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We report on our study of supernova (SN) 2022xxf based on observationsobtained during the first four months of its evolution. The light curves (LCs)display two humps of similar maximum brightness separated by 75 days,unprecedented for a broad-lined (BL) Type Ic supernova (SN IcBL). SN 2022xxf isthe most nearby SN IcBL to date (in NGC 3705, $z = 0.0037$, at a distance ofabout 20 Mpc). Optical and near-infrared photometry and spectroscopy are usedto identify the energy source powering the LC. Nearly 50 epochs of highsignal-to-noise-ratio spectroscopy were obtained within 130 days, comprising anunparalleled dataset for a SN IcBL, and one of the best-sampled SN datasets todate. The global spectral appearance and evolution of SN 2022xxf points totypical SN Ic/IcBL, with broad features (up to $\sim14000$ km s$^{-1}$) and agradual transition from the photospheric to the nebular phase. However, narrowemission lines (corresponding to $\sim1000-2500$ km s$^{-1}$) are present inthe spectra from the time of the second rise, suggesting slower-movingcircumstellar material (CSM). These lines are subtle, in comparison to thetypical strong narrow lines of CSM-interacting SNe, for example, Type IIn, Ibn,and Icn, but some are readily noticeable at late times such as in Mg I$\lambda$5170 and [O I] $\lambda$5577. Unusually, the near-infrared spectrashow narrow line peaks in a number of features formed by ions of O and Mg. Weinfer the presence of CSM that is free of H and He. We propose that theradiative energy from the ejecta-CSM interaction is a plausible explanation forthe second LC hump. This interaction scenario is supported by the colorevolution, which progresses to the blue as the light curve evolves along thesecond hump, and the slow second rise and subsequent rapid LC drop. (Abstractabridged)

The broad-lined Type-Ic supernova SN 2022xxf with extraordinary two-humped light curves