Explaining the extended GeV gamma-ray emission adjacent to HESS J1825-137. Issue 2 (10th April 2021)

• Record Type: Journal Article
• Authors: Collins, T; Rowell, G; Mitchell, A M W; Voisin, F; Fukui, Y; Sano, H; Alsulami, R; Einecke, S
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 504:Issue 2(2021)
• Page Start: 1840
• Page End: 1853
• Publication Date: 2021-04-10
• Subjects: ISM: clouds -- cosmic rays -- ISM: individual (HESS J1825-137) -- ISM: individual (LS 5039) -- ISM: supernova remnants -- gamma rays: ISM; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab983
• Languages: English
• ISSNs: 0035-8711

Abstract

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.