Power law pseudo phase-space density profiles of dark matter halos: fluke of physics?

Abstract

It has been known for nearly 20 years that the pseudo phase-space density profile of equilibrium simulated dark matter halos, $\rho (r)/{\sigma }^3(r)$, is well described by a power law over 3 decades in radius, even though both the density $\rho (r)$, and the velocity dispersion $\sigma (r)$ deviate significantly from power laws. The origin of this scale-free behavior is not understood. It could be an inherent property of self-gravitating collisionless systems, or it could be a mere coincidence. To address the question we work with equilibrium halos, and more specifically, the second derivative of the Jeans equation, which, under the assumptions of (i) Einasto density profile, (ii) linear velocity anisotropy - density slope relation, and (iii) $\rho /{\sigma }^3\propto r^{-\alpha }$, can be transformed from a differential equation to a cubic algebraic equation. Relations (i)-(iii) are all observed in numerical simulations, and are well parametrized by a total of 4 or 6 model parameters. We do not consider dynamical evolution of halos; instead, taking advantage of the fact that the algebraic Jeans equation for equilibrium halos puts relations (i)-(iii) on the same footing, we study the (approximate) solutions of this equation in the 4 and 6 dimensional spaces. We argue that the distribution of best solutions in these parameter spaces is inconsistent with $\rho /{\sigma }^3\propto r^{-\alpha }$ being an fundamental property of gravitational evolution, and conclude that the scale-free nature of this quantity is likely to be a fluke.

arXiv commentApJ, Accepted

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• Self-gravitating Equilibria of Non-minimally Coupled Dark Matter Halos
• Shaping the Milky Way: The interplay of mergers and cosmic filaments
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• Scaling Relations in the Phase-Space Structure of Dark Matter Haloes