Were the LMC Globular Clusters Formed in a Disk?
Astrophysics
2009-11-10 v1
Abstract
The radial velocities of the 13 globular clusters in the Large Magellanic Cloud have a dispersion of 28 km s relative to the HI rotation curve of the LMC, compared to a dispersion of 30 km s with regard to the mean globular cluster velocity. This shows that, contrary to a suggestion by Schommer et al. (1992), one cannot yet rule out the possibility that the LMC globular clusters formed in a pressure supported halo, rather than in rotating disk. The globular clusters in the LMC may therefore, after all, exhibit a relationship between age and kinematics that is similar to that of the clusters in M33.
Keywords
Cite
@article{arxiv.astro-ph/0311322,
title = {Were the LMC Globular Clusters Formed in a Disk?},
author = {Sidney van den Bergh},
journal= {arXiv preprint arXiv:astro-ph/0311322},
year = {2009}
}
Comments
6 pages, 1 figure, Publication in the February 2004 issue of the Astronomical Journal