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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 × 10 ^43 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 × 10 ^4 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) × 10 ^51 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 $\dot{M}\sim 0.022\,{M}_{\odot }\,{\mathrm{yr}}^{-1}$ .