Speaker
Description
Supernova remnants (SNRs), pulsar wind nebulae (PWNe) and pulsars are the usual suspects to accelerate the bulk of cosmic rays in our Galaxy. In those objects the gamma-ray emission allows us to probe the population of high-energy particles and in particular the population of accelerated hadrons radiating through the pion-decay mechanism. In case of composite SNRs, both the SNR shell and the PWN are sometimes bright enough to be observed in the same source. However, understanding the nature of the gamma-ray emission in such objects can be challenging for sources of small angular extent. Previous studies of the composite SNR G326.3-1.8 (radius=0.3°) revealed bright and extended gamma-ray emission but its origin remained uncertain.
With the recent Pass8 Fermi-LAT data that provide an increased acceptance and angular resolution, we investigate the morphology of this source to disentangle the PWN from the SNR contributions. In particular, we take advantage of the new possibility to filter events based on their angular reconstruction quality (PSF types). We also report a spectral analysis and derive some physical properties using one-zone models for the SNR spectrum.
