Reproducing the entropy structure in galaxy groups

Details Reproducing the entropy structure in galaxy groups Reproducing the entropy structure in galaxy groups

2002-12-19

arxiv.org/abs/astro-ph/0212450v1

Astron.Astrophys. 398 (2003) L35-L40

Astronomy and Astrophysics

Astrophysics

5 page, A&A in press

Scientific paper

10.1051/0004-6361:20021877

We carry out a comparison between observations and hydrodynamic simulations of entropy profiles of groups and clusters of galaxies. We use the Tree+SPH GADGET code to simulate four halos of sizes in the M_500 = 1.0 - 16.e13 h^-1 Msun range, corresponding to poor groups up to Virgo-like clusters. We concentrate on the effect of introducing radiative cooling, star formation, and a variety of non-gravitational heating schemes on the entropy structure and the stellar fraction. We show that all the simulations result in a correct entropy profile for the Virgo-like cluster. With the heating energy budget of ~0.7 keV/particle injected at z_h=3, we are also able to reproduce the entropy profiles of groups. We obtain the flat entropy cores as a combined effect of preheating and cooling, while we achieve the high entropy at outskirts by preheating. The resulting baryon fraction locked into stars is in the 25-30% range, compared to 35-40% in the case of no preheating. Heating at higher redshift, z_h=9, strongly delays the star-formation, but fails to produce a sufficiently high specific entropy.

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