X-ray calibration of the telescopes on board ASTRO-E satellite

R. Shibata; M. Ishida; H. Honda; T. Endo; J. Ishida; H. Kunieda; Y. Tawara; A. Furuzawa; Y. Ogasaka; M. Watanabe; K. Misakai; T. Yoshioka; P. J. Serlemitsos; Y. Soong; K. W. Chan

X-ray calibration of the telescopes on board ASTRO-E satellite

R. Shibata, M. Ishida, H. Honda, T. Endo, J. Ishida, H. Kunieda, Y. Tawara, A. Furuzawa, Y. Ogasaka, M. Watanabe, K. Misakai, T. Yoshioka, P. J. Serlemitsos, Y. Soong, K. W. Chan

研究成果: Conference article T › 査読

7 被引用数 (Scopus)

抄録

We present the first results of pre-flight calibrations of the X-ray telescopes on board ASTRO-E satellite. They adopt a thin foil-nesting Wolter Type-I optics, which is in principle the same as ASCA XRTs. Owing to a scale up of the telescope and a new technique of the reflector production, however, both the effective area and the imaging capability are improved. In the current measurements, the effective area is obtained to be 460, 315 and 250 cm² per XRT at 1.49, 4.51, and 8.04 keV, respectively, which is significantly larger than that of ASCA by a factor of 1.5 and 2.5 at 1.49 keV and 8.04 keV. The point spread function also shows a better focusing capability than ASCA by a factor of 2, and the half power diameter is obtained to be 1.84 arcmin at 4.51 keV. The brightness of the stray light is obtained to be 2×10^-5 counts s^-1 mm^-2 at the brightest part of the stray light image, in the case that the X-ray star with the on-axis intensity of 1 count s^-1 is the source of the stray lights, which is almost the same with ASCA.

本文言語	English
ページ（範囲）	598-609
ページ数	12
ジャーナル	Proceedings of SPIE - The International Society for Optical Engineering
巻	3444
出版ステータス	Published - 01-12-1998
外部発表	はい
イベント	Proceedings of the 1998 Conference on X-Ray Optics, Instruments, and Missions - San Diego, CA, USA 継続期間: 19-07-1998 → 22-07-1998

All Science Journal Classification (ASJC) codes

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

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引用スタイル

Shibata, R. ; Ishida, M. ; Honda, H. ; Endo, T. ; Ishida, J. ; Kunieda, H. ; Tawara, Y. ; Furuzawa, A. ; Ogasaka, Y. ; Watanabe, M. ; Misakai, K. ; Yoshioka, T. ; Serlemitsos, P. J. ; Soong, Y. ; Chan, K. W. / X-ray calibration of the telescopes on board ASTRO-E satellite. In: Proceedings of SPIE - The International Society for Optical Engineering. 1998 ; Vol. 3444. pp. 598-609.

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title = "X-ray calibration of the telescopes on board ASTRO-E satellite",

abstract = "We present the first results of pre-flight calibrations of the X-ray telescopes on board ASTRO-E satellite. They adopt a thin foil-nesting Wolter Type-I optics, which is in principle the same as ASCA XRTs. Owing to a scale up of the telescope and a new technique of the reflector production, however, both the effective area and the imaging capability are improved. In the current measurements, the effective area is obtained to be 460, 315 and 250 cm2 per XRT at 1.49, 4.51, and 8.04 keV, respectively, which is significantly larger than that of ASCA by a factor of 1.5 and 2.5 at 1.49 keV and 8.04 keV. The point spread function also shows a better focusing capability than ASCA by a factor of 2, and the half power diameter is obtained to be 1.84 arcmin at 4.51 keV. The brightness of the stray light is obtained to be 2×10-5 counts s-1 mm-2 at the brightest part of the stray light image, in the case that the X-ray star with the on-axis intensity of 1 count s-1 is the source of the stray lights, which is almost the same with ASCA.",

author = "R. Shibata and M. Ishida and H. Honda and T. Endo and J. Ishida and H. Kunieda and Y. Tawara and A. Furuzawa and Y. Ogasaka and M. Watanabe and K. Misakai and T. Yoshioka and Serlemitsos, {P. J.} and Y. Soong and Chan, {K. W.}",

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X-ray calibration of the telescopes on board ASTRO-E satellite. / Shibata, R.; Ishida, M.; Honda, H.; Endo, T.; Ishida, J.; Kunieda, H.; Tawara, Y.; Furuzawa, A.; Ogasaka, Y.; Watanabe, M.; Misakai, K.; Yoshioka, T.; Serlemitsos, P. J.; Soong, Y.; Chan, K. W.

In: Proceedings of SPIE - The International Society for Optical Engineering, Vol. 3444, 01.12.1998, p. 598-609.

研究成果: Conference article T › 査読

TY - JOUR

T1 - X-ray calibration of the telescopes on board ASTRO-E satellite

AU - Shibata, R.

AU - Ishida, M.

AU - Honda, H.

AU - Endo, T.

AU - Ishida, J.

AU - Kunieda, H.

AU - Tawara, Y.

AU - Furuzawa, A.

AU - Ogasaka, Y.

AU - Watanabe, M.

AU - Misakai, K.

AU - Yoshioka, T.

AU - Serlemitsos, P. J.

AU - Soong, Y.

AU - Chan, K. W.

PY - 1998/12/1

Y1 - 1998/12/1

N2 - We present the first results of pre-flight calibrations of the X-ray telescopes on board ASTRO-E satellite. They adopt a thin foil-nesting Wolter Type-I optics, which is in principle the same as ASCA XRTs. Owing to a scale up of the telescope and a new technique of the reflector production, however, both the effective area and the imaging capability are improved. In the current measurements, the effective area is obtained to be 460, 315 and 250 cm2 per XRT at 1.49, 4.51, and 8.04 keV, respectively, which is significantly larger than that of ASCA by a factor of 1.5 and 2.5 at 1.49 keV and 8.04 keV. The point spread function also shows a better focusing capability than ASCA by a factor of 2, and the half power diameter is obtained to be 1.84 arcmin at 4.51 keV. The brightness of the stray light is obtained to be 2×10-5 counts s-1 mm-2 at the brightest part of the stray light image, in the case that the X-ray star with the on-axis intensity of 1 count s-1 is the source of the stray lights, which is almost the same with ASCA.

AB - We present the first results of pre-flight calibrations of the X-ray telescopes on board ASTRO-E satellite. They adopt a thin foil-nesting Wolter Type-I optics, which is in principle the same as ASCA XRTs. Owing to a scale up of the telescope and a new technique of the reflector production, however, both the effective area and the imaging capability are improved. In the current measurements, the effective area is obtained to be 460, 315 and 250 cm2 per XRT at 1.49, 4.51, and 8.04 keV, respectively, which is significantly larger than that of ASCA by a factor of 1.5 and 2.5 at 1.49 keV and 8.04 keV. The point spread function also shows a better focusing capability than ASCA by a factor of 2, and the half power diameter is obtained to be 1.84 arcmin at 4.51 keV. The brightness of the stray light is obtained to be 2×10-5 counts s-1 mm-2 at the brightest part of the stray light image, in the case that the X-ray star with the on-axis intensity of 1 count s-1 is the source of the stray lights, which is almost the same with ASCA.

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AN - SCOPUS:0032299128

VL - 3444

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EP - 609

JO - Proceedings of SPIE - The International Society for Optical Engineering

JF - Proceedings of SPIE - The International Society for Optical Engineering

SN - 0277-786X

T2 - Proceedings of the 1998 Conference on X-Ray Optics, Instruments, and Missions

Y2 - 19 July 1998 through 22 July 1998

ER -