The High Resolution Echelle Spectrometer ( HIRES ) on the Keck I telescope has been used to measure the first radial velocities for stars belonging to eleven , heavily-reddened globular clusters in the direction of the inner Galaxy .
The sample consists of the clusters Terzan 3 , NGC 6256 , IC 1257 , NGC 6380 ( = Ton 1 ) , Ton 2 ( = Pismis 26 ) , Djorg 1 , NGC 6540 ( = Djorg 3 ) , IC 1276 ( = Pal 7 ) , Terzan 12 , NGC 6749 and Pal 10 .
Candidate cluster members were selected from a combination of previously published color-magnitude diagrams ( CMDs ) and new instrumental CMDs obtained with the Palomar 1.5m telescope .
The systemic velocities of Djorg 1 and Pal 10 should be considered provisional since velocities are available for only two stars .
For the remaining nine clusters , we have measured radial velocities for three to nine member stars .
Using our HIRES spectra , we estimate metallicities of [ Fe/H ] \simeq -0.75 for both Terzan 3 and IC 1276 : two cluster lacking previous metallicity estimates .
The question of kinematic substructuring among the Galactic globular cluster system is investigated using an updated catalog of globular cluster distances , metallicities and velocities .
It is found that the population of metal-rich globular clusters shows significant rotation at all Galactocentric radii .
For the metal-rich clusters within 4 kpc of the Galactic center , the measured rotation velocity and line-of-sight velocity dispersion are similar to those of bulge field stars .
We investigate claims that the metal-rich clusters are associated with the central Galactic bar by comparing the kinematics of the innermost clusters to that of the atomic hydrogen in the inner Galaxy .
The longitude-velocity diagram of both metal-rich and metal-poor clusters bears a remarkable similarity to that of the gas , including the same non-circular motions which have traditionally been interpreted as evidence for a Galactic bar , or , alternatively , a non-axisymmetric bulge .
However , uncertainties in the existing three-dimensional Galactocentric positions for most of the clusters do not yet allow an unambiguous discrimination between the competing scenarios of membership in a rigidly rotating bar , or in a bulge which is an oblate isotropic rotator .
We conclude that the majority of metal-rich clusters within the central \sim 4 kpc of the Galaxy are probably associated with the bulge/bar , and not the thick disk .