21 Centimeter Fluctuations from Cosmic Gas at High Redshifts

Abstract

The relatively large Thomson optical depth, τ es , inferred recently from the WMAP observations suggests that the universe was reionized in a more complex manner than previously believed. However, the value of τ es provides only an integral constraint on the history of reionization and, by itself, cannot be used to determine the nature of the sources responsible for this transition. Here we show that the evolution of the ionization state of the intergalactic medium (IGM) at high redshifts can be measured statistically using fluctuations in 21 cm radiation from neutral hydrogen. By analogy with the mathematical description of anisotropies in the cosmic microwave background, we develop a formalism to quantify the variations in 21 cm emission as a function of both frequency and angular scale. Prior to and following reionization, fluctuations in the 21 cm signal are mediated by density perturbations in the distribution of matter. Between these epochs, pockets of gas surrounding luminous objects become ionized, producing large H II regions. These "bubbles" of ionized material imprint features into the 21 cm power spectrum that make it possible to distinguish them from fluctuations produced by the density perturbations. The variation of the power spectrum with frequency can be used to infer the evolution of this process. As has been emphasized previously by others, the absolute 21 cm signal from neutral gas at high redshifts is difficult to detect as a result of contamination by foreground sources. However, we argue that this source of noise can be suppressed by comparing maps closely spaced in frequency, i.e., redshift, so that 21 cm fluctuations from the IGM can be measured against a much brighter, but smoothly varying (in frequency), background.