Rotational velocity model adopted for NGC 1566 (black open rectangles), based on the CO data points (blue triangles), and minimizing the residuals of Fig. 8. The Hα kinematic model from Agüero et al. (2004) is also shown in red circles. Those data were obtained with 2.̋8-wide slits, with insufficient spatial resolution to resolve the central peak. The Hα velocity model rises linearly because of the deficiency of HII regions inside a radius of 22′′ (see text).