GHASP: an H$\alpha$ kinematics survey of spiral galaxies - XII.
  Distribution of luminous and dark matter in spiral and irregular nearby
  galaxies using R$_c$-band photometry
  Mass models of 100 nearby spiral and irregular galaxies, covering
morphological types from Sa to Irr, are computed using H$\alpha$ rotation
curves and R$_c$-band surface brightness profiles. The kinematics was obtained
using a scanning Fabry-Perot interferometer. One of the aims is to compare our
results with those from Korsaga et al. (2018), which used mid-infrared (MIR)
WISE W1 (3.4 $\mu$m) photometric data. For the analysis, the same tools were
used for both bands. Pseudo-Isothermal (ISO) core and Navarro-Frenk-White (NFW)
cuspy models have been used. We test Best Fit Models (BFM), Maximum Disc Models
(MDM) and models for which M/L is fixed using the B - V colors. Similarly to
what was found in the MIR 3.4 $\mu$m band, most of the observed rotation curves
are better described by a central core density profile (ISO) than a cuspy one
(NFW) when using the optical R$_c$-band. In both bands, the dispersion in the
(M/L) values is smaller for the fixed M/L fits. As for the W1 photometry, the
derived DM halos' parameters depend on the morphological types. We find similar
relations than those in the literature, only when we compare our results for
the bulge-poor sub-sample because most of previous results were mainly based on
late-type spirals. Because the dispersion in the model parameters is smaller
and because stellar masses are better defined in that band, MIR photometry
should be preferred, when possible, to the optical bands. It is shown that for
high-z galaxies, sensible results can still be obtained without full profile
decomposition.
