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We identify the progenitor star of SN 2023ixf in the nearby galaxy Messier101 using Keck/NIRC2 adaptive optics imaging and pre-explosion HST/ACS images.The supernova position, localized with diffraction-spike pattern and highprecision relative astrometry, unambiguously coincides with a single progenitorcandidate of m_F814W=24.96(-0.04)(+0.05). Forced photometry further recovers2-sigma detections in the F673N and F675W bands and imposes robust flux limitson the bluer bands. Given the reported infrared excess and semi-regularvariability of the progenitor, we fit a time-dependent spectral energydistribution (SED) model of a dusty red supergiant (RSG) to a combined datasetof HST photometry, as well as ground-based near-infrared and Spitzer/IRAC[3.6], [4.5] photometry from the literature. The progenitor closely resembles aRSG of T_eff=3343+/-27 K and logL=5.10+/-0.02, with a 0.11+/-0.01 dex(25.2+/-1.7 per cent) variation over the mean luminosity at a period ofP=1128.3+/-6.5 days, heavily obscured by a dust envelope with an optical depthof tau=2.83+/-0.03 at 1 micron (or A_V=10.28+/-0.11 mag). Such observedsignatures match a post-main sequence star of 18.1(-1.2)(+0.7) Msun, close tothe most massive SN II progenitor, with a pulsation-enhanced mass-loss rate ofM_dot=(3.58+/-0.15) x 10^(-4) Msun/yr. The dense and confined circumstellarmaterial is likely ejected during the last episode of radial pulsation beforethe explosion. Notably, we find strong evidence for periodic variation of tau(or both T_eff and tau) along with luminosity, a necessary assumption toreproduce the wavelength dependence of the variability, which implies dustsublimation and condensation during radial pulsations. Given the observed SED,partial dust obscuration remains a possible scenario, but any unobstructedbinary companion over 7.1 Msun can be ruled out.

The Progenitor Star of SN 2023ixf: A Massive Red Supergiant with Enhanced, Episodic Pre-Supernova Mass Loss