Similar to Fig. 7, but for the matter–matter spectrum (2). The power spectra are shown in the top row, while the response functions are shown in the bottom row. We see that the model is nearly perfect (errors at the sub-percent level) across a wide range of scales and for the different feedback scenarios. We see that the amount of power-spectrum suppression increases with the feedback temperature. The critical parameter that governs this in our modelling is the halo mass M₀, which governs the halo mass below which more than half of the cosmic baryon density is missing from the halo. In the fitting parameters we see a strong preference for higher values of M₀ for stronger feedback temperatures (from blue to red). How our model fares outside the range of AGN heating temperatures to which it was fitted is also shown via the lines that have no corresponding simulation points. To generate these we have interpolated and extrapolated our model parameters as a function of AGN heating temperature, which is shown in 0.1 dex intervals between 10^7.5 (bluest) and 10^8.1 K (reddest), indicating that our model is robust to extrapolation.