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We present photometric and spectroscopic observations of Supernova 2020oi (SN2020oi), a nearby ($\sim$17 Mpc) type-Ic supernova (SN Ic) within thegrand-design spiral M100. We undertake a comprehensive analysis to characterizethe evolution of SN 2020oi and constrain its progenitor system. We detect fluxin excess of the fireball rise model $\delta t \approx 2.5$ days from the dateof explosion in multi-band optical and UV photometry from the Las CumbresObservatory and the Neil Gehrels Swift Observatory, respectively. The derivedSN bolometric luminosity is consistent with an explosion with $M_{\rm ej} =0.81 \pm 0.03 M_{\odot}$, $E_{k}= 0.79 \pm 0.09 \times 10^{51} \rm{erg}\rm{s}^{-1}$, and $M_{\rm Ni56} = 0.08 \pm 0.02 M_{\odot}$. Inspection of theevent's decline reveals the highest $\Delta m_{15,\rm{bol}}$ reported for astripped-envelope event to date. Modeling of optical spectra near event peakindicates a partially mixed ejecta comparable in composition to the ejectaobserved in SN 1994I, while the earliest spectrum shows signatures of apossible interaction with material of a distinct composition surrounding the SNprogenitor. Further, Hubble Space Telescope (HST) pre-explosion imaging revealsa stellar cluster coincident with the event. From the cluster photometry, wederive the mass and age of the SN progenitor using stellar evolution modelsimplemented in the BPASS library. Our results indicate that SN 2020oi occurredin a binary system from a progenitor of mass $M_{\rm ZAMS} \approx 9.5 \pm 1.0M_{\odot}$, corresponding to an age of $27 \pm 7$ Myr. SN 2020oi is the dimmestSN Ic event to date for which an early-time flux excess has been observed, andthe first in which an early excess is unlikely to be associated withshock-cooling.

An Early-Time Optical and Ultraviolet Excess in the type-Ic SN 2020oi