Speaker
Description
Gamma-ray astronomy plays a fundamental role in the understanding of very high energy tricky and outstanding sources in our own Galaxy and their role in particle acceleration.
In this context, despite the enormous efforts done in very recent years, both theoretically and experimentally, Cosmic Ray (CR) origin remain without clear answers. Two are the hints of CR acceleration that are sought in the gmma-ray band: the "pion bump" at about 68 MeV and an emission at energy above 100 TeV.
Their commonly accepted galactic sources, Supernova Remnants, can accelerate low-energy CRs (below 1 TeV) but theoretical models show that only very young SNRs (<100yrs) accelerate CRs at PeV energies.
In the meantime, current VHE instruments added other candidate sources for CR acceleration; massive star clusters, novae and microquasars jets that were been recently detected at VHE, adding themselves to the fascinating world of Galactic accelerators. Moreover, the last results published by the LHAASO collaboration, then confirmed by other instruments, revealed the existence of several PeV sources likely related to PWNae, well known leptonic factories (e.g. the Crab Nebula for all). And finally also some known SNRs, older than 100 yrs, were detected t E>100 TeV.
Parameters understanding, multi-wavelength comparison, lower spectral errors are fundamental ingredients to distingush hadronic and leptonic accelerators and to do another step forward the understanding of CR origin. In this context, the future Cherenkov telescopes, as ASTRI Mini-Array and CTA, and a possible gamma-ray satellite focused on the "pion bump" energies, will have a great role.
