Heather L. Morrison

The Bulge / Halo Interface Rotational Kinematics from [Fe/H] = -3.0 to Solar

Kinematics and abundances have been determined for a large sample of K giants in a field at ∼2 kpc from the center to study the relationship between the bulge and the halo. There are two different kinematic groups evident. The metal-poor stars have low rotation and high velocity dispersion, and so can be associated with the halo. The metal-richer stars have intermediate rotation. Our data suggest that the bulge and halo could be separate kinematical entities.

Comparing M and K Giants in the Bulge

Kinematics and abundances of samples of K and M giants in a field at the edge of the bulge are compared. Despite a higher mean abundance, the M giants have the same kinematics as the metal-richer K giants.