(First and third panels) Time evolution of the fractional impact of baryonic physics on the MPS at scales of |$k_\text{scale} = 10\, \,\,\text{h}\,\,\text{cMpc}^{-1}$| and |$k_\text{scale} = 1\, \,\,\text{h}\,\,\text{cMpc}^{-1}$|⁠, respectively. The solid lines displays |$P_\text{mm}$|⁠, whereas the dashed line correspond to the MPS of all matter within all haloes |$P_\text{mm, halos}$|⁠. Note that the |$P_\text{mm, halos}$| is not shown in the third panel, as it falls well below the displayed range. (Second and fourth panels) relative difference between |$P_\text{mm}$| and |$P_\text{mm, halos}$| (⁠|$\Delta P = P_\text{mm}-P_\text{mm, halos}$|⁠) for each model, at both |$k_\text{scale} = 10\, \,\,\text{h}\,\,\text{cMpc}^{-1}$| and |$k_\text{scale} = 1\, \,\,\text{h}\,\,\text{cMpc}^{-1}$|⁠, respectively. The impact of AGN feedback on |$P_\text{mm, halos}$| is responsible for most suppression of power observed in |$P_\text{mm}$| for |$k_\text{scale} = 10\, \,\,\text{h}\,\,\text{cMpc}^{-1}$| at |$z \lesssim 1$|⁠. At higher redshifts, the contribution of baryonic effects outside haloes becomes important (⁠|$>10~{{\ \rm per\ cent}}$|⁠). Precision modelling of |$P_\text{mm}\left(k_\text{scale} = 1\, \,\,\text{h}\,\,\text{cMpc}^{-1}\right)$| in the fable suite also requires accurate characterization of AGN feedback effects both within and outside haloes.