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The progenitor of SN 2023ixf was a $\sim$10$^{4.8}$ to $10^{5.0}\rm ~L_\odot$star ($\sim$9 to $14 \rm~M_\odot$ at birth) obscured by a dusty $\dot{M} \simeq10^{-5} \rm~M_\odot~yr^{-1}$ wind with a visual optical depth of $\tau_V \simeq13$. This is required by the progenitor SED, the post-SN X-ray and H$\alpha$luminosities, and the X-ray column density estimates. In Large BinocularTelescope (LBT) data spanning 5600 to 400 d before the SN, there is no evidencefor optical variability at the level of $\sim$10$^3\rm~L_\odot$ in $R$ band,roughly 3 times the predicted luminosity of the obscured progenitor. Thisconstrains direct observation of any pre-SN optical outbursts where there areLBT observations. However, models of the effects of any pre-SN outburst on thedusty wind show that an outburst of essentially any duration exceeding $\sim$5times the luminosity of the progenitor would have detectable effects on thedust optical depth for decades. While the dust obscuration here is high, allred supergiants have dusty winds, and the destruction (or formation) of dust byeven short-lived transients will always have long term effects on the observedbrightness of the star because changes in the dust optical depths after aluminous transient occur very slowly.

Constraints on pre-SN outbursts from the progenitor of SN 2023ixf using the Large Binocular Telescope