Notes. The table columns give the ejecta mass, the ejecta kinetic energy, as well as the cumulative yields of H, He, O, Mg, Si, Ca, and ⁵⁶Ni prior to decay. We specify whether the Si-rich and the O-rich shells merged before core collapse (this did not occur in the WH07 models, and only in three of the S16 models). The last two columns give the choice of mass cut M_sh for the shell shuffling, as well as the associated velocity that bounds 99% of the total ⁵⁶Ni mass in the corresponding model. The selected models from S16 were exploded with the W18 engine. ^(a) This indicates that the progenitor underwent Si-O shell merging prior to core collapse. The contamination of Si and Ca in the O-rich shell is strong in models s20p1 and s25p2 but moderate in model s26p5 (i.e., only the inner parts of the O-rich shell are contaminated by Si-rich material in model s26p5).