| The question of where the low metallicity globular clusters in early-type galaxies came from has profound implications as to how those galaxies formed. Evidence is presented that these globular clusters formed within dwarf galaxies that have been subsumed by their more massive counterparts. One of the difficulties with this idea is that the pressures of the interstellar media of dwarfs are not expected to be high enough to produce dense, bound star clusters. Therefore, this work has been extended to examine in more detail how the low metallicity clusters formed in dwarfs. It has been found that an increase in gas pressure from supernovae can produce dense star clusters and that this is consistent with the amount of chemical enrichment in the remaining interstellar gas associated with such supernovae. Additionally, the subsumation scenerio presented in this thesis suggests a theoretical reason for the decrease in the density and metallicity of globular clusters with increasing galactocentric distance in the Milky Way and other galaxies. |
