  Stars with initial masses in the range of 8-25 solar masses are thought to
end their lives as hydrogen-rich supernovae (SNe II). Based on the
pre-explosion images of Hubble Space Telescope ($HST$) and $Spitzer$ Space
Telescope, we place tight constraints on the progenitor candidate of type IIP
SN 2023ixf in Messier 101. Fitting of the spectral energy distribution (SED) of
its progenitor with dusty stellar spectral models results in an estimation of
the effective temperature as 3091$^{+422}_{-258}$ K. The luminosity is
estimated as log($L/$L$_{\odot}$)$\sim4.83$, consistent with a red supergiant
(RSG) star with an initial mass of 12$^{+2}_{-1}$ M$_{\odot}$. The derived mass
loss rate (6-9$\times10^{-6}$ M$_{\odot}$ yr$^{-1}$) is much lower than that
inferred from the flash spectroscopy of the SN, suggesting that the progenitor
experienced a sudden increase in mass loss when approaching the final
explosion. In the infrared bands, significant deviation from the range of
regular RSGs in the color-magnitude diagram and period-luminosity space of the
progenitor star indicates enhanced mass loss and dust formation. Combining with
new evidence of polarization at the early phases of SN 2023ixf, such a violent
mass loss is likely a result of binary interaction.
