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In this study, we analyze the post-maximum spectra of a sample of 27 Type Isuperluminous supernovae (SLSNe-I) in order to search for physical differencesbetween the so-called Type W and Type 15bn sub-types. This paper is acontinuation of \citet{ktr21} and \citet{ktr22}. In the former, it was revealedthat not all SLSNe-I show the W-shaped absorption feature between 4000 and 5000\AA\ in the pre-maximum spectra, and two new SLSN-subgroups were disclosed:Type W, where the W-shaped feature is present, and Type 15bn, where it ismissing. In the latter, it was shown that the pre-maximum photosphere of Type WSLSNe-I tend to be hotter compared to Type 15bn objects, and they are differentregarding their ion composition, their early light curves and their geometry aswell. For completeness, post-maximum data are analyzed in this paper. It isconcluded that in terms of photospheric temperature and velocity, Type W andType 15bn SLSNe decrease to a similar value by the post-maximum phases, andtheir pseudo-nebular spectra are nearly uniform. Pseudo-equivalent widthcalculations show that the pEW of the wavelength range between 4166 and 5266\AA\ evolve differently in case of the two sub-types, while the other parts ofthe spectra seem to evolve similarly. It was found that the host galaxies ofthe studied objects do not differ significantly in their star formation rate,morphology, stellar mass and absolute brightness. The main difference behindthe bimodality of Type W and Type 15bn SLSNe-I therefore is in theirpre-maximum evolution.

Type W and Type 15bn subgroups of hydrogen-poor superluminous supernovae: pre-maximum diversity, post-maximum homogeneity?