Can the 21 cm signal probe Population III and II star formation?

TL;DR

This paper explores how the 21 cm signal from the intergalactic medium can distinguish between Population III and II star formation histories at high redshifts, providing insights into early cosmic star formation.

Contribution

It models the 21 cm signal based on different star formation rates of Pop III and II stars, highlighting how the signal can reveal the dominant stellar population and initial mass function effects.

Findings

Pop III stars cause early IGM heating and deep absorption signals.

Pop II star formation leads to gradual heating and later signal changes.

Next-generation telescopes can differentiate Pop III and II contributions.

Abstract

Using varying models for the star formation rate (SFR) of Population (Pop) III and II stars at z>6 we derive the expected redshift history of the global 21 cm signal from the inter-galactic medium (IGM). To recover the observed Thomson scattering optical depth of the cosmic microwave background (CMB) requires SFRs at the level of ~ 10^-3 Msun/yr/Mpc^3 at z ~ 15 from Pop III stars, or ~ 10^-1Msun/yr/Mpc^3 at z ~ 7 from Pop II stars. In the case the SFR is dominated by Pop III stars, the IGM quickly heats above the CMB at z > 12 due to heating from supernovae. In addition, Lyman-alpha photons from haloes hosting Pop III stars couple the spin temperature to that of the gas, resulting in a deep absorption signal. If the SFR is dominated by Pop II stars, the IGM slowly heats and exceeds the CMB temperature at z ~ 10. However, the larger and varying fraction of Pop III stars is able to break this degeneracy. We find that the impact of the initial mass function (IMF) of Pop III stars on the 21 cm signal results in an earlier change to a positive signal if the IMF slope is ~ -1.2. Measuring the 21 cm signal at z > 10 with next generation radio telescopes such as the Square Kilometre Array will be able to investigate the contribution from Pop III and Pop II stars to the global star formation rate.