Current status of ASTRO-H Hard X-ray Telescopes (HXTs)

Awaki, Hisamitsu; Kunieda, H.; Furuzawa, Akihiro; Haba, Yoshito; Hayashi, Takayuki; Iizuka, Ryo; Ishibashi, Koji; Ishida, M.; Itoh, M.; Kosaka, Tatsuro; Maeda, Yoshitomo; Matsumoto, Hironori; Miyazawa, Tatsuo; Mori, Hajime; Nagano, Hosei; Namba, Yoshiharu; Ogasaka, Yasushi; Ogi, Keiji; Okajima, Takashi; Sugita, S.; Suzuki, Yoshio; Tamura, Kouichi; Tawara, Yuzuru; Uesugi, Kentaro; Yamashita, Koujun; Yamauchi, Shigeo

doi:10.1117/12.926753

Cited by 13 publications

(7 citation statements)

References 10 publications

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“…The technology of a hard X-ray focusing mirror has already been proven by the balloon programs InFOCµS (2001, 2004), 26,27 HEFT (2004) 28 and SUMIT (2006) 26 and recently with the NuSTAR satellite. 29 The HXT [30][31][32][33][34][35] consists of three parts, an X-ray mirror: a stray light baffle called pre-Collimator, and a thermal shield (Fig. 4, right).…”

Section: Hard X-ray Telescopesmentioning

confidence: 99%

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The ASTRO-H (Hitomi) x-ray astronomy satellite

et al. 2016

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The Hitomi (ASTRO-H) mission is the sixth Japanese X-ray astronomy satellite developed by a large international collaboration, including Japan, USA, Canada, and Europe. The mission aimed to provide the highest energy resolution ever achieved at E > 2 keV, using a microcalorimeter instrument, and to cover a wide energy range spanning four decades in energy from soft X-rays to gamma-rays. After a successful launch on 2016 February 17, the spacecraft lost its function on 2016 March 26, but the commissioning phase for about a month provided valuable information on the on-board instruments and the spacecraft

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Section: Hard X-ray Telescopesmentioning

confidence: 99%

“…The mirror is based on conically-approximated Wolter I grazing incidence optics. 32,33 The diameters of the innermost and the outermost reflectors are 120 mm and 450 mm, respectively. The total number of nested shells is 213.…”

Section: Hard X-ray Telescopesmentioning

confidence: 99%

The ASTRO-H (Hitomi) x-ray astronomy satellite

et al. 2016

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“…conical-foil mirrors with depth-graded multilayer reflecting surfaces that provide a 5 ÷ 80 keV energy range [13,14]. The focal plane imager consists of four-layers of 0.5 mm thick Double-sided Silicon Strip Detectors (DSSD) and one layer of 0.75 mm thick CdTe double sided cross-strip detector [15,16].…”

Section: Supplement/mentioning

confidence: 99%

The Astro-H Mission

et al. 2013

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A review of the Astro-H mission is presented here on behalf of the Astro-H collaboration. The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions initiated by the Institute of Space and Astronautical Science (ISAS). One of the main uniquenesses of the ASTRO-H satellite is the high sensitivity and imaging capability of the wide energy band from 0.3 keV to 600 keV. The coverage is achieved by combining the four instruments of the SXS, SXI, HXI, and SGD. The other main uniqueness is a spectroscopic capability not only for a point-like source but also for an extended source with high spectral resolution of Δ<em>E</em>~4÷7eV of SXS. Using the unique powers of these instruments, ASTRO-H will address unresolved issues in high-energy astrophysics.

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“…The HXT has conical-foil mirrors with depth-graded multilayer reflecting surfaces that provide efficient reflection over 5-80 keV energy range. 12,31,32 The effective area of the HXT is maximized for a long focal length.…”

Section: Soft X-ray Imaging Systemmentioning

confidence: 99%

The ASTRO-H X-ray Observatory

et al. 2012

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The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions initiated by the Institute of Space and Astronautical Science (ISAS). ASTRO-H will investigate the physics of the highenergy universe via a suite of four instruments, covering a very wide energy range, from 0.3 keV to 600 keV. These instruments include a high-resolution, high-throughput spectrometer sensitive over 0.3-12 keV with high spectral resolution of ∆E ≦ 7 eV, enabled by a micro-calorimeter array located in the focal plane of thin-foil X-ray optics; hard X-ray imaging spectrometers covering 5-80 keV, located in the focal plane of multilayer-coated, focusing hard X-ray mirrors; a wide-field imaging spectrometer sensitive over 0.4-12 keV, with an X-ray CCD camera in the focal plane of a soft X-ray telescope; and a non-focusing Compton-camera type soft gamma-ray detector, sensitive in the 40-600 keV band. The simultaneous broad bandpass, coupled with high spectral resolution, will enable the pursuit of a wide variety of important science themes.

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Current status of ASTRO-H Hard X-ray Telescopes (HXTs)

Cited by 13 publications

References 10 publications

The ASTRO-H (Hitomi) x-ray astronomy satellite

The ASTRO-H (Hitomi) x-ray astronomy satellite

The Astro-H Mission

The ASTRO-H X-ray Observatory

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