Density distribution of residuals as a function of wavelength for stars with different parameters. Subfigures (a), (b), and (c) are results of stars in bins of the same magnitude range 13 < G₀ < 15 but different stellar colors. Subfigures (b), (d), and (e) show the density distribution of residuals for stars within the same range of color 1.0 < (G_BP − G_RP)₀ < 1.2 but different G₀. Subfigure (f) shows the residuals of stars of the same color-magnitude as subfigures (b) but in different Galactic latitude (|b| < 10°). The black dash lines represent the P₅₀ percentiles distributions, which can be viewed as a robust representation of the patterns of wiggles. From the P₅₀ lines we can see that the wiggles change with (G_BP − G_RP)₀ and G₀ , but the stellar color has a larger impact than the magnitude. Stars of low latitude have a much more diffuse distribution of ∆Flux. The large uncertainties of the extinction map towards the Galactic disc may cause a bad extinction correction of Flux_XP for some stars. Therefore, Flux_XP is more likely to deviate from the fitting result Flux_fitting for stars at lower latitude.