Spectral energy distribution modeling of broadband emission in the pulsar wind nebula 3C 58

Abstract

We investigate the broadband emission properties of the pulsar wind nebula (PWN) 3C 58 using a spectral energy distribution (SED) model. We attempt to match simultaneously the broadband SED and spatial variations of X‑ray emission in the PWN. We further use the model to explain a possible far‑IR feature of which a hint was recently suggested in 3C 58: a small bump at ∼1011 GHz in the PLANCK and Herschel bands. While external dust emission may easily explain the observed bump, it may be the internal emission of the source, implying an additional population of particles. Although significance for the bump is not high, here we explore possible origins of the IR bump using the emission model, and find that a population of electrons with GeV energies can explain it. If it is produced in the PWN, it may provide new insights into particle acceleration and flows in PWNe.