Galactic Kinematics Derived From Data in the RAVE5, UCAC4, PPMXL, and Gaia TGAS Catalogs

In many problems of galactic kinematics we need to know the proper motions of faint stars, as well as bright stars, within some well-defined reference frame. Generally speaking, the accuracy required is greater for faint stars on account of their larger distances. Techniques at present used for determining proper motions vary according to apparent magnitude, and it is clearly desirable that all methods should give results which are capable of reduction to a common frame.

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Galactic Kinematics on the Basis of Modern Proper Motion Data

Symposium - International Astronomical Union ◽

10.1017/s0074180900228106 ◽

1995 ◽

Vol 166 ◽

pp. 217-226

Author(s):

M. Miyamoto

Keyword(s):

High Precision ◽

Proper Motion ◽

Galactic Kinematics ◽

Dark Halo ◽

Motion Data ◽

Structure And Dynamics ◽

The Galaxy ◽

Galactic Astronomy ◽

Astrometric Data

An accumulation of high precision astrometric data in conjunction with high-precision monitoring of the Earth's orientation, motivates “Galactic Astronomy”. As regards local kinematics, all of the three components of both the vorticity and the shear of stars can be completely determined, in addition to the velocity ellipsoid. We can now be released from the constraint of the “axisymmetric” galaxy. The determination of the proper motion of the LMC will be crucial to understanding the global structure and dynamics of the Galaxy with the dark halo and MACHO's motions.

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Galactic kinematics with modified Newtonian dynamics

Astronomy and Astrophysics ◽

10.1051/0004-6361/200809978 ◽

2009 ◽

Vol 500 (2) ◽

pp. 801-805 ◽

Cited By ~ 28

Author(s):

O. Bienaymé ◽

B. Famaey ◽

X. Wu ◽

H. S. Zhao ◽

D. Aubert

Keyword(s):

Galactic Kinematics ◽

Modified Newtonian Dynamics ◽

Newtonian Dynamics

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Galactic kinematics near the sun from open clusters

Proceedings of the International Astronomical Union ◽

10.1017/s1743921308019959 ◽

2007 ◽

Vol 3 (S248) ◽

pp. 502-503 ◽

Cited By ~ 1

Author(s):

M. Shen

Keyword(s):

Rotation Curve ◽

Thin Disk ◽

Open Clusters ◽

Galactic Rotation ◽

Galactic Kinematics ◽

The Sun ◽

Galactic Rotation Curve ◽

Kinematical Data ◽

Weak Trend

AbstractA catalogue of open clusters is used to analyze the Galactic kinematics near the Sun. The Galactic open clusters, which are components of Galactic thin disk, were selected for our analysis. Based on kinematical data for around 270 Galactic open clusters, we found the Galactic rotation curve remains flat near the Sun. We also found Ve = 6.40±3.39 km s−1 inside the solar circle, which shows a weak trend of stars moving toward the Galactic anti-center.

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