The morphology of the redshifted 21-cm signal from the Cosmic Dawn

Abstract

The spatial fluctuations in the tomographic maps of the redshifted 21-cm signal from the Cosmic Dawn (CD) crucially depend on the size and distribution of the regions with gas temperatures larger than the radio background temperature. In this article, we study the morphological characteristics of such emission regions and their absorption counterparts using the shape diagnostic tool {\sc surfgen2}. Using simulated CD brightness temperature cubes of the 21-cm signal, we find that the emission regions percolate at stages with the filling factor of the emission regions \(FF_{\rm emi}\gtrsim 0.15\). Percolation of the absorption regions occurs for \(FF_{\rm abs}\gtrsim 0.05\). The largest emission and absorption regions are topologically complex and highly filamentary for most parts of the CD. The number density of these regions as a function of the volume shows the power-law nature with the power-law indexes \(\approx -2\) and \(-1.6\) for the emission and absorption regions, respectively. Overall, the planarity, filamentarity and genus increase with the increase of the volume of both emission and absorption regions.