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We present the analysis of SN 2020wnt, an unusual hydrogen-poorsuper-luminous supernova (SLSN-I), at a redshift of 0.032. The light curves ofSN 2020wnt are characterised by an early bump lasting $\sim5$ days, followed bya bright main peak. The SN reaches a peak absolute magnitude ofM$_{r}^{max}=-20.52\pm0.03$ mag at $\sim77.5$ days from explosion. Thismagnitude is at the lower end of the luminosity distribution of SLSNe-I, butthe rise-time is one of the longest reported to date. Unlike other SLSNe-I, thespectra of SN 2020wnt do not show O II, but strong lines of C II and Si II aredetected. Spectroscopically, SN 2020wnt resembles the Type Ic SN 2007gr, butits evolution is significantly slower. Comparing the bolometric light curve tohydrodynamical models, we find that SN 2020wnt luminosity can be explained byradioactive powering. The progenitor of SN 2020wnt is likely a massive andextended star with a pre-SN mass of 80 M$_\odot$ and a pre-SN radius of 15R$_\odot$ that experiences a very energetic explosion of $45\times10^{51}$ erg,producing 4 M$_\odot$ of $^{56}$Ni. In this framework, the first peak resultsfrom a post-shock cooling phase for an extended progenitor, and the luminousmain peak is due to a large nickel production. These characteristics arecompatible with the pair-instability SN scenario. We note, however, that asignificant contribution of interaction with circumstellar material cannot beruled out.

SN 2020wnt: a slow-evolving carbon-rich superluminous supernova with no O II lines and a bumpy light curve