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Fig. 2

image

From top to bottom: ejecta kinetic energy, the mean expansion rate, the 56Ni mass, the mass of the H-rich shell (i.e., corresponding to the progenitor H-rich envelope), and finally the masses of the O-rich shell (which includes the O/Si, the O/Ne/Mg, and the O/C shells) and of the O/C shell in our selection of WH07 (circles) and S16 (stars) models. The Ekin is prescribed in the WH07 models, but computed ab-initio in the S16 models. This explains the more complicated trends in the latter (e.g., the systematically lower Ekin and M(56Ni) for masses above about 16 M, with some exceptions with the Ekin of s25p2), which includes regions in original mass that lead to no explosion at all (hence these models are not included in our sample; see S16 for a discussion).

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