  We present ultraviolet spectra of the dwarf Seyfert 1 nucleus of NGC 4395,
obtained with the Far Ultraviolet Spectroscopic Explorer (FUSE) and the Hubble
Space Telescope's Space Telescope Imaging Spectrograph at velocity resolutions
of 7 to 15 km/sec. We confirm our earlier claim of C IV absorption in
low-resolution UV spectra and detect a number of other absorption lines with
lower ionization potentials. In addition to the Galactic lines, we identify two
kinematic components of absorption that are likely to be intrinsic to NGC 4395.
We consider possible origins of the absorption, including the interstellar
medium (ISM) of NGC 4395, the narrow-line region (NLR), outflowing UV
absorbers, and X-ray ``warm absorbers.'' Component 1, at a radial velocity of
-770 km/sec with respect to the nucleus, is only identified in the C IV 1548.2
line. It most likely represents an outflowing UV absorber, similar to those
seen in a majority of Seyfert 1 galaxies, although additional observations are
needed to confirm the reality of this feature. Component 2, at -114 km/sec,
most likely arises in the ISM of NGC 4395; its ionic column densities cannot be
matched by photoionization models with a power-law continuum. Our models of the
highly ionized X-ray absorbers claimed for this active galactic nucleus
indicate that they would have undetectable C IV absorption, but large O VI and
H I columns should be present. We attribute our lack of detection of the O VI
and Ly-beta absorption from the X-ray absorbers to a combination of noise and
dilution of the nuclear spectrum by hot stars in the large FUSE aperture.
