particles accelerated in the converging flows. The transition between these two regimes of acceleration occurs when the energy of a particle, $E_T$, is large enough so it can easily travel between the two shocks.

This transition, occurring at $\sim 20$TeV, is seen as a bend in the neutrino spectrum shown in Fig. \[fig:spectra\_src\]. This figure shows neutrinos (solid curve) and [$\gamma$-rays]{} (dashed curve) from [$p\!-\!p$]{}-decay from CR protons that are still trapped near the SNR and stellar wind, along with IC from trapped CR electrons. This is the emission expected $\sim 400$yr after the SN explosion in a region of radius $\sim 3\!-\!4$pc. Note that the [$\gamma$-ray]{} fluxes of the sources in Fig. \[fig:spectra\_src\] are presented in ${\rm erg~cm^{-2}~s^{-1}~sr^{-1}}$ in order to be compared with the observed diffuse neutrino fluxes, while the fluxes of the sources in Fig. \[fig:gam1m\] are measured in ${\rm erg~cm^{-2}~s^{-1}}$ as usual.

In Fig. \[fig:West\] we have overlaid a schematic of this inner CSF region on a map of . At later times, these “trapped" CRs will escape the accelerator and diffuse beyond the inner CSF region into a much larger outer ISM region where they may encounter dense clouds producing neutrinos and [$\gamma$-rays]{} for an 