1995A&A...303..742D

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 in the literature for some globular clusters. It comes out that the steep mass spectral indices quoted by Richer et al. (1991) for M 13, NGC 6752 and ω Centauri cannot be brought in agreement with dynamically 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 difference between Population I and Population II mass spectra. On the other hand, these small mass spectral indices cannot explain the high M/L_V ratios in halos of galaxies. If Dark Matter is baryonic, it probably is not connected with "normal" star formation.