The Inner Structure of LambdaCDM Halos III: Universality and Asymptotic Slopes

Details The Inner Structure of LambdaCDM Halos III: Universality and Asymptotic Slopes The Inner Structure of LambdaCDM Halos III: Universality and Asymptotic Slopes

2003-11-11

arxiv.org/abs/astro-ph/0311231v2

Mon.Not.Roy.Astron.Soc.349:1039,2004

Astronomy and Astrophysics

Astrophysics

Minor editing changes to match version accepted for publication in MNRAS

Scientific paper

10.1111/j.1365-2966.2004.07586.x

We investigate the mass profile of LambdaCDM halos using a suite of numerical simulations spanning five decades in halo mass, from dwarf galaxies to rich galaxy clusters. Our analysis confirms the proposal of Navarro, Frenk & White (NFW) that the shape of LambdaCDM halo mass profiles differs strongly from a power law and depends little on mass. The logarithmic slope of the spherically-averaged density profile, as measured by beta=-dln(rho)/dln(r), decreases monotonically towards the center and becomes shallower than isothermal (beta<2) inside a characteristic radius, r_{-2}. Although the fitting formula proposed by NFW provides a reasonably good approximation to the density and circular velocity profiles of individual halos, systematic deviations from the best NFW fits are also noticeable. Inside r_{-2}, the profile of simulated halos gets shallower with radius more gradually than predicted and, as a result, NFW fits tend to underestimate the dark matter density in these regions. This discrepancy has been interpreted as indicating a steeply divergent cusp, but our results suggest a different interpretation. We use the density and enclosed mass at our innermost resolved radii to place strong constraints on beta_{0}: density cusps as steep as r^{-1.5} are inconsistent with most of our simulations, although beta_{0}=1 is still consistent with our data. Our density profiles show no sign of converging to a well-defined asymptotic inner power law. We propose a simple formula that reproduces the radial dependence of the slope better than the NFW profile, and so may minimize errors when extrapolating our results inward to radii not yet reliably probed by numerical simulations.

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