Very energy observations of PSR B1951+32

Details Very energy observations of PSR B1951+32 Very energy observations of PSR B1951+32

May 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aipc..410..592s&link_type=abstract

The fourth compton symposium. AIP Conference Proceedings, Volume 410, pp. 592-596 (1997).

Computer Science

Pulsars, Gamma-Ray, Gamma-Ray Sources, Gamma-Ray Bursts, Supernova Remnants

Scientific paper

PSR B1951+32 is a γ-ray pulsar detected by the Energetic Gamma Ray Experiment Telescope (EGRET) and identified with the 39.5 ms radio pulsar in the supernova remnant CTB 80. The EGRET data shows no evidence for a spectral turnover. Here we report on the first observations of PSR B1951+32 beyond 30 GeV. The observations were carried out with the 10 m γ-ray telescope at the Whipple Observatory on Mt. Hopkins, Arizona. In 8.1 hours of observation we find no evidence for steady or periodic emission from PSR B1951+32 above ~260 GeV. Flux upper limits are derived and compared with model extrapolations from lower energies and the predictions of emission models.

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