Reconstructing HI power spectrum with minimal parameters using the dark matter distribution beyond halos

TL;DR

This paper introduces a novel method to reconstruct the HI power spectrum from dark matter distributions beyond halos, improving modeling accuracy for large-scale structure studies using intensity mapping.

Contribution

The proposed method reconstructs the HI power spectrum from dark matter distributions truncated at specific scales, reducing reliance on halo-based assumptions and capturing the slope at BAO scales.

Findings

Reproduces HI power spectrum slope at BAO scales ($k<1 h/{ m Mpc}$)

Fluctuation of spin temperature affects brightness temperature power spectrum by up to 8%

Method compares HI and dark matter density profiles around halos

Abstract

Intensity mapping of 21-cm line by several radio telescope experiments will probe the large-scale structure of the Universe in the post-reionization epoch. It requires a theoretical framework of neutral hydrogen (HI) clustering, such as modelling of HI power spectrum for Baryon Acoustic Oscillations (BAO) analysis. We propose a new method for reconstructing the HI map from dark matter distribution using N-body simulations. Several studies attempt to compute the HI power spectrum with N-body simulations by pasting HI gas at the dark matter halo centre, assuming the relation between the halo and HI masses. On the other hand, the method proposed in this paper reproduces the HI power spectrum from simulated dark matter distribution truncated at specific scales from the halo centre. With this method, the slope of HI power spectrum is reproduced well at the BAO scales, $k<1 h/{\rm Mpc}$. Furthermore, we find the fluctuation of spin temperature, which is often ignored at the post-reionization epoch, alters the power spectrum of brightness temperature by at most 8% in the power spectrum. Finally, we discuss how our method works by comparing the density profiles of HI and dark matter around the dark matter halos.