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Galaxy Haloes and the Missing Mass Problem

Published online by Cambridge University Press:  14 August 2015

Sidney van den Bergh
Sidney van den Bergh*
Affiliation:
David Dunlap Observatory, University of Toronto

Abstract

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Available evidence on the mass-to-light ratios in binary galaxies, small clusters and in rich clusters is reviewed. The interpretation of the binary data remains ambiguous. The relative velocity of M81 and M82 implies that m/LV > 12. The Local Group data also appear to favour the existence of some hidden mass associated with M31 and the Galaxy. In the Virgo cluster a significant fraction of the virial mass may be concentrated in the halo of M87. In Coma the missing mass was probably stripped from the haloes of the two dominant E galaxies and is now distributed throughout the cluster.

It is suggested that metal-poor stars in the galactic disc have a higher CNO abundance than do halo stars of similar metallicity. This may explain why globular cluster stars lie on taller red giant branches than do moderately high-velocity stars near the Sun. The dominant old red giant population in the disc of M31 appears to be similar to that in the Galaxy. Most of the red giants in M33, NGC 6822 and in the LMC lie on taller red giant branches than do those in the Galaxy and M31. This suggests that old evolved stars in these relatively low-luminosity galaxies have a lower heavy element abundance than do their counterparts in the galactic disc. The red giants in M32 appear to be intermediate between those in M31 and M33. This supports the idea that M32 was once much more luminous than it is at present.

Type
V: The Outskirts of Galaxies
Information
Symposium - International Astronomical Union , Volume 77: Structure and Properties of Nearby Galaxies , 1978 , pp. 247 - 265
Copyright
Copyright © Reidel 1978 

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