2019ApJ...882L..15S

High-cadence ultraviolet, optical, and near-infrared photometric and low-resolution spectroscopic observations of the peculiar Type II supernova (SN) 2018hna are presented. The early-phase multiband light curves (LCs) exhibit the adiabatic cooling envelope emission following the shock breakout up to ∼ 14 days from the explosion. SN 2018hna has a rise time of ∼ 88 days in the V band, similar to SN 1987A. A ⁵⁶Ni mass of ∼0.087 ± 0.004 M_☉ is inferred for SN 2018hna from its bolometric LC. Hydrodynamical modeling of the cooling phase suggests a progenitor with a radius ∼50 R_☉, a mass of ∼14-20 M_☉, and an explosion energy of ∼1.7-2.9 x 10⁵¹ erg. The smaller inferred radius of the progenitor than a standard red supergiant is indicative of a blue supergiant progenitor of SN 2018hna. A subsolar metallicity (∼0.3 Z_☉) is inferred for the host galaxy UGC 07534, concurrent with the low-metallicity environments of 1987A-like events.