Invited contribution to be published in Vol. 8 of book "Planets, Stars, and Stellar Systems", Springer, series editor T. D. Oswalt, volume editor W. C. Keel
astro-ph/1202.6633

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LARGE SCALE STRUCTURE OF THE UNIVERSE

Alison L. Coil


University of California, San Diego
La Jolla, CA 92093


Abstract: Galaxies are not uniformly distributed in space. On large scales the Universe displays coherent structure, with galaxies residing in groups and clusters on scales of ~ 1-3 h-1 Mpc, which lie at the intersections of long filaments of galaxies that are > 10 h-1 Mpc in length. Vast regions of relatively empty space, known as voids, contain very few galaxies and span the volume in between these structures. This observed large scale structure depends both on cosmological parameters and on the formation and evolution of galaxies. Using the two-point correlation function, one can trace the dependence of large scale structure on galaxy properties such as luminosity, color, stellar mass, and track its evolution with redshift. Comparison of the observed galaxy clustering signatures with dark matter simulations allows one to model and understand the clustering of galaxies and their formation and evolution within their parent dark matter halos. Clustering measurements can determine the parent dark matter halo mass of a given galaxy population, connect observed galaxy populations at different epochs, and constrain cosmological parameters and galaxy evolution models. This chapter describes the methods used to measure the two-point correlation function in both redshift and real space, presents the current results of how the clustering amplitude depends on various galaxy properties, and discusses quantitative measurements of the structures of voids and filaments. The interpretation of these results with current theoretical models is also presented.

Index terms: clustering, angular clustering, two-point correlation function, higher-order correlation function, void, void probability function, filament, galaxy evolution, redshift space distortions, dark matter halo, halo model, bias, dark matter, halo occupation


Table of Contents

HISTORICAL BACKGROUND

THE TWO-POINT CORRELATION FUNCTION

ANGULAR CLUSTERING

REAL AND REDSHIFT SPACE CLUSTERING

GALAXY BIAS

THE DEPENDENCE OF CLUSTERING ON GALAXY PROPERTIES
Luminosity Dependence
Color and Spectral Type Dependence
Redshift Space Distortions

THE EVOLUTION OF GALAXY CLUSTERING

HALO MODEL INTERPRETATION of xi(r)
Estimating the Mean Halo Mass from the Bias
Halo Occupation Distribution Modeling
Interpreting the Luminosity and Color Dependence of Galaxy Clustering
Interpreting the Evolution of Galaxy Clustering

VOIDS AND FILAMENTS
Higher-order Clustering Measurements
Voids
Void and Void Galaxy Properties
Void Probability Function
Filaments

SUMMARY AND FUTURE

REFERENCES

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