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It is widely accepted that individual Galactic globular clusters harbor twocoeval generations of stars, the first one born with the `standard'alpha-enhanced metal mixture observed in field Halo objects, the second onecharacterized by an anticorrelated CN-ONa abundance pattern overimposed on thefirst generation, alpha-enhanced metal mixture. We have investigated withappropriate stellar population synthesis models how this second generation ofstars affects the integrated spectrum of a typical metal rich Galactic globularcluster, like 47Tuc. Our main conclusions are: 1) the age-sensitive Balmerline, Fe line and the [MgFe] indices widely used to determine age, Fe and totalmetallicity of extragalactic systems are largely insensitive to the secondgeneration population; 2) enhanced He in second generation stars affects theBalmer line indices of the integrated spectra, through the change of the turnoff temperature and the horizontal branch morphology of the underlyingisochrones, which translate into a bias towards slightly younger ages.

Modelling chemical abundance anticorrelations on globular cluster spectra