Recovered FVG host-galaxy fluxes (gal) for various S/N and time sampling. The distributions obtained for the CS are shown with the same colors as the light curves in Fig. 2. To facilitate comparison, we show in black the distributions obtained for the HS. The FVG applied to the CS appears to be considerably better than the HS; it is characterized by the smallest dispersion around the true galaxy (gal₀; vertical dotted black line) for an S/N > 100 (see text).