Mass model of spiral galaxies disk

Details Mass model of spiral galaxies disk Mass model of spiral galaxies disk

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983ap%26ss..91...93l&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 91, no. 1, March 1983, p. 93-98.

Astronomy and Astrophysics

Astrophysics

2

Disk Galaxies, Galactic Rotation, Mass Distribution, Spiral Galaxies, Astronomical Models, Astronomical Photometry, Curve Fitting

Scientific paper

The study of rotation curves is the most powerful tool for determining mass distributions inside spiral galaxies. Since the first trial by Burbridge et 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. The authors suggest here a method based on a new simple parametrization of the optical rotation curve. This method indicates disk masses substantially higher than the previous estimates and suggests an exponential increase of the M/L ratio in the disk toward the outer parts of the galaxies.

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