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Fig. 1

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Mass distribution of fragments for the nominal cluster. The line corresponds to N(> m) ∝ m−0.85, i.e., D = 2.55, and it is the fit for fragment masses above 0.002 g. We assume that below this mass, the numbers of observed fragments may not be complete. This is because the corresponding meteors are fainter and may not have been be recorded.

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