Evolution of how much H I emission in the CGM is observable as a function of the minimum baseline at 20 Mpc. The rest of the survey parameters are analogous to the MHONGOOSE survey’s low-resolution case (beam FWHM ∼ 65”, sensitivity ∼10¹⁸ cm⁻²). Solid lines show the CGM ratio with satellites removed, while the dashed–dotted lines show the ratio with satellites present. The vertical dashed line shows the MeerKAT minimum baseline (b_min = 29 m). With satellites removed, observing ∼90% of the CGM signal would require minimum baselines of a few meters, likely requiring single-dish data.