VERY-HIGH-ENERGY OBSERVATIONS OF PSR B1951+32

PSR B1951 + 32 is a gamma-ray pulsar detected by the Energetic Gamma R ay Experiment Telescope (EGRET) and identified with the 39.5 ms radio pulsar in the supernova remnant CTB 80. The pulsar energy spectrum is consistent with an unbroken power law with differential photon index o f -1.8 +/- 0.1 between 50 MeV and 10 GeV. The EGRET data shows no evid ence for a spectral turnover. Here we report on the first observations of PSR B1951 + 32 beyond 30 GeV. The observations were carried out wi th the 10 m gamma-ray telescope at the Whipple Observatory on Mount Ho pkins, Arizona. In 8.1 hours of observation we find no evidence for st eady or periodic emission from PSR B1951 + 32 above similar to 260 GeV , Flux upper limits are derived and compared with model extrapolations from lower energies and the predictions of emission models.