galaxies. However, the inner fraction of CC SNe is significantly lower in barred Sa–Sbc galaxies compared with their unbarred counterparts. It is important to note that the inner fractions of Type Ia and CC SNe are not statistically different one from another when the same morphological and barred/unbarred categories are selected.

\[table0.3ratios\]

  -------- ---- ---- ------------------------ -- ----- ------------------------ -----------
                                                                                
                                                                                
  Sa–Sbc   Ia     39  $0.26_{-0.04}^{+0.05}$        40  $0.38_{-0.05}^{+0.05}$     0.170
  Sa–Sbc   CC     50  $0.20_{-0.03}^{+0.04}$        56  $0.36_{-0.04}^{+0.04}$   **0.044**
  Sc–Sm    Ia     34  $0.26_{-0.05}^{+0.05}$        39  $0.36_{-0.05}^{+0.05}$     0.240
  Sc–Sm    CC     86  $0.26_{-0.03}^{+0.03}$       127  $0.28_{-0.02}^{+0.02}$     0.741
  -------- ---- ---- ------------------------ -- ----- ------------------------ -----------

  : Fractions of inner ($R_{\rm SN} \leq 0.3\,R_{25}$) SNe in barred and unbarred host galaxies.

The results of Table \[table0.3ratios\] agree quite well with the findings of @2015MNRAS.450.3503J that barred galaxies of earlier Hubble types have substantially suppressed star formation , hence the lack of CC SNe in the inner radial range swept by the strong bars of Sa–Sbc galaxies. On the other hand, this region is not ‘forbidden’ to Type Ia SNe, because these SNe originate from an older stellar population also located in the bulge. CC SNe in barred Sc–Sm galaxies can appear in the inner regions because the effect of star 