Constraining Reionization Morphology and Source Properties with 21cm-Galaxy Cross-Correlation Surveys

TL;DR

This paper demonstrates that 21cm-Galaxy cross-correlation surveys can significantly improve constraints on reionization morphology and source properties, especially with precise redshifts and deep galaxy surveys, using simulation-based inference.

Contribution

It introduces a framework for quantifying the constraining power of 21cm-Galaxy cross-power spectra on reionization parameters and source properties, highlighting the importance of redshift accuracy and survey depth.

Findings

Cross-power spectra provide unbiased constraints on neutral hydrogen fraction.

Cross-correlations reduce parameter uncertainty compared to 21cm auto-power.

Precise redshifts are crucial for effective cross-correlation analysis.

Abstract

Cross-correlations between 21cm observations and galaxy surveys provide a powerful probe of reionization by reducing foreground sensitivity while linking ionization morphology to galaxies. We quantify the constraining power of 21cm-Galaxy cross-power spectra for inferring neutral hydrogen fraction $x_\mathrm{HI}(z)$ and mean overdensity $\langle 1+\delta_\mathrm{HI} \rangle(z)$, exploring dependence on field of view, redshift precision $\sigma_z$, and minimum halo mass $M_\mathrm{h,min}$. We employ our simulation-based inference framework EoRFlow for likelihood-free parameter estimation. Mock observations include thermal noise for 100h SKA-Low with foreground avoidance and realistic galaxy survey effects. For a fiducial survey ($\mathrm{FOV}=100\,\mathrm{deg}^2$, $\sigma_z=0.001$, $M_\mathrm{h,min}=10^{11}\mathrm{M}_\odot$), cross-power spectra yield unbiased constraints with posterior volumes (PV) of $\sim$10% relative to priors. Cross-power measurements reduce PV by 20-30% versus 21cm auto-power alone. With foreground avoidance, spectroscopic redshift precision is essential; photometric redshifts render cross-correlations uninformative. Notably, cross-power spectra constrain ionizing source properties, the escape fraction $f_\mathrm{esc}$ and star formation efficiency $f_*$, which remain degenerate in auto-power (PV $>$60%). Tight constraints require either deep surveys detecting faint galaxies ($M_\mathrm{h,min} \sim 10^{10}\mathrm{M}_\odot$) with moderate foregrounds, or conservative mass limits with optimistic foreground removal (PV $<$15%). 21cm-Galaxy cross-correlations enhance morphology constraints beyond auto-power while enabling previously inaccessible source property constraints. Realizing full potential requires precise redshifts and either faint galaxy detection limits or improved 21cm foreground cleaning.