Same as Fig. C.1 but for M_*, the halo mass at which star formation efficiency peaks. Changing this parameter shifts the halo-stellar-mass fraction to lower and higher masses, as can be seen in the bottom-right panel, there is a small back-reaction effect on the gas abundance. Changing M_* indirectly affects the halo profiles at different masses, as can be seen in the top right panel, but note that the delta-function component of the stellar halo profile is not shown in this plot. The power spectra involving stars are affects in a more scale-dependent manner as can be seen in the top-left two panels.