2021/04/08 by T. Collins, Tiffany Collins, Gavin Rowell +10
Physics and Astronomy · #Acceleration #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Fermi Gamma-ray Space Telescope #Gamma ray #Gamma-ray bursts and supernovae #Particle acceleration #Physics #Pulsars and Gravitational Waves Research #astro-ph.HE
paper · pdf · doi:10.1093/mnras/stab983
Submitted to MNRAS: https://academic.oup.com/mnras/advance-article-abstract/doi/10.1093/mnras/stab983/6219862
openalex publication_date 2021/04/08 · arxiv created 2021/04/13 · arxiv updated 2021/04/15 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
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.