Speaker
Description
The relationship between the visible and dark components of galaxies is a complex function of mass, accretion history, and galaxy formation physics. Nevertheless, recent work using simulated galaxy clusters has shown that stars can be an accurate tracer of the splashback boundary of the dark matter halo, potentially providing a robust way to infer the dark matter in observations. Building on this, in this talk I will present results on the relationship between the dark matter splashback and the stellar and gas components of 324 simulated galaxy clusters from the Three Hundred suite. By isolating the orbiting and infalling material, I show how the splashback of the dark matter and stars is related to the first and second caustics in the density profile, and examine the prospects of using this to estimate the accretion rate.
