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NGC 5128 is a well-studied elliptical galaxy with an excellent kinematic dataset for planetary nebulae which has been modelled up till now only by solvingthe Jeans equation for spherical systems. As a first approximation beyondspherical symmetry we model the galaxy as an axisymmetric system flattened byrotation with isotropic velocity distribution. We propose a new version of suchan isotropic rotator having cuspy density profile with NFW-like behavior. Thesolutions of the Jeans equations for a single component of such form do notreproduce the data well: the rotation curve rises too slowly with radius andthe velocity dispersion profile drops too fast. The data are well fittedhowever by a system built with two components: a more compact, flattened, lessmassive, fast-rotating and cold `bulge' and an extended, almost spherical, moremassive, slow-rotating and hot `halo'. This picture agrees well with theresults of recent N-body simulations of galaxy mergers which tend to produceoblate 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 +/- 17solar units.

NGC 5128 as an isotropic rotator