Top: three-color (RGB) image of a portion of the studied field of view (field C). We used the stacked F115W and F322W2 images for the B and R channels, respectively, whereas the G channel is obtained by averaging the F115W and F322W2 stacked images (left). The right panels show the F322W2 (top) and F115W (bottom) stacked images for the region within the yellow box highlighted in the field of view on the left panel. Bottom: m _F322W2 vs. m _F115W − m _F322W2 CMD of stars in field C (left). The arrows indicate the location of the possible gaps or discontinuities along the sequence of ultracool 47 Tucanae stars. Stars fainter than m _F322W2 ∼ 25.3 mag and with colors redder than m _F115W − m _F322W2 ∼ 1.5 mag are probable brown dwarfs. The blue and red circles in the CMD highlight two of them, which are also marked in the top-right panel. We choose these two stars, among the brown-dwarf sample, for illustrative purposes, as they are located in a relatively small region of the field of view. A zoom around the MS region of 47 Tucanae populated by M dwarfs is shown in the right panel.