Early Formation and Late Merging of the Giant Galaxies

Details Early Formation and Late Merging of the Giant Galaxies Early Formation and Late Merging of the Giant Galaxies

2003-12-18

arxiv.org/abs/astro-ph/0312499v2

Astrophys.J.614:17-25,2004

Astronomy and Astrophysics

Astrophysics

25 pages, 9 figures, acctepted by ApJ. Minor changes in text

Scientific paper

10.1086/423444

The most luminous galaxies in the present Universe are found at the centers of the most massive dark matter haloes, rich galaxy clusters. In the LCDM cosmology, such massive halo cores are present at redshift z=6 with a comoving number density (as a function of mass interior to ~10 kpc) that is comparable to today's value. The identity of the matter in these central regions is, however, predicted to change as major mergers bring together stars and dark matter from initially well separated sub-units. We use N-body simulations to investigate how these mergers push pre-existing matter outwards in the dominant galaxy while preserving the inner density profile of collisionless matter. It appears that the central regions of large galaxies end up dominated by stars formed in a number of dense cores, well before the last major mergers. The density profile of collisionless matter (stars and dark matter combined) in these central regions appears to be stable and to have attractor-like behavior under merging. This suggests that the baryon loading associated with dissipative contraction and star formation may be erased as subsequent mergers drive the mass distribution back to a universal profile. Such suppression of the effects of baryon loading, along with the early assembly of mass concentrations, may help resolve some apparent challenges to the CDM model for structure formation.

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