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	Abstract
1	Introduction
2	Clustering in the Expanding Universe
	2.1	The cosmological principle
	2.2	From the Einstein equation to the Friedmann equation
	2.3	Expansion law and age of the Universe
	2.4	Einstein’s static model and Lemaître’s model
	2.5	Vacuum energy as an effective cosmological constant
	2.6	Gravitational instability
	2.7	Linear growth rate of the density fluctuation
3	Statistics of Cosmological Density Fluctuations
	3.1	Gaussian random field
	3.2	Log-normal distribution
	3.3	Higher-order correlation functions
	3.4	Genus statistics
	3.5	Minkowski functionals
4	Galaxy Biasing
	4.1	Concepts and definitions of biasing
	4.2	Modeling biasing
	4.3	Density peaks and dark matter halos as toy models for galaxy biasing
	4.4	Biasing of galaxies in cosmological hydrodynamic simulations
	4.5	Halo occupation function approach for galaxy biasing
5	Relativistic Effects Observable in Clustering at High Redshifts
	5.1	Cosmological light-cone effect on the two-point correlation functions
	5.2	Evaluating two-point correlation functions from N-body simulation data
	5.3	Cosmological redshift-space distortion
	5.4	Two-point clustering statistics on a light-cone in cosmological redshift space
6	Recent Results from 2dF and SDSS
	6.1	The latest galaxy redshift surveys
	6.2	Cosmological parameters from 2dFGRS
	6.3	Luminosity and spectral-type dependence of galaxy clustering
	6.4	Topology of the Universe: Analysis of SDSS galaxies in terms of Minkowski functionals
	6.5	Other statistical measures
7	Discussion
8	Acknowledgements
	References
	Figures

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