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It is believed that the first star-forming galaxies are the main drivers ofcosmic reionization. It is usually assumed that there is a one-to-onerelationship between the star formation rate (SFR) inside a galaxy and the hosthalo mass in semi-analytical/numerical modeling of large-scale ionization mapsduring the epoch of reionization. However, more accurate simulations andobservations suggest that the SFR and ionizing luminosity in galaxies may varyconsiderably even if the host halo mass is the same. This astrophysical scattercan introduce an additional non-Gaussianity in the cosmological [HI]$_{\text{21cm}}$ signal, which is already expected to have an inherenttime-evolving non-Gaussianity due to reionization. Here, we have studied theimpact of the scatter on the [H I]$_{\text{21cm}}$ bispectrum usingsemi-numerical simulations. The scatter primarily affects small ionizedregions, whereas the large ionized bubbles remain largely unaffected. Although,the fractional change in the [H I]$_{\text{21cm}}$ bispectra due to the scatteris found to be more than a factor of $10$ at large scales ($\lesssim 1\, {\rmMpc}^{-1}$), it is found to be statistically not significant. However, we havefound the impact due to the scatter to be significant ($|\langle \Delta B\rangle/B_{\text{no-scatter}}| \sim 1$) at small scales ($k\sim2.55\, {\rmMpc}^{-1}$) and at $\overline{x}_{\rm HI}\sim 0.8$. We have also found that1000 hours of SKA1-Low like observation is unlikely to detect the signatures ofthe scatter at these small scales.

Impact of astrophysical scatter on the Epoch of Reionization [H I]$_{\rm 21cm}$ bispectrum