Constraints from population synthesis on the mass spectra of Population II systems.

Details Constraints from population synthesis on the mass spectra of Population II systems. Constraints from population synthesis on the mass spectra of Population II systems.

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...303..742d&link_type=abstract

Astronomy and Astrophysics, v.303, p.742

Astronomy and Astrophysics

Astrophysics

2

Stars: Luminosity Function, Low-Mass, Brown Dwarfs, Dark Matter, Globular Clusters

Scientific paper

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.

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