Comparison between BAHAMAS and BCM power spectra. Left panel, top: Matter power spectrum suppression S (k) measured at ɀ = 0 in three BAHAMAS simulations, with an AGN temperature of T_AGN = 10^7.6, 10^7.8, and 10^8.0 K (red, green, and blue circles, respectively). As solid lines, we show the respective predictions of baryoniflcation when simultaneously fitting the S (k), the electron pressure, and the matter-electron pressure power spectra of each simulation. Left panel, bottom: Ratio of power spectra measured in our baryonified simulations to the BAHAMAS ones, for matter (solid lines), electron pressure (dashed lines), and the matter–electron pressure cross (dotted lines). Right panel: Power spectra of matter, dark matter, gas, galaxy, electron pressure (in units of eV cm⁻³), and matter-electron pressure, measured in BAHAMAS AGN tuned at ɀ = 0 (circles; colours are as described in the legend). We show the baryoniflcation fits to the total matter and electron pressure auto- and cross-correlation with dashed lines, and a simultaneous fit to all the power spectra with solid lines.