Halo concentrations in the standard LCDM cosmology

By Francisco Prada, Anatoly Klypin, A. Cuesta, J. Betancort-Rijo, Joel R. Primack. 2011

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We study the concentration of dark matter halos and its evolution in N-body simulations of the standard LCDM cosmology. The results presented in this paper are based on 4 large N-body simulations with about 10 billion particles each: the Millennium-I and II, Bolshoi, and MultiDark simulations. The MultiDark (or BigBolshoi) simulation is introduced in this paper. This suite of simulations with high mass resolution over a large volume allows us to compute with unprecedented accuracy the concentration over a large range of scales (about six orders of magnitude in mass), which constitutes the state-of-the-art of our current knowledge on this basic property of dark matter halos in the LCDM cosmology. We find that there is consistency among the different simulation data sets. We confirm a novel feature for halo concentrations at high redshifts: a flattening and upturn with increasing mass. The concentration c(M,z) as a function of mass and the redshift and for different cosmological parameters shows a remarkably complex pattern. However, when expressed in terms of the linear rms fluctuation of the density field sigma(M,z), the halo concentration c(sigma) shows a nearly-universal simple U-shaped behaviour with a minimum at a well defined scale at sigma=0.71. Yet, some small dependences with redshift and cosmology still remain. At the high-mass end (sigma < 1) the median halo kinematic profiles show large signatures of infall and highly radial orbits. This c-sigma(M,z) relation can be accurately parametrized and provides an analytical model for the dependence of concentration on halo mass. When applied to galaxy clusters, our estimates of concentrations are substantially larger -- by a factor up to 1.5 -- than previous results from smaller simulations, and are in much better agreement with results of observations. (abridged)

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9a957c44487621135984a30d5cd76ccf07061823

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Citations in the corpus

The halo mass function through the cosmic ages (2012, background): “Prada et al. (2012) provide a detailed exposition of the evolution of the concentration parameter over redshift.”
Modelling baryon acoustic oscillations with perturbation theory and stochastic halo biasing (2013, background): “…needs to cover is extremely large, ranging from varying the cosmological parameters, over modelling different biased tracers, to account for cosmic variance (for large-volume N -body simulations see e.g. Kim et al. 2009; Prada et al. 2012; Angulo et al. 2012; Alimi et al. 2012; Watson et al. 2013).”
The clustering of the SDSS main galaxy sample – II. Mock galaxy catalogues and a measurement of the growth of structure from redshift space distortions at z = 0.15 (2014, methodology): “…= 4ρs r rs ( 1 + r rs )2 , (3) where rs = Rvir/cvir is the characteristic radius, at which the slope of the density profile is −2, and ρs is the density at this radius. c is the concentration parameter, which we calculate for a halo of mass M using the fitting formulae of Prada et al. (2012).”
GALAXIES IN ΛCDM WITH HALO ABUNDANCE MATCHING: LUMINOSITY–VELOCITY RELATION, BARYONIC MASS–VELOCITY RELATION, VELOCITY FUNCTION, AND CLUSTERING (2010, methodology): “…parameter defined for both models as c ≡ Rvir/rs is given by the relations obtained in Paper I for distinct halos (Klypin et al. 2010; see also Prada et al. 2011): −0.075 Mvir c = 9.60 , (5) 1012 h−1 Mo and 3.16 Vcirc Mvir = h−1 Mo. (6) 2.8 × 10−2 km s−1 The Astrophysical Journal, 742:16…”
WIDE-FIELD PRECISION KINEMATICS OF THE M87 GLOBULAR CLUSTER SYSTEM (2011, background): “In particular, there is a statistical relation expected between ρs and rs (or alternatively, between halo virial mass Mvir and concentration cvir ≡ rvir/rs; e.g., Prada et al. 2011).”
A mass-dependent density profile for dark matter haloes including the influence of galaxy formation (2014, unknown): “The NFW proﬁle is a speciﬁc form of the so-called ( α , β , γ ) double power-law model (Jaffe 1983; Hernquist 1990; Merritt et al. 2006) where r s is the scale radius and ρ s the scale density. r s and ρ s are characteristics of each halo, related to their mass and formation time (e.g. Bullock et al”
The flattening of the concentration–mass relation towards low halo masses and its implications for the annihilation signal boost (2013, methodology): “The c(M) model proposed by Prada et al. (2012), which links the halo concentration with the r.m.s. amplitude of matter linear fluctuations, describes remarkably well all the available N-body simulation data down to ∼10−6h−1M⊙ microhalos.”
Combined strong and weak lensing analysis of 28 clusters from the Sloan Giant Arcs Survey (2011, methodology): “Our mass-concentration relation based on the triaxial model resides in between the Duffy et al. (2008) and Prada et al. (2011) relations, and more resemble the relation presented by Gao et al. (2008) which was essentially the modification of the model proposed by Navarro et al. (1997).”
The mass–concentration–redshift relation of cold dark matter haloes (2013, background): “10, where we compare the predictions of our model with the fitting formulae proposed by Duffy et al. (2008), Macciò et al. (2008) and Prada et al. (2012) for the WMAP5, WMAP3 and WMAP7 cosmologies, respectively.”
Scaling relations for galaxy clusters in the Millennium-XXL simulation (2012, methodology): “It is more than 200 times that of our ‘Millennium Simulation’ (MS, Springel et al. 2005), almost 30 times that of the recently completed MultiDark simulation (Prada et al. 2012) but still only 2% that of the Horizon Run 3.”
NIHAO – IV: core creation and destruction in dark matter density profiles across cosmic time (2015, background): “…Frenk and White (1997, NFW) and then confirmed via higher resolution numerical simulations by a large variety of works (e.g., Klypin et al. 2001, Diemand et al. 2004; Power et al. 2003, Macciò etal 2007, 2008, Neto et al. 2007, Navarro et al. 2010, Prada et al.2012, Dutton & Macciò 2014).”
The unexpected diversity of dwarf galaxy rotation curves (2015, background): “…and large cosmological simulations with excellent resolution have characterized conclusively the mass–concentration relation, its normalization, and scatter (see e.g. Neto et al. 2007; Duffy et al. 2008; Macciò, Dutton & van den Bosch 2008; Zhao et al. 2009; Prada et al. 2012; Ludlow et al. 2014).”
MultiDark simulations: the story of dark matter halo concentrations and density profiles (2014, methodology): “…on mass, redshift, and cosmological parameters – has been the subject of extensive analysis for a long period of time (Navarro et al. 1997; Jing 2000; Bullock et al. 2001; Neto et al. 2007; Gao et al. 2008; Macciò et al. 2008; Klypin et al. 2011; Prada et al. 2012; Dutton & Macciò 2014).”
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: mock galaxy catalogues for the BOSS Final Data Release (2015, background): “In fact, the number of current state-of-the-art large-volume N-body simulations is of order 10 (Kim et al. 2009; Alimi et al. 2012; Angulo et al. 2012; Prada et al. 2012; Fosalba et al. 2015; Ishiyama et al. 2015; Klypin et al. 2014; Skillman et al. 2014; Watson et al. 2014).”
The mass–concentration–redshift relation of cold and warm dark matter haloes (2016, methodology): “This reflects the fact that each group of authors used different equilibrium conditions (or none at all in the case of Diemer & Kravtsov 2015 and Prada et al. 2012) to define their halo samples, which can introduce subtle biases in the recovered c(M, z) relation, particularly at high redshift…”
The accretion history of dark matter haloes - III. A physical model for the concentration-mass relation (2015, background): “M relation at high-z, in agreement with Muñoz-Cuartas et al. (2011) and Prada et al. (2012).”