  We present a series of high-resolution echelle spectra of SN~2023ixf in M101,
obtained nightly during the first week or so after discovery using PEPSI on the
LBT. NaID absorption in these spectra indicates a host reddening of
$E(B-V)$=0.031~mag and a systemic velocity of $+$7~km~s$^{-1}$ relative to the
average redshift of M101. Dramatic changes are seen in in the strength and
shape of strong emission lines emitted by CSM, including HeII4686,
CIV5801,5811, H$\alpha$, and NIV7109,7123. In general, these narrow lines
broaden to become intermediate-width lines before disappearing from the
spectrum within a few days, indicating a limited extent to the dense CSM of
around 20-30 AU (or $\la$10$^{14.7}$ cm). H$\alpha$ persists in the spectrum
for about a week as an intermediate-width emission line with P~Cyg absorption
at 700-1300 km s$^{-1}$ arising in the post-shock shell of swept-up CSM. Early
narrow emission lines are blueshifted and indicate an expansion speed in the
pre-shock CSM of about 115 km s$^{-1}$, but with even broader emission in
higher ionization lines. This is faster than the normal winds of red
supergiants, suggesting some mode of eruptive mass loss from the progenitor or
radiative acceleration of the CSM. A lack of narrow blueshifted absorption
suggests that most of the CSM is not along our line of sight. This and several
other clues indicate that the CSM of SN~2023ixf is significantly aspherical. We
find that CSM lines disappear after a few days because the asymmetric CSM is
engulfed by the SN photosphere.
