Implications of the Background Radiation for Cosmic Structure Formation

Abstract

The CMB is a remarkably distortionless blackbody, and this strongly constrains the amount of energy that can have been injected at high redshift, thereby limiting the role that hydrodynamical amplification can have played in cosmic structure formation. The current data on primary anisotropies (those calculated using linear response theory) provide very strong support for the gravitational instability theory and encouraging support that the initial fluctuation spectrum was not far off the scale invariant form that inflation (and defect) models prefer. By itself, the (low resolution) 4-year DMR data allow relatively precise \sigma_8 normalization factors for density fluctuation spectra and rough information on the large scale slope of the anisotropy power, thereby focusing our attention on a relatively narrow set of viable models. Useful formulae relating the DMR bandpower to \sigma_8 and post-inflation scalar and tensor power spectra measures are given. Smaller angle data are consistent with these models, and will soon be powerful enough to strongly select among the possibilities, although there remains much room for surprises. In spite of foregrounds, future high resolution experiments should be able to allow precise determination of many combinations of the cosmological parameters that define large scale structure formation theories: mode (adiabatic/isocurvature, gravity wave content), shape functions, amplitudes, and various mean energy densities. Secondary anisotropies arising from nonlinear structures will be invaluable probes of shorter-distance aspects of structure formation theories.