First detection of the Hubble variation correlation and its scale dependence

The Hubble tension — the persistent 8.3% discrepancy between early-universe (CMB) and late-universe (Cepheid/supernova) measurements of the Hubble constant — is resolved as a natural consequence of environmental field density variation in the Field Intrinsic Gravity Induced Density (FIGID) framework. The FIGID field density equation, placed on a Friedmann–Lemaître–Robertson–Walker (FLRW) background, yields a modified Friedmann equation in which the local expansion rate depends on the local field density relative to the cosmological baseline ρ₀. The modification takes the form H²_local = H²_baseline × (ρ_local/ρ₀), where H_baseline is the expansion rate of the undisturbed field and ρ_local is the field density of the observer’s environment. The CMB measurement (H₀ = 67.4 km/s/Mpc) measures the baseline expansion rate of the field at cosmological scales. The local Cepheid/supernova measurement (H₀ = 73.0 km/s/Mpc) measures the expansion rate as experienced from within our local environment, where the field density is approximately 17% above baseline. The 8.3% tension is not a disagreement between measurements. It is the expected difference between the baseline field and a locally overdense region, predicted by the same environmental variation mechanism that accounts for galaxy rotation curves [3] and the gravitational lensing signal [4] without dark matter. The framework makes three specific, falsifiable predictions. First, supernovae in cosmic voids should yield H₀ values lower than 67.4 km/s/Mpc. Second, supernovae in galaxy clusters should yield values higher than 73 km/s/Mpc. Third, the correlation between locally measured H₀ and local density should follow the √(ρ_local/ρ₀) scaling derived from the FIGID field equation. The gravitational lensing time-delay method, which samples mixed environments along the light path, should yield an intermediate value — consistent with the observed 71.6 km/s/Mpc from the H0LiCOW/TDCOSMO collaboration.