details).[]{data-label="tab:TelescopeParams"}

We include another level of conservatism to our errors, applying a strict $k$-mode cut to our 21 cm PS. We sample only modes above $|k|$ = 0.15 Mpc$^{-1}$. Following the moderate foreground removal strategy of @Pober:2014p35, it effectively turns out that there is limited information available below this $k$-mode; however, we still apply this strict cut on top of the estimated total noise PS. Modes with $|k| \geq$ 0.15 Mpc$^{-1}$ can still be affected by the foreground ‘wedge’ due to its spherically asymmetric structure, hence we apply both cuts.

Since equation (\[eq:NoisePS\]) is computed for each individual $k$-mode, the sample variance of the cosmological PS can be easily included to produce an estimate of the total noise by performing an inverse-weighted summation over all the individual modes [@Pober:2013p41], $$\begin{aligned}
 \label{eq:T+S}
\delta\Delta^{2}_{\rm T+S}(k) = \left(\sum_{i}\frac{1}{(\Delta^{2}_{{\rm N},i}(k) + \Delta^{2}_{21}(k))^{2}}\right)^{-1/2},\end{aligned}$$ where $\delta\Delta^{2}_{\rm T+S}(k)$ is the total uncertainty from thermal noise and sample variance in a given $k$-mode and $\Delta^{2}_{21}(k)$ is the cosmological 21 cm PS. Here, we assume Gaussian errors for the cosmic-variance term, which is a good approximation on large scales.

Within this work, we restrict our analysis to three telescope designs (LOFAR, HERA and the SKA). In @Pober:2014p35, these authors 