Mass Models for Disk and Halo Components in Spiral Galaxies
Abstract
The mass distribution in spiral galaxies is investigated by means of numerical simulations, summarizing the results reported by Athanassoula et al. (1986). Details of the modeling technique employed are given, including bulgedisk decomposition; computation of bulge and disk rotation curves (assuming constant mass/light ratios for each); and determination (for spherical symmetry) of the total halo mass out to the optical radius, the concentration indices, the halodensity power law, the core radius, the central density, and the velocity dispersion. Also discussed are the procedures for incorporating galactic gas and checking the spiral structure extent. It is found that structural constraints limit disk mass/light ratios to a range of 0.3 dex, and that the most likely models are maximumdisk models with m = 1 disturbances inhibited.
 Publication:

Nearly Normal Galaxies. From the Planck Time to the Present
 Pub Date:
 1987
 Bibcode:
 1987nngp.proc..121A
 Keywords:

 Astronomical Models;
 Galactic Structure;
 Halos;
 Mass Distribution;
 Spiral Galaxies;
 Accretion Disks;
 Dark Matter;
 Galactic Rotation;
 H I Regions;
 Mass To Light Ratios;
 Astrophysics