Same as in Figure 5, but for the Std-lrg model. The larger grains are less strongly coupled to the gas and collapse much more quickly. Once in the disk, their radial drift is also faster than in the Std-med model, and they rapidly deplete into the host star. Unlike in the Std-med model, grains originating from different initial radii ranges therefore do not coexist in the embedded disk with dust parcels of different colours.