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2012MNRAS.427..274S - Mon. Not. R. Astron. Soc., 427, 274-287 (2012/November-3)
Galactic rotation and solar motion from stellar kinematics.
SCHONRICH R.
Abstract (from CDS):
The first approach compares this with rotation from the Galactic azimuthal velocities to constrain V_g, ☉_ at an assumed R0. Both V_g, ☉_and R0 can be determined using the proper motion of Sgr A* as a second constraint. The second strategy makes use of θ being roughly proportional to R0. Therefore a wrong R0 can be detected by an unphysical trend of V_g, ☉_ with the intrinsic rotation of different populations. From these two strategies I estimate R0= (8.27±0.29)kpc and V_g, ☉_= (250±9)km/s for a stellar sample from Sloan Extension for Galactic Understanding and Exploration, or, respectively, Vc = (238±9)km/s. The result is consistent with the third estimator, where I use the angle of the mean motion of stars, which should follow the geometry of the Galactic disc. This method also gives the solar radial motion with high accuracy.
The rotation effect on U velocities must not be neglected when measuring the solar radial velocity U☉. It biases U☉ in any extended sample that is lop-sided in position angle α by of the order of 10km/s. Combining different methods I find U☉ ∼ 14km/s, moderately higher than previous results from the Geneva–Copenhagen Survey.
Abstract Copyright: © 2012 The Author Monthly Notices of the Royal Astronomical Society © 2012 RAS
Journal keyword(s): stars: kinematics and dynamics - Galaxy: disc - Galaxy: fundamental parameters - Galaxy: halo - Galaxy: kinematics and dynamics - solar neighbourhood
Simbad objects: 5
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