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Investigation of the kinematics of young disk populations

We used both radial-velocity and proper-motion data to perform a rotation-curve solution on a combined sample of about 700 Population-I objects including young open clusters (lg A < 8.1), classical Cepheids, and red supergiants. The distances of all objects are derived on a homogenized scale based on Kholopov’s (1980) ZAMS,MV (B−V )0, PL relation for classical Cepheids by Berdnikov & Efremov (1985), and the absolutemagnitude calibration for red supergiants involving photometric data in Wing’s eight-color narrow-band near-infrared system. We inferred R0 = 7.3 ± 0.3 kpc for the distance of the Sun to the Galactic center and found the following parameters of the solar apex and Galactic rotation curve: U0 = 8.8 ± 0.9 km s−1, V0 = 13.5± 0.9 km s−1,W0 = 11.7± 1.5 km s−1,ω0 = 27.3± 2.0 km s−1 kpc−1, A = 19.5 ± 0.5 km s−1 kpc−1, and (dω/dr)0 = 1.13 ± 0.12 km s−1 kpc−3. 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).