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Observations of the most luminous quasars at high redshifts ($z > 6$) haverevealed that the largest supermassive black holes (SMBHs) at those epochs tendto be substantially overmassive relative to their host galaxies compared to thelocal relations, suggesting they experienced rapid early growth phases. Wepropose an assembly model for the SMBHs that end up in rare massive$\sim10^{12}~M_{\odot}$ host halos at $z \sim 6-7$, applying a kinetic feedbackprescription for BHs accreting above the Eddington rate, provided by radiationhydrodynamic simulations for the long-term evolution of the accretion-flowstructure. The large inflow rates into these halos during their assembly enablethe formation of $>10^9~M_{\odot}$ SMBHs by $z \sim 6$, even starting fromstellar-mass seeds at $z \sim 30$, and even in the presence of outflows thatreduce the BH feeding rate, especially at early times. This mechanism alsonaturally yields a high BH-to-galaxy mass ratio of $> 0.01$ before the SMBHmass reaches $M_{\rm BH} > 10^9~M_{\odot}$ by $z \sim 6$. These fast-growingSMBH progenitors are bright enough to be detected by upcoming observations withthe James Webb Space Telescope over a wide range of redshift ($7 < z < 15$),regardless of how they were seeded.

Supercritical growth pathway to overmassive black holes at cosmic dawn: coevolution with massive quasar hosts