 4.0, 8.0, 16.0, 32.0, 64.0 mJy b^-1.
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{3016fig3.ps} \end{figure}$	Figure 3: Low resolution image at 240 MHz of the central radio halo in A3562. The restoring beam is $41.9\hbox {$^{\prime \prime }$ }\times 35.1\hbox {$^{\prime \prime }$ }$ . Contour levels are -2.4, 2.4, 4.8, 9.6, 19.2, 38.4, 76.8, 153.6, 307.2, 614.4 mJy b^-1.
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$\begin{figure} \par\includegraphics[width=16.4cm,clip]{3016fig4.eps} \end{figure}$	Figure 4: Low resolution image at 332 MHz of the region including the centre of A3562 and the extended radio galaxy J1332-3146a (on the right) overlaid on the optical DSS-1 frame. The restoring beam is $41.9^{\prime \prime }\times 35.1^{\prime \prime }$ . Contour levels are -1, 1, 2, 4, 8, 16, 32, 64, 128 mJy b^-1.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3016fig5_new.ps} \end{figure}$	Figure 5: Color scale image of the spectral index distribution over the radio halo between 332 MHz and 1400 MHz, as computed from images with a restoring beam of $41.9^{\prime \prime }\times 35.1^{\prime \prime }$ , in PA 55 $^{\circ }$ . Overlaid are the GMRT 332 MHz radio contours at levels -1, 1, 2, 4, 8, 16, 32, 64, 128 mJy b^-1.
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$\begin{figure} \par\includegraphics[width=6.6cm,clip]{3016fig6.ps} \end{figure}$	Figure 6: Radio spectra of the halo source (filled dots) and of the head-tail J1333-3141 (triangles) in A3562. The 1.4 GHz flux density values are taken from V03. The 843 MHz value for the halo is from V00. For the head-tail, the 2.36 GHz flux density is taken from V00, and the 330 MHz, 4.86 GHz and 8.46 GHz values are from V03.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{3016fig7.ps} \end{figure}$	Figure 7: Color scale image of the spectral index distribution over the head-tail radio galaxy J1333-3141, between 332 MHz and 1380 MHz, as computed from images with a restoring beam of $15.0^{\prime \prime } \times 8.0^{\prime \prime }$ , in PA 26 $^{\circ }$ . Overlaid are the ATCA 1380 MHz radio contours at levels -0.5, 0.5, 1.0, 2.0, 4.0, 8.0, 16.0 mJy b^-1.
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$\begin{figure} \par\includegraphics[angle=0,width=16cm,clip]{3016fig9.ps} \end{figure}$	Figure 9: VLA-1400 MHz contours of the radio emission from A3562 and SC 1329-313 superimposed on the XMM-Newton mosaic in the 0.8-2 keV band. The radio levels are -0.15, 0.15, 0.3, 0.6, 1.2, 2.4, 4.8, 9.6, 19.2, 38.4, 76.8 and 153.6 mJy b^-1. The restoring beam is ${\it FWHM}=41.9^{\prime \prime } \times 35.1^{\prime \prime }$ , in p.a. 55 $^{\circ }$ .
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$\begin{figure} \par\includegraphics[angle=0,width=8.3cm,clip]{3016fig10.ps} \end{figure}$	Figure 10: VLA-1400 MHz image of the radio halo at the centre of A3562, overlaid on the XMM-Newton pseudo-entropy map of the cluster. Radio levels are 0.00015 $\times$ (-1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512, 1024) Jy b^-1 and the resolution is $41.9^{\prime \prime }\times 35.1^{\prime \prime }$ .
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$\begin{figure} \par\includegraphics[angle=0,width=8.3cm,clip]{3016fig11.ps} \end{figure}$	Figure 11: VLA 1400 MHz image of the radio halo, overlaid on the pressure map of A3562. Radio levels are 0.00015 $\times$ (-1, 1, 2, 4, 8, 16, 32, 64, 128, 256, 512, 1024) Jy b^-1 and the resolution is $41.9^{\prime \prime }\times 35.1^{\prime \prime }$ .
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