  We present the mass distribution of a sample of 121 nearby galaxies with high
quality optical velocity fields and available infra-red $\it{WISE}$ 3.4 $\mu$m
data. Contrary to previous studies, this sample covers all morphological types
and is not biased toward late-type galaxies. These galaxies are part of the
Fabry-Perot kinematical $\it{GHASP}$ survey of spirals and irregular nearby
galaxies. Combining the kinematical data to the $\it{WISE}$ surface brightness
data probing the emission from the old stellar population, we derive mass
models allowing us to compare the luminous to the dark matter halo mass
distribution in the optical regions of those galaxies. Dark matter (DM) models
are constructed using the isothermal core profile and the Navarro-Frenk-White
cuspy profile. We allow the M/L of the baryonic disc to vary or we keep it
fixed, constrained by stellar evolutionary models (WISE W$_1$-W$_2$ color) and
we carry out best fit (BFM) and pseudo-isothermal maximum disc (MDM) models. We
found that the MDM provides M/L values four times higher than the BFM,
suggesting that disc components, on average, tend to be maximal. The main
results are: (i) the rotation curves of most galaxies are better fitted with
core rather than cuspy profiles; (ii) the relation between the parameters of
the DM and of the luminous matter components mostly depends on morphological
types. More precisely, the distribution of the DM inside galaxies depends on
whether or not the galaxy has a bulge.
