Share Email Print

Proceedings Paper

New high-resolution gamma-ray burst detector: all-sky x-ray and gamma-ray astronomy monitor (AXGAM)
Author(s): Tumay O. Tumer; Terrence J. O'Neill; Kevin C. Hurley; Hakki Ogelman; Robert J. Paulos; Richard Charles Puetter; Eric J. Beuville; W.J. Hamilton; R Proctor
Format Member Price Non-Member Price
PDF $17.00 $21.00

Paper Abstract

A wide field-of-view, arcsecond imaging, high energy resolution x-ray and low energy gamma ray detector is proposed for a future space mission. It is specifically designed to monitor and study gamma ray bursts (GRBs) with high energy and angular resolution and also find counterparts at other wavelengths. Detection of GRBs requires wide field-of-view ((pi) to 2 (pi) field-of-view) and high sensitivity. This is achieved by using high quantum efficiency CdZnTe pixel detectors with a low energy threshold (few keV) to observe the larger flux levels at lower energies, and large effective area (625 to 1,000 cm2) per coded aperture imaging module. Counterpart searches can only be done with ultra high angular resolution detectors (10 to 30 arcsecond FWHM) which gives 1 to 5 arcsecond position determination especially for strong GRBs. A few arcsecond size error box is expected to contain at most one object observed at another wavelength. This will be achieved by using ultra high spatial resolution pixel detectors (100 by 100 microns) and a similar resolution coded aperture to achieve the required angular resolution. AXGAM also has two other important advantages over similar detectors: (1) excellent low energy response (greater than 1 keV) and (2) high energy resolution (less than 6% at 5.9 keV, less than 3% at 14 keV, less than 4% at 122 keV). The low energy range may provide important new information on GRBs and the high energy resolution is expected to help in the observation and identification of emission and absorption lines in the GRB spectrum. The effective energy range is planned to be 2 to 200 keV which is exceptionally wide for such a detector. AXGAM will be built in the form of a 'bucky ball' using a coded aperture mask in a semi-geodesic dome arrangement placed over a two-dimensional, high resolution CdZnTe pixel detector array using newly developed p-i-n detector technology. The p-i-n structure decreases the electron and hole trapping effect and increases energy resolution significantly. The major scientific goals of the proposed mission in addition to continuously monitoring gamma- ray bursts, is to observe AGNs, transient phenomena, isolated and binary pulsars, and solar flares. A space deployed AXGAM detector is expected to observe several hundred gamma ray bursts per year.

Paper Details

Date Published: 15 October 1997
PDF: 12 pages
Proc. SPIE 3114, EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy VIII, (15 October 1997); doi: 10.1117/12.283786
Show Author Affiliations
Tumay O. Tumer, Univ. of California/Riverside (United States)
Terrence J. O'Neill, Univ. of California/Riverside (United States)
Kevin C. Hurley, Univ. of California/Berkeley (United States)
Hakki Ogelman, Univ. of Wisconsin/Madison (United States)
Robert J. Paulos, Univ. of Wisconsin/Madison (United States)
Richard Charles Puetter, Univ of Cali / San Diego (United States)
Eric J. Beuville, Lawrence Berkley National Lab (United States)
W.J. Hamilton, Hughes Aircraft Co, (United States)
R Proctor, Gamma-Metrics (United States)

Published in SPIE Proceedings Vol. 3114:
EUV, X-Ray, and Gamma-Ray Instrumentation for Astronomy VIII
Oswald H. W. Siegmund; Mark A. Gummin, Editor(s)

© SPIE. Terms of Use
Back to Top
Sign in to read the full article
Create a free SPIE account to get access to
premium articles and original research
Forgot your username?