The magnetar CXOU J1647-45, discovered by @munoea06 using high resolution [*Chandra*]{} X-ray observations, has been associated with . This magnetar was likely produced about 10,000 years ago by a supernova with a progenitor star of mass $\geq$ 40 [@munoea06; @mereghetti08] and remains the only direct evidence of supernova activity in .

In our [pevatron]{} model, a SN blast wave collides with the termination shock of a strong wind generated by the collective action of many massive stars in a compact cluster. Both shocks are assumed to propagate in a homogeneous upstream plasma. We show that proton energies well above a PeV may be produced with a hard spectrum where the CR spectrum at PeV energies is most sensitive to the shock speeds and amplification of magnetic turbulence associated with CR driven instabilities. The model provides a high efficiency of conversion of SN shock–cluster wind ram pressure into PeV CRs which is needed to explain at least some of the IceCube neutrino events. We don’t consider a SN interacting with its own wind since individual stellar winds will be unimportant in the compact cluster environment where dozens of massive stars are located within a few parsecs and the wind cavity is 