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

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 $c_{200}$, $(M\mathrm{/}L{)}_{\star ,B}$ and inclination. We derive a preliminary $M_{200}\sim 1\times {10}^{12}$ M${}_{\odot }$ and flattening $q_{\mathrm{D}\mathrm{M}}\sim 1.3$ indicative of prolate/triaxial halo for NGC 5128.