X-ray properties of galaxy clusters and groups from a cosmological hydrodynamical simulation

Details X-ray properties of galaxy clusters and groups from a cosmological hydrodynamical simulation X-ray properties of galaxy clusters and groups from a cosmological hydrodynamical simulation

2003-10-28

arxiv.org/abs/astro-ph/0310794v1

Mon.Not.Roy.Astron.Soc. 348 (2004) 1078

Astronomy and Astrophysics

Astrophysics

20 pages, 14 figures, to appear in MNRAS

Scientific paper

10.1111/j.1365-2966.2004.07431.x

We present results on the X-ray properties of clusters and groups of galaxies, extracted from a large hydrodynamical simulation. We used the GADGET code to simulate a LambdaCDM model within a box of 192 Mpc/h on a side, with 480^3 dark matter particles and as many gas particles. The simulation includes radiative cooling, star formation and supernova feedback. The simulated M-T relation is consistent with observations once we mimic the procedure for mass estimates applied to real clusters. Also, with the adopted choices of Omega_m=0.3 and sigma_8=0.8 the resulting XTF agrees with observational determinations. The L-T relation also agrees with observations for clusters with T>2 keV, with no change of slope at the scale of groups. The entropy in central cluster regions is higher than predicted by gravitational heating alone, the excess being almost the same for clusters and groups. The simulated clusters appear to have suffered some overcooling, with f*~0.2, thus about twice as large as the value observed. Interestingly, temperature profiles are found to steadily increase toward cluster centers. They decrease in the outer regions, much like observational data do at r>0.2r_vir, while not showing an isothermal regime followed by a smooth temperature decline in the innermost regions.

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