Cosmological Implication of Cross-correlation between Galaxy Clustering and 21-cm Line Intensity Mapping

TL;DR

This paper demonstrates that cross-correlating galaxy clustering with 21-cm intensity mapping significantly improves constraints on cosmic structure growth and neutral hydrogen content, surpassing previous methods and enabling detailed post-reionization astrophysics.

Contribution

It introduces a Fisher matrix analysis incorporating nonlinear RSD to show the enhanced constraining power of cross-correlation surveys for cosmology and HI content.

Findings

Constraints on structure growth are doubled with cross-correlation.

Neutral hydrogen density Omega_HI can be measured to sub-percent accuracy.

Cross-correlation breaks degeneracies present in linear power spectrum analysis.

Abstract

The apparent anisotropies of galaxy clustering and 21-cm mapping in redshift space offer a unique opportunity to simultaneously probe cosmic expansion and gravity on cosmological scales through the Alcock-Paczynski (AP) effect and redshift-space distortions (RSD). Although improved theoretical models exist for anisotropic clustering, their applicability is limited by the non-perturbative smearing effect caused by the randomness of relative velocities. Here, we consider an alternative approach using the statistical power of cross-correlation between galaxy clustering and 21-cm line intensity mapping. Based on Fisher matrix analysis, fully incorporating nonlinear RSD, we estimate the benefit of combining both observables. We find that, for spectroscopy surveys like DESI combined with 21-cm line-intensity mapping surveys, the constraint on the growth of structure is improved by a factor of two relative to the galaxy auto-correlation, while the constraint on the cosmic expansion is only slightly improved. Crucially, such an observation can strongly constrain the neutral hydrogen (HI) content Omega_HI to a sub-percent level. This level of precision unlocks the potential of this method to probe post-reionization astrophysics with enhanced precision. It would far surpass existing constraints from stacked 21-cm emission (resulting in ~ 50%-100% uncertainties) and break the degeneracy between Omega_HI and the HI bias b_HI inherent in linear-regime power spectrum analysis. This cross-correlation approach effectively compensates for the loss of constraining power when using galaxy clustering alone.