  NGC 5128 is a well-studied elliptical galaxy with an excellent kinematic data
set for planetary nebulae which has been modelled up till now only by solving
the Jeans equation for spherical systems. As a first approximation beyond
spherical symmetry we model the galaxy as an axisymmetric system flattened by
rotation with isotropic velocity distribution. We propose a new version of such
an isotropic rotator having cuspy density profile with NFW-like behavior. The
solutions of the Jeans equations for a single component of such form do not
reproduce the data well: the rotation curve rises too slowly with radius and
the velocity dispersion profile drops too fast. The data are well fitted
however by a system built with two components: a more compact, flattened, less
massive, fast-rotating and cold `bulge' and an extended, almost spherical, more
massive, slow-rotating and hot `halo'. This picture agrees well with the
results of recent N-body simulations of galaxy mergers which tend to produce
oblate rotating spheroids. The total mass of the system is estimated to be (9.1
+/- 3.5) x 10^11 solar masses and the mass-to-light ratio is only 26 +/- 17
solar units.
