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Fig. 4


MBHσ relation for the galaxies of the sample, using the FWHM of [SII] (left), [NII] (middle), and the narrow component NC of Hα (right). All FWHM are in km s-1 and were corrected by the instrumental width. The solid line represents the relation given by Tremaine et al. using FWHM = 2.35σ. Typical error bars are on each plot.

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