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Fig. 8

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Top: two-component EFF fit to the surface brightness profile of R136 as in Mackey & Gilmore (2003). The data points shown are Mackey and Gilmore’s recalibrated surface brightnesses from McLaughlin & van der Marel (2005). Stars that are farther out than ~5 pc (marked by the dotted line) from the cluster center are more likely to be part of the OB association. Within this radius stars are more likely to belong to the R136 cluster itself. Bottom: normalized histograms showing the velocity distribution of the 32 stars within 5 pc in blue (211 velocities), and the 49 stars between 5 and 10 pc in red (327 velocities).

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