Speaker
Description
HESS J1804-216 is one of the brightest yet most mysterious TeV gamma-ray sources discovered so far. Previous arcminute-scale investigations of the interstellar medium (ISM) surrounding this source revealed that HESS J1804-216 is likely powered by a middle-aged supernova remnant (SNR) or pulsar. SNRs are believed to accelerate both cosmic-ray protons and electrons at their shock front. These cosmic rays interact with the ISM and produce TeV gamma rays. In this contribution, the measurements of the ISM will be summarised and the different emission scenarios will be discussed. Moreover, spatial and spectral distributions of cosmic rays are generated for a range of model parameters. Gamma-ray morphology maps are created based on these cosmic-ray distributions. The modelled morphologies of two nearby potential cosmic-ray accelerators -- SNR G8.7-0.1 and the progenitor SNR of PSR J1803-2137 -- and their comparison to recent observations will be discussed. More detailed features in the morphology may be resolved with the next-generation Cherenkov Telescope Array, which will provide unprecedented angular resolution and sensitivity.
