  There remain several definitive gamma-ray pulsars that are as yet undetected
in the optical regime. A classic case is the pulsar PSR B1951+32, associated
with the complex CTB 80 SNR. Previous ground based high speed 2-d optical
studies have ruled out candidates to V ~ 24. Hester (2000a) has reported an
analysis of archival HST/WFPC2 observations of the CTB 80 complex which suggest
a compact synchrotron nebula coincident with the pulsar's radio position.
Performing a similar analysis, we have identified a possible optical
counterpart within this synchrotron nebula at V ~ 25.5 - 26, and another
optical counterpart candidate nearby at V ~ 24.5. We assess the reality of
these counterpart candidates in the context of existing models of pulsar
emission.
