  The explosion outcome and diagnostics of core-collapse supernovae depend
sensitively on the nature of the stellar progenitor, but most studies to date
have focused exclusively on one-dimensional, spherically-symmetric massive star
progenitors. We present some of the first core-collapse supernovae simulations
of three-dimensional massive star supernovae progenitors, a 12.5- and a
15-M$_{\odot}$ model, evolved in three-dimensions from collapse to bounce
through explosion with the radiation-hydrodynamic code F{\sc{ornax}}. We
compare the results using those starting from three-dimensional progenitors to
three-dimensional simulations of spherically-symmetric, one-dimensional
progenitors of the same mass. We find that the models evolved in three
dimensions during the final stages of massive star evolution are more prone to
explosion. The turbulence arising in these multi-dimensional initial models
serve as seed turbulence that promotes shock revival. Detection of
gravitational waves and neutrinos signals could reveal signatures of pre-bounce
turbulence.
