Figure 11
The log of the gas pressure, expressed as P/k=nT (K cm−3), is shown as a function of the hydrogen density and (top panel) the cosmic ray rate relative to the Galactic background and (bottom panel) the extra-heating rate. For comparison inner regions of the Perseus cluster have nT≈ 106.5 cm−3 K.

The log of the gas pressure, expressed as P/k=nT (K cm−3), is shown as a function of the hydrogen density and (top panel) the cosmic ray rate relative to the Galactic background and (bottom panel) the extra-heating rate. For comparison inner regions of the Perseus cluster have nT≈ 106.5 cm−3 K.

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