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Among the diverse progenitor channels leading to Type Ia Supernovae (SNe Ia),there are explosions originating from white dwarfs with sub-Chandrasekharmasses. These white dwarfs undergo detonation and explosion triggered byprimary detonation in the helium shell, which has been accreted from acompanion star. The double-detonation model predicts a correlation between theage of the progenitor system and the near peak brightness: the younger theexploding progenitors, the brighter the SNe. In this paper, we present ourrecent achievements on the study of SNe Ia properties in different locationswithin host galactic discs and the estimation of their progenitor populationages. Observationally, we confirm the validity of the anticipated correlationbetween the SN photometry and the age of their progenitors.

Constraining Supernova Ia Progenitors by their Locations in Host Galactic Disc