Angle between the angular momentum of the gas in the halo and the stars in the galaxy, θ_a, as a function of the mass in the spheroidal component, f_sph, for galaxies in our sample. We show this at T_c for both disc-dominated samples and use z = 0 for the spheroid-dominated galaxies. Mostly-disc galaxies show a remarkable coherently aligned gas angular momentum with respect to that of the stars already formed at T_c, with a median cos(θ_a)∼0.95 and a few less well-aligned objects. The intermediate sample shows a preference for strong co-rotation of the components (cos(θ_a) > 0.5), but the angle between the angular momentum of gas and stars can be larger, even including counter rotation for a few objects. The spheroid-dominated galaxies are here for comparison only and show a wide range of misalignment.