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The evolution of a pulsar wind nebula (PWN) inside a supernova remnant (SNR)is sensitive to properties of the central neutron star, pulsar wind, progenitorsupernova, and interstellar medium. These properties are both difficult tomeasure directly and critical for understanding the formation of neutron starsand their interaction with the surrounding medium. In this paper, we determinethese properties for PWN G54.1+0.3 by fitting its observed properties with amodel for the dynamical and radiative evolution of a PWN inside an SNR. Ourmodeling suggests that the progenitor of G54.1+0.3 was an isolated ~15-20 SolarMass star which exploded inside a massive star cluster, creating a neutron starinitially spinning with period ~30-80ms. We also find that >99.9% of thepulsar's rotational energy is injected into the PWN as relativistic electronsand positrons whose energy spectrum is well characterized by a brokenpower-law. Lastly, we propose future observations which can both test thevalidity of this model and better determine the properties of this source -- inparticular, its distance and the initial spin period of the central pulsar.

The Properties of the Progenitor Supernova, Pulsar Wind, and Neutron Star inside PWN G54.1+0.3