KINEMATICS OF STAR-CLUSTERS IN M33

We present velocities for approximately 45 M33 star clusters, spanning the range of cluster ages (approximately 0.1-10 Gyr) in that system. We conclude that: (1) there is a kinematic halo of old clusters, with a velocity dispersion of approximately 70 km/s; (2) there is little or no sign of rotation for the old, metal poor cluster system (V / sigma greater-than-or-less-than-to 0.6); (3) young (blue) clusters rotate sensibly with the H I and H II disk gas (V / sigma greater-than-or-equal-to 5); (4) the intermediate age/color clusters have similar rotational motion to the young clusters, with a marginally lower rotational velocity and higher dispersion. Although the properties of these clusters resemble those of the LMC clusters in terms of star formation history, the kinematics of the M33 clusters appear significantly different from what has been reported for the LMC cluster system, and more closely mimic the kinematics of the Milky Way system. We briefly discuss these results in terms of disk heating and diffusion arguments versus collapse or formation scenarios.