NISP detector read out noise for the two observing modes. Top: wavelength-dependent QE of the 16 flight SCA, 5-percentile values measured at NASA (95% of pixels have at least this QE). Cen- tre+bottom: noise cumulative distribution of the 16 flight triplet SCS. Black points are the 5, 50, and 95 percentiles of the cumulative distribution. SCS and SCS are identified by their SCA number 18XXX as in Table 3.