  The Hubble classification scheme of galaxies is based on blue-light
appearance. Atlases reveal the rich variety of responses of the Population I
component (the "mask") of gas and dust to the underlying, older, stellar
population. However, the Population I component may only constitute 5 percent
of the dynamical mass of the galaxy; furthermore, dusty masks are highly
effective in hiding bars. In the 1960s, Ken Freeman presented a meticulous
study of the dynamics of bars at a time when nonbarred galaxies were called
"normal" spirals and barred galaxies were regarded as curiosities. Now we know
that it is more "normal" for a galaxy to be barred than to be nonbarred. What
is the range for gravitational torques of bars? We describe here a recently
developed method for deriving relative bar torques by using gravitational
potentials inferred from near-infrared light distributions. We incorporate a
bar torque class into the Block/Puerari dust-penetrated galaxy classification
system. We find a huge overlap in relative bar torque between Hubble (Sa, Sb,
  ...) and (SBa, SBb, ...) classifications. Application of the method to the
high redshift universe is briefly discussed.
