We have simulated the formation of a massive galaxy cluster ( M _ { 200 } ^ { crit } = 1.1 \times 10 ^ { 15 } h ^ { -1 } M _ { \odot } ) in a \Lambda CDM universe using 10Â different codes ( RAMSES , 2 incarnations of AREPO Â and 7Â of Gadget ) , modeling hydrodynamics with full radiative subgrid physics .
These codes include Smoothed-Particle Hydrodynamics ( SPH ) , spanning traditional and advanced SPH schemes , adaptive mesh and moving mesh codes .
Our goal is to study the consistency between simulated clusters modeled with different radiative physical implementations - such as cooling , star formation and AGN feedback .
We compare images of the cluster at z = 0 , global properties such as mass , and radial profiles of various dynamical and thermodynamical quantities .
We find that , with respect to non-radiative simulations , dark matter is more centrally concentrated , the extent not simply depending on the presence/absence of AGN feedback .
The scatter in global quantities is substantially higher than for non-radiative runs .
Intriguingly , adding radiative physics seems to have washed away the marked code-based differences present in the entropy profile seen for non-radiative simulations in ( 98 ) : radiative physics + classic SPH can produce entropy cores .
Furthermore , the inclusion/absence of AGN feedback is not the dividing line -as in the case of describing the stellar content- for whether a code produces an unrealistic temperature inversion and a falling central entropy profile .
However , AGN feedback does strongly affect the overall stellar distribution , limiting the effect of overcooling and reducing sensibly the stellar fraction .