these galaxies SNe Ia mostly exploded in the disc component where all CC SNe also occur. Thus, the apparent deviation of the radial distribution of Type Ia SNe in S0–S0/a galaxies from that in Sa–Sm hosts (upper panel of Fig. \[hist\_distr\]) is attributed to the contribution by SNe Ia from the bulge component of S0–S0/a galaxies.

Another interesting results stands out in Table \[diffSNe\_KS\_AD\]. The radial distributions of CC SNe in barred versus unbarred Sa–Sbc galaxies are inconsistent (middle panel of Fig. \[hist\_distr\]), while for Type Ia SNe the radial distributions between barred and unbarred Sa–Sbc galaxies are not significantly different. At the same time, the radial distributions of both Type Ia and CC SNe in Sc–Sm galaxies are not affected by bars.

Interestingly, discovered that several early-type barred spiral galaxies that had strong dips in their radial H$\alpha$ line emission profiles, near $0.25\,R_{25}$.[^14] This region is roughly where their unbarred counterparts host the strongest star formation. The H$\alpha$ emission from barred Sb–Sbc galaxies showed central components and concentrations of star formation at or just outside the bar-end radius. Except for the central component, where we have difficulties to discover SNe, the picture of is very similar to that we 