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Fig. 9

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Red: star cluster mass – rh relation from Gieles et al. (2010), normalised to have rh = 3 pc at a mass of . Green: present-day mass-radius relation (e.g. Mieske et al. 2006; Gieles et al. 2010): star clusters have a mass-independent half-light radius for masses below , and a mass-radius relation above that mass. Blue: primordial mass-radius relation (constant radius) adopted by Bailin & Harris (2009) for star clusters at time of self-enrichment. Magenta: primordial mass-radius relation adopted by renormalising the red (Gieles) curve to a mean of rh = 1 pc in the observed GC mass range [5 × 105: 4 × 106]. We note that the x-axis is the present-day mass, which is converted to original mass according to Eq. (7).

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