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The brightness temperature of the redshifted 21cm line brings richinformation on the Inter Galactic Medium (IGM) from the Cosmic Dawn and Epochof Reionization (EoR). While the power spectrum is a useful tool tostatistically investigate the 21cm signal, the 21cm brightness temperaturefield is highly non-Gaussian, and the power spectrum is inadequate tocharacterize the non-Gaussianity. The Minkowski Functionals (MFs) are promisingtools to extract non-gaussian features of the 21cm signal and give topologicalinformation such as morphology of ionized bubbles. In this work, we study the21cm line signal in detail with MFs. To promote understanding of basic featuresof the 21cm signal, we calculate the MFs of not only the hydrogen neutralfraction but the matter density and spin temperature, which contribute to thebrightness temperature fluctuations. We find that the structure of thebrightness temperature depends mainly on the ionized fraction and the spintemperature at late and early stages of the EoR, respectively. Further, weinvestigate the redshift evolution of the MFs at $7 < z < 20$. Then, we findthat, after the onset of reionization, the MFs reflect mainly the ionizedbubble property. In addition, the MFs are sensitive to model parameters whichare related to the topology of ionized bubbles and we consider the possibilityof constraining the parameters by the future 21cm signal observations.

Studying topological structure in the epoch of reionization with 3D-Minkowski functionals of 21cm line fluctuations