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We model the late evolution and mass loss history of rapidly rotatingWolf-Rayet stars in the mass range $5\,\rm{M}_{\odot}\dots100\,\rm{M}_{\odot}$. We find that quasi-chemically homogeneously evolvingsingle stars computed with enhanced mixing retain very little or no helium andare compatible with Type\,Ic supernovae. The more efficient removal of coreangular momentum and the expected smaller compact object mass in our lower massmodels lead to core spins in the range suggested for magnetar drivensuperluminous supernovae. Our more massive models retain larger specific coreangular momenta, expected for long-duration gamma-ray bursts in the collapsarscenario. Due to the absence of a significant He envelope, the rapidlyincreasing neutrino emission after core helium exhaustion leads to anaccelerated contraction of the whole star, inducing a strong spin-up, andcentrifugally driven mass loss at rates of up to$10^{-2}\,\rm{M}_{\odot}~\rm{yr^{-1}}$ in the last years to decades before corecollapse. Since the angular momentum transport in our lower mass modelsenhances the envelope spin-up, they show the largest relative amounts ofcentrifugally enforced mass loss, i.e., up to 25\% of the expected ejecta mass.Our most massive models evolve into the pulsational pair-instability regime. Wewould thus expect signatures of interaction with a C/O-rich circumstellarmedium for Type~Ic superluminous supernovae with ejecta masses below $\sim10\,\rm{M}_{\odot}$ and for the most massive engine-driven explosions withejecta masses above $\sim 30\,\rm{M}_{\odot}$. Signs of such interaction shouldbe observable at early epochs of the supernova explosion, and may be related tobumps observed in the light curves of superluminous supernovae, or to themassive circumstellar CO-shell proposed for Type~Ic superluminous supernovaGaia16apd.

Related progenitor models for long-duration gamma ray bursts and Type Ic superluminous supernovae