Analysis of the Emission and Morphology of the Pulsar Wind Nebula Candidate HAWC J2031+415

TL;DR

This study analyzes the emission and structure of the HAWC J2031+415 gamma-ray source, suggesting it is likely a pulsar wind nebula associated with PSR J2032+4127, based on multi-wavelength data.

Contribution

It provides the first detailed spectral and morphological analysis of HAWC J2031+415, proposing its identification as a pulsar wind nebula linked to PSR J2032+4127.

Findings

HAWC J2031+415 is likely a pulsar wind nebula.

The source is associated with PSR J2032+4127.

Multi-wavelength analysis supports the PWN hypothesis.

Abstract

The first TeV gamma-ray source with no lower energy counterparts, TeV J2032+4130, was discovered by HEGRA. It appears in the third HAWC catalog as 3HWC J2031+415 and it is a bright TeV gamma-ray source whose emission has previously been resolved as 2 sources: HAWC J2031+415 and HAWC J2030+409. While HAWC J2030+409 has since been associated with the \emph{Fermi-LAT} Cygnus Cocoon, no such association for HAWC J2031+415 has yet been found. In this work, we investigate the spectrum and energy-dependent morphology of HAWC J2031+415. We associate HAWC J2031+415 with the pulsar PSR J2032+4127 and perform a combined multi-wavelength analysis using radio, X-ray, and $\gamma$-ray emission. We conclude that HAWC J2031+415 and, by extension, TeV J2032+4130 are most probably a pulsar wind nebula (PWN) powered by PSR J2032+4127.