Median LOS velocity distribution at galactocentric distances of ∼35 (Upper) and 12.2 (bottom) kpc along the major axis for MW/M31 like galaxies in an edge-on configuration, in the TNG50 (blue) and Auriga (orange) simulations. Black vertical lines are our velocity measurements for NGC 4945 at those distances, corrected for its systemic velocity. Green and pink dotted vertical lines show the halo rotational velocity of the MW (halo and outer disk, Deason et al. 2017; Bland-Hawthorn & Gerhard 2016 respectively) and M31 (halo and outer disk, Ibata et al. 2005; Zhang et al. 2024, respectively). Our velocity measurements of the stellar halo of NGC 4945 at ∼35 kpc are in agreement with those of the accreted component of the simulated galaxies at ∼35 kpc. At a distance of 12.2 kpc simulations show that our results are consistent with the disk in situ component dominating the field, with little contribution from the accreted component.