The Quasar Luminosity Function evolves across cosmic time with luminous quasars peaking at z ≈ 2 to 3 and declining sharply toward z > 6. Recent observations reveal surprisingly high density of 10⁹ M☉ SMBHs already in place at z ≈ 7, requiring rapid assembly that strains standard models. Reconciling the QLF shape evolution + faint-end slope + bright-end slope simultaneously demands continuous super-Eddington accretion or massive seeds within ΛCDM.
The standard model has SMBHs grow from light stellar-remnant seeds through Eddington-limited accretion. Reaching the observed bright-end QLF abundance at z > 6 demands either super-Eddington accretion (which violates radiation-pressure constraints) or massive seeds (10 to 10⁵ M☉ at z > 30 with no formation mechanism). Neither is parsimonious within minimal ΛCDM.
SCT replaces the hot-dense-center with a superluminal collision and the thermalized debris field. From this single change, the high-z quasar luminosity function emerges naturally from cascade-seeded SMBH demographics. Cascade-direct-collapse SMBH seeds (P46) deposit 10⁷ to 10⁹ M☉ SMBHs directly through head-on cascade collisions (recid 109), giving the substantial bright-end abundance observed at z ≈ 7 without invoking super-Eddington accretion or anomalously massive stellar-remnant seeds.
Pre-existing matter from prior cycles (P25, P28) supplies the cascade-seeded gas reservoirs that fuel ongoing AGN activity at the cascade-deposition epoch. Multi-stage cascade dynamics (P36) sets the cosmic-web filament infrastructure where these AGN sit, naturally producing the QLF spatial clustering seen at high z (recid 174). The bright-end slope is steepened by the cascade-direct-collapse seed-mass distribution, and the faint-end slope reflects the broader cascade-seeded compact-object population that includes lower-mass cascade-seeded SMBHs.
The QLF declines sharply at z > 6 not because SMBHs are still being assembled hierarchically, but because the cascade-seeded bright-AGN-fueling phase ends as the cascade-deposited gas reservoirs are consumed by accretion or driven away by AGN feedback. The same M1 framework that resolves the JWST early-galaxy mass crisis (recid 7, 108), the SMBH-seed problem (recid 109), high-z quasar clustering (recid 174), and the cosmic-noon star formation cliff (recid 121) accounts for the QLF evolution without super-Eddington requirements.
If precision JWST + Roman + Euclid + Athena high-z AGN surveys find QLF evolution and bright-end abundance fully consistent with hierarchical-galaxy-driven SMBH seed-and-grow predictions at the 5% level (no cascade-seeded direct-collapse signature), the M1 cascade-seeded explanation is refuted. The signature SCT prediction is the bright-end QLF abundance matching the cascade-seeded SMBH demographics from P46.