2004/02/06 by C. J. Ragone, M. Merchan, M. Merchán +2 · 1 citation
Engineering · Physics and Astronomy · #Astronomy and Astrophysical Research #Dispersion (optics) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Redshift #Space Technology and Applications #Velocity dispersion #Virial mass #Virial theorem #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2004.07705.x
6 pages, 7 figures, accepted for publication in MNRAS
arxiv created 2004/02/06 · openalex publication_date 2004/05/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
This work analyses the properties of groups of galaxies in the vicinity 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 Mcut= 4 × 1014 M⊙h−1 are considered ‘hosts’, whereas smaller systems are taken as groups. Our results show that group 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 decreases. By analysing groups with different properties, we find that the low mass and the weakly bound (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 group velocity dispersion on the host masses in both observations and simulation, and we find that the larger the host mass, the higher the effect on its vicinity.