Simulating the impact of dust on the intergalactic medium properties and on the formation of structures

From the first stages of star and galaxy formation, non-gravitational processes such as ram pressure stripping, SNs, galactic winds, AGNs, galaxy-galaxy mergers, etc... lead to the enrichment of the IGM in stars, metals as well as dust, via the ejection of galactic material into the IGM. We know now that these processes shape, side by side with gravitation, the formation and the evolution of structures. We present here hydrodynamical simulations of structure formation implementing the presence of dust in the IGM to study its effect on the cooling of the IGM gas, and furthermore on structure formation. This study focus on the galaxy cluster scale where temperatures boost the effect of cooling by dust. We quantify the effect of this interplay between the galactic ISM and the cluster IGM, as an added non-gravitational process over the statistical properties and profiles of the simulated cluster population.