  We observed the Seyfert 1 galaxy NGC 3516 with the Goddard High Resolution
Spectrograph on the Hubble Space Telescope, and obtained UV spectra at a
resolution of about 20,000 in the redshifted C IV 1549 region. The intrinsic C
IV absorption in the core of the broad emission line is resolved for the first
time into four distinct kinematic components, which are all blue-shifted
relative to the systemic radial velocity of the host galaxy. Two components are
narrow (20 and 30 km/sec FWHM) and at small radial velocities (-90 and -30
km/sec respectively), and could arise from the interstellar medium or halo of
the host galaxy. The two broad components are centered at radial velocities of
-380 and -150 km/sec, have widths of 130 and 210 km/sec (FWHM) respectively,
and most likely arise in outflowing gas near the active nucleus. The cores of
the broad C IV absorption components are very close to zero intensity,
indicating that the absorption regions are extended enough to completely occult
the broad C IV emitting region (which is ~9 light days in extent). The total
column density of the C IV absorption is substantially larger than that
measured by Kriss et al. (1996a) from contemporaneous HUT spectra, but we agree
with their conclusion that the UV absorption is too strong to arise primarily
from the X-ray warm absorber region. The GHRS observations separated by six
months reveal no appreciable changes in the equivalent widths or radial
velocities of any of the absorption components. At present, we know of two
Seyfert galaxies, NGC 3516 and NGC 4151, with complex multiple absorption zones
that can remain stable in column density and velocity field over time scales of
months to years.
