  Using time-resolved two-dimensional aperture photometry we have put upper
limits on the pulsed emission from two proposed optical counterparts for PSR
B1951+32. Our pulsed upper limits of m_{vpulsed}>23.3, m_{bpulsed}>24.4$, for
the first candidate and m_{vpulsed}>23.6$, m_{bpulsed}>24.3 for the second,
make it unlikely that either of these is, in fact, the pulsar. We discuss three
further candidates, but also reject these on the basis of timing results. A
search of a 5.5arcs x 5.5arcs area centred close to these stars failed to find
any significant pulsations at the reported pulsar period.
