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A Large-Area Gas-Čerenkov Detector for High-Energy Gamma-Ray Astronomy

Published online by Cambridge University Press:  14 August 2015

J. Delvaille ,
K. Greisen ,
D. Koch ,
B. McBreen ,
G. Fazio ,
D. Hearn  and
H. Helmken
J. Delvaille
Affiliation:
Cornell University, Ithaca, N. Y., U.S.A.
K. Greisen
Affiliation:
Cornell University, Ithaca, N. Y., U.S.A.
D. Koch
Affiliation:
Cornell University, Ithaca, N. Y., U.S.A.
B. McBreen
Affiliation:
Cornell University, Ithaca, N. Y., U.S.A.
G. Fazio
Affiliation:
Smithsonian Astrophysical Observatory, Cambridge, Mass., U.S.A.
D. Hearn
Affiliation:
Smithsonian Astrophysical Observatory, Cambridge, Mass., U.S.A.
H. Helmken
Affiliation:
Smithsonian Astrophysical Observatory, Cambridge, Mass., U.S.A.

Extract

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Experimental upper limits of the high-energy gamma-ray flux (above 100 MeV) from point sources are about 10−5 cm−2 s−1, and realistic theoretical predictions for the strongest sources are an order of magnitude lower than this, while the diffuse background flux is about 4 × 10−5 cm−2 s−1 sr−1 in space, and 100 times higher at balloon altitudes. To meet the need for instrumental sensitivity and angular resolution adequate to measure the small but important gamma-ray source strengths, a telescope of large area (5 m2) and fine angular discrimination (0.5 deg at 300 MeV, 0.3 deg at energies above 1 GeV) has been developed.

Type
Part I: Gamma-Ray Astronomy
Information
Symposium - International Astronomical Union , Volume 41: New Technique in Space Astronomy , 1971 , pp. 75 - 76
Copyright
Copyright © Reidel 1971