2022MNRAS.513.5540M

The ultraviolet (UV) and near-infrared (NIR) photometric and optical spectroscopic observations of SN 2020acat covering ∼250 d after explosion are presented here. Using the fast rising photometric observations, spanning from the UV to NIR wavelengths, a pseudo-bolometric light curve was constructed and compared to several other well-observed Type IIb supernovae (SNe IIb). SN 2020acat displayed a very short rise time reaching a peak luminosity of Log₁₀(L) = 42.49 ±0.17 erg s^–1 in only ∼14.6 ± 0.3 d. From modelling of the pseudo-bolometric light curve, we estimated a total mass of ⁵⁶Ni synthesized by SN 2020acat of M_Ni = 0.13 ± 0.03 M_☉, with an ejecta mass of M_ej = 2.3 ± 0.4 M_☉ and a kinetic energy of E_k = 1.2 ± 0.3 x 10⁵¹ erg. The optical spectra of SN 2020acat display hydrogen signatures well into the transitional period (>= 100 d), between the photospheric and the nebular phases. The spectra also display a strong feature around 4900 Å that cannot be solely accounted for by the presence of the Fe II 5018 line. We suggest that the Fe II feature was augmented by He I 5016 and possibly by the presence of N II 5005. From both photometric and spectroscopic analysis, we inferred that the progenitor of SN 2020acat was an intermediate-mass compact star with an M_ZAMS of 15-20 M_☉.