Feedback is an essential but still not fully understood component of galaxy formation and evolution. If most of astrophysical simulations account for supernova (SN) feedback, it has been shown that it remains insufficient in producing fully realistic simulated galaxies, not only in terms of star formation regulation, but also in reproducing the temperature and metallicity content of gas in the interstellar medium (ISM) and circumgalactic medium (CGM), or the scaling of mass-loading factors with galaxy velocity. Among the other feedback sources that have been investigated over the last past years, cosmic rays are highly regarded as playing a non negligible role in galaxy evolution. Cosmic rays (CRs) are energetic charged particles, mainly consisting of protons with energy around a few GeV produced and accelerated in SN shock waves. They provide an important non thermal pressure gradient in galaxies and heat the gas through hadronic collisions and streaming losses. These effects combined have the potential to disrupt ISM clouds and drive gas away from the galaxy, hence altering the star formation rate and impacting the CGM and its observational properties. 

I will present a study of three isolated galaxies of different masses, combining supernova feedback, radiation and cosmic ray feedback together in radiation-magneto-hydrodynamics (RHMD) simulations, to know if and to what extent CRs contribute to regulate galaxy evolution. I will especially focus on the relative importance of cosmic ray feedback with galaxy mass. I will show how the cosmic ray diffusion coefficient and energy injection from SNe, not fully constrained yet, can lead to different conclusions as for our understanding of their role as a feedback source. Finally, I will briefly give an insight of their effect on zoom-in halos from the SPHINX suite of cosmological simulations.