Since their discovery in 1912, Cosmic Rays (CRs) are one of the hottest topics in High Energy Astrophysics. These relativistic particles, mainly protons and nuclei, have a spectrum that spans more than 14 decades in energy. Thanks to more than one century of technological progresses, we have studied, and still study them by both space-based and ground-based instruments, directly detecting primary particles or using gamma-ray emission produced during their interaction with the surrounding medium. Despite this, a lot of questions are still without an answer: what are their main sources? How are they accelerated? How do they propagate to us? The gamma-ray radiation could solve some of these issues; in particular, it can give us a direct proof of their origin. Even if AGILE and Fermi-LAT satellites have confirmed, for the first time, energized CR presence in the Supernova Remnants shocks, an evidence of their fresh acceleration is still missing. For this reason, gamma-ray astrophysics is focusing on the search of the so called "Pevatrons": galactic sources with a gamma-ray emission above 100 TeV that would be a direct confirmation of freshly accelerated CR with PeV energies. The current instruments had not be able to obtain conclusively this proof, mainly because of their limited sensitivity at the interesting energies but the ASTRI Mini-Array, following by the Cherenkov Telescope Array (CTA), could finally mark a turning point in the Pevatron search. Let’s take stock of the current situation.