image) and the blow-up of the inner region shows the position of the magnetar CXOU J1647-45 found by @munoea06 with a high angular resolution Chandra observation of . The outer region is 30-40pc centered around   and indicated by the large dashed circle. This is overlaid on a H.E.S.S. map of TeV emission adapted from @hessWd1. The angular resolution of IceCube is larger than the outer circle. In Fig. \[fig:Galactic\] we show the larger neutrino emitting ISM volume of radius $\sim$ 140 pc around . The volume is filled over $\sim 10^4$yr with CRs accelerated during a short CR acceleration phase $\sim$ 400 years right after the supernova explosion in which produced the magnetar. []{data-label="fig:West"}](f2.pdf){width="250"}

Colliding flows and 3D geometry effects {#3D}
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While an exact treatment of non-linear CSF with a significant backreaction from accelerated CRs is unfeasible in 3D, we have introduced an approximation to account for effects from 3D geometry in our plane-parallel model. Instead of taking the cluster wind termination shock and the SNR blast wave as plane, we account for aspects of the curved shock surfaces at positions parameterized by the angles $\theta$ or $\phi$ in Fig. \[fig:3D\]. We still assume planar shocks for the DSA 