MODERN COSMOLOGY

Quantifying large-scale structure 67 eigenmodes in the new coordinates: C′′·ψ′′i=λψ′′i. These eigenmodes must be expressible in ...

68 An introduction to the physics of cosmology Without data, we do not know this, so it is common to use the expectation value o ...

Quantifying large-scale structure 69 be the usualHankel transformpair: w(θ)= ∫∞ 0 ^2 θJ 0 (Kθ)dK/K, ^2 θ=K^2 ∫∞ 0 w(θ)J 0 (Kθ) ...

70 An introduction to the physics of cosmology correlation function in the usual way in terms of an angular power spectrum^2 θ ...

Quantifying large-scale structure 71 direction on the sky as a radial integral over the spatial overdensity, with a weighting of ...

72 An introduction to the physics of cosmology The full version of Limber’s equation therefore gains two powers ofC(y),but one o ...

Quantifying large-scale structure 73 redshift. Thus, withξ∝r−γ, we obtain the comoving evolution ξ(r,z)∝( 1 +z)γ−^3 (nonlinear). ...

74 An introduction to the physics of cosmology evolution from CDM initial conditions. (e.g. Efstathiouet al1990, Klypinet al1996 ...

Quantifying large-scale structure 75 Figure 2.10.The nonlinear evolution of various CDM power spectra, as determined by the Virg ...

76 An introduction to the physics of cosmology In principle, this statistic can be used to recover the real-space correlation fu ...

Quantifying large-scale structure 77 has been investigated in detail by a number of authors (e.g. Gazta ̃naga and Baugh 1998, Ei ...

78 An introduction to the physics of cosmology Figure 2.11.The PD94 compilation of power-spectrum measurements. The upper panel ...

Quantifying large-scale structure 79 Figure 2.12.A four-degree thick slice of the southern strip of the 2dF Galaxy Redshift Surv ...

80 An introduction to the physics of cosmology Figure 2.13. The redshift–space correlation function for the 2dFGRS,ξ(σ,π), plott ...

Quantifying large-scale structure 81 Figure 2.14. The flattening of the redshift–space correlation function is quantified by the ...

82 An introduction to the physics of cosmology a non-local process to some extent, and the modern paradigm was introduced by Whi ...

Quantifying large-scale structure 83 Figure 2.15.The correlation function of galaxies in the semi-analytical simulation of an LC ...

84 An introduction to the physics of cosmology Figure 2.16.The power spectrum for theCDM model. The full lines contrast the lin ...

Quantifying large-scale structure 85 Figure 2.17.The empirical luminosity–mass relation required to reconcile the observed AGS l ...

86 An introduction to the physics of cosmology Figure 2.18. The power spectrum for a galaxy catalogue constructed from theCDM m ...