Rotation velocity v_ϕ = j_z/R of young stars (i.e. ages < 1 Gyr, magenta dots) and circular velocity $V_{\mathrm{circ}}=\sqrt{GM(<r)/r}$ (black dashed lines) for the four example galaxies (A, B, C, and D) from Figure 1. Bottom panels show the ratio v_ϕ/V_circ (magenta solid line with circles) as a function of galactocentric distance. Except for the least massive galaxy (A), all have young stars in highly circular orbits at radii of r ≳ 2 kpc. Conversely, stellar particles with low tangential velocities are found in the inner regions (r < 1 kpc). As previously shown, higher mass galaxies have more stars born in the outer regions.