Detecting the redshifted 21cm forest during reionization

TL;DR

This paper uses simulations to show that detecting the 21cm forest during reionization with future telescopes like SKA can reveal the IGM's thermal history, with detection feasible within a year under certain conditions.

Contribution

The study provides the first detailed simulation-based analysis of 21cm forest detection prospects during reionization, incorporating x-ray heating and bubble percolation effects.

Findings

Detection of 21cm absorption is possible within a year with SKA.

Signal variance increase aids in detection.

Detection does not depend on properties of narrow absorption lines.

Abstract

The 21cm forest -- HI absorption features in the spectra of high-redshift radio sources -- can potentially provide a unique probe of the largely neutral intergalactic medium (IGM) during the epoch of reionization. We present simulations of the 21cm forest due to the large scale structure of the reionization-era IGM, including a prescription for x-ray heating and the percolation of photoionization bubbles. We show that, if detected with future instruments such as the Square Kilometer Array (SKA), the 21cm forest can provide a significant constraint on the thermal history of the IGM. Detection will be aided by consideration of the sudden increase in signal variance at the onset of 21cm absorption. If radio foregrounds and the intrinsic source spectra are well understood, the flux decrement over wide bandwidths can also improve detection prospects. Our analysis accounts for the possibility of narrow absorption lines from intervening dense regions, but, unlike previous studies, our results do not depend on their properties. Assuming x-ray heating corresponding to a local stellar population, we estimate that a statistically significant detection of 21cm absorption could be made by SKA in less than a year of observing against a Cygnus A-type source at $z \sim 9$, as opposed to nearly a decade for a significant detection of the detailed forest features. We discuss observational challenges due to uncertainties regarding the abundance of background sources and the strength of the 21cm absorption signal.