Speaker
Description
We present our new model for the description of the $\rm{PeV}-\rm{TeV}$ Galactic gamma-ray emission assuming discrete distributions of cosmic-ray sources. Based on this model, we investigate the impact of the discreteness of the locations of the cosmis-ray sources and of the diffusion mechanism responsible for the propagation of cosmic rays on the morphology of the VHE Galactic diffuse gamma-ray emission. We notably find that many features potentially observable by LHAASO arise at VHE. In particular, the gamma-ray flux tends to be more clumpy and deviates from the distribution of the interstellar gas, especially for configurations for which only a small subset of all the cosmic-ray sources are PeVatrons. We also discuss the detectability of hadronic PeVatrons in our Galaxy and elaborate a possible interpretation of their number compatible with the LHAASO catalog. Finally, we constrain the fraction of Galactic cosmic-ray sources that are PeVatrons depending on the diffusion mechanism responsible for their propagation and expect that near-future observations will help discriminate between theoretical models.
