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Proceedings Paper

Wide-field hard x-ray survey telescope: ProtoEXIST1
Author(s): J. Hong; J. E. Grindlay; N. Chammas; B. Allen; A. Copete; B. Said; M. Burke; J. Howell; T. Gauron; R. G. Baker; S. D. Barthelmy; S. Sheikh; N. Gehrels; W. R. Cook; J. A. Burnham; F. A. Harrison; J. Collins; S. Labov; A. Garson; H. Krawczynski
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Paper Abstract

We report our progress on the development of pixellated imaging CZT detector arrays for our first-generation balloon-borne wide-field hard X-ray (20 - 600 keV) telescope, ProtoEXIST1. Our ProtoEXIST program is a pathfinder for the High Energy Telescope (HET) on the Energetic X-ray Imaging Survey telescope (EXIST), a proposed implementation of the Black Hole Finder Probe. ProtoEXIST1 consists of four independent coded-aperture telescopes with close-tiled (~0.4 mm gaps) CZT detectors that preserve their 2.5mm pixel pitch. Multiple shielding/field-of-view configurations are planned to identify optimal geometry for the HET in EXIST. The primary technical challenge in ProtoEXIST is the development of large area, close-tiled modules of imaging CZT detectors (1000 cm2 for ProtoEXIST1), with all readout and control systems for the ASIC readout vertically stacked. We describe the overall telescope configuration of ProtoEXIST1 and review the current development status of the CZT detectors, from individual detector crystal units (DCUs) to a full detector module (DM). We have built the first units of each component for the detector plane and have completed a few Rev2 DCUs (2x2 cm2), which are under a series of tests. Bare DCUs (pre-crystal bonding) show high, uniform ASIC yield (~70%) and ~30% reduction in electronics noise compared to the Rev1 equivalent. A Rev1 DCU already achieved ~1.2% FWHM at 662 keV, and preliminary analysis of the initial radiation tests on a Rev2 DCU shows ~ 4 keV FWHM at 60 keV (vs. 4.7 keV for Rev1). We therefore expect about ≤1% FWHM at 662 keV with the Rev2 detectors.

Paper Details

Date Published: 21 September 2007
PDF: 11 pages
Proc. SPIE 6706, Hard X-Ray and Gamma-Ray Detector Physics IX, 67060B (21 September 2007); doi: 10.1117/12.736110
Show Author Affiliations
J. Hong, Harvard-Smithsonian Ctr. for Astrophysics (United States)
J. E. Grindlay, Harvard-Smithsonian Ctr. for Astrophysics (United States)
N. Chammas, Harvard-Smithsonian Ctr. for Astrophysics (United States)
B. Allen, Harvard-Smithsonian Ctr. for Astrophysics (United States)
A. Copete, Harvard-Smithsonian Ctr. for Astrophysics (United States)
B. Said, Harvard-Smithsonian Ctr. for Astrophysics (United States)
M. Burke, Harvard-Smithsonian Ctr. for Astrophysics (United States)
J. Howell, Harvard-Smithsonian Ctr. for Astrophysics (United States)
T. Gauron, Harvard-Smithsonian Ctr. for Astrophysics (United States)
R. G. Baker, NASA Goddard Space Flight Ctr. (United States)
S. D. Barthelmy, NASA Goddard Space Flight Ctr. (United States)
S. Sheikh, NASA Goddard Space Flight Ctr. (United States)
N. Gehrels, NASA Goddard Space Flight Ctr. (United States)
W. R. Cook, California Institute of Technology (United States)
J. A. Burnham, California Institute of Technology (United States)
F. A. Harrison, California Institute of Technology (United States)
J. Collins, Lawrence Livermore National Lab. (United States)
S. Labov, Lawrence Livermore National Lab. (United States)
A. Garson, Washington Univ. in St. Louis (United States)
H. Krawczynski, Washington Univ. in St. Louis (United States)


Published in SPIE Proceedings Vol. 6706:
Hard X-Ray and Gamma-Ray Detector Physics IX
Ralph B. James; Arnold Burger; Larry A. Franks, Editor(s)

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