Were the LMC Globular Clusters Formed in a Disk?

Abstract

The radial velocities of the 13 globular clusters in the Large Magellanic Cloud have a dispersion of 28 km s${}^{-1}$ relative to the HI rotation curve of the LMC, compared to a dispersion of 30 km s${}^{-1}$ 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.

6 pages, 1 figure, Publication in the February 2004 issue of the Astronomical Journal

References in corpus (1)

• Kinematic Evidence for an Old Stellar Halo in the Large Magellanic Cloud

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• The Distance of the First Overtone RR Lyrae Variables in the MACHO LMC Database: A New Method to Correct for the Effects of Crowding
• On the Origin of the Kinematical Differences Between the Stellar Halo and the Old Globular Cluster System in the Large Magellanic Cloud
• Chirping compact stars: gravitational radiation and detection degeneracy with binary systems A conceptual pathfinder for space-based gravitational-wave observatories