The Hubble Constant and "Too Big, Too Early" Galaxies Under a Static, Variable-Speed-of-Light Universe: A Consolidated Reassessment

This paper reports a consolidated, self-contained treatment of two open questions in the Pixel Theory (PT) research programme: the value of the Hubble constant under every PT model variant fitted to date, and the "too big, too early" galaxy problem exemplified by JADES-GS-z14-0 (z = 14.1793, ALMA-refined from the original z = 14.32 estimate). It supersedes two earlier, narrower treatments of the same two questions, now withdrawn (Section 1). On the Hubble constant, we report every joint Pantheon+/DESI/CMB fit attempted across four functional forms of the residual-expansion parameter p_a and two conventions for hbar and l_P, none of which converges on either of the two real measurements (SH0ES local, ~73.0 km/s/Mpc; Planck CMB, ~67.4 km/s/Mpc); the best of the CMB-consistent fits (H0 ~ 33-36 km/s/Mpc) remains roughly half the observed value, and we say so plainly. On the too-big-too-early problem, we derive high-redshift stellar luminosity from PT's own stellar-structure physics: hydrostatic equilibrium, the ideal gas law, and radiative diffusion, with PT's own G, m_p and hbar scaling carried through symbolically, giving a predicted suppression of stellar luminosity at this redshift of ~0.066 (15-fold), a result close enough to unity to be a genuine, load-bearing prediction rather than a rounding artefact. We report honestly that the same physics predicts a roughly 10^4-fold increase in stellar lifetime at this redshift, worsening rather than resolving a separate, related tension over how many generations of heavy-element enrichment could have occurred, and that this specific tension is not addressed by real-universe "feedback-free starburst" efficiency arguments, which operate on a different stage of galaxy formation. Three further checks, built directly from this paper's own fits, sharpen the honest-verdict framing adopted throughout: an implied-age check on the CMB-consistent H0 branch this paper prefers (Section 2.4a), a coordinate-time budget check for JADES-GS-z14-0 itself (Section 3.5a), and two object-specific tests against real 2025-2026 JWST/ALMA data (JADES-GS-z14-0's own measured heavy-element enrichment, Section 3.7, and two Population III star candidates, Section 3.8), both of which sharpen rather than resolve the stellar-lifetime tension.