  Supernova (SN) 2023ixf was discovered on May 19th, 2023. The host galaxy,
M101, was observed by the Hobby Eberly Telescope Dark Energy Experiment
(HETDEX) collaboration over the period April 30, 2020 -- July 10, 2020, using
the Visible Integral-field Replicable Unit Spectrograph (VIRUS;
$3470\lesssim\lambda\lesssim5540$ \r{A}) on the 10-m Hobby-Eberly Telescope
(HET). The fiber filling factor within $\pm$ 30 arcsec of SN 2023ixf is 80%
with a spatial resolution of 1 arcsec. The r<5.5 arcsec surroundings are 100%
covered. This allows us to analyze the spatially resolved pre-explosion local
environments of SN 2023ixf with nebular emission lines. The 2-dimensional (2D)
maps of the extinction and the star-formation rate (SFR) surface density
($\Sigma_{\rm SFR}$) show weak increasing trends in the radial distributions
within the r<5.5 arcsec regions, suggesting lower values of extinction and SFR
in the vicinity of the progenitor of SN 2023ixf. The median extinction and that
of the surface density of SFR within r<3 arcsec are $E(B-V)=0.06\pm0.14$, and
$\Sigma_{\rm SFR}=10^{-5.44\pm0.66}~\rm M_{\odot}\cdot yr^{-1}\cdot
arcsec^{-2}$. There is no significant change in extinction before and after the
explosion. The gas metallicity does not change significantly with the
separation from SN 2023ixf. The metal-rich branch of the $R_{23}$ calculations
indicates that the gas metallicity around SN 2023ixf is similar to the solar
metallicity ($\sim Z_{\odot}$). The archival deep images from the
Canada-France-Hawaii Telescope Legacy Survey (CFHTLS) show a clear detection of
the progenitor of SN 2023ixf in the $z$-band at $22.778\pm0.063$ mag, but
non-detections in the remaining four bands of CFHTLS ($u,g,r,i$). The results
suggest a massive progenitor of $\approx$ 22 $M_\odot$.
