Development and performance of Kyoto's x-ray astronomical SOI pixel (SOIPIX) sensor

Tsuru, Takeshi Go; Matsumura, Hideaki; Takeda, Ayaki; Tanaka, Takaaki; Nakashima, Shinya; Arai, Y.; Mori, Koji; Takenaka, Ryota; Nishioka, Yusuke; Kohmura, Takayoshi; Hatsui, Takaki; Kameshima, Takashi; Ozaki, Kyosuke; Kohmura, Yoshiki; Wagai, Tatsuya; Takei, Dai; Kawahito, Shoji; Kagawa, Keiichiro; Yasutomi, Keita; Kamehama, Hiroki; Shrestha, Sumeet

doi:10.1117/12.2057158

Cited by 17 publications

(12 citation statements)

References 15 publications

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“…Since the readout speed of the X-ray CCD is about several seconds, it is not suitable for the observation of the celestial bodies varying in a short time of several milliseconds. Therefore, we have developed XRPIX (X-Ray soiPIXel) which is an event-driven pixel detector using SOI (Silicon On Insulator) technology as a detector for future wide band X-ray astronomical satellites [1][2][3][4][5][6][7][8][9][10]. By implementing the trigger output function in each pixel, XR-PIX can selectively read out only the signal of the X-ray event and can obtain high time resolution of several microseconds.…”

Section: Introductionmentioning

confidence: 99%

X-ray response evaluation in subpixel level for X-ray SOI pixel detectors

Negishi

Kohmura

Hagino

et al. 2019

Nuclear Instruments and Methods in Physics Research Section A:

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We have been developing event-driven SOI Pixel Detectors, named "XRPIX" (X-Ray soiPIXel) based on the silicon-on-insulator (SOI) pixel technology, for the future X-ray astronomical satellite with wide band coverage from 0.5 keV to 40 keV. XRPIX has event trigger output function at each pixel to acquire a good time resolution of a few µs and has Correlated Double Sampling function to reduce electric noises. The good time resolution enables the XRPIX to reduce Non X-ray Background in the high energy band above 10 keV drastically by using anti-coincidence technique with active shield counters surrounding XRPIX. In order to increase the soft X-ray sensitivity, it is necessary to make the dead layer on the X-ray incident surface as thin as possible. Since XRPIX1b, which is a device at the initial stage of development, is a front-illuminated (FI) type of XRPIX, low energy X-ray photons are absorbed in the 8 µm thick circuit layer, lowering the sensitivity in the soft X-ray band. Therefore, we developed a back-illuminated (BI) device XRPIX2b, and confirmed high detection efficiency down to 2.6 keV, below which the efficiency is affected by the readout noise. In order to further improve the detection efficiency in the soft X-ray band, we developed a backilluminated device XRPIX3b with lower readout noise. In this work, we irradiated 2-5 keV X-ray beam collimated to 4 µmφ to the sensor layer side of the XRPIX3b at 6 µm pitch. In this paper, we reported the uniformity of the relative detection efficiency, gain and energy resolution in the subpixel level for the first time. We also confirmed that the variation in the relative detection efficiency at the subpixel level reported by Matsumura et al.[1] has improved.

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Section: Introductionmentioning

confidence: 99%

X-ray response evaluation in subpixel level for X-ray SOI pixel detectors

Negishi

Kohmura

Hagino

et al. 2019

Nuclear Instruments and Methods in Physics Research Section A:

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“…Figure 4 left shows a schematic view of the WHXI focal plane part. The major difference between the HXI and WHXI is that whereas the HXI consists of four layers of double-sided Si strip detectors (DSSDs) and a single layer of CdTe double-sided strip (DSD) detector [9], the WHXI replaces the former with a single SOI-CMOS pixel detector (SOIPIX) [10,11]. A low readout noise achievable by a SOIPIX is expected to lower the low-energy threshold down to 1 keV and to provide a broadband energy response required for the focal-plane detector of FORCE.…”

Section: Pos(multif2017)077mentioning

confidence: 99%

Focusing On Relativistic universe and Cosmic Evolution: the FORCE mission

Mori¹,

Tsuru²,

Nakazawa³

et al. 2018

Proceedings of XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop — PoS(MULTIF2017)

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The Focusing On Relativistic universe and Cosmic Evolution (FORCE) mission is proposed as a future Japan-lead X-ray observatory to be launched in the mid 2020s. FORCE is a successor of Hitomi, focusing on the braodband X-ray imaging spectroscopy in 1-80 keV with a significantly higher angular resolution of < 15 ′′ in half-power diameter. The sensitivity above 10 keV will be 10 times higher than that of any previous hard X-ray missions with simultaneous soft X-ray coverage. The satellite is planned to be launched by the Epsilon vehicle by ISAS/JAXA. In the current design concept, FORCE is equipped with three identical pairs of supermirrors and wideband X-ray detectors. The focal length of the mirrors is 10 m. The silicon mirror with multi-layer coating is our primary choice of optics to achieve a good angular resolution for the wide energy band while maintaining a light weight. The detector is a hybrid of a SOI-CMOS silicon-pixel detector and a CdTe detector responsible for the softer and harder energy bands, respectively. It is basically a descendant of the hard X-ray imager onboard Hitomi with its soft-band detector replaced with the SOI-CMOS. The primary scientific objective of the FORCE mission is to trace the cosmic formation history by searching for "missing black holes" in the entire range of the mass spectrum of BHs: "buried" supermassive black holes (SMBHs) (> 10 4 M ⊙ ), intermediate-mass black holes (10 2 -10 4 M ⊙ ), and "orphan" stellar-mass black holes (< 10 2 M ⊙ ). Also, investigation of the nature of relativistic particles at various astrophysical shocks is in our scope, with highangular-resolution X-ray observations with the broadband coverage. FORCE will open a new era in these fields.

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“…SOI detector for astronomical satellite X-ray observation (XRPIX) [ 16 ] has been developed to achieve a new X-ray detector system having a much faster readout and lower non-X-ray background (NXB) sensitivity than the X-ray CCDs. It is integration-type detector, and it also has trigger generation and hit position output functions (event-driven readout).…”

Section: X-ray Detector For Astrophysics (Xrpix)mentioning

confidence: 99%