nIFTy galaxy cluster simulations – II. Radiative models

摘要: We have simulated the formation of a massive galaxy cluster (M$_{200}^{\rm crit}$ = 1.1$\times$10$^{15}h^{-1}M_{\odot}$) in $\Lambda$CDM universe using 10 different codes (RAMSES, 2 incarnations AREPO and 7 GADGET), modeling hydrodynamics with full radiative subgrid physics. These include Smoothed-Particle Hydrodynamics (SPH), spanning traditional advanced SPH schemes, adaptive mesh moving codes. Our goal is to study consistency between clusters modeled physical implementations - such as cooling, star AGN feedback. compare images at $z=0$, global properties mass, radial profiles various dynamical thermodynamical quantities. find that, respect non-radiative simulations, dark matter more centrally concentrated, extent not simply depending on presence/absence The scatter quantities substantially higher than for runs. Intriguingly, adding physics seems washed away marked code-based differences present entropy profile seen simulations Sembolini et al. (2015): + classic can produce cores. Furthermore, inclusion/absence feedback dividing line -as case describing stellar content- whether code produces an unrealistic temperature inversion falling central profile. However, does strongly affect overall distribution, limiting effect overcooling reducing sensibly fraction.