Contribution of Galactic free-free emission to the foreground for EoR signal in SKA experiments

Abstract

The overwhelming foreground contamination hinders the accurate detection of the 21-cm signal of neutral hydrogen during the Epoch of Reionization (EoR). Among various foreground components, the Galactic free-free emission is less studied, so that its impact on the EoR observations remains unclear. In this work, we employ the observed $\mathrm{H}\alpha$ intensity map with the correction of dust absorption and scattering, the Simfast21 software, and the latest SKA1-Low layout configuration to simulate the SKA "observed" images of Galactic free-free emission and the EoR signal. By calculating the one-dimensional power spectra from the simulated image cubes, we find that the Galactic free-free emission is about $10^{3.5}$-$10^{2.0}$, $10^{3.0}$-$10^{1.3}$, and $10^{2.5}$-$10^{1.0}$ times more luminous than the EoR signal on scales of $0.1\mathrm{Mp}{\mathrm{c}}^{-1}<\mathrm{k}<2\mathrm{Mp}{\mathrm{c}}^{-1}$ in the $116$-$124$, $146$-$154$, and $186$-$194$ $\mathrm{MHz}$ frequency bands. We further analyse the two-dimensional power spectra inside the properly defined EoR window and find that the leaked Galactic free-free emission can still cause non-negligible contamination, as the ratios of its power (amplitude squared) to the EoR signal power can reach about $200\%$, $60\%$, and $15\%$ on scales of $1.2\mathrm{Mp}{\mathrm{c}}^{-1}$ in three frequency bands, respectively. Therefore, we conclude that the Galactic free-free emission, as a severe contaminating foreground component, needs to be carefully treated in the forthcoming deep EoR observations.

arXiv comment15 pages, 10 figures, the MNRAS published version

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