  A deep imaging survey covering the entire $23\arcmin$ diameter of the old
open cluster M67 to $V = 25$ has been carried out using the mosaic imager
(UHCam) on the Canada-France-Hawaii Telescope. The cluster color-magnitude
diagram (CMD) can be traced from stars on its giant branch at $M_{V} = +1$ down
through main sequence stars at least as faint as $M_{V} = 13.5$. Stars this low
in luminosity have masses below $0.15 M_{\odot}$. A modest white dwarf (WD)
cooling sequence is also observed commencing slightly fainter than $M_V = 10$
and, after correction for background galaxy and stellar field contamination,
terminating near $M_V = 14.6$. The observed WDs follow quite closely a
theoretical cooling sequence for $0.7 M_{\odot}$ pure carbon core WDs with
hydrogen-rich atmospheres (DA WDs). The cooling time to an $M_V$ of 14.6 for
such WDs is 4.3 Gyr which we take as the WD cooling age of the cluster. A fit
of a set of isochrones to the cluster CMD indicates a turnoff age of 4.0 Gyr.
The excellent agreement between these results suggests that ages derived from
white dwarf cooling should be considered as reliable as those from other dating
techniques. The WDs currently contribute about 9% of the total cluster mass but
the number seen appears to be somewhat low when compared with the number of
giants observed in the cluster.
