Models of cuspy triaxial stellar systems. IV: Rotating systems
  We built two self-consistent models of triaxial, cuspy, rotating stellar
systems adding rotation to non-rotating models presented in previous papers of
this series. The final angular velocity of the material is not constant and
varies with the distance to the center and with the height over the equator of
the systems, but the figure rotation is very uniform in both cases. Even though
the addition of rotation to the models modifies their original semiaxes ratios,
the final rotating models are considerably flattened and triaxial. An analysis
of the orbital content of the models shows that about two thirds of their
orbits are chaotic yet the models are very stable over intervals of the order
of one Hubble time. The bulk of regular orbits are short axis tubes, while long
axis tubes are replaced by tubes whose axes lie on the short-long axes plane,
but do not coincide with the major axis. Other types of regular orbits that do
not appear in non-rotating systems, like horseshoes and orbits that cross
themselves, are also found in the present models. Finally, our frequency maps
show empty regions where studies of orbits on fixed potentials found orbits, a
likely consequence of the self-consistency of our models that excludes them.
