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. 2018MNRAS.478...50K, which used mid-infrared (MIR) WISE (Wide-field Infrared Survey Explorer) 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-fitting models, maximum disc models, and models for which mass-to-light ratio (M/L) is fixed using the B-V colours. 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 dark matter halo' 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.

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