The gamma-ray emission from 3HWC J1928+178

TL;DR

This paper investigates the gamma-ray source 3HWC J1928+178, associated with a pulsar, using multiwavelength data and modeling to understand its extended emission and possible transition from a pulsar wind nebula to a halo.

Contribution

It presents a multi-component model of the gamma-ray emission from 3HWC J1928+178, incorporating multiwavelength data and exploring the source's extended nature and evolution.

Findings

Detection of gamma-ray emission consistent with an extended source

Model suggests a transition from pulsar wind nebula to halo

Supports the idea of electron cooling and diffusion in the source

Abstract

The gamma-ray source 3HWC J1928+178, discovered by HAWC, is coincident with the 82 kyr pulsar PSR J1928+1746, located 4 kpc away. It has not been reported by any Imaging atmospheric Cherenkov Telescope (IACT), until the recent detection of emission from this region by H.E.S.S., using an analysis adapted to extended sources. No counterpart in GeV gamma-rays from Fermi-LAT data or in X-ray has been reported so far. In this contribution, I give the multiwavelength context of the region surrounding 3HWC J1928+178 and present a multi-component model derived using the Multi-Mission Maximum Likelihood framework (3ML). I explore the possibility to model the gamma-ray emission of 3HWC J1928+178 by an extended source with continuous diffuse emission. Together with the age of the pulsar and its extended nature, it may indicate a transition from a pulsar wind nebulae to a halo, where the electrons have started to cool and diffuse away from the source.