Triaxial Modeling of Halo Density Profiles with High-resolution N-body Simulations

Details Triaxial Modeling of Halo Density Profiles with High-resolution N-body Simulations Triaxial Modeling of Halo Density Profiles with High-resolution N-body Simulations

2002-02-04

arxiv.org/abs/astro-ph/0202064v5

Astrophys.J.574:538,2002

Astronomy and Astrophysics

Astrophysics

39 pages with 19 figures; final version match the publication in ApJ (Vol 574, 538, 2002)

Scientific paper

10.1086/341065

We present a detailed non-spherical modeling of dark matter halos on the basis of a combined analysis of the high-resolution halo simulations (12 halos with $N\sim 10^6$ particles within their virial radius) and the large cosmological simulations (5 realizations with $N=512^3$ particles in a $100h^{-1}$Mpc boxsize). The density profiles of those simulated halos are well approximated by a sequence of the concentric triaxial distribution with their axis directions being fairly aligned. We characterize the triaxial model quantitatively by generalizing the universal density profile which has previously been discussed only in the framework of the spherical model. We obtain a series of practically useful fitting formulae in applying the triaxial model; the mass and redshift dependence of the axis ratio, the mean of the concentration parameter, and the probability distribution functions of the the axis ratio and the concentration parameter. These accurate fitting formulae form a complete description of the triaxial density profiles of halos in Cold Dark Matter models. Our current description of the dark halos will be particularly useful in predicting a variety of nonsphericity effects, to a reasonably reliable degree, including the weak and strong lens statistics, the orbital evolution of galactic satellites and triaxiality of galactic halos, and the non-linear clustering of dark matter. In addition, this provides a useful framework for the non-spherical modeling of the intra-cluster gas, which is crucial in discussing the gas and temperature profiles of X-ray clusters and the Hubble constant estimated via the Sunyaev -- Zel'dovich effect.

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