(a), all below 10% of the ram pressure. The IC curve is inverse Compton emission from the secondary electrons produced by the inelastic [$p\!-\!p$]{}-interactions in the cloud. Only the [$\gamma$-rays]{} from the H.E.S.S. field of view are included. The gas number density of the nearby cloud is 25[cm$^{-3}$]{}, except for the light-weight solid curve where it is 30[cm$^{-3}$]{} with $B=0.9$mG.[]{data-label="fig:gam1m"}](f4.pdf){width="300pt"}

![Neutrino emission from an extended ($\sim$ 140 pc radius) source $\sim 10^4$yr after the SN explosion when CRs produced in the short-lived accelerator have propagated into the surrounding material. The amplified magnetic fields are 0.8 mG (c), 0.9 mG (b), and 1 mG (a). We note that the [$\gamma$-rays]{} in Figs. \[fig:gam1m\] and the neutrinos here originate from different volumes: only the [$\gamma$-rays]{} from the H.E.S.S. field of view are shown in Fig. \[fig:gam1m\], while the neutrinos are from a larger region of radius 140 pc. The neutrino data points (1$\sigma$ energy flux error bars) are a subset from all 37 IceCube events [@Aartsen14]). These five events are within 2-$\sigma$ contours from  based on Fig. \[fig:Galactic\]. Two PeV events (14, “Bert") and 35 (“Big Bird"), as well as three sub-PeV (2, 15, 25) events, are included in the subset. Note 