The ASTRO-H X-ray astronomy satellite

Takahashi, Tadayuki; Mitsuda, Kazuhisa; Kelley, R. L.; Aharonian, F.; Akamatsu, Hiroki; Akimoto, Fumie; Allen, S. W.; Anabuki, Naohisa; Angelini, L.; Arnaud, Keith A.; Asai, M.; Audard, M.; Awaki, Hisamitsu; Azzarello, P.; Baluta, Chris; Bamba, Aya; Bando, Nobutaka; Bautz, Marshall W.; Bialas, Thomas G.; Blandford, R. D.; Boyce, K. R.; Brenneman, Laura; Brown, G. V.; Cackett, Edward M.; Canavan, Edgar R.; Chernyakova, M.; Chiao, Meng P.; Coppi, P.; Costantini, E.; Plaa, J. de; Herder, Jan-Willem den; DiPirro, Michael; Done, Chris; Dotani, Tadayasu; Doty, J.; Ebisawa, Ken; Eckart, Megan E.; Enoto, T.; Ezoe, Yuichiro; Fabian, A. C.; Ferrigno, C.; Foster, Adam; Fujimoto, R.; Fukazawa, Yasushi; Funk, S.; Furuzawa, Akihiro; Galeazzi, M.; Gallo, Luigi; Gandhi, P.; Gilmore, K.; Guainazzi, M.; Haas, D.; Haba, Yoshito; Hamaguchi, Kenji; Harayama, Atsushi; Hatsukade, Isamu; Hayashi, Takayuki; Hayashi, Katsuhiro; Hayashida, Kentaro; Hiraga, Junko S.; Hirose, Kazuyuki; Hornschemeier, A. E.; Hoshino, Akio; Hughes, John P.; Hwang, U.; Iizuka, Ryo; Inoue, Yoshiyuki; Ishibashi, Koji; Ishida, M.; Ishikawa, Kumi; Ishimura, Kosei; Ishisaki, Yoshitaka; Ito, Masayuki; Iwata, Nobuhisa; Iyomoto, Naoko; Jewell, C.; Kaastra, J. S.; Kallman, T. R.; Kamae, T.; Kataoka, J.; Katsuda, Satoru; Katsuta, J.; Kawaharada, Madoka; Kawai, N.; Kawano, Taro; Kawasaki, Shigeo; Khangulyan, D.; Kilbourne, C. A.; Kimball, Mark O.; Kimura, Masashi; Kitamoto, Shunji; Kitayama, Tetsu; Kohmura, Takayoshi; Kokubun, M.; Konami, Saori; Kosaka, Tatsuro; Koujelev, A.; Koyama, K.; Krimm, H. A.; Kubota, Aya; Kunieda, H.; LaMassa, Stephanie; Laurent, Philippe; Lebrun, F.; Leutenegger, Maurice A.; Limousin, O.; Loewenstein, Michael; Long, Knox S.; Lumb, D.; Madejski, G.; Maeda, Yoshitomo; Makishima, Kazuo; Markevitch, M.; Masters, Candace; Matsumoto, Hironori; Matsushita, Kyoko; McCammon, D.; McGuinness, Daniel S.; McNamara, B. R.; Miko, Joseph; Miller, J. M.; Miller, Eric D.; Mineshige, Shin; Minesugi, Kenji; Mitsuishi, Ikuyuki; Miyazawa, Tatsuo; Mizuno, T.; Mori, Koji; Mori, Hajime; Moroso, Franco; Muench, Theodore; Mukai, K.; Murakami, Hiroshi; Murakami, T.; Mushotzky, R. F.; Nagano, Hosei; Nagino, Ryo; Nakagawa, Takao; Nakajima, Hiroshi; Nakamori, Takeshi; Nakashima, Shinya; Nakazawa, K.; Namba, Yoshiharu; Natsukari, Chikara; Nishioka, Yusuke; Nobukawa, Masayoshi; Noda, Hirofumi; Nomachi, M.; Dell, Steve O'; Odaka, Hirokazu; Ogawa, H.; Ogawa, Mina; Ogi, Keiji; Ohashi, T.; Ohno, M.; Ohta, M.; Okajima, Takashi; Okamoto, Atsushi; Okazaki, Tsuyoshi; Ota, Naomi; Ozaki, Masanobu; Paerels, F.; Paltani, S.; Parmar, A. N.; Petre, Robert; Pinto, C.; Pohl, M.; Pontius, James T.; Porter, F. S.; Pottschmidt, K.; Ramsey, Brian D.; Reis, R. C.; Reynolds, C. S.; Ricci, Cláudio; Russell, H. R.; Safi‐Harb, Samar; Saito, Shinya; Sakai, Shin‐ichiro; Sameshima, Hiroaki; Sato, G.; Sato, Yoichi; Sato, Kosuke; Sato, Rie; Sawada, Makoto; Serlemitsos, P. J.; Seta, Hiromi; Shibano, Yasuko; Shida, Maki; Shimada, Takanobu; Shinozaki, Kazuo; Shirron, Peter; Simionescu, A.; Simmons, Cynthia; Smith, Randall K.; Sneiderman, Gary A.; Soong, Yang; Stawarz, Ł.; Sugawara, Y.; Sugita, Hiroyuki; Sugita, S.; Szymkowiak, Andrew E.; Tajima, H.; Takahashi, H.; Takahashi, Hiroaki; Takeda, Shin’ichiro; Takei, Yoh; Tamagawa, Toru; Tamura, Takayuki; Tamura, Kouichi; Tanaka, Takaaki; Tanaka, Yasuo; Tanaka, Yasuyuki; Tashiro, M.; Tawara, Yuzuru; Terada, Y.; Terashima, Yuichi; Tombesi, Francesco; Tomida, H.; Tsuboi, Y.; Tsujimoto, Masahiro; Tsunemi, H.; Tsuru, Takeshi Go; Uchida, Hiroyuki; Uchiyama, Y.; Uchiyama, Hideki; Ueda, Yoshihiro; Ueda, Shutaro; Ueno, S.; Uno, S.; Urry, C. Megan; Ursino, Eugenio; Vries, C. de; Wada, Atsushi; Watanabe, Shin; Watanabe, Tomomi; Werner, Norbert; White, N. E.; Wilkins, D. R.; Yamada, Takahiro; Yamada, S.; Yamaguchi, Hiroya; Yamaoka, K.; Yamasaki, Noriko Y.; Yamauchi, M.; Yamauchi, Shigeo; Yaqoob, T.; Yatsu, Yoichi; Yonetoku, Daisuke; Yoshida, A.; Yuasa, Takayuki; Zhuravleva, Irina; Zoghbi, Abderahmen; ZuHone, John

doi:10.1117/12.2055681

Cited by 58 publications

(23 citation statements)

References 45 publications

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“…Nandra et al 2013) or those that are Hitomi-like with high spectral resolution (e.g. Takahashi et al 2014) will provide the ability to more finely discern the differences between the geometries.…”

Section: Discussionmentioning

confidence: 99%

Probing the geometry and motion of AGN coronae through accretion disc emissivity profiles

Gonzalez

Wilkins

Gallo

2017

Monthly Notices of the Royal Astronomical Society

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To gain a better understanding of the inner disc region that comprises active galactic nuclei it is necessary to understand the pattern in which the disc is illuminated (the emissivity profile) by X-rays emitted from the continuum source above the black hole (corona). The differences in the emissivity profiles produced by various corona geometries are explored via general relativistic ray tracing simulations. Through the analysis of various parameters of the geometries simulated it is found that emissivity profiles produced by point source and extended geometries such as cylindrical slabs and spheroidal coronae placed on the accretion disc are distinguishable. Profiles produced by point source and conical geometries are not significantly different, requiring an analysis of reflection fraction to differentiate the two geometries. Beamed point and beamed conical sources are also simulated in an effort to model jet-like coronae, though the differences here are most evident in the reflection fraction. For a point source we determine an approximation for the measured reflection fraction with the source height and velocity. Simulating spectra from the emissivity profiles produced by the various geometries produce distinguishable differences. Overall spectral differences between the geometries do not exceed 15 per cent in the most extreme cases. It is found that emissivity profiles can be useful in distinguishing point source and extended geometries given high quality spectral data of extreme, bright sources over long exposure times. In combination with reflection fraction, timing, and spectral analysis we may use emissivity profiles to discern the geometry of the X-ray source.

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Section: Discussionmentioning

confidence: 99%

Probing the geometry and motion of AGN coronae through accretion disc emissivity profiles

Gonzalez

Wilkins

Gallo

2017

Monthly Notices of the Royal Astronomical Society

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“…In addition to improved effective area, direct imagers achieve a higher signal-to-noise ratio by focusing HXRs to a small detector area (with correspondingly lower backgrounds), resulting in a high sensitivity. The Nuclear Spectroscopic Telescope Array (NuSTAR) spacecraft ([Harrison et al, 2013], launched in 2012) and Hard X-ray Imager (HXI) [Sato et al, 2016[Sato et al, , 2014 on board the Hitomi (formerly called ASTRO-H) spacecraft ( [Takahashi et al, 2014], launched in February 2016) have already begun astrophysical observations using HXR focusing optics. NuSTAR also performs a few solar observations per year, though it is not optimized for the bright fluxes of the Sun [Grefenstette et al, 2016;Hannah et al, 2016].…”

Section: 1002/2016ja022631mentioning

confidence: 99%

Fine‐pitch CdTe detector for hard X‐ray imaging and spectroscopy of the Sun with the FOXSI rocket experiment

et al. 2016

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We have developed a fine‐pitch hard X‐ray (HXR) detector using a cadmium telluride (CdTe) semiconductor for imaging and spectroscopy for the second launch of the Focusing Optics Solar X‐ray Imager (FOXSI). FOXSI is a rocket experiment to perform high sensitivity HXR observations from 4 to 15 keV using the new technique of HXR focusing optics. The focal plane detector requires <100μm position resolution (to take advantage of the angular resolution of the optics) and ≈1 keV energy resolution (full width at half maximum (FWHM)) for spectroscopy down to 4 keV, with moderate cooling (>−30°C). Double‐sided silicon strip detectors were used for the first FOXSI flight in 2012 to meet these criteria. To improve the detectors' efficiency (66% at 15 keV for the silicon detectors) and position resolution of 75 μm for the second launch, we fabricated double‐sided CdTe strip detectors with a position resolution of 60 μm and almost 100% efficiency for the FOXSI energy range. The sensitive area is 7.67 mm × 7.67 mm, corresponding to the field of view of 791′′ × 791′′. An energy resolution of 1 keV (FWHM) and low‐energy threshold of ≈4 keV were achieved in laboratory calibrations. The second launch of FOXSI was performed on 11 December 2014, and images from the Sun were successfully obtained with the CdTe detector. Therefore, we successfully demonstrated the detector concept and the usefulness of this technique for future HXR observations of the Sun.

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“…A "supermirror" technology expands its ability by focusing hard X-rays above 10 keV beyond the conventional softer energy band. NuSTAR is the first hard-X-ray-dedicated satellite to utilize the supermirror optics [1], and Hitomi, formerly called ASTRO-H, has followed [2]. Whereas this new probe in the hard X-ray band alone is very powerful, simultaneous coverage on the soft X-ray band would be ideal, considering the broadband and time-variable nature of non-thermal emission.…”

Section: Introductionmentioning

confidence: 99%

Focusing On Relativistic universe and Cosmic Evolution: the FORCE mission

Mori¹,

Tsuru²,

Nakazawa³

et al. 2018

Proceedings of XII Multifrequency Behaviour of High Energy Cosmic Sources Workshop — PoS(MULTIF2017)

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The Focusing On Relativistic universe and Cosmic Evolution (FORCE) mission is proposed as a future Japan-lead X-ray observatory to be launched in the mid 2020s. FORCE is a successor of Hitomi, focusing on the braodband X-ray imaging spectroscopy in 1-80 keV with a significantly higher angular resolution of < 15 ′′ in half-power diameter. The sensitivity above 10 keV will be 10 times higher than that of any previous hard X-ray missions with simultaneous soft X-ray coverage. The satellite is planned to be launched by the Epsilon vehicle by ISAS/JAXA. In the current design concept, FORCE is equipped with three identical pairs of supermirrors and wideband X-ray detectors. The focal length of the mirrors is 10 m. The silicon mirror with multi-layer coating is our primary choice of optics to achieve a good angular resolution for the wide energy band while maintaining a light weight. The detector is a hybrid of a SOI-CMOS silicon-pixel detector and a CdTe detector responsible for the softer and harder energy bands, respectively. It is basically a descendant of the hard X-ray imager onboard Hitomi with its soft-band detector replaced with the SOI-CMOS. The primary scientific objective of the FORCE mission is to trace the cosmic formation history by searching for "missing black holes" in the entire range of the mass spectrum of BHs: "buried" supermassive black holes (SMBHs) (> 10 4 M ⊙ ), intermediate-mass black holes (10 2 -10 4 M ⊙ ), and "orphan" stellar-mass black holes (< 10 2 M ⊙ ). Also, investigation of the nature of relativistic particles at various astrophysical shocks is in our scope, with highangular-resolution X-ray observations with the broadband coverage. FORCE will open a new era in these fields.

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The ASTRO-H X-ray astronomy satellite

Cited by 58 publications

References 45 publications

Probing the geometry and motion of AGN coronae through accretion disc emissivity profiles

Probing the geometry and motion of AGN coronae through accretion disc emissivity profiles

Fine‐pitch CdTe detector for hard X‐ray imaging and spectroscopy of the Sun with the FOXSI rocket experiment

Focusing On Relativistic universe and Cosmic Evolution: the FORCE mission

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