\begin{document}$ 10^4\,\mathrm{deg}^2 $\end{document} and 1 year of observation, we compare continuum surveys with 10 MHz bandwidth and 21-cm forest surveys with 5 kHz resolution. Our results show that a minimum collecting area of ~6500 m2 enables detection at \begin{document}$ z \sim 6 $\end{document}, while SKA-like arrays (\begin{document}$ N_{\mathrm{st}} = 512 $\end{document}) extend the detection limit to \begin{document}$ z \sim 10 $\end{document} for 21-cm forest surveys and \begin{document}$ z \sim 16 $\end{document} for continuum surveys. Larger arrays with \begin{document}$ N_{\mathrm{st}} = 2048 $\end{document} can reach \begin{document}$ z \sim 11 $\end{document} in 21-cm forest mode. We also explore configurations that maintain fixed collecting areas while increasing the number to enhance survey efficiency. This boosts source detection but significantly increases the data volume and computational demands. These results underscore the importance of optimizing array design for different survey goals and balancing sensitivity, spectral resolution, and data management. A well-designed Moon-based array could open a new observational window to reionization and early cosmic structure formation."> Configuration requirements for 21-cm forest background quasar searches with Moon-based interferometer -
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