The effects of the small-scale DM power on the cosmological neutral hydrogen (\HI) distribution at high redshifts

TL;DR

This paper investigates how small-scale dark matter models like LFDM and ULA influence high-redshift neutral hydrogen distribution, using simulations and observations to constrain dark matter properties and their effects on reionization.

Contribution

It introduces a novel analysis of small-scale dark matter effects on the HI 21-cm signal and provides new bounds on dark matter formation redshift and axion mass from high-redshift observations.

Findings

LFDM and ULA models increase HI power spectrum by 2-10 times.

Reionization constraints imply bounds: z_f > 4×10^5, m_a > 2.6×10^{-23} eV.

Weaker bounds from damped Lyman-alpha data: z_f > 2×10^5, m_a > 10^{-23} eV.

Abstract

The particle nature of dark matter remains a mystery. In this paper, we consider two dark matter models---Late Forming Dark Matter (LFDM) and Ultra-Light Axion (ULA) models---where the matter power spectra show novel effects on small scales. The high redshift universe offers a powerful probe of their parameters. In particular, we study two cosmological observables: the neutral hydrogen (HI) redshifted 21-cm signal from the epoch of reionization, and the evolution of the collapsed fraction of HI in the redshift range $2 < z < 5$. We model the theoretical predictions of the models using CDM-like N-body simulations with modified initial conditions, and generate reionization fields using an excursion-set model. The N-body approximation is valid on the length and halo mass scales studied. We show that LFDM and ULA models predict an increase in the HI power spectrum from the epoch of reionization by a factor between 2--10 for a range of scales $0.1<k<4 \, \rm Mpc^{-1}$. Assuming a fiducial model where a neutral hydrogen fraction $\bar{x}_{HI}=0.5$ must be achieved by $z=8$, the reionization process allows us to put approximate bounds on the redshift of dark matter formation $z_f > 4 \times 10^5$ (for LFDM) and the axion mass $m_a > 2.6 \times 10^{-23} \, \rm eV$ (for ULA). The comparison of the collapsed mass fraction inferred from damped Lyman-$\alpha$ observations to the theoretical predictions of our models lead to the weaker bounds: $z_f > 2 \times 10^5$ and $m_a > 10^{-23} \, \rm eV$. These bounds are consistent with other constraints in the literature using different observables; we briefly discuss how these bounds compare with possible constraints from the observation of luminosity function of galaxies at high redshifts. In the case of ULAs, these constraints are also consistent with a solution to the cusp-core problem of CDM.