  SN 2023ixf, recently reported in the nearby galaxy M101 at a distance of
$6.85~{\rm Mpc}$, was one of the closest and brightest core-collapse supernovae
(CCSNe) in the last decade. In this work, we present multi-wavelength
photometric observation of SN 2023ixf with the Multi-channel Photometric Survey
Telescope (Mephisto) in $uvgr$ bands and with the twin 50-cm telescopes in
$griz$ bands. We find that the bolometric luminosity reached the maximum value
of $3\times10^{43}~{\rm erg~s^{-1}}$ at 3.9 days after the explosion and fully
settled onto the radioactive tail at $\sim90$ days. The effective temperature
decreased from $3.2\times10^4~{\rm K}$ at the first observation and approached
to a constant of $\sim(3000-4000)~{\rm K}$ after the first two months. The
evolution of the photospheric radius is consistent with a homologous expansion
with a velocity of $8700~{\rm km~s^{-1}}$ in the first two months, and it
shrunk subsequently. Based on the radioactive tail, the initial nickel mass is
about $M_{\rm Ni}\sim 0.098M_\odot$. The explosion energy and the ejecta mass
are estimated to be $E\simeq(1.0-5.7)\times10^{51}~{\rm erg}$ and $M_{\rm
ej}\simeq(3.8-16)M_\odot$, 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 $M_{\rm
CSM}\sim0.013M_\odot$, a CSM density of $\rho_{\rm
CSM}\sim2.5\times10^{-13}~{\rm g~cm^{-3}}$ and a mass loss rate of the
progenitor of $\dot M\sim0.022M_\odot~{\rm yr^{-1}}$.
