Assembly bias in the clustering of dark matter haloes

By Liang Gao, Simon D. M. White. 2006

290 citations recorded by the source corpus.

We use a very large simulation of structure growth in a Λ cold dark matter (ΛCDM) universe – the Millennium Simulation – to study assembly bias, the fact that the large-scale clustering of haloes of given mass varies significantly with their assembly history. We extend earlier work based on the same simulation by superposing results for redshifts from 0 to 3, by defining a less noisy estimator of clustering amplitude, and by considering halo concentration, substructure mass fraction and spin, as well as formation time, as additional parameters. These improvements lead to results with less noise than previous studies and covering a wider range of halo masses and structural properties. We find significant and significantly different assembly bias effects for all the halo properties we consider, although in all cases the dependencies on halo mass and on redshift are adequately described as a dependence on equivalent peak height ν(M, z). The ν-dependencies for different halo properties differ qualitatively and are not related as might naively be expected given the relations between formation time, concentration, substructure fraction and spin found for the halo population as a whole. These results suggest that it will be difficult to build models for the galaxy populations of dark haloes which can robustly relate the amplitude of large-scale galaxy clustering to that for mass clustering at better than the 10 per cent level.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/d72733d8f12b73f70c4671d74e27ab8033e6fa33

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Citations in the corpus

The evolution of dark matter halo properties in clusters, filaments, sheets and voids (2007, background): “Gao & White (2007) find that haloes with, e.g., high spin-parameter or formation time, tend to be more strongly clustered than younger and low-spin haloes.”
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).”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “This effect, broadly termed “halo assembly bias” (Gao & White 2007), has likely left its imprint on galaxy formation histories as well, resulting in a “galaxy assembly bias”.”
Resolving cosmic structure formation with the Millennium-II simulation (2009, background): “…substructure content, and spin (e.g., Harker et al. 2006; Wechsler et al. 2006; Wetzel et al. 2007; Jing et al. 2007; Bett et al. 2007; Gao & White 2007; Dalal et al. 2008; Angulo et al. 2008) With the MS-II, we are able to investigate assembly bias at much lower masses than was…”
THE SPIN AND ORIENTATION OF DARK MATTER HALOS WITHIN COSMIC FILAMENTS (2009, background): “In addition to the age, other halo properties such as concentration and spin have also been found to correlate with the local environment (Avila-Reese et al. 2005; Wechsler et al. 2005; Bett et al. 2007; Gao & White 2007; Macciò et al. 2007).”
Concentration, spin and shape of dark matter haloes: Scatter and the dependence on mass and environment (2006, background): “…such as halo concentration, halo spin parameter, subhalo properties and the time since the last major merger (Wechsler et al. 2006; Zhu et al. 2006; Gao & White 2007; Wetzel et al. 2007; but see also Percival et al. 2003), which is not too surprising given that all these properties correlate with…”
Observational probes of cosmic acceleration (2012, background): “While the simplest formulation of HOD is surely not the whole story of clustering bias (e.g., Gao et al., 2005; Harker et al., 2006; Gao and White, 2007), the model has passed significant tests.”
Lensing is Low: Cosmology, Galaxy Formation, or New Physics? (2016, background): “…by 35 per cent while keeping the bias fixed. addition to halo mass, the strength of halo clustering depends on other properties such as halo age, spin and concentration (Gao, Springel & White 2005; Wechsler et al. 2006; Gao & White 2007; Zentner 2007; Dalal et al. 2008; Lacerna & Padilla 2011).”
The realm of the galaxy protoclusters (2016, background): “…of galaxies in a halo may depend not only on the mass of that halo, but also on its formation time, and its effects may be particularly pronounced in massive halos (e.g., Gao & White, 2007; Cooper et al., 2010; Wang et al., 2013; Hearin et al., 2015; Lin et al., 2016; Miyatake et al., 2016).”
How do galaxies populate dark matter haloes (2009, background): “3 shows that the satellite fraction is higher for smaller stellar mass, suggesting there may be more scatter in low-mass galaxies than at high mass. Additional scatter may come from variations in halo assembly history (e.g. Croton et al. 2007; Gao & White 2007).”
Ingredients for 21 cm Intensity Mapping (2018, background): “…there is also a dependence on halo age (Sheth & Tormen 2004; Gao et al. 2005), concentration (Wechsler et al. 2006), subhalo abundance (Wechsler et al. 2006; Gao & White 2007), halo shape (Faltenbacher & White 2010), spin (Gao & White 2007), and environment (Salcedo et al. 2018; Han et al. 2018).”
Cosmological parameter constraints from galaxy-galaxy lensing and galaxy clustering with the SDSS DR7 (2012, unknown): “Moreover, these HOD models ignore issues such as assembly bias (explicit dependence of clustering properties on assembly history, rather than just mass alone; Gao et al. 2005, Gao & White 2007) that can change the relation between small- and large-scale clustering information.”
Galaxy assembly bias: a significant source of systematic error in the galaxy–halo relationship (2013, background): “The character of assembly bias depends on halo mass relative to M∗, the characteristic collapse mass at a given redshift: for halos at fixed mass M M∗, older halos cluster more strongly than young Gao & White (2007); for halos with Mvir M∗, the reverse is true (Wechsler et al. 2006).”
THE CONNECTION BETWEEN GALAXIES AND DARK MATTER STRUCTURES IN THE LOCAL UNIVERSE (2012, background): “An alternative is halo assembly bias (e.g. Wechsler 2001; Gao & White 2007; Wechsler et al. 2006).”
Halo Assembly Bias in Hierarchical Structure Formation (2008, background): “…is considerably stronger than in the high mass regime, and of the opposite sign: the oldest, highly concentrated halos have a bias more than twice as large as that of the youngest, low-concentration halos of similar mass M ≪ M⋆ (Gao, Springel & White 2005; Wechsler et al. 2006; Gao & White 2007).”