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We present a detailed analysis of nearly two decades of optical/UV and X-raydata to study the multi-wavelength pre-explosion properties and post-explosionX-ray properties of nearby SN2023ixf located in M101. We find no evidence ofprecursor activity in the optical to UV down to a luminosity of $\lesssim7\times10^{4}\, \rm L_{\odot}$, while X-ray observations covering nearly 18years prior to explosion show no evidence of luminous precursor X-ray emissiondown to an absorbed 0.3 - 10.0 keV X-ray luminosity of $\sim6\times10^{36}$ ergs$^{-1}$. Extensive Swift observations taken post-explosion did not detect softX-ray emission from SN2023ixf within the first $\sim$3.3 days after firstlight, which suggests a mass-loss rate for the progenitor of$\lesssim5\times10^{-4}\,\rm M_{\odot}$ yr$^{-1}$ or a radius of$\lesssim4\times10^{15}$ cm for the circumstellar material. Our analysis alsosuggests that if the progenitor underwent a mass-loss episode, this had tooccur $>$ 0.5 - 1.5 years prior to explosion, consistent with previousestimates. Swift detected soft X-rays from SN2023ixf $\sim4.25$ days afterfirst light, and it rose to a peak luminosity of $\sim10^{39}$ erg s$^{-1}$after 10 days and has maintained this luminosity for nearly 50 days post firstlight. This peak luminosity is lower than expected, given the evidence thatSN2023ixf is interacting with dense material. However, this might be a naturalconsequence of an asymmetric circumstellar medium. X-ray spectra derived frommerging all Swift observations over the first 50 days are best described by atwo-component bremsstrahlung model consisting of a heavily absorbed and hottercomponent similar to that found using NuSTAR, and a less-absorbed, coolercomponent. We suggest that this soft component arises from cooling of theforward shock similar to that found in Type IIn SN2010jl.

Probing the Soft X-ray Properties and Multi-Wavelength Variability of SN2023ixf and its Progenitor