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

Research output: Contribution to journal › Conference article › peer-review

8 Citations (Scopus)

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.

Original language	English
Pages (from-to)	598-609
Number of pages	12
Journal	Proceedings of SPIE - The International Society for Optical Engineering
Volume	3444
Publication status	Published - 1998
Externally published	Yes
Event	Proceedings of the 1998 Conference on X-Ray Optics, Instruments, and Missions - San Diego, CA, USA Duration: 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

Cite this

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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.}",

year = "1998",

language = "English",

volume = "3444",

pages = "598--609",

journal = "Proceedings of SPIE - The International Society for Optical Engineering",

issn = "0277-786X",

publisher = "SPIE",

note = "Proceedings of the 1998 Conference on X-Ray Optics, Instruments, and Missions ; Conference date: 19-07-1998 Through 22-07-1998",

}

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

Y1 - 1998

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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M3 - Conference article

AN - SCOPUS:0032299128

SN - 0277-786X

VL - 3444

SP - 598

EP - 609

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

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

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

Y2 - 19 July 1998 through 22 July 1998

ER -

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

Abstract

All Science Journal Classification (ASJC) codes

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