Dust Evolution in Galaxy Cluster Simulations

Understand

We implement a state-of-the-art treatment of the processes affecting the production and Interstellar Medium (ISM) evolution of carbonaceous and silicate dust grains within SPH simulations.

• We trace the dust grain size distribution by means of a two-size approximation.
• We test our method on zoom-in simulations of four massive ($M_{200} \geq 3 \times 10^{14} M_{\odot}$) galaxy clusters.
• We predict that during the early stages of assembly of the cluster at $z \gtrsim 3$, where the star formation activity is at its maximum in our simulations, the proto-cluster regions are rich of dusty gas.