  Collisionless shocks vary drastically from terrestrial to astrophysical
regimes resulting in radically different characteristics. This poses two
complexities. Firstly, separating the influences of these parameters on
physical mechanisms such as energy dissipation. Secondly, correlating
observations of shock waves over a wide range of each parameter, enough to span
across different regimes. Investigating the latter has been restricted since
the majority of studies on shocks at exotic regimes (such as supernova
remnants) have been achieved either remotely or via simulations, but rarely by
means of in-situ observations. Here we present the parameter space of MA bow
shock crossings from 2004-2014 as observed by the Cassini spacecraft. We find
that Saturn's bow shock exhibits characteristics akin to both terrestrial and
astrophysical regimes (MA of order 100), which is principally controlled by the
upstream magnetic field strength. Moreover, we determined the {\theta}Bn of
each crossing to show that Saturn's (dayside) bow shock is predominantly
quasi-perpendicular by virtue of the Parker spiral at 10 AU. Our results
suggest a strong dependence on MA in controlling the onset of physical
mechanisms in collisionless shocks, particularly non-time stationarity and
variability. We anticipate our comprehensive assessment will yield deeper
insight into high MA collisionless shocks and provide a broader scope for
understanding the structures and mechanisms of collisionless shocks.
