Astrophysics and Space Science

, Volume 91, Issue 1, pp 93–98 | Cite as

Mass model of spiral galaxies disk

  • R. Louise
  • M. Marcelin


The study of rotation curves is the most powerful tool for determining mass distributions inside spiral galaxies. Since the first trial by Burbidgeet al. (1959), followed by Brandt (1960), few methods have been proposed for the determination of the masses of galaxies (Faber and Gallagher, 1979). Monnet and Simien (1977) recently proposed a method based on a two component model (bulge and disk) which permits to compute the total mass providing that the photometry is well-known. We suggest here a method based on a new simple parametrization of the optical rotation curve. This method indicates disk masses substantially higher than the provious estimates and suggests an exponential increase of theM/L ratio in the disk toward the outer parts of the Galaxies.


Total Mass Mass Distribution Component Model Outer Part Optical Rotation 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.


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Copyright information

© D. Reidel Publishing Co. 1983

Authors and Affiliations

  • R. Louise
    • 1
  • M. Marcelin
    • 1
  1. 1.Observatoire de MarseilleMarseilleFrance

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