Triaxial Modeling of Halo Density Profiles with High‐ResolutionN‐Body Simulations

Abstract

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 ∼ 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.

Exploring the liminality: properties of haloes and subhaloes in borderlinef(R) gravity

“…7 indicates that the power-law relation holds true for the CDM (circles and solid lines) and F6 (triangles and dashed lines) simulations as well, though the slope has a weak dependence on the host halo mass (lower for low-mass host haloes). To check this result, we tested HBT on a simulation using a different N-body code (described in Jing & Suto 2002) and found the same tendency. We also tested our simulations using the ROCKSTAR code (Behroozi, Wechsler & Wu 2013) to identify subhaloes, but did not notice any dependence of this slope on the host halo mass.…”

Evolution of galaxy shapes from prolate to oblate through compaction events

“…Frenk et al 1988;Dubinski & Carlberg 1991;Jing & Suto 2002;Bailin & Steinmetz 2005;Allgood et al 2006) .…”

Characterizing strong lensing galaxy clusters using the Millennium-XXL and moka simulations

“…Haloes typically follow the NFW profile and are assumed to be triaxial -following the model by Jing & Suto (2002) and randomly oriented with respect to the line-of-sight. Each system is also populated by dark matter substructures assuming the subhalo population model by Giocoli et al (2010a).…”