Late time solutions for inhomogeneousΛCDMcosmology, their characterization, and observation

Abstract

Assuming homogeneous isotropic ÃCDM cosmology allows Ã, spatial curvature, and dark matter density to be inferred from large scale structure observations such as supernovae. The purpose of this paper is to extend this to allow observations to measure or constrain inhomogeneity and anisotropy. We obtain the general inhomogeneous anisotropic ÃCDM solution which is locally asymptotic to an expanding de Sitter solution as a late time expansion using Starobinsky's method (analogous to the ''holographic renormalization'' technique in AdS/CFT) together with a resummation of the expansion. The dark matter is modeled as perfect dust fluid. The terms in the expansion systematically describe inhomogeneous and anisotropic deformations of an expanding Friedmann-Lemaître-Robertson-Walker solution and are given as a spatial derivative expansion in terms of data characterizing the solution-a 3-metric and a perturbation of that 3-metric. Leading terms describe inhomogeneity and anisotropy on the scale set by the cosmological constant, approximately the horizon scale today. Higher terms in the expansion describe shorter scale variations. We compute the luminosity-distance-redshift relation and argue that comparison with current and future observations would allow a partial reconstruction of the characterizing data. We also comment on smoothing these solutions noting that geometric flows (such as Ricci flow) applied to the characterizing data provide a canonical smoothing method.