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Fig. 2
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Radial density profile of the population of stars ejected from the GC in the McMillan (2017) potential. The red line shows the best fit power law in the range [1, 100] kpc, ρ ∝ r−3.41±0.01. For reference, we show the halo profile found in Amarante et al. (2024), which we scaled to our data at the solar circle.
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