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We present optical spectroscopy together with ultraviolet, optical andnear-infrared photometry of SN 2019hcc, which resides in a host galaxy atredshift 0.044, displaying a sub-solar metallicity. The supernova spectrum nearpeak epoch shows a `w' shape at around 4000 {\AA} which is usually associatedwith O II lines and is typical of Type I superluminous supernovae. SN 2019hccpost-peak spectra show a well-developed H alpha P-Cygni profile from 19 dayspast maximum and its light curve, in terms of its absolute peak luminosity andevolution, resembles that of a fast-declining Hydrogen-rich supernova (SN IIL).The object does not show any unambiguous sign of interaction as there is noevidence of narrow lines in the spectra or undulations in the light curve. Ourtardis spectral modelling of the first spectrum shows that Carbon, Nitrogen andOxygen (CNO) at 19000 K reproduce the `w' shape and suggests that a combinationof non-thermally excited CNO and metal lines at 8000 K could reproduce thefeature seen at 4000 {\AA}. The Bolometric light curve modelling reveals thatSN 2019hcc could be fit with a magnetar model, showing a relatively strongmagnetic field (B > 3 x 10^14 G), which matches the peak luminosity and risetime without powering up the light curve to superluminous luminosities. Thehigh-energy photons produced by the magnetar would then be responsible for thedetected O II lines. As a consequence, SN 2019hcc shows that a `w' shapeprofile at around 4000 {\AA}, usually attributed to O II, is not only shown insuperluminous supernovae and hence it should not be treated as the soleevidence of the belonging to such a supernova type.

SN 2019hcc: A Type II Supernova Displaying Early O II Lines