High-energy studies of the 3HWC J1954+286 region: likely Gamma-ray detection of the supernova remnant G65.1+0.6

TL;DR

This study analyzes high-energy gamma-ray data of the 3HWC J1954+286 region, identifying likely gamma-ray emission from the supernova remnant G65.1+0.6 and discussing its possible origin as a TeV halo associated with the pulsar.

Contribution

First detection of gamma-ray emission from SNR G65.1+0.6 in the TeV range using Fermi LAT data, with analysis separating pulsar and SNR contributions.

Findings

Excess gamma-ray emission at ~6σ significance attributed to SNR G65.1+0.6.

Emission spectrum can be explained by hadronic or leptonic models.

Likely identification of the TeV source as a pulsar-associated TeV halo.

Abstract

We carry out high-energy studies of the region of the Galactic TeV source 3HWC J1954+286, whose location coincides with those of PSR~J1954+2836 and supernova remnant (SNR) G65.1+0.6. Analyzing the GeV $\gamma$-ray data obtained with the Large Area Telescope (LAT) onboard {\it the Fermi Gamma-ray Space Telescope}, we are able to separate the pulsar's emission from that of the region. Excess power-law--like emission of a $\sim 6\sigma$ significance level at the region is found, for which we explain as arising from the SNR~G65.1+0.6. Given the low-significance detection, either a hadronic or a leptonic model can provide a fit to the power-law spectrum. Considering the properties of the pulsar and the SNR, we discuss the possible origin of the TeV source, and suggest that it is likely the TeV halo associated with the pulsar.