This article develops a theoretical framework in which part of the large-scale gravitational phenomena commonly attributed to dark matter are interpreted as an effective infrared response of the vacuum to the ordinary gravitational potential. Rather than introducing a new collisionless matter component or modifying the local Poisson equation, the model assumes a scale-dependent vacuum susceptibility in Fourier space. Under approximate infrared scale invariance, this response leads to a marginal kernel of the form χ(k)∝1/k, regularized by a log-Gaussian coherence window f(k). The resulting mechanism produces extended nonlocal gravitational contributions that can account, at an effective level, for quasi-isothermal halo profiles, approximately flat galactic rotation curves, MOND-like intermediate scaling without introducing a new universal acceleration constant, and filamentary bridge-like structures between nearby galaxy clusters. The paper also discusses empirical bounds inferred from typical galactic and cluster scales, and frames the model as a step toward a more fundamental gravitational description based on infrared metric fluctuations, while remaining non-relativistic at this stage.
Daniel Bensaid (Sun,) studied this question.