Median cylindrical Stokes I power spectra of the 13 night simulations with the DI-calibration model (including the 1416 brightest components that account for ~99% of the flux from our sky model) and Α-team sources per LST bin with 4 different flagging conditions. Top left: uv-cells not flagged and RFI unflagged. Top right: uv-cells flagged and RFI unflagged (the condition we use for the analysis). Bottom left: uv-cells not flagged and RFI flagged. Bottom right: uv-cells flagged and RFI flagged. Dashed lines indicate, from bottom to top, 5° (the primary beam), 20° and instrumental horizon delay lines. RFI flagging adds extra power to the EoR window (bottom left and right) and unflagged bad uv-cells add vertical structures in the power spectra (top left). Hence, applying uv-cell flagging and unflagging RFI (top right) is optimal for the power spectrum estimation in this case.