for low-inclined galaxies, offer a much more reliable and capacious source for bar detection than do the other images, e.g. plate-based images on which most of the HyperLeda/NED classifications were performed. To check the consistency of bar detection in our sample with that of the SDSS-based EFIGI[^9] catalogue of nearby visually classified 4458 PGC galaxies , we select a subsample of 149 galaxies that are common to both EFIGI and to our sample of SNe hosts. Following Paper , we compare the EFIGI `Bar Length` attribute[^10] with our detection (bar or no bar). When the `Bar Length` is 0 or 2, our bar detection is different for only 6 per cent of cases. When the `Bar Length` is 3 or 4, our bar detection completely matches with that of the EFIGI. However, we do not detect bars in 30 per cent of the cases when `Bar Length` is 1. Hence, the EFIGI `Bar Length` $=$ 1 mainly corresponds to the threshold of our bar detection, i.e., barely visible bar feature with a length about one-tenth of $D_{25}$.[^11] Table \[table\_SN\_morph\] displays the distribution of all SNe types among the various considered morphological types for their barred and unbarred host galaxies.

Results 