We present a detailed analysis of nearly two decades of optical/UV and X-ray
data to study the multi-wavelength pre-explosion properties and post-explosion
X-ray properties of nearby SN2023ixf located in M101. We find no evidence of
precursor activity in the optical to UV down to a luminosity of β²7Γ104Lββ, while X-ray observations covering nearly 18
years prior to explosion show no evidence of luminous precursor X-ray emission
down to an absorbed 0.3 - 10.0 keV X-ray luminosity of βΌ6Γ1036 erg
sβ1. Extensive Swift observations taken post-explosion did not detect soft
X-ray emission from SN2023ixf within the first βΌ3.3 days after first
light, which suggests a mass-loss rate for the progenitor of
β²5Γ10β4Mββ yrβ1 or a radius of
β²4Γ1015 cm for the circumstellar material. Our analysis also
suggests that if the progenitor underwent a mass-loss episode, this had to
occur > 0.5 - 1.5 years prior to explosion, consistent with previous
estimates. Swift detected soft X-rays from SN2023ixf βΌ4.25 days after
first light, and it rose to a peak luminosity of βΌ1039 erg sβ1
after 10 days and has maintained this luminosity for nearly 50 days post first
light. This peak luminosity is lower than expected, given the evidence that
SN2023ixf is interacting with dense material. However, this might be a natural
consequence of an asymmetric circumstellar medium. X-ray spectra derived from
merging all Swift observations over the first 50 days are best described by a
two-component bremsstrahlung model consisting of a heavily absorbed and hotter
component similar to that found using NuSTAR, and a less-absorbed, cooler
component. We suggest that this soft component arises from cooling of the
forward shock similar to that found in Type IIn SN2010jl.Comment: 27 pages, 13 figure