  We carried out IFU optical spectroscopy on three pointings in and near the SQ
shock. We used PMAS on the 3.5m Calar Alto telescope to obtain measures of
emission lines that provide insight into physical properties of the gas. Severe
blending of H\alpha\ and [NII]6548,6583A emission lines in many spaxels
required the assumption of at least two kinematical components in order to
extract fluxes for the individual lines. Main results from our study include:
(a) detection of discrete emission features in the new intruder velocity range
5400-6000km/s showing properties consistent with HII regions, (b) detection of
a low velocity component spanning the range 5800-6300km/s with properties
resembling a solar metallicity shocked gas and (c) detection of a high velocity
component at ~6600km/s with properties consistent with those of a low
metallicity shocked gas. The two shocked components are interpreted as products
of a collision between NGC7318b new intruder and a debris field in its path.
This has given rise to a complex structure of ionized gas where several
components with different kinematical and physical properties coexist although
part of the original ISM associated with NGC7318b is still present and remains
unaltered. Our observations suggest that the low velocity ionized component
might have existed before the new intruder collision and could be associated
with the NW-LV HI component of Williams et al. (2002). The high velocity
ionized component might fill the gap between the HI complexes observed in SQ-A
and NGC7319's tidal filament (NW-HV, Arc-N and Arc-S in Williams et al. 2002).
