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Recent results suggest that the initial mass function (IMF) of globularclusters (GCs) is metallicity and density dependent. Here it is studied howthis variation affects the initial masses and the numbers of core collapsesupernovae (CCSNe) required to reproduce the observed iron spreads in GCs. TheIMFs of all of the investigated GCs were top-heavy implying larger initialmasses compared to previous results computed assuming an invariant canonicalIMF. This leads to more CCSNe being required to explain the observed ironabundance spreads. The results imply that the more massive GCs formed atsmaller Galactocentric radii, possibly suggesting in-situ formation of thepopulation II halo. The time until star formation (SF) ended within a proto-GCis computed to be 3.5 - 4 Myr, being slightly shorter than the 4 Myr obtainedusing the canonical IMF. Therefore, the impact of the IMF on the time for whichSF lasts is small.

The giants that were born swiftly -- Implications of the top-heavy stellar initial mass function on the birth conditions of globular clusters