The analytical model found that the intrinsic variation in the initial metallicity of the Type Ia supernova (SN Ia) progenitor stars () translates into a 25% variation in the synthesized mass, and therefore, into a difference of ∼0. 2 mag in the observed peak luminosity of SNe Ia. Previous observational studies used the currently observed global gas-phase metallicity of host galaxies, instead of that was used in the model, and the studies showed a higher scatter in the mass measurements than the model prediction. We used of 34 normal SNe Ia and employed recent SN Ia explosion models with various configurations to cover the observed mass range. Unlike previous studies, which only used samples in the sub-solar range, our sample covers the range (frac Z_⊙ < < 3 Z_⊙), where most of the effect occurs. Linear regression returns a slope of 0. 02±0. 03, which trend is opposite to that of the analytical model, but at at low statistical significance level. A comparison of our sample with SN Ia explosion models on the mass diagram allowed us to constrain the progenitor scenarios. We also explored other chemical composition indicators, such as (Fe/H) ₚrogenitor and (α/Fe) ₚrogenitor. For (Fe/H) ₚrogenitor, our sample follows the trend predicted by the analytical models, but at a low significance level (0. 4σ). Noticeably, (α/Fe) ₚrogenitor shows the opposite trend and a clear gap. When we split the sample at (α/Fe) ₚrogenitor = 0. 35 (α/Fe) _⊙, we find a 3σ difference in the weighted means of the mass. Lastly, the standardized luminosities of SNe Ia in different groups differed by 0. 14±0. 09 (1. 6σ) mag. We highlight a holistic approach (from the progenitor star to the explosion with SN Ia and host galaxy observational data) to understanding the underlying physics of SNe Ia for a more accurate and precise cosmology.
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