The ellipticities of Galactic and Large Magellanic Cloud globular clusters

@article{Goodwin1997TheEO,
  title={The ellipticities of Galactic and Large Magellanic Cloud globular clusters},
  author={S. P. Goodwin},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={1997},
  volume={286}
}
  • S. Goodwin
  • Published 3 February 1997
  • Physics
  • Monthly Notices of the Royal Astronomical Society
The globular clusters of the LMC are found to be significantly more elliptical than Galactic globular clusters, but very similar in virtually all other respects. The ellipticity of the LMC globular clusters is shown not be correlated with the age or mass of those clusters. It is proposed that the ellipticity differences are caused by the different strengths of the tidal fields in the LMC and the Galaxy. The strong Galactic tidal field erases initial velocity anisotropies and removes angular… 

Figures and Tables from this paper

THE FLATTENING OF GLOBULAR CLUSTERS
In the three nearest luminous galaxies, the Milky Way System, the Andromeda Galaxy, and NGC 5128, the brightest globular clusters are rounder than the faintest ones. On the other hand (contrary to
Morphological Distortion of Galactic Globular Clusters
The shapes and sizes of 116 Galactic globular clusters (GCs) are presented, based on the analysis of the spatial distribution of 2MASS point sources. In general, Galactic GCs are slightly flattened
Globular clusters and dwarf spheroidal galaxies
Traditionally, globular clusters and dwarf spheroidal galaxies have been distinguished by using one or more of the following criteria: (i) mass, (ii) luminosity, (iii) size, (iv) mass-to-light ratio
The properties of Galactic globular cluster subsystems
In this paper we compare the properties of three subsystems of Galactic globular clusters, which are defined according to metallicity and horizontal branch morphology. We specifically focus on
Distortion of globular clusters by galactic bulges
One of the external fields that influences the population of globular clusters is that resulting from galactic bulges. In extreme situations, at perigalactic distances rp≤ 100 pc, globular clusters
Hubble Space Telescope Observations of the Oldest Star Clusters in the Large Magellanic Cloud
We present V, V-I color-magnitude diagrams (CMDs) for three old star clusters in the Large Magellanic Cloud (LMC): NGC 1466, NGC 2257, and Hodge 11. Our data extend ~3 mag below the main-sequence
Globular clusters in modified Newtonian dynamics: velocity-dispersion profiles from self-consistent models
We test the modified Newtonian dynamics (MOND) theory with the velocity dispersion profiles of Galactic globular clusters populating the outermost region of the Milky Way halo, where the Galactic
The Star Clusters in the Starburst Irregular Galaxy NGC 1569
We examine star clusters in the irregular starburst galaxy NGC 1569 from Hubble Space Telescope images taken with filters F336W, F555W, and F814W. In addition to the two super–star clusters that are
STRUCTURAL PARAMETERS OF SEVEN SMALL MAGELLANIC CLOUD INTERMEDIATE-AGE AND OLD STAR CLUSTERS*
We present structural parameters for the seven intermediate-age and old star clusters NGC 121, Lindsay 1, Kron 3, NGC 339, NGC 416, Lindsay 38, and NGC 419 in the Small Magellanic Cloud (SMC). We fit
An enigmatic population of luminous globular clusters in a galaxy lacking dark matter
We recently found an ultra diffuse galaxy (UDG) with a half-light radius of R_e = 2.2 kpc and little or no dark matter. The total mass of NGC1052-DF2 was measured from the radial velocities of bright
...
1
2
3
...

References

SHOWING 1-4 OF 4 REFERENCES
Structure and dynamics of globular clusters
An internal combustion engine, particularly a four cylinder four stroke cycle engine, has adjoining cylinders arranged in pairs with adjacent or siamesed intake ports and timed sequentially so that
Structure and Dynamics of Globular Clusters. Astron. Soc. Pac
  • Structure and Dynamics of Globular Clusters. Astron. Soc. Pac
  • 1989
ApJ, 317, 246 c 0000 RAS, MNRAS 000
  • ApJ, 317, 246 c 0000 RAS, MNRAS 000
  • 1987
This paper has been typeset from a TEXIL ATEX file prepared by the author
  • This paper has been typeset from a TEXIL ATEX file prepared by the author