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Fig. 2


Spatial density of different stellar components at the end ofour simulations. From top to bottom, we show the density distribution of black holes and neutron stars (green), giant stars with apparent magnitudes KS < 18.5 (red), upper main-sequence stars with masses 0.6 and 0.8 M (blue), and low-mass main-sequence stars with masses 0.1 and 0.3 M (orange). For clarity, curves are shifted vertically. Dashed lines show power-law density distributions ρ (r) ~ rγ fitted to the density distribution inside the influence radius of the black hole (rBH = 2.8 pc). Because of mass segregation, the slope steepens from γ = 1.04 for the lowest-mass main-sequence stars to γ = 1.55 for black holes.

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