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SNe II show growing evidence of interaction with CSM surrounding theirprogenitor stars as a consequence of enhanced mass loss during the last yearsof the progenitor's life. We present an analysis of the progenitor mass-losshistory of SN2023ixf, a nearby SN II showing signs of interaction. We calculatethe early-time bolometric light curve (LC) for SN2023ixf based on theintegration of the observed flux covering UV, optical and NIR bands, andblack-body extrapolations for the unobserved flux. Our calculations spot thesudden increase to maximum luminosity and temperature, in addition to thesubsequent fall, displaying an evident peak. This is the first time that thisphase can be precisely estimated for a SN II showing interestingcharacteristics as: 1) slope changes during the rise to maximum luminosity; and2) a very sharp peak with a maximum luminosity of $\sim$3$\times$10$^{45}$ergs$^{-1}$. We use the bolometric LC of SN2023ixf to test the calibrations ofbolometric corrections against colours from the literature. In addition, weinclude SN2023ixf into some of the available calibrations to extend their useto earlier epochs. Comparison of the observed bolometric LC to SN II explosionmodels with CSM interaction suggests a progenitor mass-loss rate of3$\times$10$^{-3}M_{\odot}$yr$^{-1}$ confined to 12000$R_{\odot}$ and a windacceleration parameter of $\beta$=5. This model reproduces the early bolometricLC, expansion velocities, and the epoch of disappearance of interacting linesin the spectra. This model indicates that the wind was launched $\sim$80yrbefore the explosion. If the effect of the wind acceleration is not taken intoaccount, the enhanced wind must have developed over the final months to yearsprior to the SN, which may not be consistent with the lack of outburstdetection in pre-explosion images over the last $\sim$20yr before explosion.

Circumstellar interaction models for the early bolometric light curve of SN 2023ixf