Comparative testing of dark matter models with 15 HSB and 15 LSB
  galaxies
  We assemble a database of 15 HSB and 15 LSB galaxies, for which surface
brightness density and spectroscopic rotation curve data are both available and
representative for various morphologies. We use this dataset to test the
Navarro-Frenk-White, the Einasto, and the pseudo-isothermal sphere dark matter
(DM) models. We investigate the compatibility of the pure baryonic model and
baryonic plus one of the three DM models with observations on the assembled
galaxy database. When a DM component improves the fit with the spectroscopic
rotational curve, we rank the models according to the goodness of fit to the
datasets. We constructed the spatial luminosity density of the baryonic
component based on the surface brightness profile of the galaxies. We estimated
the mass-to-light (M/L) ratio of the stellar component through a previously
proposed color-mass-to-light ratio relation (CMLR). We assumed an axissymetric
baryonic mass model with variable axis ratios together with one of the three DM
models to provide the theoretical rotational velocity curves, and we compared
them with the dataset. In a second attempt, we addressed the question whether
the dark component could be replaced by a pure baryonic model with fitted M/L
ratios. We employed the Akaike information criterion (AIC) to establish the
performance of the best-fit models. For 7 galaxies, neither model fits the
dataset within the 1{\sigma} confidence level. For the other 23 cases, one of
the models with DM explains the rotation curve data best. According to the AIC,
the PSE emerges as most favored in 14 cases, followed by the NFW (6 cases) and
the Einasto (3 cases) DM models. We find that the pure baryonic model with
fitted M/L ratios falls within the 1{\sigma} confidence level for 10 HSB and 2
LSB galaxies, at the price of growing the M/Ls on average by a factor of two,
but the fits are inferior compared to the best-fitting DM model.
