  The methodology involved in deriving the Hubble Constant via the calibration
of the corrected peak luminosities of Type Ia supernovae (SNe) is reviewed. We
first present a re-analysis of the Calan-Tololo (C-T) and Center for
Astrophysics (CfA) Type Ia SN surveys. Bivariate linear least squares and
quadratic boot-strapped fits in peak apparent magnitude and light curve shape
are employed to correct this heterogeneous sample of peak apparent magnitudes,
resulting in an homogeneous (and excellent) secondary distance indicator: the
so-called corrected peak luminosity. We next provide an empirical calibration
for this corrected luminosity, using Cepheid-based distances for seven nearby
spiral galaxies host to Type Ia SNe. Included in this sample is the
spectroscopically peculiar SN 1991T (in NGC 4527), whose corrected peak
luminosity is shown to be indistinguishable from that of so-called ``normal''
SNe. A robust value of the Hubble Constant is derived and shown to be
H0=73+/-2(r)+/-7(s) km/s/Mpc.
