Fossil groups in the Millennium Simulation. Evolution of the brightest galaxies

DÍAZ-GIMÉNEZ, E.; MURIEL, H.; MENDES DE OLIVEIRA, C.

ASTRONOMY AND ASTROPHYSICS

EDP SCIENCES S A

Año: 2008 vol. 490 p. 965 - 973

0004-6361

Aims: We create a catalogue of simulated fossil groups and study their properties, in particular the merging histories of their first-ranked galaxies. We compare the simulated fossil group properties with those of both simulated non-fossil and observed fossil groups. Methods: Using simulations and a mock galaxy catalogue, we searched for massive (>5 × 10^13 h^-1 M_s) fossil groups in the Millennium Simulation Galaxy Catalogue. In addition, we attempted to identify observed fossil groups in the Sloan Digital Sky Survey Data Release 6 using identical selection criteria. Results: Our predictions on the basis of the simulation data are: (a) fossil groups comprise about 5.5% of the total population of groups/clusters with masses larger than 5 × 10^13 h^-1 M_s. This fraction is consistent with the fraction of fossil groups identified in the SDSS, after all observational biases have been taken into account; (b) about 88% of the dominant central objects in fossil groups are elliptical galaxies that have a median R-band absolute magnitude of -23.5 log h, which is typical of the observed fossil groups known in the literature; (c) first-ranked galaxies of systems with M > 5 × 10^13 h^-1 M_s, regardless of whether they are either fossil or non-fossil, are mainly formed by gas-poor mergers; (d) although fossil groups, in general, assembled most of their virial masses at higher redshifts in comparison with non-fossil groups, first-ranked galaxies in fossil groups merged later, i.e. at lower redshifts, compared with their non-fossil-group counterparts. Conclusions: We therefore expect to observe a number of luminous galaxies in the centres of fossil groups that show signs of a recent major merger.