Triaxial Modeling of Halo Density Profiles with High-Resolution N-Body Simulations

By Yipeng Jing, Y. Suto. 2002

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We present a detailed nonspherical modeling of dark matter halos on the basis of a combined analysis of high-resolution halo simulations (12 halos with N ~ 106 particles within their virial radius) and large cosmological simulations (five realizations with N = 5123 particles in a 100 h-1 Mpc box size). 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, that 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 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 nonlinear clustering of dark matter. In addition, this provides a useful framework for the nonspherical modeling of the intracluster gas, which is crucial in discussing the gas and temperature profiles of X-ray clusters and the Hubble constant estimated via the Sunyaev-Zeldovich effect.

Subfields: Astronomy and Astrophysics, Instrumentation, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/507f57b9cc4a1bd3404a86e69e5367d9fa6af87e

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Citations in the corpus

Combined strong and weak lensing analysis of 28 clusters from the Sloan Giant Arcs Survey (2011, methodology): “To derive more accurate theoretical predictions based on the ΛCDM model, in Appendix A we conduct a series of semianalytic calculations with ray-tracing of extended sources to estimate the effect of the lensing bias, based on a triaxial halo model of Jing & Suto (2002).”
A Two Micron All-Sky Survey View of the Sagittarius Dwarf Galaxy. IV. Modeling the Sagittarius Tidal Tails (2004, methodology): “In this case, the flattening is introduced in the density q rather than in potential contours, and the approximate form of the potential is adopted from Jing & Suto (2002).”
Galaxy formation theory (2010, background): “Dark matter halos have triaxial shapes and the distribution of axial ratios has been well characterized from N-body simulations (Frenk et al. 1988; Jing and Suto 2002; Bett et al. 2007).”
Structure finding in cosmological simulations: the state of affairs (2013, background): “Both Jing & Suto (2002) and Bailin & Steinmetz (2005) have noted that iterative methods have difficulty in achieving convergence in simulations in which haloes are very well resolved and contain a population of satellites.”
The Phoenix Project: the dark side of rich galaxy clusters (2012, background): “…by N-body simulations of ever increasing numerical resolution and dynamic range (e.g. Frenk et al. 1985; Navarro et al. 1997; Moore et al. 1999; Jing & Suto 2002; Navarro et al. 2004; Gao et al. 2004b; Diemand et al. 2004a, 2007; Gao et al. 2008; Springel et al. 2008a; Stadel et al. 2009;…”
The growth and structure of dark matter haloes (2002, positive): “For example, Jing & Suto (2002) found that for the standard CDM model with Ωm = 1, c grows much faster for a fixed mass, c ∝ a 3/2, and indeed a scaling, c ∝ H−1(z) [where H(z) is the Hubble constant at redshift z] may work better.”
Semianalytical Model of Galaxy Formation with High-Resolution N-Body Simulations (2004, methodology): “This simulation was used to derive the triaxial model for dark matter halos in Jing & Suto (2002), to which we refer the reader for some complementary information about the simulation.”
The Dependence of Dark Halo Clustering on Formation Epoch and Concentration Parameter (2006, methodology): “We use an upgraded version of the particle-particle-particlemesh (P3M) code of Jing & Suto (1998, 2002) to simulate structure formation in the universe.”
The local dark matter density (2014, background): “The shape of dark matter halos DMO simulations also make predictions for the shape of dark matter halos, which are found to be triaxial (Dubinski & Carlberg, 1991; Warren et al., 1992; Navarro et al., 1996b; Jing & Suto, 2002, and see Figure 3a).”
ACCURATE UNIVERSAL MODELS FOR THE MASS ACCRETION HISTORIES AND CONCENTRATIONS OF DARK MATTER HALOS (2008, methodology): “In order to examine the dependence on cosmological parameters, we also use simulations for the ‘Standard’ CDM model (Ωm,0 = 1) and the open CDM model (Ωm,0 = 0.3, ΩΛ,0 = 0), as described in Jing & Suto (2002, 1998).”
ON THE ACCURACY OF WEAK-LENSING CLUSTER MASS RECONSTRUCTIONS (2010, background): “First, the triaxial shapes of Cold Dark Matter (CDM) halos (e.g., Warren et al. 1992; Jing & Suto 2002; Bailin & Steinmetz 2005; Kasun & Evrard 2005; Allgood et al. 2006; Shaw et al. 2006; Bett et al. 2007; Macciò et al. 2007, 2008) can bias a spherically-symmetric model fit of the reduced…”
The three‐point correlation function in cosmology (2002, positive): “Recently, based on high-resolution simulations, Jing & Suto (2002) showed that haloes are more accurately described by triaxial halo profiles than the spherically symmetric NFW profile.”
The Causes of Halo Shape Changes Induced by Cooling Baryons: Disks versus Substructures (2007, background): “…generally triaxial with mean axial ratios b/a ∼ 0.6 and c/a ∼ 0.4, where c < b < a are the short, intermediate, and long axes, respectively (Bardeen et al. 1986; Barnes & Efstathiou 1987; Frenk et al. 1988; Dubinski & Carlberg 1991; Jing & Suto 2002; Bailin & Steinmetz 2005; Allgood et al. 2006).”
On the Mass-to-Light Ratio of Large-Scale Structure (2004, methodology): “They are triaxial objects that can exhibit significant flattening (see, e.g. Jing & Suto 2002).”
A halo-based galaxy group finder: calibration and application to the 2dFGRS (2004, methodology): “The mock samples are constructed using a set of N-body simulations carried out by Y.P. Jing and Y. Suto (see Jing 2002; Jing & Suto 2002) on the VPP5000 Fujitsu supercomputer of the National Astronomical Observatory of Japan using a vectorized-parallel P3M code.”
Galaxy-induced transformation of dark matter haloes (2009, background): “CDM halos are distinctly triaxial systems supported by anisotropic velocity dispersion tensors (Frenk et al., 1988; Jing & Suto, 2002; Allgood et al., 2006; Hayashi et al., 2007; Bett et al., 2007), a result that reflects the highly aspherical nature of gravitationally-amplified density…”
Concentration, spin and shape of dark matter haloes as a function of the cosmological model: WMAP1, WMAP3 and WMAP5 results (2008, background): “Determining the shape of a three-dimensional distribution of particles is a non-trivial task (e.g., Jing & Suto 2002).”
The MICE Grand Challenge lightcone simulation – II. Halo and galaxy catalogues (2013, background): “Central galaxies are placed at the halo centre of mass. Satellite galaxies are positioned into the haloes following a triaxial NFW profile with fixed axis ratios (e.g. Jing & Suto 2002).”