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Fig. 1


Line-of-sight velocity dispersion for clusters listed in Table 1 for various masses as found by N-MODY. In order to compare with the real cluster, the half-mass radii of all models are fixed. For low masses, which mean low internal accelerations, the prediction of Newtonian dynamics differs from the numerical solution. As the mass increases (at about 106 M), the internal acceleration grows and the system enters the Newtonian regime and the numerical solutions get close to the Newtonian prediction. In order to focus on a reasonable range of mass for these clusters, we show the results in the range of 500−2 × 105. Dashed vertical lines show the expected cluster mass, calculated from the absolute luminosity by assuming a stellar mass-to-light ratio of M/LV = 2. This value agrees with observed mass-to-light ratios of galactic GCs (Mieske et al. 2008).

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