  As one of the closest supernovae (SNe) in the last decade, SN 2023ixf is an
unprecedented 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 with
two independent analyses. We first modelled its spectral energy distribution
(SED) based on Hubble Space Telescope optical, Spitzer mid-infrared (IR), and
ground-based near-IR data. We find that stellar pulsation and circumstellar
extinction have great impacts on SED fitting, and the result suggests a
relatively massive red supergiant (RSG) surrounded by C-rich dust with an
initial mass of 16.2--17.4 Msun. The corresponding rate of mass-loss occurring
at 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 SN
environment based on resolved stellar populations, and the most recent
star-forming epoch corresponds to a progenitor initial mass of 17--19 Msun, in
agreement with that from our SED fitting. Therefore, we conclude that the
progenitor of SN 2023ixf is close to the high-mass end for Type II SN
progenitors.
