Same as Fig. C.1 but for σ_*, which governs the width of the stellar-mass distribution around the peak (which is at M_* = 10^12.5 h⁻¹ M_⊙ here). As can be seen in the bottom-left panel, decreasing σ_* shrinks the stellar-mass distribution, resulting in fewer stars in both higher and lower mass haloes than M_*. The top-right panel shows that this has the biggest impact on 10¹⁴ h⁻¹ M_⊙ haloes, not higher-mass haloes due to the saturation we impose at high masses. In the left-hand panels we see that the effects of this are constrained to be on power spectra involving the stars. There is only a tiny effect on gas spectra which is due to baryonic mass conservation.