2024ApJ...969..126Y

SN 2023ixf, recently reported in the nearby galaxy M101 at a distance of 6.85 Mpc, was one of the closest and brightest core-collapse supernovae in the last decade. In this work, we present multiwavelength photometric observation of SN 2023ixf with the Multi-channel Photometric Survey Telescope (Mephisto) in the uvgr bands and with the twin 50 cm telescopes in the griz bands. We find that the bolometric luminosity reached the maximum value of 3 × 10⁴³ erg s^–1 at 3.9 days after the explosion and fully settled onto the radioactive tail at ∼90 days. The effective temperature decreased from 3.2 × 10⁴ K at the first observation and approached a constant of ∼(3000-4000) K after the first 2 months. The evolution of the photospheric radius is consistent with a homologous expansion with a velocity of 8700 km s^–1 in the first 2 months, and it shrunk subsequently. Based on the radioactive tail, the initial nickel mass is about M_Ni ∼ 0.098 M_⊙. The explosion energy and the ejecta mass are estimated to be E ≃ (1.0-5.7) × 10⁵¹ erg and M_ej ≃ (3.8-16) M_⊙, respectively. The peak bolometric luminosity is proposed to be contributed by the interaction between the ejecta and the circumstellar medium (CSM). We find a shocked CSM mass of M_CSM ∼ 0.013 M_⊙, a CSM density of ρ_CSM ∼ 2.5 × 10^–13 g cm^–3, and a mass-loss rate of the progenitor of $\dot{M}\sim 0.022\,{M}_{\odot }\,{\mathrm{yr}}^{-1}$.