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As one of the closest supernovae (SNe) in the last decade, SN 2023ixf is anunprecedented target to investigate the progenitor star that exploded. However,there is still significant uncertainty in the reported progenitor properties.In this work, we present a detailed study of the progenitor of SN 2023ixf withtwo independent analyses. We first modelled its spectral energy distribution(SED) based on Hubble Space Telescope optical, Spitzer mid-infrared (IR), andground-based near-IR data. We find that stellar pulsation and circumstellarextinction have great impacts on SED fitting, and the result suggests arelatively massive red supergiant (RSG) surrounded by C-rich dust with aninitial mass of 16.2--17.4 Msun. The corresponding rate of mass-loss occurringat least 3 years before the SN explosion is about $2 \times 10^{-4}M_\odot$yr$^{-1}$. We also derived the star formation history of the SNenvironment based on resolved stellar populations, and the most recentstar-forming epoch corresponds to a progenitor initial mass of 17--19 Msun, inagreement with that from our SED fitting. Therefore, we conclude that theprogenitor of SN 2023ixf is close to the high-mass end for Type II SNprogenitors.

The dusty red supergiant progenitor and the local environment of the Type II SN 2023ixf in M101