Simulations indicate that stellar and AGN feedback mechanisms significantly influence star formation and the distribution of baryons in the Universe. Despite this consensus, there is no agreement on the exact model for these processes. The Simba suite of hydrodynamical cosmological simulations includes variants with several stellar/AGN feedback models, providing an ideal testbed for assessing the impact of different astrophysical processes on key observables. I will present the predictions of the different Simba runs on the distribution of various baryonic phases (e.g., hot/warm/cool gas) within and outside haloes. I find that the radial profiles of the gas density around galaxy groups and clusters decays more gently with radial distance once AGN-jet feedback is introduced. Such distinctive feature is driven by the increased share of hot gas surrounding the most massive haloes. I will discuss the prospects of exploiting this observable signature to constrain numerical AGN feedback models, especially with X-ray data.