Fig. 10
Pixel distribution of the stellar velocity dispersion from our continuum fit. a) shows the σ ∗ fitted to CO(2–0) overlayed by a fitted Gaussian. b) shows the same but for the CO(6–3) fit. The fitted velocity dispersions were sorted and binned with a bin size of ten km s-1. The velocities at the Gaussian peaks were used for the black-hole mass estimation.
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