All Figures

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{0179fig1.ps}\end{figure}$ Figure 1: Radio power at 1.4 GHz versus X-ray luminosity in the [0.1-2.4] keV band of clusters with GHs (black circles), MHs (red asterisks), and small-scale radio emissions (magenta open circles). Arrows are upper limits to the radio power of CCCs without MHs (see text). The black solid line is the best-fit correlation for GHs (from Cassano et al. 2006).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0179fig2.ps}\end{figure}$ Figure 2: Radio power at 1.4 GHz versus radio size of GHs (black circles) and MHs (red asterisks), and small-scale radio emissions (magenta open circles). The black solid line and the red dashed line are the best-fit correlations for GHs ( $P_{1.4}\propto R_{\rm H}^{4.18}$ , from Cassano et al. 2007) and for MHs ( $P_{1.4}\propto R_{\rm H}^{3.4}$ ), respectively.
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0179fig3.ps}\end{figure}$ Figure 3: Ratio between turbulence energy densities of MHs and GHs normalized to the thermal ones as a function of $B_{\rm MH}$ . The calculations are reported for $f\approx 1$ , z=0.1, $T_{\rm GH}/T_{\rm MH}\approx 3$ and in the case of $B_{\rm MH}\approx 3~B_{\rm GH}$ (solid line) and in the case $B_{\rm MH}\approx 6~B_{\rm GH}$ (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=6.7cm,clip]{0179fig1.ps}\end{figure}$	Figure 1: Radio power at 1.4 GHz versus X-ray luminosity in the [0.1-2.4] keV band of clusters with GHs (black circles), MHs (red asterisks), and small-scale radio emissions (magenta open circles). Arrows are upper limits to the radio power of CCCs without MHs (see text). The black solid line is the best-fit correlation for GHs (from Cassano et al. 2006).
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0179fig2.ps}\end{figure}$	Figure 2: Radio power at 1.4 GHz versus radio size of GHs (black circles) and MHs (red asterisks), and small-scale radio emissions (magenta open circles). The black solid line and the red dashed line are the best-fit correlations for GHs ( $P_{1.4}\propto R_{\rm H}^{4.18}$ , from Cassano et al. 2007) and for MHs ( $P_{1.4}\propto R_{\rm H}^{3.4}$ ), respectively.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{0179fig3.ps}\end{figure}$	Figure 3: Ratio between turbulence energy densities of MHs and GHs normalized to the thermal ones as a function of $B_{\rm MH}$ . The calculations are reported for $f\approx 1$ , z=0.1, $T_{\rm GH}/T_{\rm MH}\approx 3$ and in the case of $B_{\rm MH}\approx 3~B_{\rm GH}$ (solid line) and in the case $B_{\rm MH}\approx 6~B_{\rm GH}$ (dashed line).
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