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Cosmological simulations predict dark matter shapes that deviate fromspherical symmetry. The exact shape depends on the prescription of thesimulation and the interplay between dark matter and baryons. This signature ismost pronounced in the diffuse galactic haloes that can be observationallyprobed with planetary nebulae and globular clusters (GCs). The kinematicobservations of these halo tracers support intrinsic triaxial shape for themass generating the gravitational potential. With discrete axisymmetricmodelling of GCs as the halo tracers of NGC 5128 we investigate the overallmass distribution of this nearby giant elliptical galaxy. Our modellingapproach constrains $c_{200}$, $(M/L)_{\star, B}$ and inclination. We derive apreliminary $M_{200}\sim 1 \times 10^{12}$ M$_\odot$ and flattening$q_{\mathrm{DM}}\sim 1.3$ indicative of prolate/triaxial halo for NGC 5128.

The flattening of dark matter halo of Centaurus A galaxy (NGC 5128) out to 40 kpc