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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1826fig1.eps}\end{figure}$ Figure 1: The simulated differential flux of $\gamma$ -rays from Perseus reaching the Earth. Shown are upper limits of the IC emission of secondary CRe (power-laws, assuming zero magnetic field) as well as pion decay induced $\gamma$ -ray emission (represented by broad distribution centered on $E_{{\rm peak}}\simeq 67.5 \mbox{ MeV}$ ). The normalization of the spectra differing in their values of the CRp spectral index $\alpha _\gamma =\alpha _{\rm p}$ (Dermer's model) depends on the assumed scaling between CRp and thermal energy density. We fix this scaling parameter $X_{\rm CRp}$ assuming the isobaric model by comparing the integrated flux above 100 MeV to EGRET upper limits (see Reimer et al. 2003).
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