Left: reproduction of the m _F322W2 vs. m _F115W − m _F322W2 CMD of Figure 4, where we used black colors to mark the probable MS and brown dwarfs of 47 Tucanae. We superimposed on the CMD the best-fit isochrones for MS stars (Dotter et al. 2008; Milone et al. 2023a) and the isochrone of Phillips et al. (2020) for low-mass stars. The horizontal lines mark the magnitudes corresponding to four stellar masses inferred from the red isochrone and from Gerasimov et al. (2024). Right: F322W2 luminosity function of 47 Tucanae stars along the MS and the brown-dwarf sequence obtained by using 0.4 mag wide bins. The open circles are derived from stars where the correction for the incompleteness of the photometric sample is smaller than 50%. The top panel shows the luminosity functions of stars in detectors A and B of the long-wavelength channel of NIRCam, separately, which have different radial distances ∼ 11.′5 and 14.′5 from the cluster center. The middle panel shows the results from the entire field of view. The gray points in the middle panel are derived by using 0.4 mag wide bins but by changing the starting magnitude value of the luminosity function by 0.1, 0.2, and 0.3 mag with respect to the value used for the black points. The bottom panel shows the MF for stars in the entire field of view. The vertical dotted line corresponds to 0.11 M _⊙. See the text for details.