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A New Approach to the Construction of Dynamical Structure of our Galaxy

Published online by Cambridge University Press:  21 October 2010

H. Ueda ,
N. Gouda ,
T. Yano ,
H. Koyama  and
M. Sakagami
H. Ueda
Affiliation:
Faculty of Education and Human Studies, Akita University, Tegata-gakuen, Akita 010-0852, Japan email: ueda@ipc.akita-u.ac.jp
N. Gouda
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan email:naoteru.gouda@nao.ac.jp, yano.t@nao.ac.jp
T. Yano
Affiliation:
National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan email:naoteru.gouda@nao.ac.jp, yano.t@nao.ac.jp
H. Koyama
Affiliation:
Graduate School of Human and Environmental Studies, Kyoto University, Kyoto 606-8501, Japan email: sakagami@grav.mbox.media.kyoto-u.ac.jp
M. Sakagami
Affiliation:
Department of Physics, Waseda University, Shinjuku, Tokyo 169-8555, Japan email: koyama@gravity.phys.waseda.ac.jp
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Information about positions and velocities of stars that will be gained in the era of GAIA is crucial for determining dynamical structure in our Galaxy. The distribution function of all component objects in our Galaxy is fundamental for describing its dynamics. However, only the distribution function of observable stars is obtained from space astrometry observations, and it is therefore necessary to develop theoretical studies of how to construct the distribution function of all matter including dark matter and unobservable stars using astrometric data of observable stars. This procedure falls into three categories.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 202
Copyright
Copyright © International Astronomical Union 2010