baselines within an array configuration can reduce uncertainties in the thermal noise estimates [@Parsons:2012p95]. However, the gain depends on whether they are perfectly or partially coherent [@Hazelton:2013p1481].

In @Pober:2014p35, these authors consider numerous foreground removal strategies, including a variety of treatments for the summation over redundant baselines and how to define the transition from the foreground ‘wedge’. We defer the reader to their work for more detailed discussions, and highlight that throughout this work, we adopt what they refer to as their ‘moderate’ foreground removal. For this, we assume a fixed location of the foreground ‘wedge’ to extend $\Delta k_{\parallel} = 0.1 \,h$ Mpc$^{-1}$ beyond the horizon limit [@Pober:2014p35] and compute our estimates of the thermal noise PS sampling only $k$-modes that fall within the [EoR]{} observing window. This strategy further assumes the coherent addition of all redundant baselines.

  Parameter                  LOFAR   HERA             SKA           
  ------------------------- ------- ------- ----------------------- --
  Telescope antennas          48      331             866           
  Diameter (m)               30.8     14              35            
  Collecting area (m$^2$)    35762   50953          833190          
  $T_{\rm rec}$ (K)           140     100    0.1T$_{\rm sky}$ + 40  
  Bandwidth (MHz)              8       8               8            
  Integration time (hrs)     1000    1000            1000           

  : Summary of telescope parameters we use to compute sensitivity profiles (see the text for further 