On-ground calibration of the Hitomi Hard X-ray Telescopes

Hideyuki Mori; Takuya Miyazawa; Hisamitsu Awaki; Hironori Matsumoto; Yasunori Babazaki; Ayako Bandai; Tadatsugu Demoto; Akihiro Furuzawa; Yoshito Haba; Takayuki Hayashi; Ryo Iizuka; Kazunori Ishibashi; Manabu Ishida; Naoki Ishida; Masayuki Itoh; Toshihiro Iwase; Hiroyoshi Kato; Hiroaki Kobayashi; Tatsuro Kosaka; Hideyo Kunieda; Shou Kurashima; Daichi Kurihara; Yuuji Kuroda; Yoshitomo Maeda; Yoshifumi Meshino; Ikuyuki Mitsuishi; Yuusuke Miyata; Housei Nagano; Yoshiharu Namba; Yasushi Ogasaka; Keiji Ogi; Takashi Okajima; Shigetaka Saji; Fumiya Shimasaki; Takuro Sato; Toshiki Sato; Naotsugu Shima; Satoshi Sugita; Yoshio Suzuki; Kenji Tachibana; Sasagu Tachibana; Shun'Ya Takizawa; Keisuke Tamura; Yuzuru Tawara; Kazuki Tomikawa; Tatsuharu Torii; Kentaro Uesugi; Koujun Yamashita; Shigeo Yamauchi

doi:10.1117/1.JATIS.4.1.011210

On-ground calibration of the Hitomi Hard X-ray Telescopes

Hideyuki Mori, Takuya Miyazawa, Hisamitsu Awaki, Hironori Matsumoto, Yasunori Babazaki, Ayako Bandai, Tadatsugu Demoto, Akihiro Furuzawa, Yoshito Haba, Takayuki Hayashi, Ryo Iizuka, Kazunori Ishibashi, Manabu Ishida, Naoki Ishida, Masayuki Itoh, Toshihiro Iwase, Hiroyoshi Kato, Hiroaki Kobayashi, Tatsuro Kosaka, Hideyo KuniedaShou Kurashima, Daichi Kurihara, Yuuji Kuroda, Yoshitomo Maeda, Yoshifumi Meshino, Ikuyuki Mitsuishi, Yuusuke Miyata, Housei Nagano, Yoshiharu Namba, Yasushi Ogasaka, Keiji Ogi, Takashi Okajima, Shigetaka Saji, Fumiya Shimasaki, Takuro Sato, Toshiki Sato, Naotsugu Shima, Satoshi Sugita, Yoshio Suzuki, Kenji Tachibana, Sasagu Tachibana, Shun'Ya Takizawa, Keisuke Tamura, Yuzuru Tawara, Kazuki Tomikawa, Tatsuharu Torii, Kentaro Uesugi, Koujun Yamashita, Shigeo Yamauchi

Research output: Contribution to journal › Article › peer-review

13 Citations (Scopus)

Abstract

We present x-ray characteristics of the Hard X-ray Telescopes (HXTs) on board the Hitomi (ASTRO-H) satellite. Measurements were conducted at the SPring-8 BL20B2 beamline and the ISAS/JAXA 27-m beamline. The angular resolution defined by a half-power diameter was 1.9′ (HXT-1) and 2.1′ (HXT-2) at 8 keV, 1.9′ at 30 keV, and 1.8′ at 50 keV. The effective area was found to be 620cm2 at 8 keV, 178cm2 at 30 keV, and 82cm2 at 50 keV per mirror module. Although the angular resolutions were slightly worse than the requirement (1.7′), the effective areas sufficiently exceeded the requirements of 150cm2 at 30 keV and 55cm2 at 50 keV. The off-axis measurements of the effective areas resulted in the field of view being 6.1′ at 50 keV, 7.7′ at 30 keV, and 9.7′ at 8 keV in diameter. We confirmed that the main component of the stray x-ray light was significantly reduced by mounting the precollimator as designed. Detailed analysis of the data revealed that the angular resolution was degraded mainly by figure errors of mirror foils, and the angular resolution is completely explained by the figure errors, positioning errors of the foils, and conical approximation of the foil shape. We found that the effective areas were ∼80% of the designed values below 40 keV, whereas they steeply decline above 40 keV and become only ∼50%. We investigated this abrupt decline and found that neither the error of the multilayer design nor the errors of the incident angles induced by the positioning errors of the foils can be the cause. The reflection profile of each foil pair from the defocused image strongly suggests that the figure errors of the foils probably bring about the reduction in the effective areas at higher energies.

Original language	English
Article number	044001
Journal	Journal of Astronomical Telescopes, Instruments, and Systems
Volume	4
Issue number	1
DOIs	https://doi.org/10.1117/1.JATIS.4.1.011210
Publication status	Published - 01-01-2018
Externally published	Yes

All Science Journal Classification (ASJC) codes

Electronic, Optical and Magnetic Materials
Control and Systems Engineering
Instrumentation
Astronomy and Astrophysics
Mechanical Engineering
Space and Planetary Science

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10.1117/1.JATIS.4.1.011210

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Mori, H., Miyazawa, T., Awaki, H., Matsumoto, H., Babazaki, Y., Bandai, A., Demoto, T., Furuzawa, A., Haba, Y., Hayashi, T., Iizuka, R., Ishibashi, K., Ishida, M., Ishida, N., Itoh, M., Iwase, T., Kato, H., Kobayashi, H., Kosaka, T., ... Yamauchi, S. (2018). On-ground calibration of the Hitomi Hard X-ray Telescopes. Journal of Astronomical Telescopes, Instruments, and Systems, 4(1), Article 044001. https://doi.org/10.1117/1.JATIS.4.1.011210

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title = "On-ground calibration of the Hitomi Hard X-ray Telescopes",

abstract = "We present x-ray characteristics of the Hard X-ray Telescopes (HXTs) on board the Hitomi (ASTRO-H) satellite. Measurements were conducted at the SPring-8 BL20B2 beamline and the ISAS/JAXA 27-m beamline. The angular resolution defined by a half-power diameter was 1.9′ (HXT-1) and 2.1′ (HXT-2) at 8 keV, 1.9′ at 30 keV, and 1.8′ at 50 keV. The effective area was found to be 620cm2 at 8 keV, 178cm2 at 30 keV, and 82cm2 at 50 keV per mirror module. Although the angular resolutions were slightly worse than the requirement (1.7′), the effective areas sufficiently exceeded the requirements of 150cm2 at 30 keV and 55cm2 at 50 keV. The off-axis measurements of the effective areas resulted in the field of view being 6.1′ at 50 keV, 7.7′ at 30 keV, and 9.7′ at 8 keV in diameter. We confirmed that the main component of the stray x-ray light was significantly reduced by mounting the precollimator as designed. Detailed analysis of the data revealed that the angular resolution was degraded mainly by figure errors of mirror foils, and the angular resolution is completely explained by the figure errors, positioning errors of the foils, and conical approximation of the foil shape. We found that the effective areas were ∼80% of the designed values below 40 keV, whereas they steeply decline above 40 keV and become only ∼50%. We investigated this abrupt decline and found that neither the error of the multilayer design nor the errors of the incident angles induced by the positioning errors of the foils can be the cause. The reflection profile of each foil pair from the defocused image strongly suggests that the figure errors of the foils probably bring about the reduction in the effective areas at higher energies.",

keywords = "Hitomi (ASTRO-H), astronomical optics, multilayer mirrors, x-ray mirrors",

author = "Hideyuki Mori and Takuya Miyazawa and Hisamitsu Awaki and Hironori Matsumoto and Yasunori Babazaki and Ayako Bandai and Tadatsugu Demoto and Akihiro Furuzawa and Yoshito Haba and Takayuki Hayashi and Ryo Iizuka and Kazunori Ishibashi and Manabu Ishida and Naoki Ishida and Masayuki Itoh and Toshihiro Iwase and Hiroyoshi Kato and Hiroaki Kobayashi and Tatsuro Kosaka and Hideyo Kunieda and Shou Kurashima and Daichi Kurihara and Yuuji Kuroda and Yoshitomo Maeda and Yoshifumi Meshino and Ikuyuki Mitsuishi and Yuusuke Miyata and Housei Nagano and Yoshiharu Namba and Yasushi Ogasaka and Keiji Ogi and Takashi Okajima and Shigetaka Saji and Fumiya Shimasaki and Takuro Sato and Toshiki Sato and Naotsugu Shima and Satoshi Sugita and Yoshio Suzuki and Kenji Tachibana and Sasagu Tachibana and Shun'Ya Takizawa and Keisuke Tamura and Yuzuru Tawara and Kazuki Tomikawa and Tatsuharu Torii and Kentaro Uesugi and Koujun Yamashita and Shigeo Yamauchi",

note = "Publisher Copyright: {\textcopyright} 2018 The Authors.",

year = "2018",

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doi = "10.1117/1.JATIS.4.1.011210",

language = "English",

volume = "4",

journal = "Journal of Astronomical Telescopes, Instruments, and Systems",

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Mori, H, Miyazawa, T, Awaki, H, Matsumoto, H, Babazaki, Y, Bandai, A, Demoto, T, Furuzawa, A, Haba, Y, Hayashi, T, Iizuka, R, Ishibashi, K, Ishida, M, Ishida, N, Itoh, M, Iwase, T, Kato, H, Kobayashi, H, Kosaka, T, Kunieda, H, Kurashima, S, Kurihara, D, Kuroda, Y, Maeda, Y, Meshino, Y, Mitsuishi, I, Miyata, Y, Nagano, H, Namba, Y, Ogasaka, Y, Ogi, K, Okajima, T, Saji, S, Shimasaki, F, Sato, T, Sato, T, Shima, N, Sugita, S, Suzuki, Y, Tachibana, K, Tachibana, S, Takizawa, SY, Tamura, K, Tawara, Y, Tomikawa, K, Torii, T, Uesugi, K, Yamashita, K & Yamauchi, S 2018, 'On-ground calibration of the Hitomi Hard X-ray Telescopes', Journal of Astronomical Telescopes, Instruments, and Systems, vol. 4, no. 1, 044001. https://doi.org/10.1117/1.JATIS.4.1.011210

TY - JOUR

T1 - On-ground calibration of the Hitomi Hard X-ray Telescopes

AU - Mori, Hideyuki

AU - Miyazawa, Takuya

AU - Awaki, Hisamitsu

AU - Matsumoto, Hironori

AU - Babazaki, Yasunori

AU - Bandai, Ayako

AU - Demoto, Tadatsugu

AU - Furuzawa, Akihiro

AU - Haba, Yoshito

AU - Hayashi, Takayuki

AU - Iizuka, Ryo

AU - Ishibashi, Kazunori

AU - Ishida, Manabu

AU - Ishida, Naoki

AU - Itoh, Masayuki

AU - Iwase, Toshihiro

AU - Kato, Hiroyoshi

AU - Kobayashi, Hiroaki

AU - Kosaka, Tatsuro

AU - Kunieda, Hideyo

AU - Kurashima, Shou

AU - Kurihara, Daichi

AU - Kuroda, Yuuji

AU - Maeda, Yoshitomo

AU - Meshino, Yoshifumi

AU - Mitsuishi, Ikuyuki

AU - Miyata, Yuusuke

AU - Nagano, Housei

AU - Namba, Yoshiharu

AU - Ogasaka, Yasushi

AU - Ogi, Keiji

AU - Okajima, Takashi

AU - Saji, Shigetaka

AU - Shimasaki, Fumiya

AU - Sato, Takuro

AU - Sato, Toshiki

AU - Shima, Naotsugu

AU - Sugita, Satoshi

AU - Suzuki, Yoshio

AU - Tachibana, Kenji

AU - Tachibana, Sasagu

AU - Takizawa, Shun'Ya

AU - Tamura, Keisuke

AU - Tawara, Yuzuru

AU - Tomikawa, Kazuki

AU - Torii, Tatsuharu

AU - Uesugi, Kentaro

AU - Yamashita, Koujun

AU - Yamauchi, Shigeo

PY - 2018/1/1

Y1 - 2018/1/1

N2 - We present x-ray characteristics of the Hard X-ray Telescopes (HXTs) on board the Hitomi (ASTRO-H) satellite. Measurements were conducted at the SPring-8 BL20B2 beamline and the ISAS/JAXA 27-m beamline. The angular resolution defined by a half-power diameter was 1.9′ (HXT-1) and 2.1′ (HXT-2) at 8 keV, 1.9′ at 30 keV, and 1.8′ at 50 keV. The effective area was found to be 620cm2 at 8 keV, 178cm2 at 30 keV, and 82cm2 at 50 keV per mirror module. Although the angular resolutions were slightly worse than the requirement (1.7′), the effective areas sufficiently exceeded the requirements of 150cm2 at 30 keV and 55cm2 at 50 keV. The off-axis measurements of the effective areas resulted in the field of view being 6.1′ at 50 keV, 7.7′ at 30 keV, and 9.7′ at 8 keV in diameter. We confirmed that the main component of the stray x-ray light was significantly reduced by mounting the precollimator as designed. Detailed analysis of the data revealed that the angular resolution was degraded mainly by figure errors of mirror foils, and the angular resolution is completely explained by the figure errors, positioning errors of the foils, and conical approximation of the foil shape. We found that the effective areas were ∼80% of the designed values below 40 keV, whereas they steeply decline above 40 keV and become only ∼50%. We investigated this abrupt decline and found that neither the error of the multilayer design nor the errors of the incident angles induced by the positioning errors of the foils can be the cause. The reflection profile of each foil pair from the defocused image strongly suggests that the figure errors of the foils probably bring about the reduction in the effective areas at higher energies.

AB - We present x-ray characteristics of the Hard X-ray Telescopes (HXTs) on board the Hitomi (ASTRO-H) satellite. Measurements were conducted at the SPring-8 BL20B2 beamline and the ISAS/JAXA 27-m beamline. The angular resolution defined by a half-power diameter was 1.9′ (HXT-1) and 2.1′ (HXT-2) at 8 keV, 1.9′ at 30 keV, and 1.8′ at 50 keV. The effective area was found to be 620cm2 at 8 keV, 178cm2 at 30 keV, and 82cm2 at 50 keV per mirror module. Although the angular resolutions were slightly worse than the requirement (1.7′), the effective areas sufficiently exceeded the requirements of 150cm2 at 30 keV and 55cm2 at 50 keV. The off-axis measurements of the effective areas resulted in the field of view being 6.1′ at 50 keV, 7.7′ at 30 keV, and 9.7′ at 8 keV in diameter. We confirmed that the main component of the stray x-ray light was significantly reduced by mounting the precollimator as designed. Detailed analysis of the data revealed that the angular resolution was degraded mainly by figure errors of mirror foils, and the angular resolution is completely explained by the figure errors, positioning errors of the foils, and conical approximation of the foil shape. We found that the effective areas were ∼80% of the designed values below 40 keV, whereas they steeply decline above 40 keV and become only ∼50%. We investigated this abrupt decline and found that neither the error of the multilayer design nor the errors of the incident angles induced by the positioning errors of the foils can be the cause. The reflection profile of each foil pair from the defocused image strongly suggests that the figure errors of the foils probably bring about the reduction in the effective areas at higher energies.

KW - Hitomi (ASTRO-H)

KW - astronomical optics

KW - multilayer mirrors

KW - x-ray mirrors

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U2 - 10.1117/1.JATIS.4.1.011210

DO - 10.1117/1.JATIS.4.1.011210

M3 - Article

AN - SCOPUS:85041208273

SN - 2329-4124

VL - 4

JO - Journal of Astronomical Telescopes, Instruments, and Systems

JF - Journal of Astronomical Telescopes, Instruments, and Systems

IS - 1

M1 - 044001

ER -

On-ground calibration of the Hitomi Hard X-ray Telescopes

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