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Fig. 24


Comparison to the results from Donato et al. (2009). Upper panel: open squares show the stellar velocity dispersion profile (BSG94), filles squares are the blue GCs (BlueFinal). The velocity dispersion profile for the joint isotropic model (blue GCs and stars, S.B.iso, Burkert halo) is shown as dashed line. The solid line shows the dispersion for a Burkert dark matter halo r0 = 20   kpc, ϱ0 = 1.115  ×  10-2 (i.e. log μ0.D = 2.35) which is consistent with the relation by Donato et al. (2009) (see text for details). Lower panel: circular velocity curves. Again, the thin solid line shows the curve for the halo with log 0D = 2.35, and the dashed line is the joint model. For reference, the circular velocity curve for the stars alone (Υ  ,R = 5.8) is shown as long-dashed line. The MOND circular velocity curve (Eq. (19)) is shown as a thick solid line. The dotted vertical line at 40 kpc indicates the location of the outermost velocity dispersion bin for the blue GCs.

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