The Michalski Kernel

The Michalski Kernel introduces a scale-invariant, non-local gravitational field model that addresses persistent residuals in dark matter mass profile fitting across galaxy cluster environments. By treating the dark sector background as a dynamic fluid component rather than a static geometric prior, the framework achieves significant fit improvements over standard Navarro-Frenk-White (NFW) profiles in high-entropy cluster merger environments. Observational analyses against neutral Hubble Frontier Fields (HFF) data demonstrate a 2.46x chi-squared improvement at Abell 2744 (NFW χ²=37.66, Michalski χ²=15.28) and 2.48x at MACS J0717 (NFW χ²=182.96, Michalski χ²=73.76), with consistent improvements across galactic rotation curve targets including M31. The framework proposes that Dark Matter and Dark Energy represent two thermodynamic states of a unified underlying field, with entropy governing transitions between localized geometric and diffuse vacuum floor configurations. A localized vacuum energy surplus approximately 3,200 times the cosmological constant is identified in high-entropy merger zones, offering a candidate mechanical contributor to Hubble Tension variances. The normalization integral and scaling parameters are published in full for independent replication.