What a black-hole identification would require

A physical successor must supply:

1. a named microscopic gravitational theory and a source input space with a justified encoding;

2. an independently motivated interaction law, rather than a designed private-channel circuit;

3. the relation of emitted degrees of freedom to local or asymptotic field observables, including species and angular resolution;

4. collapse, propagation, and accessible-mode identification;

5. the regime of validity, approximation topology, renormalization where relevant, and remainder estimates;

6. a receiver coupling and calibrated coherent-access model.

The compact-test peeling estimate in Em03-A is not a collapse packet theorem. The effective port of Em03-B–C is not a local Schwarzschild detector. Neither missing identification is supplied by the finite exchange interactions here.