To date, most of the hydrodynamic calculations that have followed the details of the physics during an iron core collapse (see Bowers, these proceedings, for a review) have been restricted to spherical symmetry and therefore have neglected the role that rotation may play in the hydrodynamics of the collapse (see, however, LeBlanc and Wilson, 1970). If rotation is important, the core will flatten to an oblate spheroidal shape allowing some loss of energy through gravitational radiation; the core could conceivably, dynamically evolve to a toroidal configuration, as has been observed in some models of rotating protostellar clouds (Tohline, 1980b; Boss, 1980b and references cited therein); and it may, through a rotational instability, eventually evolve into a non-axisymmetric structure. It is important to know just how much rotational energy must be present in the pre-collapse core in order for these, or any other significant deviations from spherical symmetry, to become important considerations during a core collapse.