Extended rotation curves of high-luminosity spiral galaxies. I - The angle between the rotation axis of the nucleus and the outer disk of NGC 3672

1977 ◽  
Vol 217 ◽  
pp. L1 ◽  
Author(s):  
V. C. Rubin ◽  
N. Thonnard ◽  
W. K., Jr. Ford
Keyword(s):  
Spiral Galaxies ◽  
Rotation Axis ◽  
High Luminosity ◽  
Rotation Curves ◽  
Outer Disk

Extended rotation curves of high-luminosity spiral galaxies. III - The spiral galaxy NGC 7217

1978 ◽  
Vol 226 ◽  
pp. 770 ◽  
Author(s):  
C. J. Peterson ◽  
M. S. Roberts ◽  
V. C. Rubin ◽  
W. K., Jr. Ford
Keyword(s):  
Spiral Galaxy ◽  
Spiral Galaxies ◽  
High Luminosity ◽  
Rotation Curves

Extended rotation curves of high-luminosity spiral galaxies. II - The anemic SA galaxy NGC 4378

1978 ◽  
Vol 224 ◽  
pp. 782 ◽  
Author(s):  
V. C. Rubin ◽  
W. K., Jr. Ford ◽  
K. M. Strom ◽  
S. E. Strom ◽  
W. Romanishin
Keyword(s):  
Spiral Galaxies ◽  
High Luminosity ◽  
Rotation Curves

scholarly journals Rotation curves of high-luminosity spiral galaxies and the rotation curve of our galaxy

1979 ◽  
Vol 84 ◽  
pp. 211-220 ◽  
Author(s):  
Vera C. Rubin
Keyword(s):  
Rotation Curve ◽  
Spiral Galaxies ◽  
Rotational Velocity ◽  
Density Wave ◽  
Wave Theory ◽  
High Luminosity ◽  
Rotation Curves ◽  
Flat Rotation Curve ◽  
Density Wave Theory ◽  
Spiral Arm

Rotation curves of high luminosity spiral galaxies are flat, to distances as great as r=49 kpc. This implies a significant mass at large r. Rotational velocities increase about 20 km/s across a spiral arm, as predicted by the density wave theory. By analogy, it is suggested that our Galaxy has a flat rotation curve out to r∼60 kpc, with V ∼ constant at near the solar rotational velocity, and m ∼7×1011 m⊙. Values of A and B imply that the sun is not located in a spiral arm.

Density waves in the outer disk of spiral galaxies

2010 ◽  
Author(s):  
G. Bertin ◽  
N. C. Amorisco ◽  
Giuseppe Bertin ◽  
Franca De Luca ◽  
Giuseppe Lodato ◽  
...  
Keyword(s):  
Spiral Galaxies ◽  
Density Waves ◽  
Outer Disk

scholarly journals Kinematics of Nuclei of Sc Galaxies

1980 ◽  
Vol 5 ◽  
pp. 191-191
Author(s):  
V. C. Rubin
Keyword(s):  
High Velocity ◽  
Stellar Population ◽  
Hii Regions ◽  
Emission Lines ◽  
High Luminosity ◽  
Rotation Curves ◽  
Velocity Gradients ◽  
Wide Range ◽  
Central Regions ◽  
Velocity Dispersions

For a sample of 21 Sc galaxies with a wide range of luminosities, of radii, and of masses, W. K. Ford and I have obtained spectra and determined rotation curves. By their kinematical behavior in their central regions, the Sc’s can be separated into two groups. Some galaxies, generally small and of low luminosity, have shallow central velocity gradients, reflecting their low central masses and densities. Other galaxies, most often large ones of high luminosity, have steep central velocity gradients. One reason this separation by central velocity gradients is of interest is because these galaxies exhibit other significant spectral differences which go hand-in-hand with the kinematical differences.The small, low luminosity galaxies show emission lines of Hα and [NII], with nuclear Ha sharp and stronger than [NII], and little or no stellar nuclear continuum, just as conventional HII regions. In contrast, the high luminosity galaxies show broad nuclear emission, with [NII] stronger than Ha. These galaxies have a strong red stellar continuum, arising from a red stellar population. The cause of the Hα[NII] intensity reversal in the nuclei of some galaxies remains unknown. However, the strong [NII] emission in generally high luminosity galaxies with massive nuclei, nuclei which show strong red continua, suggests that [Nil] intensity correlates with nuclear luminosity, and in turn with the density and velocity properties of the nuclear populations. We would expect high velocity dispersions and high bulge luminosities for galaxies with strong nuclear [NII] and steep central velocity gradients.

Sign in / Sign up

Export Citation Format

Share Document