Gamma-ray astronomy is generally viewed as an adjunct to cosmic ray physics. As such, the observation of very high energy gamma-rays will allow a new and complementary means of examining the origin and evolution of cosmic rays. However, at present the atmospheric Cerenkov technique (the technique by which very high energy gamma-rays are observed) is seriously hampered by limited flux sensitivity. Monte Carlo simulations suggest that the application of imaging to the atmospheric Cerenkov technique will provide a much needed increase in sensitivity. The successful application of imaging to very high energy gamma-ray observations of the Crab nebula will be discussed, as will improved techniques for calibration and noise rejection. These observations permit an improved estimate of the nebular magnetic field strength.
| Identifer | oai:union.ndltd.org:arizona.edu/oai:arizona.openrepository.com:10150/184235 |
| Date | January 1987 |
| Creators | GIBBS, KENNETH GERARD. |
| Contributors | Bowen, Theodore |
| Publisher | The University of Arizona. |
| Source Sets | University of Arizona |
| Language | English |
| Detected Language | English |
| Type | text, Dissertation-Reproduction (electronic) |
| Rights | Copyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author. |
Page generated in 0.0252 seconds