Distributions of the latitudinal component of the velocity, |v_θ|, in Newtonian gravity and in QUMOND for 4 M_⊙ HVSs. Left panel: distributions of |v_θ| for different models of the Galactic potential: Newtonian gravity with a spherical dark matter halo (gray shaded histogram) and QUMOND with γ = 1 (orange histogram) and γ = 2 (red histogram). As the gravitational pull of the baryonic disk is enhanced in QUMOND, the fraction of HVSs with high |v_θ| is larger than in Newtonian gravity with a spherical halo. Right panel: distributions of |v_θ| for three different shapes of the dark matter halo in Newtonian gravity. The three halos have q_y = 1 but different q_z: a spherical halo with q_z = 1 (gray shaded histogram), a prolate halo with q_z = 1.1 (blue histogram), and an oblate halo with q_z = 0.9 (red histogram). An oblate halo enhances the gravitational pull of the baryonic disk, as shown by the larger fraction of HVSs with high |v_θ| and the smaller fraction of HVSs with low |v_θ| (compare the shaded and red histograms). The opposite occurs with a prolate halo (compare the shaded and blue histograms).