Evolution of globular cluster systems in elliptical galaxies. I. Log-normal initial mass function

Details Evolution of globular cluster systems in elliptical galaxies. I. Log-normal initial mass function Evolution of globular cluster systems in elliptical galaxies. I. Log-normal initial mass function

2000-07-18

arxiv.org/abs/astro-ph/0007266v1

Mon.Not.Roy.Astron.Soc.318:841,2000

Astronomy and Astrophysics

Astrophysics

17 pages, accepted for publication in MNRAS

Scientific paper

10.1046/j.1365-8711.2000.03869.x

We study the evolution of globular cluster systems (GCS) in elliptical galaxies and explore the dependence of their main properties on the mass and the size of the host galaxy.The dependence of the evolution of the GCS mass function (GCMF), of the fraction of surviving clusters and of the ratio of the final to initial mass in clusters on the structure of the host galaxy as well as their variation with the galactocentric distance inside individual host galaxies has been thoroughly investigated.After a survey over a large number of different host galaxies we have restricted our attention to a sample of galaxies with effective masses and radii equal to those observed for dwarf,normal and giant ellipticals. We show that, in spite of large differences in the fraction of surviving clusters, the final mean masses of the GCMF in massive galaxies are very similar to each other with a small galaxy-to-galaxy dispersion;low-mass compact galaxies tend to have smaller values of the final mean mass and a larger galaxy-to-galaxy dispersion. These findings are in agreement with those of recent observational analyses. The fraction of surviving clusters increases with the mass of the host galaxy. We show that a small difference between the initial and the final mean mass and dispersion of the GCMF and the lack of a significant radial dependence of the mean mass inside individual galaxies do not necessarily imply that evolutionary processes have been unimportant in the evolution of the initial population of clusters. For giant galaxies most disruption occurs within the effective radius while for low-mass galaxies a significant disruption of clusters takes place also at larger galactocentric distances. The dependence of the results obtained on the initial mean mass of the GCMF is investigated. (abridged)

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