Formation of the large-scale structure of the Universe
arXiv:1209.0371 · doi:10.3367/UFNr.0181.201110a.1017
Abstract
In this review, the formation, evolution, and decay of the large-scale structure of the Universe is discussed in the context of observational data, numerical simulations, and the Cosmological Standard Model (CSM). Problems concerning measuring and interpreting cosmological parameters, determining the composition of matter, and normalizing density perturbation spectra are especially highlighted.
arXiv comment66 pages, 19 figures
References in corpus (22)
- A Universal Density Profile from Hierarchical Clustering
- Seven-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
- Large scale bias and the peak background split
- Toward a halo mass function for precision cosmology: the limits of universality
- A Unified Model for the Evolution of Galaxies and Quasars
- The Large Scale Bias of Dark Matter Halos: Numerical Calibration and Model Tests
- Measuring the Baryon Acoustic Oscillation scale using the SDSS and 2dFGRS
- Optical Mass Estimates of Galaxy Clusters
- Hierarchical galaxy formation and substructure in the Galaxy's stellar halo
- A new measurement of the bulk flow of X-ray luminous clusters of galaxies
- Local galaxy flows within 5 Mpc
- The Observational Mass Function of Nearby Galaxy Clusters
- Hierarchical Clustering and the Butcher-Oemler Effect
- Weak lensing, dark matter and dark energy
- Dark energy: myths and reality
- A Map of the Integrated Sachs-Wolfe Signal from Luminous Red Galaxies
- The DEEP2 Galaxy Redshift Survey: The Evolution of Void Statistics from z~1 to z~0
- Legacy data and cosmological constraints from the angular-size/redshift relation for ultra-compact radio sources
- Large-scale fluctuations in the distribution of galaxies from the Two Degree Field Galaxy Redshift Survey
- Halo Concentration and the Dark Matter Power Spectrum
- Direct Distance Measurements to Superluminal Radio Sources
- Detectability of High Redshift Ellipticals in the Hubble Deep Field