Interpretation of 21 cm Auto Power Spectrum Measurement at $z\sim 1$ by the Canadian Hydrogen Intensity Mapping Experiment

TL;DR

This paper interprets 21 cm auto power spectrum measurements at redshift ~1 from CHIME using parametric modeling and simulation comparisons, revealing insights into hydrogen distribution and redshift-space distortions.

Contribution

It introduces two approaches for interpreting 21 cm power spectrum data, including a parametric model constraining hydrogen bias and density, and a comparison with IllustrisTNG simulations highlighting nonlinear effects.

Findings

Measurement disagrees with TNG simulations at 3-4 sigma

Redshift-space distortions significantly impact the power spectrum

Results demonstrate 21 cm mapping's potential for astrophysical insights

Abstract

Observations with the Canadian Hydrogen Intensity Mapping Experiment (CHIME) have been used to measure the 21 cm intensity mapping auto power spectrum, at $z\sim 1$, over a frequency range from 608.2 MHz to 707.8 MHz at wavenumbers $0.4~h~{\rm Mpc}^{-1} \lesssim k \lesssim 1.5~h~{\rm Mpc}^{-1}$. In this paper, we present the results of two different approaches to interpreting this measurement. In the first approach, we use a parametric power spectrum model to constrain an amplitude parameter, defined as $\mathcal{A}^2_{\rm HI} \equiv 10^6 \Omega_{\rm HI}^2(b^2_{\rm HI}+\langle f \mu^2\rangle)^2$, where $\Omega_{\rm HI}$ is the cosmological density parameter for atomic hydrogen ($\rm HI$), $b_{\rm HI}$ is the linear bias for $\rm HI$, and $\langle f \mu^2\rangle$ incorporates the dominant large-scale impact of redshift-space distortions on the angle-averaged power spectrum. Imposing an additional prior on either $\Omega_{\rm HI}$ or $b_{\rm HI}$, based on values in the literature, allows us to break the pairwise degeneracy between those two parameters. In the second approach, we compare CHIME's measurement with predictions for the power spectrum of $\rm HI$ from the IllustrisTNG simulations, finding that the measurement disagrees with the TNG100 run at $3.1\sigma$ and the TNG300 run at $4.0\sigma$. This disagreement is most likely attributable to the strength of nonlinear redshift-space clustering of $\rm HI$ in the simulations, rather than the total abundance of $\rm HI$, and invites further investigation of the physical processes in the simulations that determine the behavior of $\rm HI$ at nonlinear scales. These results exemplify the ability of 21 cm intensity mapping to provide astrophysical information using measurements at nonlinear scales.