The ASTRO-H Mission

Takahashi, Tadayuki; Mitsuda, Kazuhisa; Kelley, R. L.; Aharonian, F.; Akimoto, Fumie; Allen, S. W.; Anabuki, Naohisa; Angelini, L.; Arnaud, Keith A.; Awaki, Hisamitsu; Bamba, Aya; Bando, Nobutaka; Bautz, M. W.; Blandford, R. D.; Boyce, K. R.; Brown, G. V.; Chernyakova, M.; Coppi, P.; Costantini, E.; Cottam, J.; Crow, John; Plaa, J. de; Vries, C. de; Herder, Jan-Willem den; DiPirro, Michael; Done, Chris; Dotani, Tadayasu; Ebisawa, Ken; Enoto, T.; Ezoe, Yuichiro; Fabian, A. C.; Fujimoto, R.; Fukazawa, Yasushi; Funk, S.; Furuzawa, Akihiro; Galeazzi, M.; Gandhi, P.; Gendreau, Keith C.; Gilmore, K.; Haba, Yoshito; Hamaguchi, Kenji; Hatsukade, Isamu; Hayashida, Kentaro; Hiraga, Junko S.; Hirose, Kazuyuki; Hornschemeier, A. E.; Hughes, John P.; Hwang, U.; Iizuka, Ryo; Ishibashi, Koji; Ishida, M.; Ishimura, Kosei; Ishisaki, Yoshitaka; Isobe, Naoki; Ito, Masayuki; Iwata, Nobuhisa; Kaastra, J. S.; Kallman, Tim; Kamae, T.; Katagiri, H.; Kataoka, J.; Katsuda, Satoru; Kawaharada, Madoka; Kawai, N.; Kawasaki, Shigeo; Khangaluyan, Dmitry; Kilbourne, Caroline A.; Kinugasa, K.; Kitamoto, Shunji; Kitayama, Tetsu; Kohmura, Takayoshi; Kokubun, M.; Kosaka, Tatsuro; Kotani, Takayuki; Koyama, K.; Kubota, Aya; Kunieda, H.; Laurent, Philippe; Lebrun, F.; Limousin, O.; Loewenstein, Michael; Long, Knox S.; Madejski, G.; Maeda, Yoshitomo; Makishima, Kazuo; Markevitch, M.; Matsumoto, Hironori; Matsushita, Kyoko; McCammon, D.; Miller, J. M.; Mineshige, Shin; Minesugi, Kenji; Miyazawa, Tatsuo; Mizuno, T.; Mori, Koji; Mori, Hajime; Mukai, K.; Murakami, Hiroshi; Murakami, T.; Mushotzky, R. F.; Nakagawa, Y. E.; Nakagawa, Takao; Nakajima, Hiroshi; Nakamori, Takeshi; Nakazawa, K.; Namba, Yoshiharu; Nomachi, M.; O’Dell, Stephen L.; Ogawa, H.; Ogawa, Mina; Ogi, Keiji; Ohashi, T.; Ohno, M.; Ohta, M.; Okajima, Takashi; Ota, Naomi; Ozaki, Masanori; Paerels, F.; Paltani, S.; Parmar, A. N.; Petre, Robert; Pohl, M.; Porter, Scott; Ramsey, Brian D.; Reynolds, C. S.; Sakai, Shin‐ichiro; Sambruna, R. M.; Sato, G.; Sato, Yoichi; Serlemitsos, P. J.; Shida, Maki; Shimada, Takanobu; Shinozaki, Kazuo; Shirron, Peter; Smith, Randall K.; Sneiderman, Gary A.; Soong, Yang; Stawarz, Ł.; Sugita, Hiroyuki; Szymkowiak, Andrew E.; Tajima, H.; Takahashi, H.; Takei, Yoh; Tamagawa, T.; Tamura, Takayuki; Tamura, Kouichi; Tanaka, Takaaki; Tanaka, Y.; Tanaka, Yasuo; Tashiro, M.; Tawara, Yuzuru; Terada, Y.; Terashima, Yuichi; Tombesi, Francesco; Tomida, H.; Tozuka, Miyako; Tsuboi, Y.; Tsujimoto, Masahiro; Tsunemi, H.; Tsuru, Takeshi Go; Uchida, Hiroyuki; Uchiyama, Y.; Uchiyama, Hideki; Ueda, Yoshihiro; Uno, S.; Urry, C. Megan; Watanabe, Shin; White, N. E.; Yamada, Takahiro; Yamaguchi, Hiroya; Yamaoka, K.; Yamasaki, Noriko Y.; Yamauchi, M.; Yamauchi, Shigeo; Yatsu, Yoichi; Yonetoku, Daisuke; Yoshida, A.

doi:10.1117/12.857875

Cited by 130 publications

(22 citation statements)

References 38 publications

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“…The spiral bulk flows should be directly observable with future telescopes, for example using the next international X-ray satellite, ASTRO-H (Takahashi et al 2010), scheduled for launch in 2014. In particular, ASTRO-H should be able to spectroscopically resolve the fast flows near the centers of nearby, well-resolved clusters, in which the spiral is not observed face-on (alongẑ).…”

Section: Summary and Discussionmentioning

confidence: 99%

Spiral Flows in Cool-Core Galaxy Clusters

Keshet

2012

ApJ

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We argue that bulk spiral flows are ubiquitous in the cool cores (CCs) of clusters and groups of galaxies. Such flows are gauged by spiral features in the thermal and chemical properties of the intracluster medium, by the multiphase properties of CCs, and by X-ray edges known as cold fronts. We analytically show that observations of piecewise-spiral fronts impose strong constraints on the CC, implying the presence of a cold, fast flow, which propagates below a hot, slow inflow, separated by a slowly rotating, trailing, quasi-spiral, tangential discontinuity surface. This leads to the nearly logarithmic spiral pattern, two-phase plasma, ρ ∼ r −1 density (or T ∼ r 0.4 temperature) radial profile, and ∼100 kpc size, characteristic of CCs. By advecting heat and mixing the gas, such flows can eliminate the cooling problem, provided that a feedback mechanism regulates the flow. In particular, we present a quasi-steady-state model for an accretion-quenched, composite flow, in which the fast phase is an outflow, regulated by active galactic nucleus bubbles, reproducing the observed low star formation rates and explaining some features of bubbles such as their R b ∝ r size. The simplest two-component model reproduces several key properties of CCs, so we propose that all such cores harbor a spiral flow. Our results can be tested directly in the next few years, for example by ASTRO-H.

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Section: Summary and Discussionmentioning

confidence: 99%

Spiral Flows in Cool-Core Galaxy Clusters

Keshet

2012

ApJ

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“…We can assess the possibility of directly detecting the missing population of heavily obscured AGNs with future hard X-ray observatories. One of the science goals of several future hard X-ray missions, such as the Nuclear Spectroscopic Telescope Array (NuSTAR; Harrison et al 2010) and ASTRO-H (Takahashi et al 2010), is to resolve better the XRB at ≈10-30 keV via detecting heavily obscured and CT AGNs directly in the distant universe. While IR-selected heavily obscured AGN candidates at z ≈ 2 are likely below their sensitivity limits, 16 candidates at z ≈ 0.5-1 should be more easily detectable, and we will critically assess such possibilities.…”

Section: The Cdf-s and E-cdf-s Are Excellent Fields In Whichmentioning

confidence: 99%

“…Several future hard X-ray missions, such as NuSTAR (planned launch year 2012; Harrison et al 2010) and ASTRO-H (planned launch year 2014; Takahashi et al 2010), have as one science goal to detect hard X-ray emission from distant heavily obscured AGNs. For the three typical hard X-ray bands of NuSTAR, 6-10 keV, 10-30 keV, and 30-60 keV, the expected sensitivity limits are ≈2 × 10 −15 , 2 × 10 −14 , and 6 × 10 −14 erg cm −2 s −1 for a 1 Ms exposure, 27 respectively.…”

Section: Observational Prospects For Distant Heavily Obscured Agnsmentioning

confidence: 99%

REVEALING A POPULATION OF HEAVILY OBSCURED ACTIVE GALACTIC NUCLEI ATz≈ 0.5-1 IN THE CHANDRA DEEP FIELD-SOUTH

Brandt

Xue

Alexander

et al. 2011

ApJ

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Heavily obscured (N H 3 × 10 23 cm −2 ) Active Galactic Nuclei (AGNs) not detected in even the deepest X-ray surveys are often considered to be comparably numerous to the unobscured and moderately obscured AGNs. Such sources are required to fit the cosmic X-ray background (XRB) emission in the 10-30 keV band. We identify a numerically significant population of heavily obscured AGNs at z ≈ 0.5-1 in the Chandra Deep Field-South (CDF-S) and Extended Chandra Deep Field-South by selecting 242 X-ray undetected objects with infrared-based star formation rates (SFRs) substantially higher (a factor of 3.2 or more) than their SFRs determined from the UV after correcting for dust extinction. An X-ray stacking analysis of 23 candidates in the central CDF-S region using the 4 Ms Chandra data reveals a hard X-ray signal with an effective power-law photon index of Γ = 0.6 +0.3 −0.4 , indicating a significant contribution from obscured AGNs. Based on Monte Carlo simulations, we conclude that 74 ± 25% of the selected galaxies host obscured AGNs, within which ≈ 95% are heavily obscured and ≈ 80% are Compton-thick (CT; N H > 1.5 × 10 24 cm −2 ). The heavily obscured objects in our sample are of moderate intrinsic X-ray luminosity [≈ (0.9-4) × 10 42 erg s −1 in the 2-10 keV band]. The space density of the CT AGNs is (1.6 ± 0.5) × 10 −4 Mpc −3 . The z ≈ 0.5-1 CT objects studied here are expected to contribute ≈ 1% of the total XRB flux in the 10-30 keV band, and they account for ≈ 5-15% of the emission in this energy band expected from all CT AGNs according to population-synthesis models. In the 6-8 keV band, the stacked signal of the 23 heavily obscured candidates accounts for < 5% of the unresolved XRB flux, while the unresolved ≈ 25% of the XRB in this band can probably be explained by a stacking analysis of the X-ray undetected optical galaxies in the CDF-S (a 2.5 σ stacked signal). We discuss prospects to identify such heavily obscured objects using future hard X-ray observatories.

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“…• Effective area for the detector must be >20 cm 2 at 100 keV to obtain sufficient number of photons in a reasonable observation time (typically 100 ks).…”

Section: Instrument Conceptmentioning

confidence: 99%

Design and performance of Soft Gamma-ray Detector onboard the Hitomi (ASTRO-H) satellite

Tajima

Watanabe

Fukazawa

et al. 2018

J. Astron. Telesc. Instrum. Syst.

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Abstract. Hitomi (ASTRO-H) was the sixth Japanese x-ray satellite that carried instruments with exquisite energy resolution of <7 eV and broad energy coverage of 0.3 to 600 keV. The Soft Gamma-ray Detector (SGD) was the Hitomi instrument that observed the highest energy band (60 to 600 keV). The SGD design achieves a low background level by combining active shields and Compton cameras where Compton kinematics is utilized to reject backgrounds coming from outside of the field of view. A compact and highly efficient Compton camera is realized using a combination of silicon and cadmium telluride semiconductor sensors with a good energy resolution. Compton kinematics also carries information for gamma-ray polarization, making the SGD an excellent polarimeter. Following several years of development, the satellite was successfully launched on February 17, 2016. After proper functionality of the SGD components were verified, the nominal observation mode was initiated on March 24, 2016. The SGD observed the Crab Nebula for approximately two hours before the spacecraft ceased to function on March 26, 2016. We present concepts of the SGD design followed by detailed description of the instrument and its performance measured on ground and in orbit. © The Authors.Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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The ASTRO-H Mission

Cited by 130 publications

References 38 publications

Spiral Flows in Cool-Core Galaxy Clusters

Spiral Flows in Cool-Core Galaxy Clusters

REVEALING A POPULATION OF HEAVILY OBSCURED ACTIVE GALACTIC NUCLEI ATz≈ 0.5-1 IN THE CHANDRA DEEP FIELD-SOUTH

Design and performance of Soft Gamma-ray Detector onboard the Hitomi (ASTRO-H) satellite

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