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It is now well-established that most (if not all) ancient globular clustershost multiple popula- tions, that are characterised by distinct chemicalfeatures such as helium abundance variations along with N-C and Na-Oanti-correlations, at fixed [Fe/H]. These very distinct chemical fea- tures aresimilar to what is found in the centres of the massive early-type galaxies andmay influence measurements of the global properties of the galaxies.Additionally, recent results have suggested that M/L variations found in thecentres of massive early-type galaxies might be due to a bottom-heavy stellarinitial mass function. We present an analysis of the effects of globularcluster-like multiple populations on the integrated properties of early-typegalaxies. In particular, we focus on spectral features in the integratedoptical spectrum and the global mass-to-light ratio that have been used toinfer variations in the stellar initial mass function. To achieve this wedevelop appropriate stellar population synthesis models and take into account,for the first time, an initial-final mass relation which takes intoconsideration a varying He abundance. We conclude that while the multiplepopulations may be present in massive early-type galaxies, they are likely notresponsible for the observed variations in the mass- to-light ratio and IMFsensitive line strengths. Finally, we estimate the fraction of stars withmultiple populations chemistry that come from disrupted globular clusterswithin massive ellipticals and find that they may explain some of the observedchemical patterns in the centres of these galaxies.

Multiple populations within globular clusters in Early-type galaxies Exploring their effect on stellar initial mass function estimates