2002/08/31 by Wayne Hu · 9 citations
Physics and Astronomy · #Astrophysics #Context (archaeology) #Cosmic microwave background #Cosmology #Cosmology and Gravitation Theories #Dark Matter and Cosmic Phenomena #Dark energy #Dark matter #Galaxies: Formation, Evolution, Phenomena #Galaxy #Omega #Physics #Quantum mechanics #Redshift #astro-ph
paper · pdf · doi:10.1103/physrevd.66.083515
published as Phys.Rev.D66:083515,2002 · errata version: coding bug in Omega_{DE} variation fixed, leading to stronger Fisher conclusions on dark energy constraints
openalex publication_date 2002/10/30 · arxiv created 2002/11/27 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Reconstructed from lensing tomography, the evolution of the dark matter density field in the well-understood linear regime can provide model-independent constraints on the growth function of structure and the evolution of the dark energy density. We examine this potential in the context that high-redshift cosmology has in the future been fixed by cosmic microwave background measurements. We construct sharp tests for the existence of multiple dark matter components or a dark energy component that is not a cosmological constant. These functional constraints can be transformed into physically motivated model parameters. From the growth function, the fraction of the dark matter in a smooth component, such as a light neutrino, may be constrained to a statistical precision of \ensuremathσ(f)\ensuremath≈0.0006fsky^\ensuremath-1/2 by a survey covering a fraction of sky fsky with a redshift resolution \ensuremathΔz=0.1. For the dark energy, a parametrization in terms of the present energy density \ensuremathΩDE, equation of state w, and its redshift derivative w^\ensuremath', the constraints correspond to \ensuremathσ(w)=0.009fsky^\ensuremath-1/2 and a degenerate combination of the other two parameters. For a fixed \ensuremathΩDE, \ensuremathσ(w^\ensuremath')=0.046fsky^\ensuremath-1/2.