Spectral and Energy Morphology Analysis Study of HAWC J2031+415

TL;DR

This study analyzes the spectral and energy morphology of the TeV gamma-ray source 3HWC J2031+415 in the Cygnus region, using HAWC data to disentangle emissions from the star cluster and a pulsar wind nebula.

Contribution

It introduces spectral and morphological models to distinguish the PWN emission from the Cygnus Cocoon using latest HAWC data.

Findings

Spectral models successfully describe PWN emission.

Energy morphology analysis reveals spatial characteristics of the PWN.

Disentangling emission components improves understanding of the region.

Abstract

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.