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 m _ { V } \sim 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 m _ { V } \sim 25.5 - 26 , and another optical counterpart candidate nearby at m _ { V } \sim 24.5 .
We assess the reality of these counterpart candidates in the context of existing models of pulsar emission .