Predictions of the Besançon model for field stars (Robin et al. 2003) in our VIMOS field. Compared to Fig. 8, the RGB window (23.9 <I₀ < 24.7 and 1.5 < (V − I)₀ < 3.5, as described in Sect. 4.2), is mostly uncontaminated by the Milky Way’s stars as the majority are brighter than NGC 5128’s TRGB at I₀ = 23.9. Our chosen magnitude limits of I₀ = 27.0 and V₀ = 28.2, based on the depth of our VIMOS data, yield the diagonal cut on the righthand side of the field star predictions.