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We have conducted nineteen state-of-the-art 3D core-collapse supernovasimulations spanning a broad range of progenitor masses. This is the largestcollection of sophisticated 3D supernova simulations ever performed. We havefound that while the majority of these models explode, not all do, and thateven models in the middle of the available progenitor mass range may be lessexplodable. This does not mean that those models for which we did not witnessexplosion would not explode in Nature, but that they are less prone toexplosion than others. One consequence is that the "compactness" measure is nota metric for explodability. We find that lower-mass massive star progenitorslikely experience lower-energy explosions, while the higher-mass massive starslikely experience higher-energy explosions. Moreover, most 3D explosions have adominant dipole morphology, have a pinched, wasp-waist structure, andexperience simultaneous accretion and explosion. We reproduce the general rangeof residual neutron-star masses inferred for the galactic neutron-starpopulation. The most massive progenitor models, however, in particular vis \`avis explosion energy, need to be continued for longer physical times toasymptote to their final states. We find that while the majority of the innerejecta have Y$_e = 0.5$, there is a substantial proton-rich tail. This resulthas important implications for the nucleosynthetic yields as a function ofprogenitor. Finally, we find that the non-exploding models eventually evolveinto compact inner configurations that experience a quasi-periodic spiral SASImode. We otherwise see little evidence of the SASI in the exploding models.

The Overarching Framework of Core-Collapse Supernova Explosions as Revealed by 3D Fornax Simulations