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Fig. 6


Black points: distribution in areas and magnitudes for the negative clumps detected applying the same method on the inverted galaxy image. The contours depict the 68%, 90%, and 95% levels of the positive clump detections in our data. Most of the negative detections are found at Mclump > −18 which is fainter than the peak for the fainter clumps that is observed in the magnitude distribution (see Fig. 10). This indicates that the smaller clumps with Mclump < −18 are mostly real physical clumps.

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