Orateur
Description
Galaxy clusters are the most massive gravitationally bound objects in the Universe, and therefore contain an extraordinary amount of information for both cosmology and astrophysics. These are formed by gravitational collapse of dark matter and baryons from primordial density fluctuations. They then continue to accrete matter throughout their history, preferentially through cosmic filaments that connect to their outskirts and form the so called cosmic web. Furthermore, galaxy cluster properties also depend on complex baryonic physics, such as accretion shocks, for example. All these processes are expected to influence the matter distribution in the environment of galaxy clusters.
In this talk, I will present our analysis on the gas distribution from the centre to the outskirts of galaxy clusters from the IllustrisTNG simulation. We show how both the radial and azimuthal distributions are affected by the cluster environments, tracing cluster structural properties as well as showing a strong correlation with the mass assembly history of the cluster.
| Field | Cosmology |
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