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We present near and mid-infrared observations of the pulsar-wind nebula (PWN)B0540-69.3 and its associated supernova remnant made with the {\it SpitzerSpace Telescope}. We report detections of the PWN with all four IRAC bands, the24 $\mu$m band of MIPS, and the Infrared Spectrograph (IRS). We find noevidence of IR emission from the X-ray/radio shell surrounding the PWNresulting from the forward shock of the supernova blast wave. The flux of thePWN itself is dominated by synchrotron emission at shorter (IRAC) wavelengths,with a warm dust component longward of 20 $\mu$m. We show that this dustcontinuum can be explained by a small amount ($\sim 1-3 \times 10^{-3} \msun$)of dust at a temperature of $\sim 50-65$ K, heated by the shock wave generatedby the PWN being driven into the inner edge of the ejecta. This is evidentlydust synthesized in the supernova. We also report the detection of severallines in the spectrum of the PWN, and present kinematic information about thePWN as determined from these lines. Kinematics are consistent with previousoptical studies of this object. Line strengths are also broadly consistent withwhat one expects from optical line strengths. We find that lines arise fromslow ($\sim 20$ km s$^{-1}$) shocks driven into oxygen-rich clumps in the shellswept-up by an iron-nickel bubble, which have a density contrast of $\sim100-200$ relative to the bulk of the ejecta, and that faster shocks ($\sim 250$km s$^{-1}$) in the hydrogen envelope are required to heat dust grains toobserved temperatures. We infer from estimates of heavy-element ejectaabundances that the progenitor star was likely in the range of 20-25 $M_\odot$.

Ejecta, Dust, and Synchrotron Radiation in B0540-69.3: A More Crab-Like Remnant than the Crab