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Article Contents

ABSTRACT

1.PREAMBLE

1.1.The perturbed universe

1.2.Relativistic viewpoint and gauge issues

2.NEWTONIAN EQUATIONS OF MOTION

2.1.Matter-dominated universe

2.2.Radiation-dominated universe

2.3.Mészáros effect

2.4.Coupled perturbations

2.5.Transfer functions and characteristic scales

3.NONLINEAR EVOLUTION OF COSMIC STRUCTURE

3.1.The Zeldovich approximation

3.2.The spherical model

3.3.N-body models

4.STATISTICS OF COSMOLOGICAL DENSITY FIELDS

4.1.Fourier analysis of density fluctuations

4.2.CDM models for structure formation

5.COMPARISON WITH 2dFGRS DATA

5.1.Survey overview

5.2.The 2dFGRS power spectrum and CDM models

5.3.Robustness of results

6.RELATION OF GALAXIES AND DARK MATTER

6.1.History and general aspects of bias

6.2.The peak-background split

6.3.Observations of biased clustering

6.4.Scale dependence of bias

6.5.The halo model - I: mass

6.6.The Halo model - II: biased galaxy populations

7.ANISOTROPIES IN THE CMB

7.1.Anisotropy mechanisms

7.2.Inflationary predictions

7.3.Characteristic scales

7.4.Evolution of CMB data

8.MODEL DEGENERACIES INHERENT IN CMB DATA

8.1.Geometrical degeneracy

8.2.Horizon-angle degeneracy

8.3.Tensor degeneracy

9.COMBINATION OF THE CMB AND LARGE-SCALE STRUCTURE

9.1.Matter fluctuation amplitude and bias

10.LESS-STANDARD INGREDIENTS

10.1.Limits to the neutrino mass

10.2.The equation of state of the vacuum

10.3.The total relativistic density

11.CONCLUSIONS

REFERENCES