  Extending the earlier measurements reported in Hitomi collaboration (2016,
Nature, 535, 117), we examine the atmospheric gas motions within the central
100~kpc of the Perseus cluster using observations obtained with the Hitomi
satellite. After correcting for the point spread function of the telescope and
using optically thin emission lines, we find that the line-of-sight velocity
dispersion of the hot gas is remarkably low and mostly uniform. The velocity
dispersion reaches maxima of approximately 200~km~s$^{-1}$ toward the central
active galactic nucleus (AGN) and toward the AGN inflated north-western `ghost'
bubble. Elsewhere within the observed region, the velocity dispersion appears
constant around 100~km~s$^{-1}$. We also detect a velocity gradient with a
100~km~s$^{-1}$ amplitude across the cluster core, consistent with large-scale
sloshing of the core gas. If the observed gas motions are isotropic, the
kinetic pressure support is less than 10\% of the thermal pressure support in
the cluster core. The well-resolved optically thin emission lines have Gaussian
shapes, indicating that the turbulent driving scale is likely below 100~kpc,
which is consistent with the size of the AGN jet inflated bubbles. We also
report the first measurement of the ion temperature in the intracluster medium,
which we find to be consistent with the electron temperature. In addition, we
present a new measurement of the redshift to the brightest cluster galaxy
NGC~1275.
