Much progress has been made in measuring black hole (BH) masses in
(non-active) galactic nuclei using the tight correlation between
stellar velocity dispersions (sigma) in galaxies and the mass of
their central BH. The use of this correlation in quasars, however,
is hampered by the difficulty in measuring sigma in host galaxies that
tend to be overpowered by their very bright nuclei. I discuss
results from a project that focuses on z~0.3 quasars suffering from
heavy extinction at shorter wavelengths. This makes it possible to
obtain clean spectra of the hosts in the spectral regions of interest, 
while broad lines (like H-alpha) are still visible at longer
wavelengths. We compare BH masses obtained from velocity dispersions
to those obtained from the BLR and thus probe the evolution of this
relation and BH growth with redshift and luminosity