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We present UV/optical observations and models of supernova (SN) 2023ixf, atype II SN located in Messier 101 at 6.9 Mpc. Early-time ("flash") spectroscopyof SN 2023ixf, obtained primarily at Lick Observatory, reveals emission linesof H I, He I/II, C IV, and N III/IV/V with a narrow core and broad, symmetricwings arising from the photo-ionization of dense, close-in circumstellarmaterial (CSM) located around the progenitor star prior to shock breakout.These electron-scattering broadened line profiles persist for $\sim$8 days withrespect to first light, at which time Doppler broadened features from thefastest SN ejecta form, suggesting a reduction in CSM density at $r \gtrsim10^{15}$ cm. The early-time light curve of SN2023ixf shows peak absolutemagnitudes (e.g., $M_{u} = -18.6$ mag, $M_{g} = -18.4$ mag) that are $\gtrsim2$ mag brighter than typical type II supernovae, this photometric boost alsobeing consistent with the shock power supplied from CSM interaction. Comparisonof SN 2023ixf to a grid of light curve and multi-epoch spectral models from thenon-LTE radiative transfer code CMFGEN and the radiation-hydrodynamics codeHERACLES suggests dense, solar-metallicity, CSM confined to $r = (0.5-1) \times10^{15}$ cm and a progenitor mass-loss rate of $\dot{M} = 10^{-2}$M$_{\odot}$yr$^{-1}$. For the assumed progenitor wind velocity of $v_w = 50$ kms$^{-1}$, this corresponds to enhanced mass-loss (i.e., ``super-wind'' phase)during the last $\sim$3-6 years before explosion.

SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova