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 can not 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 .