  The Far Ultraviolet Spectroscopic Explorer (FUSE) has surveyed a large sample
(> 100) of active galactic nuclei in the low-redshift universe (z < 1). Its
response at short wavelengths makes it possible to measure directly the far
ultraviolet spectral properties of quasistellar objects (QSOs) and Seyfert 1
galaxies at z < 0.3. Using archival FUSE spectra, we form a composite extreme
ultraviolet (EUV) spectrum of QSOs at z < 0.67. After consideration of many
possible sources of systematic error in our analysis, we find that the spectral
slope of the FUSE composite spectrum, \alpha= -0.56^+0.38_-0.28 for F_\nu
\propto \nu^\alpha, is significantly harder than the EUV (\lambda \lesssim 1200
A) portion of the composite spectrum of QSOs with z > 0.33 formed from archival
Hubble Space Telescope spectra, \alpha=-1.76 \pm 0.12. We identify several
prominent emission lines in the \fuse composite and find that the
high-ionization O VI and Ne VIII emission lines are enhanced relative to the
HST composite. Power law continuum fits to the individual FUSE AGN spectra
reveal a correlation between EUV spectral slope and AGN luminosity in the FUSE
and FUSE + HST samples in the sense that lower luminosity AGNs show harder
spectral slopes. We find an anticorrelation between the hardness of the EUV
spectral slope and AGN black hole mass, using estimates of this quantity found
in the literature. We interpret these results in the context of the well-known
anticorrelation between AGN luminosity and emission line strength, the Baldwin
effect, given that the median luminosity of the FUSE AGN sample is an order of
magnitude lower than that of the HST sample.
