Comparison of the results from the Schwarzschild modelling fits to the observed velocity dispersion along the major (left column) and minor (right column) axis. From top to bottom: best-fit Evans (red line) and Vogelsberger (blue line) models for kinematic datasets containing N = 10⁵, N = 10⁴, and 2000 stars, respectively. The shaded regions denote the error bands computed as described in the text. Black dotted lines indicate the input (theoretical, Eq. (4)) velocity dispersions.