Globular Clusters (GCs) – tightly-bound spherical agglomerations of (as much as 10^6) stars – have long been regarded as being the ideal stellar laboratories, mainly owing to the fact that they constitute a “simple stellar population”. As such coeval/mono-metallic assemblies of stars, they have been extensively used for testing models of stellar evolution and population synthesis. This simple notion has, however, been shaken in recent years due to puzzling findings such as the presence of multiple stellar populations within single clusters. Lately, additional studies have emerged, which not only provide more evidence for the “non-simplicity” of the populations of GCs, but such that address with greater magnitude the question as for the possible origins/formation mechanisms. Can it ultimately be proven that a few, or maybe even a significant fraction, of the galactic GCs are indeed relics of the cores (the survived nuclei) of dwarf spheroidal galaxies, disrupted and dissolved within the Milky Way?
