Results from the ongoing Bulge Radial Velocity Assay ( BRAVA ) are presented . BRAVA uses M red giant stars , selected from the 2MASS catalog to lie within a bound of reddening corrected color and luminosity , as targets for the Cerro Tololo Inter-American Observatory 4-m Hydra multi-object spectrograph . Three years of observations investigate the kinematics of the Galactic bulge major ( - 10 ^ { \circ } < l < + 10 ^ { \circ } , b = - 4 ^ { \circ } ) and minor ( - 6 ^ { \circ } < b < + 5 ^ { \circ } , - 0.4 ^ { \circ } < l < - 0 ^ { \circ } ) axes with \sim 3300 radial velocities from 32 bulge fields and one disk field . We construct a longitude-velocity plot for the bulge stars and find that , contrary to previous studies , the bulge does not rotate as a solid body ; from - 4 ^ { \circ } < l < + 4 ^ { \circ } the rotation curve has a slope of roughly 100 km s ^ { -1 } kpc ^ { -1 } and flattens considerably at greater l , reaching a maximum rotation of 75 km s ^ { -1 } . We compare our rotation curve and velocity dispersion profile to both the self-consistent model of Zhao ( 1996 ) and to N-body models ; neither fits both our observed rotation curve and velocity dispersion profile . We place the bulge on the plot of ( V _ { max } / \sigma ) vs . \epsilon and find that the bulge lies near the oblate rotator line , and very close to the parameters of NGC 4565 , an edge-on spiral galaxy with a bulge similar to that of the Milky Way . We find that our summed velocity distribution of bulge stars appears to be sampled from a Gaussian distribution , with \sigma = 116 \pm 2 km s ^ { -1 } for our summed bulge fields . Furthermore , the high precision of our radial velocities ( \sim 5 km s ^ { -1 } ) allows us to investigate hints of cold kinematic features that were seen in a number of the line-of-sight velocity distributions from our earlier observations . In the past , optical radial velocity studies in the bulge have not emphasized high precision , because of the large velocity dispersion and the expectation that the short orbital periods would erase any cold structures in well under a gigayear . Thus our precision is sufficient to enable a search for more cold streams analogous to those associated with the Sagittarius dwarf spheroidal galaxy ; some candidate cold features were seen and follow-up observations are reported herein .