Extended Data Fig. 1: Elemental mass ratios in Cas A compared to supernova nucleosynthesis models across a wider range of model parameters.
From: Chlorine and potassium enrichment in the Cassiopeia A supernova remnant
Top: Comparison with 15M⊙ models with the several initial metalicities ([Fe/H]= − 2, − 1, 0) and rotation velocities (v = 0, 150, 300 km s−1) provided by Limongi & Chieffi21. Middle: Comparison with 13, 14, 15, 16M⊙ models of the single star cases and the binary cases provided by farmer et al.12. In each binary case, the companion star mass is set to 0.8 times of the progenitor. Bottom: Comparison with non-rotating single star models with several masses provided by Sukhbold et al.22. The 14.9M⊙ and 19.3M⊙ models shows onion-like layers constituted with O-, Ne-, and C-burning layers. In contrast, in the 19.8M⊙ and 20.1M⊙ models, the O-burning layers are merging with the outer layers like shell mergers (see Figure ?). To facilitate comparison between the observed values and the model values, only the model values are connected with lines.
