Halo Models of Large Scale Structure

By A. Cooray, R. Sheth. 2002

1,496 citations recorded by the source corpus.

Abstract We review the formalism and applications of the halo-based description of non-linear gravitational clustering. In this approach, all mass is associated with virialized dark matter halos; models of the number and spatial distribution of the halos, and the distribution of dark matter within each halo, are used to provide estimates of how the statistical properties of large scale density and velocity fields evolve as a result of non-linear gravitational clustering. We first describe the model, and demonstrate its accuracy by comparing its predictions with exact results from numerical simulations of non-linear gravitational clustering. We then present several astrophysical applications of the halo model: these include models of the spatial distribution of galaxies, the non-linear velocity, momentum and pressure fields, descriptions of weak gravitational lensing, and estimates of secondary contributions to temperature fluctuations in the cosmic microwave background.

Subfields: Astronomy and Astrophysics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/a159ca226d0813ffecd45896e170e288707e7f4b

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Citations in the corpus

Calibrating Redshift Distributions beyond Spectroscopic Limits with Cross-Correlations (2008, methodology): “This assumption is somewhat unrealistic – in real applications, precision measurements should use a halo model (cf. Cooray & Sheth 2002 and references therein) or other more sophisticated methods – but is sufficiently accurate to predict uncertainties for crosscorrelation methods.”
Constraining the galaxy–halo connection over the last 13.3 Gyr: star formation histories, galaxy mergers and structural properties (2017, background): “The next two are the halo occupation distribution (HOD) model (Jing, Mo & Börner 1998; Seljak 2000; Scoccimarro et al. 2001; Berlind & Weinberg 2002; Cooray & Sheth 2002; Kravtsov et al. 2004; Zehavi et al. 2005; Zheng et al. 2005; Leauthaud et al. 2011; Rodŕıguez-Puebla, Avila-Reese & Drory…”
The VIMOS Public Extragalactic Redshift Survey (VIPERS) - Galaxy clustering and redshift-space distortions at z ≃ 0.8 in the first data release (2013, methodology): “…realistic mock samples of the survey, we model our wp(rp) measurements within the context of the HOD (Seljak 2000; Peacock & Smith 2000; Berlind & Article number, page 10 of 19 S. de la Torre et al.: Galaxy clustering and redshift-space distortions in VIPERS Weinberg 2002; Cooray & Sheth 2002).”
CLASH: JOINT ANALYSIS OF STRONG-LENSING, WEAK-LENSING SHEAR, AND MAGNIFICATION DATA FOR 20 GALAXY CLUSTERS (2015, background): “In the context of the ΛCDM model, the two outermost radial bins lie in the transition between the one-halo and two-halo regimes (Cooray & Sheth 2002), r200m <∼ R <∼ 2R200m, where the large-scale two-halo contribution to Σ(R) is expected to become important (Oguri & Hamana 2011; Beraldo e Silva et…”
Halo Assembly Bias in Hierarchical Structure Formation (2008, methodology): “There are many applications for statistical mass determination, including (for example) cluster mass-observable self-calibration (e.g. Lima & Hu 2004; Wu et al. 2008) or reconstruction of the halo occupation distribution of galaxies or quasars (e.g. Cooray & Sheth 2002).”
The C4 Clustering Algorithm: Clusters of Galaxies in the Sloan Digital Sky Survey (2005, background): “As gravitational clustering is amplified into the non-linear regime, a description of the matter distribution as a point set of extended dark matter halos becomes more appropriate (e.g., Cooray & Sheth 2002).”
Theoretical Models of the Halo Occupation Distribution: Separating Central and Satellite Galaxies (2004, background): “…1997; Benson et al. 2000; Seljak 2000; Scoccimarro et al. 2001; Sheth & Diaferio 2001; White, Hernquist, & Springel 2001; Yoshikawa et al. 2001; Cooray & Sheth 2002; Guzik & Seljak 2002; Scranton 2003; B03; K04), showing good agreement in the qualitative features predicted by the different…”
REJUVENATING THE MATTER POWER SPECTRUM: RESTORING INFORMATION WITH A LOGARITHMIC DENSITY MAPPING (2009, background): “At least in a halo model (e.g., Cooray & Sheth 2002) of large-scale structure, this effect comes from cosmic variance in the halo population: a chance preponderance of large halos in a survey increases the power spectrum disproportionately on translinear scales (Neyrinck et al. 2006).”
Mapping stellar content to dark matter haloes using galaxy clustering and galaxy–galaxy lensing in the SDSS DR7 (2015, background): “…Halo Occupation Distribution (HOD; Jing et al. 1998; Ma & Fry 2000; Peacock & Smith 2000; Seljak 2000; Yang et al. 2003; Scoccimarro et al. 2001; Cooray & Sheth 2002; Berlind & Weinberg 2002; Guzik & Seljak 2002; Zheng et al. 2005; Mandelbaum et al. 2006; van den Bosch et al. 2007) framework,…”
The impact of non‐Gaussian errors on weak lensing surveys (2008, methodology): “Therefore, the aim of this paper is to study the covariances of the lensing power spectrum based on the halo model approach(Cooray & Sheth 2002 for a thorough review), and to estimate the impact of the non-Gaussian errors on the power spectrum measurement as well as on the determination of…”
The EAGLE project: Simulating the evolution and assembly of galaxies and their environments (2014, methodology): “Driven in part by the failure of hydrodynamical simulations to reproduce key observations, semi-analytic and halo-based models have become the tools of choice for detailed comparisons between galaxy surveys and theory (see Baugh 2006 and Cooray & Sheth 2002 for reviews).”
The Luminosities, Sizes, and Velocity Dispersions of Brightest Cluster Galaxies: Implications for Formation History (2006, background): “And recently, halo model (see Cooray & Sheth 2002 for a review) interpretations of galaxy clustering strongly suggest that this is indeed the case (Berlind et al. 2005; Skibba et al. 2006).”
Multipoint propagators in cosmological gravitational instability (2008, background): “[16, 23], originate either from the near universal transform advocated in [8] or are based on an even more empirical construction, the halo model [2].”
The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions at z ∼ 1.4 (2015, background): “Galaxies are populated into the halos according to the halo occupation distribution (HOD) model (Cooray & Sheth 2002; Zheng et al. 2005) constrained by the real-space clustering of the FastSound galaxies (Hikage et al. in preparation).”
A halo model of galaxy colours and clustering in the Sloan Digital Sky Survey (2008, background): “The halo model is a useful language for discussing how galaxy clustering depends on galaxy type: galaxy bias (see Cooray & Sheth 2002 for a review).”