Same as Fig. C.1 but for M₀, which governs the halo mass below which haloes have lost most of their gas. As can be seen in the bottom-right panel, changing M₀ changes the split of gas between the bound component, which dominates high-mass haloes and the unbound component, which is the case for low-mass haloes that have jettisoned most of their gas. The effects of this on the bound halo profiles can be seen in the top-right panel. Decreasing M₀ adds to the amplitude of the gas density profiles and this boosts power in power spectra involving gas. We see a similar, but more limited effect on spectra involving the electron pressure. This limitation arises because low-mass haloes are lower temperature, so contribute much less to spectra involving the electron pressure than they do to those involving the gas density. There is also an overall amplitude affect on the pressure spectra because the unbound gas is taken to have a fixed T_w = 10⁶ K that contributes power on large scales.