The Shadow of a Bounced Core: Event Horizon Telescope Imaging of Supermassive Objects in the Aldred Frame

In Einstein-Cartan spin-torsion gravity, in the frame defined by the Aldred Limit rho_A = 9.72e54 g/cm^3, gravitational collapse halts at finite density and leaves a bounced core of radius R_A(M) = [3M/(4 pi rho_A)]^(1/3) in place of a singularity. This paper prices the imaging channel for that statement: what the Event Horizon Telescope (EHT) would see if the supermassive objects M87* and Sgr A* contain such cores, under stated assumptions (Kerr exterior at and outside the photon sphere; core surface at R_A(M); no surface optical coefficient assumed). The result is a narrowing of the premise: at these masses the bounced core is not horizonless. R_A/r_s = 3.55e-20 for M87* and 4.68e-18 for Sgr A*, so the core sits deep inside its Schwarzschild radius, below the Buchdahl radius, and a horizon and photon sphere stand in the exterior exactly as for a Kerr black hole. The predicted shadow is therefore the Kerr shadow identically (37.0-39.7 microarcsec for M87*, 49.7-53.3 microarcsec for Sgr A*, over all spins and inclinations), a fractional difference from Kerr of 0.00%. Published EHT measurements sit on the prediction (pulls -0.68 sigma to +0.65 sigma across five comparisons); current uncertainties can exclude a deviation from Kerr only above about 26% (M87*) and 29% (Sgr A*). The photon-ring substructure difference from Kerr is exactly zero, with the n=1 subring narrower than 0.91 microarcsec at M87* and unresolvable by any Earth-diameter array including the next-generation EHT; the interior surface emission is exactly zero because the surface lies inside the horizon. The imaging channel contains no test of the density cap at these masses. All numbers are produced by the deposited compute.py. AI-use disclosure: this paper was drafted and computed with the assistance of Dave, an AI assistant operated by Aldred Industries, under the direction of the author.