stronger in galaxies classified as barred Sb or Sbc, where the overall distributions of star formation markedly different from that in their unbarred counterparts.

In this context, we are investigating the possible impact of stellar bars and bulges on the radial distributions of the different types of supernovae (SNe) in S0–Sm host galaxies. SNe are generally divided into two categories according to their progenitors: core-collapse (CC) and Type Ia SNe. CC SNe result from massive young stars that undergo CC ,[^2] while Type Ia SNe are the end point in the evolution of binary stars when an older white dwarf (WD) accretes material from its companion, causing the WD mass to exceed the Chandrasekhar limit, or a double WD system loses angular momentum due to gravitational wave emission, leading to coalescence and explosion . The distribution of Type Ia SNe traces the distribution of $R$-band continuum emission/stellar mass in host disc galaxies, while the distribution of CC SNe is strongly related to the distribution of H$\alpha$ emission/star formation [for the most recent review, see @2015PASA...32...19A]. Therefore, it is expected that the above mentioned bar effect and a possible contribution from the old bulge populations in disc galaxies would leave their 