Mass and Redshift Dependence of Dark Halo Structure

By Dong Zhao, Yipeng Jing, H. Mo, G. Börner. 2003

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Using a combination of N-body simulations with different resolutions, we study in detail how the concentrations of cold dark matter halos depend on halo mass at different redshifts. We confirm that halo concentrations at the present time depend strongly on halo mass, but our results also show marked differences from the predictions of some early empirical models. Our main results are that the mass dependence of the concentrations becomes weaker at higher redshifts and that at z ≳ 3, halos of mass greater than 1011 h-1 M☉ all have a similar median concentration, c ~ 3.5. While the median concentrations of low-mass halos grow significantly with time, those of massive halos change very little with redshift. These results are quantitatively in good agreement with the empirical model proposed by Zhao et al., which shows that halos in the early fast accretion phase all have similar concentrations.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/4d22cdace2d136672baea872ba6385b7ce3241c1

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Citations in the corpus

Lyα COOLING EMISSION FROM GALAXY FORMATION (2010, background): “(A3) This expression is valid at z & 1 (where the cosmological constant can be neglected) and fiducially assumes c = 5, approximately the median concentration of all massive halos at z ∼ 2− 3 (e.g., Zhao et al. 2003).”
Concentration, spin and shape of dark matter haloes as a function of the cosmological model: WMAP1, WMAP3 and WMAP5 results (2008, methodology): “A slightly lower normalization, K = 3.4, was advocated by M07 for a WMAP1 cosmology (see Zhao et al. 2003a and Kuhlen et al. 2005 for more details).”
The dark matter haloes of massive, relaxed galaxy clusters observed with Chandra (2006, background): “Finally, Zhao et al. (2003) argue that at the highest masses, the Bullock et al. (2001) model may over-predict the evolution of cvir with redshift.”
There's no place like home? Statistics of Milky Way-mass dark matter haloes (2009, methodology): “…studied extensively via N -body simulations and extended Press-Schechter (1974) theory (Lacey & Cole 1993, 1994; Wechsler et al. 2002; van den Bosch 2002; Zhao et al. 2003b,a; Tasitsiomi et al. 2004; Cohn & White 2005; Neistein et al. 2006; Li et al. 2008; Zhao et al. 2009; McBride et al. 2009).”
The morgana model for the rise of galaxies and active nuclei (2006, result): “…an adequate description of the hierarchical formation of DM haloes, in excellent agreement with the results of N-body simulations (see also Zhao et al. 2003; Li, Mo & van den Bosch 2005); for instance, the mass function of DM haloes is recovered to within a 5–10 per cent accuracy (Monaco…”
The mass profile and accretion history of cold dark matter haloes (2013, background): “Better results have been obtained with empirical models that relate concentration to halo mass accretion history and, in particular, to the time when the main halo progenitor switches from a period of “fast growth” to one of “slow growth” (Wechsler et al. 2002; Zhao et al. 2003; Lu et al. 2006).”
The redshift dependence of the structure of massive Λ cold dark matter haloes (2007, methodology): “…B01 model and our measurements can be reduced by changing the parameters to K = 2.8 and F = 0.001 (see Wechsler et al 2006), neither for this model nor for the ENS model can parameter changes produce agreement with the weak redshift evolution seen at high mass both here and by Zhao et al. (2003b).”
WHY BARYONS MATTER: THE KINEMATICS OF DWARF SPHEROIDAL SATELLITES (2012, background): “…of galaxy formation in the CDM cosmological model, as galaxies that form at higher redshifts are more concentrated (Wechsler et al. 2002; Zhao et al. 2003), and early forming subhalos are found preferentially closer to the center of MW-mass galaxies (Diemand et al. 2005; Moore et al.…”
Halo Assembly Bias in Hierarchical Structure Formation (2008, background): “Previous work has shown that assembly history and concentration are correlated (Wechsler et al. 2002; Zhao et al. 2003a,b), so the relation between peak curvature and accretion rate discussed above suggests that concentration and peak curvature may be correlated.”
The masses and density profiles of halos in a LCDM galaxy formation simulation (2014, background): “…between halo mass and concentration has been studied by many authors (e.g. AvilaReese et al. 1999; Jing 2000; Bullock et al. 2001; Eke, Navarro & Steinmetz 2001; Zhao et al. 2003; Neto et al. 2007; Duffy et al. 2008; Gao et al. 2008; Navarro et al. 2010; Dutton & Macciò 2014; Ludlow et al. 2014).”
The mass–concentration–redshift relation of cold and warm dark matter haloes (2016, background): “Most notably, the concentrations of very massive haloes are found to be approximately constant and to evolve little with redshift (Zhao et al. 2003, 2009; Gao et al. 2008).”
The Observed Growth of Massive Galaxy Clusters II: X-ray Scaling Relations (2009, background): “Assuming the total mass follows a Navarro, Frenk & White (1997) profile with a typical concentration parameter c = 4 (Zhao et al. 2003, 2009; Gao et al. 2008), the ratio r500/r2500 is approximately 2.3, yielding a scaled, mean gas mass fraction estimate of fgas(r500) ≈ 0.115 from the A08 value of…”
The statistics of lambda CDM Halo Concentrations (2007, methodology): “The first thing to note is that there is no unique way of defining when a particular halo formed, and so different definitions have been adopted (Lacey & Cole 1993; Navarro, Frenk, & White 1997; Wechsler et al. 2002; Zhao et al. 2003a).”
DARK MATTER HALO PROFILES OF MASSIVE CLUSTERS: THEORY VERSUS OBSERVATIONS (2011, background): “Regarding the modeling of the scatter in the concentration,it is natural to examine this in the context of different assembly histories for halos with the same mass (Wechsler et al. 2002; Zhao et al. 2003) (See also, Cohn & White 2005.)”
The evolution of massive black holes and their spins in their galactic hosts (2012, methodology): “(5) The concentration parameter has been studied by several authors (Bullock et al. 2001; Wechsler et al. 2002; Zhao et al. 2003a,b; Macciò et al. 2007), and found to present a large scatter for a fixed halo mass, but to scale generally with the halo’s main-progenitor history.”
Concentration, spin and shape of dark matter haloes: Scatter and the dependence on mass and environment (2006, result): “This is 15 per cent lower than the K = 4.0 originally advocated by B01, but consistent with Zhao et al. (2003) and Kuhlen et al. (2005), who found K = 3.5 (both for F = 0.01).”
A BARYONIC SOLUTION TO THE MISSING SATELLITES PROBLEM (2012, background): “Further, concentrations at these halo masses are expected to decrease with increasing z (Bullock et al. 2001; Eke et al. 2001; Zhao et al. 2003; Macciò et al. 2008; Prada et al. 2012).”
ACCURATE UNIVERSAL MODELS FOR THE MASS ACCRETION HISTORIES AND CONCENTRATIONS OF DARK MATTER HALOS (2008, methodology): “Comparison with the Zhao et al. (2003a) Model As mentioned above, the Z03a model for the halo concentrations is based on the tight correlation between Rs and Ms.”
Mass accretion rates and histories of dark matter haloes (2009, background): “The relationship between halo structure and accretion was further addressed in Zhao et al. (2003) and Zhao et al. (2003), where the redshift dependence of c was observed to be more complicated than a simple proportionality.”