  We have applied a new method to analyze the horizontal branch (HB) morphology
in relation to the distribution of stars near the red giant branch (RGB) tip
for the globular clusters M22, M5, M68, M107, M72, M92, M3 and 47 Tuc. This new
method permits determination of the cluster ages to greater accuracy than
conventional isochrone fitting. Using the method in conjunction with our new
high-quality photometric data for RGB and HB stars in the first five of these
clusters, we discuss the origins of the spread in color on the HB and its
relation to the `second parameter' problem. The oldest clusters in our sample
are found to have relatively low ages ($13.5 \pm 2$ Gyr).
  A 1$\sigma$ uncertainty in each of the parameters of mass and helium content
combined with the effects of helium diffusion gives a lower limit for the age
of the oldest clusters of 9.7 Gyr.
