A study of rotating globular clusters: The case of the old, metal-poor globular cluster NGC 4372

NGC 4372 is a poorly studied old, very metal-poor globular cluster (GC) located in the inner Milky Way halo. We present the first in-depth study of the kinematic properties and derive the structural parameters of NGC 4372 based on the fit of a Plummer profile and a rotating, physical model. We explore the link between internal rotation to different cluster properties and together with similar studies of more GCs, we put these in the context of globular cluster formation and evolution. Our results show that NGC 4372 has an unusually high ratio of rotation amplitude to velocity dispersion (1.2 vs. 4.5 km s[sup -1]) for its metallicity.