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CTB 87 (G74.9+1.2) is an evolved supernova remnant (SNR) which hosts apeculiar pulsar wind nebula (PWN). The X-ray peak is offset from that observedin radio and lies towards the edge of the radio nebula. The putative pulsar,CXOU~J201609.2+371110, was first resolved with \textit{Chandra} and issurrounded by a compact and a more extended X-ray nebula. Here we use a deep{\textit{XMM-Newton}} observation to examine the morphology and evolutionarystage of the PWN and to search for thermal emission expected from a supernovashell or reverse shock interaction with supernova ejecta. We do not findevidence of thermal X-ray emission from the SNR and place an upper limit on theelectron density of 0.05~cm$^{-3}$ for a plasma temperature $kT\sim 0.8$ keV.The morphology and spectral properties are consistent with a $\sim$20~kyr-oldrelic PWN expanding into a stellar wind-blown bubble. We also present the firstX-ray spectral index map from the PWN and show that we can reproduce itsmorphology by means of 2D axisymmetric relativistic hydrodynamical simulations.

Deciphering the Nature of the Pulsar Wind Nebula CTB 87 with XMM-Newton