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Fig. 9
Input M/L profile obtained from N-body simulations (left) and χ2 for the different Jeans models from Fig. 8 (right) with a best-fit black-hole mass of M• = (2.4 ± 0.4) × 104 M⊙. While the rise in the M/L in the central region is due to stellar remnants, the rise at larger radii originates from low-mass stars.
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