Experimental studies on the charge transfer inefficiency of CCD developed for the soft X-ray imaging telescope Xtend aboard the XRISM satellite

Kanemaru, Yoshiaki; Sato, Jin; Takaki, Toshiyuki; Terada, Yuta; Mori, Koji; Saito, Mariko; Nobukawa, Kumiko K.; Tanaka, Takaaki; Uchida, Hiroyuki; Hayashida, Kentaro; Matsumoto, Hironori; Noda, Hirofumi; Hanaoka, Maho; Yoneyama, T.; Okazaki, Koki; Asakura, Kiyotaka; Sakuma, Shotaro; Hattori, Koichi; Ishikura, Ayami; Amano, Yoshiharu; Okon, Hiromichi; Tsuru, Takeshi Go; Tomida, H.; Kashimura, Hikari; Nakajima, Hiroshi; Kohmura, Takayoshi; Hagino, K.; Murakami, Hiroshi; Kobayashi, Shōgo; Nishioka, Yusuke; Yamauchi, M.; Hatsukade, Isamu; Sako, T.; Nobukawa, Masayoshi; Urabe, Yukino; Hiraga, Junko S.; Uchiyama, Hideki; Yamaoka, K.; Dotani, Tadayasu; Tsunemi, H.

doi:10.1016/j.nima.2020.164646

Cited by 8 publications

(6 citation statements)

References 19 publications

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“…Charge transfer inefficiency (CTI) refers to the loss of charge when a charge packet is moved from one pixel to the next. It depends on several different parameters such as trap populations, trap densities, clocking time, clocking sequence, and temperature [43][44][45][46]. CTI in the Oscura CCDs -7 -…”

Section: Charge Transfer Inefficiencymentioning

confidence: 99%

Skipper-CCD sensors for the Oscura experiment: requirements and preliminary tests

Cervantes-Vergara,

Perez,

Estrada

et al. 2023

J. Inst.

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Oscura is a proposed multi-kg skipper-CCD experiment designed for a dark matter (DM) direct detection search that will reach unprecedented sensitivity to sub-GeV DM-electron interactions with its 10 kg detector array. Oscura is planning to operate at SNOLAB with 2070 m overburden, and aims to reach a background goal of less than one event in each electron bin in the 2–10 electron ionization-signal region for the full 30 kg-year exposure, with a radiation background rate of 0.01 dru.[1 dru (differential rate unit) corresponds to 1 event/kg/day/keV.] In order to achieve this goal, Oscura must address each potential source of background events, including instrumental backgrounds. In this work, we discuss the main instrumental background sources and the strategy to control them, establishing a set of constraints on the sensors' performance parameters. We present results from the tests of the first fabricated Oscura prototype sensors, evaluate their performance in the context of the established constraints and estimate the Oscura instrumental background based on these results.

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Section: Charge Transfer Inefficiencymentioning

confidence: 99%

Skipper-CCD sensors for the Oscura experiment: requirements and preliminary tests

Cervantes-Vergara,

Perez,

Estrada

et al. 2023

J. Inst.

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“…From the count map, we confirmed that the count rate, irradiated location, and region size are as designed. The spectrum is made with events taken in the segment CCD2AB, and CTI corrections 23,24 are not applied. The energy resolution of this spectrum is 177.5±0.6 eV in FWHM and as expected from on-ground calibrations held in advance, which is discussed in the next section.…”

Section: Sxi Performance Verification In Sub-system Testsmentioning

confidence: 99%

“…Parameters of the CTI correction are derived following Ref. 24. Before the CTI correction, the pulse height generally decreases as a function of row number with periodic recovery at the .…”

Section: Sxi On-ground Calibrationmentioning

confidence: 99%

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Xtend, the soft x-ray imaging telescope for the x-ray imaging and spectroscopy mission (XRISM)

Mori

Tomida

Nakajima

et al. 2022

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray

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Xtend is a soft X-ray imaging telescope developed for the X-Ray Imaging and Spectroscopy Mission (XRISM). XRISM is scheduled to be launched in the Japanese fiscal year 2022. Xtend consists of the Soft X-ray Imager (SXI), an X-ray CCD camera, and the X-ray Mirror Assembly (XMA), a thin-foil-nested conically approximated Wolter-I optics. The SXI uses the P-channel, back-illuminated type CCD with an imaging area size of 31 mm on a side. The four CCD chips are arranged in a 2×2 grid and can be cooled down to −120 • C with a single-stage Stirling cooler. The XMA nests thin aluminum foils coated with gold in a confocal way with an outer diameter of 45 cm. A pre-collimator is installed in front of the X-ray mirror for the reduction of the stray light. Combining the SXI and XMA with a focal length of 5.6m, a field of view of 38 × 38 over the energy range from 0.4 to 13 keV is realized. We have completed the fabrication of the flight model of both SXI and XMA. The performance verification has been successfully conducted in a series of sub-system level tests. We also carried out on-ground calibration measurements and the data analysis is ongoing.

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“…The basic design of the CCD camera is identical to that of the Hitomi SXI, and some improvements are adopted on the CCD chip and the scheme for preventing light leakage. The development and on-ground calibration status are reported in [26][27][28][29].…”

Section: Development Status Of Science Instrumentsmentioning

confidence: 99%

Status of x-ray imaging and spectroscopy mission (XRISM)

Tashiro

Maejima

Toda

et al. 2020

Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray

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The X-Ray Imaging and Spectroscopy Mission (XRISM) is the successor to the 2016 Hitomi mission that ended prematurely. Like Hitomi, the primary science goals are to examine astrophysical problems with precise highresolution X-ray spectroscopy. XRISM promises to discover new horizons in X-ray astronomy. XRISM carries a 6 x 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly and a co-aligned X-ray CCD camera that covers the same energy band over a large field of view. XRISM utilizes Hitomi heritage, but all designs were reviewed. The attitude and orbit control system were improved in hardware and software. The number of star sensors were increased from two to three to improve coverage and robustness in onboard attitude determination and to obtain a wider field of view sun sensor. The fault detection, isolation, and reconfiguration (FDIR) system was carefully examined and reconfigured. Together with a planned increase of ground support stations, the survivability of the spacecraft is significantly improved.

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Experimental studies on the charge transfer inefficiency of CCD developed for the soft X-ray imaging telescope Xtend aboard the XRISM satellite

Cited by 8 publications

References 19 publications

Skipper-CCD sensors for the Oscura experiment: requirements and preliminary tests

Skipper-CCD sensors for the Oscura experiment: requirements and preliminary tests

Xtend, the soft x-ray imaging telescope for the x-ray imaging and spectroscopy mission (XRISM)

Status of x-ray imaging and spectroscopy mission (XRISM)

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