SIMBAD references

To define a framework for the formation and evolution of the cooling cores in X-ray galaxy clusters, we study how the physical properties change as a function of the cosmic time in the inner regions of a 4-keV and an 8-keV galaxy cluster under the action of radiative cooling and gravity only. The cooling radius, R_cool, defined as the radius at which the cooling time equals the Universe age at given redshift, evolves from ∼0.01R₂₀₀ at z>2, where the structures begin their evolution, to ∼0.05R₂₀₀ at z = 0. The values measured at 0.01R₂₀₀show an increase of about 15-20 per cent per Gyr in the gas density and surface brightness and a decrease with a mean rate of 10 per cent per Gyr in the gas temperature. The emission-weighted temperature diminishes by about 25 per cent and the bolometric X-ray luminosity rises by a factor ∼2 after 10 Gyr when all the cluster emission is considered in the computation. On the contrary, when the core region within 0.15 R₅₀₀ is excluded, the gas temperature value does not change and the X-ray luminosity varies by 10-20 per cent only. The cooling time and gas entropy radial profiles are well represented by power-law functions, t_cool=t_0+t0.01(η/0.01R₂₀₀)^γ and K=K_0+K_0.1_(r/0.1R₂₀₀)^α, with t₀ and K₀that decrease with time from 13.4 Gyr and 270 keV.cm2 in the hot system (8.6 Gyr and 120 keV.cm2in the cool one) and reach zero after about 8 (3) Gyr. The slopes vary slightly with the age, with γ~1.3 and α~1.1. The behaviour of the inner slopes of the gas temperature and density profiles are the most sensitive and unambiguous tracers of an evolving cooling core. Their values after 10 Gyr of radiative losses, T_gas∝ r^0.4 and n_gas∝ r^–1.2, are remarkably in agreement with the observational constraints available for nearby X-ray luminous cooling core clusters. Because our simulations do not consider any AGN heating, they imply that the feedback process does not greatly alter the gas density and temperature profiles as generated by radiative cooling alone.