Speaker
Description
HESS J1804-216 is one of the brightest and most mysterious sources discovered and is currently classified as an unidentified source. To unveil the origin of its TeV gamma-ray emission, several scenarios have been considered. For the hadronic scenario, we focus on TeV gamma-ray emission produced by cosmic rays (CRs) from either the SNR G8.7-0.1 or the undetected progenitor of PSR J1803-2137. For the leptonic scenario, we focus on TeV gamma-ray emission produced by electrons from a pulsar wind nebula powered by PSR J1803-2137. From the modelled CR proton and electron spectra, we can model the gamma-ray flux maps. The gamma-ray flux maps are compared with measurements, using various model parameters and multiple sources as accelerators of CRs. These maps are also used to predict what both HESS and CTA might see. This allows us to investigate the observing conditions (observation time, zenith angle, offset angle etc) required for CTA. Comparing the morphology of these maps with observations may reveal the emission scenario. In this contribution, the measurements of the ISM will be summarised and the different emission scenarios will be discussed. Moreover, the simulated gamma-ray morphology will be compared to recent observations. More detailed features in the morphology may be resolved with the next-generation Cherenkov Telescope Array, which will provide unprecedented angular resolution and sensitivity.
