A comparison of the stellar mass-(upper panel) and black hole mass-(lower panel) halo mass relation between simulations with varying values of ${ϵ}_{\mathrm{cr}}^{\mathrm{SNe}}$. Lower values effectively result in weaker CR pressure support in the halo, yielding a more realistic SMHM relation. However, the growth of SMBHs is still suppressed in all cases, due to high CR pressures in the very center regions of star-forming galaxies.