Distribution Function in Center of Dark Matter Halo

Abstract

N-body simulations of dark matter halos show that the density profiles of halos behave as $\rho (r)\propto r^{-\alpha (r)}$, where the density logarithmic slope $\alpha \simeq 1\sim 1.5$ in the center and $\alpha \simeq 3\sim 4$ in the outer parts of halos. However, some observations are not in agreement with simulations in the very central region of halos. The simulations also show that velocity dispersion anisotropy parameter $\beta \approx 0$ in the inner part of the halo and the so called "pseudo phase-space density" $\rho /{\sigma }^3$ behaves as a power-law in radius $r$. With these results in mind, we study the distribution function and the pseudo phase-space density $\rho /{\sigma }^3$ of the center of dark matter halos and find that they are closely-related.

8 pages, accepted by Int. J. Mod. Phys. D, add a quotation and remove the appendix

References in corpus (7)

• A universal density slope - velocity anisotropy relation for relaxed structures
• Angular Momentum Transfer in Dark Matter Halos: Erasing the Cusp
• Hiding Cusps in Cores: Kinematics of Disk Galaxies in Triaxial Dark Matter Halos
• On Universal Halos and the Radial Orbit Instability
• Evolution of Phase-Space Density in Dark Matter Halos
• Density Profiles of Collisionless Equilibria. II. Anisotropic Spherical Systems
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Cited by in corpus (1)

• Structural and dynamical modeling of WINGS clusters. III. The pseudo phase-space density profile