Abstract
In this paper the dark matter in spiral galaxies is studied on the basis of models for the stellar velocity dispersion and stellar rotation velocity. The models are based on Satoh's potential-density pairs and the isothermal dark halo. The resulting parameters for the total potential are used to predict the H I rotation curves. We apply the models to the Sc galaxies NGC 6503 and NGC 3198 with the aim of restricting the dark matter distribution in these systems
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