The stability and masses of disc galaxies

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Astronomical Models, Disk Galaxies, Dynamic Stability, Galactic Evolution, Mass, Astronomical Photometry, Density Distribution, Galactic Rotation, Mass To Light Ratios

Scientific paper

Using N-body experiments, the global stability of a series of models designed to match the observed photometric and kinematic properties of disk galaxies are investigated. The models are characterized by two dimensionless numbers, one of which measures the concentration of the halo component and the other of which determines the mass of the halo relative to that in the disk. The models are stable to axisymmetric instabilities but are unstable to bar formation unless they possess a hot component. The results are insensitive to changes in the shape of the rotation curve or the adopted surface density, and to a substantial increase in the random motions of the central part of the disk. It is found that the cool disk component must have a low mass-to-light ratio, and that the dark material is the dominant contributor to the total mass. The population models predict much lower masses for early-type disk galaxies than those deduced from their rotation curves.

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