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G54.1+0.3 is a young pulsar wind nebula (PWN), closely resembling the Crab,for which no thermal shell emission has been detected in X-rays. Recent Spitzerobservations revealed an infrared (IR) shell containing a dozen point sourcesarranged in a ring-like structure, previously proposed to be young stellarobjects. An extended knot of emission located in the NW part of the shellappears to be aligned with the pulsar's X-ray jet, suggesting a possibleinteraction with the shell material. Surprisingly, the IRS spectrum of the knotresembles the spectrum of freshly formed dust in Cas A, and is dominated by anunidentified dust emission feature at 21 microns. The spectra of the shell alsocontain various emission lines and show that some are significantly broadened,suggesting that they originate in rapidly expanding supernova (SN) ejecta. Wepresent the first evidence that the PWN is driving shocks into expanding SNejecta and we propose an alternative explanation for the origin of the IRemission in which the shell is composed entirely of SN ejecta. In thisscenario, the freshly formed SN dust is being heated by early-type starsbelonging to a cluster in which the SN exploded. Simple dust models show thatthis interpretation can give rise to the observed shell emission and the IRpoint sources.

Deep Chandra Observations of the Crab-like Pulsar Wind Nebula G54.1+0.3 and Spitzer Spectroscopy of the Associated Infrared Shell