  Recent hard X-ray spectroscopy of active galactic nuclei has strongly
suggested that double-peaked, very broad Fe K emission arises from an accretion
disk around the central engine. Model fitting of the observed Fe K emission
line profile makes it possible to estimate a probable inclination angle of the
accretion disk. In order to study the geometrical relationship between the
accretion disk and broad emission-line regions (BLRs), we investigate the
correlation between the inclination angle of the accretion disk and the
velocity width of BLRs for 18 type-1 Seyfert galaxies. We found that there may
be a negative correlation between them, i.e., Seyfert nuclei with a more
face-on accretion disk tend to have larger BLR velocity widths, suggesting that
the BLRs are not coplanar with respect to the accretion disk. The most probable
interpretation may be that the BLRs arise from outer parts ({\it r} $\sim$ 0.01
pc) of a warped accretion disk illuminated by the central engine.
