Explaining the extended GeV gamma-ray emission adjacent to HESS J1825-137

Abstract

HESS J1825-137 is one of the most powerful and luminous TeV gamma-ray pulsar wind nebulae (PWN). To the south of HESS J1825-137, Fermi-LAT observation revealed a new region of GeV gamma-ray emission with three apparent peaks (termed here, GeV-ABC). This study presents interstellar medium (ISM) data and spectral energy distribution (SED) modelling towards the GeV emission to understand the underlying particle acceleration. We considered several particle accelerator scenarios - the PWN associated with HESS J1825-137, the progenitor SNR also associated with HESS J1825-137, plus the gamma-ray binary system LS\,5039. It was found that the progenitor SNR of HESS J1825-137 has insufficient energetics to account for all GeV emission. GeV-ABC may be a reflection of an earlier epoch in the history of the PWN associated with HESS\,1825-137, assuming fast diffusion perhaps including advection. LS\,5039 cannot meet the required energetics to be the source of particle acceleration. A combination of HESS J1825-137 and LS 5039 could be plausible sources.

Submitted to MNRAS: https://academic.oup.com/mnras/advance-article-abstract/doi/10.1093/mnras/stab983/6219862

References in corpus (11)

• The ATNF Pulsar Catalogue
• Teraelectronvolt Astronomy
• Energy dependent gamma-ray morphology in the Pulsar wind nebula HESSJ1825-137
• Gamma rays from molecular clouds
• Orbital X-Ray Variability of the Microquasar LS 5039
• Confirmation of persistent radio jets in the microquasar LS 5039
• Energy dependent morphology of the pulsar wind nebula HESS J1825-137 with Fermi-LAT
• Newly confirmed and high quality candidate Galactic SNRs uncovered from the AAO/UKST HAlpha survey
• Spectral evolution of non-thermal electron distributions in intense radiation fields
• Revealing a new region of gamma-ray emission in the vicinity of HESS J1825-137
• Energy-dependent morphology of the pulsar wind nebula HESS J1825-137 seen by Fermi-LAT