Median cylindrical Stokes I power spectra of the 13 night simulations with two different sky models per LST bin based on the 13 observations including uv-cell flagging. Left: Cas A and Cyg A model. Dashed lines indicate, from bottom to top, 5° (the primary beam), 20° and instrumental horizon delay lines. Right: the DI-calibration model (including the 1416 brightest components that account for ~99% of the flux from our sky model) and Α-team sources. LST03-06 and LST06-09 in both simulations show lower power compared to other LST bins and this trend is consistent with what we have seen with the excess variance in Fig. 7 and the top panel of Fig. 8.