Investigation of the kinematics of young disk populations

Details Investigation of the kinematics of young disk populations Investigation of the kinematics of young disk populations

Jan 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998a%26a...329..514g&link_type=abstract

Astronomy and Astrophysics, v.329, p.514-521 (1998)

Astronomy and Astrophysics

Astrophysics

31

Galaxy: Kinematics And Dynamics, Open Clusters And Associations, Cepheids, Supergiants, Galaxy: Structure, Galaxy: Fundamental Parameters

Scientific paper

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, M_V (B-V)_0, PL relation for classical Cepheids by Berdnikov & Efremov (1985), and the absolute-magnitude calibration for red supergiants involving photometric data in Wing's eight-color narrow-band near-infrared system. We inferred R_0 = 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: U_0 = 8.8 +/- 0.9 km s(-1) , V_0 = 13.5 +/- 0.9 km s(-1) , W_0 = 11.7 +/- 1.5 km s(-1) , omega_0 = 27.3 +/- 2.0 km s(-1) kpc(-1) , A = 19.5 +/- 0.5 km s(-1) kpc(-1) , and (d(2) omega /dr(2)_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).

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