Profiles in Galactocentric radius r_gc, of the three velocity dispersion components σ_r, σ_θ, and σ_ϕ, and anisotropy parameter β, for three metallicity bins, using our sample of halo K giants after efforts to remove Sagittarius stars as in Figure 5. The top left, top right, and lower left panels show the three dispersion profiles, σ_r, σ_θ, and σ_ϕ, respectively, divided into three metallicity bins. The lower right panel shows the anisotropy profile β. The two more metal-rich bins share a common amplitude of β ≈ 0.9 with r_gc < 25 kpc and gradually declining value of β at larger radii. The anisotropy profile is strikingly different for stars with [Fe/H] < −1.8, where the amplitude of β has dropped to ≈0.6 and remains relatively constant out to large radii; such stars are still on quite radial orbits, but substantially less so than the rest of the sample. This change in the underlying velocities used to form β can also be seen in the left-hand panels of Figure 3. We note that substructure, particularly beyond ≈25 kpc, is still affecting β and the behavior should be regarded with care until careful structure identification and removal is performed.