qualitatively compare the merits of a variety of telescope designs through a measurement of the overall sensitivity of the 21 cm PS. To perform this direct comparison, these authors set a variety of design specific parameters to be equivalent. Instead, we perform our comparison using the exact design specifics of each experiment as outlined below. Note, the difference is marginal, however using system specific parameters we better mimic the expected overall sensitivities of the modelled telescope. For all, we model $T_{\rm sky}$ using the frequency dependent scaling $T_{\rm sky} = 60\left(\frac{\nu}{300~{\rm MHz}}\right)^{-2.55}~{\rm K}$ [@Thompson2007].

-   *LOFAR:* we model LOFAR using the antennas positions listed in @vanHaarlem:2013p200. Following the approach of @Pober:2014p35, we focus solely on the Netherlands core for the purposes of detecting the 21 cm PS assuming that all 48 high-band antennas (HBA) stations can be correlated separately maximizing the total number of redundant baselines. We assume $T_{\rm rec} =140$ K consistent with @Jensen:2013p1389.\

-   *HERA:* we follow the design specifics outlined in @Beardsley:2014p1529, where they propose a final design including 331 antennas. Each antennas is 14m in diameter closely packed into a hexagonal configuration to maximize the total number of redundant baselines [@Parsons:2012p95]. While the total observing area 