The Halo Occupation Distribution: Toward an Empirical Determination of the Relation between Galaxies and Mass

2001/09/30 by Andreas A. Berlind, David H. Weinberg · 37 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Correlation function (quantum field theory) #Dark matter #Dark matter halo #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy rotation curve #Halo #Redshift #Statistical Mechanics and Entropy #Velocity dispersion #astro-ph

paper · pdf · doi:10.1086/341469

published as Astrophys.J. 575 (2002) 587-616 · 60 pages + 21 eps figures. Replaced with accepted ApJ version. Minor changes + added references

arxiv created 2002/04/22 · openalex publication_date 2002/08/20 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06

Abstract

We investigate galaxy bias in the framework of the "halo occupation distribution" (HOD), which defines the bias of a population of galaxies by the conditional probability P ( N | M ) that a dark matter halo of virial mass M contains N galaxies, together with prescriptions that specify the relative spatial and velocity distributions of galaxies and dark matter within halos. By populating the halos of a cosmological N -body simulation using a variety of HOD models, we examine the sensitivity of different galaxy clustering statistics to properties of the HOD. The galaxy correlation function responds to different aspects of P ( N | M ) on different scales. Obtaining the observed power-law form of ξ g ( r ) requires rather specific combinations of HOD parameters, implying a strong constraint on the physics of galaxy formation; the success of numerical and semianalytic models in reproducing this form is entirely nontrivial. Other clustering statistics such as the galaxy-mass correlation function, the bispectrum, the void probability function, the pairwise velocity dispersion, and the group multiplicity function are sensitive to different combinations of HOD parameters and thus provide complementary information about galaxy bias. We outline a strategy for determining the HOD empirically from redshift survey data. This method starts from an assumed cosmological model, but we argue that cosmological and HOD parameters will have nondegenerate effects on galaxy clustering, so that a substantially incorrect cosmological model will not reproduce the observations for any choice of HOD. Empirical determinations of the HOD as a function of galaxy type from the Two-Degree Field (2dF) and Sloan Digital Sky Survey (SDSS) redshift surveys will provide a detailed target for theories of galaxy formation, insight into the origin of galaxy properties, and sharper tests of cosmological models.

Citations

• Linear Redshift Distortions: A Review
• Do Distinct Cosmological Models Predict Degenerate Halo Populations?
• Spatial Correlation Functions and the Pairwise Peculiar Velocity Dispersion of Galaxies in the Point Source Catalog Redshift Survey: Implications for the Galaxy Biasing in Cold Dark Matter Models
• Eulerian bias and the galaxy density field
• A comparison of different cluster mass estimates: consistency or discrepancy?
• Bias and Hierarchical Clustering
• Spatial Correlation Function and Pairwise Velocity Dispersion of Galaxies: Cold Dark Matter Models versus the Las Campanas Survey
• Galaxy‐Galaxy Lensing in the Hubble Deep Field: The Halo Tully‐Fisher Relation at Intermediate Redshift
• Evolution of Bias in Different Cosmological Models
• A measurement of the cosmological mass density from clustering in the 2dF Galaxy Redshift Survey
• A survey of galaxy redshifts. V - The two-point position and velocity correlations
• The nature of galaxy bias and clustering

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• The Pairwise Velocity Dispersion of Galaxies: Luminosity Dependence and a New Test of Galaxy Formation Models
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• Clustering of quasars in the first year of the SDSS-IV eBOSS survey: interpretation and halo occupation distribution
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