  We used the widths of H$\beta$ and [OIII] emission lines to investigate the
black hole--bulge relation in radio-loud AGNs, radio-quiet AGNs and NLS1s. The
central black hole mass, $M_{bh}$, is estimated from the H$\beta$ line width
and the optical luminosity, and the bulge velocity dispersion, $\sigma$, is
directly from the width of [OIII] line. We found that the radio-quiet AGNs
follow the established $M_{bh}-\sigma$ relationship in nearby inactive
galaxies, while the radio-loud AGNs and NLS1s deviate from this relationship.
There are two plausible interpretations for the deviation of radio-loud AGNs.
One is that the size of broad line regions (BLRs) emitting H$\beta$ line is
overestimated because of the overestimation of optical luminosity, the other is
that the dynamics of BLRs and/or narrow line regions (NLRs) in radio-loud AGNs
is different from that in radio-quiet AGNs. The deviation of NLS1s may be due
to the small inclination of BLRs to the line of sight or the reliability of
[OIII] line width as the indicator of stellar velocity dispersion because of
its complex multiple components.
