To compare the angular momentum of the arm and inter-arm populations, we plotted luminous mass as a function of velocity gradient, $\nabla v$, in Fig.~\ref{vgrad}, where $\nabla v$ is generally a signature of both turbulence and large scale shearing motions within the galaxy. Note that we ignored clouds with balanced emissions and thus negligible velocity gradients. The geometric means, $\overline{\nabla v}$, and standard errors, $SE({\nabla v})$, of $\nabla v$ in Table \ref{means}, show that $\overline{\nabla v}$ is highest in the nuclear population. Even though $\overline{\nabla v}$ is slightly higher in the spiral arms than in the inter-arm region, it is not statistically significant, and thus we conclude that the velocity gradient is due to turbulent motion rather than shear. This is supported by the fairly tight correlation between $\sigma_0$ and $\nabla v$ in Fig.~\ref{sig_velgrad}. 