We use the best imaging field of Cen A (b = 19°, E(B − V) = 0.12) to assess the effects of MW disk contamination and extinction in detecting dwarf galaxies. (a) Same as Figure 8 and shown here just for comparison reasons. (b) Our Cen A simulation results for a distance of 3.5 Mpc, demonstrating that both extinction and foreground MW star counts may strongly affect dwarf detectibility, especially for low surface brightness systems (μ_V,0 ≳ 29 mag arcsec⁻²) and objects fainter than M_V ≈ −8.