Table A.1: List of progenitors used in the simulations. $M_{{\rm Fe-Si}}$ and $M_{{\rm Si-O}}$ are the enclosed masses at composition interfaces defined by entropy jumps. With (e) we denote that a shell interface is connected with a gradual enrichment of the lighter nucleus, i.e. these cases are Fe-FeSi and Si-SiO interfaces where the mass fractions of Si or O grows gradually outwards. The underlined numbers indicate an entropy increase of more than $1~\ensuremath{k_{\rm B}} $ per nucleon in case of an Fe-Si interface and an entropy increase of more than $2~\ensuremath{k_{\rm B}} $/by in case of a Si-O interface.
Model  $M_{\rm ZAMS}$ [ $\ensuremath{M_{\odot}} $] Reference $M_{{\rm Fe-Si}}$ [ $\ensuremath{M_{\odot}} $] $M_{{\rm Si-O}}$ [ $\ensuremath{M_{\odot}} $] Notes
s1b >2.26 Woosley, personal comm. 1.34 1.38 model for Type Ib supernova
s11.2 11.2 Woosley et al. (2002) 1.24 1.30(e) from www.stellarevolution.org
n13 13 Nomoto & Hashimoto (1988) 1.18 1.50  
s15s7b2 15 Woosley & Weaver (1995) 1.28(e) 1.43(e)  
l15 15 Limongi et al. (2000) 1.16(e) 1.60  
s15a28 15 Heger et al. (2001) 1.42(e) 1.81  
s20.0 20.0 Woosley et al. (2002) 1.46 1.82 from www.stellarevolution.org
l25 25 Limongi et al. (2000) 1.58 1.84(e)  
s25a28 25 Heger et al. (2001) 1.62 1.98(e)  


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