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Mass models of 100 nearby spiral and irregular galaxies, coveringmorphological types from Sa to Irr, are computed using H$\alpha$ rotationcurves and R$_c$-band surface brightness profiles. The kinematics was obtainedusing a scanning Fabry-Perot interferometer. One of the aims is to compare ourresults 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 wereused 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 towhat was found in the MIR 3.4 $\mu$m band, most of the observed rotation curvesare 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, thederived DM halos' parameters depend on the morphological types. We find similarrelations than those in the literature, only when we compare our results forthe bulge-poor sub-sample because most of previous results were mainly based onlate-type spirals. Because the dispersion in the model parameters is smallerand because stellar masses are better defined in that band, MIR photometryshould be preferred, when possible, to the optical bands. It is shown that forhigh-z galaxies, sensible results can still be obtained without full profiledecomposition.

monthly notices of the royal astronomical society

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