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.
Keywords
Cite
@article{arxiv.2104.05953,
title = {Explaining the extended GeV gamma-ray emission adjacent to HESS J1825-137},
author = {T. Collins and G. Rowell and A. M. W. Mitchell and F. Voisin and Y. Fukui and H. Sano and R. Alsulami and S. Einecke},
journal= {arXiv preprint arXiv:2104.05953},
year = {2021}
}
Comments
Submitted to MNRAS: https://academic.oup.com/mnras/advance-article-abstract/doi/10.1093/mnras/stab983/6219862