Images obtained at 1.87μm (F187N; first column) and 4.80μm (F480M; middle and right columns) before (top row) and after (bottom row) subtraction of point-source models at the location of protoplanets c (first and last column) and b (middle column) using fluxes different than the optimal ones found with NEGFC. We test whether the predicted flux for planet c with the DRIFT-PHOENIX model presented in Wang et al. (2021b) could account for the observed flux in the F187N (panels a vs. d) and F480M (panels c vs. f) images at the location of c. We also show the F480M image obtained after subtracting the lower uncertainty limit from the optimal flux found by NEGFC for planet b (panels b vs. e), which illustrates our uncertainty associated with the underlying inner-disk signal contribution.