Revealing a new region of gamma-ray emission in the vicinity of HESS J1825-137

Abstract

HESS J1825-137 is a bright very-high-energy (VHE) gamma-ray source that has been firmly established as a pulsar wind nebula (PWN), and one of the most extended gamma-ray objects within this category. The progenitor supernova remnant (SNR) for this PWN has not been firmly established. We carried out an analysis of gamma-ray observations in the region of HESS J1825-137 with the Fermi-LAT which reveal emission in the direction away from the Galactic plane. The region lies beyond the PWN and reaches a distance from the pulsar compatible with the supposed location of the SNR shock front. The spectrum of the gamma-rays is hard with a photon index of $\sim 1.9$ in the 10-250 GeV range. Several scenarios for the origin of the emission are discussed, including the SNR as a source of high-energy particles and the "leakage"' of leptons from the PWN.

To be published in MNRAS

References in corpus (6)

• The ATNF Pulsar Catalogue
• Energy dependent gamma-ray morphology in the Pulsar wind nebula HESSJ1825-137
• Discovery of New Interacting Supernova Remnants in the Inner Galaxy
• Chandra Observation of PSR B1823-13 and its Pulsar Wind Nebula
• Newly confirmed and high quality candidate Galactic SNRs uncovered from the AAO/UKST HAlpha survey
• X-Ray and Gamma-Ray Emission from Middle-aged Supernova Remnants in Cavities. I. Spherical Symmetry

Cited by in corpus (4)

• Incremental Fermi Large Area Telescope Fourth Source Catalog
• A 3D Diffusive and Advective Model of Electron Transport Applied to the Pulsar Wind Nebula HESS J1825-137
• Explaining the extended GeV gamma-ray emission adjacent to HESS J1825-137
• The primary proton spectrum of the hadronic PeVatron candidate HAWC J1825-134