  High resolution spectra of the hot central star of the planetary nebula
(CSPN) M27, acquired with the Far Ultraviolet Spectroscopic Explorer (\FUSE),
have revealed an unusually rich set of narrow molecular hydrogen absorption
features. This object is also unique in that the velocity of nebular absorption
features are cleanly separated from the velocity of the intervening
interstellar medium. These features blend with and in many cases obscure atomic
features. We have developed a continuum model of the CSPN including atomic and
molecular hydrogen absorption. Using this model we have identified and
tabulated the metal lines as arising from either photospheric, nebular and/or
non-nebular velocity systems. We find the nebular outflow and ionization
balance to be stratified with high ionization states favored at low velocity
and low ionization states favored at high velocity. Neutrals and molecules are
found at a velocity that marks the transistion between these two regimes. These
observations are a challenge to the interacting wind model of PN evolution.
Mappings at high resolution of the line profiles for \ion{C}{1} \ion{-}{4},
\ion{N}{1} \ion{-}{3}, \ion{O}{1}, \ion{O}{6}, \ion{Si}{2} \ion{-}{4},
\ion{P}{2} \ion{-}{5}, \ion{S}{2} \ion{-}{4}, \ion{Ar}{1} \ion{-}{2} and
\ion{Fe}{2} \ion{-}{3} within the \FUSE and STIS bandpasses are presented. The
digitial spectra of the stars and the model are freely available on the
H$_2$ools website. They will be useful for photospheric analyses seeking to
determine the metallicity of the central star and for absorption line based
atomic and molecular abundance determination of the nebular outflow.
