Median values of the RMP slopes, α, for each simulation used in this work as a function of |$\dot{M}_{\rm accr}$|⁠. Top and bottom panels show galaxies at z = 0 and 1, respectively. The left- and right-hand panels depict different regions of the galaxies, as labelled. Galaxies are colour-coded by the simulation they are generated with, being red for Recal-L25N752 and blue for Ref-L100N1504. Dashed lines depict the 16th–84th percentiles. We show individual galaxies where bins have fewer than 10 objects (circles). The RMP slope in the inner region (r/r₅₀ ≤ 1) is negative and it is tightly correlated with |$\dot{M}_{\rm accr}$| for both simulations at all redshifts analysed, becoming more negative for higher |$\dot{M}_{\rm accr}$|⁠. The Recal-L25N752 simulation shows a more negative slope, especially for higher values of |$\dot{M}_{\rm accr}$|⁠. At larger radii (1 < r/r₅₀ ≤ 5), we find a weaker correlation between α and |$\dot{M}_{\rm accr}$| with much larger scatter, with values of α ≈ −0.08. As explained in Section 2.2, the cuts in stellar mass for our galaxy samples are M_⋆ ≥ 10⁹ M_⊙ for Recal-L25N752 and M_⋆ ≥ 10¹⁰ M_⊙ for Ref-L100N1504. The difference in mass accounts for most of the difference between the simulations (see Section 3.3). Note that the y-axis range changes from the left- to the right-hand panels, which is done to better highlight the values spanned by the data.