The growth and structure of dark matter haloes

By Dong Zhao, H. Mo, Yipeng Jing, G. Boerner. 2002

287 citations recorded by the source corpus.

In this paper, we analyse in detail the mass-accretion histories and structural properties of dark haloes in high-resolution N-body simulations. We model the density distribution in individual haloes using the Navarro-Frenk-White (NFW) profile. For a given halo, there is a tight correlation between its inner-scale radius r(s) and the mass within it, M-s, for all its main progenitors. Using this correlation, one can predict quite well the structural properties of a dark halo at any time in its history from its mass-accretion history, implying that the structure properties and the mass-accretion history are closely correlated. The predicted growing rate of concentration c with time tends to increase with decreasing mass-accretion rate. The build-up of dark haloes in cold dark matter (CDM) models generally consists of an early phase of fast accretion (where the halo mass M-h increases with time much faster than the expansion rate of the Universe) and a late phase of slow accretion (where M-h increases with time approximately as the expansion rate). These two phases are separated at a time when c similar to 4 and the typical binding energy of the halo is approximately equal to that of a singular isothermal sphere with the same circular velocity. Haloes in the two accretion phases show systematically different properties, for example, the circular velocity v(h) increases rapidly with time in the fast accretion phase but remains almost constant in the slow accretion phase, the inner properties of a halo, such as r(s) and M-s increase rapidly with time in the fast accretion phase but change only slowly in the slow accretion phase, the inner circular velocity v(s) is approximately equal to v(h) in the fast accretion phase but is larger in the slow accretion phase. The potential well associated with a halo is built up mainly in the fast accretion phase, while a large amount of mass can be accreted in the slow accretion phase without changing the potential well significantly. We discuss our results in connection with the formation of dark haloes and galaxies in hierarchical models.

Subfields: Astronomy and Astrophysics, Global and Planetary Change, Instrumentation

View Paper: https://www.semanticscholar.org/paper/bc20dd2a818614a801be50f82805d5920a9828e4

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Citations in the corpus

The Dependence of Dark Halo Clustering on Formation Epoch and Concentration Parameter (2006, background): “…of halos at a given mass, c(M ), has a broad lognormal distribution, and is correlated with the halo formation epoch zform in such a way that halos of earlier formation have a higher concentration (Jing 2000; Bullock et al. 2001; Jing& Suto 2002;Wechsler et al. 2002; Zhao et al. 2003a, 2003b).”
DEPENDENCE OF THE OUTER DENSITY PROFILES OF HALOS ON THEIR MASS ACCRETION RATE (2014, background): “Their paper, however, focuses on the inner regions (r < R200m) and the connection between the shape of the inner profile and a halo’s mass accretion history (see also Wechsler et al. 2002; Zhao et al. 2003, 2009).”
Dark halo response and the stellar initial mass function in early-type and late-type galaxies (2010, unknown): “…N-body simulations (e.g., Navarro, Frenk, & White 1996a; 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;…”
Merger Histories of Galaxy Halos and Implications for Disk Survival (2007, background): “Accretion Histories and Mass Functions The literature is rich with work on the cumulative mass accretion histories of halos as a function of redshift (e.g Wechsler et al. 2002; Zhao et al. 2003; Tasitsiomi et al. 2004; Li et al. 2007, and references therein).”
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.”
An Accurate Physical Model for Halo Concentrations (2018, methodology): “…that predict both the average concentration and scatter (Navarro et al. 1996, 1997; Bullock et al. 2001; Eke et al. 2001; Wechsler et al. 2002; Zhao et al. 2003a, 2009; Lu et al. 2006; Dalal et al. 2008; Giocoli et al. 2012; Ludlow et al. 2014, 2016; van den Bosch et al. 2014; Correa et al.…”
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.”
HERSCHEL-ATLAS GALAXY COUNTS AND HIGH-REDSHIFT LUMINOSITY FUNCTIONS: THE FORMATION OF MASSIVE EARLY-TYPE GALAXIES (2011, background): “…(hereafter referred to as the ‘toy model’) relying on the following assumptions: • Most of the star formation occurs soon after the fast collapse phase of the halo, as identified by Zhao et al. (2003) and by several subsequent works (e.g., Diemand et al. 2007, Genel et al. 2010, Wang et al. 2011).”
Numerical study of halo concentrations in dark-energy cosmologies (2003, unknown): “Recently, Zhao et al. (2003) found that the dependence of halo concentrations on halo mass becomes shallower with increasing redshift.”
Resolving cosmic structure formation with the Millennium-II simulation (2009, background): “For example, the innermost region of a halo – where the galaxy resides – typically assembles much earlier than the outer regions which contain most of the mass (Zhao et al. 2003b; Gao et al. 2004a).”
The accretion history of dark matter haloes - III. A physical model for the concentration-mass relation (2015, background): “As a result, various authors (Bullock et al. 2001; Wechsler et al. 2002; Zhao et al. 2003; Ludlow et al. 2014) have provided models that relate c to the halo mass history.”
Mass and Redshift Dependence of Dark Halo Structure (2003, methodology): “In a forthcoming paper (D H. Zhao et al. 2003, in preparation), we will show that the ZMJB pre- diction is valid for a wide range of cosmological models, in- cluding the standard CDM model, an open CDM model, and scale-free models.”
THE PSEUDO-EVOLUTION OF HALO MASS (2012, background): “Much work has been invested into quantifying MAHs, but the contributions from physical accretion and pseudo-evolution are generally not distinguished (see, e.g.,Wechsler et al. 2002; van den Bosch 2002; Zhao et al. 2003; Miller et al. 2006; Zhao et al. 2009).”
THE SPLASHBACK RADIUS AS A PHYSICAL HALO BOUNDARY AND THE GROWTH OF HALO MASS (2015, background): “D , is approximately equal to four as long as the halo is in the fast accretion regime (Zhao et al. 2003, 2009).8 In this regime, where the contribution of pseudo-evolution to the mass growth is relatively small, M r4 s< approximately tracks MD. Subsequently, as the mass growth and physical…”
Chemical Abundance Distributions of Galactic Halos and Their Satellite Systems in a ΛCDM Universe (2005, methodology): “Some inferences about the growth of the stellar component of galaxy halos have been made based on scaled-down versions of cluster simulations and by assuming physically motivated properties for the baryonic material (Zhao et al. 2003; Helmi, White & Springel 2003).”
MultiDark simulations: the story of dark matter halo concentrations and density profiles (2014, background): “This results in the growth of both the virial radius and the core, which in turn leads to a constant concentration (Zhao et al. 2003, 2009).”