  3C 84 (NGC 1275) is the bright radio core of the Perseus Cluster. Even in the
absence of strong relativistic effects, the source has been detected at
Gamma-rays up to TeV energies. Despite its intensive study, the physical
processes responsible for the high-energy emission in the source remain
unanswered. We present a detailed kinematics study of the source and its
connection to Gamma-ray emission. The sub-parsec scale radio structure is
dominated by slow-moving features in both the eastern and western lanes of the
jet. The jet appears to have accelerated to its maximum speed within less than
125 000 gravitational radii. The fastest reliably detected speed in the jet was
~0.9 c. This leads to a minimum Lorentz factor of ~1.35. Our analysis suggests
the presence of multiple high-energy sites in the source. If Gamma-rays are
associated with kinematic changes in the jet, they are being produced in both
eastern and western lanes in the jet. Three Gamma-ray flares are
contemporaneous with epochs where the slowly moving emission region splits into
two sub-regions. We estimate the significance of these events being associated
as ~2-3 sigma. We tested our results against theoretical predictions for
magnetic reconnection-induced mini-jets and turbulence and find them
compatible.
