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Table 5:

Supernovae type Ia mass fraction, $\xi = M_{\rm Fe,SNIa}/(M_{\rm Fe,SNIa}+M_{\rm Fe,SNcc})$, obtained for different theoretical SNe silicon-to-iron and nickel-to-iron ratios from the observed Si/Fe and Ni/Fe ratios.
mekal model       SNIa      
SNcc W7 W70 WDD1 WDD2 WDD3 CDD1 CDD2
No06,S 0.528-0.571 0.515-0.734          
No06,T 0.575-0.579 0.562-0.760          
CL04,S   0.505-0.582   0.546-0.789 0.505-0.728   0.534-0.770
CL04,T   0.559-0.728   0.600-0.727 0.559-0.758   0.588-0.727
W95,S     0.616-0.677 0.518-0.775 0.476-0.712 0.635-0.652 0.505-0.756
W95,T       0.554-0.792 0.512-0.732   0.541-0.774

apec model

      SNIa      
SNcc W7 W70 WDD1 WDD2 WDD3 CDD1 CDD2
No06,S   0.475-0.511   0.514-0.764 0.475-0.707   0.502-0.747
No06,T       0.564-0.789 0.526-0.735   0.553-0.773
CL04,S     0.591-0.886 0.502-0.759 0.581-0.701 0.608-0.841 0.490-0.741
CL04,T     0.647-0.855 0.561-0.787 0.523-0.734 0.663-0.799 0.549-0.771
W95,S     0.560-0.885 0.640-0.744   0.577-0.885 0.640-0.725
W95,T     0.598-0.895 0.561-0.763   0.615-0.868 0.561-0.745

SNIa yields are computed from the full set of models for deflagration (W7, W70) and delayed detonation (WDDs, CDDs) scenarios by Iwamoto et al. (1999). SNcc yields are integrated over a Salpeter (x=1.35) or a AY top-heavy (x=0.95) IMF, with abundance of the progenitor Z=0.02. Models for SNcc are taken from Nomoto et al. (2006, No06), Chieffi & Limongi (2004, CL04) and Woosley & Weaver (1995, W95).

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