Halo Assembly Bias in Hierarchical Structure Formation

By N. Dalal, M. White, J. Richard Bond, A. Shirokov. 2008

218 citations recorded by the source corpus.

We investigate the origin of halo assembly bias, the dependence of halo clustering on assembly history. We relate halo assembly to peak properties measured in the Lagrangian space of the initial linear Gaussian random density field and show how these same Lagrangian properties determine large-scale bias. We focus on the two regimes where assembly bias has been observed to be significant: at masses very large and very small compared to the nonlinear mass scale. At high masses, we show that assembly bias is expected from the statistics of the peaks of Gaussian random fluctuations, and we show that the extent of assembly bias found in N-body simulations of rare halos is in excellent agreement with our theoretical prediction. At low masses, we argue that assembly bias largely arises from a subpopulation of low-mass halos whose mass accretion has ceased. Due to their arrested development, these halos naturally become unbiased, in contrast to their antibiased peers. We show that a simple toy model incorporating these effects can roughly reproduce the bias trends found in N-body simulations.

Subfields: Astronomy and Astrophysics, Global and Planetary Change, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/2cd5987e864af7c5076431501b5d70d24458e300

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Global and Planetary Change

In Statistical and Nonlinear Physics

Citations in the corpus

THE LARGE-SCALE BIAS OF DARK MATTER HALOS: NUMERICAL CALIBRATION AND MODEL TESTS (2010, background): “The mass contained within the peak does not completely map onto the mass within the collapsed halo (Dalal et al. 2008).”
A UNIVERSAL MODEL FOR HALO CONCENTRATIONS (2014, background): “As shown in previous studies, the mass dependence of the concentration of halos is a consequence of their MAH (Wechsler et al. 2002; Zhao et al. 2003b, 2009; Ludlow et al. 2013), which, in turn, is determined by the parameters of the background cosmological model.”
Galaxy assembly bias: a significant source of systematic error in the galaxy–halo relationship (2013, background): “Relaxing this assumption, excursion set theory also predicts a correlation between halo formation time and halo environment (e.g., Zentner 2007; Dalal et al. 2008).”
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).”
DEPENDENCE OF THE OUTER DENSITY PROFILES OF HALOS ON THEIR MASS ACCRETION RATE (2014, background): “The Gaussian peaks in realistic cosmological initial conditions have shallow inner slopes and steep outer slopes, corresponding to the fast and slow mass accretion regimes of halos (Dalal et al. 2008).”
Consistent modeling of velocity statistics and redshift-space distortions in one-loop perturbation theory (2020, unknown): “[74]).”
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).”
GALAXY CLUSTERING IN THE COMPLETED SDSS REDSHIFT SURVEY: THE DEPENDENCE ON COLOR AND LUMINOSITY (2010, background): “…since halo concentrations and assembly histories show some environmental correlations (Sheth & Tormen 2004; Gao, Springel & White 2005; Harker et al. 2006; Wechsler et al. 2006; Zhu et al. 2006; Croton, Gao & White 2007; Jing, Suto, & Mo 2007; Wetzel et al. 2007; Dalal et al. 2008; Zu et al. 2008).”
Resolving cosmic structure formation with the Millennium-II simulation (2009, methodology): “…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 previously possible: M…”
THE SPLASHBACK RADIUS AS A PHYSICAL HALO BOUNDARY AND THE GROWTH OF HALO MASS (2015, background): “It is well-known that the large-scale bias of halos depends upon their assembly history (Gao et al. 2005; Wechsler et al. 2006; Dalal et al. 2008; Li et al. 2008).”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “However, since the halo assembly histories in cosmological simulations are affected by the large-scale environment (Wang et al. 2007; Dalal et al. 2008), some halo properties, including age, concentration, spin, richness, and most importantly clustering, exhibit systematic differences between low…”
MASS FUNCTION PREDICTIONS BEYOND ΛCDM (2010, background): “In addition, it also depends on the assembly history of the halos (Dalal et al. 2008).”