181   0.349   0.132   **0.000**   **0.000**
  $U/R_{25}$ versus $V/r_{25}$   Ia    180   0.394   0.387     0.561       0.646        105   0.385   0.390     0.174       0.321
  $U/R_{25}$ versus $V/r_{25}$   CC    320   0.382   0.384     0.120       0.162        181   0.349   0.327     0.564       0.568
  ------------------------------ ---- ----- ------- ------- ----------- ----------- -- ----- ------- ------- ----------- -----------

It is worth mentioning that Sa–Sm galaxies contain stellar populations of different ages and host both Type Ia and CC SNe. While S0 and S0/a galaxies, which are mostly populated by old stars and have prominent bulges, host Type Ia SNe. A tiny fraction of CC SNe has also been detected in galaxies classified as S0. Nevertheless, in these rare cases, there is some evidence of residual star formation in the SN hosts, due to merging/accretion or interaction with close neighbours in the past (e.g. ; Paper ). The distribution of SNe types versus morphology of the host galaxies, shown in Table \[table\_SN\_morph\], is consistent with this picture. In this sense, when selecting only Sa–Sm hosts, the $P_{\rm KS}$ for Type Ia SNe in the face-on sample becomes significant (it is reduced to 0.045), suggestive of a possible contribution from bulge SNe Ia in S0–S0/a galaxies. For Sa–Sm galaxies, the probabilities of KS and 