Bibcode
DOI
Srinivasan, R.; Boyle, P. J.; Buckley, J. H.; Carter-Lewis, D. A.; Catanese, M.; Cawley, M. F.; Colombo, E.; Fegan, D. J.; Finley, J. P.; Gaidos, J. A.; Bussons Gordo, J.; Hillas, A. M.; Krennrich, F.; Lamb, R. C.; Lessard, R. W.; McEnery, J. M.; Moriarty, P.; Quinn, J.; Rose, H. J.; Samuelson, F. W.; Sembroski, G.; Weekes, T. C.; Wilson, C.; Zweerink, J.
Referencia bibliográfica
Astrophysical Journal v.489, p.170
Fecha de publicación:
11
1997
Número de citas
20
Número de citas referidas
14
Descripción
PSR B1951+32 is a gamma -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 pulsar energy spectrum is
consistent with an unbroken power law with differential photon index of
-1.8 +/- 0.1 between 50 MeV and 10 GeV. 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
gamma -ray telescope at the Whipple Observatory on Mount 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.