Galaxy Kinematics and Mass Calibration in Massive SZE Selected Galaxy
  Clusters to z=1.3
  The galaxy phase-space distribution in galaxy clusters provides insights into
the formation and evolution of cluster galaxies, and it can also be used to
measure cluster mass profiles. We present a dynamical study based on $\sim$3000
passive, non-emission line cluster galaxies drawn from 110 galaxy clusters. The
galaxy clusters were selected using the Sunyaev-Zel'dovich effect (SZE) in the
2500~deg$^2$ SPT-SZ survey and cover the redshift range $0.2 < z < 1.3$. We
model the clusters using the Jeans equation, while adopting NFW mass profiles
and a broad range of velocity dispersion anisotropy profiles. The data prefer
velocity dispersion anisotropy profiles that are approximately isotropic near
the center and increasingly radial toward the cluster virial radius, and this
is true for all redshifts and masses we study. The pseudo-phase-space density
profile of the passive galaxies is consistent with expectations for dark matter
particles and subhalos from cosmological $N$-body simulations. The dynamical
mass constraints are in good agreement with external mass estimates of the SPT
cluster sample from either weak lensing, velocity dispersions, or X-ray $Y_X$
measurements. However, the dynamical masses are lower (at the 2.2$\sigma$
level) when compared to the mass calibration favored when fitting the SPT
cluster data to a $\Lambda$CDM model with external cosmological priors,
including CMB anisotropy data from Planck. The discrepancy grows with redshift,
where in the highest redshift bin the ratio of dynamical to SPT+Planck masses
is $\eta=0.63^{+0.13}_{-0.08}\pm0.06$ (statistical and systematic),
corresponding to a $2.6\sigma$ discrepancy.
