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Fig. 4


Rotation curves (top) and velocity dispersions (bottom) derived by fitting 3D tilted-ring models to Hα data cubes of our galaxy sample with 3DBarolo. Left panels refer to galaxies with log (M/M) < 10.1; right panels to galaxies with log (M/M) > 10.1. Empty data points indicate uncertain measurements in the inner regions of galaxies. For these points, we assumed the derived velocity dispersion as the error for the rotation velocity. Galaxies are numbered as in Fig. 1. Radii are slightly oversampled (about 2 rings per resolution element). Rotation curves are remarkably flat from the first to the last point; velocity dispersion are lower than ~ 40 km s-1.

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