(@F07 [@foglizzo09; @guilet2012]). The most unstable modes of the SASI reside on the largest spatial scales. Convection and the SASI are easily distinguishable in the linear regime, but their effects become intertwined in the non-linear turbulent flow that follows the stalling of the bounce supernova shock (e.g., @scheck08).

Recent three-dimensional studies of core-collapse supernova hydrodynamics have found that large-scale oscillation modes of the shock attain smaller amplitudes than in two dimensions [@nordhaus10a; @wongwathanarat2010; @hanke2012; @takiwaki2012; @murphy2012]. This has been interpreted as a consequence of the different behavior of turbulence in two- and three-dimensions [@hanke2012], and has led to the suggestion that the SASI may play a secondary role in the explosion mechanism, if it arises at all [@burrows2012; @burrows2013]. These models have largely focused on a small sample of stellar progenitors, however, and in many cases do not include physical effects that are favorable for the growth of the SASI [@janka2012b].

@mueller2012 followed the collapse and bounce of $8.1$ and $27M_\sun$ progenitors using a two-dimensional, general relativistic hydrodynamic code with energy dependent neutrino transport, finding that differences in progenitor structure lead to very different paths to explosion. In particular, the $27M_\sun$ progenitor evolution is such that the SASI dominates the 