Observations of NP 0532 at 1000 to 10000 GeV gamma ray energies

Details Observations of NP 0532 at 1000 to 10000 GeV gamma ray energies Observations of NP 0532 at 1000 to 10000 GeV gamma ray energies

Nov 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974csgr.conf..301g&link_type=abstract

In ESRO The Context and Status of Gamma Ray Astronomy p 301-306 (SEE N75-25813 16-93)

Astronomy and Astrophysics

Astronomy

1

Cerenkov Radiation, Crab Nebula, Gamma Rays, Night Sky, Pulsars, Pulsed Radiation, Cosmic Ray Showers, Emission Spectra, Ground Based Control, Photomultiplier Tubes, Photon Density, Pulse Amplitude, Standard Deviation

Scientific paper

Observations of NP 0532 (Crab) pulsar were made at the Mount Hopkins high-energy gamma ray Observatory. The ground-based technique is based on the analysis of Cerenkov light emitted in the night sky by E or = 1000 GeV cosmic and electromagnetic air showers. Observations were made with photomultiplier tube and mirror configurations: (1) a single-beam technique that has an energy threshold of 1000 GeV but does not distinguish shower types, (2) a double-beam technique at a higher energy threshold that distinguishes cosmic ray and electromagnetic air showers, and (3) a single beam with a guard ring that discriminates against off-axis cosmic ray air showers. Preliminary results for the double-beam technique indicate the detection of a net pulsed flux. The width of the pulse is approximately 1 ms and lags the main pulse by 6 ms. A pulsed flux is implied that varies in phase relative to the optical pulsation and appears at 1000 to 10000 GeV energies as a new component with a relatively flat energy spectrum.

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