  Cosmological simulations predict dark matter shapes that deviate from
spherical symmetry. The exact shape depends on the prescription of the
simulation and the interplay between dark matter and baryons. This signature is
most pronounced in the diffuse galactic haloes that can be observationally
probed with planetary nebulae and globular clusters (GCs). The kinematic
observations of these halo tracers support intrinsic triaxial shape for the
mass generating the gravitational potential. With discrete axisymmetric
modelling of GCs as the halo tracers of NGC 5128 we investigate the overall
mass distribution of this nearby giant elliptical galaxy. Our modelling
approach constrains $c_{200}$, $(M/L)_{\star, B}$ and inclination. We derive a
preliminary $M_{200}\sim 1 \times 10^{12}$ M$_\odot$ and flattening
$q_{\mathrm{DM}}\sim 1.3$ indicative of prolate/triaxial halo for NGC 5128.
