A search for TeV γ-ray emission from binary systems
Abstract
A survey of six binary systems containing pulsars was conducted with the intention of detecting galactic sources of very high energy γ-ray emission. Observations were made with the Whipple 10 m Imaging Atmospheric Čerenkov Telescope located in southern Arizona primarily during the 1998 and 1999 observing seasons. Standard analysis techniques were applied to all sources to search for steady, unpulsed emission. Periodic tests were performed to search for emission correlated with both the orbital and spin phases, where appropriate. Results of analyses indicate that these binaries do not emit detectable levels of very high energy photons within the sensitivity limits of our telescope. Flux upper limits for both steady and pulsed emission fail to constrain emission predictions of the polar cap and shock acceleration models. In order to detect emission from these binary systems, and to place more restrictive constraints on these models, instruments with much greater sensitivity operating at much lower energy thresholds (such as those currently in development) are required.
Degree
Ph.D.
Advisors
Finley, Purdue University.
Subject Area
Astronomy|Astrophysics
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