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Stars with initial masses in the range of 8-25 solar masses are thought toend their lives as hydrogen-rich supernovae (SNe II). Based on thepre-explosion images of Hubble Space Telescope ($HST$) and $Spitzer$ SpaceTelescope, we place tight constraints on the progenitor candidate of type IIPSN 2023ixf in Messier 101. Fitting of the spectral energy distribution (SED) ofits progenitor with dusty stellar spectral models results in an estimation ofthe effective temperature as 3091$^{+422}_{-258}$ K. The luminosity isestimated 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 massloss rate (6-9$\times10^{-6}$ M$_{\odot}$ yr$^{-1}$) is much lower than thatinferred from the flash spectroscopy of the SN, suggesting that the progenitorexperienced a sudden increase in mass loss when approaching the finalexplosion. In the infrared bands, significant deviation from the range ofregular RSGs in the color-magnitude diagram and period-luminosity space of theprogenitor star indicates enhanced mass loss and dust formation. Combining withnew evidence of polarization at the early phases of SN 2023ixf, such a violentmass loss is likely a result of binary interaction.

The Dusty and Extremely Red Progenitor of the Type II Supernova 2023ixf in Messier 101