  The UV to soft X-rays of luminous AGNs dominate their bolometric luminosity,
driven by an accretion-powered dynamo at the center. These photons ionize the
surrounding gas, thereby providing clues to fueling and exhaust. Two sets of
important relationships - neither of them understood - link the continuum and
gas properties. (i) Boroson & Green's `eigenvector 1' relationships: Steeper
soft X-ray spectra are clearly related to narrower Hbeta emission and stronger
optical Fe II emission from the BLR, and weaker [O III] 5007 from the NLR. We
show that these relationships extend to UV spectra: narrower C III] 1909,
stronger low ionization lines, larger Si III] 1892/C III] 1909 (a density
indicator), weaker C IV 1549 but stronger higher-ionization N V 1240. We
speculate that high accretion rates are linked to high columns of dense (1e10 -
1e11 cm-3), nitrogen-enhanced, low-ionization gas from nuclear starbursts.
Linewidth, inverse Fe II-[O III] and inverse Fe II-C IV relationships hint at
the geometrical arrangement of this gas. (ii) The Baldwin effect (inverse
equivalent width - luminosity relationships): Our correlation analyses suggest
that these are independent of the above eigenvector 1 relationships. The
eigenvector 1 relationships can therefore be used in future work, to reduce
scatter in the Baldwin relationships, perhaps fulfilling the dream of using the
Baldwin effect for cosmological studies.
