Fig. 10.
Top: number of contaminants brighter than P ∼ 21.1 as a function of the Euclidean distance from the target stars (7.66 ≤ P ≤ 12.66). Maximum values have 95% confidence level. Bottom: cumulative fraction of the differential P magnitude between contaminant and target stars, the former located at up to 10 pixels in distance from the latter.
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