in the neutrino spectrum above $\sim 10$TeV reflects the transition from CR acceleration in the single SNR shock for low-energy particles to the more efficient acceleration for high-energy particles as they scatter back and forth between the SNR shock and the cluster wind. The data points for the H.E.S.S. source, and the five Ice Cube events explained in Fig. \[fig:NeuOnly\], are presented to illustrate how they compare to our model predictions when the source is $\sim 400$ yr old and point-like, i.e.,  about 10$^4$ years ago. The simulated [$\gamma$-ray]{} and neutrino emission at the present time from CRs that escaped the accelerator in  $\sim 10^4$ yr ago are summarized in Figs. \[fig:gam1m\] and \[fig:NeuOnly\].[]{data-label="fig:spectra_src"}](f3.pdf){width="300pt"}

Neutrinos and Gamma rays from the Westerlund 1 Cluster {#sec:WestI}
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Emission from Trapped CRs {#sec:trap}
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To explain the IceCube neutrinos, we combine the [nonlinear]{}, time-dependent model of particle acceleration in CSFs with a propagation model applied to the  compact cluster (Fig. \[fig:West\]). The time-dependent simulations provide the evolving energy spectra of CR protons and electrons as the SNR shock approaches the strong wind of a nearby early-type star. For relativistic electrons/positrons we account for the energy losses due to synchrotron and inverse Compton (IC) 