SN 2020acat: an energetic fast rising Type IIb supernova

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 $mathrm{{ m Log}_{10}}(L) = 42.49 pm 0.17 , mathrm{erg , s^{-1}}$ in only ~14.6 ± 0.3 d. From modelling of the pseudo-bolometric light curve, we estimated a total mass of <SUP>56</SUP>Ni synthesized by SN 2020acat of M<SUB>Ni</SUB> = 0.13 ± 0.03 M<SUB>⊙</SUB>, with an ejecta mass of M<SUB>ej</SUB> = 2.3 ± 0.4 M<SUB>⊙</SUB> and a kinetic energy of E<SUB>k</SUB> = 1.2 ± 0.3 × 10<SUP>51</SUP> 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<SUB>ZAMS</SUB> of 15-20 M<SUB>⊙</SUB>.