The Density Parity Model for the Evolution of the Subhalo Inner Spin Alignments with the Cosmic Web

Abstract

Abstract We develop a new model within which the radius-dependent transition of the subhalo inner spins with respect to the cosmic web and the variation of the transition threshold radius (r th) with subhalo mass (M vir), smoothing scale (r f ), and redshift (z) can be coherently explained. The key tenet of this model is that the competition between the pressure effect of the inner mass and the compression effect of the local tidal field determines which principal direction of the tidal field the inner spins are aligned with. If the former predominates, then only the tidal torques turn on, resulting in the alignments of the inner spins with the intermediate principal axes of the tidal field. Otherwise, the subhalo spins acquire a tendency to be aligned with the shortest axes of the subhalo shapes, which is in the major principal directions of the tidal field. Quantifying the two effects in terms of the densities, we make a purely analytical prediction for r th (M vir, z, r f ). Testing this model against the numerical results from a high-resolution dark-matter-only N-body simulation in the redshift range of 0 ≤ z ≤ 3 on the galactic mass scale of 11.8 ≤ log M vir / ( h − 1 M ⊙ ) ≤ 12.6 for two different cases of r f /(h -1 Mpc) = 0.5 and 1, we find excellent agreements of the model predictions with the numerical results. It is also shown that this model naturally predicts the alignments between the inner spins of the present subhalos with the principal axes of the high-z tidal field at the progenitors’ locations.