http://arxiv.org/abs/2305.09822
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.
T. Veršič, M. Rejkuba, M. Arnaboldi, et. al.
Thu, 18 May 23
22/67
Comments: 6 pages, 2 figures, Accepted for publication in Proceedings of the IAUS 379: Dynamical Masses of Local Group Galaxies, Potsdam, March 20-24, 2023