Development of the hard x-ray monitor onboard WF-MAXI

Makoto Arimoto; Yoichi Yatsu; Nobuyuki Kawai; Hirokazu Ikeda; Atsushi Harayama; Shin'Ichiro Takeda; Tadayuki Takahashi; Hiroshi Tomida; Shiro Ueno; Masashi Kimura; Tatehiro Mihara; Motoko Serino; Hiroshi Tsunemi; Atsumasa Yoshida; Takanori Sakamoto; Tadayoshi Kohmura; Hitoshi Negoro; Yoshihiro Ueda

doi:10.1117/12.2054942

Development of the hard x-ray monitor onboard WF-MAXI

Makoto Arimoto^*, Yoichi Yatsu, Nobuyuki Kawai, Hirokazu Ikeda, Atsushi Harayama, Shin'Ichiro Takeda, Tadayuki Takahashi, Hiroshi Tomida, Shiro Ueno, Masashi Kimura, Tatehiro Mihara, Motoko Serino, Hiroshi Tsunemi, Atsumasa Yoshida, Takanori Sakamoto, Tadayoshi Kohmura, Hitoshi Negoro, Yoshihiro Ueda

^*Corresponding author for this work

Research output: Chapter in Book/Report/Conference proceeding › Conference contribution

3 Citations (Scopus)

Abstract

WF-MAXI is a mission to detect and localize X-ray transients with short-term variability as gravitational-wave (GW) candidates including gamma-ray bursts, supernovae etc. We are planning on starting observations by WF-MAXI to be ready for the initial operation of the next generation GW telescopes (e.g., KAGRA, Advanced LIGO etc.). WF-MAXI consists of two main instruments, Soft X-ray Large Solid Angle Camera (SLC) and Hard X-ray Monitor (HXM) which totally cover 0.7 keV to 1 MeV band. HXM is a multi-channel array of crystal scintillators coupled with APDs observing photons in the hard X-ray band with an effective area of above 100 cm². We have developed an analog application specific integrated circuit (ASIC) dedicated for the readout of 32-channel APDs' signals using 0.35 μm CMOS technology based on Open IP project and an analog amplifier was designed to achieve a low-noise readout. The developed ASIC showed a low-noise performance of 2080 e^- + 2.3 e^-/pF at root mean square and with a reverse-type APD coupled to a Ce:GAGG crystal a good FWHM energy resolution of 6.9% for 662 keV -rays.

Original language	English
Title of host publication	Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray
Publisher	SPIE
Volume	9144
ISBN (Electronic)	9780819496126
DOIs	https://doi.org/10.1117/12.2054942
Publication status	Published - 2014
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

Keywords

APD
ASIC
low noise
WF-MAXI
X-ray detectors

ASJC Scopus subject areas

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

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10.1117/12.2054942

Cite this

Arimoto, M., Yatsu, Y., Kawai, N., Ikeda, H., Harayama, A., Takeda, SI., Takahashi, T., Tomida, H., Ueno, S., Kimura, M., Mihara, T., Serino, M., Tsunemi, H., Yoshida, A., Sakamoto, T., Kohmura, T., Negoro, H., & Ueda, Y. (2014). Development of the hard x-ray monitor onboard WF-MAXI. In Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray (Vol. 9144). [91445Z] SPIE. https://doi.org/10.1117/12.2054942

Arimoto, M, Yatsu, Y, Kawai, N, Ikeda, H, Harayama, A, Takeda, SI, Takahashi, T, Tomida, H, Ueno, S, Kimura, M, Mihara, T, Serino, M, Tsunemi, H, Yoshida, A, Sakamoto, T, Kohmura, T, Negoro, H & Ueda, Y 2014, Development of the hard x-ray monitor onboard WF-MAXI. in Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray. vol. 9144, 91445Z, SPIE, Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray, Montreal, 14/6/22. https://doi.org/10.1117/12.2054942

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title = "Development of the hard x-ray monitor onboard WF-MAXI",

abstract = "WF-MAXI is a mission to detect and localize X-ray transients with short-term variability as gravitational-wave (GW) candidates including gamma-ray bursts, supernovae etc. We are planning on starting observations by WF-MAXI to be ready for the initial operation of the next generation GW telescopes (e.g., KAGRA, Advanced LIGO etc.). WF-MAXI consists of two main instruments, Soft X-ray Large Solid Angle Camera (SLC) and Hard X-ray Monitor (HXM) which totally cover 0.7 keV to 1 MeV band. HXM is a multi-channel array of crystal scintillators coupled with APDs observing photons in the hard X-ray band with an effective area of above 100 cm2. We have developed an analog application specific integrated circuit (ASIC) dedicated for the readout of 32-channel APDs' signals using 0.35 μm CMOS technology based on Open IP project and an analog amplifier was designed to achieve a low-noise readout. The developed ASIC showed a low-noise performance of 2080 e- + 2.3 e-/pF at root mean square and with a reverse-type APD coupled to a Ce:GAGG crystal a good FWHM energy resolution of 6.9% for 662 keV -rays.",

keywords = "APD, ASIC, low noise, WF-MAXI, X-ray detectors",

author = "Makoto Arimoto and Yoichi Yatsu and Nobuyuki Kawai and Hirokazu Ikeda and Atsushi Harayama and Shin'Ichiro Takeda and Tadayuki Takahashi and Hiroshi Tomida and Shiro Ueno and Masashi Kimura and Tatehiro Mihara and Motoko Serino and Hiroshi Tsunemi and Atsumasa Yoshida and Takanori Sakamoto and Tadayoshi Kohmura and Hitoshi Negoro and Yoshihiro Ueda",

year = "2014",

doi = "10.1117/12.2054942",

language = "English",

volume = "9144",

booktitle = "Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray",

publisher = "SPIE",

address = "United States",

note = "Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray ; Conference date: 22-06-2014 Through 26-06-2014",

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AU - Arimoto, Makoto

AU - Yatsu, Yoichi

AU - Kawai, Nobuyuki

AU - Ikeda, Hirokazu

AU - Harayama, Atsushi

AU - Takeda, Shin'Ichiro

AU - Takahashi, Tadayuki

AU - Tomida, Hiroshi

AU - Ueno, Shiro

AU - Kimura, Masashi

AU - Mihara, Tatehiro

AU - Serino, Motoko

AU - Tsunemi, Hiroshi

AU - Yoshida, Atsumasa

AU - Sakamoto, Takanori

AU - Kohmura, Tadayoshi

AU - Negoro, Hitoshi

AU - Ueda, Yoshihiro

PY - 2014

Y1 - 2014

N2 - WF-MAXI is a mission to detect and localize X-ray transients with short-term variability as gravitational-wave (GW) candidates including gamma-ray bursts, supernovae etc. We are planning on starting observations by WF-MAXI to be ready for the initial operation of the next generation GW telescopes (e.g., KAGRA, Advanced LIGO etc.). WF-MAXI consists of two main instruments, Soft X-ray Large Solid Angle Camera (SLC) and Hard X-ray Monitor (HXM) which totally cover 0.7 keV to 1 MeV band. HXM is a multi-channel array of crystal scintillators coupled with APDs observing photons in the hard X-ray band with an effective area of above 100 cm2. We have developed an analog application specific integrated circuit (ASIC) dedicated for the readout of 32-channel APDs' signals using 0.35 μm CMOS technology based on Open IP project and an analog amplifier was designed to achieve a low-noise readout. The developed ASIC showed a low-noise performance of 2080 e- + 2.3 e-/pF at root mean square and with a reverse-type APD coupled to a Ce:GAGG crystal a good FWHM energy resolution of 6.9% for 662 keV -rays.

AB - WF-MAXI is a mission to detect and localize X-ray transients with short-term variability as gravitational-wave (GW) candidates including gamma-ray bursts, supernovae etc. We are planning on starting observations by WF-MAXI to be ready for the initial operation of the next generation GW telescopes (e.g., KAGRA, Advanced LIGO etc.). WF-MAXI consists of two main instruments, Soft X-ray Large Solid Angle Camera (SLC) and Hard X-ray Monitor (HXM) which totally cover 0.7 keV to 1 MeV band. HXM is a multi-channel array of crystal scintillators coupled with APDs observing photons in the hard X-ray band with an effective area of above 100 cm2. We have developed an analog application specific integrated circuit (ASIC) dedicated for the readout of 32-channel APDs' signals using 0.35 μm CMOS technology based on Open IP project and an analog amplifier was designed to achieve a low-noise readout. The developed ASIC showed a low-noise performance of 2080 e- + 2.3 e-/pF at root mean square and with a reverse-type APD coupled to a Ce:GAGG crystal a good FWHM energy resolution of 6.9% for 662 keV -rays.

KW - APD

KW - ASIC

KW - low noise

KW - WF-MAXI

KW - X-ray detectors

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M3 - Conference contribution

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VL - 9144

BT - Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray

PB - SPIE

T2 - Space Telescopes and Instrumentation 2014: Ultraviolet to Gamma Ray

Y2 - 22 June 2014 through 26 June 2014

ER -

Development of the hard x-ray monitor onboard WF-MAXI

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Keywords

ASJC Scopus subject areas

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