LST-dependence of excess variance and two sky models. Top: excess variance averaged over k per night and per LST in orange. Middle: simulated Stokes I cylindrical power spectra averaged over k per night and LST with Cas A and Cyg A in red. Bottom: simulated Stokes I cylindrical power spectra averaged over k per night and LST with the DI-calibration model (including the 1416 brightest components that account for ~99% of the flux from our sky model) and A-team sources in green. Different markers indicate different observations. The difference between nights in simulations mainly comes from the different number of sub-bands per night (see Table 1) and flagging based on uv-cells. The excess variance from observations and the simulated Stokes I power from the two models (in middle and bottom) shows a similar LST-dependence.