**Table 4:** **Cooling flow clusters:** upper limits on the CRp density parameter $\tilde{n}_{{\rm CRp},0}$ and average CRp luminosity $L_{\rm CRp}$ of the central active galaxy by comparing the integrated flux above 100 MeV to EGRET upper limits assuming a $\gamma$ -ray spectral index in Dermer's model $\alpha _\gamma =\alpha _{\rm p}$ . The spatial distribution of CRp is is calculated according to the diffusion model of CRp away from a central AGN assuming $\alpha _{\rm p}= \alpha _{\rm inj} + \alpha _{\rm diff}$ , where $\alpha _{\rm diff} = 1/3$ . **Non-cooling flow clusters:** upper limits on the CRp number parameter $\tilde{N}_{\rm CRp}$ and average CRp luminosity $L_{\rm CRp}$ without any diffusion induced spectral steepening, i.e. $\alpha _{\rm p}= \alpha _{\rm inj}$ . Note that $L_{\rm CRp}$ scales in the case of cooling flow clusters with the diffusion coefficient $\kappa _0$ while it only depends on the CRp injection time $t_{\rm inj}$ for non-cooling flow clusters (see Sect. 3.2.3).
$\begin{displaymath}\begin{tabular}{lc*{8}{c}} \hline \hline \vphantom{\LARGE A}%... ...s 10^{45}$ & $4.2 \times 10^{45}$ \\ \par\hline \end{tabular}\end{displaymath}$

Source LaTeX | All tables | In the text