CONSTRAINTS FROM POPULATION SYNTHESIS ON THE MASS-SPECTRA OF POPULATION-II SYSTEMS

We calculate M/L(V) ratios of old stellar populations in dependence on the mass spectral index and the low mass cut-off, and the metallicity . The results are compared with mass spectra and M/L(V) values found i n the literature for some globular clusters. It comes out that the ste ep mass spectral indices quoted by Richer et al. (1991) for M 13, NGC 6752 and omega Centauri cannot be brought in agreement with dynamicall y derived M/L(V)-values. Only small mass spectral indices can explain the actually low M/L(V) ratios, in which case there is no obvious diff erence between Population I and Population II mass spectra. On the oth er hand, these small mass spectral indices cannot explain the high M/L (V) ratios in halos of galaxies. If Dark Matter is baryonic, it probab ly is not connected with ''normal'' star formation.