Computer Science
Scientific paper
Jan 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996phdt.........4b&link_type=abstract
Thesis (PH.D.)--UNIVERSITY OF CALIFORNIA, RIVERSIDE, 1996.Source: Dissertation Abstracts International, Volume: 57-03, Section:
Computer Science
Scientific paper
The results which are presented in this manuscript include an outline of the development and use of Direct Linear Algebraic Deconvolution (DLAD) image reconstruction on the UCR Compton Double Scatter Gamma Ray Telescope data. This telescope is sensitive to the energy range of 1 to 30 MeV. Two sources (Crab Nebula and Pulsar and the Galactic Center) are emphasized in this paper. The northern hemisphere sources (Crab, etc.) were analyzed using data from a 30 September, 1989 UCR balloon-borne flight, and southern hemisphere sources (Galactic Center) were analyzed using data from an 15 April, 1988 UCR balloon flight. Monte Carlo simulation results are presented for discrete (and slightly diffuse) sources transversing the field-of-view of our Compton telescope for a typical non -pointing balloon flight observation. A method is described for producing source images in a fixed celestial coordinate system which are deconvolved from data obtained in a detector coordinate system where the source coordinates are continuously changing. This method has been applied to real data. The Crab Nebula was detected in the 3-10 and 10-30 MeV ranges at fluxes of rm 1.5 times 10^ {-4} phcdot cm^{-2} cdot s^{-1} and rm 1.1 times 10^{-4} phcdot cm^{-2}cdot s^ {-1}, respectively, with statistical significances of 1.2sigma and 1.7sigma , respectively. It is important to note that the method described in this dissertation for estimating the errors in the deconvolved fluxes (section 3.3) provides an underestimation of the significance of these results. Excess emission in the energy range from 1.7 to 1.9 MeV, believed to be due to 1.8 MeV ^ {26}Al de-exitation in the Galactic center and plane regions, was observed at the level of rm 1.1 times 10^{-4} phcdot cm^{-2}cdot s^ {-1} with a calculated significance of 1.4sigma. Due to the low statistical significance of these excesses, these fluxes should be considered upper limits.
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