Clustering Scale of a Spin-Fluid Dark Component: Where Torsion Pressure Would Smooth Structure

A dark component with pressure does not cluster on all scales. This paper computes the smoothing scale for a spin-fluid dark component whose effective sound speed is set by the ratio of the local density to the density limit. At halo and cosmic densities that ratio is extremely small, so the predicted smoothing length lies far below any scale on which galaxy surveys or the Lyman-alpha forest measure structure. The component would therefore cluster effectively like pressureless matter for observational purposes. The same calculation shows the density a region would need to reach before torsion pressure altered its collapse, placing that threshold far above the densities of halos, filaments, and clusters. Headline values are: ratio halo = 1.029e-79, smoothing halo m = 6.598e-16, ratio halo system = 1.100e-36, density for order unity ratio kg m3 = 9.718e+57. This study is simulated and computed from stated assumptions; it is not a measurement.