  We examine the dynamics structure of the rich cluster A1689, combining
VLT/VIMOS spectroscopy with Subaru/Suprime-Cam imaging. The radial velocity
distribution of $\sim 500$ cluster members is bounded by a pair of clearly
defined velocity caustics, with a maximum amplitude of $\sim|4000|$ km/s at
$\simeq$ 300 h$^{-1}$ kpc, beyond which the amplitude steadily declines,
approaching zero velocity at a limiting radius of $\sim$ 2 h$^{-1}$ Mpc. We
derive the 3D velocity anisotropy and galaxy number density profiles using a
model-independent method to solve the Jeans equation, simultaneously
incorporating the observed velocity dispersion profile, the galaxy counts from
deep Subaru imaging, and our previously derived cluster mass profile from a
joint lensing and X-ray analysis. The velocity anisotropy is found to be
predominantly radial at large radius, becoming increasingly tangential towards
the center, in accord with expectations. We also analyze the galaxy data
independently of our previous analysis using two different methods: The first
is based on a solution of the Jeans equation assuming an NFW form for the mass
distribution, whereas in the second method the caustic amplitude is used to
determine the escape velocity. The cluster virial mass derived by both of these
dynamical methods is in good agreement with results from our earlier lensing
and X-ray analysis. We also confirm the high NFW concentration parameter, with
results from both methods combined to yield $c_{\rm vir}>13$ (1$\sigma$). The
inferred virial radius is consistent with the limiting radius where the
caustics approach zero velocity and where the counts of cluster members drop
off, suggesting that infall onto A1689 is currently not significant.
