The early universe built billion-solar-mass black holes faster than ΛCDM growth allows. QSO J0313-1806 hosts a 1.6 billion solar mass black hole at z = 7.642, when the universe was under 700 million years old: starting from any stellar-mass seed, continuous Eddington-limited accretion cannot assemble that mass in the time available even if seeding began at z = 30. UHZ1 at z near 10.1 shows a black hole whose mass rivals its host galaxy's entire stellar content, and the JWST era has multiplied such cases: black-hole-to-stellar-mass ratios run 10 to 1000 times above the local Magorrian relation, with overmassive central objects appearing as early as observations can reach.
ΛCDM has no seeding mechanism that fits. Population III stellar remnants top out near 100 solar masses and would need sustained super-Eddington growth with implausibly perfect duty cycles; direct-collapse black holes from pristine atomic-cooling halos can reach 10^4 to 10^6 solar masses but require finely tuned conditions, metal-free gas bathed in strong Lyman-Werner radiation, expected to be vanishingly rare, far rarer than the observed population now demands. Heavy seeds of 10^8 solar masses and above, which the demographics increasingly point toward, have no standard formation channel at all. Each JWST discovery cycle has moved the required seed masses up and the available growth time down.
The standing is a hard timing crisis at the heart of structure formation: the model must either produce heavy seeds it has no mechanism for, sustain super-Eddington accretion it has no stable physics for, or accept that the first billion years contained a black hole formation channel outside the standard picture. Euclid and Roman quasar censuses and JWST spectroscopy of the overmassive population will quantify exactly how heavy and how early the seeds must be.