extended period of time, as we discuss in Section \[sec:esc\]. For clarity, the regions are not drawn to scale in Fig. \[fig:West\].

To derive the gamma-emissivity of PeV CRs we accounted for the Breit-Wheeler effect of pair production by energetic photons interacting with the interstellar radiation field as well as the extragalactic light background [see e.g. @aharonian04; @Dwekea13]. This interaction leads to a significant suppression of the [$\gamma$-ray]{} flux at the high-energy end of the spectrum for distant ($\geq10$ kpc) sources.

For the emission from , with an estimated distance of $\sim$ 4 kpc, this effect leads to a relatively small suppression of the [$\gamma$-ray]{} flux at $1-10$ PeV, as can be seen in Figs. \[fig:spectra\_src\] and \[fig:gam1m\]. In addition to the [$\gamma$-rays]{}  produced by pion decay, we have also included [$\gamma$-rays]{} produced by the IC radiation of the secondary $e^{\pm}$ pairs produced [*in situ*]{} by the same [$p\!-\!p$]{}-interactions (see the IC curve in Fig. \[fig:gam1m\]). In this calculation, we accounted for the pair energy losses in a mean magnetic field of magnitude 10 $\mu$G in the extended cloud of number density 25$\cmc$ [see e.g. @strongea14].

Emission from Escaping CRs {#sec:esc}
--------------------------

The initial acceleration stage lasts a few hundred 