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We present an analysis of the relative frequencies of different supernova(SN) types in spirals with various morphologies and in barred or unbarredgalaxies. We use a well-defined and homogeneous sample of spiral host galaxiesof 692 SNe from the Sloan Digital Sky Survey in different stages ofgalaxy-galaxy interaction and activity classes of nucleus. We propose that theunderlying mechanisms shaping the number ratios of SNe types can be interpretedwithin the framework of interaction-induced star formation, in addition to theknown relations between morphologies and stellar populations. We find a strongtrend in behaviour of the NIa/NCC ratio depending on host morphology, such thatearly spirals include more Type Ia SNe. The NIbc/NII ratio is higher in a broadbin of early-type hosts. The NIa/NCC ratio is nearly constant when changingfrom normal, perturbed to interacting galaxies, then declines in merginggalaxies, whereas it jumps to the highest value in post-merging/remnantgalaxies. In contrast, the NIbc/NII ratio jumps to the highest value in merginggalaxies and slightly declines in post-merging/remnant subsample. Theinterpretation is that the star formation rates and morphologies of galaxies,which are strongly affected in the final stages of interaction, have an impacton the number ratios of SNe types. The NIa/NCC (NIbc/NII) ratio increases(decreases) from star-forming to active galactic nuclei (AGN) classes ofgalaxies. These variations are consistent with the scenario of aninteraction-triggered starburst evolving into AGN during the later stages ofinteraction, accompanied with the change of star formation and transformationof the galaxy morphology into an earlier type.

Supernovae and their host galaxies - II. The relative frequencies of supernovae types in spirals