  Scaling relations between central black hole (BH) mass and host galaxy
properties are of fundamental importance to studies of BH and galaxy evolution
throughout cosmic time. Here we investigate the relationship between BH mass
and host galaxy total stellar mass using a sample of 262 broad-line active
galactic nuclei (AGN) in the nearby Universe (z < 0.055), as well as 79
galaxies with dynamical BH masses. The vast majority of our AGN sample is
constructed using Sloan Digital Sky Survey spectroscopy and searching for
Seyfert-like narrow-line ratios and broad H-alpha emission. BH masses are
estimated using standard virial techniques. We also include a small number of
dwarf galaxies with total stellar masses M_stellar < 10^9.5 Msun and a
sub-sample of the reverberation-mapped AGNs. Total stellar masses of all 341
galaxies are calculated in the most consistent manner feasible using
color-dependent mass-to-light ratios. We find a clear correlation between BH
mass and total stellar mass for the AGN host galaxies, with M_BH proportional
to M_stellar, similar to that of early-type galaxies with dynamically-detected
BHs. However, the relation defined by the AGNs has a normalization that is
lower by more than an order of magnitude, with a BH-to-total stellar mass
fraction of M_BH/M_stellar ~ 0.025% across the stellar mass range 10^8 <
M_stellar/Msun < 10^12. This result has significant implications for studies at
high redshift and cosmological simulations in which stellar bulges cannot be
resolved.
