Estimates of the KLF within R ≤ 1 pc of Sgr A*. Upper left: model K_s luminosity function (KLF) based on the star formation history derived by Pfuhl et al. (2011). Upper right: KLFs for stellar populations in certain time windows, using the star formation model by Pfuhl et al. (2011). Lower left: the red line is the model KLF smoothed with a Gaussian kernel to roughly take differential extinction into account. The blue line with error bars is the KLF as determined in Paper I. Lower right: fraction of total flux contributed by stars of different magnitudes, i.e. the KLF multiplied by the flux density of stars in a given bin and divided by the total flux. Please note the different range of the x-axis in this plot, which is chosen to show the decrease of the flux contribution at K_s > 22.