Properties of groups of galaxies in the vicinity of massive clusters

Abstract

This work analyses the properties of groups of galaxies in the surroundings of clusters. On the basis of a very large public Virgo Consortium Simulation, we identified systems of galaxies in a wide range of masses. Systems with masses greater than $M_{cut}=4\times 10^{14}{M}_{\odot }{h}^{-1}$ are considered "host", whereas smaller systems are taken as groups. Our results show that groups properties are affected by the proximity of massive hosts. Physical properties such as velocity dispersion, internal energy ($E$) and virial radius, show an increment, whereas the mean density decreases as the host-group distance is smaller. By analysing groups with different properties, we find that the low mass and the weakly bounded ($E>0$) subsamples, are strongly affected by the presence of the host; on the other hand, massive groups and groups with $E<0$ do not show dependence on the host-group distance. Using a sample of groups identified in the final version of the 2dF Galaxy Redshift Survey, we find a very similar velocity dispersion behaviour in the observational data compared to results in the simulation. We also study the dependence of the groups velocity dispersion on the host masses in both, observations and simulation; finding that the larger is the host mass the higher is the effect on its vicinity.

6 pages, 7 figures, accepted for publication in MNRAS

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• LoCuSS: The infall of X-ray groups onto massive clusters
• Environmental Influences on the Morphology and Dynamics of Group Size Haloes
• Toward Understanding Environmental Effects in SDSS Clusters
• Environmental Enhancement of DM Haloes
• Discrete Spectrum of Inflationary Fluctuations
• Cosmic microwave background constraints on the strong equivalence principle
• Correlated Mixture Between Adiabatic and Isocurvature Fluctuations and Recent CMB Observations