Abstract
Abstract We performed a rotation-curve solution on an extensive sample consisting of 770 Population-I objects with well-established, homogeneous, and consistent distance scales. The sample under study includes 202 young open clusters (log A < 8.1), 440 classical Cepheids, and 128 red su-pergiants with distances derived on a homogenized scale based on Kholopov's (1980) ZAMS, Mv(B - V)o, multicolour PL relation for classical Cepheids by Berdnikov et al. (1996a), and the absolute-magnitude calibration for red supergiants by Dambis (1993), which uses photometric data in Wing's eight-colour narrow-band near-infrared system. We inferred R 0 = 7.4 ± 0.3 kpc for the distance of the Sun to the Galactic centre and found the following parameters of the solar apex and Galactic rotation curve: U 0 = 10.2 ± 1.0 km s−l, V 0 = 14.1 ± 0.9 km s−l, W0 = 8.2 ± 1.0 km s−', ω0 = 27.5 ± 2.0 km 8−1 kpc−1, A = 18.7 ± 0.4 km s−1 kpc−1, and (d2ω/dr2)o = 0.96 ± 0.10 km s−1 kpc−1. These values are in good agreement with the results of our analysis of the radial-velocity and proper-motion fields of classical Cepheids (Dambis et al., 1995) and with most recent determinations of the distance from the Sun to the Galactic centre.
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