Abstract
The Soft Gamma-ray Detector (SGD) is a Si/CdTe Compton telescope surrounded by a thick BGO active shield and is scheduled to be onboard the ASTRO-H satellite when it is launched in 2015. The SGD covers the energy range from 40 to 600 keV with high sensitivity, which allows us to study nonthermal phenomena in the universe. The SGD uses a Compton camera with the narrow field-of-view (FOV) concept to reduce the non-Xray background (NXB) and improve the sensitivity. Since the SGD is essentially a nonimaging instrument, it also has to cope with the cosmic X-ray background (CXB) within the FOV. The SGD adopts passive shields called "fine collimators" (FCs) to restrict the FOV to ≤ 0.6° for low-energy photons (≤ 100 keV), which reduces contamination from CXB to less than what is expected due to NXB. Although the FC concept was already adopted by the Hard X-ray Detector onboard Suzaku, FCs for the SGD are about four times larger in size and are technically more difficult to operate. We developed FCs for the SGD and confirmed that the prototypes function as required by subjecting them to an X-ray test and environmental tests, such as vibration tests. We also developed an autocollimator system, which uses visible light to determine the transmittance and the optical axis, and calibrated it against data from the X-ray test. The acceptance tests of flight models started in December 2013: five out of six FCs were deemed acceptable, and one more unit is currently being produced. The activation properties were studied based on a proton-beam test and the results were used to estimate the in-orbit NXB.
| Original language | English |
|---|---|
| Title of host publication | Space Telescopes and Instrumentation 2014 |
| Subtitle of host publication | Ultraviolet to Gamma Ray |
| Publisher | SPIE |
| Volume | 9144 |
| ISBN (Electronic) | 9780819496126 |
| DOIs | |
| Publication status | Published - 2014 Jan 1 |
| Externally published | Yes |
| Event | Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray - Montreal Duration: 2014 Jun 22 → 2014 Jun 26 |
Other
| Other | Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray |
|---|---|
| City | Montreal |
| Period | 14/6/22 → 14/6/26 |
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Keywords
- activation
- collimator
- cosmic X-ray background
- Hard X-rays
- soft gamma-rays
ASJC Scopus subject areas
- Electronic, Optical and Magnetic Materials
- Condensed Matter Physics
- Computer Science Applications
- Applied Mathematics
- Electrical and Electronic Engineering
Cite this
Development and calibration of fine collimators for the ASTRO-H Soft Gamma-ray Detector. / Mizuno, T.; Kimura, D.; Fukazawa, Y.; Furui, S.; Goto, K.; Hayashi, T.; Kawabata, K. S.; Kawano, T.; Kitamura, Y.; Shirakawa, H.; Tanabe, T.; Makishima, K.; Nakajima, K.; Nakazawa, K.; Fukuyama, T.; Ichinohe, Y.; Ishimura, Kosei; Ohta, M.; Sato, T.; Takahashi, T.; Uchida, Y.; Watanabe, S.; Ishibashi, K.; Sakanobe, K.; Matsumoto, H.; Miyazawa, T.; Mori, H.; Sakai, M.; Tajima, H.
Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray. Vol. 9144 SPIE, 2014. 91445F.Research output: Chapter in Book/Report/Conference proceeding › Conference contribution
}
TY - GEN
T1 - Development and calibration of fine collimators for the ASTRO-H Soft Gamma-ray Detector
AU - Mizuno, T.
AU - Kimura, D.
AU - Fukazawa, Y.
AU - Furui, S.
AU - Goto, K.
AU - Hayashi, T.
AU - Kawabata, K. S.
AU - Kawano, T.
AU - Kitamura, Y.
AU - Shirakawa, H.
AU - Tanabe, T.
AU - Makishima, K.
AU - Nakajima, K.
AU - Nakazawa, K.
AU - Fukuyama, T.
AU - Ichinohe, Y.
AU - Ishimura, Kosei
AU - Ohta, M.
AU - Sato, T.
AU - Takahashi, T.
AU - Uchida, Y.
AU - Watanabe, S.
AU - Ishibashi, K.
AU - Sakanobe, K.
AU - Matsumoto, H.
AU - Miyazawa, T.
AU - Mori, H.
AU - Sakai, M.
AU - Tajima, H.
PY - 2014/1/1
Y1 - 2014/1/1
N2 - The Soft Gamma-ray Detector (SGD) is a Si/CdTe Compton telescope surrounded by a thick BGO active shield and is scheduled to be onboard the ASTRO-H satellite when it is launched in 2015. The SGD covers the energy range from 40 to 600 keV with high sensitivity, which allows us to study nonthermal phenomena in the universe. The SGD uses a Compton camera with the narrow field-of-view (FOV) concept to reduce the non-Xray background (NXB) and improve the sensitivity. Since the SGD is essentially a nonimaging instrument, it also has to cope with the cosmic X-ray background (CXB) within the FOV. The SGD adopts passive shields called "fine collimators" (FCs) to restrict the FOV to ≤ 0.6° for low-energy photons (≤ 100 keV), which reduces contamination from CXB to less than what is expected due to NXB. Although the FC concept was already adopted by the Hard X-ray Detector onboard Suzaku, FCs for the SGD are about four times larger in size and are technically more difficult to operate. We developed FCs for the SGD and confirmed that the prototypes function as required by subjecting them to an X-ray test and environmental tests, such as vibration tests. We also developed an autocollimator system, which uses visible light to determine the transmittance and the optical axis, and calibrated it against data from the X-ray test. The acceptance tests of flight models started in December 2013: five out of six FCs were deemed acceptable, and one more unit is currently being produced. The activation properties were studied based on a proton-beam test and the results were used to estimate the in-orbit NXB.
AB - The Soft Gamma-ray Detector (SGD) is a Si/CdTe Compton telescope surrounded by a thick BGO active shield and is scheduled to be onboard the ASTRO-H satellite when it is launched in 2015. The SGD covers the energy range from 40 to 600 keV with high sensitivity, which allows us to study nonthermal phenomena in the universe. The SGD uses a Compton camera with the narrow field-of-view (FOV) concept to reduce the non-Xray background (NXB) and improve the sensitivity. Since the SGD is essentially a nonimaging instrument, it also has to cope with the cosmic X-ray background (CXB) within the FOV. The SGD adopts passive shields called "fine collimators" (FCs) to restrict the FOV to ≤ 0.6° for low-energy photons (≤ 100 keV), which reduces contamination from CXB to less than what is expected due to NXB. Although the FC concept was already adopted by the Hard X-ray Detector onboard Suzaku, FCs for the SGD are about four times larger in size and are technically more difficult to operate. We developed FCs for the SGD and confirmed that the prototypes function as required by subjecting them to an X-ray test and environmental tests, such as vibration tests. We also developed an autocollimator system, which uses visible light to determine the transmittance and the optical axis, and calibrated it against data from the X-ray test. The acceptance tests of flight models started in December 2013: five out of six FCs were deemed acceptable, and one more unit is currently being produced. The activation properties were studied based on a proton-beam test and the results were used to estimate the in-orbit NXB.
KW - activation
KW - collimator
KW - cosmic X-ray background
KW - Hard X-rays
KW - soft gamma-rays
UR - http://www.scopus.com/inward/record.url?scp=84922551407&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84922551407&partnerID=8YFLogxK
U2 - 10.1117/12.2054649
DO - 10.1117/12.2054649
M3 - Conference contribution
AN - SCOPUS:84922551407
VL - 9144
BT - Space Telescopes and Instrumentation 2014
PB - SPIE
ER -