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Supernova detection is a major objective of the Super-Kamiokande (SK)experiment. In the next stage of SK (SK-Gd), gadolinium (Gd) sulfate will beadded to the detector, which will improve the ability of the detector toidentify neutrons. A core-collapse supernova will be preceded by an increasingflux of neutrinos and anti-neutrinos, from thermal and weak nuclear processesin the star, over a timescale of hours; some of which may be detected at SK-Gd.This could provide an early warning of an imminent core-collapse supernova,hours earlier than the detection of the neutrinos from core collapse. Electronanti-neutrino detection will rely on inverse beta decay events below the usualanalysis energy threshold of SK, so Gd loading is vital to reduce backgroundswhile maximising detection efficiency. Assuming normal neutrino mass ordering,more than 200 events could be detected in the final 12 hours before corecollapse for a 15-25 solar mass star at around 200 pc, which is representativeof the nearest red supergiant to Earth, $\mathrm{\alpha}$Ori (Betelgeuse). At astatistical false alarm rate of 1 per century, detection could be up to 10hours before core collapse, and a pre-supernova star could be detected by SK-Gdup to 600 pc away. A pre-supernova alert could be provided to the astrophysicscommunity following gadolinium loading.

Sensitivity of Super-Kamiokande with Gadolinium to Low Energy Anti-neutrinos from Pre-supernova Emission