Redshift evolution of the fractional impact of baryonic physics on the MPS of all haloes in each simulation. Displayed quantities and simulations are the same as Fig. 3, except now we show |$P_\text{mm, halos}/P_\text{mm, DMO}$| instead of |$P_\text{mm}/P_\text{mm, DMO}$|⁠. Panels show the Fiducial (top left), RadioWeak (top right), Quasar (bottom left), and RadioStrong (bottom right) feedback models, respectively. The qualitative behaviour of the Quasar model being more efficient at higher redshift and the RadioStrong AGN more important at late times is also reproduced. The power of haloes has a subdominant contribution to |$P_\text{mm}$| at large scales (⁠|$k \sim 1\, \,\,\text{h}\,\,\text{cMpc}^{-1}$|⁠), and evolves approximately equivalently in all models.