scholarly journals Galactic kinematics near the sun from open clusters

2007 ◽  
Vol 3 (S248) ◽  
pp. 502-503 ◽  
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.

scholarly journals Galactic rotation measurements based on H2O maser astrometry with VERA

2007 ◽  
Vol 3 (S242) ◽  
pp. 361-365
Author(s):  
Mareki Honma ◽  
Takeshi Bushimata ◽  
Yoon Kyung Choi ◽  
Tomoya Hirota ◽  
Hiroshi Imai ◽  
...  
Keyword(s):  
Rotation Curve ◽  
Rotation Velocity ◽  
Galactic Rotation ◽  
The Sun ◽  
Proper Motions ◽  
Source Distance ◽  
Galactic Rotation Curve

AbstractWe present results of astrometric observations of S269 H2O maser performed with VERA (VLBI Exploration of Radio Astrometry). We have monitored the positions of S269 H2O masers for 1 year and successfully detected its parallax to be 189±8 micro-arcsecond. This corresponds to a source distance of 5.28+0.24−0.22kpc, and is the smallest parallax (and thus the largest distance) that has ever been measured by means of annual parallax. Proper motions of S269 H2O maser were also measured and used to determine the Galactic rotation velocity at the position of S269. Our measurements show that the Galactic rotation velocity at S269 is the same to that at the Sun within 3%, indicating that the Galactic rotation curve is flat out to R~13 kpc.

Galactic rotation curve from the space velocities of selected masers

2011 ◽  
Vol 37 (4) ◽  
pp. 254-266 ◽  
Author(s):  
A. S. Stepanishchev ◽  
V. V. Bobylev
Keyword(s):  
Rotation Curve ◽  
Galactic Rotation ◽  
Galactic Rotation Curve

Accelerated frames and galactic rotation curves

2019 ◽  
Vol 34 (27) ◽  
pp. 1950218
Author(s):  
S. C. Ulhoa ◽  
F. L. Carneiro
Keyword(s):  
Experimental Data ◽  
General Relativity ◽  
Dark Matter ◽  
Reference Frame ◽  
Rotation Curve ◽  
Reference Frames ◽  
Galactic Rotation ◽  
Inertial Reference Frame ◽  
Galactic Rotation Curve ◽  
Accelerated Frames

In this paper, the galactic rotation curve is analyzed as an effect of an accelerated reference frame. Such a rotation curve was the first evidence for the so-called dark matter. We show another possibility for this experimental data: non-inertial reference frame can fit the experimental curve. We also show that general relativity is not enough to completely explain that which encouraged alternatives paths such as the MOND approach. The accelerated reference frames hypothesis is well-suited to deal with the rotation curve of galaxies and perhaps has some role to play concerning other evidences for dark matter.

scholarly journals The Massive Dark Corona Of Our Galaxy

1996 ◽  
Vol 173 ◽  
pp. 175-176
Author(s):  
K.C. Freeman
Keyword(s):  
Rotation Curve ◽  
Spiral Galaxies ◽  
Galactic Center ◽  
Galactic Disk ◽  
Galactic Rotation ◽  
Rotation Curves ◽  
Stellar Component ◽  
The Galaxy ◽  
Galactic Rotation Curve

From their rotation curves, most spiral galaxies appear to have massive dark coronas. The inferred masses of these dark coronas are typically 5 to 10 times the mass of the underlying stellar component. I will review the evidence that our Galaxy also has a dark corona. Our position in the galactic disk makes it difficult to measure the galactic rotation curve beyond about 20 kpc from the galactic center. However it does allow several other indicators of the total galactic mass out to very large distances. It seems clear that the Galaxy does indeed have a massive dark corona. The data indicate that the enclosed mass within radius R increases like M(R) ≈ R(kpc) × 1010M⊙, out to a radius of more than 100 kpc. The total galactic mass is at least 12 × 1011M⊙.

Planetary nebulae and the galactic rotation curve

1983 ◽  
Vol 274 ◽  
pp. L61 ◽  
Author(s):  
S. E. Schneider ◽  
Y. Terzian
Keyword(s):  
Rotation Curve ◽  
Planetary Nebulae ◽  
Galactic Rotation ◽  
Galactic Rotation Curve

scholarly journals The Galactic Rotation Curve to R = 18 Kpc

1980 ◽  
Vol 87 ◽  
pp. 213-220 ◽  
Author(s):  
Leo Blitz ◽  
Michel Fich ◽  
Antony A. Stark
Keyword(s):  
Rotation Curve ◽  
Hii Regions ◽  
Molecular Gas ◽  
Galactic Rotation ◽  
Galactocentric Distance ◽  
The Past ◽  
The Galaxy ◽  
Galactic Rotation Curve ◽  
Sizable Number

The major stumbling block in the determination of a rotation curve beyond the solar circle has been the lack of a suitable set of objects with well defined and independently measured distances and velocities which can be observed to large galactocentric radii. Two things have changed this situation. The first was the realization that essentially all local HII regions have associated molecular material. The second was the acquisition of reliable distances to the stars exciting a sizable number of HII regions at large galactocentric radii (Moffat, FitzGerald, and Jackson 1979). Because the velocity of the associated molecular gas can be measured very accurately by means of radio observations of CO, we have been able to overcome the past difficulties and have measured the rotation curve of the Galaxy to a galactocentric distance of 18 kpc.

scholarly journals Galactic rotation curve and the effect of density waves from data on young objects

2008 ◽  
Vol 34 (8) ◽  
pp. 515-528 ◽  
Author(s):  
V. V. Bobylev ◽  
A. T. Bajkova ◽  
A. S. Stepanishchev
Keyword(s):  
Rotation Curve ◽  
Galactic Rotation ◽  
Density Waves ◽  
Galactic Rotation Curve
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