  We have imaged the Sunyaev-Zel'dovich (SZ) effect signals at 140 and 270 GHz
towards ten galaxy clusters with Bolocam and AzTEC/ASTE. We also used Planck
data to constrain the signal at large angular scales, Herschel-SPIRE images to
subtract the brightest galaxies that comprise the cosmic infrared background
(CIB), Chandra imaging to map the electron temperature $T_e$ of the
intra-cluster medium (ICM), and HST imaging to derive models of each galaxy
cluster's mass density. The galaxy clusters gravitationally lens the background
CIB, which produced an on-average reduction in brightness towards the galaxy
clusters' centers after the brightest galaxies were subtracted. We corrected
for this deficit, which was between 5-25% of the 270 GHz SZ effect signal
within $R_{2500}$. Using the SZ effect measurements, along with the X-ray
constraint on $T_e$, we measured each galaxy cluster's average line of sight
(LOS) velocity $v_z$ within $R_{2500}$, with a median per-cluster uncertainty
of +-700 km/s. We found an ensemble-mean <$v_z$> of 430+-210 km/s, and an
intrinsic cluster-to-cluster scatter $\sigma_{int}$ of 470+-340 km/s. We also
obtained maps of $v_z$ over each galaxy cluster's face with an angular
resolution of 70". All four galaxy clusters previously identified as having a
merger oriented along the LOS showed an excess variance in these maps at a
significance of 2-4$\sigma$, indicating an internal $v_z$ rms of $\gtrsim$1000
km/s. None of the six galaxy clusters previously identified as relaxed or plane
of sky mergers showed any such excess variance.
