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Galactocentric distance of the Sun derived from kinematic data

Published online by Cambridge University Press:  26 February 2013

Zi Zhu  and
Ming Shen
Zi Zhu
Affiliation:
School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China email: zhuzi@nju.edu.cn Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing 210093, China
Ming Shen
Affiliation:
National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China email: shenming@nao.edu.cn
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Abstract

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Based on radial velocity data and Hipparcos proper motions, we present a new determination of the Galactocentric distance based on a purely kinematic model. We have selected three subgroups of Galactic thin-disk components (O–B5 stars, classical Cepheids and Galactic open clusters) to trace the local structure and kinematics of the Galactic disk. Adopting the approximation of axisymmetric circular rotation, we have derived the Sun's distance to the Galactic Center, R0 = 8.25 ± 0.79 kpc based on O–B5 stars, R0 = 7.98 ± 0.79 kpc based on Galactic Cepheids and R0 = 8.03 ± 0.70 kpc using open clusters, all of which are in excellent agreement with the current-best estimate of the Galactocentric distance.

Keywords

Galaxy: diskGalaxy: fundamental parametersGalaxy: kinematics and dynamicssolar neighborhood
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S289: Advancing the Physics of Cosmic Distances , August 2012 , pp. 444 - 447
Copyright
Copyright © International Astronomical Union 2013

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