Development of BGO active shield for the ASTRO-H soft Gamma-ray Detector

Y. Hanabata, Y. Fukazawa, K. Yamaoka, H. Tajima, Jun Kataoka, K. Nakazawa, H. Takahashi, T. Mizuno, M. Ohno, M. Kokubun, T. Takahashi, S. Watanabe, M. Tashiro, Y. Terada, C. Sasaki, K. Nakajima, T. Mizushima

    Research output: Chapter in Book/Report/Conference proceedingConference contribution

    Abstract

    Soft Gamma-ray Detector (SGD:40-600 keV) will be mounted on the 6th Japanese X-ray observatory ASTRO-H to be launched in 2014. The main part of the SGD is a Compton camera with a narrow field of view and surrounded by BGO active shields (SGD-BGO). Via this combination, the SGD can achieve sensitivity more than ten times superior to the Suzaku/HXD. The BGO active shield will also function as a gamma-ray burst monitor as proven by the wide-band all-sky monitor (WAM) of the Suzaku/HXD. Avalanche Photodiodes (APDs) are used to read out scintillation lights from the BGO. The size of the former also means we need to focus on collecting light from large, complex-shaped BGO blocks. The significant leakage current of the APD means a lower temperature is preferred to minimize the noise while a higher temperature is preferred to simplify the cooling system. To optimize the BGO shape and the operating temperature, we tested the performance of the BGO readout system with various BGO shapes under different operating temperatures. We also apply waveform sampling by flash-ADC and digital filter instead of a conventional analog filter and ADC scheme to reduce the space and power of the circuit with increased flexibilities. As an active shield, we need to achieve a threshold level of 50-100 keV. Here, we report on the studies of threshold energy of active shield under various conditions and signal processings.

    Original languageEnglish
    Title of host publicationProceedings of SPIE - The International Society for Optical Engineering
    Volume7732
    DOIs
    Publication statusPublished - 2010
    EventSpace Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray - San Diego, CA
    Duration: 2010 Jun 282010 Jul 2

    Other

    OtherSpace Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray
    CitySan Diego, CA
    Period10/6/2810/7/2

    Fingerprint

    Avalanche Photodiode
    Gamma Rays
    operating temperature
    Gamma rays
    avalanches
    photodiodes
    monitors
    Monitor
    Detector
    gamma rays
    Detectors
    filters
    Gamma-ray Bursts
    Leakage Current
    Avalanche photodiodes
    digital filters
    Digital Filter
    thresholds
    Scintillation
    detectors

    Keywords

    • Active shield
    • ASTRO-H
    • SGD
    • Soft gamma-rays

    ASJC Scopus subject areas

    • Applied Mathematics
    • Computer Science Applications
    • Electrical and Electronic Engineering
    • Electronic, Optical and Magnetic Materials
    • Condensed Matter Physics

    Cite this

    Hanabata, Y., Fukazawa, Y., Yamaoka, K., Tajima, H., Kataoka, J., Nakazawa, K., ... Mizushima, T. (2010). Development of BGO active shield for the ASTRO-H soft Gamma-ray Detector. In Proceedings of SPIE - The International Society for Optical Engineering (Vol. 7732). [77323B] https://doi.org/10.1117/12.856745

    Development of BGO active shield for the ASTRO-H soft Gamma-ray Detector. / Hanabata, Y.; Fukazawa, Y.; Yamaoka, K.; Tajima, H.; Kataoka, Jun; Nakazawa, K.; Takahashi, H.; Mizuno, T.; Ohno, M.; Kokubun, M.; Takahashi, T.; Watanabe, S.; Tashiro, M.; Terada, Y.; Sasaki, C.; Nakajima, K.; Mizushima, T.

    Proceedings of SPIE - The International Society for Optical Engineering. Vol. 7732 2010. 77323B.

    Research output: Chapter in Book/Report/Conference proceedingConference contribution

    Hanabata, Y, Fukazawa, Y, Yamaoka, K, Tajima, H, Kataoka, J, Nakazawa, K, Takahashi, H, Mizuno, T, Ohno, M, Kokubun, M, Takahashi, T, Watanabe, S, Tashiro, M, Terada, Y, Sasaki, C, Nakajima, K & Mizushima, T 2010, Development of BGO active shield for the ASTRO-H soft Gamma-ray Detector. in Proceedings of SPIE - The International Society for Optical Engineering. vol. 7732, 77323B, Space Telescopes and Instrumentation 2010: Ultraviolet to Gamma Ray, San Diego, CA, 10/6/28. https://doi.org/10.1117/12.856745
    Hanabata Y, Fukazawa Y, Yamaoka K, Tajima H, Kataoka J, Nakazawa K et al. Development of BGO active shield for the ASTRO-H soft Gamma-ray Detector. In Proceedings of SPIE - The International Society for Optical Engineering. Vol. 7732. 2010. 77323B https://doi.org/10.1117/12.856745
    Hanabata, Y. ; Fukazawa, Y. ; Yamaoka, K. ; Tajima, H. ; Kataoka, Jun ; Nakazawa, K. ; Takahashi, H. ; Mizuno, T. ; Ohno, M. ; Kokubun, M. ; Takahashi, T. ; Watanabe, S. ; Tashiro, M. ; Terada, Y. ; Sasaki, C. ; Nakajima, K. ; Mizushima, T. / Development of BGO active shield for the ASTRO-H soft Gamma-ray Detector. Proceedings of SPIE - The International Society for Optical Engineering. Vol. 7732 2010.
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    abstract = "Soft Gamma-ray Detector (SGD:40-600 keV) will be mounted on the 6th Japanese X-ray observatory ASTRO-H to be launched in 2014. The main part of the SGD is a Compton camera with a narrow field of view and surrounded by BGO active shields (SGD-BGO). Via this combination, the SGD can achieve sensitivity more than ten times superior to the Suzaku/HXD. The BGO active shield will also function as a gamma-ray burst monitor as proven by the wide-band all-sky monitor (WAM) of the Suzaku/HXD. Avalanche Photodiodes (APDs) are used to read out scintillation lights from the BGO. The size of the former also means we need to focus on collecting light from large, complex-shaped BGO blocks. The significant leakage current of the APD means a lower temperature is preferred to minimize the noise while a higher temperature is preferred to simplify the cooling system. To optimize the BGO shape and the operating temperature, we tested the performance of the BGO readout system with various BGO shapes under different operating temperatures. We also apply waveform sampling by flash-ADC and digital filter instead of a conventional analog filter and ADC scheme to reduce the space and power of the circuit with increased flexibilities. As an active shield, we need to achieve a threshold level of 50-100 keV. Here, we report on the studies of threshold energy of active shield under various conditions and signal processings.",
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    AU - Kataoka, Jun

    AU - Nakazawa, K.

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    AU - Mizuno, T.

    AU - Ohno, M.

    AU - Kokubun, M.

    AU - Takahashi, T.

    AU - Watanabe, S.

    AU - Tashiro, M.

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    AU - Sasaki, C.

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