years after the SN explosion producing high-energy CRs that escape the CSF system and diffuse through the ambient ISM. However, the estimated age of the supernova which produced the magnetar CXOU J1647-45 in  is $\sim 10^4$yr [@NS_WesterlundI_muno06; @mereghetti08]. If the CSF acceleration occurred $\sim 10^4$yrs ago, these CRs will have produced pions over a much longer time span as the TeV-PeV particles diffuse away, fill a region of about 140 pc radius, and interact with the ambient ISM (the outer ISM region indicated in Fig. \[fig:West\] is about 30 pc).

In Figs. \[fig:gam1m\] and \[fig:NeuOnly\] we show simulated [$\gamma$-ray]{} and neutrino spectra produced by the CRs that escaped from the accelerator and diffused into the surrounding cloudy medium over $10^4$yr. At this point the acceleration responsible for the emission in Fig. \[fig:spectra\_src\] has ceased long ago.

The diffusion model used to propagate the CRs has three regions. Within the accelerator of 3-4 pc radius we assume a Bohm diffusion coefficient $D_B = 3 \times10^{27} E_\mathrm{PeV} \diff$. Outside of the dense cloud region we use an ISM value $D_B = 3 \times10^{29} E^{0.33}_\mathrm{PeV} \diff$, which is consistent with the standard models of CR propagation in the Galaxy [see e.g. @Strong2007]. Between 