  We present black hole mass--bulge velocity dispersion relation for a complete
sample of 75 soft X-ray selected AGNs: 43 broad line Seyfert 1s and 32 narrow
line Seyfert 1s. We use luminosity and FWHM(H-beta) as surrogates for black
hole mass and FWHM([OIII]) as a surrogate for the bulge velocity dispersion. We
find that NLS1s lie below the M-BH - sigma relation of BLS1s, confirming the
Mathur et al. (2001) result. The statistical result is robust and not due to
any systematic measurement error. This has important consequences towards our
understanding of black hole formation and growth: black holes grow by accretion
in well formed bulges, possibly after a major merger. As they grow, they get
closer to the M-BH - sigma relation for normal galaxies. The accretion is
highest in the beginning and dwindles as the time goes by. Our result does not
support theories of M-BH - sigma relation in which the black hole mass is a
constant fraction of the bulge mass/ velocity dispersion at all times or those
in which bulge growth is controlled by AGN feedback.
