Disentangling the growth rate of perturbations from the HI bias using only clustering data from galaxy surveys

TL;DR

This paper introduces a method to determine the growth rate of cosmic density perturbations directly from galaxy clustering data, without relying on additional datasets, and extends it to measure the 21-cm bias from intensity maps.

Contribution

It presents a novel approach to extract the growth rate of perturbations solely from clustering data, bypassing the need for external bias measurements or additional datasets.

Findings

Reconstructs the growth rate $f(z)$ using BAO and RSD measurements alone.

Demonstrates the potential to measure 21-cm bias from clustering data.

Provides a new way to interpret intensity mapping signals.

Abstract

This work serves two-fold purpose. Firstly, we provide an alternative to the traditional method of determining the growth rate of density perturbations $f(z)$. In usual practice, $f(z)$ can not be directly measured from tracer clustering at some redshift without knowledge of the bias. While the bayron acoustic oscillation (BAO) imprint allows the determination of $(D_A(z), H(z))$, redshift space anisotropy (RSD) allows the measurement of a quantity $f_8(z) = f(z) \sigma_{8,0} D_{+}(z)$. To extract $f(z)$ from $f_8(z)$, one usually requires some other data set. We show that precise BAO and RSD measurements in and around some key redshifts themselves can solely reconstruct $f(z)$ without requiring any other data sets. Secondly, we extend this approach to another tracer, namely the post-reionization 21-cm brightness temperature intensity maps. We demonstrate that the measured $f(z)$ from purely redshift space clustering allows us to measure the 21-cm bias, which is a largely unknown quantity. This may help interpret the observed intensity mapping signal in the future.