Speaker
Tiffany Collins
(The University of Adelaide)
Description
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. This study presents gas data and spectral energy distribution (SED) modelling towards the GeV emission to understand the underlying particle acceleration. Lying to the north of HESS J1825-137, HESS J1826-130 is a possible PeVatron candidate and will be the focus of future multizone modelling.
