The role of Pop III stars and early black holes in the 21cm signal from Cosmic Dawn

TL;DR

This paper models the Cosmic Dawn 21cm signal using a semi-analytical approach, highlighting the influence of Pop III stars and early black holes on the signal's features and matching observations like EDGES.

Contribution

It introduces the Cosmic Archaeology Tool (CAT) to simulate early universe evolution, incorporating Pop III stars and black holes, and reproduces key 21cm signal features.

Findings

The model predicts a maximum absorption of -95 mK at z~26.5.

Early black holes heat the IGM, suppressing absorption and causing emission at z<27.

Reproduces EDGES signal timing and depth with a modified radio background.

Abstract

Modeling the 21cm global signal from the Cosmic Dawn is challenging due to the many poorly constrained physical processes that come into play. We address this problem using the semi-analytical code "Cosmic Archaeology Tool" (CAT). CAT follows the evolution of dark matter halos tracking their merger history and provides an ab initio description of their baryonic evolution, starting from the formation of the first (Pop III) stars and black holes (BHs) in mini-halos at z > 20. The model is anchored to observations of galaxies and AGN at z < 6 and predicts a reionization history consistent with constraints. In this work we compute the evolution of the mean global 21cm signal between $4\leq z \leq 40$ based on the rate of formation and emission properties of stars and accreting black holes. We obtain an absorption profile with a maximum depth $\delta {\rm T_b} = -95$ mK at $z \sim 26.5$ (54 MHz). This feature is quickly suppressed turning into an emission signal at $z = 20$ due to the contribution of accreting BHs that efficiently heat the IGM at $z < 27$. The high-$z$ absorption feature is caused by the early coupling between the spin and kinetic temperature of the IGM induced by Pop III star formation episodes in mini-halos. Once we account for an additional radio background from early BHs, we are able to reproduce the timing and the depth of the EDGES signal only if we consider a smaller X-ray background from accreting BHs, but not the shape.