  We present a comparison between ionized gas and stellar kinematics for a
sample of 5 early-to-intermediate disc galaxies. We measured the major axis V
and sigma radial profiles for both gas and stars, and the h3 and h4 radial
profiles of the stars. We also derived from the R-band surface photometry of
each galaxy the light contribution of their bulges and discs.
  In order to investigate the differences between the velocity fields of the
sample galaxies we adopted the self-consistent dynamical model by Pignatelli &
Galletta (1999), which takes into account the asymmetric drift effects, the
projection effects along the line-of-sight and the non-Gaussian shape of the
line profiles due to the presence of different components with distinct
dynamical behavior. We find for the stellar component a sizeable asymmetric
drift effect in the inner regions of all the sample galaxies, as it results by
comparing their stellar rotation curves with the circular velocity predicted by
the models.
  The galaxy sample is not wide enough to draw general conclusions. However, we
have found a possible correlation between the presence of slowly-rising gas
rotation curves and the ratio of the bulge/disc half luminosity radii, while
there is no obvious correlation with the key parameter represented by the
morphological classification, namely the bulge/disc luminosity ratio. Systems
with a diffuse dynamically hot component (bulge or lens) with a scale length
comparable to that of the disc are characterized by slowly-rising gas rotation
curves. On the other hand, in systems with a small bulge the gas follows almost
circular motions, regardless of the luminosity of the bulge itself.
