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27 September 2012 A ground calibration of the engineering model of the SXT onboard ASTRO-H using the ISAS 30m pencil beam facility
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Abstract
The Japanese ASTRO-H mission, planned to be launched in 2014, will carry several instruments for covering a wide energy range from a few keV to 600 keV. Among them there are four thin-foil-nested Wolter-I X-ray telescopes. Two of them are Soft X-ray Telescopes (SXTs) covering up to ~12 keV. Each of them focuses an image on the focal plane detectors of the CCD camera (SXI) and the calorimeter (SXS-XCS), respectively. In 2011, we performed a ground calibration of a quadrant engineering model (EM) of SXT that was fabricated at MASA's Goddard Space Flight Center (GSFC). The ground calibration was made with a combination of the measurements at the GSFC and Institute of Space and Astronautical Science (ISAS) facilities. In this paper we report the results of the calibration at the ISAS 30m beamline facility. We used a raster san method with a pencil beam at the baseline length of 30m. An effective area and angular resolution of the EM quadrant were measured. The effective area is 147 cm2 at 1.49 keV and 116 cm2 at 4.51 keV, respectively, while the angular longer by ~20mm from nominal length. We also measured imaging performance in separate parts of nested mirrors. The angular resolution of parts at outer radius is larger than those at inner radius, and the quadrant have different focal lengths in radius.
© (2012) COPYRIGHT Society of Photo-Optical Instrumentation Engineers (SPIE). Downloading of the abstract is permitted for personal use only.
K. Ichihara, T. Hayashi, M. Ishida, Y. Maeda, H. Mori, T. Sato, K. Tomikawa, K. Ishibashi, R. Iizuka, T. Okajima, P. J. Serlemitsos, and Y. Soong "A ground calibration of the engineering model of the SXT onboard ASTRO-H using the ISAS 30m pencil beam facility", Proc. SPIE 8443, Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray, 844357 (27 September 2012); https://doi.org/10.1117/12.925860
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