Hydrodynamical simulations of coupled and uncoupled quintessence models II: Galaxy clusters

Understand

We study the $z=0$ properties of clusters (and large groups) of galaxies within the context of interacting and non-interacting quintessence cosmological models, using a series of adiabatic SPH simulations.

• Initially, we examine the average properties of groups and clusters, quantifying their differences in LCDM, uncoupled Dark Energy (\ude) and coupled Dark Energy (\cde) cosmologies.
• In particular, we focus upon radial profiles of the gas density, temperature and pressure, and we also investigate how the standard hydrodynamic equilibrium hypothesis holds in quintessence cosmologies.
• While we are able to confirm previous results about the distribution of baryons, we also find that the main discrepancy (with differences up to $20\%$) can be seen in cluster pressure profiles.