The age dependence of halo clustering

By Liang Gao, Volker Springel, Simon D. M. White. 2005

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We use a very large simulation of the concordance Λ cold dark matter cosmogony to study the clustering of dark matter haloes. For haloes less massive than about 1013 h−1 M⊙ the amplitude of the two-point correlation function on large scales depends strongly on halo formation time. Haloes that assembled at high redshift are substantially more clustered than those that assembled more recently. The effect is a smooth function of halo formation time and its amplitude increases with decreasing halo mass. At 1011 h−1 M⊙ the ‘oldest’ 10 per cent of haloes are more than five times more strongly correlated than the ‘youngest’ 10 per cent. This unexpected result is incompatible with the standard excursion set theory for structure growth, and it contradicts a fundamental assumption of the halo occupation distribution models often used to study galaxy clustering, namely that the galaxy content of a halo of given mass is statistically independent of its larger scale environment.

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

View Paper: https://www.semanticscholar.org/paper/9ca136d1ae926bb7a512de4c98145960b94ee575

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Citations in the corpus

THE LARGE-SCALE BIAS OF DARK MATTER HALOS: NUMERICAL CALIBRATION AND MODEL TESTS (2010, methodology): “Gao et al. (2005) and Angulo et al. (2008) use the halo-halo correlation 14 We do not include the 768h−1 Mpc HOT simulation in this section because the results at highν are possibly biased due to numerical issues.”
What Aspects of Galaxy Environment Matter? (2006, result): “However, recent results found correlations to this effect (Gao et al. 2005).”
The spin and shape of dark matter haloes in the Millennium simulation of a Λ cold dark matter universe (2006, methodology): “We compute the bias parameter as a function of mass, b(Mh), using a similar method to that of Gao et al. (2005).”
Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure (2007, background): “Many of the existing definitions are based on the evolution of M200 or Mvir (e.g. Wechsler et al. 2002; Zhao et al. 2003; Gao et al. 2005).”
Properties of dark matter haloes in clusters, filaments, sheets and voids (2006, result): “Our results are in very good agreement with Sheth & Tormen (2004), Gao et al. (2005), Harker et al. (2006) and Reed et al. (2006).”
Scaling relations for galaxy clusters in the Millennium-XXL simulation (2012, background): “Models that follow galaxy formation explicitly predict a dependence of the HOD on other properties such as the halo formation time (e.g. Gao et al. 2005; Zhu et al. 2006; Croton et al. 2007).”
Galaxy Evolution from Halo Occupation Distribution Modeling of DEEP2 and SDSS Galaxy Clustering (2007, background): “Gao et al. (2005) find in simulations a signature of age-dependent halo clustering (the so-called “halo assembly bias”, see also Croton et al. 2007; Jing et al. 2007; Harker et al. 2006; Wechsler et al. 2006; Wetzel et al. 2007; Zhu et al. 2006; Gao & White 2007).”
Properties of galaxy groups in the Sloan Digital Sky Survey – I. The dependence of colour, star formation and morphology on halo mass (2005, background): “Secondly, Gao et al. (2005) have shown that the bias only depends on halo assembly time for haloes less massive than ∼1013 h−1 M .”
A kinematic classification of the cosmic web (2012, background): “The properties of galaxies are observed to depend on their environment (Dressler 1980; Blanton et al. 2005; Avila-Reese et al. 2005; Gao et al. 2005; Maulbetsch et al. 2007; Forero-Romero et al. 2011).”
The evolution of dark matter halo properties in clusters, filaments, sheets and voids (2007, background): “Rather, they also depend on the environment in which the halo resides (e.g. Gao et al. 2005; Wechsler et al. 2006; Harker et al. 2006; Wang et al. 2007; Hahn et al. 2007, Paper I in the following).”
Assembly bias in the clustering of dark matter haloes (2006, methodology): “As in Gao et al. (2005), we examine assembly bias by comparing the spatial clustering of a subset of haloes of given mass to that of the set as a whole.”
Resolving cosmic structure formation with the Millennium-II simulation (2009, methodology): “Gao et al. (2005) used the MS to show that clustering depends strongly on formation time at masses M .”
The detectability of baryonic acoustic oscillations in future galaxy surveys. (2007, methodology): “However, recent analyses of high resolution, large volume simulations have revealed some dependence of halo clustering on a second parameter besides mass, such as the halo’s formation redshift or concentration parameter (Gao et al. 2005; Harker et al. 2006; Wechsler et al. 2006).”
Modelling galaxy clustering in a high-resolution simulation of structure formation (2006, background): “Recently (Gao et al. 2005) have shown that there exists an age dependence of halo clustering: haloes that are formed earlier are more clustered than haloes that are assembled more recently, indicating that this assumption may not be as safe as previously thought.”
THE SPIN AND ORIENTATION OF DARK MATTER HALOS WITHIN COSMIC FILAMENTS (2009, background): “In a recent study, using high-resolution N-body simulations, Gao et al. (2005) found that the halo clustering strength not only depends on the masses of the halos but also on their formation times (see also Sheth & Tormen 2004; Wang et al. 2007; Dalal et al. 2008; Hahn et al. 2009).”