Luminous quasars at redshift 6 and beyond cluster far more strongly than their abundance should allow. The EIGER JWST survey measured the quasar-galaxy cross-correlation at z above 6 and inferred host halo masses around 10^12.3 solar masses with duty cycles approaching unity (arXiv:2403.07986): essentially every sufficiently massive halo must host an actively shining quasar, leaving no room for the dormant majority that black hole demographics at every later epoch require. Wide-field clustering analyses reach similar minimum halo masses, and the inferred correlation lengths rival those of the most biased populations known. Simultaneously, JWST environment studies complicate the picture from the other side: [O III]-emitter counts around z of 6 to 7 quasars range from density enhancements of 65 down to fields consistent with average density, and two quasars at z of 7.3 show no galaxy excess at all.
ΛCDM is squeezed from both directions at once. Strong clustering plus high luminosity demands that quasars occupy the rarest halos with implausible unanimity, while the average-density detections show luminous quasars living where the rarest halos are not, which under abundance matching should be nearly impossible. The combination, strong statistical clustering with enormous object-to-object environmental scatter, does not fit a picture in which black hole mass and activity are tight functions of host halo mass; something other than halo rank is deciding where the brightest early quasars sit and shine.
The standing is statistics-limited and rapidly evolving: samples are small, fields are few, and cosmic variance is severe, with ASPIRE, EIGER extensions, and wide JWST/Euclid programs steadily enlarging the census. The tension already on the books is the duty-cycle crisis: clustering says the halos are rare and always on, demographics say black holes spend most of their time off.