BACKGROUND GIANTS IN THE FIELD OF THE GLOBULAR-CLUSTER M22 - KINEMATICS OF THE GALACTIC BULGE

We report radial velocities, metallicities, and near-IR photometry for about 100 giants in the field of the globular cluster M22, at l,b=(9. 9 degrees,-7.6 degrees). Most of them are bulge giants, non-members of the cluster from proper motions. Dividing the sample according to met allicity, we find that the giants more metal-poor than [Fe/H]approxima te to-1 have halo-like kinematics, while the more metal-rich giants ha ve higher rotation and smaller velocity dispersion, which we identify with the bulge. Such dependences of kinematics on metal abundance (whi ch may be due to a mix of populations) are predicted by dissipational collapse models of formation for the inner Galaxy. The 11 M giants in the field follow bulge rather than halo kinematics. (C) 1996 American Astronomical Society.