The statistics of lambda CDM Halo Concentrations

By A. F. Neto, Liang Gao, P. Bett, Shaun Cole, J. Navarro, Carlos S. Frenk, Simon D. M. White, Volker Springel, A. V. I. D. F'isica, Universidade Federal do Rio Grande do Sul and 12 more. 2007

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We use the Millennium Simulation (MS) to study the statistics of Λ cold dark matter (ΛCDM) halo concentrations at z= 0. Our results confirm that the average halo concentration declines monotonically with mass; the concentration–mass relation is well fitted by a power law over three decades in mass, up to the most massive objects that form in a ΛCDM universe (∼ 1015 h−1 M⊙). This is in clear disagreement with the predictions of the model proposed by Bullock et al. for these rare objects, and agrees better with the original predictions of Navarro, Frenk & White. The large volume surveyed, together with the unprecedented numerical resolution of the MS, allows us to estimate with confidence the distribution of concentrations and, consequently, the abundance of systems with unusual properties. About one in a hundred cluster haloes (M200≳ 3 × 1014 h−1 M⊙) have concentrations exceeding c200= 7.5, a result that may be useful in interpreting the likelihood of unusually strong massive gravitational lenses, such as Abell 1689, in the ΛCDM cosmogony. A similar fraction of about 1 per cent of galaxy-sized haloes (M200∼ 1012 h−1 M⊙) have c200 < 4.5 and this could be relevant to models that attempt to reconcile the ΛCDM cosmology with rotation curves of low surface brightness galaxies by appealing to haloes of unexpectedly low concentration. We find that halo concentrations are independent of spin once haloes manifestly out of equilibrium have been removed from the sample. Compared to their relaxed brethren, the concentrations of out-of-equilibrium haloes tend to be lower and have more scatter, while their spins tend to be higher. A number of previously noted trends within the halo population are induced primarily by these properties of unrelaxed systems. Finally, we compare the result of predicting halo concentrations using the mass assembly history of the main progenitor with predictions based on simple arguments regarding the assembly time of all progenitors. The latter are typically as good or better than the former, suggesting that halo concentration depends not only on the evolutionary path of a halo's main progenitor, but on how and when all of its constituents collapsed to form non-linear objects.

Subfields: Astronomy and Astrophysics

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Citations in the corpus

Mass models of the Milky Way (2011, background): “(6) Cosmological simulations predict that typical halo concentration varies with halo mass, but typically only weakly (e.g. cv ∝ M −0.1 v , Neto et al. 2007) when compared to the intrinsic scatter in c at a given virial mass, so we accept the relationship given by Boylan-Kolchin et al. (2010) as…”
Dark matter halo concentrations in the Wilkinson Microwave Anisotropy Probe year 5 cosmology (2008, background): “The resulting c(M) relation is well described by a power law, c ∝ M−0.1 (Neto et al. 2007, hereafter N07).”
Galactic stellar haloes in the CDM model (2009, methodology): “We select 0.07r1/2 in accordance with the criterion of 0.14rvir used to select relaxed objects in the study of Neto et al. (2007), taking rvir ∼ 2r1/2.”
Impact of baryon physics on dark matter structures: a detailed simulation study of halo density profiles (2010, methodology): “Following Neto et al. (2007), only haloes with more than 104 DM particles within Rvir are initially selected.”
CLASH: JOINT ANALYSIS OF STRONG-LENSING, WEAK-LENSING SHEAR, AND MAGNIFICATION DATA FOR 20 GALAXY CLUSTERS (2015, background): “This is significantly smaller than the typical intrinsic scatter predicted for the full (relaxed) population of halos, σ(log10 c200c) ∼ 0.14– 0.16 (0.1–0.12) (Neto et al. 2007; Duffy et al. 2008; Bhattacharya et al. 2013).”
The effects of galaxy formation on the matter power spectrum: a challenge for precision cosmology (2011, methodology): “These models improve on the HALOFIT model by including a variable concentration-mass relation (such as those derived by Neto et al. 2007; Duffy et al. 2008) and have been shown to reproduce the power spectra from simulations with higher accuracy (e.g. Hilbert et al. 2009).”
Weighing the giants – IV. Cosmology and neutrino mass (2014, methodology): “…by WtG10 (specifically, using the color-cut method) to the shear profile predicted from an NFW profile with mass given by mlens and concentration parameter c = 4 (consistent with the mean concentration measured in WtG and the mean population concentration in N -body simulations; Neto et al. 2007).”
A UNIVERSAL MODEL FOR HALO CONCENTRATIONS (2014, methodology): “M relation that is biased high because low concentrations are typical of halos in the rapid mass accretion stage which are more likely to be removed by a relaxation cut (e.g., Neto et al. 2007; Macciò et al. 2008; Bhattacharya et al. 2013; see also the discussion in Section 5.2).”
DARK MATTER HALOS IN THE STANDARD COSMOLOGICAL MODEL: RESULTS FROM THE BOLSHOI SIMULATION (2010, methodology): “Thus the MS-I c200 is 8% larger than the concentrations in Bolshoi for Mvir = 10 12h−1M⊙, with a small (∼10”
Weighing the Giants – III. Methods and measurements of accurate galaxy cluster weak-lensing masses (2012, methodology): “Such large shifts in the massconcentration relation are extreme: Bhattacharya et al. (2013) find that the normalization of the mass-concentration relations from the literature (Neto et al. 2007, for example) and their own workvary by ∼ 10− 20%.”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, background): “…Navarro, Frenk, & White 1997; Bullock et al. 2001; Eke, Navarro & Steinmetz 2001; Zhao et al. 2003; Navarro et al. 2004; Diemand et al. 2005, 2007; Macciò et al. 2007; Neto et al. 2007; Macciò et al. 2008; Zhao et al. 2009; Navarro et al. 2010; Klypin et al. 2010; Muñoz-Cuartas et al. 2011).”
CLASH: WEAK-LENSING SHEAR-AND-MAGNIFICATION ANALYSIS OF 20 GALAXY CLUSTERS (2014, background): “The degree of mass concentration, c200c = r200c/rs, 22, is predicted to correlate with halo mass, since DM halos that are more massive collapse later on average, when the mean background density of the universe is correspondingly lower (Bullock et al. 2001; Neto et al. 2007).”
Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters (2007, methodology): “By default, we adopt the mean mass-concentration (M200 − c200) relation derived from the Millennium Simulation (Springel et al. 2005) by Neto et al. (2007).”
The redshift dependence of the structure of massive Λ cold dark matter haloes (2007, methodology): “They can also lead to spurious correlations (see for example figure 9 of Neto et al. 2007).”
A constant dark matter halo surface density in galaxies (2009, unknown): “…in Cold Dark Matter (CDM) simulations of structure formation (Navarro, Frenk & White 1996, NFW hereafter; Moore et al., 1999; Navarro et al., 2004; Neto et al. 2007) but is not seen in observed data (e.g. de Blok, McGaugh & Rubin, 2001; de Blok & Bosma, 2002; Marchesini et al., 2002; Gentile et…”
New Multiply-Lensed Galaxies Identified in ACS/NIC3 Observations of Cl0024+1654, Using an Improved Mass Model (2009, result): “This value is significantly larger than theoretically expected (cvir ' 5) for the standard ΛCDM model (Bullock et al. 2001, Neto et al. 2007, Duffy et al. 2008), even after accounting for expected projection bias (Oguri et al. 2005, Hennawi et al. 2007, Corless, King & Clowe 2008).”
Ray-tracing through the Millennium Simulation: Born corrections and lens-lens coupling in cosmic shear and galaxy-galaxy lensing (2008, methodology): “A prediction based on the popular halo model (Seljak 2000; Cooray & Sheth 2002) and the halo concentration-mass relation of Neto et al. (2007) provides a better fit to the convergence power spectrum.”
Galaxy clustering and galaxy-galaxy lensing: a promising union to constrain cosmological parameters (2008, background): “…are known to depend on both halo mass and cosmology, and various analytical models have been developed to describe these dependencies (Navarro et al. 1997; Bullock et al. 2001; Eke, Navarro & Steinmetz 2001; Macciò et al. 2007; Neto et al. 2007; Macciò, Dutton & van den Bosch 2008).”