X-ray heating before reionization

Many models of early structure formation predict a period of heating immediately preceding reionization, when X-rays raise the gas temperature above that of the cosmic microwave background. These X-rays are often assumed to heat the intergalactic medium (IGM) uniformly, but in reality will heat the gas more strongly closer to the sources. We develop a framework for calculating fluctuations in the 21 cm brightness temperature that originate from this spatial variation in the heating rate. High-redshift sources are highly clustered, leading to significant gas temperature fluctuations (with fractional variations ∼ 40%, peaking on k ∼ 0.1 Mpc scales). This induces a distinctive peak-trough structure in the angle-averaged 21 cm power spectrum, which may be accessible to the proposed Square Kilometre Array. This signal reaches the ∼ 10 mK level, and is stronger than that induced by Lyα flux fluctuations. As well as probing the thermal evolution of the IGM before reionization, this 21 cm signal contains information about the spectra of the first X-ray sources. Finally, we consider disentangling temperature, density, and Lyα flux fluctuations as functions of redshift.