  Currently there are two main techniques for independently determining the
ages of stellar populations: main sequence evolution theory (via cluster
isochrones) and white dwarf cooling theory. Open clusters provide the ideal
environment for the calibration of these two clocks. Because current techniques
to derive cluster ages from white dwarfs are observationally challenging, we
discuss the feasibility of determining white dwarf ages from the brighter white
dwarfs alone. This would eliminate the requirement of observing the coolest
(i.e., faintest) white dwarfs. We discuss our method for testing this new idea,
as well as the required photometric precision and prior constraints on
metallicity, distance, and reddening. We employ a new Bayesian statistical
technique to obtain and interpret results.
