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The evolution of a pulsar wind nebula (PWN) depends on properties of theprogenitor star, supernova, and surrounding environment. As some of thesequantities are difficult to measure, reproducing the observed dynamicalproperties and spectral energy distribution (SED) with an evolutionary model isoften the best approach in estimating their values. G21.5-0.9, powered by thepulsar J1833-1034, is a well observed PWN for which previous modeling effortshave struggled to reproduce the observed SED. In this study, we reanalyzearchival infrared (IR; Herschel, Spitzer) and X-ray (Chandra, NuSTAR, Hitomi)observations. The similar morphology observed between IR line and continuumimages of this source indicates that a significant portion of this emission isgenerated by surrounding dust and gas, and not synchrotron radiation from thePWN. Furthermore, we find the broadband X-ray spectrum of this source is bestdescribed by a series of power laws fit over distinct energy bands. For allX-ray detectors, we find significant softening and decreasing unabsorbed fluxat higher energy bands. Our model for the evolution of a PWN is able toreproduce the properties of this source when the supernova ejecta has a lowinitial kinetic energy $E_{\mathrm{sn}} \approx 1.2 \times10^{50}\,\mathrm{ergs}$ and the spectrum of particles injected into the PWN atthe termination shock is softer at low energies. Lastly, our hydrodynamicalmodeling of the SNR can reproduce its morphology if there is a significantdensity increase of the ambient medium ${\sim} 1.8$ pc north of the explosioncenter.

The Nonstandard Properties of a "Standard" PWN: Unveiling the Mysteries of PWN G21.5-0.9 Using its IR and X-ray emission