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Several recent studies have provided evidence for a `bottom-heavy' stellarinitial mass function (IMF) in massive elliptical galaxies. Here we investigatethe influence of the IMF shape on the recently discovered color-magnituderelation (CMR) among globular clusters (GCs) in such galaxies. To this end weuse calculations of GC mass loss due to stellar and dynamical evolution toevaluate (i) the shapes of stellar mass functions in GCs after 12 Gyr ofevolution as a function of current GC mass along with their effects onintegrated-light colors and mass-to-light ratios, and (ii) their impact on theeffects of GC self-enrichment using the 2009 `reference' model of Bailin &Harris. As to the class of metal-poor GCs, we find the observed shape of theCMR (often referred to as the `blue tilt') to be very well reproduced by Bailin& Harris' reference self-enrichment model once 12 Gyr of GC mass loss is takeninto account. The influence of the IMF on this result is found to beinsignificant. However, we find that the observed CMR among the class ofmetal-rich GCs (the `red tilt') can only be adequately reproduced if the IMFwas bottom-heavy (e.g., $-3.0 <~ \alpha <~ -2.3$ in $dN/dM \proptoM^{\alpha}$), which causes the stellar mass function at subsolar masses todepend relatively strongly on GC mass. This constitutes additional evidencethat the metal-rich stellar populations in giant elliptical galaxies wereformed with a bottom-heavy IMF.

astrophysical journal/the astrophysical journal

Color-Magnitude Relations within Globular Cluster Systems of Giant  Elliptical Galaxies: The Effects of Globular Cluster Mass Loss and the  Stellar Initial Mass Function