The arXiv preprint by Hiramatsu et al. (2026) presents SN 2023vbw as the strongest observational match yet to pair-instability supernova (PISN) theory, with a 170-350 solar-mass ejecta, 1.2-1.6 solar masses of nickel, and 6-13 x 10^52 erg explosion energy derived from semi-analytical light-curve fits to a low-metallicity dwarf galaxy host at z=0.088. Unlike earlier candidates such as SN 2007bi (Gal-Yam et al. 2009, Nature), whose spectra lacked clear hydrogen and whose nickel mass estimates were lower, 2023vbw shows both hydrogen-rich ejecta and an extended 190-day peak radiating 3 x 10^50 erg, directly matching the full predicted PISN light-curve morphology for 140-260 solar-mass progenitors. The study relies on a single well-observed event with ground-based photometry and spectroscopy plus circumstellar interaction signatures; limitations include reliance on semi-analytical rather than full radiation-hydrodynamics models and the absence of nebular-phase data that could confirm complete stellar disruption. This detection also connects to JWST findings of unexpectedly massive stars at z>6 (e.g., Finkelstein et al. 2023, ApJL), suggesting PISNe contributed to early chemical enrichment patterns previously attributed only to core-collapse events. The original coverage underplays the aspherical CSM interaction evidence, which may indicate binary-driven mass loss missed in isolated-star PISN simulations (Woosley et al. 2007, ApJ). As a preprint, these conclusions await peer review and multi-wavelength follow-up.