  Stephan's Quintet (SQ) is a nearby compact galaxy group and a perfect
laboratory for studying the process of galaxy evolution through galaxy
harassment and interaction. By analysing the kinematics of SQ we aim to provide
an increased understanding of the group, the history of the interactions, their
cause and effect, and the details regarding the physical processes occurring as
galaxies interact. We have studied the ionised gas and stellar kinematics using
the Large Binocular Telescope, and the molecular gas kinematics via CO using
the IRAM 30m. Large areas of the group have been mapped and analysed. We obtain
a total ionised gas mass in the regions chosen for closer analysis of
20.1$\pm$0.2x10^10 Msun and a total H2 gas mass of 21$\pm$2x10^9 Msun in the
observed area (spectra integrated over the velocity range of SQ), while the
star-forming (SF) clouds show an impressive complexity, with gas congregations
at multiple velocities throughout the group. We map the large-scale nuclear
wind in NGC7319 and its decoupled gas and stellar disk. With our high
resolution data we can, for the first time, reveal the Seyfert 1 nature of
NGC7319 and fit the narrow-line and broad-line regions. While the 12CO(1-0) map
shows significant emission in the area of NGC7319, the bridge, and the SF
ridge, the 12CO(2-1) emission shows a prevalence to the SF ridge, an area south
of the NGC7318 pair, and an extension towards NGC7317 - connecting NGC7317 to
the centre of the group, indicating a previous interaction. NGC7317 may also be
a prime candidate for studies of the process of galaxy harassment. Furthermore,
we connect the kinematical structures in SQ to the history of the group and the
ongoing interaction with NGC7318B. Through our extensive observations of SQ we
trace the kinematics and evolution of the complex processes and structures
occurring in this nearby interactive group. [Abstract abridged]
