Structure and History of Dark Matter Halos Probed with Gravitational Lensing

TL;DR

This paper uses gravitational lensing data to test models of dark matter halos in galaxy clusters, deriving ta-profiles from Jeans equations that align well with observations and simulations.

Contribution

It introduces physically motivated ta-profiles based on the Jeans equation, providing a better fit to lensing data than the empirical NFW profile.

Findings

ta-profiles fit lensing data well at different scales.

The halo in A1689 has a mass of about 10^15 solar masses.

The concentration parameter c  10 is consistent with ta-profile predictions.

Abstract

We test with gravitational lensing data the dark matter (DM) halos embedding the luminous baryonic component of galaxy clusters; our benchmark is provided by their two-stage cosmogonical development that we compute with its variance, and by the related '\alpha-profiles' we derive. The latter solve the Jeans equation for the self-gravitating, anisotropic DM equilibria, and yield the radial runs of the density \rho(r) and the velocity dispersion \sigma_r^2(r) in terms of the DM 'entropy' K = \sigma_r^2/\rho^(2/3) ~ r^(\alpha) highlighted by recent N-body simulations; the former constrains the slope to the narrow range \alpha ~ 1.25 - 1.3. These physically based \alpha-profiles meet the overall requirements from gravitational lensing observations, being intrinsically flatter at the center and steeper in the outskirts relative to the empirical NFW formula. Specifically, we project them along the l.o.s. and compare with a recent extensive dataset from strong and weak lensing observations in and around the cluster A1689. We find an optimal fit at both small and large scales in terms of a halo constituted by an early body with \alpha ~ 1.25 and by recent extensive outskirts, that make up an overall mass 10^15 M_sun with a concentration parameter c ~ 10 consistent with the variance we compute in the \LambdaCDM cosmogony. The resulting structure corresponds to a potential well shallow in the outskirts as that inferred from the X rays radiated from the hot electrons and baryons constituting the intracluster plasma.