  The Cygnus Cocoon region is a complex region containing an OB star cluster
that is prominent in the TeV energy range. Located in this region is 3HWC
J2031+415, a significant TeV gamma-ray source whose emission is possibly
associated with 2 components, the Cygnus OB2 star cluster and a pulsar wind
nebula (PWN). In this work, several modelling methods are presented to best
describe the emission. These models disentangle emission believed to be from
the Cocoon and isolate the component emitted by the probable PWN. I will
present several spectral models to describe the emission of the probable PWN
using the latest data set from the High-Altitude Water Cherenkov (HAWC)
observatory. Furthermore, I will present an energy morphology study of the PWN
component of 3HWC J2031+415 in distinct energy bands.
