  Massive Black Holes detected in the centers of many nearby galaxies show an
approximately linear relation with the luminosity of the host bulge, with the
black hole mass being 0.001-0.002 of the bulge mass. Previous work suggested
that black holes of active (Seyfert 1) galaxies follow a similar relation, but
apparently with a significantly lower value of $M_{\rm BH}/M_{\rm bulge}$
(Wandel 1999). New data show that this difference was mainly due to
overestimating the black hole mass in quiescent galaxies and overestimating the
bulge magnitude of Seyfert galaxies. Using new and updated data we show that
AGNs (Seyfert galaxies and quasars) follow the same BH-bulge relation as
ordinary (inactive) galaxies. We derive the BH-bulge relation for a sample of
55 AGNs and 35 quiescent galaxies, finding that broad line AGNs have an average
black hole/bulge mass fraction of $\sim 0.0015$ with a strong correlation (Mbh
~ Lbulge^{0.9\pm 0.16}). This BH-bulge relation is consistent with the BH-bulge
relation of quiescent galaxies and much tighter than previous results. Narrow
line AGNs appear to have a lower ratio, Mbh/Mbulge ~ 10^{-4}-10^{-3}. We find
this to be a more general feature, the BH/bulge ratio in AGNs being inversely
correlated with the emission-line width, implying a strong linear relation
between the size of the broad emission line region and the luminosity of the
bulge. Finally, combining AGNs with observed and estimated stellar velocity
dispersion, we find a significant correlation (Mbh ~ v^{3.5-5}), consistent
with that of quiescent galaxies.
