  We present stellar and ionized-gas velocity curves and velocity dispersion
profiles for the Sa galaxies NGC 2179 and NGC 2775. Using their luminosity
profiles and modeling both their stellar and gaseous kinematics, we have
derived the mass distribution of the dark and the luminous matter.
  This unambiguously shows that, inside one disk length-scale R_D, the stellar
bulge and disk account for the whole gravitating mass. The dark matter halo,
likely present also at inner radii, becomes an important mass component only
for R > 2 R_D. Giving the quantity and quality of the data, our results on
these two luminous galaxies serve as strong counter-example to the recent claim
according to which also high-luminosity spirals are dark matter dominated at
essentially all radii.
