On The Rapid Early Growth of the CANUCS-LRD- z8.6 Black Hole

This work examines the unexpectedly large mass of the supermassive black hole in the CANUCS-LRD-z8.6 galaxy, observed only about 570 million years after the Big Bang. Standard accretion models require either unusually massive primordial seeds or prolonged super-Eddington growth to explain a ~100-million-solar-mass black hole at such an early cosmic epoch. The analysis presented here explores a different possibility: that the extreme mass arises from a dependence of inertial mass on a coherence factor of the spacetime–energy configuration. In this framework, moderate changes in coherence can lead to large increases in effective mass even when the available energy supply is relatively modest. When applied to CANUCS-LRD-z8.6, the model shows that a typical modal-energy reservoir, combined with reduced coherence in the young universe, is sufficient to reproduce the observed black-hole mass without requiring heavy primordial seeds or sustained super-Eddington accretion. The work also provides observational predictions that allow the mechanism to be tested: (1) elevated and dispersed black-hole-to-stellar-mass ratios at high redshift, (2) a transitional regime around redshifts 3–6 as coherence stabilizes, and (3) convergence toward the local scaling relation at low redshift. In this interpretation, the CANUCS-LRD-z8.6 black hole is not an anomaly, but a natural outcome of a low-coherence phase of the early universe.