(GAIA) tool according to the approaches presented in Paper .[^6] First, we construct $25~{\rm mag~arcsec^{-2}}$ isophotes in the SDSS DR10 $g$-band, and then we visually fit on to each isophote an elliptical aperture centred at each galaxy centroid position. From the fitted elliptical apertures, we derive the major axes ($D_{25}$), elongations ($a/b$), and position angles (PA) of the major axes of galaxies. In further analysis, we use the $D_{25}$ corrected for Galactic and host galaxy internal extinction. We then calculate the inclinations of host galaxies using elongations and morphological types following the classical Hubble formula. More details on these procedures are found in Paper . Finally, an additional restriction on the inclinations ($i \leq 60^\circ$) of hosts is required to minimize absorption and projection effects in the discs of galaxies.[^7]

After these restrictions, we are left with a sample of 500 SNe within 419 host galaxies.[^8] For these host galaxies, we do visual inspection of the combined SDSS $g$-, $r$-, and $i$-band images, as well as check the different bands separately to detect any sign of barred structure in the stellar discs. In Paper , we demonstrated that given their superior angular resolution and three-colour representations, the SDSS images, especially 