The search for pevatrons (objects capable of accelerating 10^15 eV particles) has become one of the key targets of the high—energy gamma—ray community. These objects are of crucial importance in the context of the origin of cosmic rays (CRs), since the sources of Galactic CRs are expected to be pevatrons.
Currently, the most famous candidates for the origin of Galactic CRs are supernova remnants (SNRs), the shocks expanding in the interstellar medium after the explosion of massive stars. But surprisingly, all detected SNRs have been shown to not be pevatrons, making the situation somewhat bewildering.
A special attention is currently being devoted to the search of a SNR pevatron, and we will discuss the possibility of detecting and identifying one with next-generation gamma-ray instruments, such as the Cherenkov Telescope Array.

[Webinar]
By facing strong experimental constraints notably from direct detection, many dark matter scenarios based on the Weakly Interacting Massive Particles (WIMPs) paradigm are pushed towards corners of viable parameter space. Several alternative production mechanisms have received a lot of attention over the past few years. In this talk, I will present various possibilities of producing dark matter in a state out of thermal equilibrium. I will show that the non-thermal nature of the dark matter can leave an imprint on the matter power spectrum, which features a cutoff analogous to that for warm dark matter. I will present a mapping procedure that allows to translate the Lyman-alpha forest mass bound to such scenarios and discuss the phenomenological implications of these results.

Cosmology has entered an era of unprecedented precision. With measurements of the fluctuations in the cosmic microwave background radiation, their counterparts in large-scale structure in the form of baryon acoustic oscillations and the development of the cosmic distance ladder, the concordance model of cosmology is established as a robust standard model, able to describe the universe from seconds after the Big Bang to today and on spatial scales ranging from galaxies to the entire visible universe. The values of its free parameters are now pinned down to remarkable precision and future galaxy surveys will allow further improvement in precision.
However, with growing precision, some tensions have started to emerge. Although it is tempting to attribute these growing tensions to signs of new, exciting physics, it is important to make sure that our cosmological model is accurate on top of being precise; that is, to ensure that these tensions are not, in part or completely, systematic offsets due to our imperfect modelling of a complex, multi-scale system.
In this talk, I will present some tests of the accuracy of our standard model, focusing on some central assumptions of the model and addressing in particular: the geometry of the very large-scale universe, the propagation of light in an inhomogeneous universe, and ways to probe the small scale distribution of matter.