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TERADA Yukikatsu
| Material Science Division | Professor |
| Physics |
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Researcher information
■ Degree■ Research Keyword
- CTA project, Gamma-ray observation, high energy astrophysical objects
- Astro-H satellite, X-ray observation, high energy astrophysical objects
- Suzaku satellite, X-ray observation, high energy astrophysical objects
- High energy astrophysical objects
- Gamma-ray
- X-ray
- Space Experiment
- Astrophysics
■ Career
- Oct. 2007 - Present, Saitama Univ., Graduate School of Science and Engineering, Associated Prof.
- 01 Oct. 2003 - 30 Sep. 2007
- 01 Mar. 2003 - 30 Sep. 2003
- 01 Apr. 2002 - 28 Feb. 2003
- Apr. 1999 - 2002, The University of Tokyo, Japan
- Apr. 1997 - Mar. 1999, The University of Tokyo, Japan
- Apr. 1993 - Mar. 1997, University of Tokyo
Performance information
■ Paper- Development and quality control of PMT modules for the large-sized telescopes of the Cherenkov Telescope Array Observatory
Saito, T.; Takahashi, M.; Inome, Y.; Abe, H.; Artero, M.; Blanch, O.; Becerra González, J.; Fukami, S.; Hadasch, D.; Hanabata, Y.; Hattori, Y.; Herrera Llorente, J.; Ishio, K.; Iwasaki, H.; Katagiri, H.; Kawamura, K.; Kerszberg, D.; Kimura, S.; Kiyomoto, T.; Kojima, T.; Konno, Y.; Kobayashi, Y.; Koyama, S.; Kubo, H.; Kushida, J.; López-Oramas, A.; Masuda, S.; Matsuoka, S.; Mazin, D.; Nakajima, D.; Nakamori, T.; Nagayoshi, T.; Ninci, D.; Nishijima, K.; Nishiyama, G.; Nogami, Y.; Nozaki, S.; Ogino, M.; Ohoka, H.; Oka, T.; Ono, S.; Okumura, A.; Orito, R.; Rugliancich, A.; Sakurai, S.; Sasaki, N.; Sunada, Y.; Suzuki, M.; Tamura, K.; Takeda, J.; Terada, Y.; Teshima, M.; Tokanai, F.; Tomono, Y.; Tsujimoto, S.; Tsukamoto, Y.; Umetsu, Y.; Yamamoto, T.; Yoshida, T.
Nuclear Instruments and Methods in Physics Research A, Apr. 2025, [Reviewed]
The camera of the Large-Sized Telescopes (LSTs) of the Cherenkov Telescope Array Observatory (CTAO) consists of 1855 pixels that are grouped into 265 high-performance photomultiplier tube (PMT) modules. Each module comprises a seven-light-guide plate, seven PMT units, a slow control board, and a readout board with a trigger board. The requirements for the PMT modules include various aspects, such as photon detection efficiency, dynamic range, buffer depth, and test pulse functionality. We have developed a high-performance PMT module that fulfills all these requirements. Mass-production and quality control (QC) of modules for all four LSTs of the northern CTAO have been completed. Here we report on the technical details of each element of the module and its performance, together with the methods and results of QC measurements....
Scientific journal
DOI：https://doi.org/10.1016/j.nima.2025.170229
DOI ID：10.1016/j.nima.2025.170229, ORCID：181063603, arXiv ID：arXiv:2502.02045, Bibcode：2025NIMPA107370229S - XRISM/Xtend Transient Search (XTS) detected an X-ray flare at the galactic center
Yoneyama, T.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nagashima, N.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Sugai, H.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoshimoto, M.
Mar. 2025
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1747-2832 located at the Galactic central region on 2025-03-19 TT. The source position is determined to be (R.A., Dec.) = (266.761, -28.538), with a systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181063681, Bibcode：2025ATel17092....1Y - XRISM follow-up observation of a new transient MAXI J1744-294 at the Galactic central region
Mandel, S.; Mori, K.; Hailey, C.; Bachetti, M.; Degenaar, N.; Draghis, P.; Grindlay, J.; Hong, J.; Ponti, G.; Reynolds, M.; Tomsick, J.; Wijnands, R.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Iizuka, R.; Baluta, C.; Terada, Y.; Costantini, E.; Guainazzi, M.; Kelley, R.; Matsushita, K.; Petre, R.; Williams, B.; Yamaguchi, H.; Watanabe, S.; Tashiro, M.
Mar. 2025
A follow-up XRISM observation has been performed for the new Galactic centre transient MAXI J1744-294 detected by MAXI on January 2, 2025 (ATels #16975 and #16983)....
The Astronomer's Telegram
ORCID：181063684, Bibcode：2025ATel17063....1M - XRISM/Xtend Transient Search (XTS) detected an X-ray high state of 2SXPS J171724.0-371717
Sugai, H.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nagashima, N.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Mar. 2025
XRISM/Xtend Transient Search (XTS) detected an increase in X-ray intensity from an X-ray source XRISM J1717-3717 on 2025-02-28 TT. The source position is determined to be (R.A., Dec.) = (259.347, -37.28648), with a systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181063685, Bibcode：2025ATel17060....1S - XRISM/Xtend Transient Search (XTS) detected an X-ray flare from a YSO candidate
Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nagashima, N.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Sugai, H.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Mar. 2025
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1718-3711 on 2025-03-06 TT. The source position is determined to be (R.A., Dec.) = (259.375, -37.183), with a systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181063683, Bibcode：2025ATel17067....1F - XRISM/Xtend Transient Search (XTS) detected an X-ray flare possibly from an M dwarf star
Yoneyama, T.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nagashima, N.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Sugai, H.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoshimoto, M.
Mar. 2025
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1748-2832 on 2025-03-09 TT. The source position is determined to be (R.A., Dec.) = (266.890 -28.538), with a systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181063682, Bibcode：2025ATel17071....1Y - Detection of RS Oph with LST-1 and modelling of its HE/VHE gamma-ray emission
Abe, K.; Abe, S.; Abhishek, A.; Acero, F.; Aguasca-Cabot, A.; Agudo, I.; Alispach, C.; Alvarez Crespo, N.; Ambrosino, D.; Antonelli, L. A.; Aramo, C.; Arbet-Engels, A.; Arcaro, C.; Asano, K.; Aubert, P.; Baktash, A.; Balbo, M.; Bamba, A.; Baquero Larriva, A.; Barres de Almeida, U.; Barrio, J. A.; Barrios Jiménez, L.; Batkovic, I.; Baxter, J.; Becerra González, J.; Bernardini, E.; Bernete, J.; Berti, A.; Bezshyiko, I.; Bhattacharjee, P.; Bigongiari, C.; Bissaldi, E.; Blanch, O.; Bonnoli, G.; Bordas, P.; Borkowski, G.; Brunelli, G.; Bulgarelli, A.; Bunse, M.; Burelli, I.; Burmistrov, L.; Buscemi, M.; Cardillo, M.; Caroff, S.; Carosi, A.; Carrasco, M. S.; Cassol, F.; Castrejón, N.; Cerasole, D.; Ceribella, G.; Chai, Y.; Cheng, K.; Chiavassa, A.; Chikawa, M.; Chon, G.; Chytka, L.; Cicciari, G. M.; Cifuentes, A.; Contreras, J. L.; Cortina, J.; Costantini, H.; Da Vela, P.; Dalchenko, M.; Dazzi, F.; De Angelis, A.; de Bony de Lavergne, M.; De Lotto, B.; de Menezes, R.; Del Burgo, R.; Del Peral, L.; Delgado, C.; Delgado Mengual, J.; della Volpe, D.; Dellaiera, M.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Díaz, C.; Dominik, R. M.; Dominis Prester, D.; Donini, A.; Dore, D.; Dorner, D.; Doro, M.; Eisenberger, L.; Elsässer, D.; Emery, G.; Escudero, J.; Fallah Ramazani, V.; Ferrarotto, F.; Fiasson, A.; Foffano, L.; Freixas Coromina, L.; Fröse, S.; Fukazawa, Y.; Garcia López, R.; Gasbarra, C.; Gasparrini, D.; Geyer, D.; Giesbrecht Paiva, J.; Giglietto, N.; Giordano, F.; Gliwny, P.; Godinovic, N.; Grau, R.; Green, D.; Green, J.; Gunji, S.; Günther, P.; Hackfeld, J.; Hadasch, D.; Hahn, A.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Herrera Llorente, J.; Hirotani, K.; Hoffmann, D.; Horns, D.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Hui, D.; Iarlori, M.; Imazawa, R.; Inada, T.; Inome, Y.; Inoue, S.; Ioka, K.; Iori, M.; Iuliano, A.; Jahanvi, J.; Jimenez Martinez, I.; Jimenez Quiles, J.; Jurysek, J.; Kagaya, M.; Kalashev, O.; Karas, V.; Katagiri, H.; Kataoka, J.; Kerszberg, D.; Kobayashi, Y.; Kohri, K.; Kong, A.; Kubo, H.; Kushida, J.; Lacave, B.; Lainez, M.; Lamanna, G.; Lamastra, A.; Lemoigne, L.; Linhoff, M.; Longo, F.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Lorini, A.; Lozano Bahilo, J.; Luciani, H.; Luque-Escamilla, P. L.; Majumdar, P.; Makariev, M.; Mallamaci, M.; Mandat, D.; Manganaro, M.; Manicò, G.; Mannheim, K.; Marchesi, S.; Mariotti, M.; Marquez, P.; Marsella, G.; Martí, J.; Martinez, O.; Martínez, G.; Martínez, M.; Mas-Aguilar, A.; Maurin, G.; Mazin, D.; Méndez-Gallego, J.; Menon, S.; Mestre Guillen, E.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Molero Gonzalez, M.; Molina, E.; Montaruli, T.; Moralejo, A.; Morcuende, D.; Morselli, A.; Moya, V.; Muraishi, H.; Nagataki, S.; Nakamori, T.; Neronov, A.; Nickel, L.; Nieto Castaño, D.; Nievas Rosillo, M.; Nikolic, L.; Nishijima, K.; Noda, K.; Nosek, D.; Novotny, V.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Oka, T.; Okumura, A.; Orito, R.; Otero-Santos, J.; Ottanelli, P.; Owen, E.; Palatiello, M.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Pech, M.; Pecimotika, M.; Peresano, M.; Pfeifle, F.; Pietropaolo, E.; Pihet, M.; Pirola, G.; Plard, C.; Podobnik, F.; Pons, E.; Prandini, E.; Prouza, M.; Rainò, S.; Rando, R.; Rhode, W.; Ribó, M.; Righi, C.; Rizi, V.; Rodriguez Fernandez, G.; Rodríguez Frías, M. D.; Romano, P.; Ruina, A.; Ruiz-Velasco, E.; Saito, T.; Sakurai, S.; Sanchez, D. A.; Sano, H.; Šarić, T.; Sato, Y.; Saturni, F. G.; Savchenko, V.; Schiavone, F.; Schleicher, B.; Schmuckermaier, F.; Schubert, J. L.; Schussler, F.; Schweizer, T.; Seglar Arroyo, M.; Siegert, T.; Simongini, A.; Sitarek, J.; Sliusar, V.; Stamerra, A.; Strišković, J.; Strzys, M.; Suda, Y.; Sunny, A.; Tajima, H.; Takahashi, H.; Takahashi, M.; Takata, J.; Takeishi, R.; Tam, P. H. T.; Tanaka, S. J.; Tateishi, D.; Tavernier, T.; Temnikov, P.; Terada, Y.; Terauchi, K.; Terzic, T.; Teshima, M.; Tluczykont, M.; Toennis, C.; Tokanai, F.; Torres, D. F.; Travnicek, P.; Tutone, A.; Vacula, M.; van Scherpenberg, J.; Vázquez Acosta, M.; Ventura, S.; Vercellone, S.; Verna, G.; Viale, I.; Vigliano, A.; Vigorito, C. F.; Visentin, E.; Vitale, V.; Voitsekhovskyi, V.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Walter, R.; Wan, L.; Will, M.; Wójtowicz, J.; Yamamoto, T.; Yamazaki, R.; Yao, Y.; Yeung, P. K. H.; Yoshida, T.; Yoshikoshi, T.; Zhang, W.; Zywucka, N.
Astronomy and Astrophysics, Mar. 2025, [Reviewed]
Context. The recurrent nova RS Ophiuchi (RS Oph) underwent a thermonuclear eruption in August 2021. In this event, RS Oph was detected by the High Energy Stereoscopic System (H.E.S.S.), the Major Atmospheric Gamma Imaging Cherenkov (MAGIC), and the first Large-Sized Telescope (LST-1) of the future Cherenkov Telescope Array Observatory (CTAO) at very-high gamma-ray energies above 100 GeV. This means that novae are a new class of very-high-energy (VHE) gamma-ray emitters. Aims. We report the analysis of the RS Oph observations with LST-1. We constrain the particle population that causes the observed emission in hadronic and leptonic scenarios. Additionally, we study the prospects of detecting further novae using LST-1 and the upcoming LST array of CTAO-North. Methods. We conducted target-of-opportunity observations with LST-1 from the first day of this nova event. The data were analysed in the framework of cta-lstchain and Gammapy, the official CTAO-LST reconstruction and analysis packages. One-zone hadronic and leptonic models were considered to model the gamma-ray emission of RS Oph using the spectral information from Fermi-LAT and LST-1, together with public data from the MAGIC and H.E.S.S. telescopes. Results. RS Oph was detected at 6.6σ with LST-1 in the first 6.35 hours of observations following the eruption. The hadronic scenario is preferred over the leptonic scenario considering a proton energy spectrum with a power-law model with an exponential cutoff whose position increases from (0.26 ± 0.08) TeV on day 1 up to (1.6 ± 0.6) TeV on day 4 after the eruption. The deep sensitivity and low energy threshold of the LST-1/LST array will allow us to detect faint novae and increase their discovery rate....
Scientific journal
DOI：https://doi.org/10.1051/0004-6361/202452447
DOI ID：10.1051/0004-6361/202452447, ORCID：181063601, arXiv ID：arXiv:2503.13283, Bibcode：2025A&A...695A.152A - XRISM Reveals Low Nonthermal Pressure in the Core of the Hot, Relaxed Galaxy Cluster A2029
Xrism Collaboration; Audard, Marc; Awaki, Hisamitsu; Ballhausen, Ralf; Bamba, Aya; Behar, Ehud; Boissay-Malaquin, Rozenn; Brenneman, Laura; Brown, Gregory V.; Corrales, Lia; Costantini, Elisa; Cumbee, Renata; Diaz Trigo, Maria; Done, Chris; Dotani, Tadayasu; Ebisawa, Ken; Eckart, Megan E.; Eckert, Dominique; Eguchi, Satoshi; Enoto, Teruaki; Ezoe, Yuichiro; Foster, Adam; Fujimoto, Ryuichi; Fujita, Yutaka; Fukazawa, Yasushi; Fukushima, Kotaro; Furuzawa, Akihiro; Gallo, Luigi; García, Javier A.; Gu, Liyi; Guainazzi, Matteo; Hagino, Kouichi; Hamaguchi, Kenji; Hatsukade, Isamu; Hayashi, Katsuhiro; Hayashi, Takayuki; Hell, Natalie; Hodges-Kluck, Edmund; Hornschemeier, Ann; Ichinohe, Yuto; Ishida, Manabu; Ishikawa, Kumi; Ishisaki, Yoshitaka; Kaastra, Jelle; Kallman, Timothy; Kara, Erin; Katsuda, Satoru; Kanemaru, Yoshiaki; Kelley, Richard; Kilbourne, Caroline; Kitamoto, Shunji; Kobayashi, Shogo; Kohmura, Takayoshi; Kubota, Aya; Leutenegger, Maurice; Loewenstein, Michael; Maeda, Yoshitomo; Markevitch, Maxim; Matsumoto, Hironori; Matsushita, Kyoko; McCammon, Dan; McNamara, Brian; Mernier, François; Miller, Eric D.; Miller, Jon M.; Mitsuishi, Ikuyuki; Mizumoto, Misaki; Mizuno, Tsunefumi; Mori, Koji; Mukai, Koji; Murakami, Hiroshi; Mushotzky, Richard; Nakajima, Hiroshi; Nakazawa, Kazuhiro; Ness, Jan-Uwe; Nobukawa, Kumiko; Nobukawa, Masayoshi; Noda, Hirofumi; Odaka, Hirokazu; Ogawa, Shoji; Ogorzalek, Anna; Okajima, Takashi; Ota, Naomi; Paltani, Stephane; Petre, Robert; Plucinsky, Paul; Porter, Frederick S.; Pottschmidt, Katja; Sato, Kosuke; Sato, Toshiki; Sawada, Makoto; Seta, Hiromi; Shidatsu, Megumi; Simionescu, Aurora; Smith, Randall; Suzuki, Hiromasa; Szymkowiak, Andrew; Takahashi, Hiromitsu; Takeo, Mai; Tamagawa, Toru; Tamura, Keisuke; Tanaka, Takaaki; Tanimoto, Atsushi; Tashiro, Makoto; Terada, Yukikatsu; Terashima, Yuichi; Tsuboi, Yohko; Tsujimoto, Masahiro; Tsunemi, Hiroshi; Tsuru, Takeshi; Uchida, Hiroyuki; Uchida, Nagomi; Uchida, Yuusuke; Uchiyama, Hideki; Ueda, Yoshihiro; Uno, Shinichiro; Vink, Jacco; Watanabe, Shin; Williams, Brian J.; Yamada, Satoshi; Yamada, Shinya; Yamaguchi, Hiroya; Yamaoka, Kazutaka; Yamasaki, Noriko; Yamauchi, Makoto; Yamauchi, Shigeo; Yaqoob, Tahir; Yoneyama, Tomokage; Yoshida, Tessei; Yukita, Mihoko; Zhuravleva, Irina; Bartalesi, Tommaso; Ettori, Stefano; Kosarzycki, Roman; Lovisari, Lorenzo; Rose, Tom; Sarkar, Arnab; Sun, Ming; Tamhane, Prathamesh
The Astrophysical Journal, Mar. 2025, [Reviewed]
We present XRISM Resolve observations of the core of the hot, relaxed galaxy cluster Abell 2029 (A2029). We find that the line-of-sight bulk velocity of the intracluster medium (ICM) within the central 180 kpc is at rest with respect to the brightest cluster galaxy, with a 3σ upper limit of ∣vbulk∣ < 100 km s‑1. We robustly measure the field-integrated ICM velocity dispersion to be σv = 169 ± 10 km s‑1, obtaining similar results for both single-temperature and two-temperature plasma models to account for the cluster cool core. This result, if ascribed to isotropic turbulence, implies a subsonic ICM with Mach number
Scientific journal
DOI：https://doi.org/10.3847/2041-8213/ada7cd
DOI ID：10.3847/2041-8213/ada7cd, ORCID：181063602, arXiv ID：arXiv:2501.05514, Bibcode：2025ApJ...982L...5X - Development of the Timing System for the X-Ray Imaging and Spectroscopy Mission
Terada, Yukikatsu; Shidatsu, Megumi; Sawada, Makoto; Kominato, Takashi; Kato, So; Sato, Ryohei; Sakama, Minami; Shioiri, Takumi; Niida, Yuki; Natsukari, Chikara; Tashiro, Makoto S; Toda, Kenichi; Maejima, Hironori; Hayashi, Katsuhiro; Yoshida, Tessei; Ogawa, Shoji; Kanemaru, Yoshiaki; Hoshino, Akio; Fukushima, Kotaro; Takahashi, Hiromitsu; Nobukawa, Masayoshi; Mizuno, Tsunefumi; Nakazawa, Kazuhiro; Uno, Shin'ichiro; Ebisawa, Ken; Eguchi, Satoshi; Katsuda, Satoru; Kubota, Aya; Ota, Naomi; Tanimoto, Atsushi; Terashima, Yuichi; Tsuboi, Yohko; Uchida, Yuusuke; Uchiyama, Hideki; Yamauchi, Shigeo; Yoneyama, Tomokage; Yamada, Satoshi; Uchida, Nagomi; Watanabe, Shin; Iizuka, Ryo; Sato, Rie; Baluta, Chris; Holland, Matt; Loewenstein, Michael; Miller, Eric D; Yaqoob, Tahir; Hill, Robert S.; Waddy, Morgan D.; Mekosh, Mark; Fox, Joseph B.; Aldoretta, Emily; Brewer, Isabella; Mukai, Koji; Hamaguchi, Kenji; Mernier, Francois; Ogorzalek, Anna; Pottschmidt, Katja; Yukita, Mihoko; Takagi, Toshihiro; Motogami, Yugo; Enoto, Teruaki; Tanaka, Takaaki; Nakamoto, Taichi; Kang, Chulsoo; Miyazaki, Tsuyoshi
Mar. 2025
This paper describes the development, design, ground verification, and in-orbit verification, performance measurement, and calibration of the timing system for the X-Ray Imaging and Spectroscopy Mission (XRISM). The scientific goals of the mission require an absolute timing accuracy of 1.0~ms. All components of the timing system were designed and verified to be within the timing error budgets, which were assigned by component to meet the requirements. After the launch of XRISM, the timing capability of the ground-tuned timing system was verified using the millisecond pulsar PSR~B1937+21 during the commissioning period, and the timing jitter of the bus and the ground component were found to be below $15~\mu$s compared to the NICER (Neutron star Interior Composition ExploreR) profile. During the performance verification and calibration period, simultaneous observations of the Crab pulsar by XRISM, NuSTAR (Nuclear Spectroscopic Telescope Array), and NICER were made to measure the absolute timing offset of the system, showing that the arrival time of the main pulse with XRISM was aligned with that of NICER and NuSTAR to within $200~\mu$s. In conclusion, the absolute timing accuracy of the bus and the ground component of the XRISM timing system meets the timing error budget of $500~\mu$s....
arXiv e-prints
DOI：https://doi.org/10.48550/arXiv.2503.13807
DOI ID：10.48550/arXiv.2503.13807, ORCID：181063624, arXiv ID：arXiv:2503.13807, Bibcode：2025arXiv250313807T - The bulk motion of gas in the core of the Centaurus galaxy cluster
Xrism Collaboration; Audard, Marc; Awaki, Hisamitsu; Ballhausen, Ralf; Bamba, Aya; Behar, Ehud; Boissay-Malaquin, Rozenn; Brenneman, Laura; Brown, Gregory V.; Corrales, Lia; Costantini, Elisa; Cumbee, Renata; Done, Chris; Dotani, Tadayasu; Ebisawa, Ken; Eckart, Megan E.; Eckert, Dominique; Enoto, Teruaki; Eguchi, Satoshi; Ezoe, Yuichiro; Foster, Adam; Fujimoto, Ryuichi; Fujita, Yutaka; Fukazawa, Yasushi; Fukushima, Kotaro; Furuzawa, Akihiro; Gallo, Luigi; García, Javier A.; Gu, Liyi; Guainazzi, Matteo; Hagino, Kouichi; Hamaguchi, Kenji; Hatsukade, Isamu; Hayashi, Katsuhiro; Hayashi, Takayuki; Hell, Natalie; Hodges-Kluck, Edmund; Hornschemeier, Ann; Ichinohe, Yuto; Ishida, Manabu; Ishikawa, Kumi; Ishisaki, Yoshitaka; Kaastra, Jelle; Kallman, Timothy; Kara, Erin; Katsuda, Satoru; Kanemaru, Yoshiaki; Kelley, Richard; Kilbourne, Caroline; Kitamoto, Shunji; Kobayashi, Shogo; Kohmura, Takayoshi; Kubota, Aya; Leutenegger, Maurice; Loewenstein, Michael; Maeda, Yoshitomo; Markevitch, Maxim; Matsumoto, Hironori; Matsushita, Kyoko; McCammon, Dan; McNamara, Brian; Mernier, François; Miller, Eric D.; Miller, Jon M.; Mitsuishi, Ikuyuki; Mizumoto, Misaki; Mizuno, Tsunefumi; Mori, Koji; Mukai, Koji; Murakami, Hiroshi; Mushotzky, Richard; Nakajima, Hiroshi; Nakazawa, Kazuhiro; Ness, Jan-Uwe; Nobukawa, Kumiko; Nobukawa, Masayoshi; Noda, Hirofumi; Odaka, Hirokazu; Ogawa, Shoji; Ogorzalek, Anna; Okajima, Takashi; Ota, Naomi; Paltani, Stephane; Petre, Robert; Plucinsky, Paul; Porter, Frederick Scott; Pottschmidt, Katja; Sato, Kosuke; Sato, Toshiki; Sawada, Makoto; Seta, Hiromi; Shidatsu, Megumi; Simionescu, Aurora; Smith, Randall; Suzuki, Hiromasa; Szymkowiak, Andrew; Takahashi, Hiromitsu; Takeo, Mai; Tamagawa, Toru; Tamura, Keisuke; Tanaka, Takaaki; Tanimoto, Atsushi; Tashiro, Makoto; Terada, Yukikatsu; Terashima, Yuichi; Trigo, María Díaz; Tsuboi, Yohko; Tsujimoto, Masahiro; Tsunemi, Hiroshi; Tsuru, Takeshi G.; Uchida, Hiroyuki; Uchida, Nagomi; Uchida, Yuusuke; Uchiyama, Hideki; Ueda, Yoshihiro; Uno, Shinichiro; Vink, Jacco; Watanabe, Shin; Williams, Brian J.; Yamada, Satoshi; Yamada, Shinya; Yamaguchi, Hiroya; Yamaoka, Kazutaka; Yamasaki, Noriko Y.; Yamauchi, Makoto; Yamauchi, Shigeo; Yaqoob, Tahir; Yoneyama, Tomokage; Yoshida, Tessei; Yukita, Mihoko; Zhuravleva, Irina; Kondo, Marie; Werner, Norbert; Plšek, Tomáš; Sun, Ming; Hosogi, Kokoro; Majumder, Anwesh
Nature, Feb. 2025, [Reviewed]
Galaxy clusters contain vast amounts of hot ionized gas known as the intracluster medium (ICM). In relaxed cluster cores, the radiative cooling time of the ICM is shorter than the age of the cluster. However, the absence of line emission associated with cooling suggests heating mechanisms that offset the cooling, with feedback from active galactic nuclei (AGNs) being the most likely source1,2. Turbulence and bulk motions, such as the oscillating ('sloshing') motion of the core gas in the cluster potential well, have also been proposed as mechanisms for heat distribution from the outside of the core3,4. Here we present X-ray spectroscopic observations of the Centaurus galaxy cluster with the X-Ray Imaging and Spectroscopy Mission satellite. We find that the hot gas flows along the line of sight relative to the central galaxy, with velocities from 130 km s‑1 to 310 km s‑1 within about 30 kpc of the centre. This indicates bulk flow consistent with core gas sloshing. Although the bulk flow may prevent excessive accumulation of cooled gas at the centre, it could distribute the heat injected by the AGN and bring in thermal energy from the surrounding ICM. The velocity dispersion of the gas is found to be only ≲120 km s‑1 in the core, even within about 10 kpc of the AGN. This suggests that the influence of the AGN on the surrounding ICM motion is limited in the cluster....
Scientific journal
DOI：https://doi.org/10.1038/s41586-024-08561-z
DOI ID：10.1038/s41586-024-08561-z, ORCID：181063599, arXiv ID：arXiv:2502.08722, Bibcode：2025Natur.638..365X - XRISM/Xtend Transient Search (XTS) detected an X-ray flare from High Proper Motion Star UCAC4 661-042690
Sugai, H.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nagashima, N.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Feb. 2025
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J0604+4209 on 2025-02-23 TT. The source position is determined to be (R.A., Dec.) = (90.974, 42.144), with a systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181063774, Bibcode：2025ATel17049....1S - Overionized plasma in the supernova remnant Sagittarius A East anchored by XRISM observations
XRISM Collaboration; Audard, Marc; Awaki, Hisamitsu; Ballhausen, Ralf; Bamba, Aya; Behar, Ehud; Boissay-Malaquin, Rozenn; Brenneman, Laura; Brown, Gregory V; Corrales, Lia; Costantini, Elisa; Cumbee, Renata; Diaz-Trigo, Maria; Done, Chris; Dotani, Tadayasu; Ebisawa, Ken; Eckart, Megan; Eckert, Dominique; Enoto, Teruaki; Eguchi, Satoshi; Ezoe, Yuichiro; Foster, Adam; Fujimoto, Ryuichi; Fujita, Yutaka; Fukazawa, Yasushi; Fukushima, Kotaro; Furuzawa, Akihiro; Gallo, Luigi; García, Javier A; Gu, Liyi; Guainazzi, Matteo; Hagino, Kouichi; Hamaguchi, Kenji; Hatsukade, Isamu; Hayashi, Katsuhiro; Hayashi, Takayuki; Hell, Natalie; Hodges-Kluck, Edmund; Hornschemeier, Ann; Ichinohe, Yuto; Ishida, Manabu; Ishikawa, Kumi; Ishisaki, Yoshitaka; Kaastra, Jelle; Kallman, Timothy; Kara, Erin; Katsuda, Satoru; Kanemaru, Yoshiaki; Kelley, Richard; Kilbourne, Caroline; Kitamoto, Shunji; Kobayashi, Shogo; Kohmura, Takayoshi; Kubota, Aya; Leutenegger, Maurice; Loewenstein, Michael; Maeda, Yoshitomo; Markevitch, Maxim; Matsumoto, Hironori; Matsushita, Kyoko; McCammon, Dan; McNamara, Brian; Mernier, François; Miller, Eric D; Miller, Jon M; Mitsuishi, Ikuyuki; Mizumoto, Misaki; Mizuno, Tsunefumi; Mori, Koji; Mukai, Koji; Murakami, Hiroshi; Mushotzky, Richard; Nakajima, Hiroshi; Nakazawa, Kazuhiro; Ness, Jan-Uwe; Nobukawa, Kumiko; Nobukawa, Masayoshi; Noda, Hirofumi; Odaka, Hirokazu; Ogawa, Shoji; Ogorzalek, Anna; Okajima, Takashi; Ota, Naomi; Paltani, Stephane; Petre, Robert; Plucinsky, Paul; Scott Porter, Frederick; Pottschmidt, Katja; Sato, Kosuke; Sato, Toshiki; Sawada, Makoto; Seta, Hiromi; Shidatsu, Megumi; Simionescu, Aurora; Smith, Randall; Suzuki, Hiromasa; Szymkowiak, Andrew; Takahashi, Hiromitsu; Takeo, Mai; Tamagawa, Toru; Tamura, Keisuke; Tanaka, Takaaki; Tanimoto, Atsushi; Tashiro, Makoto; Terada, Yukikatsu; Terashima, Yuichi; Tsuboi, Yohko; Tsujimoto, Masahiro; Tsunemi, Hiroshi; Tsuru, Takeshi G; Uchida, Hiroyuki; Uchida, Nagomi; Uchida, Yuusuke; Uchiyama, Hideki; Ueda, Yoshihiro; Uno, Shinichiro; Vink, Jacco; Watanabe, Shin; Williams, Brian J; Yamada, Satoshi; Yamada, Shinya; Yamaguchi, Hiroya; Yamaoka, Kazutaka; Yamasaki, Noriko; Yamauchi, Makoto; Yamauchi, Shigeo; Yaqoob, Tahir; Yoneyama, Tomokage; Yoshida, Tessei; Yukita, Mihoko; Zhuravleva, Irina; Wang, Q Daniel; Amano, Yuki; Tanaka, Kojiro; Narita, Takuto; Ohshiro, Yuken; Yoshimoto, Anje; Aoki, Yuma; Balakrishnan, Mayura
Publications of the Astronomical Society of Japan, Feb. 2025, [Reviewed]
Sagittarius A East is a supernova remnant with a unique surrounding environment, as it is located in the immediate vicinity of the supermassive black hole at the Galactic center, Sagittarius A$^{*}$ $1.39 \pm 0.12$ $\gt\! 4\:$ $\lt\! 8 \times 10^{11} \:$ $^{-3}\:$ $109 \pm 6\:$ $\:$ $^{-1}$ $\lt\! 8\:$ $\lt\! 200\:$ $\:$ $^{-1}$ $^{*}$
Scientific journal
DOI：https://doi.org/10.1093/pasj/psae111
DOI ID：10.1093/pasj/psae111, ORCID：181063703, Bibcode：2025PASJ...77L...1X - XRISM/Xtend Transient Search (XTS) detected an X-ray flare from the flare star HD 120476
Sugai, H.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nagashima, N.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Jan. 2025
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1349+2659 on 2025-01-21 TT. The source position is determined to be (R.A., Dec.) = (207.270, 26.975), with a systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181063777, Bibcode：2025ATel16990....1S - International Astrophysical Consortium for High-energy Calibration: Summary of the 16th IACHEC Workshop
Grant, C. E.; Madsen, K. K.; Burwitz, V.; Forster, K.; Guainazzi, M.; Kashyap, V. L.; Marshall, H. L.; Markwardt, C. B.; Miller, E. D.; Natalucci, L.; Plucinsky, P. P.; Shidatsu, M.; Terada, Y.
Jan. 2025
In this report we summarize the activities of the International Astronomical Consortium for High Energy Calibration (IACHEC) from the 16th IACHEC Workshop at Parador de La Granja, Spain. Sixty-one scientists directly involved in the calibration of operational and future high-energy missions gathered during 3.5 days to discuss the status of the cross-calibration between the current international complement of X-ray observatories, and the possibilities to improve it. This summary consists of reports from the Working Groups with topics ranging across: the identification and characterization of standard calibration sources, multi-observatory cross-calibration campaigns, appropriate and new statistical techniques, calibration of instruments and characterization of background, preservation of knowledge, and results for the benefit of the astronomical community....
arXiv e-prints
DOI：https://doi.org/10.48550/arXiv.2501.17199
DOI ID：10.48550/arXiv.2501.17199, ORCID：181063776, arXiv ID：arXiv:2501.17199, Bibcode：2025arXiv250117199G - The XRISM first-light observation: Velocity structure and thermal properties of the supernova remnant N 132D
XRISM Collaboration; Audard, Marc; Awaki, Hisamitsu; Ballhausen, Ralf; Bamba, Aya; Behar, Ehud; Boissay-Malaquin, Rozenn; Brenneman, Laura; Brown, Gregory V.; Corrales, Lia; Costantini, Elisa; Cumbee, Renata; Diaz-Trigo, Maria; Done, Chris; Dotani, Tadayasu; Ebisawa, Ken; Eckart, Megan; Eckert, Dominique; Enoto, Teruaki; Eguchi, Satoshi; Ezoe, Yuichiro; Foster, Adam; Fujimoto, Ryuichi; Fujita, Yutaka; Fukazawa, Yasushi; Fukushima, Kotaro; Furuzawa, Akihiro; Gallo, Luigi; García, Javier A.; Gu, Liyi; Guainazzi, Matteo; Hagino, Kouichi; Hamaguchi, Kenji; Hatsukade, Isamu; Hayashi, Katsuhiro; Hayashi, Takayuki; Hell, Natalie; Hodges-Kluck, Edmund; Hornschemeier, Ann; Ichinohe, Yuto; Ishida, Manabu; Ishikawa, Kumi; Ishisaki, Yoshitaka; Kaastra, Jelle; Kallman, Timothy; Kara, Erin; Katsuda, Satoru; Kanemaru, Yoshiaki; Kelley, Richard; Kilbourne, Caroline; Kitamoto, Shunji; Kobayashi, Shogo; Kohmura, Takayoshi; Kubota, Aya; Leutenegger, Maurice; Loewenstein, Michael; Maeda, Yoshitomo; Markevitch, Maxim; Matsumoto, Hironori; Matsushita, Kyoko; McCammon, Dan; McNamara, Brian; Mernier, François; Miller, Eric D.; Miller, Jon M.; Mitsuishi, Ikuyuki; Mizumoto, Misaki; Mizuno, Tsunefumi; Mori, Koji; Mukai, Koji; Murakami, Hiroshi; Mushotzky, Richard; Nakajima, Hiroshi; Nakazawa, Kazuhiro; Ness, Jan-Uwe; Nobukawa, Kumiko; Nobukawa, Masayoshi; Noda, Hirofumi; Odaka, Hirokazu; Ogawa, Shoji; Ogorzalek, Anna; Okajima, Takashi; Ota, Naomi; Paltani, Stephane; Petre, Robert; Plucinsky, Paul; Porter, Frederick Scott; Pottschmidt, Katja; Sato, Kosuke; Sato, Toshiki; Sawada, Makoto; Seta, Hiromi; Shidatsu, Megumi; Simionescu, Aurora; Smith, Randall; Suzuki, Hiromasa; Szymkowiak, Andrew; Takahashi, Hiromitsu; Takeo, Mai; Tamagawa, Toru; Tamura, Keisuke; Tanaka, Takaaki; Tanimoto, Atsushi; Tashiro, Makoto; Terada, Yukikatsu; Terashima, Yuichi; Tsuboi, Yohko; Tsujimoto, Masahiro; Tsunemi, Hiroshi; Tsuru, Takeshi G.; Uchida, Hiroyuki; Uchida, Nagomi; Uchida, Yuusuke; Uchiyama, Hideki; Ueda, Yoshihiro; Uno, Shinichiro; Vink, Jacco; Watanabe, Shin; Williams, Brian J.; Yamada, Satoshi; Yamada, Shinya; Yamaguchi, Hiroya; Yamaoka, Kazutaka; Yamasaki, Noriko; Yamauchi, Makoto; Yamauchi, Shigeo; Yaqoob, Tahir; Yoneyama, Tomokage; Yoshida, Tessei; Yukita, Mihoko; Zhuravleva, Irina; Agarwal, Manan; Ohshiro, Yuken
Publications of the Astronomical Society of Japan, Dec. 2024, [Reviewed]
We present an initial analysis of the X-Ray Imaging and Spectroscopy Mission (XRISM) first-light observation of the supernova remnant (SNR) N 132D in the Large Magellanic Cloud. The Resolve microcalorimeter has obtained the first high-resolution spectrum in the 1.6-10 keV band, which contains K-shell emission lines of Si, S, Ar, Ca, and Fe. We find that the Si and S lines are relatively narrow, with a broadening represented by a Gaussian-like velocity dispersion of$\sigma _v \sim 450$ $^{-1}$ $\alpha$ $\sigma _v \sim 1670$ $^{-1}$ $\alpha$ $-1000 \lesssim V_{\rm rs}$ $^{-1}$ $\lesssim 3300$ $\alpha$ $\sim 890$ $^{-1}$
Scientific journal
DOI：https://doi.org/10.1093/pasj/psae080
DOI ID：10.1093/pasj/psae080, ORCID：181063875, arXiv ID：arXiv:2408.14301, Bibcode：2024PASJ...76.1186X - The XRISM/Resolve View of the Fe K Region of Cyg X-3
Xrism Collaboration; Audard, Marc; Awaki, Hisamitsu; Ballhausen, Ralf; Bamba, Aya; Behar, Ehud; Boissay-Malaquin, Rozenn; Brenneman, Laura; Brown, Gregory V.; Corrales, Lia; Costantini, Elisa; Cumbee, Renata; Díaz Trigo, María; Done, Chris; Dotani, Tadayasu; Ebisawa, Ken; Eckart, Megan E.; Eckert, Dominique; Eguchi, Satoshi; Enoto, Teruaki; Ezoe, Yuichiro; Foster, Adam; Fujimoto, Ryuichi; Fujita, Yutaka; Fukazawa, Yasushi; Fukushima, Kotaro; Furuzawa, Akihiro; Gallo, Luigi; García, Javier A.; Gu, Liyi; Guainazzi, Matteo; Hagino, Kouichi; Hamaguchi, Kenji; Hatsukade, Isamu; Hayashi, Katsuhiro; Hayashi, Takayuki; Hell, Natalie; Hodges-Kluck, Edmund; Hornschemeier, Ann; Ichinohe, Yuto; Ishida, Manabu; Ishikawa, Kumi; Ishisaki, Yoshitaka; Kaastra, Jelle; Kallman, Timothy; Kara, Erin; Katsuda, Satoru; Kanemaru, Yoshiaki; Kelley, Richard; Kilbourne, Caroline; Kitamoto, Shunji; Kobayashi, Shogo; Kohmura, Takayoshi; Kubota, Aya; Leutenegger, Maurice; Loewenstein, Michael; Maeda, Yoshitomo; Markevitch, Maxim; Matsumoto, Hironori; Matsushita, Kyoko; McCammon, Dan; McNamara, Brian; Mernier, François; Miller, Eric D.; Miller, Jon M.; Mitsuishi, Ikuyuki; Mizumoto, Misaki; Mizuno, Tsunefumi; Mori, Koji; Mukai, Koji; Murakami, Hiroshi; Mushotzky, Richard; Nakajima, Hiroshi; Nakazawa, Kazuhiro; Ness, Jan-Uwe; Nobukawa, Kumiko; Nobukawa, Masayoshi; Noda, Hirofumi; Odaka, Hirokazu; Ogawa, Shoji; Ogorzalek, Anna; Okajima, Takashi; Ota, Naomi; Paltani, Stephane; Petre, Robert; Plucinsky, Paul; Porter, Frederick S.; Pottschmidt, Katja; Sato, Kosuke; Sato, Toshiki; Sawada, Makoto; Seta, Hiromi; Shidatsu, Megumi; Simionescu, Aurora; Smith, Randall; Suzuki, Hiromasa; Szymkowiak, Andrew; Takahashi, Hiromitsu; Takeo, Mai; Tamagawa, Toru; Tamura, Keisuke; Tanaka, Takaaki; Tanimoto, Atsushi; Tashiro, Makoto; Terada, Yukikatsu; Terashima, Yuichi; Tsuboi, Yohko; Tsujimoto, Masahiro; Tsunemi, Hiroshi; Tsuru, Takeshi; Uchida, Hiroyuki; Uchida, Nagomi; Uchida, Yuusuke; Uchiyama, Hideki; Ueda, Yoshihiro; Uno, Shinichiro; Vink, Jacco; Watanabe, Shin; Williams, Brian J.; Yamada, Satoshi; Yamada, Shinya; Yamaguchi, Hiroya; Yamaoka, Kazutaka; Yamasaki, Noriko; Yamauchi, Makoto; Yamauchi, Shigeo; Yaqoob, Tahir; Yoneyama, Tomokage; Yoshida, Tessei; Yukita, Mihoko; Zhuravleva, Irina; Tomaru, Ryota; Hayashi, Tasuku; Hakamata, Tomohiro; Miura, Daiki; Koljonen, Karri; McCollough, Mike
The Astrophysical Journal, Dec. 2024, [Reviewed]
The X-ray binary system Cygnus X-3 (4U 2030+40, V1521 Cyg) is luminous but enigmatic owing to the high intervening absorption. High-resolution X-ray spectroscopy uniquely probes the dynamics of the photoionized gas in the system. In this Letter, we report on an observation of Cyg X-3 with the XRISM/Resolve spectrometer, which provides unprecedented spectral resolution and sensitivity in the 2–10 keV band. We detect multiple kinematic and ionization components in absorption and emission whose superposition leads to complex line profiles, including strong P Cygni profiles on resonance lines. The prominent Fe XXV Heα and Fe XXVI Lyα emission complexes are clearly resolved into their characteristic fine-structure transitions. Self-consistent photoionization modeling allows us to disentangle the absorption and emission components and measure the Doppler velocity of these components as a function of binary orbital phase. We find a significantly higher velocity amplitude for the emission lines than for the absorption lines. The absorption lines generally appear blueshifted by ∼‑500–600 km s‑1. We show that the wind decomposes naturally into a relatively smooth and large-scale component, perhaps associated with the background wind itself, plus a turbulent, denser structure located close to the compact object in its orbit....
Scientific journal
DOI：https://doi.org/10.3847/2041-8213/ad8ed0
DOI ID：10.3847/2041-8213/ad8ed0, ORCID：181063589, arXiv ID：arXiv:2411.00597, Bibcode：2024ApJ...977L..34X - XRISM/Xtend Transient Search (XTS) detected an X-ray flare from XRISM J0057+6021
Nagashima, N.; Kanemaru, Y.; Yoshida, T.; Fukushima, K.; Hayashi, K.; Ogawa, S.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Sugai, H.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Dec. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J0057+6021 on 2024-12-29 TT. The source position is determined to be (R.A., Dec.) = (14.195, 60.356), with a systematic error of & #8764; 40 arcsec....
The Astronomer's Telegram
ORCID：181063877, Bibcode：2024ATel16962....1N - Container-Based Pre-Pipeline Data Processing on HPC for XRISM
Eguchi, Satoshi; Tashiro, Makoto; Terada, Yukikatsu; Takahashi, Hiromitsu; Nobukawa, Masayoshi; Ebisawa, Ken; Hayashi, Katsuhiro; Yoshida, Tessei; Kanemaru, Yoshiaki; Ogawa, Shoji; Holland, Matthew P.; Loewenstein, Michael; Miller, Eric D.; Yaqoob, Tahir; Hill, Robert S.; Waddy, Morgan D.; Mekosh, Mark M.; Fox, Joseph B.; Brewer, Isabella S.; Aldoretta, Emily; XRISM Science Operations Team
Dec. 2024
The X-Ray Imaging and Spectroscopy Mission (XRISM) is the 7th Japanese X-ray observatory, whose development and operation are in collaboration with universities and research institutes in Japan, U.S., and Europe, including JAXA, NASA, and ESA. The telemetry data downlinked from the satellite are reduced to scientific products by the pre-pipeline (PPL) and pipeline (PL) software running on standard Linux virtual machines on the JAXA and NASA sides, respectively. We ported the PPL to the JAXA "TOKI-RURI" high-performance computing (HPC) system capable of completing $\simeq 160$ PPL processes within 24 hours by utilizing the container platform of Singularity and its "--bind" option. In this paper, we briefly show the data processing in XRISM and present our porting strategy of PPL to the HPC environment in detail....
arXiv e-prints
DOI：https://doi.org/10.48550/arXiv.2412.13225
DOI ID：10.48550/arXiv.2412.13225, ORCID：181063891, arXiv ID：arXiv:2412.13225, Bibcode：2024arXiv241213225E - A new method of reconstructing images of gamma-ray telescopes applied to the LST-1 of CTAO
Abe, K.; Abe, S.; Abhishek, A.; Acero, F.; Aguasca-Cabot, A.; Agudo, I.; Alispach, C.; Alvarez Crespo, N.; Ambrosino, D.; Antonelli, L. A.; Aramo, C.; Arbet-Engels, A.; Arcaro, C.; Asano, K.; Aubert, P.; Baktash, A.; Balbo, M.; Bamba, A.; Baquero Larriva, A.; Barres de Almeida, U.; Barrio, J. A.; Barrios Jiménez, L.; Batkovic, I.; Baxter, J.; Becerra González, J.; Bernardini, E.; Bernete Medrano, J.; Berti, A.; Bezshyiko, I.; Bhattacharjee, P.; Bigongiari, C.; Bissaldi, E.; Blanch, O.; Bonnoli, G.; Bordas, P.; Borkowski, G.; Brunelli, G.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Buscemi, M.; Cardillo, M.; Caroff, S.; Carosi, A.; Carrasco, M. S.; Cassol, F.; Castrejón, N.; Cauz, D.; Cerasole, D.; Ceribella, G.; Chai, Y.; Cheng, K.; Chiavassa, A.; Chikawa, M.; Chon, G.; Chytka, L.; Cicciari, G. M.; Cifuentes, A.; Contreras, J. L.; Cortina, J.; Costantini, H.; Da Vela, P.; Dalchenko, M.; Dazzi, F.; De Angelis, A.; de Bony de Lavergne, M.; De Lotto, B.; de Menezes, R.; Del Burgo, R.; Del Peral, L.; Delgado, C.; Delgado Mengual, J.; della Volpe, D.; Dellaiera, M.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Díaz, C.; Dominik, R. M.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro, M.; Eisenberger, L.; Elsässer, D.; Emery, G.; Escudero, J.; Fallah Ramazani, V.; Ferrarotto, F.; Fiasson, A.; Foffano, L.; Freixas Coromina, L.; Fröse, S.; Fukazawa, Y.; Garcia López, R.; Gasbarra, C.; Gasparrini, D.; Geyer, D.; Giesbrecht Paiva, J.; Giglietto, N.; Giordano, F.; Gliwny, P.; Godinovic, N.; Grau, R.; Green, D.; Green, J.; Gunji, S.; Günther, P.; Hackfeld, J.; Hadasch, D.; Hahn, A.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Herrera Llorente, J.; Hirotani, K.; Hoffmann, D.; Horns, D.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Hui, D.; Iarlori, M.; Imazawa, R.; Inada, T.; Inome, Y.; Inoue, S.; Ioka, K.; Iori, M.; Iuliano, A.; Jimenez Martinez, I.; Jimenez Quiles, J.; Jurysek, J.; Kagaya, M.; Kalashev, O.; Karas, V.; Katagiri, H.; Kataoka, J.; Kerszberg, D.; Kobayashi, Y.; Kohri, K.; Kong, A.; Kubo, H.; Kushida, J.; Lainez, M.; Lamanna, G.; Lamastra, A.; Lemoigne, L.; Linhoff, M.; Longo, F.; López-Coto, R.; López-Oramas, A.; Loporchio, S.; Lorini, A.; Lozano Bahilo, J.; Luciani, H.; Luque-Escamilla, P. L.; Majumdar, P.; Makariev, M.; Mallamaci, M.; Mandat, D.; Manganaro, M.; Manicò, G.; Mannheim, K.; Marchesi, S.; Mariotti, M.; Marquez, P.; Marsella, G.; Martí, J.; Martinez, O.; Martínez, G.; Martínez, M.; Mas-Aguilar, A.; Maurin, G.; Mazin, D.; Méndez-Gallego, J.; Mestre Guillen, E.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Molero Gonzalez, M.; Molina, E.; Montaruli, T.; Moralejo, A.; Morcuende, D.; Morselli, A.; Moya, V.; Muraishi, H.; Nagataki, S.; Nakamori, T.; Neronov, A.; Nickel, L.; Nievas Rosillo, M.; Nikolic, L.; Nishijima, K.; Noda, K.; Nosek, D.; Novotny, V.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Oka, T.; Okumura, A.; Orito, R.; Otero-Santos, J.; Ottanelli, P.; Owen, E.; Palatiello, M.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Pech, M.; Pecimotika, M.; Peresano, M.; Pfeifle, F.; Pietropaolo, E.; Pihet, M.; Pirola, G.; Plard, C.; Podobnik, F.; Pons, E.; Prandini, E.; Priyadarshi, C.; Prouza, M.; Rainò, S.; Rando, R.; Rhode, W.; Ribó, M.; Righi, C.; Rizi, V.; Rodriguez Fernandez, G.; Rodríguez Frías, M. D.; Ruina, A.; Ruiz-Velasco, E.; Saito, T.; Sakurai, S.; Sanchez, D. A.; Sano, H.; Šarić, T.; Sato, Y.; Saturni, F. G.; Savchenko, V.; Schiavone, F.; Schleicher, B.; Schmuckermaier, F.; Schubert, J. L.; Schussler, F.; Schweizer, T.; Seglar Arroyo, M.; Siegert, T.; Sitarek, J.; Sliusar, V.; Strišković, J.; Strzys, M.; Suda, Y.; Tajima, H.; Takahashi, H.; Takahashi, M.; Takata, J.; Takeishi, R.; Tam, P. H. T.; Tanaka, S. J.; Tateishi, D.; Tavernier, T.; Temnikov, P.; Terada, Y.; Terauchi, K.; Terzic, T.; Teshima, M.; Tluczykont, M.; Tokanai, F.; Torres, D. F.; Travnicek, P.; Tutone, A.; Vacula, M.; Vallania, P.; van Scherpenberg, J.; Vázquez Acosta, M.; Ventura, S.; Verna, G.; Viale, I.; Vigliano, A.; Vigorito, C. F.; Visentin, E.; Vitale, V.; Voitsekhovskyi, V.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Walter, R.; Wan, L.; Will, M.; Wójtowicz, J.; Yamamoto, T.; Yamazaki, R.; Yeung, P. K. H.; Yoshida, T.; Yoshikoshi, T.; Zhang, W.; Zywucka, N.
Astronomy and Astrophysics, Nov. 2024, [Reviewed]
Context. Imaging atmospheric Cherenkov telescopes (IACTs) are used to observe very high-energy photons from the ground. Gamma rays are indirectly detected through the Cherenkov light emitted by the air showers they induce. The new generation of experiments, in particular the Cherenkov Telescope Array Observatory (CTAO), sets ambitious goals for discoveries of new gamma-ray sources and precise measurements of the already discovered ones. To achieve these goals, both hardware and data analysis must employ cuttingedge techniques. This also applies to the LST-1, the first IACT built for the CTAO, which is currently taking data on the Canary island of La Palma. Aims. This paper introduces a new event reconstruction technique for IACT data, aiming to improve the image reconstruction quality and the discrimination between the signal and the background from misidentified hadrons and electrons. Methods. The technique models the development of the extensive air shower signal, recorded as a waveform per pixel, seen by CTAO telescopes' cameras. Model parameters are subsequently passed to random forest regressors and classifiers to extract information on the primary particle. Results. The new reconstruction was applied to simulated data and to data from observations of the Crab Nebula performed by the LST-1. The event reconstruction method presented here shows promising performance improvements. The angular and energy resolution, and the sensitivity, are improved by 10 to 20% over most of the energy range. At low energy, improvements reach up to 22%, 47%, and 50%, respectively. A future extension of the method to stereoscopic analysis for telescope arrays will be the next important step....
Scientific journal
DOI：https://doi.org/10.1051/0004-6361/202450889
DOI ID：10.1051/0004-6361/202450889, ORCID：181063586, arXiv ID：arXiv:2410.16042, Bibcode：2024A&A...691A.328A - XRISM/Xtend Transient Search (XTS) detected an X-ray flare from EQ CVn
Maeda, Y.; Yoshida, T.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Nov. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1226+3347 on 2024-11-10 TT. The source position is determined to be (R.A., Dec.) = (186.488, 33.781), with a systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181063878, Bibcode：2024ATel16905....1M - Prospects for a survey of the galactic plane with the Cherenkov Telescope Array
Abe, S.; Abhir, J.; Abhishek, A.; Acero, F.; Acharyya, A.; Adam, R.; Aguasca-Cabot, A.; Agudo, I.; Aguirre-Santaella, A.; Alfaro, J.; Alvarez-Crespo, N.; Alves Batista, R.; Amans, J. -P.; Amato, E.; Ambrosi, G.; Ambrosino, F.; Angüner, E. O.; Aramo, C.; Arcaro, C.; Arrabito, L.; Asano, K.; Ascasíbar, Y.; Aschersleben, J.; Augusto Stuani, L.; Backes, M.; Balazs, C.; Balbo, M.; Ballet, J.; Baquero Larriva, A.; Barbosa Martins, V.; Barres de Almeida, U.; Barrio, J. A.; Batković, I.; Batzofin, R.; Baxter, J.; Becerra González, J.; Beck, G.; Beiske, L.; Belmont, R.; Benbow, W.; Bernardini, E.; Bernete, J.; Bernlöhr, K.; Berti, A.; Bertucci, B.; Beshley, V.; Bhattacharjee, P.; Bhattacharyya, S.; Bi, B.; Biederbeck, N.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Blazek, J.; Bocchino, F.; Boisson, C.; Bolmont, J.; Bonneau Arbeletche, L.; Bonnoli, G.; Bonollo, A.; Bordas, P.; Bosnjak, Z.; Bottacini, E.; Braiding, C.; Bronzini, E.; Brose, R.; Brown, A. M.; Brun, F.; Brunelli, G.; Bucciantini, N.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Burton, M.; Burtovoi, A.; Bylund, T.; Calisse, P. G.; Campoy-Ordaz, A.; Cantlay, B. K.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Caroff, S.; Carosi, A.; Carosi, R.; Carquin, E.; Carrasco, M. -S.; Cascone, E.; Cassol, F.; Castrejon, N.; Castro-Tirado, A. J.; Cerasole, D.; Cerruti, M.; Chadwick, P. M.; Chambery, P.; Chaty, S.; Chen, A. W.; Chernyakova, M.; Chiavassa, A.; Chytka, L.; Cifuentes, A.; Coimbra Araujo, C. H.; Conforti, V.; Conte, F.; Contreras, J. L.; Cortina, J.; Costa, A.; Costantini, H.; Cotter, G.; Crestan, S.; Cristofari, P.; Cuevas, O.; Curtis-Ginsberg, Z.; D'Aì, A.; D'Amico, G.; D'Ammando, F.; Dadina, M.; Dalchenko, M.; David, L.; Dazzi, F.; de Bony de Lavergne, M.; De Caprio, V.; De Frondat Laadim, F.; de Gouveia Dal Pino, E. M.; De Lotto, B.; De Lucia, M.; de Martino, D.; de Menezes, R.; de Naurois, M.; de Ona Wilhelmi, E.; de Souza, V.; del Peral, L.; Delgado Giler, A. G.; Delgado, C.; Dell'aiera, M.; Della Valle, M.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Díaz, C.; Diebold, S.; Dinesh, A.; Djannati-Ataï, A.; Djuvsland, J.; Domínguez, A.; Dominik, R. M.; Donini, A.; Dörner, J.; Doro, M.; dos Anjos, R. D. C.; Dournaux, J. -L.; Duangchan, C.; Dubos, C.; Dubus, G.; Duffy, S.; Dumora, D.; Dwarkadas, V. V.; Ebr, J.; Eckner, C.; Egberts, K.; Einecke, S.; Elsässer, D.; Emery, G.; Errando, M.; Escanuela, C.; Escarate, P.; Escobar Godoy, M.; Escudero, J.; Esposito, P.; Evoli, C.; Falceta-Goncalves, D.; Fattorini, A.; Fegan, S.; Feijen, K.; Feng, Q.; Ferrand, G.; Ferrarotto, F.; Fiandrini, E.; Fiasson, A.; Filipovic, M.; Fioretti, V.; Fiori, M.; Flores, H.; Foffano, L.; Font Guiteras, L.; Fontaine, G.; Fröse, S.; Fukazawa, Y.; Fukui, Y.; Funk, S.; Furniss, A.; Gaggero, D.; Galanti, G.; Galaz, G.; Gallant, Y. A.; Gallozzi, S.; Gammaldi, V.; Garczarczyk, M.; Gasbarra, C.; Gasparrini, D.; Gaug, M.; Ghalumyan, A.; Giarrusso, M.; Giesbrecht, J.; Giglietto, N.; Giordano, F.; Giuffrida, R.; Giuliani, A.; Glicenstein, J. -F.; Glombitza, J.; Godinovic, N.; Goldoni, P.; González, J. M.; Goulart Coelho, J.; Granot, J.; Grasso, D.; Grau, R.; Gréaux, L.; Green, D.; Green, J. G.; Greenshaw, T.; Grenier, I.; Grolleron, G.; Grondin, M. -H.; Gueta, O.; Gunji, S.; Hackfeld, J.; Hadasch, D.; Hanlon, W.; Hara, S.; Harvey, V. M.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Hermann, G.; Hernández Cadena, S.; Hervet, O.; Hinton, J.; Hiroshima, N.; Hnatyk, B.; Hnatyk, R.; Hofmann, W.; Holder, J.; Holler, M.; Horan, D.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Iarlori, M.; Inada, T.; Incardona, F.; Inoue, S.; Iocco, F.; Iori, M.; Jamrozy, M.; Janecek, P.; Jankowsky, F.; Jarnot, C.; Jean, P.; Jiménez Martínez, I.; Jin, W.; Juramy-Gilles, C.; Jurysek, J.; Kagaya, M.; Kalekin, O.; Kantzas, D.; Karas, V.; Katagiri, H.; Kataoka, J.; Kaufmann, S.; Kazanas, D.; Kerszberg, D.; Khélifi, B.; Kieda, D. B.; Kissmann, R.; Kleiner, T.; Kluge, G.; Kluźniak, W.; Knödlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kornecki, P.; Kosack, K.; Kostunin, D.; Kowal, G.; Kubo, H.; Kushida, J.; La Barbera, A.; La Palombara, N.; Láinez, M.; Lamastra, A.; Lapington, J.; Laporte, P.; Lazarević, S.; Lazendic-Galloway, J.; Lemoine-Goumard, M.; Lenain, J. -P.; Leone, F.; Leto, G.; Leuschner, F.; Lindfors, E.; Linhoff, M.; Liodakis, I.; Lombardi, S.; Longo, F.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Lozano Bahilo, J.; Lucarelli, F.; Luque-Escamilla, P. L.; Lyard, E.; Macias, O.; Mackey, J.; Maier, G.; Malyshev, D.; Mandat, D.; Manicò, G.; Marcowith, A.; Marinos, P.; Mariotti, M.; Markoff, S.; Marquez, P.; Marsella, G.; Martí, J.; Martin, P.; Martínez, G. A.; Martínez, M.; Martinez, O.; Marty, C.; Mas-Aguilar, A.; Mastropietro, M.; Maurin, G.; Mazin, D.; McKeague, S.; Mello, A. J. T. S.; Menchiari, S.; Mereghetti, S.; Mestre, E.; Meunier, J. -L.; Meyer, D. M. -A.; Miceli, D.; Miceli, M.; Michailidis, M.; Michałowski, J.; Miener, T.; Miranda, J. M.; Mitchell, A.; Mizuno, T.; Moderski, R.; Mohrmann, L.; Molero, M.; Molfese, C.; Molina, E.; Montaruli, T.; Moralejo, A.; Morcuende, D.; Morik, K.; Morlino, G.; Morselli, A.; Moulin, E.; Moya Zamanillo, V.; Mukherjee, R.; Munari, K.; Murach, T.; Muraczewski, A.; Muraishi, H.; Nagataki, S.; Nakamori, T.; Nemmen, R.; Nickel, L.; Niemiec, J.; Nieto, D.; Nievas Rosillo, M.; Nikołajuk, M.; Nikolić, L.; Noda, K.; Nosek, D.; Novosyadlyj, B.; Novotny, V.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Okumura, A.; Olive, J. -F.; Olmi, B.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Orlando, S.; Ostrowski, M.; Oya, I.; Pagano, I.; Pagliaro, A.; Palatiello, M.; Panebianco, G.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Parmiggiani, N.; Patel, S. R.; Patricelli, B.; Pavlović, D.; Pech, M.; Pecimotika, M.; Peresano, M.; Pérez-Romero, J.; Pérez-Torres, M. A.; Peron, G.; Persic, M.; Petrucci, P. -O.; Petruk, O.; Piano, G.; Pierre, E.; Pietropaolo, E.; Pihet, M.; Pintore, F.; Pittori, C.; Plard, C.; Podobnik, F.; Pohl, M.; Pons, E.; Ponti, G.; Prandini, E.; Principe, G.; Priyadarshi, C.; Produit, N.; Prokhorov, D.; Pueschel, E.; Pühlhofer, G.; Pumo, M. L.; Punch, M.; Queiroz, F.; Quirrenbach, A.; Rando, R.; Ravel, T.; Razzaque, S.; Regeard, M.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Reposeur, T.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richtler, T.; Rico, J.; Rieger, F.; Rigoselli, M.; Rizi, V.; Roache, E.; Rodriguez Fernandez, G.; Rodríguez-Vázquez, J. J.; Romano, P.; Romeo, G.; Rosado, J.; Rosales de Leon, A.; Rowell, G.; Rudak, B.; Ruiter, A. J.; Rulten, C. B.; Russo, F.; Sadeh, I.; Saha, L.; Saito, T.; Salzmann, H.; Sánchez-Conde, M.; Sangiorgi, P.; Sano, H.; Santander, M.; Santangelo, A.; Santos-Lima, R.; Sapienza, V.; Šarić, T.; Sarkar, S.; Saturni, F. G.; Scherer, A.; Schiavone, F.; Schipani, P.; Schleicher, B.; Schovanek, P.; Schubert, J. L.; Schussler, F.; Schwanke, U.; Schwefer, G.; Seglar Arroyo, M.; Seitenzahl, I.; Sergijenko, O.; Servillat, M.; Sguera, V.; Sharma, P.; Siejkowski, H.; Siqueira, C.; Sizun, P.; Sliusar, V.; Slowikowska, A.; Sol, H.; Spencer, S. T.; Spiga, D.; Stamerra, A.; Stanič, S.; Starling, R.; Stawarz, Ł.; Steinmassl, S.; Steppa, C.; Stolarczyk, T.; Suda, Y.; Suomijärvi, T.; Tajima, H.; Takeishi, R.; Tanaka, S. J.; Tavecchio, F.; Tavernier, T.; Terada, Y.; Terrier, R.; Teshima, M.; Tian, W. W.; Tibaldo, L.; Tibolla, O.; Torradeflot, F.; Torres, D. F.; Tothill, N.; Toussenel, F.; Touzard, V.; Travnicek, P.; Tripodo, G.; Trois, A.; Tsiahina, A.; Tutone, A.; Umana, G.; Vaclavek, L.; Vacula, M.; Vallania, P.; van Eldik, C.; Vassiliev, V.; Vazquez Acosta, M. L.; Vecchi, M.; Ventura, S.; Vercellone, S.; Verna, G.; Viana, A.; Viaux, N.; Vigliano, A.; Vignatti, J.; Vigorito, C. F.; Villanueva, J.; Vink, J.; Vitale, V.; Vodeb, V.; Voisin, V.; Vorobiov, S.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Waegebaert, V.; Wagner, S. J.; Walter, R.; Wechakama, M.; White, R.; Wierzcholska, A.; Williams, D. A.; Wohlleben, F.; Yamazaki, R.; Yang, L.; Yoshida, T.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zampieri, L.; Zanin, R.; Zavrtanik, D.; Zavrtanik, M.; Zdziarski, A. A.; Zech, A.; Zhdanov, V. I.; Ziętara, K.; Živec, M.; Zuriaga-Puig, J.; De la Torre Luque, P.; Guillemot, L.; Smith, D. A.; CTA Consortium
Journal of Cosmology and Astroparticle Physics, Oct. 2024, [Reviewed]
Approximately one hundred sources of very-high-energy (VHE) gamma rays are known in the Milky Way, detected with a combination of targeted observations and surveys. A survey of the entire Galactic Plane in the energy range from a few tens of GeV to a few hundred TeV has been proposed as a Key Science Project for the upcoming Cherenkov Telescope Array Observatory (CTAO). This article presents the status of the studies towards the Galactic Plane Survey (GPS). We build and make publicly available a sky model that combines data from recent observations of known gamma-ray emitters with state-of-the-art physically-driven models of synthetic populations of the three main classes of established Galactic VHE sources (pulsar wind nebulae, young and interacting supernova remnants, and compact binary systems), as well as of interstellar emission from cosmic-ray interactions in the Milky Way. We also perform an optimisation of the observation strategy (pointing pattern and scheduling) based on recent estimations of the instrument performance. We use the improved sky model and observation strategy to simulate GPS data corresponding to a total observation time of 1620 hours spread over ten years. Data are then analysed using the methods and software tools under development for real data. Under our model assumptions and for the realisation considered, we show that the GPS has the potential to increase the number of known Galactic VHE emitters by almost a factor of five. This corresponds to the detection of more than two hundred pulsar wind nebulae and a few tens of supernova remnants at average integral fluxes one order of magnitude lower than in the existing sample above 1 TeV, therefore opening the possibility to perform unprecedented population studies. The GPS also has the potential to provide new VHE detections of binary systems and pulsars, to confirm the existence of a hypothetical population of gamma-ray pulsars with an additional TeV emission component, and to detect bright sources capable of accelerating particles to PeV energies (PeVatrons). Furthermore, the GPS will constitute a pathfinder for deeper follow-up observations of these source classes. Finally, we show that we can extract from GPS data an estimate of the contribution to diffuse emission from unresolved sources, and that there are good prospects of detecting interstellar emission and statistically distinguishing different scenarios. Thus, a survey of the entire Galactic plane carried out from both hemispheres with CTAO will ensure a transformational advance in our knowledge of Galactic VHE source populations and interstellar emission....
Scientific journal
DOI：https://doi.org/10.1088/1475-7516/2024/10/081
DOI ID：10.1088/1475-7516/2024/10/081, ORCID：181063903, arXiv ID：arXiv:2310.02828, Bibcode：2024JCAP...10..081A - A detailed study of the very high-energy Crab pulsar emission with the LST-1
Abe, K.; Abe, S.; Abhishek, A.; Acero, F.; Aguasca-Cabot, A.; Agudo, I.; Alvarez Crespo, N.; Antonelli, L. A.; Aramo, C.; Arbet-Engels, A.; Arcaro, C.; Artero, M.; Asano, K.; Aubert, P.; Baktash, A.; Bamba, A.; Baquero Larriva, A.; Baroncelli, L.; Barres de Almeida, U.; Barrio, J. A.; Batkovic, I.; Baxter, J.; Becerra Gonzáilez, J.; Bernardini, E.; Bernete Medrano, J.; Berti, A.; Bhattacharjee, P.; Bigongiari, C.; Bissaldi, E.; Blanch, O.; Bonnoli, G.; Bordas, P.; Brunelli, G.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Buscemi, M.; Cardillo, M.; Caroff, S.; Carosi, A.; Carrasco, M. S.; Cassol, F.; Castrejón, N.; Cauz, D.; Cerasole, D.; Ceribella, G.; Chai, Y.; Cheng, K.; Chiavassa, A.; Chikawa, M.; Chon, G.; Chytka, L.; Cicciari, G. M.; Cifuentes, A.; Contreras, J. L.; Cortina, J.; Costantini, H.; Da Vela, P.; Dalchenko, M.; Dazzi, F.; De Angelis, A.; de Bony de Lavergne, M.; De Lotto, B.; de Menezes, R.; Del Peral, L.; Delgado, C.; Delgado Mengual, J.; della Volpe, D.; Dellaiera, M.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Díaz, C.; Dominik, R. M.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro, M.; Eisenberger, L.; Elsässer, D.; Emery, G.; Escudero, J.; Fallah Ramazani, V.; Ferrarotto, F.; Fiasson, A.; Foffano, L.; Freixas Coromina, L.; Fröse, S.; Fukazawa, Y.; Garcia López, R.; Gasbarra, C.; Gasparrini, D.; Gavira, L.; Geyer, D.; Giesbrecht Paiva, J.; Giglietto, N.; Giordano, F.; Gliwny, P.; Godinovic, N.; Grau, R.; Green, D.; Green, J.; Gunji, S.; Günther, P.; Hackfeld, J.; Hadasch, D.; Hahn, A.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Herrera Llorente, J.; Hirotani, K.; Hoffmann, D.; Horns, D.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Hui, D.; Iarlori, M.; Imazawa, R.; Inada, T.; Inome, Y.; Ioka, K.; Iori, M.; Jimenez Martinez, I.; Jiménez Quiles, J.; Jurysek, J.; Kagaya, M.; Karas, V.; Katagiri, H.; Kataoka, J.; Kerszberg, D.; Kobayashi, Y.; Kohri, K.; Kong, A.; Kubo, H.; Kushida, J.; Lainez, M.; Lamanna, G.; Lamastra, A.; Lemoigne, L.; Linhoff, M.; Longo, F.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Lorini, A.; Lozano Bahilo, J.; Luque-Escamilla, P. L.; Majumdar, P.; Makariev, M.; Mallamaci, M.; Mandat, D.; Manganaro, M.; Manicò, G.; Mannheim, K.; Marchesi, S.; Mariotti, M.; Marquez, P.; Marsella, G.; Martí, J.; Martinez, O.; Martínez, G.; Martínez, M.; Mas-Aguilar, A.; Maurin, G.; Mazin, D.; Mestre Guillen, E.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Molero Gonzalez, M.; Molina, E.; Montaruli, T.; Moralejo, A.; Morcuende, D.; Morselli, A.; Moya, V.; Muraishi, H.; Nagataki, S.; Nakamori, T.; Neronov, A.; Nickel, L.; Nievas Rosillo, M.; Nikolic, L.; Nishijima, K.; Noda, K.; Nosek, D.; Novotny, V.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Oka, T.; Okumura, A.; Orito, R.; Otero-Santos, J.; Ottanelli, P.; Owen, E.; Palatiello, M.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Pech, M.; Pecimotika, M.; Peresano, M.; Pfeiffle, F.; Pietropaolo, E.; Pihet, M.; Pirola, G.; Plard, C.; Podobnik, F.; Pons, E.; Prandini, E.; Priyadarshi, C.; Prouza, M.; Rando, R.; Rhode, W.; Ribó, M.; Righi, C.; Rizi, V.; Rodriguez Fernandez, G.; Rodríguez Frías, M. D.; Saito, T.; Sakurai, S.; Sanchez, D. A.; Sano, H.; Šarić, T.; Sato, Y.; Saturni, F. G.; Savchenko, V.; Schiavone, F.; Schleicher, B.; Schmuckermaier, F.; Schubert, J. L.; Schussler, F.; Schweizer, T.; Seglar Arroyo, M.; Siegert, T.; Silvia, R.; Sitarek, J.; Sliusar, V.; Strišković, J.; Strzys, M.; Suda, Y.; Tajima, H.; Takahashi, H.; Takahashi, M.; Takata, J.; Takeishi, R.; Tam, P. H. T.; Tanaka, S. J.; Tateishi, D.; Tavernier, T.; Temnikov, P.; Terada, Y.; Terauchi, K.; Terzic, T.; Teshima, M.; Tluczykont, M.; Tokanai, F.; Torres, D. F.; Travnicek, P.; Truzzi, S.; Tutone, A.; Vacula, M.; Vallania, P.; van Scherpenberg, J.; Vázquez Acosta, M.; Verna, G.; Viale, I.; Vigliano, A.; Vigorito, C. F.; Visentin, E.; Vitale, V.; Voitsekhovskyi, V.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Walter, R.; Wan, L.; Will, M.; Yamamoto, T.; Yamazaki, R.; Yeung, P. K. H.; Yoshida, T.; Yoshikoshi, T.; Zhang, W.; Zywucka, N.
Astronomy and Astrophysics, Oct. 2024, [Reviewed]
Context. To date, three pulsars have been firmly detected by imaging atmospheric Cherenkov telescopes (IACTs). Two of them reached the TeV energy range, challenging models of very high-energy (VHE) emission in pulsars. More precise observations are needed to better characterize pulsar emission at these energies. The LST-1 is the prototype of the large-sized telescopes, which will be part of the Cherenkov Telescope Array Observatory (CTAO). Its improved performance over previous IACTs makes it well suited for studying pulsars. Aims. In this work we study the Crab pulsar emission with the LST-1, improving upon and complementing the results from other telescopes. Crab pulsar observations can also be used to characterize the potential of the LST-1 to study other pulsars and detect new ones. Methods. We analyzed a total of ∼103 hours of gamma-ray observations of the Crab pulsar conducted with the LST-1 in the period from September 2020 to January 2023. The observations were carried out at zenith angles of less than 50 degrees. To characterize the Crab pulsar emission over a broader energy range, a new analysis of the Fermi/LAT data, including ∼14 years of observations, was also performed. Results. The Crab pulsar phaseogram, long-term light curve, and phase-resolved spectra are reconstructed with the LST-1 from 20 GeV to 450 GeV for the first peak and up to 700 GeV for the second peak The pulsed emission is detected with a significance level of 15.2σ. The two characteristic emission peaks of the Crab pulsar are clearly detected (> 10σ), as is the so-called bridge emission between them (5.7σ). We find that both peaks are described well by power laws, with spectral indices of ∼3.44 and ∼3.03, respectively. The joint analysis of Fermi/LAT and LST-1 data shows a good agreement between the two instruments in their overlapping energy range. The detailed results obtained from the first observations of the Crab pulsar with the LST-1 show the potential that CTAO will have to study this type of source....
Scientific journal
DOI：https://doi.org/10.1051/0004-6361/202450059
DOI ID：10.1051/0004-6361/202450059, ORCID：181063905, arXiv ID：arXiv:2407.02343, Bibcode：2024A&A...690A.167A - XRISM Spectroscopy of the Fe Kα Emission Line in the Seyfert Active Galactic Nucleus NGC 4151 Reveals the Disk, Broad-line Region, and Torus
Xrism Collaboration; Audard, Marc; Awaki, Hisamitsu; Ballhausen, Ralf; Bamba, Aya; Behar, Ehud; Boissay-Malaquin, Rozenn; Brenneman, Laura; Brown, Gregory V.; Corrales, Lia; Costantini, Elisa; Cumbee, Renata; Diaz Trigo, Maria; Done, Chris; Dotani, Tadayasu; Ebisawa, Ken; Eckart, Megan E.; Eckert, Dominique; Enoto, Teruaki; Eguchi, Satoshi; Ezoe, Yuichiro; Foster, Adam; Fujimoto, Ryuichi; Fujita, Yutaka; Fukazawa, Yasushi; Fukushima, Kotaro; Furuzawa, Akihiro; Gallo, Luigi; García, Javier A.; Gu, Liyi; Guainazzi, Matteo; Hagino, Kouichi; Hamaguchi, Kenji; Hatsukade, Isamu; Hayashi, Katsuhiro; Hayashi, Takayuki; Hell, Natalie; Hodges-Kluck, Edmund; Hornschemeier, Ann; Ichinohe, Yuto; Ishida, Manabu; Ishikawa, Kumi; Ishisaki, Yoshitaka; Kaastra, Jelle; Kallman, Timothy; Kara, Erin; Katsuda, Satoru; Kanemaru, Yoshiaki; Kelley, Richard; Kilbourne, Caroline; Kitamoto, Shunji; Kobayashi, Shogo; Kohmura, Takayoshi; Kubota, Aya; Leutenegger, Maurice; Loewenstein, Michael; Maeda, Yoshitomo; Markevitch, Maxim; Matsumoto, Hironori; Matsushita, Kyoko; McCammon, Dan; McNamara, Brian; Mernier, François; Miller, Eric D.; Miller, Jon M.; Mitsuishi, Ikuyuki; Mizumoto, Misaki; Mizuno, Tsunefumi; Mori, Koji; Mukai, Koji; Murakami, Hiroshi; Mushotzky, Richard; Nakajima, Hiroshi; Nakazawa, Kazuhiro; Ness, Jan-Uwe; Nobukawa, Kumiko; Nobukawa, Masayoshi; Noda, Hirofumi; Odaka, Hirokazu; Ogawa, Shoji; Ogorzalek, Anna; Okajima, Takashi; Ota, Naomi; Paltani, Stephane; Petre, Robert; Plucinsky, Paul; Porter, Frederick S.; Pottschmidt, Katja; Sato, Kosuke; Sato, Toshiki; Sawada, Makoto; Seta, Hiromi; Shidatsu, Megumi; Simionescu, Aurora; Smith, Randall; Suzuki, Hiromasa; Szymkowiak, Andrew; Takahashi, Hiromitsu; Takeo, Mai; Tamagawa, Toru; Tamura, Keisuke; Tanaka, Takaaki; Tanimoto, Atsushi; Tashiro, Makoto; Terada, Yukikatsu; Terashima, Yuichi; Tsuboi, Yohko; Tsujimoto, Masahiro; Tsunemi, Hiroshi; Tsuru, Takeshi; Uchida, Hiroyuki; Uchida, Nagomi; Uchida, Yuusuke; Uchiyama, Hideki; Ueda, Yoshihiro; Uno, Shinichiro; Vink, Jacco; Watanabe, Shin; Williams, Brian J.; Yamada, Satoshi; Yamada, Shinya; Yamaguchi, Hiroya; Yamaoka, Kazutaka; Yamasaki, Noriko; Yamauchi, Makoto; Yamauchi, Shigeo; Yaqoob, Tahir; Yoneyama, Tomokage; Yoshida, Tessei; Yukita, Mihoko; Zhuravleva, Irina; Xiang, Xin; Minezaki, Takeo; Buhariwalla, Margaret; Gerolymatou, Dimitra; Hagen, Scott
The Astrophysical Journal, Sep. 2024, [Reviewed]
We present an analysis of the first two XRISM/Resolve spectra of the well-known Seyfert-1.5 active galactic nucleus (AGN) in NGC 4151, obtained in 2023 December. Our work focuses on the nature of the narrow Fe K α emission line at 6.4 keV, the strongest and most common X-ray line observed in AGN. The total line is found to consist of three components. Even the narrowest component of the line is resolved with evident Fe K α,1 (6.404 keV) and K α,2 (6.391 keV) contributions in a 2:1 flux ratio, fully consistent with neutral gas with negligible bulk velocity. Subject to the limitations of our models, the narrowest and intermediate-width components are consistent with emission from optically thin gas, suggesting that they arise in a disk atmosphere and/or wind. Modeling the three line components in terms of Keplerian broadening, they are readily associated with (1) the inner wall of the "torus," (2) the innermost optical "broad-line region" (or "X-ray BLR"), and (3) a region with a radius of r ≃ 100 GM/c 2 that may signal a warp in the accretion disk. Viable alternative explanations of the broadest component include a fast-wind component and/or scattering; however, we find evidence of variability in the narrow Fe K α line complex on timescales consistent with small radii. The best-fit models are statistically superior to simple Voigt functions, but when fit with Voigt profiles the time-averaged lines are consistent with a projected velocity broadening of FWHM
Scientific journal
DOI：https://doi.org/10.3847/2041-8213/ad7397
DOI ID：10.3847/2041-8213/ad7397, ORCID：168902928, arXiv ID：arXiv:2408.14300, Bibcode：2024ApJ...973L..25X - Pile-up simulator for XRISM/Xtend
Tomokage Yoneyama; Tsubasa Tamba; Hirokazu Odaka; Aya Bamba; Hiroshi Murakami; Koji Mori; Yukikatsu Terada; Masayoshi Nobukawa; Tsunefumi Mizuno
Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：227, Last page：227, Aug. 2024
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.3018665
DOI ID：10.1117/12.3018665 - Development and operation status of X-Ray Imaging and Spectroscopy Mission (XRISM)
Makoto S. Tashiro; Shin Watanabe; Hironori Maejima; Kenichi Toda; Kyoko Matsushita; Hiroya Yamaguchi; Richard L. Kelley; Lillian S. Reichenthal; Leslie S. Hartz; Robert Petre; Brian J. Williams; Matteo Guainazzi; Andrea Santovincenzo; Elisa Costantini; Yoh Takei; Yoshitaka Ishisaki; Ryuichi Fujimoto; Joy Henegar-Leon; Gary Sneiderman; Hiroshi Tomida; Koji Mori; Hiroshi Nakajima; Yukikatsu Terada; Matt Holland; Micheal Loewenstein; Tomothey Kallman; Jelle Kaastra; Eric Miller; Makoto Sawada; Chris Done; Teruaki Enoto; Aya Bamba; Paul Plucinsky; Yoshitaka Ueda; Erin Kara; Irina Zhuravleva; Yutaka Fujita; Jose Antonio Quero; Yoshitaka Arai; Marc Audard; Hisamitsu Awaki; Chris Baluta; Nobutaka Bando; Ehud Behar; Thomas Bialas; Rozenn Boissay-Malaquin; Laura Brenneman; Gregory V. Brown; Meng Chiao; Lia Corrales; Renata Cumbee; Cor de Vries; Jan-Willem den Herder; Maria Diaz-Trigo; Michael DiPirro; Tadayasu Dotani; Jacobo Ebrero Carrero; Ken Ebisawa; Megan Eckart; Dominique Eckart; Satoshi Eguchi; Yuichiro Ezoe; Carlo Ferrgno; Adam Foster; Yasushi Fukazawa; Kotaro Fukushima; Akihiro Furuzawa; Luigi Gallo; Nathalie Gorter; Martin Grim; Liyi Gu; Koichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Natalie Hell; Edmund Hodges-Kluck; Takafumi Horiuchi; Ann Hornschemeier; Akio Hoshino; Yuto Ichinohe; Chisato Ikuta; Ryo Iizuka; Daiki Ishi; Manabu Ishida; Naoki Ishihama; Kumi Ishikawa; Kosei Ishimura; Tess Jaffe; Satoru Katsuda; Yoshiaki Kanemaru; Steven Kenyon; Caroline Kilbourne; Mark Kimball; Shunji Kitamoto; Shogo Kobayashi; Akihide Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Muzi Li; Yoshitomo Maeda; Maxim Markevitch; Hironori Matsumoto; Keiichi Matsuzaki; Dan McCammon; Brian McLaughlin; Brian McNamara; Josegh Miko; Jon Miller; Kenji Minesugi; Shinji Mitani; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Kazuhiro Nakazawa; Chikara Natsukari; Jan-Uwe Ness; Kenichiro Nigo; Mari Nishiyama; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Mina Ogawa; Shoji Ogawa; Takashi Okajima; Atsushi Okamoto; Naomi Ota; Masanobu Ozaki; Stephane Paltani; F. Scott Porter; Katja Pottschmidt; Takahiro Sasaki; Kosuke Sato; Rie Sato; Toshiki Sato; Yoichi Sato; Hiromi Seta; Maki Shida; Megumi Shidatsu; Shuhei Shigeto; Russel Shipman; Keisuke Shinozaki; Peter Shirron; Aurora Simionescu; Randall Smith; Young Soong; Hiromasa Suzuki; Andy Szymkowiak; Hiromitsu Takahashi; Mai Takeo; Toru Tamagawa; Keisuke Tamura; Takaaki Tanaka; Atsushi Tanimoto; Yoichi Terashima; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Tsuru; Hiroyuki Uchida; Nagomi Ucghida; Yuusuke Uchida; Hideki Uchiyama; Shinichiro Uno; Erik Van der Meer; Jacco Vink; Michael Wittheof; Rob Wolf; Satoshi Yamada; Shinya Yamada; Kazutaka Yamaoka; Noriko Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Keiichi Yamagase; Tahir Yaqoob; Susumu Yasuda; Tomokage Yoneyama; Tessei Yoshida
Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：52, Last page：52, Aug. 2024
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.3019325
DOI ID：10.1117/12.3019325 - X-ray transient search using XRISM/Xtend
Yohko Tsuboi; Koichiro Akasu; Noboru Nemoto; Tomokage Yoneyama; Marina Yoshimoto; Kotaro Fukushima; Katsuhiro Hayashi; Yoshiaki Kanemaru; Shoji Ogawa; Tessei Yoshida; Marc Audard; Ehud Behar; Shun Inoue; Yuiko Ishihara; Takayoshi Komura; Yoshitomo Maeda; Misaki Mizumoto; Masayoshi Nobukawa; Katja Pottschmidt; Megumi Shidatsu; Yukikatsu Terada; Yuichi Terashima; Hiroyuki Uchida
Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：236, Last page：236, Aug. 2024
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.3019733
DOI ID：10.1117/12.3019733 - Evaluation of the initial pointing accuracy of XRISM
Yoshiaki Kanemaru; Ryo Iizuka; Yoshitomo Maeda; Takashi Okajima; Takayuki Hayashi; Kazuhiro Kiyokane; Yuto Nihei; Takashi Kominato; Manabu Ishida; Chikara Natsukari; Shin Watanabe; Kosuke Sato; Yukikatsu Terada; Katsuhiro Hayashi; Chris Baluta; Tessei Yoshida; Akio Hoshino; Shoji Ogawa; Kotaro Fukushima; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Kazuhiro Nakazawa; Shin'ichiro Uno; Ken Ebisawa; Satoshi Eguchi; Satoru Katsuda; Aya Kubota; Naomi Ota; Megumi Shidatsu; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Yoneyama Tomokage; Satoshi Yamada; Nagomi Uchida; Rie Sato; Matt Holland; Michael Loewenstein; Eric D. Miller; Tahir Yaqoob; Robert S. Hill; Trisha F. Doyle; Efrain Perez-Solis; Morgan D. Waddy; Mark Mekosh; Joseph B. Fox; Makoto S. Tashiro; Kenichi Toda; Hironori Maejima
Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：224, Last page：224, Aug. 2024
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.3016594
DOI ID：10.1117/12.3016594 - Verification of the XRISM timing system in the GPS unsynchronized mode
Megumi Shidatsu; Yukikatsu Terada; Takashi Kominato; So Kato; Ryohei Sato; Minami Sakama; Takumi Shioiri; Yugo Motogami; Yuki Niida; Toshihiro Takagi; Chikara Natsukari; Makoto S. Tashiro; Kenichi Toda; Hironori Maejima; Shin Watanabe; Ryo Iizuka; Rie Sato; Chris Baluta; Katsuhiro Hayashi; Tessei Yoshida; Shoji Ogawa; Yoshiaki Kanemaru; Kotaro Fukushima; Akio Hoshino; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Kazuhiro Nakazawa; Shin'ichiro Uno; Ken Ebisawa; Satoshi Eguchi; Satoru Katsuda; Aya Kubota; Naomi Ota; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tomokage Yoneyama; Satoshi Yamada; Nagomi Uchida; Matt Holland; Michael Loewenstein; Eric D. Miller; Tahir Yaqoob; Robert S. Hill; Trisha F. Doyle; Efrain Perez-Solis; Morgan D. Waddy; Mark Mekosh; Joseph B. Fox
Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：235, Last page：235, Aug. 2024
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.3019651
DOI ID：10.1117/12.3019651 - Detail design of the XRISM Timing System and its verification in the nominal operation mode
Yukikatsu Terada; Megumi Shidatsu; Makoto Sawada; Takashi Kominato; So Kato; Ryohei Sato; Minami Sakama; Takumi Shioiri; Yuki Niida; Chikara Natsukari; Makoto S. Tashiro; Kenichi Toda; Hironori Maejima; Katsuhiro Hayashi; Tessei Yoshida; Shoji Ogawa; Yoshiaki Kanemaru; Akio Hoshino; Kotaro Fukushima; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Kazuhiro Nakazawa; Shin'ichiro Uno; Ken Ebisawa; Satoshi Eguchi; Satoru Katsuda; Aya Kubota; Naomi Ota; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tomokage Yoneyama; Satoshi Yamada; Nagomi Uchida; Shin Watanabe; Ryo Iizuka; Rie Sato; Chris Baluta; Matt Holland; Michael Loewenstein; Eric D. Miller; Tahir Yaqoob; Robert S. Hill; Trisha F. Doyle; Efrain Perez-Solis; Morgan D. Waddy; Mark Mekosh; Joseph B. Fox; Toshihiro Takagi; Yugo Motogami; Katja Pottschmidt; Teruaki Enoto; Takaaki Tanaka
Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：61, Last page：61, Aug. 2024
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.3019329
DOI ID：10.1117/12.3019329 - The in-orbit XRISM science operations
Katsuhiro Hayashi; Makoto S. Tashiro; Yukikatsu Terada; Tessei Yoshida; Shoji Ogawa; Yoshiaki Kanemaru; Kotaro Fukushima; Akio Hoshino; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Kazuhiro Nakazawa; Shin'ichiro Uno; Ken Ebisawa; Satoshi Eguchi; Satoru Katsuda; Takao Kitaguchi; Aya Kubota; Naomi Ota; Megumi Shidatsu; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tomokage Yoneyama; Satoshi Yamada; Nagomi Uchida; Seiko Sakurai; Shin Watanabe; Ryo Iizuka; Rie Sato; Chris Baluta; Takayuki Tamura; Yasushi Fukazawa; Hirokazu Odaka; Tsubasa Tamba; Ryohei Sato; Sou Kato; Minami Sakama; Takumi Shioiri; Yuki Niida; Natsuki Sakamoto; Noboru Nemoto; Yuki Omiya; Nari Suzuki; Toshihiro Takagi; Yugo Motogami; Matt Holland; Michael Loewenstein; Eric D. Miller; Tahir Yaqoob; Robert S. Hill; Trisha F. Doyle; Efrain Perez-Solis; Morgan D. Waddy; Mark Mekosh; Joseph B. Fox; Matteo Guainazzi; Jan-Uwe Ness; Hironori Maejima; Kenichi Toda; Chikara Natsukari
Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：60, Last page：60, Aug. 2024
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.3018908
DOI ID：10.1117/12.3018908 - Wide-band x-ray observatory for the time domain astronomy era: CHRONOS
Kazuhiro Nakazawa; Teruaki Enoto; Wataru B. Iwakiri; Megumi Shidatsu; Hiromitsu Takahashi; Takashi Okajima; Manabu Ishida; Hiromasa Suzuku; Hiroya Yamaguchi; Shin Watanabe; Mariko Kimura; Hiroshi Nakajima; Takaaki Tanaka; Hiroyuki Uchida; Yoshihiro Ueda; Takeshi G. Tsuru; Kosuke Namekata; Koji Mori; Masayoshi Nobukawa; Hironori Matsumoto; Hiroki Akamatsu; Taiki Kawamuro; Satoshi Yamada; Yukikatsu Terada; Yoichi Yatsu; Hirofumi Noda
Space Telescopes and Instrumentation 2024: Ultraviolet to Gamma Ray, First page：92, Last page：92, Aug. 2024
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.3018366
DOI ID：10.1117/12.3018366 - XRISM/Xtend Transient Search (XTS) detected a possible stellar flare from 1RXS J113700.0-651617
Ogawa, S.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Aug. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1137-6516 on 2024-08-13 TT. The source position is determined to be (R.A., Dec.) = (174.244, -65.273), with a systematic error of & ndash; 40 arcsec....
The Astronomer's Telegram
ORCID：181064024, Bibcode：2024ATel16773....1O - XRISM/Xtend Transient Search (XTS) detected a possible stellar flare from 2MASS J11414215-6521298
Ogawa, S.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Aug. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1142-6522 on 2024-08-13 TT. The source position is determined to be (R.A., Dec.) = (175.418, -65.363), with a systematic error of & ndash; 40 arcsec....
The Astronomer's Telegram
ORCID：181064023, Bibcode：2024ATel16774....1O - XRISM/Xtend Transient Search (XTS) reported the second detection of a prestellar flare from 2MASS J11414215-6521298
Ogawa, S.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Aug. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from the X-ray source XRISM J1142-6522, whose possible counterpart is 2MASS J11414215-6521298 at 101 pc, on 2024-08-14 TT. This is the second report by XRISM of a brightening of this source following the last one (ATel #16774)....
The Astronomer's Telegram
ORCID：181064022, Bibcode：2024ATel16775....1O - XRISM/Xtend Transient Search (XTS) reported the third detection of a prestellar flare from 2MASS J11414215-6521298
Ogawa, S.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Aug. 2024
XRISM/Xtend Transient Search (XTS) detected X-ray flares from the X-ray source XRISM J1142-6522, whose possible counterpart is 2MASS J11414215-6521298 at 101 pc, on 2024-08-15 TT. We report the largest flare in this period although the activity is continued....
The Astronomer's Telegram
ORCID：181064021, Bibcode：2024ATel16777....1O - XRISM/Xtend Transient Search (XTS) detected a possible stellar flare from 4XMM J114021.0-651852/1eRASS J114021.5-651851
Ogawa, S.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Aug. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1140-6519 on 2024-08-17 TT. The source position is determined to be (R.A., Dec.) = (175.081, -65.316), with a systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181064020, Bibcode：2024ATel16779....1O - XRISM/Xtend Transient Search (XTS) detected a possible stellar flare from the Galactic center
Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yanagi, T.; Yoneyama, T.; Yoshimoto, M.
Aug. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1745-2914 on 2024-08-29 TT. The source position is determined to be (R.A., Dec.) = (266.276, -29.246), with a systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181064019, Bibcode：2024ATel16794....1F - On the X-ray efficiency of the white dwarf pulsar candidate ZTF J190132.9+145808.7
Bamba, Aya; Terada, Yukikatsu; Kashiyama, Kazumi; Kisaka, Shota; Minami, Takahiro; Takahashi, Tadayuki
Publications of the Astronomical Society of Japan, Aug. 2024, [Reviewed]
Strongly magnetized, rapidly rotating massive white dwarfs (WDs) emerge as potential outcomes of double degenerate mergers. These WDs can act as sources of non-thermal emission and cosmic rays, gethering attention as WD pulsars. In this context, we studied the X-ray emissions from ZTF J190132.9+145808.7 (hereafter ZTF J1901+14), a notable massive isolated WD in the Galaxy, using the Chandra X-ray observatory. Our results showed 3.5σ level evidence of X-ray signals, although it is marginal. Under the assumption of a photon index of 2, we derived its intrinsic flux to be 2.3 (0.9-4.7) × 10-15 erg cm-2 s-1 and luminosity 4.6 (2.0-9.5) × 1026 erg s-1 for a 0.5-7 keV band in the $90\%$ confidence range, given its distance of 41 pc. We derived the X-ray efficiency (η) concerning the spin-down luminosity to be 0.012 (0.0022-0.074), a value comparable to that of ordinary neutron star pulsars. The inferred X-ray luminosity may be compatible with curvature radiation from sub-TeV electrons accelerated within open magnetic fields in the magnetosphere of ZTF J1901+14. Conducting more extensive X-ray observations is crucial to confirm whether ZTF J1901+14-like isolated WDs are also significant sources of X-rays and sub-TeV electron cosmic rays, similar to other WD pulsars in accreting systems....
Scientific journal
DOI：https://doi.org/10.1093/pasj/psae041
DOI ID：10.1093/pasj/psae041, ORCID：181064005, arXiv ID：arXiv:2404.14722, Bibcode：2024PASJ...76..702B - XRISM/Xtend Transient Search (XTS) detected the second X-ray flare from a BY Dra variable MS Ser
Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoneyama, T.; Yoshimoto, M.
Jul. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from the X-ray source XRISM J1558+2534, whose plausible counterpart is MS Ser, on 2024-07-02 TT. This is the second flare of this source during the XRISM observation of T CrB (ATel #16683)....
The Astronomer's Telegram
ORCID：181064051, Bibcode：2024ATel16685....1F - International Astrophysical Consortium for High-energy Calibration: Summary of the 15th IACHEC Workshop
Madsen, K. K.; Burwitz, V.; Forster, K.; Grant, C. E.; Guainazzi, M.; Kashyap, V.; Marshall, H. L.; Miller, E. D.; Natalucci, L.; Plucinsky, P. P.; Terada, Y.
Jul. 2024
In this report, we summarize the activities of the International Astronomical Consortium for High Energy Calibration (IACHEC) from the 15th IACHEC Workshop in Pelham, Germany. Sixty scientists directly involved in the calibration of operational and future high-energy missions gathered for 3.5 days to discuss the status of the cross-calibration between the current international complement of X-ray observatories and the possibilities to improve it. This summary consists of reports from the Working Groups with topics ranging across the identification and characterization of standard calibration sources, multi-observatory cross-calibration campaigns, appropriate and new statistical techniques, calibration of instruments and characterization of background, preservation of knowledge, and results for the benefit of the astronomical community....
arXiv e-prints
DOI：https://doi.org/10.48550/arXiv.2407.09432
DOI ID：10.48550/arXiv.2407.09432, ORCID：181064026, arXiv ID：arXiv:2407.09432, Bibcode：2024arXiv240709432M - XRISM/Xtend Transient Search (XTS) detected the second X-ray flare from UCAC2 15735923
Hayashi, K.; Fukushima, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoneyama, T.; Yoshimoto, M.
Jul. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1138-3742, whose plausible counterpart is UCAC2 15735923, on 2024-07-21....
The Astronomer's Telegram
ORCID：181064027, Bibcode：2024ATel16731....1H - XRISM/Xtend Transient Search (XTS) detected an X-ray flare from a BY Dra variable MS Ser
Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoneyama, T.; Yoshimoto, M.
Jul. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1558+2534 on 2024-07-01 TT. The source position is determined to be (R.A., Dec.) = (239.679 deg, +25.573 deg), with systematic error of & sim; 40 arcsec....
The Astronomer's Telegram
ORCID：181064052, Bibcode：2024ATel16683....1F - XRISM/Xtend Transient Search (XTS) detected a possible stellar flare from UCAC2 15735923
Yoshida, T.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoneyama, T.; Yoshimoto, M.
Jul. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source XRISM J1138-3742 on 2024-07-19 TT. The source position is determined to be (R.A., Dec.) = (174.415 deg, -37.707 deg), with a systematic error of -40 arcsec....
The Astronomer's Telegram
ORCID：181064050, Bibcode：2024ATel16728....1Y - XRISM/Xtend Transient Search (XTS) detected an X-ray flare possibly from a spectroscopic binary
Yoshida, T.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoneyama, T.; Yoshimoto, M.
Jun. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source candidate XRISM J1045-5954 on 2024-06-10 TT in the direction of the Carina Nebula....
The Astronomer's Telegram
ORCID：181064058, Bibcode：2024ATel16652....1Y - Probing Shocked Ejecta in SN 1987A with XRISM-Resolve: The Effects of the Gate Valve Closed
Sapienza, Vincenzo; Miceli, Marco; Bamba, Aya; Orlando, Salvatore; Lee, Shiu-Hang; Nagataki, Shigehiro; Ono, Masaomi; Katsuda, Satoru; Mori, Koji; Sawada, Makoto; Terada, Yukikatsu; Giuffrida, Roberta; Bocchino, Fabrizio
Research Notes of the American Astronomical Society, Jun. 2024
Supernova (SN) 1987A is widely regarded as an excellent candidate for leveraging the capabilities of the freshly launched XRISM satellite. Recent researches indicate that the X-ray emission from SN 1987A will increasingly originate from its ejecta in the years to come. In a previous study, we thoroughly examined the proficiency of XRISM-Resolve in identifying signatures of shocked ejecta in SN 1987A, synthesizing the XRISM-Resolve spectrum based on a state-of-the-art magneto-hydrodynamic simulation. However, following the satellite's launch, a technical issue arose with the XRISM instrument's gate valve, which failed to open, thereby affecting observations with the Resolve spectrometer. Here, we update our analysis, reevaluating our diagnostic approach under the assumption that the gate valve remains closed. We find that, even with the reduced instrumental capabilities, it will be possible to pinpoint the ejecta contribution through the study of the line profiles in the XRISM-Resolve spectrum of SN 1987A....
Scientific journal
DOI：https://doi.org/10.3847/2515-5172/ad55f6
DOI ID：10.3847/2515-5172/ad55f6, ORCID：168902927, arXiv ID：arXiv:2406.00090, Bibcode：2024RNAAS...8..156S - XRISM/Xtend Transient Search (XTS) detected an X-ray outburst from a high-mass X-ray binary AX J1910.7+0917
Yoshida, T.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoneyama, T.; Yoshimoto, M.
May 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray outburst from a high-mass X-ray binary AX J1910.7+0917 on 2024-04-28 TT. Due to a bad time interval of XRISM, the outburst start time was not detected, but only a rough constraint, 2024-04-28 19:52 & ndash; 20:41 TT, is given....
The Astronomer's Telegram
ORCID：181064062, Bibcode：2024ATel16607....1Y - XRISM/Xtend Transient Search (XTS) detected SN2024iss
Yoshida, T.; Fukushima, K.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoneyama, T.; Yoshimoto, M.; Fukazawa, Y.; Plucinsky, P.; bamba, A.; Murakami, H.; Tsuru, T.; Ezoe, Y.; Nakajima, H.; Enoto, T.; Nobukawa, K.; Vink, J.; Hamaguchi, K.; Odaka, H.; Sato, T.; Suzuki, H.; Ichinohe, Y.; Sawada, M.; Foster, A.; Ishida, M.; Smith, R.; Katsuda, S.; Tamura, K.; Matsumoto, H.; Tanaka, T.; Mori, K.
May 2024
XRISM team detected SN2024iss with Xtend during the ToO observation from 2024-05-24 16:56 TT to 2024-05-25 16:54 TT aimed at (RA, DEC) = (12h 59m 06s, 28d 48m 36s)....
The Astronomer's Telegram
ORCID：181064059, Bibcode：2024ATel16632....1Y - XRISM/Xtend Transient Search (XTS) detected an X-ray flare possibly from a spectroscopic binary
Yoneyama, T.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Audard, M.; Behar, E.; Inoue, S.; Ishihara, Y.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoshimoto, M.
Apr. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source candidate XRISM J1911+0509 on 2024-04-12 TT. The source position is determined to be (R.A., Dec.) = (287.737 deg, 5.152 deg) with systematic error of ~ 50 arcsec....
The Astronomer's Telegram
ORCID：181064063, Bibcode：2024ATel16592....1Y - XRISM/Xtend Transient Search (XTS) detected an X-ray flare possibly from a YSO candidate
Yoneyama, T.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Akasu, K.; Audard, M.; Behar, E.; Inoue, S.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nemoto, N.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoshimoto, M.
Mar. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source candidate XRISM J1628-4846 on 2024-03-30 TT. The source position is determined to be (R.A., Dec.) = (247.092 deg, -48.771 deg) with systematic error of ~ 1 arcmin....
The Astronomer's Telegram
ORCID：181064120, Bibcode：2024ATel16561....1Y - XRISM/Xtend Transient Search (XTS) detected an X-ray flare from a plausible optical counterpart LP 593-21
Yoshimoto, M.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Akasu, K.; Audard, M.; Behar, E.; Inoue, S.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nemoto, N.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoneyama, T.
Mar. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from a new X-ray source candidate XRISM J0335+0025 at 2024-03-09 TT. The source position is determined to be (R.A., Dec.) = (53.897 deg, 0.422 deg) with a systematic uncertainty of ~ 40 arcsec....
The Astronomer's Telegram
ORCID：181064122, Bibcode：2024ATel16532....1Y - XRISM/Xtend Transient Search (XTS) detected an X-ray flare possibly from 4XMM J190821.5+065854
Yoshimoto, M.; Hayashi, K.; Kanemaru, Y.; Ogawa, S.; Yoshida, T.; Akasu, K.; Audard, M.; Behar, E.; Inoue, S.; Kohmura, T.; Maeda, Y.; Mizumoto, M.; Nemoto, N.; Nobukawa, M.; Pottschmidt, K.; Shidatsu, M.; Terada, Y.; Terashima, Y.; Tsuboi, Y.; Uchida, H.; Yoneyama, T.
Mar. 2024
XRISM/Xtend Transient Search (XTS) detected an X-ray flare from an X-ray source candidate XRISM J1908+0659 on 2024-03-27 TT. The source position is determined to be (R.A., Dec.) = (287.089 deg, 6.976 deg) with a systematic uncertainty of 40 arcsec....
The Astronomer's Telegram
ORCID：181064121, Bibcode：2024ATel16558....1Y - Probing Shocked Ejecta in SN 1987A: A Novel Diagnostic Approach Using XRISM-Resolve
Sapienza, Vincenzo; Miceli, Marco; Bamba, Aya; Orlando, Salvatore; Lee, Shiu-Hang; Nagataki, Shigehiro; Ono, Masaomi; Katsuda, Satoru; Mori, Koji; Sawada, Makoto; Terada, Yukikatsu; Giuffrida, Roberta; Bocchino, Fabrizio
The Astrophysical Journal, Jan. 2024, [Reviewed]
Supernova (SN) 1987A is one of the best candidates to exploit the capabilities of the freshly launched XRISM satellite. This celestial object offers the unique opportunity to study the evolution of an SN into a young supernova remnant. To date, the X-ray emission has been dominated by the shocked circumstellar medium, with no shocked ejecta firmly detected. However, recent studies provide compelling evidence that in the forthcoming years, the X-ray emission from SN 1987A will increasingly stem from the ejecta. Our aim is to assess the proficiency of the XRISM-Resolve high-resolution spectrometer in pinpointing signatures of the shocked ejecta in SN 1987A. Taking advantage of a self-consistent state-of-the-art magneto-hydrodynamic simulation that describes the evolution from SN 1987A to its remnant, we synthesized the XRISM-Resolve spectrum of SN 1987A, as it would be collected in the allocated observation during the performance verification phase, which is foreseen for 2024. Our predictions clearly show the leading role of shocked ejecta in shaping the profile of the emission lines. The Doppler broadening associated with the bulk motion along the line of sight of the rapidly expanding ejecta is shown to increase the line widths well above the values observed so far. The quantitative comparison between our synthetic spectra and the XRISM spectra will enable us to establish a strong connection between the broadened line emission and the freshly shocked ejecta. This, in turn, will allow us to retrieve the ejecta dynamics and chemical composition from the X-ray emission....
Scientific journal
DOI：https://doi.org/10.3847/2041-8213/ad16e3
DOI ID：10.3847/2041-8213/ad16e3, ORCID：168902917, arXiv ID：arXiv:2312.11129, Bibcode：2024ApJ...961L...9S - The High Energy X-ray Probe (HEX-P): supernova remnants, pulsar wind nebulae, and nuclear astrophysics
Reynolds, Stephen; An, Hongjun; Abdelmaguid, Moaz; Alford, Jason; Fryer, Chris; Mori, Kaya; Nynka, Melania; Park, Jaegeun; Terada, Yukikatsu; Woo, Jooyun; Bamba, Aya; Bangale, Priyadarshini; Diesing, Rebecca; Eagle, Jordan; Gabici, Stefano; Gelfand, Joseph; Grefenstette, Brian; Garcia, Javier; Kim, Chanho; Kumar, Sajan; Intyre, Brydyn Mac; Madsen, Kristin; Manconi, Silvia; Motogami, Yugo; Ohsumi, Hayato; Olmi, Barbara; Sato, Toshiki; Shang, Ruo-Yu; Stern, Daniel; Tsuji, Naomi; Younes, George; Zoglauer, Andreas
Frontiers in Astronomy and Space Sciences, Dec. 2023, [Reviewed]
HEX-P is a probe-class mission concept that will combine high spatial resolution X-ray imaging (<10″ full width at half maximum) and broad spectral coverage (0.2–80 keV) with an effective area far superior to current facilities (including XMM-Newton and NuSTAR) to enable revolutionary new insights into a variety of important astrophysical problems. HEX-P is ideally suited to address important problems in the physics and astrophysics of supernova remnants (SNRs) and pulsar wind nebulae (PWNe). For shell SNRs, HEX-P can greatly improve our understanding via more accurate spectral characterization and localization of non-thermal X-ray emission from both non-thermal-dominated SNRs and those containing both thermal and non-thermal components, and can discover previously unknown non-thermal components in SNRs. Multi-epoch HEX-P observations of several young SNRs (e.g., Cas A and Tycho) are expected to detect year-scale variabilities of X-ray filaments and knots, thus enabling us to determine fundamental parameters related to diffusive shock acceleration, such as local magnetic field strengths and maximum electron energies. For PWNe, HEX-P will provide spatially-resolved, broadband X-ray spectral data separately from their pulsar emission, allowing us to study how particle acceleration, cooling, and propagation operate in different evolution stages of PWNe. HEX-P is also poised to make unique and significant contributions to nuclear astrophysics of Galactic radioactive sources by improving detections of, or limits on, 44Ti in the youngest SNRs and by potentially discovering rare nuclear lines as evidence of double neutron star mergers. Throughout the paper, we present simulations of each class of objects, demonstrating the power of both the imaging and spectral capabilities of HEX-P to advance our knowledge of SNRs, PWNe, and nuclear astrophysics....
Scientific journal
DOI：https://doi.org/10.3389/fspas.2023.1321278
DOI ID：10.3389/fspas.2023.1321278, ORCID：181064206, arXiv ID：arXiv:2311.04952, Bibcode：2023FrASS..1021278R - The high energy X-ray probe (HEX-P): Galactic PeVatrons, star clusters, superbubbles, microquasar jets, and gamma-ray binaries
Mori, Kaya; Reynolds, Stephen; An, Hongjun; Bamba, Aya; Krivonos, Roman; Tsuji, Naomi; Abdelmaguid, Moaz; Alford, Jason; Bangale, Priyadarshini; Celli, Silvia; Diesing, Rebecca; Eagle, Jordan; Fryer, Chris L.; Gabici, Stefano; Gelfand, Joseph; Grefenstette, Brian; Garcia, Javier; Kim, Chanho; Kumar, Sajan; Kuznetsova, Ekaterina; Mac Intyre, Brydyn; Madsen, Kristin; Manconi, Silvia; Motogami, Yugo; Ohsumi, Hayato; Olmi, Barbara; Park, Jaegeun; Ponti, Gabriele; Sato, Toshiki; Shang, Ruo-Yu; Stern, Daniel; Terada, Yukikatsu; Woo, Jooyun; Younes, George; Zoglauer, Andreas
Frontiers in Astronomy and Space Sciences, Dec. 2023, [Reviewed]
HEX-P is a probe-class mission concept that will combine high spatial resolution X-ray imaging (<10″ FWHM) and broad spectral coverage (0.2–80 keV) with an effective area far superior to current facilities (including XMM-Newton and NuSTAR) to enable revolutionary new insights into a variety of important astrophysical problems. With the recent discoveries of over 40 ultra-high-energy gamma-ray sources (detected above 100 TeV) and neutrino emission in the Galactic Plane, we have entered a new era of multi-messenger astrophysics facing the exciting reality of Galactic PeVatrons. In the next decade, as more Galactic PeVatrons and TeV gamma-ray sources are expected to be discovered, the identification of their acceleration and emission mechanisms will be the most pressing issue in both particle and high-energy astrophysics. In this paper, along with its companion papers, we will present that HEX-P is uniquely suited to address important problems in various cosmic-ray accelerators, including Galactic PeVatrons, through investigating synchrotron X-ray emission of TeV–PeV electrons produced by both leptonic and hadronic processes. For Galactic PeVatron candidates and other TeV gamma-ray sources, HEX-P can fill in a large gap in the spectral-energy distributions (SEDs) of many objects observed in radio, soft X-rays, and gamma rays, constraining the maximum energies to which electrons can be accelerated, with implications for the nature of the Galactic PeVatrons and their contributions to the spectrum of Galactic cosmic rays beyond the knee at ∼3 PeV. In particular, X-ray observation with HEX-P and TeV observation with CTAO will provide the most powerful multi-messenger diagnostics to identify Galactic PeVatrons and explore a variety of astrophysical shock mechanisms. We present simulations of each class of Galactic TeV–PeV sources, demonstrating the power of both the imaging and spectral capabilities of HEX-P to advance our knowledge of Galactic cosmic-ray accelerators. In addition, we discuss HEX-P's unique and complementary roles to upcoming gamma-ray and neutrino observatories in the 2030s....
Scientific journal
DOI：https://doi.org/10.3389/fspas.2023.1303197
DOI ID：10.3389/fspas.2023.1303197, ORCID：181064210, arXiv ID：arXiv:2311.04851, Bibcode：2023FrASS..1003197M - Performance of the joint LST-1 and MAGIC observations evaluated with Crab Nebula data
Abe, H.; Abe, K.; Abe, S.; Acciari, V. A.; Aguasca-Cabot, A.; Agudo, I.; Alvarez Crespo, N.; Aniello, T.; Ansoldi, S.; Antonelli, L. A.; Aramo, C.; Arbet-Engels, A.; Arcaro, C.; Artero, M.; Asano, K.; Aubert, P.; Baack, D.; Babić, A.; Baktash, A.; Bamba, A.; Baquero Larriva, A.; Baroncelli, L.; Barres de Almeida, U.; Barrio, J. A.; Batković, I.; Baxter, J.; Becerra González, J.; Bednarek, W.; Bernardini, E.; Bernardos, M. I.; Bernete Medrano, J.; Berti, A.; Besenrieder, J.; Bhattacharjee, P.; Biederbeck, N.; Bigongiari, C.; Biland, A.; Bissaldi, E.; Blanch, O.; Bonnoli, G.; Bordas, P.; Bošnjak, Ž.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Buscemi, M.; Busetto, G.; Campoy Ordaz, A.; Cardillo, M.; Caroff, S.; Carosi, A.; Carosi, R.; Carrasco, M. S.; Carretero-Castrillo, M.; Cassol, F.; Castro-Tirado, A. J.; Cauz, D.; Cerasole, D.; Ceribella, G.; Chai, Y.; Cheng, K.; Chiavassa, A.; Chikawa, M.; Chytka, L.; Cifuentes, A.; Cikota, S.; Colombo, E.; Contreras, J. L.; Cornelia, A.; Cortina, J.; Costantini, H.; Covino, S.; D'Amico, G.; D'Elia, V.; Da Vela, P.; Dalchenko, M.; Dazzi, F.; De Angelis, A.; de Bony de Lavergne, M.; De Lotto, B.; De Lucia, M.; de Menezes, R.; Del Peral, L.; Del Popolo, A.; Deleglise, G.; Delfino, M.; Delgado Mendez, C.; Delgado Mengual, J.; della Volpe, D.; Dellaiera, M.; Depaoli, D.; De Angelis, A.; Di Piano, A.; Di Pierro, F.; Di Pilato, A.; Di Tria, R.; Di Venere, L.; Dominik, R. M.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro, M.; Díaz, C.; Eisenberger, L.; Elsässer, D.; Emery, G.; Escudero, J.; Fallah Ramazani, V.; Fariña, L.; Fattorini, A.; Ferrara, G.; Ferrarotto, F.; Fiasson, A.; Foffano, L.; Font, L.; Freixas Coromina, L.; Fröse, S.; Fukami, S.; Fukazawa, Y.; Garcia López, R. J.; Garcia, E.; Garczarczyk, M.; García López, R. J.; Gasbarra, C.; Gasparrini, D.; Gasparyan, S.; Gaug, M.; Geyer, D.; Giesbrecht Paiva, J. G.; Giglietto, N.; Giordano, F.; Gliwny, P.; Godinović, N.; Grau, R.; Green, D.; Green, J. G.; Gunji, S.; Günther, P.; Hackfeld, J.; Hadasch, D.; Hahn, A.; Hashiyama, K.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Herrera Llorente, J.; Hirotani, K.; Hoffmann, D.; Horns, D.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Hui, D.; Hütten, M.; Iarlori, M.; Imazawa, R.; Inada, T.; Inome, Y.; Ioka, K.; Iori, M.; Iotov, R.; Ishio, K.; Jacquemont, M.; Jiménez Martínez, I.; Jobst, E.; Jormanainen, J.; Jurysek, J.; Kagaya, M.; Karas, V.; Katagiri, H.; Kataoka, J.; Kerszberg, D.; Kluge, G. W.; Kobayashi, Y.; Kohri, K.; Kong, A.; Kouch, P. M.; Kubo, H.; Kushida, J.; Lainez, M.; Lamanna, G.; Lamastra, A.; Le Flour, T.; Leone, F.; Lindfors, E.; Linhoff, L.; Linhoff, M.; Lombardi, S.; Longo, F.; Loporchio, S.; Lorini, A.; Lozano Bahilo, J.; Luque-Escamilla, P. L.; Lyard, E.; Láinez Lezáun, M.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Machado de Oliveira Fraga, B.; Majumdar, P.; Makariev, M.; Mandat, D.; Maneva, G.; Manganaro, M.; Mangano, S.; Mang, N.; Manicò, G.; Mannheim, K.; Mariotti, M.; Marquez, P.; Marsella, G.; Martinez, O.; Martínez, G.; Martínez, M.; Martí, J.; Mas-Aguilar, A.; Maurin, G.; Mazin, D.; Menchiari, S.; Mender, S.; Mestre Guillen, E.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Mićanović, S.; Molero González, M.; Molina, E.; Mondal, H. A.; Montaruli, T.; Monteiro, I.; Moralejo, A.; Morcuende, D.; Morselli, A.; Moya, V.; Muraishi, H.; Murase, K.; Nagataki, S.; Nakamori, T.; Nanci, C.; Neronov, A.; Neustroev, V.; Nickel, L.; Nievas Rosillo, M.; Nigro, C.; Nikolić, L.; Nilsson, K.; Nishijima, K.; Njoh Ekoume, T.; Noda, K.; Nosek, D.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Oka, T.; Okumura, A.; Orito, R.; Otero-Santos, J.; Paiano, S.; Palatiello, M.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Pavletić, L.; Pech, M.; Pecimotika, M.; Peresano, M.; Persic, M.; Pfeiffle, F.; Pietropaolo, E.; Pihet, M.; Pirola, G.; Plard, C.; Podobnik, F.; Poireau, V.; Polo, M.; Pons, E.; Prada Moroni, P. G.; Prandini, E.; Prast, J.; Principe, G.; Priyadarshi, C.; Prouza, M.; Rando, R.; Rhode, W.; Ribó, M.; Rico, J.; Righi, C.; Rizi, V.; Rodriguez Fernandez, G.; Rodríguez Frías, M. D.; Sahakyan, N.; Saito, T.; Sakurai, S.; Sanchez, D. A.; Satalecka, K.; Sato, M.; Sato, Y.; Saturni, F. G.; Savchenko, V.; Schleicher, B.; Schmidt, K.; Schmuckermaier, F.; Schubert, J. L.; Schussler, F.; Schweizer, T.; Sciaccaluga, A.; Siegert, T.; Silvia, R.; Sitarek, J.; Sliusar, V.; Sobczynska, D.; Spolon, A.; Stamerra, A.; Strišković, J.; Strom, D.; Strzys, M.; Suda, Y.; Suutarinen, S.; Šarić, T.; Tajima, H.; Takahashi, H.; Takahashi, M.; Takata, J.; Takeishi, R.; Tam, P. H. T.; Tanaka, S. J.; Tateishi, D.; Tavecchio, F.; Temnikov, P.; Terada, Y.; Terauchi, K.; Terzić, T.; Teshima, M.; Tluczykont, M.; Tokanai, F.; Torres, D. F.; Tosti, L.; Travnicek, P.; Truzzi, S.; Tutone, A.; Ubach, S.; Vacula, M.; Vallania, P.; van Scherpenberg, J.; Vazquez Acosta, M.; Ventura, S.; Verguilov, V.; Viale, I.; Vigliano, A.; Vigorito, C. F.; Visentin, E.; Vitale, V.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Vázquez Acosta, M.; Walter, R.; Wei, Z.; Will, M.; Yamamoto, T.; Yamazaki, R.; Yoshida, T.; Yoshikoshi, T.; Zywucka, N.
Astronomy and Astrophysics, Dec. 2023, [Reviewed]
Aims: Large-Sized Telescope 1 (LST-1), the prototype for the Large-Sized Telescope at the upcoming Cherenkov Telescope Array Observatory, is concluding its commissioning phase at the Observatorio del Roque de los Muchachos on the island of La Palma. The proximity of LST-1 to the two MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes makes it possible to carry out observations of the same gamma-ray events with both systems.
Methods: We describe the joint LST-1+MAGIC analysis pipeline and used simultaneous Crab Nebula observations and Monte Carlo simulations to assess the performance of the three-telescope system. The addition of the LST-1 telescope allows for the recovery of events in which one of the MAGIC images is too dim to survive analysis quality cuts.
Results: Thanks to the resulting increase in the collection area and stronger background rejection, we found a significant improvement in sensitivity, allowing for the detection of 30% weaker fluxes in the energy range between 200 GeV and 3 TeV. The spectrum of the Crab Nebula, reconstructed in the energy range between ~60 GeV and ~10 TeV, is in agreement with previous measurements....
Scientific journal
DOI：https://doi.org/10.1051/0004-6361/202346927
DOI ID：10.1051/0004-6361/202346927, ORCID：181064209, arXiv ID：arXiv:2310.01954, Bibcode：2023A&A...680A..66A - Star tracking for pointing determination of Imaging Atmospheric Cherenkov Telescopes. Application to the Large-Sized Telescope of the Cherenkov Telescope Array
Abe, K.; Abe, S.; Aguasca-Cabot, A.; Agudo, I.; Alvarez Crespo, N.; Antonelli, L. A.; Aramo, C.; Arbet-Engels, A.; Cornelia, A.; Artero, M.; Asano, K.; Aubert, P.; Baktash, A.; Bamba, A.; Baquero Larriva, A.; Baroncelli, L.; Barres de Almeida, U.; Barrio, J. A.; Batkovic, I.; Baxter, J.; Becerra González, J.; Bernardini, E.; Bernardos, M. I.; Bernete Medrano, J.; Berti, A.; Bhattacharjee, P.; Biederbeck, N.; Bigongiari, C.; Bissaldi, E.; Blanch, O.; Bonnoli, G.; Bordas, P.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Buscemi, M.; Cardillo, M.; Caroff, S.; Carosi, A.; Cassol, F.; Cauz, D.; Ceribella, G.; Chai, Y.; Cheng, K.; Chiavassa, A.; Chikawa, M.; Chytka, L.; Cifuentes, A.; Contreras, J. L.; Cortina, J.; Costantini, H.; Dalchenko, M.; De Angelis, A.; de Bony de Lavergne, M.; De Lotto, B.; de Menezes, R.; Deleglise, G.; Delgado, C.; Delgado Mengual, J.; della Volpe, D.; Dellaiera, M.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Díaz, C.; Dominik, R. M.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro, M.; Elsässer, D.; Emery, G.; Escudero, J.; Fallah Ramazani, V.; Ferrara, G.; Ferrarotto, F.; Fiasson, A.; Freixas Coromina, L.; Fröse, S.; Fukami, S.; Fukazawa, Y.; Garcia, E.; Garcia López, R.; Gasbarra, C.; Gasparrini, D.; Geyer, D.; Giesbrecht Paiva, J.; Giglietto, N.; Giordano, F.; Giro, E.; Gliwny, P.; Godinovic, N.; Grau, R.; Green, D.; Green, J.; Gunji, S.; Günther, P.; Hackfeld, J.; Hadasch, D.; Hahn, A.; Hashiyama, K.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Herrera Llorente, J.; Hirotani, K.; Hoffmann, D.; Horns, D.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Hui, D.; Hütten, M.; Iarlori, M.; Imazawa, R.; Inada, T.; Inome, Y.; Ioka, K.; Iori, M.; Ishio, K.; Jacquemont, M.; Jimenez Martinez, I.; Jurysek, J.; Kagaya, M.; Karas, V.; Katagiri, H.; Kataoka, J.; Kerszberg, D.; Kobayashi, Y.; Kohri, K.; Kong, A.; Kubo, H.; Kushida, J.; Lainez, M.; Lamanna, G.; Lamastra, A.; Le Flour, T.; Linhoff, M.; Longo, F.; López-Coto, R.; López-Oramas, A.; Loporchio, S.; Lorini, A.; Luque-Escamilla, P. L.; Majumdar, P.; Makariev, M.; Mandat, D.; Manganaro, M.; Manicò, G.; Mannheim, K.; Mariotti, M.; Marquez, P.; Marsella, G.; Martí, J.; Martinez, O.; Martínez, G.; Martínez, M.; Mas-Aguilar, A.; Maurin, G.; Mazin, D.; Mestre Guillen, E.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Molero Gonzalez, M.; Molina, E.; Montaruli, T.; Monteiro, I.; Moralejo, A.; Morcuende, D.; Morselli, A.; Muraishi, H.; Murase, K.; Nagataki, S.; Nakamori, T.; Nickel, L.; Nievas, M.; Nishijima, K.; Noda, K.; Nosek, D.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Oka, T.; Okumura, A.; Orito, R.; Otero-Santos, J.; Palatiello, M.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Pech, M.; Pecimotika, M.; Peresano, M.; Pfeiffle, F.; Pietropaolo, E.; Pirola, G.; Plard, C.; Podobnik, F.; Poireau, V.; Polo, M.; Pons, E.; Prandini, E.; Prast, J.; Principe, G.; Priyadarshi, C.; Prouza, M.; Rando, R.; Rhode, W.; Ribó, M.; Rizi, V.; Rodriguez Fernandez, G.; Saito, T.; Sakurai, S.; Sanchez, D. A.; Šarić, T.; Sato, Y.; Saturni, F. G.; Schleicher, B.; Schmuckermaier, F.; Schubert, J. L.; Schussler, F.; Schweizer, T.; Sato, M.; Siegert, T.; Silvia, R.; Sitarek, J.; Sliusar, V.; Spolon, A.; Strišković, J.; Strzys, M.; Suda, Y.; Tajima, H.; Takahashi, H.; Takahashi, M.; Takata, J.; Takeishi, R.; Tam, P. H. T.; Tanaka, S. J.; Tateishi, D.; Temnikov, P.; Terada, Y.; Terauchi, K.; Terzic, T.; Teshima, M.; Tluczykont, M.; Tokanai, F.; Torres, D. F.; Travnicek, P.; Truzzi, S.; Tutone, A.; Vacula, M.; Vallania, P.; van Scherpenberg, J.; Vázquez Acosta, M.; Viale, I.; Vigliano, A.; Vigorito, C. F.; Vitale, V.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Walter, R.; Wei, Z.; Will, M.; Yamamoto, T.; Yamazaki, R.; Yoshida, T.; Yoshikoshi, T.; Zywucka, N.
Astronomy and Astrophysics, Nov. 2023, [Reviewed]
We present a novel approach to the determination of the pointing of Imaging Atmospheric Cherenkov Telescopes (IACTs) using the trajectories of the stars in their camera's field of view. The method starts with the reconstruction of the star positions from the Cherenkov camera data, taking into account the point spread function of the telescope, to achieve a satisfying reconstruction accuracy of the pointing position. A simultaneous fit of all reconstructed star trajectories is then performed with the orthogonal distance regression (ODR) method. ODR allows us to correctly include the star position uncertainties and use the time as an independent variable. Having the time as an independent variable in the fit makes it better suitable for various star trajectories. This method can be applied to any IACT and requires neither specific hardware nor interface or special data-taking mode. In this paper, we use the Large-Sized Telescope (LST) data to validate it as a useful tool to improve the determination of the pointing direction during regular data taking. The simulation studies show that the accuracy and precision of the method are comparable with the design requirements on the pointing accuracy of the LST (≤14″). With the typical LST event acquisition rate of 10 kHz, the method can achieve up to 50 Hz pointing monitoring rate, compared to ��(1) Hz achievable with standard techniques. The application of the method to the LST prototype (LST-1) commissioning data shows the stable pointing performance of the telescope....
Scientific journal
DOI：https://doi.org/10.1051/0004-6361/202347128
DOI ID：10.1051/0004-6361/202347128, ORCID：181064215, Bibcode：2023A&A...679A..90A - Observations of the Crab Nebula and Pulsar with the Large-sized Telescope Prototype of the Cherenkov Telescope Array
Abe, H.; Abe, K.; Abe, S.; Aguasca-Cabot, A.; Agudo, I.; Alvarez Crespo, N.; Antonelli, L. A.; Aramo, C.; Arbet-Engels, A.; Arcaro, C.; Artero, M.; Asano, K.; Aubert, P.; Baktash, A.; Bamba, A.; Baquero Larriva, A.; Baroncelli, L.; Barres de Almeida, U.; Barrio, J. A.; Batkovic, I.; Baxter, J.; Becerra González, J.; Bernardini, E.; Bernardos, M. I.; Bernete Medrano, J.; Berti, A.; Bhattacharjee, P.; Biederbeck, N.; Bigongiari, C.; Bissaldi, E.; Blanch, O.; Bonnoli, G.; Bordas, P.; Borghese, A.; Bulgarelli, A.; Burelli, I.; Buscemi, M.; Cardillo, M.; Caroff, S.; Carosi, A.; Cassol, F.; Cauz, D.; Ceribella, G.; Chai, Y.; Cheng, K.; Chiavassa, A.; Chikawa, M.; Chytka, L.; Cifuentes, A.; Contreras, J. L.; Cortina, J.; Costantini, H.; D'Amico, G.; Dalchenko, M.; De Angelis, A.; de Bony de Lavergne, M.; De Lotto, B.; de Menezes, R.; Deleglise, G.; Delgado, C.; Delgado Mengual, J.; della Volpe, D.; Dellaiera, M.; Depaoli, D.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Díaz, C.; Dominik, R. M.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro, M.; Elsässer, D.; Emery, G.; Escudero, J.; Fallah Ramazani, V.; Ferrara, G.; Ferrarotto, F.; Fiasson, A.; Freixas Coromina, L.; Fröse, S.; Fukami, S.; Fukazawa, Y.; Garcia, E.; Garcia López, R.; Gasbarra, C.; Gasparrini, D.; Geyer, F.; Giesbrecht Paiva, J.; Giglietto, N.; Giordano, F.; Giro, E.; Gliwny, P.; Godinovic, N.; Grau, R.; Green, D.; Green, J.; Gunji, S.; Hackfeld, J.; Hadasch, D.; Hahn, A.; Hashiyama, K.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Herrera Llorente, J.; Hirotani, K.; Hoffmann, D.; Horns, D.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Hui, D.; Hütten, M.; Iarlori, M.; Imazawa, R.; Inada, T.; Inome, Y.; Ioka, K.; Iori, M.; Ishio, K.; Iwamura, Y.; Jacquemont, M.; Jimenez Martinez, I.; Jurysek, J.; Kagaya, M.; Karas, V.; Katagiri, H.; Kataoka, J.; Kerszberg, D.; Kobayashi, Y.; Kong, A.; Kubo, H.; Kushida, J.; Lainez, M.; Lamanna, G.; Lamastra, A.; Le Flour, T.; Linhoff, M.; Longo, F.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Lorini, A.; Luque-Escamilla, P. L.; Majumdar, P.; Makariev, M.; Mandat, D.; Manganaro, M.; Manicò, G.; Mannheim, K.; Mariotti, M.; Marquez, P.; Marsella, G.; Martí, J.; Martinez, O.; Martínez, G.; Martínez, M.; Marusevec, P.; Mas-Aguilar, A.; Maurin, G.; Mazin, D.; Mestre Guillen, E.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Molero Gonzalez, M.; Molina, E.; Montaruli, T.; Monteiro, I.; Moralejo, A.; Morcuende, D.; Morselli, A.; Mrakovcic, K.; Murase, K.; Nagai, A.; Nagataki, S.; Nakamori, T.; Nickel, L.; Nievas, M.; Nishijima, K.; Noda, K.; Nosek, D.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Oka, T.; Okazaki, N.; Okumura, A.; Orito, R.; Otero-Santos, J.; Palatiello, M.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Pech, M.; Pecimotika, M.; Peresano, M.; Pérez, A.; Pietropaolo, E.; Pirola, G.; Plard, C.; Podobnik, F.; Poireau, V.; Polo, M.; Pons, E.; Prandini, E.; Prast, J.; Principe, G.; Priyadarshi, C.; Prouza, M.; Rando, R.; Rhode, W.; Ribó, M.; Rizi, V.; Rodriguez Fernandez, G.; Ruiz, J. E.; Saito, T.; Sakurai, S.; Sanchez, D. A.; Šarić, T.; Sato, Y.; Saturni, F. G.; Schleicher, B.; Schmuckermaier, F.; Schubert, J. L.; Schussler, F.; Schweizer, T.; Seglar Arroyo, M.; Silvia, R.; Sitarek, J.; Sliusar, V.; Spolon, A.; Strišković, J.; Strzys, M.; Suda, Y.; Sunada, Y.; Tajima, H.; Takahashi, H.; Takahashi, M.; Takata, J.; Takeishi, R.; Tam, P. H. T.; Tanaka, S. J.; Tateishi, D.; Tejedor, L. A.; Temnikov, P.; Terada, Y.; Terauchi, K.; Terzic, T.; Teshima, M.; Tluczykont, M.; Tokanai, F.; Torres, D. F.; Travnicek, P.; Truzzi, S.; Tutone, A.; Uhlrich, G.; Vacula, M.; Vallania, P.; van Scherpenberg, J.; Vázquez Acosta, M.; Verguilov, V.; Viale, I.; Vigliano, A.; Vigorito, C. F.; Vitale, V.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Walter, R.; Will, M.; Yamamoto, T.; Yamazaki, R.; Yoshida, T.; Yoshikoshi, T.; Zywucka, N.; Bernlöhr, K.; Gueta, O.; Kosack, K.; Maier, G.; Watson, J.
The Astrophysical Journal, Oct. 2023, [Reviewed]
The Cherenkov Telescope Array (CTA) is a next-generation ground-based observatory for gamma-ray astronomy at very high energies. The Large-Sized Telescope prototype (LST-1) is located at the CTA-North site, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to ≃20 GeV. LST-1 started performing astronomical observations in 2019 November, during its commissioning phase, and it has been taking data ever since. We present the first LST-1 observations of the Crab Nebula, the standard candle of very-high-energy gamma-ray astronomy, and use them, together with simulations, to assess the performance of the telescope. LST-1 has reached the expected performance during its commissioning period-only a minor adjustment of the preexisting simulations was needed to match the telescope's behavior. The energy threshold at trigger level is around 20 GeV, rising to ≃30 GeV after data analysis. Performance parameters depend strongly on energy, and on the strength of the gamma-ray selection cuts in the analysis: angular resolution ranges from 0.°12-0.°40, and energy resolution from 15%-50%. Flux sensitivity is around 1.1% of the Crab Nebula flux above 250 GeV for a 50 hr observation (12% for 30 minutes). The spectral energy distribution (in the 0.03-30 TeV range) and the light curve obtained for the Crab Nebula agree with previous measurements, considering statistical and systematic uncertainties. A clear periodic signal is also detected from the pulsar at the center of the Nebula....
Scientific journal
DOI：https://doi.org/10.3847/1538-4357/ace89d
DOI ID：10.3847/1538-4357/ace89d, ORCID：168902915, arXiv ID：arXiv:2306.12960, Bibcode：2023ApJ...956...80A - Gravitational Redshift Detection from the Magnetic White Dwarf Harbored in RX J1712.6-2414
Hayashi, Takayuki; Mori, Hideyuki; Mukai, Koji; Terada, Yukikatsu; Ishida, Manabu
The Astrophysical Journal, Aug. 2023, [Reviewed]
Gravitational redshift is a fundamental parameter that allows us to determine the mass-to-radius ratio of compact stellar objects, such as black holes, neutron stars, and white dwarfs (WDs). In the X-ray spectra of the close binary system, RX J1712.6-2414, obtained from the Chandra High Energy Transmission Grating observation, we detected significant redshifts for characteristic X-rays emitted from hydrogen-like magnesium, silicon (ΔE/E rest ~ 7 × 10-4), and sulfur (ΔE/E rest ~ 15 × 10-4) ions, which are over the instrumental absolute energy accuracy (ΔE/E rest ~ 3.3 × 10-4). Considering some possible factors, such as Doppler shifts associated with the plasma flow, systemic velocity, and optical depth, we concluded that the major contributor to the observed redshift is the gravitational redshift of the WD harbored in the binary system, which is the first gravitational redshift detection from a magnetic WD. Moreover, the gravitational redshift provides us with a new method of WD mass measurement by invoking the plasma-flow theory with strong magnetic fields in close binaries. Regardless of large uncertainty, our new method estimated the WD mass to be M WD > 0.9 M ⊙....
Scientific journal
DOI：https://doi.org/10.3847/1538-4357/acd001
DOI ID：10.3847/1538-4357/acd001, ORCID：168902909, arXiv ID：arXiv:2305.01496, Bibcode：2023ApJ...953...30H - Multiwavelength study of the galactic PeVatron candidate LHAASO J2108+5157
Abe, S.; Aguasca-Cabot, A.; Agudo, I.; Alvarez Crespo, N.; Antonelli, L. A.; Aramo, C.; Arbet-Engels, A.; Artero, M.; Asano, K.; Aubert, P.; Baktash, A.; Bamba, A.; Baquero Larriva, A.; Baroncelli, L.; Barres de Almeida, U.; Barrio, J. A.; Batkovic, I.; Baxter, J.; Becerra González, J.; Bernardini, E.; Bernardos, M. I.; Bernete Medrano, J.; Berti, A.; Bhattacharjee, P.; Biederbeck, N.; Bigongiari, C.; Bissaldi, E.; Blanch, O.; Bordas, P.; Buisson, C.; Bulgarelli, A.; Burelli, I.; Buscemi, M.; Cardillo, M.; Caroff, S.; Carosi, A.; Cassol, F.; Cauz, D.; Ceribella, G.; Chai, Y.; Cheng, K.; Chiavassa, A.; Chikawa, M.; Chytka, L.; Cifuentes, A.; Contreras, J. L.; Cortina, J.; Costantini, H.; D'Amico, G.; Dalchenko, M.; De Angelis, A.; de Bony de Lavergne, M.; De Lotto, B.; de Menezes, R.; Deleglise, G.; Delgado, C.; Delgado Mengual, J.; della Volpe, D.; Dellaiera, M.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Díaz, C.; Dominik, R. M.; Dominis Prester, D.; Donini, A.; Dorner, D.; Doro, M.; Elsässer, D.; Emery, G.; Escudero, J.; Fallah Ramazani, V.; Ferrara, G.; Fiasson, A.; Freixas Coromina, L.; Fröse, S.; Fukami, S.; Fukazawa, Y.; Garcia, E.; Garcia López, R.; Gasparrini, D.; Geyer, D.; Giesbrecht Paiva, J.; Giglietto, N.; Giordano, F.; Giro, E.; Gliwny, P.; Godinovic, N.; Grau, R.; Green, D.; Green, J.; Gunji, S.; Hackfeld, J.; Hadasch, D.; Hahn, A.; Hashiyama, K.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Herrera Llorente, J.; Hirotani, K.; Hoffmann, D.; Horns, D.; Houles, J.; Hrabovsky, M.; Hrupec, D.; Hui, D.; Hütten, M.; Imazawa, R.; Inada, T.; Inome, Y.; Ioka, K.; Iori, M.; Ishio, K.; Iwamura, Y.; Jacquemont, M.; Jimenez Martinez, I.; Jurysek, J.; Kagaya, M.; Karas, V.; Katagiri, H.; Kataoka, J.; Kerszberg, D.; Kobayashi, Y.; Kong, A.; Kubo, H.; Kushida, J.; Lainez, M.; Lamanna, G.; Lamastra, A.; Le Flour, T.; Linhoff, M.; Longo, F.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Lorini, A.; Luque-Escamilla, P. L.; Majumdar, P.; Makariev, M.; Mandat, D.; Manganaro, M.; Manicò, G.; Mannheim, K.; Mariotti, M.; Marquez, P.; Marsella, G.; Martí, J.; Martinez, O.; Martínez, G.; Martínez, M.; Marusevec, P.; Mas-Aguilar, A.; Maurin, G.; Mazin, D.; Mestre Guillen, E.; Micanovic, S.; Miceli, D.; Miener, T.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Molero Gonzalez, M.; Molina, E.; Montaruli, T.; Monteiro, I.; Moralejo, A.; Morcuende, D.; Morselli, A.; Mrakovcic, K.; Murase, K.; Nagai, A.; Nakamori, T.; Nickel, L.; Nievas, M.; Nishijima, K.; Noda, K.; Nosek, D.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Okazaki, N.; Okumura, A.; Orito, R.; Otero-Santos, J.; Palatiello, M.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Pavletić, L.; Pech, M.; Pecimotika, M.; Pietropaolo, E.; Pirola, G.; Podobnik, F.; Poireau, V.; Polo, M.; Pons, E.; Prandini, E.; Prast, J.; Priyadarshi, C.; Prouza, M.; Rando, R.; Rhode, W.; Ribó, M.; Rizi, V.; Rodriguez Fernandez, G.; Saito, T.; Sakurai, S.; Sanchez, D. A.; Šarić, T.; Saturni, F. G.; Scherpenberg, J.; Schleicher, B.; Schmuckermaier, F.; Schubert, J. L.; Schussler, F.; Schweizer, T.; Seglar Arroyo, M.; Sitarek, J.; Sliusar, V.; Spolon, A.; Strišković, J.; Strzys, M.; Suda, Y.; Sunada, Y.; Tajima, H.; Takahashi, M.; Takahashi, H.; Takata, J.; Takeishi, R.; Tam, P. H. T.; Tanaka, S. J.; Tateishi, D.; Temnikov, P.; Terada, Y.; Terauchi, K.; Terzic, T.; Teshima, M.; Tluczykont, M.; Tokanai, F.; Torres, D. F.; Travnicek, P.; Truzzi, S.; Tutone, A.; Uhlrich, G.; Vacula, M.; Vázquez Acosta, M.; Verguilov, V.; Viale, I.; Vigliano, A.; Vigorito, C. F.; Vitale, V.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Walter, R.; Will, M.; Yamamoto, T.; Yamazaki, R.; Yoshida, T.; Yoshikoshi, T.; Zywucka (CTA-LST Project), N.; Balbo, M.; Eckert, D.; Tramacere, A.
Astronomy and Astrophysics, May 2023, [Reviewed]
Context. Several new ultrahigh-energy (UHE) γ-ray sources have recently been discovered by the Large High Altitude Air Shower Observatory (LHAASO) collaboration. These represent a step forward in the search for the so-called Galactic PeVatrons, the enigmatic sources of the Galactic cosmic rays up to PeV energies. However, it has been shown that multi-TeV γ-ray emission does not necessarily prove the existence of a hadronic accelerator in the source; indeed this emission could also be explained as inverse Compton scattering from electrons in a radiation-dominated environment. A clear distinction between the two major emission mechanisms would only be made possible by taking into account multi-wavelength data and detailed morphology of the source.
Aims: We aim to understand the nature of the unidentified source LHAASO J2108+5157, which is one of the few known UHE sources with no very high-energy (VHE) counterpart.
Methods: We observed LHAASO J2108+5157 in the X-ray band with XMM-Newton in 2021 for a total of 3.8 hours and at TeV energies with the Large-Sized Telescope prototype (LST-1), yielding 49 hours of good-quality data. In addition, we analyzed 12 years of Fermi-LAT data, to better constrain emission of its high-energy (HE) counterpart 4FGL J2108.0+5155. We used naima and jetset software packages to examine the leptonic and hadronic scenario of the multi-wavelength emission of the source.
Results: We found an excess (3.7σ) in the LST-1 data at energies E > 3 TeV. Further analysis of the whole LST-1 energy range, assuming a point-like source, resulted in a hint (2.2σ) of hard emission, which can be described with a single power law with a photon index of Γ = 1.6 ± 0.2 the range of 0.3 − 100 TeV. We did not find any significant extended emission that could be related to a supernova remnant (SNR) or pulsar wind nebula (PWN) in the XMM-Newton data, which puts strong constraints on possible synchrotron emission of relativistic electrons. We revealed a new potential hard source in Fermi-LAT data with a significance of 4σ and a photon index of Γ = 1.9 ± 0.2, which is not spatially correlated with LHAASO J2108+5157, but including it in the source model we were able to improve spectral representation of the HE counterpart 4FGL J2108.0+5155.
Conclusions: The LST-1 and LHAASO observations can be explained as inverse Compton-dominated leptonic emission of relativistic electrons with a cutoff energy of 100−30+70 TeV. The low magnetic field in the source imposed by the X-ray upper limits on synchrotron emission is compatible with a hypothesis of a PWN or a TeV halo. Furthermore, the spectral properties of the HE counterpart are consistent with a Geminga-like pulsar, which would be able to power the VHE-UHE emission. Nevertheless, the lack of a pulsar in the neighborhood of the UHE source is a challenge to the PWN/TeV-halo scenario. The UHE γ rays can also be explained as π0 decay-dominated hadronic emission due to interaction of relativistic protons with one of the two known molecular clouds in the direction of the source. Indeed, the hard spectrum in the LST-1 band is compatible with protons escaping a shock around a middle-aged SNR because of their high low-energy cut-off, but the origin of the HE γ-ray emission remains an open question....
Scientific journal
DOI：https://doi.org/10.1051/0004-6361/202245086
DOI ID：10.1051/0004-6361/202245086, ORCID：121420405, arXiv ID：arXiv:2210.00775, Bibcode：2023A&A...673A..75A - Long‐Term Density Trend in the Mesosphere and Lower Thermosphere From Occultations of the Crab Nebula With X‐Ray Astronomy Satellites
Satoru Katsuda; Teruaki Enoto; Andrea N. Lommen; Koji Mori; Yuko Motizuki; Motoki Nakajima; Nathaniel C. Ruhl; Kosuke Sato; Gunter Stober; Makoto S. Tashiro; Yukikatsu Terada; Kent S. Wood
Journal of Geophysical Research: Space Physics, Volume：128, Number：2, Feb. 2023, [Reviewed]
We present long-term density trends of the Earth's upper atmosphere at altitudes between 71 and 116 km, based on atmospheric occultations of the Crab Nebula observed with X-ray astronomy satellites, ASCA, RXTE, Suzaku, NuSTAR, and Hitomi. The combination of the five satellites provides a time period of 28 years from 1994 to 2022. To suppress seasonal and latitudinal variations, we concentrate on the data taken in autumn (49 < doy < 111) and spring (235 < doy < 297) in the northern hemisphere with latitudes of 0°-40°. With this constraint, local times are automatically limited either around noon or midnight. We obtain four sets (two seasons × two local times) of density trends at each altitude layer. We take into account variations due to a linear trend and the 11-year solar cycle using linear regression techniques. Because we do not see significant differences among the four trends, we combine them to provide a single vertical profile of trend slopes. We find a negative density trend of roughly -5%/decade at every altitude. This is in reasonable agreement with inferences from settling rate of the upper atmosphere. In the 100-110-km altitude, we found an exceptionally high density decline of about -12%/decade. This peak may be the first observational evidence for strong cooling due to water vapor and ozone near 110 km, which was first identified in a numerical simulation by Akmaev et al. (2006, https://doi.org/10.1016/j.jastp.2006.03.008). Further observations and numerical simulations with suitable input parameters are needed to establish this feature....
American Geophysical Union (AGU), Scientific journal
DOI：https://doi.org/10.1029/2022ja030797
DOI ID：10.1029/2022ja030797, ISSN：2169-9380, eISSN：2169-9402, ORCID：168902882, arXiv ID：arXiv:2302.05335, Bibcode：2023JGRA..12830797K - Spectral break of energetic pulsar wind nebulae detected with wideband X-ray observations
Bamba, Aya; Shibata, Shinpei; Tanaka, Shuta J.; Mori, Koji; Uchida, Hiroyuki; Terada, Yukikatsu; Ishizaki, Wataru
Publications of the Astronomical Society of Japan, Oct. 2022, [Reviewed]
Pulsar wind nebulae (PWNe) are one of the most energetic galactic sources with bright emissions from radio waves to very high-energy gamma-rays. We perform wideband X-ray spectroscopy of four energetic PWNe, N 157 B, PSR J1813-1749, PSR J1400-6325, and G21.5-0.9, with the Suzaku, Chandra, NuSTAR, and Hitomi observatories. A significant spectral break or cut-off feature is found in the hard X-ray band for all the samples, except for N 157 B. The break energies in the broken power-law fitting are in the range of 4-14 keV, whereas the cut-off energies in the cut-off power-law fitting are at 22 keV or higher. The break or cut-off energy does not show a significant correlation with either the spin-down energy or characteristic age of the hosting pulsars. A possible correlation is found between the photon index change in the broken power-law fitting and the X-ray emitting efficiency of the pulsars, although its significance is not high enough to be conclusive. We discuss what determines the break parameters based on simple models....
Scientific journal
DOI：https://doi.org/10.1093/pasj/psac062
DOI ID：10.1093/pasj/psac062, ORCID：121420373, arXiv ID：arXiv:2207.10880, Bibcode：2022PASJ...74.1186B - X-ray line diagnostics of ion temperature at cosmic ray accelerating collisionless shocks
Jiro Shimoda; Yutaka Ohira; Aya Bamba; Yukikatsu Terada; Ryo Yamazaki; Tsuyoshi Inoue; Shuta J. Tanaka
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：74, Number：5, First page：1022, Last page：1040, Oct. 2022, [Reviewed]
A novel collisionless shock jump condition is suggested by modeling the entropy production at the shock transition region. We also calculate downstream developments of the atomic ionization balance and the ion temperature relaxation in supernova remnants (SNRs). The injection process and subsequent acceleration of cosmic rays (CRs) in the SNR shocks are closely related to the formation process of the collisionless shocks. The formation of the shock is caused by wave-particle interactions. Since the wave-particle interactions result in energy exchanges between electromagnetic fields and charged particles, the randomization of particles associated with the shock transition may occur at a rate given by the scalar product of the electric field and current. We find that order-of-magnitude estimates of the randomization with reasonable strength of the electromagnetic fields in the SNR constrain the amount of CR nuclei and the ion temperatures. The constrained amount of CR nuclei can be sufficient to explain the Galactic CRs. The ion temperature becomes significantly lower than that in the case without CRs. To distinguish the case without CRs, we perform synthetic observations of atomic line emissions from the downstream region of the SNR RCW 86. Future observations by XRISM and Athena can distinguish whether the SNR shock accelerates the CRs or not from the ion temperatures.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psac053
DOI ID：10.1093/pasj/psac053, ISSN：0004-6264, eISSN：2053-051X, ORCID：114720040, arXiv ID：arXiv:2201.07607, Web of Science ID：WOS:000827218100001, Bibcode：2022PASJ...74.1022S - Vibration Characteristics of a Continuously Rotating Superconducting Magnetic Bearing and Potential Influence to TES and SQUID
S. Sugiyama; T. Ghigna; Y. Hoshino; N. Katayama; S. Katsuda; K. Komatsu; T. Matsumura; Y. Sakurai; K. Sato; R. Takaku; M. Tashiro; Y. Terada
Journal of Low Temperature Physics, Volume：209, Number：5-6, First page：1088, Last page：1096, Sep. 2022, [Reviewed]
We measured the vibration of a prototype superconducting magnetic bearing (SMB) operating at liquid nitrogen temperature. This prototype system was designed as a breadboard model for LiteBIRD low-frequency telescope (LFT) polarization modulator unit. We set an upper limit of the vibration amplitude at $36~\mathrm{\mu m}$ at the rotational synchronous frequency. During the rotation, the amplitude of the magnetic field produced varies. From this setup, we compute the static and AC amplitude of the magnetic fields produced by the SMB magnet at the location of the LFT focal plane as $0.24~\mathrm{G}$ and $3\times10^{-5}$$~\mathrm{G}$, respectively. From the AC amplitude, we compute TES critical temperature variation of $7\times10^{-8}$$~\mathrm{K}$ and fractional change of the SQUID flux is $\delta \Phi/\Phi_0|_{ac}=3.1\times10^{-5}$. The mechanical vibration can be also estimated to be $3.6\times 10^{-2}$$~\mathrm{N}$ at the rotation mechanism location....
Springer Science and Business Media LLC, English, Scientific journal
DOI：https://doi.org/10.1007/s10909-022-02846-1
DOI ID：10.1007/s10909-022-02846-1, ISSN：0022-2291, eISSN：1573-7357, ORCID：121420379, arXiv ID：arXiv:2210.13219, Bibcode：2022JLTP..209.1088S - Balloon-borne narrow field of view semiconductor Compton telescope concept: miniSGD
Kazuhiro Nakazawa; Keigo Okuma; Yuna Tsuji; Shinichiro Takeda; Mii Ando; Yuki Omiya; Manari Oguchi; Atsuya Tanaka; Shin Watanabe; Tadayuki Takahashi; Mitsunobu Onishi; Toshihiko Arai; Masahiko Kobayashi; Naoki Ishida
Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray, Aug. 2022
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.2628199
DOI ID：10.1117/12.2628199 - A broadband x-ray imaging spectroscopy in the 2030s: the FORCE mission
Koji Mori; Takeshi G. Tsuru; Kazuhiro Nakazawa; Yoshihiro Ueda; Shin Watanabe; Takaaki Tanaka; Manabu Ishida; Hironori Matsumoto; Hisamitsu Awaki; Hiroshi Murakami; Masayoshi Nobukawa; Ayaki Takeda; Yasushi Fukazawa; Hiroshi Tsunemi; Tadayuki Takahashi; Ann E. Hornschemeier; Takashi Okajima; William W. Zhang; Brian J. Williams; Tonia Venters; Kristin Madsen; Mihoko Yukita; Hiroki Akamatsu; Aya Bamba; Teruaki Enoto; Yutaka Fujita; Akihiro Furuzawa; Kouichi Hagino; Kosei Ishimura; Masayuki Itoh; Tetsu Kitayama; Shogo B. Kobayashi; Takayoshi Kohmura; Aya Kubota; Misaki Mizumoto; Tsunefumi Mizuno; Hiroshi Nakajima; Kumiko K. Nobukawa; Hirofumi Noda; Hirokazu Odaka; Naomi Ota; Toshiki Sato; Megumi Shidatsu; Hiromasa Suzuki; Hiromitsu Takahashi; Atsushi Tanimoto; Yukikatsu Terada; Yuichi Terashima; Hiroyuki Uchida; Yasunobu Uchiyama; Hiroya Yamaguchi; Yoichi Yatsu
Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray, Aug. 2022
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.2628772
DOI ID：10.1117/12.2628772 - Xappl: software framework for the XRISM pre-pipeline
Satoshi Eguchi; Makoto Tashiro; Yukikatsu Terada; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Shin'ichiro Uno; Aya Kubota; Kazuhiro Nakazawa; Shin Watanabe; Ryo Iizuka; Rie Sato; Tomokage Yoneyama; Chris Baluta; Ken Ebisawa; Yasushi Fukazawa; Katsuhiro Hayashi; So Kato; Satoru Katsuda; Takao Kitaguchi; Hirokazu Odaka; Masanori Ohno; Naomi Ota; Minami Sakama; Ryohei Sato; Megumi Shidatsu; Yasuharu Sugawara; Tsubasa Tamba; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Nagomi Uchida; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Masaaki Sakano; Tessei Yoshida; Satoshi Yamada
Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray, Aug. 2022
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.2629316
DOI ID：10.1117/12.2629316 - A Spatially Resolved Study of Hard X-Ray Emission in Kepler’s Supernova Remnant: Indications of Different Regimes of Particle Acceleration
Vincenzo Sapienza; Marco Miceli; Aya Bamba; Satoru Katsuda; Tsutomu Nagayoshi; Yukikatsu Terada; Fabrizio Bocchino; Salvatore Orlando; Giovanni Peres
The Astrophysical Journal, Aug. 2022, [Reviewed]
Synchrotron X-ray emission in young supernova remnants (SNRs) is a powerful diagnostic tool to study the population of high-energy electrons accelerated at the shock front and the acceleration process. We performed a spatially resolved spectral analysis of NuSTAR and XMM-Newton observations of the young Kepler's SNR, aiming to study in detail its nonthermal emission in hard X-rays. We selected a set of regions all around the rim of the shell and extracted the corresponding spectra. The spectra were analyzed by adopting a model of synchrotron radiation in the loss-limited regime, to constrain the dependence of the cutoff energy of the synchrotron radiation on the shock velocity. We identify two different regimes of particle acceleration, characterized by different Bohm factors. In the north, where the shock interacts with a dense circumstellar medium (CSM), we found a more efficient acceleration than in the south, where the shock velocity is higher and there are no signs of shock interaction with the dense CSM. Our results suggest an enhanced efficiency of the acceleration process in regions where the shock-CSM interaction generates an amplified and turbulent magnetic field. By combining hard X-ray spectra with radio and γ-ray observations of Kepler's SNR, we modeled the spectral energy distribution. In the light of our results we propose that the observed γ-ray emission is mainly hadronic and originates in the northern part of the shell....
Scientific journal
DOI：https://doi.org/10.3847/1538-4357/ac8160
DOI ID：10.3847/1538-4357/ac8160, ORCID：117693224, arXiv ID：arXiv:2207.06804, Bibcode：2022ApJ...935..152S - Gamma-Ray Diagnostics of r-process Nucleosynthesis in the Remnants of Galactic Binary Neutron-star Mergers
Yukikatsu Terada; Yuya Miwa; Hayato Ohsumi; Shin-ichiro Fujimoto; Satoru Katsuda; Aya Bamba; Ryo Yamazaki
The Astrophysical Journal, Volume：933, Number：1, First page：111, Last page：111, Jul. 2022, [Reviewed], [Lead]
Abstract
We perform a full nuclear-network numerical calculation of the r-process nuclei in binary neutron-star mergers (NSMs), with the aim of estimating gamma-ray emissions from the remnants of Galactic NSMs up to 106 yr old. The nucleosynthesis calculation of 4070 nuclei is adopted to provide the elemental composition ratios of nuclei with an electron fraction Ye between 0.10 and 0.45. The decay processes of 3237 unstable nuclei are simulated to extract the gamma-ray spectra. As a result, the NSMs have different spectral colors in the gamma-ray band from various other astronomical objects at less than 105 yr old. In addition, we propose a new line diagnostic method for Ye that uses the line ratios of either 137mBa/85K or 243Am/60mCo, which become larger than unity for young and old r-process sites, respectively, with a low-Ye environment. From an estimation of the distance limit for gamma-ray observations as a function of age, the high sensitivity in the sub-megaelectronvolt band, at approximately 10−9 photons s−1 cm−2 or 10−15 erg s−1 cm−2, is required to cover all the NSM remnants in our Galaxy, if we assume that the population of NSMs by Wu et al. A gamma-ray survey with sensitivities of 10−8–10−7 photons s−1 cm−2 or 10−14–10−13 erg s−1 cm−2 in the 70–4000 keV band is expected to find emissions from at least one NSM remnant under the assumption of an NSM rate of 30 Myr−1. The feasibility of gamma-ray missions observing Galactic NSMs is also studied.
American Astronomical Society, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/ac721f
DOI ID：10.3847/1538-4357/ac721f, ISSN：0004-637X, eISSN：1538-4357, ORCID：114720000, arXiv ID：arXiv:2205.05407, Bibcode：2022ApJ...933..111T - NuSTAR discovery of the hard X-ray emission and a wide-band X-ray spectrum from the Pictor A western hotspot
Yuji Sunada; Arisa Morimoto; Makoto S Tashiro; Yukikatsu Terada; Satoru Katsuda; Kosuke Sato; Dai Tateishi; Nobuaki Sasaki
Publications of the Astronomical Society of Japan, Jun. 2022, [Reviewed]
Utilizing Chandra, XMM-Newton, and NuSTAR, a wide-band X-ray spectrum from 0.2 to 20 keV is reported from the western hotspot of Pictor A. In particular, the X-ray emission is significantly detected in the 3 to 20 keV band at 30σ by NuSTAR. This is the first detection of hard X-rays with energies above 10 keV from a jet termination hotspot of active galactic nuclei. The hard X-ray spectrum is well described with a power-law model with a photon index of Γ = 1.8 ± 0.2, and the flux is obtained to be (4.5 ± 0.4) × 10-13 erg s-1 cm-2 in the 3 to 20 keV band. The obtained spectrum is smoothly connected with those soft X-ray spectra observed by Chandra and XMM-Newton. The wide-band spectrum shows a single power-law spectrum with a photon index of Γ = 2.07 ± 0.03, excluding any cut-off/break features. Assuming the X-rays to be synchrotron radiation of the electrons, the energy index of the electrons is estimated as p = 2Γ - 1 = 3.14 ± 0.06 from the wide-band spectrum. Given that the X-ray synchrotron-emitting electrons quickly lose their initial energies via synchrotron radiation, the energy index of electrons at acceleration sites is estimated as pacc = p - 1 = 2.14 ± 0.06. This is consistent with the prediction of the diffusive shock acceleration. Since the spectrum has no cut-off feature up to 20 keV, the maximum electron energy is estimated to be no less than 40 TeV....
Oxford University Press ({OUP}), English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psac022
DOI ID：10.1093/pasj/psac022, ORCID：112970970, arXiv ID：arXiv:2203.02066, Bibcode：2022PASJ...74..602S - VizieR Online Data Catalog: 2nd cat. of IPN localizations of Konus short GRBs (Svinkin+, 2022)
Svinkin, D. S.; Hurley, K.; Ridnaia, A. V.; Lysenko, A. L.; Frederiks, D. D.; Golenetskii, S. V.; Tsvetkova, A. E.; Ulanov, M. V.; Kokomov, A.; Cline, T. L.; Mitrofanov, I.; Golovin, D.; Kozyrev, A.; Litvak, M.; Sanin, A.; Goldstein, A.; Briggs, M. S.; Wilson-Hodge, C.; Burns, E.; von Kienlin, A.; Zhang, X. -L.; Rau, A.; Savchenko, V.; Bozzo, E.; Ferrigno, C.; Barthelmy, S.; Cummings, J.; Krimm, H.; Palmer, D. M.; Tohuvavohu, A.; Yamaoka, K.; Ohno, M.; Fukazawa, Y.; Hanabata, Y.; Takahashi, T.; Tashiro, M.; Terada, Y.; Murakami, T.; Makishima, K.; Boynton, W.; Fellows, C. W.; Harshman, K. P.; Enos, H.; Starr, R.; Goldsten, J.; Gold, R.; Ursi, A.; Tavani, M.; Bulgarelli, A.; Casentini, C.; Del, Monte E.; Evangelista, Y.; Galli, M.; Longo, F.; Marisaldi, M.; Parmiggiani, N.; Pittori, C.; Romani, M.; Verrecchia, F.; Smith, D. M.; Hajdas, W.; Xiao, S.; Cai, C.; Yi, Q. B.; Zhang, Y. Q.; Xiong, S. L.; Li, X. B.; Huang, Y.; Li, C. K.; Zhang, S. N.; Song, L. M.; Liu, C. Z.; Li, X. Q.; Peng, W. X.; Martinez-Castellanos, I.
VizieR Online Data Catalog, Jun. 2022
During the period covered in the present catalog (2011-2021), the InterPlanetary Network (IPN) contained between seven and nine missions: the Konus-Wind (KW), in orbit around the Lagrangian point L1; Mars Odyssey (a gamma-ray spectrometer, GRS, that includes the High-Energy Neutron Detector, HEND, with GRB detection capabilities, Hurley+ 2006ApJS..164..124H), in orbit around Mars; the Mercury Surface, Space Environment, Geochemistry, and Ranging mission (MESSENGER); the Gamma-Ray and Neutron Spectrometer (GRNS; Gold+ 2001P&SS...49.1467G), in an eccentric orbit around Mercury; the International Gamma-Ray Laboratory (INTEGRAL; the anticoincidence shield of the spectrometer SPI (SPI-ACS), in an eccentric Earth orbit; Rau+ 2005, J/A+A/438/1175); RHESSI and the array of germanium detectors (GeD; Smith+ 2002SoPh..210...33S); the Neil Gehrels Swift Observatory (the Burst Alert Telescope, BAT); the Fermi Gamma-ray Space Telescope's Gamma-Ray Burst Monitor (GBM); the Suzaku mission (the Wide-band All-sky Monitor, WAM); the Astro-rivelatore Gamma a Immagini LEggero mission (AGILE); the Mini-Calorimeter (MCAL; Tavani+ 2009A&A...502..995T); the CALorimetric Electron Telescope on board the International Space Station (CALET); the Gamma-ray Burst Monitor; the Hard X-ray Modulation Telescope (Insight-HXMT; the High-energy X-ray Telescope, HE); and the Gravitational Wave High-energy Electromagnetic Counterpart All-sky Monitor (GECAM; gamma-ray detectors, GRDs; GECAM consists of two microsatellites, GECAM-A and GECAM-B, but currently only GECAM-B is in operation): all in low-Earth orbit. See Section 2. (3 data files)....
Scientific journal
DOI：https://doi.org/10.26093/cds/vizier.22590034
DOI ID：10.26093/cds/vizier.22590034, ORCID：181064294, Bibcode：2022yCat..22590034S - Simulation-based spectral analysis of X-ray CCD data affected by photon pile-up
Tsubasa Tamba; Hirokazu Odaka; Aya Bamba; Hiroshi Murakami; Koji Mori; Kiyoshi Hayashida; Yukikatsu Terada; Tsunefumi Mizuno; Masayoshi Nobukawa
Publications of the Astronomical Society of Japan, Volume：74, Number：2, First page：364, Last page：383, Apr. 2022, [Reviewed]
Abstract
We have developed a simulation-based method of spectral analysis for pile-up-affected data of X-ray CCDs without any loss of photon statistics. As effects of the photon pile-up appear as complicated nonlinear detector responses, we employ a detailed simulation to calculate the important processes in an X-ray observation including physical interactions, detector signal generation, detector readout, and a series of data reduction processes. This simulation naturally reproduces X-ray-like and background-like events as results of X-ray photon merging in a single pixel or in a chunk of adjacent pixels, allowing us to construct a nonlinear spectral analysis framework that can treat pile-up-affected observation data. For validation, we have performed data analysis of Suzaku X-ray Imaging Spectrometer (XIS) observations using this framework with various parameters of the detector simulation, all of which are optimized for that instrument. We present three cases of different pile-up degrees: PKS 2155−304 (negligible pile-up), Aquila X-1 (moderate pile-up), and the Crab Nebula (strong pile-up); we show that the nonlinear analysis method produces results consistent with a conventional linear analysis for the negligible pile-up condition, and accurately corrects well-known pile-up effects such as spectral hardening and flux decrease for the pile-up cases. These corrected results are consistent with those obtained by a widely used core-exclusion method or by other observatories with much higher timing resolutions (without pile-up). Our framework is applicable to any types of CCDs used for X-ray astronomy, including future missions such as X-ray Imaging and Spectroscopy Mission (XRISM), by appropriate optimization of the simulation parameters.
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psab131
DOI ID：10.1093/pasj/psab131, ISSN：0004-6264, eISSN：2053-051X, ORCID：114719998, arXiv ID：arXiv:2112.14176, Bibcode：2022PASJ...74..364T - The Second Catalog of Interplanetary Network Localizations of Konus Short-duration Gamma-Ray Bursts
Svinkin, D. S.; Hurley, K.; Ridnaia, A. V.; Lysenko, A. L.; Frederiks, D. D.; Golenetskii, S. V.; Tsvetkova, A. E.; Ulanov, M. V.; Kokomov, A.; Cline, T. L.; Mitrofanov, I.; Golovin, D.; Kozyrev, A.; Litvak, M.; Sanin, A.; Goldstein, A.; Briggs, M. S.; Wilson-Hodge, C.; Burns, E.; von Kienlin, A.; Zhang, X. -L.; Rau, A.; Savchenko, V.; Bozzo, E.; Ferrigno, C.; Barthelmy, S.; Cummings, J.; Krimm, H.; Palmer, D. M.; Tohuvavohu, A.; Yamaoka, K.; Ohno, M.; Fukazawa, Y.; Hanabata, Y.; Takahashi, T.; Tashiro, M.; Terada, Y.; Murakami, T.; Makishima, K.; Boynton, W.; Fellows, C. W.; Harshman, K. P.; Enos, H.; Starr, R.; Goldsten, J.; Gold, R.; Ursi, A.; Tavani, M.; Bulgarelli, A.; Casentini, C.; Del Monte, E.; Evangelista, Y.; Galli, M.; Longo, F.; Marisaldi, M.; Parmiggiani, N.; Pittori, C.; Romani, M.; Verrecchia, F.; Smith, D. M.; Hajdas, W.; Xiao, S.; Cai, C.; Yi, Q. B.; Zhang, Y. Q.; Xiong, S. L.; Li, X. B.; Huang, Y.; Li, C. K.; Zhang, S. N.; Song, L. M.; Liu, C. Z.; Li, X. Q.; Peng, W. X.; Martinez-Castellanos, I.
The Astrophysical Journal Supplement Series, Apr. 2022, [Reviewed]
We present the catalog of InterPlanetary Network (IPN) localizations for 199 short-duration gamma-ray bursts (sGRBs) detected by the Konus-Wind (KW) experiment between 2011 January 1 and 2021 August 31, which extends the initial sample of IPN-localized KW sGRBs to 495 events. We present the most comprehensive IPN localization data on these events, including probability sky maps in Hierarchical Equal Area isoLatitude Pixelization format....
Scientific journal
DOI：https://doi.org/10.3847/1538-4365/ac4607
DOI ID：10.3847/1538-4365/ac4607, ORCID：114720003, arXiv ID：arXiv:2203.08738, Bibcode：2022ApJS..259...34S - Possible Detection of X-Ray Emitting Circumstellar Material in the Synchrotron-dominated Supernova Remnant RX J1713.7-3946
Tateishi, Dai; Katsuda, Satoru; Terada, Yukikatsu; Acero, Fabio; Yoshida, Takashi; Fujimoto, Shin-ichiro; Sano, Hidetoshi
The Astrophysical Journal, Dec. 2021, [Reviewed]
We report on a discovery of an X-ray emitting circumstellar material knot inside the synchrotron dominant supernova remnant (SNR) RX J1713.7-3946. This knot was previously thought to be a Wolf-Rayet star (WR 85), but we realized that it is in fact $\sim$40$^{\prime\prime}$ away from WR 85, indicating no relation to WR 85. We performed high-resolution X-ray spectroscopy with the Reflection Grating Spectrometer (RGS) on board XMM-Newton. The RGS spectrum clearly resolves a number of emission lines, such as N Ly$\alpha$, O Ly$\alpha$, Fe XVIII, Ne X, Mg XI, and Si XIII. The spectrum can be well represented by an absorbed thermal emission model with a temperature of $k_{\rm B}T_{\rm e} = 0.65\pm 0.02$ keV. The elemental abundances are obtained to be ${\rm N/H} = 3.5\pm 0.8{\rm \left(N/H\right)_{\odot } }$, ${\rm O/H} = 0.5\pm0.1{\rm \left(O/H\right)_{\odot } }$, ${\rm Ne/H} = 0.9\pm0.1{\rm \left(Ne/H\right)_{\odot } }$, ${\rm Mg/H} = 1.0\pm0.1{\rm \left(Mg/H\right)_{\odot } }$, ${\rm Si/H} = 1.0\pm0.2{\rm \left(Si/H\right)_{\odot } }$, and ${\rm Fe/H} = 1.3\pm0.1{\rm \left(Fe/H\right)_{\odot } }$. The enhanced N abundance with others being about the solar values allows us to infer that this knot is circumstellar material ejected when the progenitor star evolved into a red supergiant. The abundance ratio of N to O is obtained to be $\rm N/O = 6.8_{-2.1}^{+2.5}\left(N/O\right)_{\odot}$. By comparing this to those in outer layers of red supergiant stars expected from stellar evolution simulations, we estimate the initial mass of the progenitor star to be $15\, \rm M_{\odot} \lesssim \rm M \lesssim 20\, \rm M_{\odot}$....
arXiv e-prints, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/ac2c00
DOI ID：10.3847/1538-4357/ac2c00, ORCID：101133486, arXiv ID：arXiv:2110.01560, Bibcode：2021ApJ...923..187T - IACHEC 2020/2021 Pandemic Report
Madsen, K. K.; Burwitz, V.; Forster, K.; Grant, C. E.; Guainazzi, M.; Kashyap, V.; Marshall, H. L.; Miller, E. D.; Natalucci, L.; Plucinsky, P. P.; Terada, Y.
Nov. 2021
In this report we summarize the activities of the International Astronomical Consortium for High Energy Calibration (IACHEC) and the work done since the last in-person meeting in Japan (Shonan Village Center), May 2019, through two virtual meetings that were held in November 2020 and May 2021. The on-line only meetings divided the contents of the usual in-person workshop between mission updates and working group updates. The November meeting was dedicated to mission calibration updates and the current status of the cross-calibration between NuSTAR, Swift, and NICER, which frequently join together in observations of bright transients, and a review of the XMM-Newton and Chandra cross-calibration. Results between \nustar\ and \swift\ overall show good agreement, but issues persist in the overlap region 3--5 keV for bright source with large dust scattering halos. The NICER cross-calibration is still progressing and evolving, while for the XMM-Newton and Chandra cross-calibration systematic differences both in the absolute flux and spectral shape determination still exists on different classes of sources. The meeting in May was focused on the Working Group progress and reports summarized here....
arXiv e-prints
ORCID：114720047, arXiv ID：arXiv:2111.01613, Bibcode：2021arXiv211101613M - Detailed design of the science operations for the XRISM mission
Yukikatsu Terada; Matt Holland; Michael Loewenstein; Makoto Tashiro; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Takayuki Tamura; Shin’ichiro Uno; Shin Watanabe; Chris Baluta; Laura Burns; Ken Ebisawa; Satoshi Eguchi; Yasushi Fukazawa; Katsuhiro Hayashi; Ryo Iizuka; Satoru Katsuda; Takao Kitaguchi; Aya Kubota; Eric Miller; Koji Mukai; Shinya Nakashima; Kazuhiro Nakazawa; Hirokazu Odaka; Masanori Ohno; Naomi Ota; Rie Sato; Makoto Sawada; Yasuharu Sugawara; Megumi Shidatsu; Tsubasa Tamba; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tahir Yaqoob
Journal of Astronomical Telescopes, Instruments, and Systems, Volume：7, Number：03, Jul. 2021, [Reviewed], [Lead]
SPIE-Intl Soc Optical Eng, Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.7.3.037001
DOI ID：10.1117/1.JATIS.7.3.037001, ISSN：2329-4124, ORCID：101088758 - Detection of the hard X-ray non-thermal emission from Kepler’s supernova remnant
Tsutomu Nagayoshi; Aya Bamba; Satoru Katsuda; Yukikatsu Terada
Publications of the Astronomical Society of Japan, Apr. 2021, [Reviewed]
Oxford University Press ({OUP}), Scientific journal
DOI：https://doi.org/10.1093/pasj/psaa121
DOI ID：10.1093/pasj/psaa121, ORCID：88186843 - New Measurement of the Vertical Atmospheric Density Profile From Occultations of the Crab Nebula With X‐Ray Astronomy Satellites Suzaku and Hitomi
Satoru Katsuda; Hitoshi Fujiwara; Yoshitaka Ishisaki; Maeda Yoshitomo; Koji Mori; Yuko Motizuki; Kosuke Sato; Makoto S. Tashiro; Yukikatsu Terada
Journal of Geophysical Research: Space Physics, Volume：126, Number：4, Apr. 2021, [Reviewed]
American Geophysical Union (AGU), Scientific journal
DOI：https://doi.org/10.1029/2020ja028886
DOI ID：10.1029/2020ja028886, ISSN：2169-9380, eISSN：2169-9402, ORCID：91119041 - Calibration and performance of the readout system based on switched capacitor arrays for the Large-Sized Telescope of the Cherenkov Telescope Array
Seiya Nozaki; Kyosuke Awai; Aya Bamba; Juan Abel Barrio; Maria Isabel Bernardos; Oscar Blanch; Joan Boix; Franca Cassol; Yuuki Choushi; Carlos Delgado; Carlos Diaz; Nadia Fouque; Lluis Freixas; Pawel Gliwny; Shuichi Gunji; Daniela Hadasch; Dirk Hoffmann; Julien Houles; Yusuke Inome; Yuki Iwamura; Lea Jouvin; Hideaki Katagiri; Kiomei Kawamura; Daniel Kerszberg; Yusuke Konno; Hidetoshi Kubo; Junko Kushida; Yukiho Kobayashi; Ruben Lopez; Gustavo Martinez; Shu Masuda; Daniel Mazin; Abelardo Moralejo; Elena Moretti; Tsutomu Nagayoshi; Takeshi Nakamori; Kyoshi Nishijima; Yuto Nogami; Leyre Nogués; Hideyuki Ohoka; Tomohiko Oka; Nao Okazaki; Akira Okumura; Reiko Orito; Jean-Luc Panazol; Riccardo Paoletti; Cristobal Pio; Miguel Polo; Julie Prast; Takayuki Saito; Shunsuke Sakurai; Julian Sitarek; Yuji Sunada; Megumi Suzuki; Mitsunari Takahashi; Kenji Tamura; Manobu Tanaka; Luis Angel Tejedor; Yukikatsu Terada; Masahiro Teshima; Yusuke Tsukamoto; Tokonatsu Yamamoto
Ground-based and Airborne Instrumentation for Astronomy VIII, First page：114470H, Dec. 2020
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.2560018
DOI ID：10.1117/12.2560018 - Planning in-flight calibration for XRISM
Eric D. Miller; Makoto Sawada; Matteo Guainazzi; Aurora Simionescu; Maxim Markevitch; Liyi Gu; Megan E. Eckart; Caroline A. Kilbourne; Maurice A. Leutenegger; Frederick S. Porter; Masahiro Tsujimoto; Cor P. de Vries; Takashi Okajima; Takayuki Hayashi; Rozenn Boissay-Malaquin; Keisuke Tamura; Hironori Matsumoto; Koji Mori; Hiroshi Nakajima; Takaaki Tanaka; Yukikatsu Terada; Michael Loewenstein; Tahir Yaqoob; Marc Audard; Ehud Behar; Laura Brenneman; Lia Corrales; Renata S. Cumbee; Teruaki Enoto; Edmund Hodges-Kluck; Yoshitomo Maeda; Paul P. Plucinsky; Katja Pottschmidt; Makoto S. Tashiro; Richard L. Kelley; Robert Petre; Brian J. Williams; Hiroya Yamaguchi
Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, Dec. 2020
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.2561608
DOI ID：10.1117/12.2561608 - Status of x-ray imaging and spectroscopy mission (XRISM)
Makoto S. Tashiro; Hironori Maejima; Kenichi Toda; Richard L. Kelley; Lillian Reichenthal; Leslie Hartz; Robert Petre; Brian J. Williams; Matteo Guainazzi; Elisa Costantini; Ryuichi Fujimoto; Kiyoshi Hayashida; Joy Henegar-Leon; Matt Holland; Yoshitaka Ishisaki; Caroline Kilbourne; Mike Loewenstein; Kyoko Matsushita; Koji Mori; Takashi Okajima; F. Scott Porter; Gary Sneiderman; Yoh Takei; Yukikatsu Terada; Hiroshi Tomida; Hiroya Yamaguchi; Shin Watanabe; Hiroki Akamatsu; Yoshitaka Arai; Marc Audard; Hisamitsu Awaki; Iurii Babyk; Aya Bamba; Nobutaka Bando; Ehud Behar; Thomas Bialas; Rozenn Boissay-Malaquin; Laura Brenneman; Greg Brown; Edgar Canavan; Meng Chiao; Brian Comber; Lia Corrales; Renata Cumbee; Cor de Vries; Jan-Willem den Herder; Johannes Dercksen; Maria Diaz-Trigo; Michael DiPirro; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan Eckart; Dominique Eckert; Satoshi Eguchi; Teruaki Enoto; Yuichiro Ezoe; Carlo Ferrigno; Yutaka Fujita; Yasushi Fukazawa; Akihiro Furuzawa; Luigi Gallo; Nathalie Gorter; Martin Grim; Liyi Gu; Kouichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; David Hawthorn; Katsuhiro Hayashi; Natalie Hell; Junko Hiraga; Edmund Hodges-Kluck; Takafumi Horiuchi; Ann Hornschemeier; Akio Hoshino; Yuto Ichinohe; Sayuri Iga; Ryo Iizuka; Manabu Ishida; Naoki Ishihama; Kumi Ishikawa; Kosei Ishimura; Tess Jaffe; Jelle Kaastra; Timothy Kallman; Erin Kara; Satoru Katsuda; Steven Kenyon; Mark Kimball; Takao Kitaguti; Shunji Kitamoto; Shogo Kobayashi; Akihide Kobayashi; Takayoshi Kohmura; Aya Kubota; Maurice Leutenegger; Muzi Li; Tom Lockard; Yoshitomo Maeda; Maxim Markevitch; Connor Martz; Hironori Matsumoto; Keiichi Matsuzaki; Dan McCammon; Brian McLaughlin; Brian McNamara; Joseph Miko; Eric Miller; Jon Miller; Kenji Minesugi; Shinji Mitani; Ikuyuki Mitsuishi; Misaki Mizumoto; Tsunefumi Mizuno; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Hiroshi Nakajima; Hideto Nakamura; Kazuhiro Nakazawa; Chikara Natsukari; Kenichiro Nigo; Yusuke Nishioka; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Mina Ogawa; Takaya Ohashi; Masahiro Ohno; Masayuki Ohta; Atsushi Okamoto; Naomi Ota; Masanobu Ozaki; Stephane Paltani; Paul Plucinsky; Katja Pottschmidt; Michael Sampson; Takahiro Sasaki; Kosuke Sato; Rie Sato; Toshiki Sato; Makoto Sawada; Hiromi Seta; Yasuko Shibano; Maki Shida; Megumi Shidatsu; Shuhei Shigeto; Keisuke Shinozaki; Peter Shirron; Aurora Simionescu; Randall Smith; Kazunori Someya; Yang Soong; Keisuke Sugawara; Yasuharu Sugawara; Andy Szymkowiak; Hiromitsu Takahashi; Toshiaki Takeshima; Toru Tamagawa; Keisuke Tamura; Takaaki Tanaka; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Tsuru; Hiroyuki Uchida; Yuusuke Uchida; Hideki Uchiyama; Yoshihiro Ueda; Shinichiro Uno; Jacco Vink; Tomomi Watanabe; Michael Wittheof; Rob Wolfs; Shinya Yamada; Kazutaka Yamaoka; Noriko Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Keiichi Yanagase; Tahir Yaqoob; Susumu Yasuda; Tessei Yoshida; Nasa Yoshioka; Irina Zhuravleva
Space Telescopes and Instrumentation 2020: Ultraviolet to Gamma Ray, Dec. 2020
SPIE, International conference proceedings
DOI：https://doi.org/10.1117/12.2565812
DOI ID：10.1117/12.2565812 - Low X-ray Efficiency of a Young High-B Pulsar PSR J1208-6238 Observed with Chandra
Bamba, Aya; Watanabe, Eri; Mori, Koji; Shibata, Shinpei; Terada, Yukikatsu; Sano, Hidetoshi; Filipovic, Miroslav D.
Astrophysics and Space Science, Volume：365, Number：11, Nov. 2020, [Reviewed]
Springer Science and Business Media LLC, Scientific journal
DOI：https://doi.org/10.1007/S10509-020-03891-6
DOI ID：10.1007/S10509-020-03891-6, ISSN：0004-640X, eISSN：1572-946X, ORCID：101088814, Web of Science ID：WOS:000590263600001 - Discovery of a hot, transiting, Earth-sized planet and a second temperate, non-transiting planet around the M4 dwarf GJ 3473 (TOI-488)
Kemmer, J.; Stock, S.; Kossakowski, D.; Kaminski, A.; Molaverdikhani, K.; Schlecker, M.; Caballero, J. A.; Amado, P. J.; Astudillo-Defru, N.; Bonfils, X.; Ciardi, D.; Collins, K. A.; Espinoza, N.; Fukui, A.; Hirano, T.; Jenkins, J. M.; Latham, D. W.; Matthews, E. C.; Narita, N.; Pallé, E.; Parviainen, H.; Quirrenbach, A.; Reiners, A.; Ribas, I.; Ricker, G.; Schlieder, J. E.; Seager, S.; Vanderspek, R.; Winn, J. N.; Almenara, J. M.; Béjar, V. J. S.; Bluhm, P.; Bouchy, F.; Boyd, P.; Christiansen, J. L.; Cifuentes, C.; Cloutier, R.; Collins, K. I.; Cortés-Contreras, M.; Crossfield, I. J. M.; Crouzet, N.; de Leon, J. P.; Della-Rose, D. D.; Delfosse, X.; Dreizler, S.; Esparza-Borges, E.; Essack, Z.; Forveille, Th.; Figueira, P.; Galadí-Enríquez, D.; Gan, T.; Glidden, A.; Gonzales, E. J.; Guerra, P.; Harakawa, H.; Hatzes, A. P.; Henning, Th.; Herrero, E.; Hodapp, K.; Hori, Y.; Howell, S. B.; Ikoma, M.; Isogai, K.; Jeffers, S. V.; Kürster, M.; Kawauchi, K.; Kimura, T.; Klagyivik, P.; Kotani, T.; Kurokawa, T.; Kusakabe, N.; Kuzuhara, M.; Lafarga, M.; Livingston, J. H.; Luque, R.; Matson, R.; Morales, J. C.; Mori, M.; Muirhead, P. S.; Murgas, F.; Nishikawa, J.; Nishiumi, T.; Omiya, M.; Reffert, S.; Rodríguez López, C.; Santos, N. C.; Schöfer, P.; Schwarz, R. P.; Shiao, B.; Tamura, M.; Terada, Y.; Twicken, J. D.; Ueda, A.; Vievard, S.; Watanabe, N.; Zechmeister, M.
Astronomy and Astrophysics, Volume：642, Oct. 2020, [Reviewed]
We present the confirmation and characterisation of GJ 3473 b (G 50-16, TOI-488.01), a hot Earth-sized planet orbiting an M4 dwarf star, whose transiting signal (P = 1.1980035 ± 0.0000018 d) was first detected by the Transiting Exoplanet Survey Satellite (TESS). Through a joint modelling of follow-up radial velocity observations with CARMENES, IRD, and HARPS together with extensive ground-based photometric follow-up observations with LCOGT, MuSCAT, and MuSCAT2, we determined a precise planetary mass, Mb = 1.86 ± 0.30 M⊕, and radius, Rb = 1.264 ± 0.050 R⊕. Additionally, we report the discovery of a second, temperate, non-transiting planet in the system, GJ 3473 c, which has a minimum mass, Mc sin i = 7.41 ± 0.91 M⊕, and orbital period, Pc = 15.509 ± 0.033 d. The inner planet of the system, GJ 3473 b, is one of the hottest transiting Earth-sized planets known thus far, accompanied by a dynamical mass measurement, which makes it a particularly attractive target for thermal emission spectroscopy. RV data are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/cat/J/A+A/642/A236...
EDP SCIENCES S A, English, Scientific journal
DOI：https://doi.org/10.1051/0004-6361/202038967
DOI ID：10.1051/0004-6361/202038967, ISSN：0004-6361, eISSN：1432-0746, ORCID：101133499, arXiv ID：arXiv:2009.10432, Web of Science ID：WOS:000586587400006, Bibcode：2020A&A...642A.236K - Inverse First Ionization Potential Effects in Giant Solar Flares Found from Earth X-Ray Albedo with Suzaku/XIS
Satoru Katsuda; Masanori Ohno; Koji Mori; Tatsuhiko Beppu; Yoshiaki Kanemaru; Makoto S. Tashiro; Yukikatsu Terada; Kosuke Sato; Kae Morita; Hikari Sagara; Futa Ogawa; Haruya Takahashi; Hiroshi Murakami; Masayoshi Nobukawa; Hiroshi Tsunemi; Kiyoshi Hayashida; Hironori Matsumoto; Hirofumi Noda; Hiroshi Nakajima; Yuichiro Ezoe; Yohko Tsuboi; Yoshitomo Maeda; Takaaki Yokoyama; Noriyuki Narukage
The Astrophysical Journal, Volume：891, Number：2, First page：126, Last page：126, Mar. 2020, [Reviewed]
American Astronomical Society, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/ab7207
DOI ID：10.3847/1538-4357/ab7207, eISSN：1538-4357, ORCID：70510147 - Systematic Study of the Peak Energy of Broadband Gamma-Ray Burst Spectra
Katsukura, Daisuke; Sakamoto, Takanori; Tashiro, Makoto S.; Terada, Yukikatsu
The Astrophysical Journal, Feb. 2020, [Reviewed]
We have performed a systematic study of gamma-ray bursts (GRBs), which have various values in the peak energy of the νFν spectrum of prompt emission, Epeak, observed by the Swift/Burst Alert Telescope (BAT) and Fermi/Gamma-ray Burst Monitor, investigating their prompt and X-ray afterglow emissions. We cataloged long-lasting GRBs observed by Swift between 2004 December and 2014 February in three categories according to the classification by Sakamoto et al.: X-ray flashes (XRFs), X-ray-rich GRBs (XRRs), and classical GRBs (C-GRBs). We then derived ${E}_{\mathrm{peak } }^{\mathrm{obs } }$ , as well as ${E}_{\mathrm{peak } }^{\mathrm{src } }$ if viable, of the Swift spectra of their prompt emission. We also analyzed their X-ray afterglows and found that GRB events with a lower ${E}_{\mathrm{peak } }^{\mathrm{src } }$ , I.e., softer GRBs, are fainter in 0.3-10 keV X-ray luminosity and decay more slowly than harder GRBs. The intrinsic event rates of the XRFs, XRRs, and C-GRBs were calculated using the Swift/BAT trigger algorithm. Those of the XRRs and XRFs are larger than that of the C-GRBs. If we assume that the observational diversity of Epeak is explained using the off-axis model, these results yield a jet half-opening angle of Δθ ∼ 0°3, and a variance of the observing angles θobs ≲ 0°6. This implies that this tiny variance would be responsible for the Epeak diversity observed by Swift/BAT, which is unrealistic. Therefore, we conclude that the Epeak diversity is not explained with the off-axis model, but is likely to originate from some intrinsic properties of the jets....
Scientific journal
DOI：https://doi.org/10.3847/1538-4357/ab6167
DOI ID：10.3847/1538-4357/ab6167, ORCID：101133500, arXiv ID：arXiv:1912.03902, Bibcode：2020ApJ...889..110K - A wide-band X-ray observatory FORCE: Current status of science study and mission proposal
Nakazawa K.; Mori K.; Tsuru T. G.; Ueda Y.; Ishida M.; Matsumoto H.; Awaki H.; Murakami H.; Terada Y.; Kubota A.; Bamba A.; Odaka H.; Yatsu Y.; Kohmura T.; Hagino K.; Kobayashi S. B.; Uchiyama Y.; Kitayama T.; Takahashi T.; Watanabe S.; Iizuka R.; Yamaguchi H.; Ohashi T.; Nakajima M.; Furuzawa A.; Tanaka T.; Uchida H.; Noda H.; Tsunemi H.; Ito M.; Nobukawa M.; Nobukawa K.; Ota N.; Terashima Y.; Fukazawa Y.; Mizuno T.; Takahashi H.; Ohno M.; Takeda A.; Hornschemeier A. E.; Okajima T.; Zhang W. W.; Williams B. J.; the FORCE team
Meeting Abstracts of the Physical Society of Japan, Volume：75.1, First page：523, Last page：523, 2020
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.75.1.0_523
DOI ID：10.11316/jpsgaiyo.75.1.0_523, eISSN：2189-0803, CiNii Articles ID：130008157369 - Origin of the in-orbit instrumental background of the Hard X-ray Imager onboard Hitomi
Hagino, Kouichi; Odaka, Hirokazu; Sato, Goro; Sato, Tamotsu; Suzuki, Hiromasa; Mizuno, Tsunefumi; Kawaharada, Madoka; Ohno, Masanori; Nakazawa, Kazuhiro; Kobayashi, Shogo B.; Murakami, Hiroaki; Miyake, Katsuma; Asai, Makoto; Koi, Tatsumi; Madejski, Greg; Saito, Shinya; Wright, Dennis H.; Enoto, Teruaki; Fukazawa, Yasushi; Hayashi, Katsuhiro; Kataoka, Jun; Katsuta, Junichiro; Kokubun, Motohide; Laurent, Philippe; Lebrun, Francois; Limousin, Olivier; Maier, Daniel; Makishima, Kazuo; Mori, Kunishiro; Nakamori, Takeshi; Nakano, Toshio; Noda, Hirofumi; Ohta, Masayuki; Sato, Rie; Tajima, Hiroyasu; Takahashi, Hiromitsu; Takahashi, Tadayuki; Takeda, Shin'ichiro; Tanaka, Takaaki; Terada, Yukikatsu; Uchiyama, Hideki; Uchiyama, Yasunobu; Watanabe, Shin; Yamaoka, Kazutaka; Yatsu, Yoichi; Yuasa, Takayuki
Journal of Astronomical Telescopes, Instruments, and Systems, Volume：6, Number：4, 2020
Understanding and reducing in-orbit instrumental backgrounds are essential to achieving high sensitivity in hard x-ray astronomical observations. The observational data of the Hard X-ray Imager (HXI) onboard the Hitomi satellite provide useful information on the background components due to its multilayer configuration with different atomic numbers: the HXI consists of a stack of four layers of Si (Z = 14) detectors and one layer of cadmium telluride (CdTe) (Z = 48, 52) detector surrounded by well-type Bi4Ge3O12 active shields. Based on the observational data, the backgrounds of the top Si layer, the three underlying Si layers, and the CdTe layer are inferred to be dominated by different components, namely, low-energy electrons, albedo neutrons, and proton-induced radioactivation, respectively. Monte Carlo simulations of the in-orbit background of the HXI reproduce the observed background spectrum of each layer well, thereby quantitatively verifying the above hypothesis. In addition, we suggest the inclusion of an electron shield to reduce the background....
Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.6.4.046003
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85098732976&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85098732976&origin=inward
DOI ID：10.1117/1.JATIS.6.4.046003, ISSN：2329-4124, eISSN：2329-4221, ORCID：101088816, arXiv ID：arXiv:2011.10317, SCOPUS ID：85098732976, Web of Science ID：WOS:000605111500021, Bibcode：2020JATIS...6d6003H - Summary of the 14th IACHEC Meeting
Madsen, K. K.; Terada, Y.; Burwitz, V.; Belanger, G.; Grant, C. E.; Guainazzi, M.; Kashyap, V.; Marshall, H. L.; Miller, E. D.; Natalucci, L.; Plucinsky, P. P.
Jan. 2020
We summarize the 14th meeting of the International Astronomical Consortium for High Energy Calibration (IACHEC) held at \textit{Shonan Village} (Kanagawa, Japan) in May 2019. Sixty scientists directly involved in the calibration of operational and future high-energy missions gathered during 3.5 days to discuss the status of the cross-calibration between the current international complement of X-ray observatories, and the possibilities to improve it. This summary consists of reports from the various WGs with topics ranging from the identification and characterization of standard calibration sources, multi-observatory cross-calibration campaigns, appropriate and new statistical techniques, calibration of instruments and characterization of background, communication and preservation of knowledge, and results for the benefit of the astronomical community....
arXiv e-prints
ORCID：101133501, arXiv ID：arXiv:2001.11117, Bibcode：2020arXiv200111117M - The XRISM science data center: Optimizing the scientific return from a unique X-ray observatory
Michael Loewenstein; Robert S. Hill; Matthew P. Holland; Eric D. Miller; Tahir Yaqoob; Trisha F. Doyle; Patricia L. Hall; Efrem Braun; Chris Baluta; Koji Mukai; Yukikatsu Terada; Makoto Tashiro; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Takayuki Tamura; Shin'ichiro Uno; Shin Watanabe; Ken Ebisawa; Satoshi Eguchi; Yasushi Fukazawa; Katsuhiro Hayashi; Ryo Iizuka; Satoru Katsuda; Takao Kitaguchi; Aya Kubota; Shinya Nakashima; Kazuhiro Nakazawa; Hirokazu Odaka; Masanori Ohno; Naomi Ota; Rie Sato; Yasuharu Sugawara; Megumi Shidatsu; Tsubasa Tamba; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchiq
Proceedings of SPIE - The International Society for Optical Engineering, Volume：11444, 2020
© 2020 SPIE The X-Ray Imaging and Spectroscopy Mission, XRISM, is currently scheduled to launch in 2022 with the objective of building on the brief, but significant, successes of the ASTRO-H (Hitomi) mission in solving outstanding astrophysical questions using high resolution X-ray spectroscopy. The XRISM Science Operations Team (SOT) consists of the JAXA-led Science Operations Center (SOC) and NASA-led Science Data Center (SDC), which work together to optimize the scientific output from the Resolve high-resolution spectrometer and the Xtend wide-field imager through planning and scheduling of observations, processing and distribution of data, development and distribution of software tools and the calibration database (CaldB), support of ground and in-flight calibration, and support of XRISM users in their scientific investigations of the energetic universe. Here, we summarize the roles and responsibilities of the SDC and its current status and future plans. The Resolve instrument poses particular challenges due to its unprecedented combination of high spectral resolution and throughput, broad spectral coverage, and relatively small field-of-view and large pixel-size. We highlight those challenges and how they are being met.
International conference proceedings
DOI：https://doi.org/10.1117/12.2560840
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85099287387&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85099287387&origin=inward
DOI ID：10.1117/12.2560840, ISSN：0277-786X, eISSN：1996-756X, SCOPUS ID：85099287387 - Detail plans and preparations for the science operations of the XRISM mission
Yukikatsu Terada; Matt Holland; Michael Loewenstein; Makoto Tashiro; Hiromitsu Takahashi; Masayoshi Nobukawa; Tsunefumi Mizuno; Takayuki Tamura; Shin'ichiro Uno; Shin Watanabe; Chris Baluta; Laura Burns; Ken Ebisawa; Satoshi Eguchi; Yasushi Fukazawa; Katsuhiro Hayashi; Ryo Iizuka; Satoru Katsuda; Takao Kitaguchi; Aya Kubota; Eric Miller; Koji Mukai; Shinya Nakashima; Kazuhiro Nakazawa; Hirokazu Odaka; Masanori Ohno; Naomi Ota; Rie Sato; Yasuharu Sugawara; Megumi Shidatsu; Tsubasa Tamba; Atsushi Tanimoto; Yuichi Terashima; Yohko Tsuboi; Yuusuke Uchida; Hideki Uchiyama; Shigeo Yamauchi; Tahir Yaqoob
Proceedings of SPIE - The International Society for Optical Engineering, Volume：11444, 2020
© 2020 SPIE The XRISM is the X-ray astronomical mission led by JAXA/NASA/ESA with international participation, plan to be launched in 2022 (Japanese fiscal year), to quickly recover the high-resolution X-ray spectroscopy of astrophysical objects using the micro-calorimeter array after the failure of Hitomi. To enhance the scientific outputs of the mission, the Science Operations Team (SOT) is structured independently from the instrument teams and the mission operation team (MOT). The responsibilities of the SOT are summarized into four categories: 1) Guest observer program and data distributions, 2) Distribution of the analyses software and calibration database, 3) Guest observer supporting activities, and 4) the performance verification and optimization (PVO) activities. Before constructing the Operations Concept of the XRISM mission, the lessons on the Science Operations learned from the past Japanese X-ray missions (ASCA, Suzaku, and Hitomi) are reviewed, and 16 kinds of lessons are identified by the above categories: lessons on the importance of avoiding nonpublic (“animal”) tools, coding quality of public tools both on the engineering viewpoint and the calibration accuracy, tight communications with instrument teams and operations team, well-defined task division between scientists and engineers etc. Among these lessons, a) importance of the early preparations of the operations from the ground stage, b) construction of the independent team for the Science Operations from the instrument developments, and c) operations with well-defined duties by appointed members are recognized as the key lessons for XRISM. Then, i) the task division between the Mission and Science Operations and ii) the subgroup structure within the XRISM team are defined in detail as the XRISM Operations Concept. Then, following the Operations Concept, the detail plan of the Science Operations is designed as follows. The Science Operations tasks are shared among Japan, US, and Europe operated by three centers, the Science Operations Center (SOC) at JAXA, the Science Data Center (SDC) at NASA, and European Space Astronomy Centre (ESAC) at ESA. The SOT is defined as a combination of the SOC and SDC; the SOC is designed to perform tasks close to the spacecraft operations, such as spacecraft planning of science targets, quick-look health checks, pre-pipeline data processing, etc., and the SDC covers the tasks on the data calibration processing (pipeline processing), maintenance of the analysis tools etc. The data-archive and users-support activities are planned to be covered both by the SOC and SDC. Finally, the details of the Science Operations tasks and the tools for the Science Operations are also described in this paper. This information would be helpful for a construction of Science Operations of future X-ray missions.
International conference proceedings
DOI：https://doi.org/10.1117/12.2560861
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85099288779&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85099288779&origin=inward
DOI ID：10.1117/12.2560861, ISSN：0277-786X, eISSN：1996-756X, SCOPUS ID：85099288779 - Spectral properties of gamma-ray bursts observed by the Suzaku wide-band all-sky monitor
Yukikatsu Terada
Publications of the Astronomical Society of Japan, Volume：71, Number：4, Aug. 2019, [Reviewed]
Scientific journal
DOI：https://doi.org/10.1093/PASJ/PSZ054
DOI ID：10.1093/PASJ/PSZ054, ISSN：0004-6264, ORCID：67259908, Web of Science ID：WOS:000482425000010 - Science with the Cherenkov Telescope Array
Cherenkov Telescope Array Consortium; Acharya, B. S.; Agudo, I.; Al Samarai, I.; Alfaro, R.; Alfaro, J.; Alispach, C.; Alves Batista, R.; Amans, J. -P.; Amato, E.; Ambrosi, G.; Antolini, E.; Antonelli, L. A.; Aramo, C.; Araya, M.; Armstrong, T.; Arqueros, F.; Arrabito, L.; Asano, K.; Ashley, M.; Backes, M.; Balazs, C.; Balbo, M.; Ballester, O.; Ballet, J.; Bamba, A.; Barkov, M.; Barres de Almeida, U.; Barrio, J. A.; Bastieri, D.; Becherini, Y.; Belfiore, A.; Benbow, W.; Berge, D.; Bernardini, E.; Bernardini, M. G.; Bernardos, M.; Bernlöhr, K.; Bertucci, B.; Biasuzzi, B.; Bigongiari, C.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Blazek, J.; Boisson, C.; Bolmont, J.; Bonanno, G.; Bonardi, A.; Bonavolontà, C.; Bonnoli, G.; Bosnjak, Z.; Böttcher, M.; Braiding, C.; Bregeon, J.; Brill, A.; Brown, A. M.; Brun, P.; Brunetti, G.; Buanes, T.; Buckley, J.; Bugaev, V.; Bühler, R.; Bulgarelli, A.; Bulik, T.; Burton, M.; Burtovoi, A.; Busetto, G.; Canestrari, R.; Capalbi, M.; Capitanio, F.; Caproni, A.; Caraveo, P.; Cárdenas, V.; Carlile, C.; Carosi, R.; Carquín, E.; Carr, J.; Casanova, S.; Cascone, E.; Catalani, F.; Catalano, O.; Cauz, D.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chaves, R. C. G.; Chen, A.; Chen, X.; Chernyakova, M.; Chikawa, M.; Christov, A.; Chudoba, J.; Cieślar, M.; Coco, V.; Colafrancesco, S.; Colin, P.; Conforti, V.; Connaughton, V.; Conrad, J.; Contreras, J. L.; Cortina, J.; Costa, A.; Costantini, H.; Cotter, G.; Covino, S.; Crocker, R.; Cuadra, J.; Cuevas, O.; Cumani, P.; D'Aì, A.; D'Ammando, F.; D'Avanzo, P.; D'Urso, D.; Daniel, M.; Davids, I.; Dawson, B.; Dazzi, F.; De Angelis, A.; de Cássia dos Anjos, R.; De Cesare, G.; De Franco, A.; de Gouveia Dal Pino, E. M.; de la Calle, I.; de los Reyes Lopez, R.; De Lotto, B.; De Luca, A.; De Lucia, M.; de Naurois, M.; de Oña Wilhelmi, E.; De Palma, F.; De Persio, F.; de Souza, V.; Deil, C.; Del Santo, M.; Delgado, C.; della Volpe, D.; Di Girolamo, T.; Di Pierro, F.; Di Venere, L.; Díaz, C.; Dib, C.; Diebold, S.; Djannati-Ataï, A.; Domínguez, A.; Dominis Prester, D.; Dorner, D.; Doro, M.; Drass, H.; Dravins, D.; Dubus, G.; Dwarkadas, V. V.; Ebr, J.; Eckner, C.; Egberts, K.; Einecke, S.; Ekoume, T. R. N.; Elsässer, D.; Ernenwein, J. -P.; Espinoza, C.; Evoli, C.; Fairbairn, M.; Falceta-Goncalves, D.; Falcone, A.; Farnier, C.; Fasola, G.; Fedorova, E.; Fegan, S.; Fernandez-Alonso, M.; Fernández-Barral, A.; Ferrand, G.; Fesquet, M.; Filipovic, M.; Fioretti, V.; Fontaine, G.; Fornasa, M.; Fortson, L.; Freixas Coromina, L.; Fruck, C.; Fujita, Y.; Fukazawa, Y.; Funk, S.; Füßling, M.; Gabici, S.; Gadola, A.; Gallant, Y.; Garcia, B.; Garcia López, R.; Garczarczyk, M.; Gaskins, J.; Gasparetto, T.; Gaug, M.; Gerard, L.; Giavitto, G.; Giglietto, N.; Giommi, P.; Giordano, F.; Giro, E.; Giroletti, M.; Giuliani, A.; Glicenstein, J. -F.; Gnatyk, R.; Godinovic, N.; Goldoni, P.; Gómez-Vargas, G.; González, M. M.; González, J. M.; Götz, D.; Graham, J.; Grandi, P.; Granot, J.; Green, A. J.; Greenshaw, T.; Griffiths, S.; Gunji, S.; Hadasch, D.; Hara, S.; Hardcastle, M. J.; Hassan, T.; Hayashi, K.; Hayashida, M.; Heller, M.; Helo, J. C.; Hermann, G.; Hinton, J.; Hnatyk, B.; Hofmann, W.; Holder, J.; Horan, D.; Hörandel, J.; Horns, D.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Humensky, T. B.; Hütten, M.; Iarlori, M.; Inada, T.; Inome, Y.; Inoue, S.; Inoue, T.; Inoue, Y.; Iocco, F.; Ioka, K.; Iori, M.; Ishio, K.; Iwamura, Y.; Jamrozy, M.; Janecek, P.; Jankowsky, D.; Jean, P.; Jung-Richardt, I.; Jurysek, J.; Kaaret, P.; Karkar, S.; Katagiri, H.; Katz, U.; Kawanaka, N.; Kazanas, D.; Khélifi, B.; Kieda, D. B.; Kimeswenger, S.; Kimura, S.; Kisaka, S.; Knapp, J.; Knödlseder, J.; Koch, B.; Kohri, K.; Komin, N.; Kosack, K.; Kraus, M.; Krause, M.; Krauß, F.; Kubo, H.; Kukec Mezek, G.; Kuroda, H.; Kushida, J.; La Palombara, N.; Lamanna, G.; Lang, R. G.; Lapington, J.; Le Blanc, O.; Leach, S.; Lees, J. -P.; Lefaucheur, J.; Leigui de Oliveira, M. A.; Lenain, J. -P.; Lico, R.; Limon, M.; Lindfors, E.; Lohse, T.; Lombardi, S.; Longo, F.; López, M.; López-Coto, R.; Lu, C. -C.; Lucarelli, F.; Luque-Escamilla, P. L.; Lyard, E.; Maccarone, M. C.; Maier, G.; Majumdar, P.; Malaguti, G.; Mandat, D.; Maneva, G.; Manganaro, M.; Mangano, S.; Marcowith, A.; Marín, J.; Markoff, S.; Martí, J.; Martin, P.; Martínez, M.; Martínez, G.; Masetti, N.; Masuda, S.; Maurin, G.; Maxted, N.; Mazin, D.; Medina, C.; Melandri, A.; Mereghetti, S.; Meyer, M.; Minaya, I. A.; Mirabal, N.; Mirzoyan, R.; Mitchell, A.; Mizuno, T.; Moderski, R.; Mohammed, M.; Mohrmann, L.; Montaruli, T.; Moralejo, A.; Morcuende-Parrilla, D.; Mori, K.; Morlino, G.; Morris, P.; Morselli, A.; Moulin, E.; Mukherjee, R.; Mundell, C.; Murach, T.; Muraishi, H.; Murase, K.; Nagai, A.; Nagataki, S.; Nagayoshi, T.; Naito, T.; Nakamori, T.; Nakamura, Y.; Niemiec, J.; Nieto, D.; Nikołajuk, M.; Nishijima, K.; Noda, K.; Nosek, D.; Novosyadlyj, B.; Nozaki, S.; O'Brien, P.; Oakes, L.; Ohira, Y.; Ohishi, M.; Ohm, S.; Okazaki, N.; Okumura, A.; Ong, R. A.; Orienti, M.; Orito, R.; Osborne, J. P.; Ostrowski, M.; Otte, N.; Oya, I.; Padovani, M.; Paizis, A.; Palatiello, M.; Palatka, M.; Paoletti, R.; Paredes, J. M.; Pareschi, G.; Parsons, R. D.; Pe'er, A.; Pech, M.; Pedaletti, G.; Perri, M.; Persic, M.; Petrashyk, A.; Petrucci, P.; Petruk, O.; Peyaud, B.; Pfeifer, M.; Piano, G.; Pisarski, A.; Pita, S.; Pohl, M.; Polo, M.; Pozo, D.; Prandini, E.; Prast, J.; Principe, G.; Prokhorov, D.; Prokoph, H.; Prouza, M.; Pühlhofer, G.; Punch, M.; Pürckhauer, S.; Queiroz, F.; Quirrenbach, A.; Rainò, S.; Razzaque, S.; Reimer, O.; Reimer, A.; Reisenegger, A.; Renaud, M.; Rezaeian, A. H.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richtler, T.; Rico, J.; Rieger, F.; Riquelme, M.; Rivoire, S.; Rizi, V.; Rodriguez, J.; Rodriguez Fernandez, G.; Rodríguez Vázquez, J. J.; Rojas, G.; Romano, P.; Romeo, G.; Rosado, J.; Rovero, A. 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A.; Wischnewski, R.; Wood, M.; Yamamoto, T.; Yamazaki, R.; Yanagita, S.; Yang, L.; Yoshida, T.; Yoshiike, S.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zampieri, L.; Zandanel, F.; Zanin, R.; Zavrtanik, M.; Zavrtanik, D.; Zdziarski, A. A.; Zech, A.; Zechlin, H.; Zhdanov, V. I.; Ziegler, A.; Zorn, J.
Mar. 2019
The Cherenkov Telescope Array, CTA, will be the major global observatory for very high energy gamma-ray astronomy over the next decade and beyond. The scientific potential of CTA is extremely broad: from understanding the role of relativistic cosmic particles to the search for dark matter. CTA is an explorer of the extreme universe, probing environments from the immediate neighbourhood of black holes to cosmic voids on the largest scales. Covering a huge range in photon energy from 20 GeV to 300 TeV, CTA will improve on all aspects of performance with respect to current instruments. The observatory will operate arrays on sites in both hemispheres to provide full sky coverage and will hence maximize the potential for the rarest phenomena such as very nearby supernovae, gamma-ray bursts or gravitational wave transients. With 99 telescopes on the southern site and 19 telescopes on the northern site, flexible operation will be possible, with sub-arrays available for specific tasks. CTA will have important synergies with many of the new generation of major astronomical and astroparticle observatories. Multi-wavelength and multi-messenger approaches combining CTA data with those from other instruments will lead to a deeper understanding of the broad-band non-thermal properties of target sources. The CTA Observatory will be operated as an open, proposal-driven observatory, with all data available on a public archive after a pre-defined proprietary period. Scientists from institutions worldwide have combined together to form the CTA Consortium. This Consortium has prepared a proposal for a Core Programme of highly motivated observations. The programme, encompassing approximately 40% of the available observing time over the first ten years of CTA operation, is made up of individual Key Science Projects (KSPs), which are presented in this document....
Science with the Cherenkov Telescope Array
DOI：https://doi.org/10.1142/10986
DOI ID：10.1142/10986, ORCID：101133505, arXiv ID：arXiv:1709.07997, Bibcode：2019scta.book.....C - Spectral and Timing Analysis of the Accretion-powered Pulsar 4U 1626-67 Observed with Suzaku and NuSTAR
Yukikatsu Terada
The Astrophysical Journal, 2019
We present an analysis of the spectral shape and pulse profile of the accretion-powered pulsar 4U 1626-67 observed with Suzaku and Nuclear Spectroscopic Telescope Array (NuSTAR) during a spin-up state. The pulsar, which experienced a torque reversal to spin-up in 2008, has a spin period of ∼7.7 s. Comparing the phase-averaged spectra obtained with Suzaku in 2010 and with NuSTAR in 2015, we find that the spectral shape changed between the two observations: the 3-10 keV flux increased by ∼5%, while the 30-60 keV flux decreased significantly by ∼35%. Phase-averaged and phase-resolved spectral analysis shows that the continuum spectrum observed by NuSTAR is well described by an empirical negative and positive power law times exponential continuum with an added broad Gaussian emission component around the spectral peak at ∼20 keV. Taken together with the observed \dot{P} value obtained from the Fermi/gamma-ray burst monitor data, we conclude that the spectral change between the Suzaku and NuSTAR observations was likely caused by an increase in the accretion rate. We also report the possible detection of asymmetry in the profile of the fundamental cyclotron line. Furthermore, we present a study of the energy-resolved pulse profiles using a new relativistic ray tracing code, where we perform a simultaneous fit to the pulse profiles assuming a two-column geometry with a mixed pencil- and fan-beam emission pattern. The resulting pulse profile decompositions enable us to obtain geometrical parameters of accretion columns (inclination, azimuthal and polar angles) and a fiducial set of beam patterns. This information is important to validate the theoretical predictions from radiation transfer in a strong magnetic field....
Scientific journal
DOI：https://doi.org/10.3847/1538-4357/AB1F87
DOI ID：10.3847/1538-4357/AB1F87, ORCID：101088819, arXiv ID：arXiv:1905.05356, Web of Science ID：WOS:000509095700010, Bibcode：2019ApJ...878..121I - Introduction to CTA Science
Yukikatsu Terada
Science with the Cherenkov Telescope Array, 2019
Scientific journal
DOI：https://doi.org/10.1142/9789813270091_0001
DOI ID：10.1142/9789813270091_0001, ORCID：67259911, Web of Science ID：WOS:000467612100001 - Summary of the 13th IACHEC Meeting
Madsen, K. K.; Natalucci, L.; Belanger, G.; Grant, C. E.; Guainazzi, M.; Kashyap, V.; Marshall, H. L.; Miller, E. D.; Nevalainen, J.; Plucinsky, P. P.; Terada, Y.
Jan. 2019
We summarize the outcome of the 13th meeting of the International Astronomical Consortium for High Energy Calibration (IACHEC), held at Tenuta dei Ciclamini (Avigliano Umbro, Italy) in April 2018. Fifty-one scientists directly involved in the calibration of operational and future high-energy missions gathered during 3.5 days to discuss the current status of the X-ray payload inter-calibration and possible approaches to improve it. This summary consists of reports from the various working groups with topics ranging from the identification and characterization of standard calibration sources, multi-observatory cross-calibration campaigns, appropriate and new statistical techniques, calibration of instruments and characterization of background, and communication and preservation of knowledge and results for the benefit of the astronomical community....
arXiv e-prints
ORCID：101133507, arXiv ID：arXiv:1901.00934, Bibcode：2019arXiv190100934M - Detection of polarized gamma-ray emission from the Crab nebula with the Hitomi Soft Gamma-ray Detector
Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W. Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W. Bautz; Roger Blandford; Laura W. Brenneman; Gregory V. Brown; Esra Bulbul; Edward M. Cackett; Maria Chernyakova; Meng P. Chiao; Paolo S. Coppi; Elisa Costantini; Jelle de Plaa; Cor P. de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E. Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C. Fabian; Carlo Ferrigno; Adam R. Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C. Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M. Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S. Hiraga; Ann Hornschemeier; Akio Hoshino; John P. Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L. Kelley; Caroline A. Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A. Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A. Leutenegger; Olivier Limousin; Michael Loewenstein; Knox S. Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R. McNamara; Missagh Mehdipour; Eric D. Miller; Jon M. Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F. Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K. Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stephane Paltani; Robert Petre; Ciro Pinto; Frederick S. Porter; Katja Pottschmidt; Christopher S. Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter J. Serlemtsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K. Smith; Yang Soong; Lukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin'ichiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T. Tanaka; Makoto S. Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shin'ichiro Uno; C. Megan Urry; Eugenio Ursino; Shin Watanabe; Norbert Werner; Dan R. Wilkins; Brian J. Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y. Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi; Yuusuke Uchida
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：6, Dec. 2018, [Reviewed]
We present the results from the Hitomi Soft Gamma-ray Detector (SGD) observation of the Crab nebula. The main part of SGD is a Compton camera, which in addition to being a spectrometer, is capable of measuring polarization of gamma-ray photons. The Crab nebula is one of the brightest X-ray / gamma-ray sources on the sky, and, the only source from which polarized X-ray photons have been detected. SGD observed the Crab nebula during the initial test observation phase of Hitomi. We performed the data analysis of the SGD observation, the SGD background estimation and the SGD Monte Carlo simulations, and, successfully detected polarized gamma-ray emission from the Crab nebula with only about 5 ks exposure time. The obtained polarization fraction of the phase-integrated Crab emission (sum of pulsar and nebula emissions) is (22.1% +/- 10.6%), and, the polarization angle is 110.degrees 7 + 13.degrees 2 /-13.degrees 0 in the energy range of 60-160 keV (The errors correspond to the 1 sigma deviation). The confidence level of the polarization detection was 99.3%. The polarization angle measured by SGD is about one sigma deviation with the projected spin axis of the pulsar, 124.degrees 0 +/- 0.degrees 1.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psy118
DOI ID：10.1093/pasj/psy118, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000456072300015 - A technique for estimating the absolute gain of a photomultiplier tube
Yukikatsu Terada
Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：894, First page：1, Last page：7, Jun. 2018, [Reviewed]
English, Scientific journal
DOI：https://doi.org/10.1016/J.NIMA.2018.03.034
DOI ID：10.1016/J.NIMA.2018.03.034, ISSN：0168-9002, ORCID：67259902, Web of Science ID：WOS:000430704600001 - Hitomi X-ray observation of the pulsar wind nebula G21.5-0.9
Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W Bautz; Roger Blandford; Laura W Brenneman; Gregory V Brown; Esra Bulbul; Edward M Cackett; Maria Chernyakova; Meng P Chiao; Paolo S Coppi; Elisa Costantini; Jelle de Plaa; Cor P de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C Fabian; Carlo Ferrigno; Adam R Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S Hiraga; Ann Hornschemeier; Akio Hoshino; John P Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L Kelley; Caroline A Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A Leutenegger; Olivier Limousin; Michael Loewenstein; Knox S Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R McNamara; Missagh Mehdipour; Eric D Miller; Jon M Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stéphane Paltani; Robert Petre; Ciro Pinto; Frederick S Porter; Katja Pottschmidt; Christopher S Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter J Serlemtsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K Smith; Yang Soong; Łukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin’ichiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T Tanaka; Makoto S Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shin’ichiro Uno; C Megan Urry; Eugenio Ursino; Shin Watanabe; Norbert Werner; Dan R Wilkins; Brian J Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi; Toshiki Sato; Nozomu Nakaniwa; Hiroaki Murakami; Benson Guest
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：3, Jun. 2018, [Reviewed]
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psy027
DOI ID：10.1093/pasj/psy027, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000439655600009 - Modeling of proton-induced radioactivation background in hard X-ray telescopes: Geant4-based simulation and its demonstration by Hitomi's measurement in a low Earth orbit
Hirokazu Odaka; Makoto Asai; Kouichi Hagino; Tatsumi Koi; Greg Madejski; Tsunefumi Mizuno; Masanori Ohno; Shinya Saito; Tamotsu Sato; Dennis H. Wright; Teruaki Enoto; Yasushi Fukazawa; Katsuhiro Hayashi; Jun Kataoka; Junichiro Katsuta; Madoka Kawaharada; Shogo B. Kobayashi; Motohide Kokubun; Philippe Laurent; Francois Lebrun; Olivier Limousin; Daniel Maier; Kazuo Makishima; Taketo Mimura; Katsuma Miyake; Kunishiro Mori; Hiroaki Murakami; Takeshi Nakamori; Toshio Nakano; Kazuhiro Nakazawa; Hirofumi Noda; Masayuki Ohta; Masanobu Ozaki; Goro Sato; Rie Sato; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin'ichiro Takeda; Takaaki Tanaka; Yasuyuki Tanaka; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Shin Watanabe; Kazutaka Yamaoka; Tetsuya Yasuda; Yoichi Yatsu; Takayuki Yuasa; Andreas Zoglauer
NUCLEAR INSTRUMENTS & METHODS IN PHYSICS RESEARCH SECTION A-ACCELERATORS SPECTROMETERS DETECTORS AND ASSOCIATED EQUIPMENT, Volume：891, First page：92, Last page：105, May 2018, [Reviewed]
Hard X-ray astronomical observatories in orbit suffer from a significant amount of background due to radioactivation induced by cosmic-ray protons and/or geomagnetically trapped protons. Within the framework of a full Monte Carlo simulation, we present modeling of in-orbit instrumental background which is dominated by radioactivation. To reduce the computation time required by straightforward simulations of delayed emissions from activated isotopes, we insert a semi-analytical calculation that converts production probabilities of radioactive isotopes by interaction of the primary protons into decay rates at measurement time of all secondary isotopes. Therefore, our simulation method is separated into three steps: (1) simulation of isotope production, (2) semi-analytical conversion to decay rates, and (3) simulation of decays of the isotopes at measurement time. This method is verified by a simple setup that has a CdTe semiconductor detector, and shows a 100-fold improvement in efficiency over the straightforward simulation. To demonstrate its experimental performance, the simulation framework was tested against data measured with a CdTe sensor in the Hard X-ray Imager onboard the Hitomi X-ray Astronomy Satellite, which was put into a low Earth orbit with an altitude of 570 km and an inclination of 31 degrees, and thus experienced a large amount of irradiation from geomagnetically trapped protons during its passages through the South Atlantic Anomaly. The simulation is able to treat full histories of the proton irradiation and multiple measurement windows. The simulation results agree very well with the measured data, showing that the measured background is well described by the combination of proton-induced radioactivation of the CdTe detector itself and thick Bi4Ge3O12 scintillator shields, leakage of cosmic X-ray background and albedo gamma-ray radiation, and emissions from naturally contaminated isotopes in the detector system.
ELSEVIER SCIENCE BV, English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2018.02.071
DOI ID：10.1016/j.nima.2018.02.071, ISSN：0168-9002, eISSN：1872-9576, Web of Science ID：WOS:000428344600014 - Design and performance of Soft Gamma-ray Detector onboard the Hitomi (ASTRO-H) satellite
Hiroyasu Tajima; Shin Watanabe; Yasushi Fukazawa; Roger Blandford; Teruaki Enoto; Andrea Goldwurm; Kouichi Hagino; Katsuhiro Hayashi; Yuto Ichinohe; Jun Kataoka; Junichiro Katsuta; Takao Kitaguchi; Motohide Kokubun; Philippe Laurent; François Lebrun; Olivier Limousin; Grzegorz M. Madejski; Kazuo Makishima; Tsunefumi Mizuno; Kunishiro Mori; Takeshi Nakamori; Toshio Nakano; Kazuhiro Nakazawa; Hirofumi Noda; Hirokazu Odaka; Masanori Ohno; Masayuki Ohta; Shinya Saito; Goro Sato; Rie Sato; Shinichiro Takeda; Hiromitsu Takahashi; Tadayuki Takahashi; Takaaki Tanaka; Yasuyuki Tanaka; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Kazutaka Yamaoka; Yoichi Yatsu; Daisuke Yonetoku; Takayuki Yuasa
Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：2, Apr. 2018, [Reviewed]
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.
SPIE, English, Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.4.2.021411
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85046023600&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85046023600&origin=inward
DOI ID：10.1117/1.JATIS.4.2.021411, ISSN：2329-4221, eISSN：2329-4221, SCOPUS ID：85046023600, Web of Science ID：WOS:000439235200011 - In-orbit performance and calibration of the Hard X-ray Imager onboard Hitomi (ASTRO-H)
Kouichi Hagino; Kazuhiro Nakazawa; Goro Sato; Motohide Kokubun; Teruaki Enoto; Yasushi Fukazawa; Katsuhiro Hayashi; Jun Kataoka; Junichiro Katsuta; Shogo B. Kobayashi; Philippe Laurent; Francois Lebrun; Olivier Limousin; Daniel Maier; Kazuo Makishima; Taketo Mimura; Katsuma Miyake; Tsunefumi Mizuno; Kunishiro Mori; Hiroaki Murakami; Takeshi Nakamori; Toshio Nakano; Hirofumi Noda; Hirokazu Odaka; Masanori Ohno; Masayuki Ohta; Shinya Saito; Rie Sato; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin'ichiro Takeda; Takaaki Tanaka; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Shin Watanabe; Kazutaka Yamaoka; Yoichi Yatsu; Takayuki Yuasa
Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：2, Apr. 2018, [Reviewed]
The Hard X-ray Imager (HXI) onboard Hitomi (ASTRO-H) is an imaging spectrometer covering hard x-ray energies of 5 to 80 keV. Combined with the Hard X-ray Telescope, it enables imaging spectroscopy with an angular resolution of 10.7 half-power diameter, in a field of view of 9' × 9'. The main imager is composed of four layers of Si detectors and one layer of CdTe detector, stacked to cover a wide energy band up to 80 keV, surrounded by an active shield made of Bi4Ge3O12 scintillator to reduce the background. The HXI started observations 12 days before the Hitomi loss and successfully obtained data from G21.5-0.9, Crab, and blank sky. Utilizing these data, we calibrate the detector response and study properties of in-orbit background. The observed Crab spectra agree well with a powerlaw model convolved with the detector response, within 5% accuracy. We find that albedo electrons in specified orbit strongly affect the background of the Si top layer and establish a screening method to reduce it. The background level over the full field of view after all the processing and screening is as low as the preflight requirement of 1 - 3 × 10-4 counts s-1 cm-2 keV-1.
SPIE, English, Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.4.2.021409
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85042871785&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85042871785&origin=inward
DOI ID：10.1117/1.JATIS.4.2.021409, ISSN：2329-4221, eISSN：2329-4221, SCOPUS ID：85042871785, Web of Science ID：WOS:000439235200009 - HITOMI (ASTRO-H) X-ray astronomy satellite
Tadayuki Takahashi; Motohide Kokubun; Kazuhisa Mitsuda; Richard L. Kelley; Takaya Ohashi; Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W. Allen; Naohisa Anabuki; Lorella Angelini; Keith Arnaud; Makoto Asai; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Philipp Azzarello; Chris Baluta; Aya Bamba; Nobutaka Bando; Marshall W. Bautz; Thomas Bialas; Roger Blandford; Kevin Boyce; Laura W. Brenneman; Gregory V. Brown; Esra Bulbul; Edward M. Cackett; Edgar Canavan; Maria Chernyakova; Meng P. Chiao; Paolo S. Coppi; Elisa Costantini; Steve O' Dell; Michael DiPirro; Chris Done; Tadayasu Dotani; John Doty; Ken Ebisawa; Megan E. Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C. Fabian; Carlo Ferrigno; Adam R. Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Stefan Funk; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C. Gallo; Poshak Gandhi; Kirk Gilmore; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Daniel Haas; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M. Harrus; Isamu Hatsukade; Takayuki Hayashi; Katsuhiro Hayashi; Kiyoshi Hayashida; Jan Willem Den Herder; Junko S. Hiraga; Kazuyuki Hirose; Ann Hornschemeier; Akio Hoshino; John P. Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Kazunori Ishibashi; Manabu Ishida; Kumi Ishikawa; Kosei Ishimura; Yoshitaka Ishisaki; Masayuki Itoh; Masachika Iwai; Naoko Iwata; Naoko Iyomoto; Chris Jewell; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Erin Kara; Jun Kataoka; Satoru Katsuda; Junichiro Katsuta; Madoka Kawaharada; Nobuyuki Kawai; Taro Kawano; Shigeo Kawasaki; Dmitry Khangulyan; Caroline A. Kilbourne; Mark Kimball
Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：2, Apr. 2018, [Reviewed]
© The Authors. 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 February 17, 2016, the spacecraft lost its function on March 26, 2016, but the commissioning phase for about a month provided valuable information on the onboard instruments and the spacecraft system, including astrophysical results obtained from first light observations. The paper describes the Hitomi (ASTRO-H) mission, its capabilities, the initial operation, and the instruments/spacecraft performances confirmed during the commissioning operations for about a month.
DOI：https://doi.org/10.1117/1.JATIS.4.2.021402
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85062992860&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85062992860&origin=inward
DOI ID：10.1117/1.JATIS.4.2.021402, ISSN：2329-4124, eISSN：2329-4221, SCOPUS ID：85062992860, Web of Science ID：WOS:000439235200002 - Hard x-ray imager onboard Hitomi (ASTRO-H)
Nakazawa Kazuhiro; Sato Goro; Kokubun Motohide; Enoto Teruaki; Fukazawa Yasushi; Hagino Kouichi; Hayashi Katsuhiro; Kataoka Jun; Katsuta Junichiro; Kobayashi Shogo B; Laurent Philippe; Lebrun Francois; Limousin Olivier; Maier Daniel; Makishima Kazuo; Mizuno Tsunefumi; Mori Kunishiro; Nakamori Takeshi; Nakano Toshio; Noda Hirofumi; Odaka Hirokazu; Ohno Masanori; Ohta Masayuki; Saito Shinya; Sato Rie; Tajima Hiroyasu; Takahashi Hiromitsu; Takahashi Tadayuki; Takeda Shin'ichiro; Tanaka Takaaki; Terada Yukikatsu; Uchiyama Hideki; Uchiyama Yasunobu; Watanabe Shin; Yamaoka Kazutaka; Yatsu Yoichi; Yuasa Takayuki
JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS, Volume：4, Number：2, Apr. 2018, [Reviewed]
DOI：https://doi.org/10.1117/1.JATIS.4.2.021410
DOI ID：10.1117/1.JATIS.4.2.021410, ISSN：2329-4124, Web of Science ID：WOS:000439235200010 - In-flight calibration of Hitomi Soft X-ray Spectrometer. (1) Background
Kilbourne Caroline A; Sawada Makoto; Tsujimoto Masahiro; Angellini Lorella; Boyce Kevin R; Eckart Megan E; Fujimoto Ryuichi; Ishisaki Yoshitaka; Kelley Richard L; Koyama Shu; Leutenegger Maurice A; Loewenstein Michael; McCammon Dan; Mitsuda Kazuhisa; Nakashima Shinya; Porter Frederick S; Seta Hiromi; Takei Yoh; Tashiro Makoto S; Terada Yukikatsu; Yamada Shinya; Yamasaki Noriko Y
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：2, Mar. 2018, [Reviewed]
The X-Ray Spectrometer (XRS) instrument of Suzaku provided the first measurement of the non-X-ray background (NXB) of an X-ray calorimeter spectrometer, but the data set was limited. The Soft X-ray Spectrometer (SXS) instrument of Hitomi was able to provide a more detailed picture of X-ray calorimeter background, with more than 360 ks of data while pointed at the Earth, and a comparable amount of blank-sky data. These data are important not only for analyzing SXS science data, but also for categorizing the contributions to the NXB in X-ray calorimeters as a class. In this paper, we present the contributions to the SXS NXB, the types and effectiveness of the screening, the interaction of the screening with the broad-band redistribution, and the residual background spectrum as a function of magnetic cut-off rigidity. The orbit-averaged SXS NXB in the range 0.3-12 keV was 4 x 10(-2) counts s(-1) cm(-2). This very low background in combination with groundbreaking spectral resolution gave SXS unprecedented sensitivity to weak spectral lines.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psx139
DOI ID：10.1093/pasj/psx139, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000432287600010 - Hitomi observation of radio galaxy NGC 1275: The first X-ray microcalorimeter spectroscopy of Fe-K alpha line emission from an active galactic nucleus
Hitomi Collaboration, Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W Bautz; Roger Blandford; Laura W Brenneman; Gregory V Brown; Esra Bulbul; Edward M Cackett; Maria Chernyakova; Meng P Chiao; Paolo S Coppi; Elisa Costantini; Jelle de Plaa; Cor P de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C Fabian; Carlo Ferrigno; Adam R Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S Hiraga; Ann Hornschemeier; Akio Hoshino; John P Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L Kelley; Caroline A Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A Leutenegger; Olivier O Limousin; Michael Loewenstein; Knox S Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R McNamara; Missagh Mehdipour; Eric D Miller; Jon M Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stéphane Paltani; Robert Petre; Ciro Pinto; Frederick S Porter; Katja Pottschmidt; Christopher S Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter J Serlemitsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K Smith; Yang Soong; Łukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin’ichiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T Tanaka; Makoto S Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shin’ichiro Uno; C Megan Urry; Eugenio Ursino; Shin Watanabe; Norbert Werner; Dan R Wilkins; Brian J Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi; Taiki Kawamuro
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：2, Mar. 2018, [Reviewed]
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psx147
DOI ID：10.1093/pasj/psx147, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000432287600005 - Search for thermal X-ray features from the Crab nebula with the Hitomi soft X-ray spectrometer
Hitomi Collaboration, Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W Bautz; Roger Blandford; Laura W Brenneman; Gregory V Brown; Esra Bulbul; Edward M Cackett; Maria Chernyakova; Meng P Chiao; Paolo S Coppi; Elisa Costantini; Jelle de Plaa; Cor P de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C Fabian; Carlo Ferrigno; Adam R Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S Hiraga; Ann Hornschemeier; Akio Hoshino; John P Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L Kelley; Caroline A Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A Leutenegger; Olivier Limousin; Michael Loewenstein; Knox S Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R McNamara; Missagh Mehdipour; Eric D Miller; Jon M Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stéphane Paltani; Robert Petre; Ciro Pinto; Frederick S Porter; Katja Pottschmidt; Christopher S Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Toshiki Sato; Makoto Sawada; Norbert Schartel; Peter J Serlemtsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K Smith; Yang Soong; Łukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin΄ichiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T Tanaka; Makoto S Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shin΄ichiro Uno; C Megan Urry; Eugenio Ursino; Shin Watanabe; Norbert Werner; Dan R Wilkins; Brian J Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi; Nozomu Tominaga; Takashi J Moriya
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：2, Mar. 2018, [Reviewed]
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psx072
DOI ID：10.1093/pasj/psx072, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000432287600006 - Glimpse of the highly obscured HMXB IGR J16318-4848 with Hitomi
Hitomi Collaboration; Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W Bautz; Roger Blandford; Laura W Brenneman; Gregory V Brown; Esra Bulbul; Edward M Cackett; Maria Chernyakova; Meng P Chiao; Paolo S Coppi; Elisa Costantini; Jelle de Plaa; Cor P de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C Fabian; Carlo Ferrigno; Adam R Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S Hiraga; Ann Hornschemeier; Akio Hoshino; John P Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L Kelley; Caroline A Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A Leutenegger; Olivier O Limousin; Michael Loewenstein; Knox S Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R McNamara; Missagh Mehdipour; Eric D Miller; Jon M Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stéphane Paltani; Robert Petre; Ciro Pinto; Frederick S Porter; Katja Pottschmidt; Christopher S Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter J Serlemtsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K Smith; Yang Soong; Łukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shiníchiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T Tanaka; Makoto S Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shiníchiro Uno; C Megan Urry; Eugenio Ursino; Shin Watanabe; Norbert Werner; Dan R Wilkins; Brian J Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi; Nozomi Nakaniwa
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：2, Mar. 2018, [Reviewed]
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psx154
DOI ID：10.1093/pasj/psx154, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000432287600009 - Hitomi X-ray studies of giant radio pulses from the Crab pulsar
Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W. Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W. Bautz; Roger Blandford; Laura W. Brenneman; Gregory V. Brown; Esra Bulbul; Edward M. Cackett; Maria Chernyakova; Meng P. Chiao; Paolo S. Coppi; Elisa Costantini; Jelle De Plaa; Cor P. De Vries; Jan Willem Den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E. Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C. Fabian; Carlo Ferrigno; Adam R. Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C. Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M. Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S. Hiraga; Ann Hornschemeier; Akio Hoshino; John P. Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L. Kelley; Caroline A. Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A. Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; L. E.E. Shiu-Hang; Maurice A. Leutenegger; Olivier O. Limousin; Michael Loewenstein; Knox S. Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R. McNamara; Missagh Mehdipour; Eric D. Miller; Jon M. Miller; Shin Mineshige
Publications of the Astronomical Society of Japan, Volume：70, Number：2, Mar. 2018, [Reviewed]
© The Author(s) 2017. Published by Oxford University Press on behalf of the Astronomical Society of Japan. To search for giant X-ray pulses correlated with the giant radio pulses (GRPs) from the Crab pulsar, we performed a simultaneous observation of the Crab pulsar with the X-ray satellite Hitomi in the 2-300 keV band and the Kashima NICT radio telescope in the 1.4-1.7 GHz band with a net exposure of about 2 ks on 2016 March 25, just before the loss of the Hitomi mission. The timing performance of the Hitomi instruments was confirmed to meet the timing requirement and about 1000 and 100 GRPs were simultaneously observed at the main pulse and inter-pulse phases, respectively, and we found no apparent correlation between the giant radio pulses and the X-ray emission in either the main pulse or inter-pulse phase. All variations are within the 2 σ fluctuations of the X-ray fluxes at the pulse peaks, and the 3 σ upper limits of variations of main pulse or inter-pulse GRPs are 22% or 80% of the peak flux in a 0.20 phase width, respectively, in the 2-300 keV band. The values for main pulse or inter-pulse GRPs become 25% or 110%, respectively, when the phase width is restricted to the 0.03 phase. Among the upper limits from the Hitomi satellite, those in the 4.5-10 keV and 70-300 keV bands are obtained for the first time, and those in other bands are consistent with previous reports. Numerically, the upper limits of the main pulse and inter-pulse GRPs in the 0.20 phase width are about (2.4 and 9.3) × 10−11 erg cm−2, respectively. No significant variability in pulse profiles implies that the GRPs originated from a local place within the magnetosphere. Although the number of photon-emitting particles should temporarily increase to account for the brightening of the radio emission, the results do not statistically rule out variations correlated with the GRPs, because the possible X-ray enhancement may appear due to a >0.02% brightening of the pulse-peak flux under such conditions.
Scientific journal
DOI：https://doi.org/10.1093/pasj/psx083
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85060148955&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=85060148955&origin=inward
DOI ID：10.1093/pasj/psx083, ISSN：0004-6264, eISSN：2053-051X, SCOPUS ID：85060148955, Web of Science ID：WOS:000432287600007 - Atmospheric gas dynamics in the Perseus cluster observed with Hitomi
Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W Bautz; Roger Blandford; Laura W Brenneman; Gregory V Brown; Esra Bulbul; Edward M Cackett; Rebecca E A Canning; Maria Chernyakova; Meng P Chiao; Paolo S Coppi; Elisa Costantini; Jelle de Plaa; Cor P de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C Fabian; Carlo Ferrigno; Adam R Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Tasuku Hayashi; Kiyoshi Hayashida; Junko S Hiraga; Ann Hornschemeier; Akio Hoshino; John P Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Shota Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L Kelley; Caroline A Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A Leutenegger; Olivier Limousin; Michael Loewenstein; Knox S Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R McNamara; Missagh Mehdipour; Eric D Miller; Jon M Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stéphane Paltani; Robert Petre; Ciro Pinto; Frederick S Porter; Katja Pottschmidt; Christopher S Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter J Serlemtsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K Smith; Yang Soong; Łukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin’ichiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Keigo Tanaka; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T Tanaka; Makoto S Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shin’ichiro Uno; C Megan Urry; Eugenio Ursino; Qian H S Wang; Shin Watanabe; Norbert Werner; Dan R Wilkins; Brian J Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：2, Mar. 2018, [Reviewed]
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psx138
DOI ID：10.1093/pasj/psx138, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000432287600001 - Measurements of resonant scattering in the Perseus Cluster core with Hitomi SXS
Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W Bautz; Roger Blandford; Laura W Brenneman; Gregory V Brown; Esra Bulbul; Edward M Cackett; Maria Chernyakova; Meng P Chiao; Paolo S Coppi; Elisa Costantini; Jelle de Plaa; Cor P de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C Fabian; Carlo Ferrigno; Adam R Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Maki Furukawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S Hiraga; Ann Hornschemeier; Akio Hoshino; John P Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L Kelley; Caroline A Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A Leutenegger; Olivier O Limousin; Michael Loewenstein; Knox S Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R McNamara; Missagh Mehdipour; Eric D Miller; Jon M Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Anna Ogorzalek; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stéphane Paltani; Robert Petre; Ciro Pinto; Frederick S Porter; Katja Pottschmidt; Christopher S Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter J Serlemtsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K Smith; Yang Soong; Łukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shiníchiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T Tanaka; Makoto S Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shiníchiro Uno; C Megan Urry; Eugenio Ursino; Shin Watanabe; Norbert Werner; Dan R Wilkins; Brian J Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：2, Mar. 2018, [Reviewed]
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psx127
DOI ID：10.1093/pasj/psx127, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000432287600002 - Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta
Hitomi Collaboration, Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W Bautz; Roger Blandford; Laura W Brenneman; Gregory V Brown; Esra Bulbul; Edward M Cackett; Maria Chernyakova; Meng P Chiao; Paolo S Coppi; Elisa Costantini; Jelle de Plaa; Cor P de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C Fabian; Carlo Ferrigno; Adam R Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S Hiraga; Ann Hornschemeier; Akio Hoshino; John P Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L Kelley; Caroline A Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A Leutenegger; Olivier Limousin; Michael Loewenstein; Knox S Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R McNamara; Missagh Mehdipour; Eric D Miller; Jon M Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stéphane Paltani; Robert Petre; Ciro Pinto; Frederick S Porter; Katja Pottschmidt; Christopher S Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Toshiki Sato; Makoto Sawada; Norbert Schartel; Peter J Serlemtsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K Smith; Yang Soong; Łukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin’ichiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T Tanaka; Makoto S Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shin’ichiro Uno; C Megan Urry; Eugenio Ursino; Shin Watanabe; Norbert Werner; Dan R Wilkins; Brian J Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：2, Mar. 2018, [Reviewed]
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psx151
DOI ID：10.1093/pasj/psx151, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000432287600008 - Temperature structure in the Perseus cluster core observed with Hitomi
Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W Bautz; Roger Blandford; Laura W Brenneman; Gregory V Brown; Esra Bulbul; Edward M Cackett; Maria Chernyakova; Meng P Chiao; Paolo S Coppi; Elisa Costantini; Jelle de Plaa; Cor P de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C Fabian; Carlo Ferrigno; Adam R Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Maki Furukawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S Hiraga; Ann Hornschemeier; Akio Hoshino; John P Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Yuichi Kato; Satoru Katsuda; Nobuyuki Kawai; Richard L Kelley; Caroline A Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A Leutenegger; Olivier Limousin; Michael Loewenstein; Knox S Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R McNamara; Missagh Mehdipour; Eric D Miller; Jon M Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stéphane Paltani; Robert Petre; Ciro Pinto; Frederick S Porter; Katja Pottschmidt; Christopher S Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter J Serlemtsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K Smith; Yang Soong; Łukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shiníchiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T Tanaka; Makoto S Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shiníchiro Uno; C Megan Urry; Eugenio Ursino; Shin Watanabe; Norbert Werner; Dan R Wilkins; Brian J Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：2, Mar. 2018, [Reviewed]
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psy004
DOI ID：10.1093/pasj/psy004, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000432287600003 - Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi
Hitomi Collaboration, Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W Bautz; Roger Blandford; Laura W Brenneman; Gregory V Brown; Esra Bulbul; Edward M Cackett; Maria Chernyakova; Meng P Chiao; Paolo S Coppi; Elisa Costantini; Jelle de Plaa; Cor P de Vries; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C Fabian; Carlo Ferrigno; Adam R Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Natalie Hell; Junko S Hiraga; Ann Hornschemeier; Akio Hoshino; John P Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L Kelley; Caroline A Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A Leutenegger; Olivier Limousin; Michael Loewenstein; Knox S Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R McNamara; Missagh Mehdipour; Eric D Miller; Jon M Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stéphane Paltani; Robert Petre; Ciro Pinto; Frederick S Porter; Katja Pottschmidt; Christopher S Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter J Serlemtsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K Smith; Yang Soong; Łukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin’ichiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T Tanaka; Makoto S Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shin’ichiro Uno; C Megan Urry; Eugenio Ursino; Shin Watanabe; Norbert Werner; Dan R Wilkins; Brian J Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi; A J J Raassen
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：70, Number：2, Mar. 2018, [Reviewed]
Oxford University Press (OUP), Scientific journal
DOI：https://doi.org/10.1093/pasj/psx156
DOI ID：10.1093/pasj/psx156, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000432287600004 - The Transition from Young to Middle-aged Supernova Remnants: Thermal and Nonthermal Aspects of SNR N132D
Aya Bamba; Yutaka Ohira; Ryo Yamazaki; Makoto Sawada; Yukikatsu Terada; Katsuji Koyama; Eric D. Miller; Hiroya Yamaguchi; Satoru Katsuda; Masayoshi Nobukawa; Kumiko K. Nobukawa
Astrophysical Journal, Volume：854, Number：1, Feb. 2018, [Reviewed]
Supernova remnants (SNRs) are the primary candidate of Galactic cosmic-ray accelerators. It is still an open issue when and how young SNRs, which typically exhibit strong synchrotron X-rays and GeV and TeV gamma rays, undergo the state transition to middle-aged SNRs dominated by thermal X-rays and GeV gamma rays. SNR N132D in the Large Magellanic Cloud is an ideal target to study such a transition, exhibiting bright X-rays and gamma rays, and with an expected age of ∼2500 years. In this paper we present results of NuSTAR and Suzaku spectroscopy. We reveal that N132D has a nearly equilibrium plasma with a temperature of >
5 keV or a recombining plasma with a lower temperature (∼1.5 keV) and a recombining timescale (net) of cm-3s. Together with the center-filled morphology observed in the iron K line image, our results suggest that N132D is now at the transition stage from being a young SNR to being middle-aged. We have constrained the tight upper limit of nonthermal X-rays. Bright gamma rays compared to faint nonthermal X-rays suggest that the gamma rays are hadronic in origin. The spectral energy distribution from radio to gamma rays shows a proton cutoff energy of ∼30 TeV. These facts confirm that N132D is undergoing the transition from a young to a middle-aged SNR. The large thermal energy of erg and accelerated proton energy of erg suggest the supernova explosion might have been very energetic.
Institute of Physics Publishing, English, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/aaa5a0
DOI ID：10.3847/1538-4357/aaa5a0, ISSN：1538-4357, ORCID：41613333, SCOPUS ID：85042371955, Web of Science ID：WOS:000425000100011 - Supermirror design for Hard X-Ray Telescopes on-board Hitomi (ASTRO-H)
Tamura, Keisuke; Kunieda, Hideyo; Miyata, Yusuke; Okajima, Takashi; Miyazawa, Takuya; Furuzawa, Akihiro; Awaki, Hisamitsu; Haba, Yoshito; Ishibashi, Kazunori; Ishida, Manabu; Maeda, Yoshitomo; MorI, Hideyuki; Tawara, Yuzuru; Yamauchi, Shigeo; Uesugi, Kentaro; Suzuki, Yoshio; HXT Team
Journal of Astronomical Telescopes, Instruments, and Systems, Jan. 2018
We designed depth-graded multilayers, so-called supermirrors, with platinum/carbon (Pt/C) layer pairs for the Hard X-Ray Telescope (HXT) that was on-board the sixth Japanese X-Ray Astronomy Satellite Hitomi (ASTRO-H). The HXT has multinested thin foil optics, and the grazing angles of the x-ray mirrors are 0.07 to 0.27 deg. Supermirrors for HXTs are designed to provide a broad energy response (up to 80 keV) for astronomical requests. Under practical boundary conditions, we establish a block method applying empirical rules to maximize the integrated reflectivity. We fabricated Pt/C supermirrors using a DC magnetron sputtering system. The reflectivity of the mirrors was measured in a synchrotron radiation facility, SPring-8. We describe the design method for the supermirrors and our results....
Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.4.1.011209
DOI ID：10.1117/1.JATIS.4.1.011209, ORCID：101134405, Bibcode：2018JATIS...4a1209T - On-ground calibration of the Hitomi Hard X-ray Telescopes
Mori, Hideyuki; Miyazawa, Takuya; Awaki, Hisamitsu; Matsumoto, Hironori; Babazaki, Yasunori; Bandai, Ayako; Demoto, Tadatsugu; Furuzawa, Akihiro; Haba, Yoshito; Hayashi, Takayuki; Iizuka, Ryo; Ishibashi, Kazunori; Ishida, Manabu; Ishida, Naoki; Itoh, Masayuki; Iwase, Toshihiro; Kato, Hiroyoshi; Kobayashi, Hiroaki; Kosaka, Tatsuro; Kunieda, Hideyo; Kurashima, Shou; Kurihara, Daichi; Kuroda, Yuuji; Maeda, Yoshitomo; Meshino, Yoshifumi; Mitsuishi, Ikuyuki; Miyata, Yuusuke; Nagano, Housei; Namba, Yoshiharu; Ogasaka, Yasushi; Ogi, Keiji; Okajima, Takashi; Saji, Shigetaka; Shimasaki, Fumiya; Sato, Takuro; Sato, Toshiki; Shima, Naotsugu; Sugita, Satoshi; Suzuki, Yoshio; Tachibana, Kenji; Tachibana, Sasagu; Takizawa, Shun'ya; Tamura, Keisuke; Tawara, Yuzuru; Tomikawa, Kazuki; Torii, Tatsuharu; Uesugi, Kentaro; Yamashita, Koujun; Yamauchi, Shigeo
Journal of Astronomical Telescopes, Instruments, and Systems, Jan. 2018
We present x-ray characteristics of the Hard X-ray Telescopes (HXTs) on board the Hitomi (ASTRO-H) satellite. Measurements were conducted at the SPring-8 BL20B2 beamline and the ISAS/JAXA 27-m beamline. The angular resolution defined by a half-power diameter was 1.9‧ (HXT-1) and 2.1‧ (HXT-2) at 8 keV, 1.9‧ at 30 keV, and 1.8‧ at 50 keV. The effective area was found to be 620 cm2 at 8 keV, 178 cm2 at 30 keV, and 82 cm2 at 50 keV per mirror module. Although the angular resolutions were slightly worse than the requirement (1.7‧), the effective areas sufficiently exceeded the requirements of 150 cm2 at 30 keV and 55 cm2 at 50 keV. The off-axis measurements of the effective areas resulted in the field of view being 6.1‧ at 50 keV, 7.7‧ at 30 keV, and 9.7‧ at 8 keV in diameter. We confirmed that the main component of the stray x-ray light was significantly reduced by mounting the precollimator as designed. Detailed analysis of the data revealed that the angular resolution was degraded mainly by figure errors of mirror foils, and the angular resolution is completely explained by the figure errors, positioning errors of the foils, and conical approximation of the foil shape. We found that the effective areas were ∼80% of the designed values below 40 keV, whereas they steeply decline above 40 keV and become only ∼50%. We investigated this abrupt decline and found that neither the error of the multilayer design nor the errors of the incident angles induced by the positioning errors of the foils can be the cause. The reflection profile of each foil pair from the defocused image strongly suggests that the figure errors of the foils probably bring about the reduction in the effective areas at higher energies....
Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.4.1.011210
DOI ID：10.1117/1.JATIS.4.1.011210, ORCID：101134400, Bibcode：2018JATIS...4a1210M - Vibration isolation system for cryocoolers of soft x-ray spectrometer on-board ASTRO-H (Hitomi)
Yoh Takei; Susumu Yasuda; Kosei Ishimura; Naoko Iwata; Atsushi Okamoto; Yoichi Sato; Mina Ogawa; Makoto Sawada; Taro Kawano; Shingo Obara; Chikara Natsukari; Atsushi Wada; Shinya Yamada; Ryuichi Fujimoto; Motohide Kokubun; Noriko Y. Yamasaki; Hiroyuki Sugita; Kenji Minesugi; Yasuo Nakamura; Kazuhisa Mitsuda; Tadayuki Takahashi; Seiji Yoshida; Shoji Tsunematsu; Kenichi Kanao; Katsuhiro Narasaki; Kiyomi Otsuka; F. Scott Porter; Caroline A. Kilbourne; Meng P. Chiao; Megan E. Eckart; Gary A. Sneiderman; James T. Pontius; Dan McCammon; Paul Wilke; John Basile
JOURNAL OF ASTRONOMICAL TELESCOPES INSTRUMENTS AND SYSTEMS, Volume：4, Number：1, Jan. 2018
The soft x-ray spectrometer (SXS) onboard ASTRO-H (named Hitomi after launch) is a microcalorimeter-type spectrometer, installed in a dewar to be cooled at 50 mK. The energy resolution of the SXS engineering model suffered from microvibration from cryocoolers mounted on the dewar. This is mitigated for the flight model (FM) by introducing vibration isolation systems between the cryocoolers and the dewar. The detector performance of the FM was verified before launch of the spacecraft in both ambient condition and thermal-vacuum condition, showing no detectable degradation in energy resolution. The in-orbit detector spectral performance and cryocooler cooling performance were also consistent with that on ground, indicating that the cryocoolers were not damaged by launch environment. The design and performance of the vibration isolation system along with the mechanism of how the microvibration could degrade the cryogenic detector is shown. Lessons learned from the development to mitigate unexpected issues are also described. (c) The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License.
SPIE-SOC PHOTO-OPTICAL INSTRUMENTATION ENGINEERS, English, Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.4.1.011216
DOI ID：10.1117/1.JATIS.4.1.011216, ISSN：2329-4124, eISSN：2329-4221, Web of Science ID：WOS:000429569000022 - CTA Report 134：Study of the aging effect of the photomultiplier tube for the CTA Large Size Telescope
Sakurai S.; Kataoka J.; Katagiri H.; Kimura S.; Kushida J.; Kubo H.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Sawada M.; Nagayoshi T.; Sunada Y.; Takahashi M.; Tsujimoto S.; Teshima M.; Terada Y.; Tokanai F.; Nakajima D.; Nakamori T.; Nishijima K.; Nishiyama G.; Inada T.; Nozaki S.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Yoshida T.; Hadasch D.; Mazin D.; Inome Y.; the CTA-Japan consortium; Iwamura Y.; Ohoka H.; Okumura A.; Okazaki N.; Orito R.
Meeting Abstracts of the Physical Society of Japan, Volume：73, First page：417, Last page：417, 2018
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.73.1.0_417
DOI ID：10.11316/jpsgaiyo.73.1.0_417, CiNii Articles ID：130007648543 - CTA Report 133: Integration test of the focal plane camera for the first CTA Large Sized Telescope
Nozaki S.; Katagiri H.; Kato S.; Kimura S.; Kushida J.; Kubo H.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Sakurai S.; Inada T.; Sawada M.; Sunada Y.; Takahashi M.; Takahara H.; Tanaka M.; Tsujimoto S.; Teshima M.; Terada Y.; Okanai F.; NakajimaT D.; Inome Y.; Nakamori T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Iwamura Y.; Yoshida T.; Hadasch D.; Mazin D.; the CTA-Japan consortium; Ikeno M.; Uchida T.; Ohoka H.; Okumura A.; Okazaki N.; Orito R.; Kataoka J.
Meeting Abstracts of the Physical Society of Japan, Volume：73, First page：416, Last page：416, 2018
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.73.1.0_416
DOI ID：10.11316/jpsgaiyo.73.1.0_416, CiNii Articles ID：130007648544 - CTA Report 142: Integration test of the focal plane camera for the first CTA Large Sized Telescope(II)
Sunada Y.; Katagiri H.; Kushida J.; Kimura S.; Kubo H.; Gunji S.; Koyama S.; Saito T.; Sakurai S.; Sawada M.; Suzuki M.; Inada T.; Takahashi M.; Takahara H.; Tanaka M.; Tujimoto S.; Teshima M.; Terada Y.; Tokanai F.; Nakajima D.; Nakamori K.; Nagayoshi T.; Inome Y.; Nishijima K.; Nishiyama G.; Nozaki S.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Yoshida T.; Iwamura Y.; Hadasch Daniela; Mazin Daniel; the CTA-Japan consortium; Ohoka H.; Okazaki N.; Okumura A.; Orito R.; Kataoka J.
Meeting Abstracts of the Physical Society of Japan, Volume：73, First page：191, Last page：191, 2018
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.73.2.0_191
DOI ID：10.11316/jpsgaiyo.73.2.0_191, CiNii Articles ID：130007735618 - Long-term test of a stacked CdTe mini-HXI setup
Daniel Maier; Benoit Horeau; Philippe Laurent; Olivier Limousin; Diana Renaud; Madoka Kawaharada; Motohide Kokubun; Goro Sato; Tadayuki Takahashi; Shin Watanabe; Kazuhiro Nakazawa; Cesar Boatella Polo
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 2018, [Reviewed]
This work presents a long-term operation of two stacked CdTe double sided strip detectors that are comparable with the CdTe detectors onboard Hitomi's HXI. The goal of this test is to study the evolution of the spectroscopic performance of the detectors during a one year operation cycle which resembles the in-orbit operation cycle of Hitomi HXI. Crystal defects inside CdTe cause a degradation of the spectroscopic performance (polarization effect) of the crystal which is becoming worse during detector operation. In order to prevent crystal polarization, the detectors are reset (switch-off of the depletion voltage) once a day. Our main investigation was to study if a long-term degradation can occur as a result of incomplete depolarization during the reset. We present the hardware setup and the analytical steps that were used to investigate the detector stability during each day and over the whole testing period. For the anode signals our results show at 60 keV: a daily line drift of (−2.8±0.7) eV/ks while the long-term drift is (−1.5±1.2) eV/day. The degradation of the energy resolution is measured to be (+2.4±0.3) eV/ks FWHM and the loss of efficiency is (−0.29±0.02) %/ks.
Elsevier B.V., English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2017.11.035
DOI ID：10.1016/j.nima.2017.11.035, ISSN：0168-9002, SCOPUS ID：85044765263 - Time assignment system and its performance aboard the Hitomi satellite
Yukikatsu Terada; Sunao Yamaguchi; Shigenobu Sugimoto; Taku Inoue; Souhei Nakaya; Maika Murakami; Seiya Yabe; Kenya Oshimizu; Mina Ogawa; Tadayasu Dotani; Yoshitaka Ishisaki; Kazuyo Mizushima; Takashi Kominato; Hiroaki Mine; Hiroki Hihara; Kaori Iwase; Tomomi Kouzu; Makoto S. Tashiro; Chikara Natsukari; Masanobu Ozaki; Motohide Kokubun; Tadayuki Takahashi; Satoko Kawakami; Masaru Kasahara; Susumu Kumagai; Lorella Angelini; Michael Witthoeft
Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：1, Jan. 2018, [Reviewed]
Fast timing capability in x-ray observation of astrophysical objects is one of the key properties for the ASTRO-H (Hitomi) mission. Absolute timing accuracies of 350 or 35 μs are required to achieve nominal scientific goals or to study fast variabilities of specific sources. The satellite carries a GPS receiver to obtain accurate time information, which is distributed from the central onboard computer through the large and complex SpaceWire network. The details of the time system on the hardware and software design are described. In the distribution of the time information, the propagation delays and jitters affect the timing accuracy. Six other items identified within the timing system will also contribute to absolute time error. These error items have been measured and checked on ground to ensure the time error budgets meet the mission requirements. The overall timing performance in combination with hardware performance, software algorithm, and the orbital determination accuracies, etc. under nominal conditions satisfies the mission requirements of 35 μs. This work demonstrates key points for space-use instruments in hardware and software designs and calibration measurements for fine timing accuracy on the order of microseconds for midsized satellites using the SpaceWire (IEEE1355) network.
SPIE, English, Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.4.1.011206
DOI ID：10.1117/1.JATIS.4.1.011206, ISSN：2329-4221, SCOPUS ID：85040443094, Web of Science ID：WOS:000429569000012 - In-flight performance of pulse-processing system of the ASTRO-H/Hitomi soft x-ray spectrometer
Yoshitaka Ishisaki; Shinya Yamada; Hiromi Seta; Makoto S. Tashiro; Sawako Takeda; Yukikatsu Terada; Yuka Kato; Masahiro Tsujimoto; Shu Koyama; Kazuhisa Mitsuda; Makoto Sawada; Kevin R. Boyce; Meng P. Chiao; Tomomi Watanabe; Maurice A. Leutenegger; Megan E. Eckart; Frederick Scott Porter; Caroline Anne Kilbourne
Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：1, Jan. 2018, [Reviewed]
We summarize results of the initial in-orbit performance of the pulse shape processor (PSP) of the soft x-ray spectrometer instrument onboard ASTRO-H (Hitomi). Event formats, kind of telemetry, and the pulse-processing parameters are described, and the parameter settings in orbit are listed. The PSP was powered-on 2 days after launch, and the event threshold was lowered in orbit. The PSP worked fine in orbit, and there was neither memory error nor SpaceWire communication error until the break-up of spacecraft. Time assignment, electrical crosstalk, and the event screening criteria are studied. It is confirmed that the event processing rate at 100% central processing unit load is ∼200 c / s / array, compliant with the requirement on the PSP.
SPIE, English, Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.4.1.011217
DOI ID：10.1117/1.JATIS.4.1.011217, ISSN：2329-4221, SCOPUS ID：85042850963, Web of Science ID：WOS:000429569000023 - Astro-H/Hitomi data analysis, processing, and archive
Lorella Angelini; Yukikatsu Terada; Michael Dutka; Joseph Eggen; Ilana Harrus; Robert S. Hill; Hans Krimm; Michael Loewenstein; Eric D. Miller; Masayoshi Nobukawa; Kristin Rutkowski; Andrew Sargent; Makoto Sawada; Hiromitsu Takahashi; Hiroya Yamaguchi; Tahir Yaqoob; Michael Witthoeft
Journal of Astronomical Telescopes, Instruments, and Systems, Volume：4, Number：1, Jan. 2018, [Reviewed]
Astro-H is the X-ray/gamma-ray mission led by Japan with international participation, launched on February 17, 2016. Soon after launch, Astro-H was renamed Hitomi. The payload consists of four different instruments (SXS, SXI, HXI, and SGD) that operate simultaneously to cover the energy range from 0.3 keV up to 600 keV. On March 27, 2016, JAXA lost contact with the satellite and, on April 28, they announced the cessation of the efforts to restore mission operations. Hitomi collected about one month's worth of data with its instruments. This paper presents the analysis software and the data processing pipeline created to calibrate and analyze the Hitomi science data, along with the plan for the archive. These activities have been a collaborative effort shared between scientists and software engineers working in several institutes in Japan and United States.
SPIE, English, Scientific journal
DOI：https://doi.org/10.1117/1.JATIS.4.1.011207
DOI ID：10.1117/1.JATIS.4.1.011207, ISSN：2329-4221, SCOPUS ID：85041171567, Web of Science ID：WOS:000429569000013 - Concept of X-ray Astronomy Recovery Mission
Makoto Tashiro; Hironori Maejima; Kenichi Toda; Richard Kelley; Lillian Reichenthal; James Lobell; Robert Petre; Matteo Guainazzi; Elisa Costantini; Mark Edison; Ryuichi Fujimoto; Martin Grim; Kiyoshi Hayashida; Jan-Willem den Herder; Yoshitaka Ishisaki; Stephane Paltani; Kyoko Matsushita; Koji Mori; Gary Sneiderman; Yoh Takei; Yukikatsu Terada; Hiroshi Tomida; Hiroki Akamatsu; Lorella Angelini; Yoshitaka Arai; Hisamitsu Awaki; Iurii Babyk; Aya Bamba; Peter Barfknecht; Kim Barnstable; Thomas Bialas; Branimir Blagojevic; Joseph Bonafede; Clifford Brambora; Laura Brenneman; Greg Brown; Kimberly Brown; Laura Burns; Edgar Canavan; Tim Carnahan; Meng Chiao; Brian Comber; Lia Corrales; Cor de Vries; Johannes Dercksen; Maria Diaz-Trigo; Tyrone Dillard; Michael DiPirro; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan Eckart; Teruaki Enoto; Yuichiro Ezoe; Carlo Ferrigno; Yutaka Fujita; Yasushi Fukazawa; Akihiro Furuzawa; Luigi Gallo; Steve Graham; Liyi Gu; Kohichi Hagino; Kenji Hamaguchi; Isamu Hatsukade; Dean Hawes; Takayuki Hayashi; Cailey Hegarty; Natalie Hell; Junko Hiraga; Edmund Hodges-Kluck; Matt Holland; Ann Hornschemeier; Akio Hoshino; Yuto Ichinohe; Ryo Iizuka; Kazunori Ishibashi; Manabu Ishida; Kumi Ishikawa; Kosei Ishimura; Bryan James; Timothy Kallman; Erin Kara; Satoru Katsuda; Steven Kenyon; Caroline Kilbourne; Mark Kimball; Takao Kitaguchi; Shunji Kitamoto; Shogo Kobayashi; Takayoshi Kohmura; Shu Koyama; Aya Kubota; Maurice Leutenegger; Tom Lockard; Mike Loewenstein; Yoshitomo Maeda; Lynette Marbley; Maxim Markevitch; Connor Martz; Hironori Matsumoto; Keiichi Matsuzaki; Dan McCammon; Brian McNamara; Joseph Miko; Eric Miller; Jon Miller; Kenji Minesugi; Ikuyuki Mitsuishi; Tsunefumi Mizuno; Hideyuki Mori; Koji Mukai; Hiroshi Murakami; Richard Mushotzky; Hiroshi Nakajima; Hideto Nakamura; Shinya Nakashima; Kazuhiro Nakazawa; Chikara Natsukari; Kenichiro Nigo; Yusuke Nishioka; Kumiko Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Mina Ogawa; Takaya Ohashi; Masahiro Ohno; Masayuki Ohta; Takashi Okajima; Atsushi Okamoto; Michitaka Onizuka; Naomi Ota; Masanobu Ozaki; Paul Plucinsky; F. Scott Porter; Katja Pottschmidt; Kosuke Sato; Rie Sato; Makoto Sawada; Hiromi Seta; Ken Shelton; Yasuko Shibano; Maki Shida; Megumi Shidatsu; Peter Shirron; Aurora Simionescu; Randall Smith; Kazunori Someya; Yang Soong; Yasuharu Sugawara; Andy Szymkowiak; Hiromitsu Takahashi; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yuichi Terashima; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yoshihiro Ueda; Shinichiro Uno; Thomas Walsh; Shin Watanabe; Brian Williams; Rob Wolfs; Michael Wright; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Yamasaki; Shigeo Yamauchi; Makoto Yamauchi; Keiichi Yanagase; Tahir Yaqoob; Susumu Yasuda; Nasa Yoshioka; Jaime Zabala; Irina Zhuravleva
SPACE TELESCOPES AND INSTRUMENTATION 2018: ULTRAVIOLET TO GAMMA RAY, Volume：10699, 2018, [Reviewed]
The ASTRO-H mission was designed and developed through an international collaboration of JAXA, NASA, ESA, and the CSA. It was successfully launched on February 17, 2016, and then named Hitomi. During the in-orbit verification phase, the on-board observational instruments functioned as expected. The intricate coolant and refrigeration systems for soft X-ray spectrometer (SXS, a quantum micro-calorimeter) and soft X-ray imager (SXI, an X-ray CCD) also functioned as expected. However, on March 26, 2016, operations were prematurely terminated by a series of abnormal events and mishaps triggered by the attitude control system. These errors led to a fatal event: the loss of the solar panels on the Hitomi mission. The X-ray Astronomy Recovery Mission (or, XARM) is proposed to regain the key scientific advances anticipated by the international collaboration behind Hitomi. XARM will recover this science in the shortest time possible by focusing on one of the main science goals of Hitomi, "Resolving astrophysical problems by precise high-resolution X-ray spectroscopy".(1) This decision was reached after evaluating the performance of the instruments aboard Hitomi and the mission's initial scientific results, and considering the landscape of planned international X-ray astrophysics missions in 2020's and 2030's.Hitomi opened the door to high-resolution spectroscopy in the X-ray universe. It revealed a number of discrepancies between new observational results and prior theoretical predictions. Yet, the resolution pioneered by Hitomi is also the key to answering these and other fundamental questions. The high spectral resolution realized by XARM will not offer mere refinements; rather, it will enable qualitative leaps in astrophysics and plasma physics. XARM has therefore been given a broad scientific charge: "Revealing material circulation and energy transfer in cosmic plasmas and elucidating evolution of cosmic structures and objects". To fulfill this charge, four categories of science objectives that were defined for Hitomi will also be pursued by XARM; these include (1) Structure formation of the Universe and evolution of clusters of galaxies; (2) Circulation history of baryonic matters in the Universe; (3) Transport and circulation of energy in the Universe; (4) New science with unprecedented high resolution X-ray spectroscopy. In order to achieve these scientific objectives, XARM will carry a 6 x 6 pixelized X-ray micro-calorimeter on the focal plane of an X-ray mirror assembly, and an aligned X-ray CCD camera covering the same energy band and a wider field of view. This paper introduces the science objectives, mission concept, and observing plan of XARM.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2309455
DOI ID：10.1117/12.2309455, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000452819200049 - Design and development of a polarization modulator unit based on a continuous rotating half-wave plate for LiteBIRD
Sakurai Yuki; Matsumura Tomotake; Katayama Nobuhiko; Imada Hiroaki; Komatsu Kunimoto; Kanai Hiroaki; Takaku Ryota; Shugiyama Shinya; Ghigna Tommaso; Iida Teruhito; Sugai Hajime; Ohsaki Hiroyuki; Terao Yutaka; Shimomura Toshiki; Konishi Kuniaki; Sakurai Haruyuki; Yumoto Junji; Maki Muneyoshi; Suzuki Junichi; Ishino Hirokazu; Nakamura Shogo; Kusaka Akito; Hill Charles; Hazumi Masashi; Kataza Hirokazu; Utsunomiya Shin; Yamamoto Ryo; Tashiro Makoto; Terada Yukikatsu
MILLIMETER, SUBMILLIMETER, AND FAR-INFRARED DETECTORS AND INSTRUMENTATION FOR ASTRONOMY IX, Volume：10708, 2018, [Reviewed]
DOI：https://doi.org/10.1117/12.2312391
DOI ID：10.1117/12.2312391, ISSN：0277-786X, Web of Science ID：WOS:000451719300008 - Solar abundance ratios of the iron-peak elements in the Perseus cluster
Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W. Allen; Lorella Angelini; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall W. Bautz; Roger Blandford; Laura W. Brenneman; Gregory V. Brown; Esra Bulbul; Edward M. Cackett; Maria Chernyakova; Meng P. Chiao; Paolo S. Coppi; Elisa Costantini; Jelle De Plaa; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan E. Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C. Fabian; Carlo Ferrigno; Adam R. Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi C. Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana M. Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko S. Hiraga; Ann Hornschemeier; Akio Hoshino; John P. Hughes; Yuto Ichinohe; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masachika Iwai; Jelle Kaastra; Tim Kallman; Tsuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Nobuyuki Kawai; Richard L. Kelley; Caroline A. Kilbourne; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Katsuji Koyama; Shu Koyama; Peter Kretschmar; Hans A. Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Shiu-Hang Lee; Maurice A. Leutenegger; Olivier Limousine; Michael Loewenstein; Knox S. Long; David Lumb; Greg Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian R. McNamara; Missagh Mehdipour; Eric D. Miller; Jon M. Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Koji Mukai; Hiroshi Murakami; Richard F. Mushotzky; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Shinya Nakashima; Kazuhiro Nakazawa; Kumiko K. Nobukawa; Masayoshi Nobukawa; Hirofumi Noda; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; StPhane Paltani; Robert Petre; Ciro Pinto; Frederick S. Porter; Katja Pottschmidt; Christopher S. Reynolds; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Toru Sasaki; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter J. Serlemitsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall K. Smith; Yang Soong; Lukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin'ichiro Takeda; Yoh Takei; Toru Tamagawa; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki T. Tanaka; Makoto S. Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Go Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shin'ichiro Uno; C. Megan Urry; Eugenio Ursino; Cor P. de Vries; Shin Watanabe; Norbert Werner; Daniel R. Wik; Dan R. Wilkins; Brian J. Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y. Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Irina Zhuravleva; Abderahmen Zoghbi
NATURE, Volume：551, Number：7681, First page：478, Last page：+, Nov. 2017, [Reviewed]
The metal abundance of the hot plasma that permeates galaxy clusters represents the accumulation of heavy elements produced by billions of supernovae(1). Therefore, X-ray spectroscopy of the intracluster medium provides an opportunity to investigate the nature of supernova explosions integrated over cosmic time. In particular, the abundance of the iron-peak elements (chromium, manganese, iron and nickel) is key to understanding how the progenitors of typical type Ia supernovae evolve and explode(2-6). Recent X-ray studies of the intracluster medium found that the abundance ratios of these elements differ substantially from those seen in the Sun(7-11), suggesting differences between the nature of type Ia supernovae in the clusters and in the Milky Way. However, because the K-shell transition lines of chromium and manganese are weak and those of iron and nickel are very close in photon energy, highresolution spectroscopy is required for an accurate determination of the abundances of these elements. Here we report observations of the Perseus cluster, with statistically significant detections of the resonance emission from chromium, manganese and nickel. Our measurements, combined with the latest atomic models, reveal that these elements have near-solar abundance ratios with respect to iron, in contrast to previous claims. Comparison between our results and modern nucleosynthesis calculations(12-14) disfavours the hypothesis that type Ia supernova progenitors are exclusively white dwarfs with masses well below the Chandrasekhar limit (about 1.4 times the mass of the Sun). The observed abundance pattern of the iron-peak elements can be explained by taking into account a combination of near-and sub-Chandrasekhar-mass type Ia supernova systems, adding to the mounting evidence that both progenitor types make a substantial contribution to cosmic chemical enrichment(5,15,16).
NATURE PUBLISHING GROUP, English, Scientific journal
DOI：https://doi.org/10.1038/nature24301
DOI ID：10.1038/nature24301, ISSN：0028-0836, eISSN：1476-4687, Web of Science ID：WOS:000416043700039 - Summary of the 12th IACHEC Meeting
Forster, K.; Grant, C. E.; Guainazzi, M.; Kashyap, V.; Marshall, H. L.; Miller, E. D.; Natalucci, L.; Nevalainen, J.; Plucinsky, P. P.; Terada, Y.
Aug. 2017
We summarize the outcome of the 12th meeting of the International Astronomical Consortium for High Energy Calibration (IACHEC), held at the UCLA conference center in Lake Arrowhead (California) in March 2017. 56 scientists directly involved in the calibration of operational and future high-energy missions gathered during 3.5 days to discuss the status of the X-ray payload inter-calibration, as well as possible ways to improve it. The "Thermal Supernovas Remnant" (SNR) Working Group presented a recently published paper on 1E0102.2-7219 as a calibration standard in the 0.5-1.0 keV band. A new method to measure the high-energy spectrum of the Crab Nebula and pulsar with NuSTAR without using its optics may yield a new absolute flux standard in the 3-7 keV band. A new ACIS contamination model - released with CALDB version 4.7.3 - leads to a significant improvement in modeling the spectral, spatial, and temporal properties of the contaminant. The first calibration results of the scientific payload on board Hitomi confirm the excellent performance of the instruments before the spacecraft operation problems leading to its loss. Finally, the meeting discussed extensively a novel statistic approach to formally identify in which direction the effective areas of different instruments would need to be changed to bring them into concordance. This method could inform future further calibration efforts....
arXiv e-prints
ORCID：101133982, arXiv ID：arXiv:1708.01446, Bibcode：2017arXiv170801446F - Suzaku Wide-band All-sky Monitor (WAM) observations of GRBs and SGRs
Kazutaka Yamaoka; Masanori Ohno; Makoto S. Tashiro; Kevin Hurley; Hans A. Krimm; Amy Y. Lien; Norisuke Ohmori; Satoshi Sugita; Yuji Urata; Tetsuya Yasuda; Junichi Enomoto; Takeshi Fujinuma; Yasushi Fukazawa; Yoshitaka Hanabata; Wataru Iwakiri; Takafumi Kawano; Ryuuji Kinoshita; Motohide Kokubun; Kazuo Makishima; Shunsuke Matsuoka; Tsutomu Nagayoshi; Yujin Nakagawa; Souhei Nakaya; Kazuhiro Nakazawa; Yusuke Nishioka; Takanori Sakamoto; Tadayuki Takahashi; Sawako Takeda; Yukikatsu Terada; Seiya Yabe; Makoto Yamauchi; Hiraku Yoshida
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：69, Number：3, Jun. 2017, [Reviewed]
We will review results for gamma-ray bursts (GRBs) and soft gamma repeaters (SGRs), obtained from the Suzaku Wide-band All-sky Monitor (WAM) which operated for about 10 years from 2005 to 2015. The WAM is a BGO (bismuth germanate: Bi4Ge3O12) lateral shield for the Hard X-ray Detector (HXD),used mainly for rejecting its detector background, but it also works as an all-sky monitor for soft gamma-ray transients in the 50-5000 keV range thanks to its large effective area (similar to 600 cm(2) at 1MeV for one detector) and wide field of view (about half of the entire sky). The WAM actually detected more than 1400 GRBs and 300 bursts from SGRs, and this detection number is comparable to that of other GRB-specific instruments. Based on the 10 years of operation, we describe timing and spectral performance for short GRBs, weak GRBs with high redshifts, and time-resolved pulses with good statistics.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/psx026
DOI ID：10.1093/pasj/psx026, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000404642800004 - Prospects for Cherenkov Telescope Array Observations of the Young Supernova Remnant RX J1713.7-3946
F. Acero; R. Aloisio; J. Amans; E. Amato; L. A. Antonelli; C. Aramo; T. Armstrong; F. Arqueros; K. Asano; M. Ashley; M. Backes; C. Balazs; A. Balzer; A. Bamba; M. Barkov; J. A. Barrio; W. Benbow; K. Bernloehr; V. Beshley; C. Bigongiari; A. Biland; A. Bilinsky; E. Bissaldi; J. Biteau; O. Blanch; P. Blasi; J. Blazek; C. Boisson; G. Bonanno; A. Bonardi; C. Bonavolonta; G. Bonnoli; C. Braiding; S. Brau-Nogue; J. Bregeon; A. M. Brown; V. Bugaev; A. Bulgarelli; T. Bulik; M. Burton; A. Burtovoi; G. Busetto; M. Bottcher; R. Cameron; M. Capalbi; A. Caproni; P. Caraveo; R. Carosi; E. Cascone; M. Cerruti; S. Chaty; A. Chen; X. Chen; M. Chernyakova; M. Chikawa; J. Chudoba; J. Cohen-Tanugi; S. Colafrancesco; V. Conforti; J. L. Contreras; A. Costa; G. Cotter; S. Covino; G. Covone; P. Cumani; G. Cusumano; F. D'Ammando; D. D'Urso; M. Daniel; F. Dazzi; A. De Angelis; G. De Cesare; A. De Franco; F. De Frondat; E. M. de Gouveia Dal Pino; C. De Lisio; R. de los Reyes Lopez; B. De Lotto; M. de Naurois; F. De Palma; M. Del Santo; C. Delgado; D. della Volpe; T. Di Girolamo; C. Di Giulio; F. Di Pierro; L. Di Venere; M. Doro; J. Dournaux; D. Dumas; V. Dwarkadas; C. Diaz; J. Ebr; K. Egberts; S. Einecke; D. Elsaesser; S. Eschbach; D. Falceta-Goncalves; G. Fasola; E. Fedorova; A. Fernandez-Barral; G. Ferrand; M. Fesquet; E. Fiandrini; A. Fiasson; M. D. Filipovic; V. Fioretti; L. Font; G. Fontaine; F. J. Franco; L. Freixas Coromina; Y. Fujita; Y. Fukui; S. Funk; A. Forster; A. Gadola; R. Garcia Lopez; M. Garczarczyk; N. Giglietto; F. Giordano; A. Giuliani; J. Glicenstein; R. Gnatyk; P. Goldoni; T. Grabarczyk; R. Graciani; J. Graham; P. Grandi; J. Granot; A. J. Green; S. Griffiths; S. Gunji; H. Hakobyan; S. Hara; T. Hassan; M. Hayashida; M. Heller; J. C. Helo; J. Hinton; B. Hnatyk; J. Huet; M. Huetten; T. B. Humensky; M. Hussein; J. Horandel; Y. Ikeno; T. Inada; Y. Inome; S. Inoue; T. Inoue; Y. Inoue; K. Ioka; M. Iori; J. Jacquemier; P. Janecek; D. Jankowsky; I. Jung; P. Kaaret; H. Katagiri; S. Kimeswenger; S. Kimura; J. Knodlseder; B. Koch; J. Kocot; K. Kohri; N. Komin; Y. Konno; K. Kosack; S. Koyama; M. Kraus; H. Kubo; G. Kukec Mezek; J. Kushida; N. La Palombara; K. Lalik; G. Lamanna; H. Landt; J. Lapington; P. Laporte; S. Lee; J. Lees; J. Lefaucheur; J. -P. Lenain; G. Leto; E. Lindfors; T. Lohse; S. Lombardi; F. Longo; M. Lopez; F. Lucarelli; P. L. Luque-Escamilla; R. Lopez-Coto; M. C. Maccarone; G. Maier; G. Malaguti; D. Mandat; G. Maneva; S. Mangano; A. Marcowith; J. Marti; M. Martinez; G. Martinez; S. Masuda; G. Maurin; N. Maxted; C. Melioli; T. Mineo; N. Mirabal; T. Mizuno; R. Moderski; M. Mohammed; T. Montaruli; A. Moralejo; K. Mori; G. Morlino; A. Morselli; E. Moulin; R. Mukherjee; C. Mundell; H. Muraishi; K. Murase; S. Nagataki; T. Nagayoshi; T. Naito; D. Nakajima; T. Nakamori; R. Nemmen; J. Niemiec; D. Nieto; M. Nievas-Rosillo; M. Nikolajuk; K. Nishijima; K. Noda; L. Nogues; D. Nosek; B. Novosyadlyj; S. Nozaki; Y. Ohira; M. Ohishi; S. Ohm; A. Okumura; R. A. Ong; R. Orito; A. Orlati; M. Ostrowski; I. Oya; M. Padovani; J. Palacio; M. Palatka; J. M. Paredes; S. Pavy; A. Pe'er; M. Persic; P. Petrucci; O. Petruk; A. Pisarski; M. Pohl; A. Porcelli; E. Prandini; J. Prast; G. Principe; M. Prouza; E. Pueschel; G. Puelhofer; A. Quirrenbach; M. Rameez; O. Reimer; M. Renaud; M. Ribo; J. Rico; V. Rizi; J. Rodriguez; G. Rodriguez Fernandez; J. J. Rodriguez Vazquez; P. Romano; G. Romeo; J. Rosado; J. Rousselle; G. Rowell; B. Rudak; I. Sadeh; S. Safi-Harb; T. Saito; N. Sakaki; D. Sanchez; P. Sangiorgi; H. Sano; M. Santander; S. Sarkar; M. Sawada; E. J. Schioppa; H. Schoorlemmer; P. Schovanek; F. Schussler; O. Sergijenko; M. Servillat; A. Shalchi; R. C. Shellard; H. Siejkowski; A. Sillanpaa; D. Simone; V. Sliusar; H. Sol; S. Stanic; R. Starling; L. Stawarz; S. Stefanik; M. Stephan; T. Stolarczyk; M. Szanecki; T. Szepieniec; G. Tagliaferri; H. Tajima; M. Takahashi; J. Takeda; M. Tanaka; S. Tanaka; L. A. Tejedor; I. Telezhinsky; P. Temnikov; Y. Terada; D. Tescaro; M. Teshima; V. Testa; S. Thoudam; F. Tokanai; D. F. Torres; E. Torresi; G. Tosti; C. Townsley; P. Travnicek; C. Trichard; M. Trifoglio; S. Tsujimoto; V. Vagelli; P. Vallania; L. Valore; W. van Driel; C. van Eldik; J. Vandenbroucke; V. Vassiliev; M. Vecchi; S. Vercellone; S. Vergani; C. Vigorito; S. Vorobiov; M. Vrastil; M. L. Vazquez Acosta; S. J. Wagner; R. Wagner; S. P. Wakely; R. Walter; J. E. Ward; J. J. Watson; A. Weinstein; M. White; R. White; A. Wierzcholska; P. Wilcox; D. A. Williams; R. Wischnewski; P. Wojcik; T. Yamamoto; H. Yamamoto; R. Yamazaki; S. Yanagita; L. Yang; T. Yoshida; M. Yoshida; S. Yoshiike; T. Yoshikoshi; M. Zacharias; L. Zampieri; R. Zanin; M. Zavrtanik; D. Zavrtanik; A. Zdziarski; A. Zech; H. Zechlin; V. Zhdanov; A. Ziegler; J. Zorn
ASTROPHYSICAL JOURNAL, Volume：840, Number：2, First page：74, May 2017, [Reviewed]
We perform simulations for future Cherenkov Telescope Array (CTA) observations of RX J1713.7-3946, a young supernova remnant (SNR) and one of the brightest sources ever discovered in very high energy (VHE) gamma rays. Special attention is paid to exploring possible spatial (anti) correlations of gamma rays with emission at other wavelengths, in particular X-rays and CO/H I emission. We present a series of simulated images of RX J1713.7-3946 for CTA based on a set of observationally motivated models for the gamma-ray emission. In these models, VHE gamma rays produced by high-energy electrons are assumed to trace the nonthermal X-ray emission observed by XMM-Newton, whereas those originating from relativistic protons delineate the local gas distributions. The local atomic and molecular gas distributions are deduced by the NANTEN team from CO and H I observations. Our primary goal is to show how one can distinguish the emission mechanism(s) of the gamma rays (i.e., hadronic versus leptonic, or a mixture of the two) through information provided by their spatial distribution, spectra, and time variation. This work is the first attempt to quantitatively evaluate the capabilities of CTA to achieve various proposed scientific goals by observing this important cosmic particle accelerator.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/aa6d67
DOI ID：10.3847/1538-4357/aa6d67, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000403228100003 - Hitomi Constraints on the 3.5 keV Line in the Perseus Galaxy Cluster
F. A. Aharonian; H. Akamatsu; F. Akimoto; S. W. Allen; L. Angelini; K. A. Arnaud; M. Audard; H. Awaki; M. Axelsson; A. Bamba; M. W. Bautz; R. D. Blandford; E. Bulbul; L. W. Brenneman; G. V. Brown; E. M. Cackett; M. Chernyakova; M. P. Chiao; P. Coppi; E. Costantini; J. de Plaa; J. -W. den Herder; C. Done; T. Dotani; K. Ebisawa; M. E. Eckart; T. Enoto; Y. Ezoe; A. C. Fabian; C. Ferrigno; A. R. Foster; R. Fujimoto; Y. Fukazawa; A. Furuzawa; M. Galeazzi; L. C. Gallo; P. Gandhi; M. Giustini; A. Goldwurm; L. Gu; M. Guainazzi; Y. Haba; K. Hagino; K. Hamaguchi; I. Harrus; I. Hatsukade; K. Hayashi; T. Hayashi; K. Hayashida; J. Hiraga; A. E. Hornschemeier; A. Hoshino; J. P. Hughes; Y. Ichinohe; R. Iizuka; H. Inoue; S. Inoue; Y. Inoue; K. Ishibashi; M. Ishida; K. Ishikawa; Y. Ishisaki; M. Itoh; M. Iwai; N. Iyomoto; J. S. Kaastra; T. Kallman; T. Kamae; E. Kara; J. Kataoka; S. Katsuda; J. Katsuta; M. Kawaharada; N. Kawai; R. L. Kelley; D. Khangulyan; C. A. Kilbourne; A. L. King; T. Kitaguchi; S. Kitamoto; T. Kitayama; T. Kohmura; M. Kokubun; S. Koyama; K. Koyama; P. Kretschmar; H. A. Krimm; A. Kubota; H. Kunieda; P. Laurent; F. Lebrun; S. -H. Lee; M. A. Leutenegger; O. Limousin; M. Loewenstein; K. S. Long; D. H. Lumb; G. M. Madejski; Y. Maeda; D. Maier; K. Makishima; M. Markevitch; H. Matsumoto; K. Matsushita; D. McCammon; B. R. McNamara; M. Mehdipour; E. D. Miller; J. M. Miller; S. Mineshige; K. Mitsuda; I. Mitsuishi; T. Miyazawa; T. Mizuno; H. Mori; K. Mori; H. Moseley; K. Mukai; H. Murakami; T. Murakami; R. F. Mushotzky; T. Nakagawa; H. Nakajima; T. Nakamori; T. Nakano; S. Nakashima; K. Nakazawa; K. Nobukawa; M. Nobukawa; H. Noda; M. Nomachi; S. L. O'Dell; H. Odaka; T. Ohashi; M. Ohno; T. Okajima; N. Ota; M. Ozaki; F. Paerels; S. Paltani; A. Parmar; R. Petre; C. Pinto; M. Pohl; F. S. Porter; K. Pottschmidt; B. D. Ramsey; C. S. Reynolds; H. R. Russell; S. Safi-Harb; S. Saito; K. Sakai; H. Sameshima; T. Sasaki; G. Sato; K. Sato; R. Sato; M. Sawada; N. Schartel; P. J. Serlemitsos; H. Seta; M. Shidatsu; A. Simionescu; R. K. Smith; Y. Soong; L. Stawarz; Y. Sugawara; S. Sugita; A. E. Szymkowiak; H. Tajima; H. Takahashi; T. Takahashi; S. Takeda; Y. Takei; T. Tamagawa; K. Tamura; T. Tamura; T. Tanaka; Yasuo Tanaka; Yasuyuki Tanaka; M. Tashiro; Y. Tawara; Y. Terada; Y. Terashima; F. Tombesi; H. Tomida; Y. Tsuboi; M. Tsujimoto; H. Tsunemi; T. Tsuru; H. Uchida; H. Uchiyama; Y. Uchiyama; S. Ueda; Y. Ueda; S. Ueno; S. Uno; C. M. Urry; E. Ursino; C. P. de Vries; S. Watanabe; N. Werner; D. R. Wik; D. R. Wilkins; B. J. Williams; S. Yamada; H. Yamaguchi; K. Yamaoka; N. Y. Yamasaki; M. Yamauchi; S. Yamauchi; T. Yaqoob; Y. Yatsu; D. Yonetoku; A. Yoshida; I. Zhuravleva; A. Zoghbi
ASTROPHYSICAL JOURNAL LETTERS, Volume：837, Number：1, First page：668, Last page：672, Mar. 2017, [Reviewed]
X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E approximate to 3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of S XVI (E similar or equal to 3.44 keV rest-frame)-a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.3847/2041-8213/aa61fa
DOI ID：10.3847/2041-8213/aa61fa, ISSN：2041-8205, eISSN：2041-8213, Web of Science ID：WOS:000396122600001 - Multi-year X-Ray Variations of Iron-K and Continuum Emissions in the Young Supernova Remnant Cassiopeia A
Toshiki Sato; Yoshitomo Maeda; Aya Bamba; Satoru Katsuda; Yutaka Ohira; Ryo Yamazaki; Kuniaki Masai; Hironori Matsumoto; Makoto Sawada; Yukikatsu Terada; John P. Hughes; Manabu Ishida
ASTROPHYSICAL JOURNAL, Volume：836, Number：2, Feb. 2017, [Reviewed]
We found a simultaneous decrease of the Fe-K line and 4.2-6 keV continuum of Cassiopeia A with the monitoring data taken by the Chandra X-ray Observatory in 2000-2013. The flux change rates in the whole remnant are -0.65 +/- 0.02% yr(-1) in the 4.2-6.0 keV continuum and -0.6 +/- 0.1% yr(-1) in the Fe-K line. In the eastern region where the thermal emission is considered to dominate, the variations show the largest values: -1.03 +/- 0.05% yr(-1) (4.2-6 keV band) and -0.6 +/- 0.1% yr(-1) (Fe-K line). In this region, the time evolution of the emission measure and the temperature have a decreasing trend. This could be interpreted as adiabatic cooling with the expansion of m = 0.66. On the other hand, in the non-thermal emission dominated regions, variations of the 4.2-6 keV continuum show smaller rates: -0.60 +/- 0.04% yr(-1) in the southwestern region, -0.46 +/- 0.05% yr(-1) in the inner region, and + 0.00 +/- 0.07% yr(-1) in the forward shock region. In particular, flux does not show significant change in the forward shock region. These results imply that strong braking in shock velocity has not been occurring in Cassiopeia A (< 5 km s(-1) yr(-1)). All of our results support the idea that X-ray flux decay in the remnant is mainly caused by thermal components.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.3847/1538-4357/836/2/225
DOI ID：10.3847/1538-4357/836/2/225, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000395870900018 - CTA Report 125：Status report for the construction of Focal Plane Instrument of LST-1
Sakurai S.; Orito R.; Kataoka J.; Katagiri H.; Kimura S.; Kushida J.; Kubo H.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Ikeno M.; Sawada M.; Sunada Y.; Takahashi M.; Tanaka M.; Tsujimoto S.; Teshima M.; Terada Y.; Tokanai F.; Nakajima D.; Nakamori T.; Inada T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Nozaki S.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Inome Y.; Yoshida T.; Hadasch D.; Mazin D.; the CTA-Japan consortium; Iwamura Y.; Uchida T.; Ohoka H.; Okumura A.; Okazaki N.
Meeting Abstracts of the Physical Society of Japan, Volume：72, Number：0, First page：360, Last page：360, 2017
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.72.2.0_360
DOI ID：10.11316/jpsgaiyo.72.2.0_360, CiNii Articles ID：130007510715 - CTA Report 126 : Improvement and calibration of the focal plane detector for LST
Sunada Y.; Orito R.; Kataoka J.; Katagiri H.; Kimura S.; Kushida J.; Kubo H.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Ikeno M.; Sawada M.; Sakurai S.; Takahashi M.; Tanaka M.; Tsujimoto S.; Teshima M.; Terada Y.; Tokanai F.; Nakajima D.; Nakamori T.; Inada T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Nozaki S.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Masuda S.; Yamamoto T.; Inome Y.; Yoshida T.; Hadasch D.; Mazin D.; the CTA-Japan consortium; Iwamura Y.; Uchida T.; Ohoka H.; Okumura A.; Okazaki N.
Meeting Abstracts of the Physical Society of Japan, Volume：72, Number：0, First page：361, Last page：361, 2017
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.72.2.0_361
DOI ID：10.11316/jpsgaiyo.72.2.0_361, CiNii Articles ID：130007510716 - CTA Report 119: Integration test of the focal plane camera of the first CTA Large Size Telescope
Nakajima D.; Kushida J.; Gunji S.; Konno Y.; Saito T.; Sakurai S.; Takahashi M.; Takeda J.; Tanigawa S.; Tan D.V.; Tsujimoto S.; Inome Y.; Teshima M.; Terada Y.; Tokanai F.; Nakamori T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Nozaki S.; Hayashida M.; Bamba A.; Ohoka H.; Masuda S.; Yamamoto T.; Yoshida T.; Yoshida M.; Mazine D.; Hadasch D.; CTA-Japan consortium; Okumura Akira; Orito R.; Katagiri H.; Kishida S.; Kimura S.; Kubo H.
Meeting Abstracts of the Physical Society of Japan, Volume：72, Number：0, First page：466, Last page：466, 2017現在スペイン領ラパルマ島においてCTA計画の大口径望遠鏡の建設が進められている。望遠鏡の焦点面検出器は265台のPMTモジュールで構成される。PMTモジュールは7本のPMTと付随するコントロール用回路基板、信号読み出し回路基板で構成される。PMTモジュールのこれらの構成要素は日本グループ中心に開発、量産を行った。本公演では、量産したPMTモジュールを複数台組み込んだ、カメラシステムとしての統合試験の結果を報告する。
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.72.1.0_466
DOI ID：10.11316/jpsgaiyo.72.1.0_466, CiNii Articles ID：130006711512 - TWO DISTINCT-ABSORPTION X-RAY COMPONENTS FROM TYPE IIn SUPERNOVAE: EVIDENCE FOR ASPHERICITY IN THE CIRCUMSTELLAR MEDIUM
Satoru Katsuda; Keiichi Maeda; Aya Bamba; Yukikatsu Terada; Yasushi Fukazawa; Koji Kawabata; Masanori Ohno; Yasuharu Sugawara; Yohko Tsuboi; Stefan Immler
ASTROPHYSICAL JOURNAL, Volume：832, Number：2, Dec. 2016, [Reviewed]
We present multi-epoch X-ray spectral observations of three Type IIn supernovae (SNe), SN 2005kd, SN 2006jd, and SN 2010jl, acquired with Chandra, XMM-Newton, Suzaku, and Swift. Previous extensive X-ray studies of SN. 2010jl have revealed that X-ray spectra are dominated by thermal emission, which likely arises from a hot plasma heated by a forward shock propagating into a massive circumstellar medium (CSM). Interestingly, an additional soft X-ray component was required to reproduce the spectra at a period of similar to 1-2 years after the SN explosion. Although this component is likely associated with the SN, its origin remained an open question. We find a similar, additional soft X-ray component from the other two SNe IIn as well. Given this finding, we present a new interpretation for the origin of this component; it is thermal emission from a forward shock essentially identical to the hard X-ray component, but directly reaches us from a void of the dense CSM. Namely, the hard and soft components are responsible for the heavily and moderately absorbed components, respectively. The co-existence of the two components with distinct absorptions as well as the delayed emergence of the moderately absorbed X-ray component could be evidence for asphericity of the CSM. We show that the X-ray spectral evolution can be qualitatively explained by considering a torus-like geometry for the dense CSM. Based on our X-ray spectral analyses, we estimate the radius of the torus-like CSM to be on the order of similar to 5 x 10(16) cm.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.3847/0004-637X/832/2/194
DOI ID：10.3847/0004-637X/832/2/194, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000390490100054 - Progenitors of type Ia supernovae
Keiichi Maeda; Yukikatsu Terada
INTERNATIONAL JOURNAL OF MODERN PHYSICS D, Volume：25, Number：10, Sep. 2016, [Reviewed]
Natures of progenitors of type Ia Supernovae (SNe Ia) have not yet been clarified. There has been long and intensive discussion on whether the so-called single degenerate (SD) scenario or the double degenerate (DD) scenario, or anything else, could explain a major population of SNe Ia, but the conclusion has not yet been reached. With rapidly increasing observational data and new theoretical ideas, the field of studying the SN Ia progenitors has been quickly developing, and various new insights have been obtained in recent years. This paper aims at providing a summary of the current situation regarding the SN Ia progenitors, both in theory and observations. It seems difficult to explain the emerging diversity seen in observations of SNe Ia by a single population, and we emphasize that it is important to clarify links between different progenitor scenarios and different sub-classes of SNe Ia.
WORLD SCIENTIFIC PUBL CO PTE LTD, English
DOI：https://doi.org/10.1142/S021827181630024X
DOI ID：10.1142/S021827181630024X, ISSN：0218-2718, eISSN：1793-6594, Web of Science ID：WOS:000383808100004 - The quiescent intracluster medium in the core of the Perseus cluster
Felix Aharonian; Hiroki Akamatsu; Fumie Akimoto; Steven W. Allen; Naohisa Anabuki; Lorella Angelini; Keith Arnaud; Marc Audard; Hisamitsu Awaki; Magnus Axelsson; Aya Bamba; Marshall Bautz; Roger Blandford; Laura Brenneman; Gregory V. Brown; Esra Bulbul; Edward Cackett; Maria Chernyakova; Meng Chiao; Paolo Coppi; Elisa Costantini; Jelle de Plaa; Jan-Willem den Herder; Chris Done; Tadayasu Dotani; Ken Ebisawa; Megan Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew C. Fabian; Carlo Ferrigno; Adam Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi Gallo; Poshak Gandhi; Margherita Giustini; Andrea Goldwurm; Liyi Gu; Matteo Guainazzi; Yoshito Haba; Kouichi Hagino; Kenji Hamaguchi; Ilana Harrus; Isamu Hatsukade; Katsuhiro Hayashi; Takayuki Hayashi; Kiyoshi Hayashida; Junko Hiraga; Ann Hornschemeier; Akio Hoshino; John Hughes; Ryo Iizuka; Hajime Inoue; Yoshiyuki Inoue; Kazunori Ishibashi; Manabu Ishida; Kumi Ishikawa; Yoshitaka Ishisaki; Masayuki Itoh; Naoko Iyomoto; Jelle Kaastra; Timothy Kallman; Tuneyoshi Kamae; Erin Kara; Jun Kataoka; Satoru Katsuda; Junichiro Katsuta; Madoka Kawaharada; Nobuyuki Kawai; Richard Kelley; Dmitry Khangulyan; Caroline Kilbourne; Ashley King; Takao Kitaguchi; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Shu Koyama; Katsuji Koyama; Peter Kretschmar; Hans Krimm; Aya Kubota; Hideyo Kunieda; Philippe Laurent; Francois Lebrun; Shiu-Hang Lee; Maurice Leutenegger; Olivier Limousin; Michael Loewenstein; Knox S. Long; David Lumb; Grzegorz Madejski; Yoshitomo Maeda; Daniel Maier; Kazuo Makishima; Maxim Markevitch; Hironori Matsumoto; Kyoko Matsushita; Dan McCammon; Brian McNamara; Missagh Mehdipour; Eric Miller; Jon Miller; Shin Mineshige; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Takuya Miyazawa; Tsunefumi Mizuno; Hideyuki Mori; Koji Mori; Harvey Moseley; Koji Mukai; Hiroshi Murakami; Toshio Murakami; Richard Mushotzky; Ryo Nagino; Takao Nakagawa; Hiroshi Nakajima; Takeshi Nakamori; Toshio Nakano; Shinya Nakashima; Kazuhiro Nakazawa; Masayoshi Nobukawa; Hirofumi Noda; Masaharu Nomachi; Steve O'Dell; Hirokazu Odaka; Takaya Ohashi; Masanori Ohno; Takashi Okajima; Naomi Ota; Masanobu Ozaki; Frits Paerels; Stephane Paltani; Arvind Parmar; Robert Petre; Ciro Pinto; Martin Pohl; F. Scott Porter; Katja Pottschmidt; Brian Ramsey; Christopher Reynolds; Helen Russell; Samar Safi-Harb; Shinya Saito; Kazuhiro Sakai; Hiroaki Sameshima; Goro Sato; Kosuke Sato; Rie Sato; Makoto Sawada; Norbert Schartel; Peter Serlemitsos; Hiromi Seta; Megumi Shidatsu; Aurora Simionescu; Randall Smith; Yang Soong; Lukasz Stawarz; Yasuharu Sugawara; Satoshi Sugita; Andrew Szymkowiak; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin'ichiro Takeda; Yoh Takei; Toru Tamagawa; Keisuke Tamura; Takayuki Tamura; Takaaki Tanaka; Yasuo Tanaka; Yasuyuki Tanaka; Makoto Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Francesco Tombesi; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Takeshi Tsuru; Hiroyuki Uchida; Hideki Uchiyama; Yasunobu Uchiyama; Shutaro Ueda; Yoshihiro Ueda; Shiro Ueno; Shin'ichiro Uno; Meg Urry; Eugenio Ursino; Cor De Vries; Shin Watanabe; Norbert Werner; Daniel Wik; Dan Wilkins; Brian Williams; Shinya Yamada; Hiroya Yamaguchi; Kazutaka Yamaoka; Noriko Y. Yamasaki; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Yoichi Yatsu; Daisuke Yonetoku; Atsumasa Yoshida; Takayuki Yuasa; Irina Zhuravleva; Abderahmen Zoghbi
NATURE, Volume：535, Number：7610, First page：117, Last page：+, Jul. 2016, [Reviewed]
Clusters of galaxies are the most massive gravitationally bound objects in the Universe and are still forming. They are thus important probes(1) of cosmological parameters and many astrophysical processes. However, knowledge of the dynamics of the pervasive hot gas, the mass of which is much larger than the combined mass of all the stars in the cluster, is lacking. Such knowledge would enable insights into the injection of mechanical energy by the central supermassive black hole and the use of hydrostatic equilibrium for determining cluster masses. X-rays from the core of the Perseus cluster are emitted by the 50-million-kelvin diffuse hot plasma filling its gravitational potential well. The active galactic nucleus of the central galaxy NGC 1275 is pumping jetted energy into the surrounding intracluster medium, creating buoyant bubbles filled with relativistic plasma. These bubbles probably induce motions in the intracluster medium and heat the inner gas, preventing runaway radiative cooling-a process known as active galactic nucleus feedback(2-6). Here we report X-ray observations of the core of the Perseus cluster, which reveal a remarkably quiescent atmosphere in which the gas has a line-of-sight velocity dispersion of 164 +/- 10 kilometres per second in the region 30-60 kiloparsecs from the central nucleus. A gradient in the line-of-sight velocity of 150 +/- 70 kilometres per second is found across the 60-kiloparsec image of the cluster core. Turbulent pressure support in the gas is four per cent of the thermodynamic pressure, with large-scale shear at most doubling this estimate. We infer that a total cluster mass determined from hydrostatic equilibrium in a central region would require little correction for turbulent pressure.
NATURE PUBLISHING GROUP, English, Scientific journal
DOI：https://doi.org/10.1038/nature18627
DOI ID：10.1038/nature18627, ISSN：0028-0836, eISSN：1476-4687, Web of Science ID：WOS:000379015600035 - New identification of the mixed-morphology supernova remnant G298.6-0.0 with possible gamma-ray association
Aya Bamba; Makoto Sawada; Yuto Nakano; Yukikatsu Terada; John Hewitt; Robert Petre; Lorella Angelini
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：68, Jun. 2016, [Reviewed]
We present an X-ray analysis on the Galactic supernova remnant (SNR) G298.6-0.0 observed with Suzaku. The X-ray image shows a center-filled structure inside a radio shell, implying that this SNR can be categorized as a mixed-morphology (MM) SNR. The spectrum is well reproduced by a single-temperature plasma model in ionization equilibrium, with a temperature of 0.78 (0.70-0.87) keV. The total plasma mass of 30 M-circle dot indicates that the plasma has an interstellar medium origin. The association with a GeV gamma-ray source, 3FGL J1214.0-6236, on the shell of the SNR is discussed, in comparison with other MM SNRs with GeV gamma-ray associations. It is found that the flux ratio between absorption-corrected thermal X-rays and GeV gamma-rays decreases as the physical size of MM SNRs becomes larger. The absorption-corrected thermal X-ray flux of G298.6-0.0 and the GeV gamma-ray flux of 3FGL J1214.0-6236 closely follow this trend, implying that 3FGL J1214.0-6236 is likely to be a GeV counterpart of G298.6-0.0.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psv096
DOI ID：10.1093/pasj/psv096, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000377426700005 - Suzaku observations of the hard X-ray spectrum of Vela Jr. (SNR RX J0852.0-4622)
Sawako Takeda; Aya Bamba; Yukikatsu Terada; Makoto S. Tashiro; Satoru Katsuda; Ryo Yamazaki; Yutaka Ohira; Wataru Iwakiri
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：68, Jun. 2016, [Reviewed]
We report the results of Suzaku observations of the young supernova remnant, Vela Jr. (RX J0852.0-4622), which is known to emit synchrotron X-rays, as well as TeV gamma-rays. Utilizing 39 Suzaku mapping observation data from Vela Jr., a significant hard X-ray emission is detected with the hard X-ray detector (HXD) from the northwest TeV-emitting region. The X-ray spectrum is reproduced well by a single power-law model with a photon index of 3.15(-1.14)(+1.18) in the 12-22 keV band. Compiling this hard X-ray spectrum with the soft X-ray spectrum simultaneously observed with the X-ray imaging spectrometer (XIS) onboard Suzaku, we find that the wide-band X-ray spectrum in the 2-22 keV band is reproduced with a single power-law or concave broken power-law model, which are statistically consistent with each other. Whichever of the two models, single or broken power-law, is appropriate, clearly the spectrum has no roll-off structure. Applying this result to the method introduced in Yamazaki et al. (2014, Res. Astron. Astrophys., 14, 165), we find that a one-zone synchrotron model with electron spectrum having a power-law plus exponential cut-off may not be applicable to Vela Jr.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psw036
DOI ID：10.1093/pasj/psw036, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000377426700010 - Suzaku Wide-band All-sky Monitor measurements of duration distributions of gamma-ray bursts
Norisuke Ohmori; Kazutaka Yamaoka; Masanori Ohno; Satoshi Sugita; Ryuuji Kinoshita; Yusuke Nishioka; Kevin Hurley; Yoshitaka Hanabata; Makoto S. Tashiro; Junichi Enomoto; Takeshi Fujinuma; Yasushi Fukazawa; Wataru Iwakiri; Takafumi Kawano; Motohide Kokubun; Kazuo Makishima; Shunsuke Matsuoka; Tsutomu Nagayoshi; Yujin E. Nakagawa; Souhei Nakaya; Kazuhiro Nakazawa; Tadayuki Takahashi; Sawako Takeda; Yukikatsu Terada; Yuji Urata; Seiya Yabe; Tetsuya Yasuda; Makoto Yamauchi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：68, Jun. 2016, [Reviewed]
We report on the T-90 and T-50 duration distributions and their relations with spectral hardness using 1464 gamma-ray bursts (GRBs), which were observed by the Suzaku Wide-band All-sky Monitor (WAM) from 2005 August 4 to 2010 December 29. The duration distribution is clearly bimodal in three energy ranges (50-120, 120-250, and 250-550 keV), but is unclear in the 550-5000 keV range, probably because of the limited sample size. The WAM durations decrease with energy according to a power-law index of -0.058(-0.034, +0.033). The hardness-duration relation reveals the presence of short-hard and long-soft GRBs. The short: long event ratio tends to be higher with increasing energy. We compared the WAM distribution with ones measured by eight other GRB instruments. The WAM T-90 distribution is very similar to those of INTEGRAL/SPI-ACS and Granat/PHEBUS, and least likely to match the Swift/BAT distribution. The WAM short: long event ratio (0.25:0.75) is much different from Swift/BAT (0.08:0.92), but is almost the same as CGRO/BATSE (0.25:0.75). To explain this difference for BAT, we examined three effects: BAT trigger types, energy dependence of the duration, and detection sensitivity differences between BAT and WAM. As a result, we found that the ratio difference could be explained mainly by energy dependence including soft extended emissions for short GRBs and much better sensitivity for BAT which can detect weak/long GRBs. The reason for the same short: long event ratio for BATSE and WAM was confirmed by calculation using the trigger efficiency curve.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psw009
DOI ID：10.1093/pasj/psw009, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000377426700030 - MEASUREMENTS OF THE SOFT GAMMA-RAY EMISSION FROM SN2014J WITH SUZAKU
Yukikatsu Terada
The Astrophysical Journal, Volume：823, Number：1, May 2016, [Reviewed]
The hard X-ray detector (HXD) on board Suzaku measured soft gamma-rays from the SN Ia SN2014J at 77 +/- 2 days after the explosion. Although the confidence level of the signal is about 90% (i. e., 2 sigma), the 3 sigma upper limit has been derived at < 2.2 x 10(-4) ph s(-1) cm(-2) in the 170-250 keV band as the first independent measurement of soft gamma-rays with an instrument other than INTEGRAL. For this analysis, we have examined the reproducibility of the NXB model of HXD/GSO using blank sky data. We find that the residual count rate in the 90-500 keV band is distributed around an average of 0.19% with a standard deviation of 0.42% relative to the NXB rate. The averaged residual signals are consistent with that expected from the cosmic X-ray background. The flux of SN2014J derived from Suzaku measurements taken in one snapshot at t = 77 +/- 2 days after the explosion is consistent with the INTEGRAL values averaged over the period between t = 50 and 100 days and also with explosion models of single or double degenerate scenarios. Being sensitive to the total ejecta mass surrounding the radioactive material, the ratio between continuum and line flux in the soft gamma-ray regime
IOP PUBLISHING LTD, Scientific journal
DOI：https://doi.org/10.3847/0004-637X/823/1/43
DOI ID：10.3847/0004-637X/823/1/43, ISSN：0004-637X, ORCID：67259866, Web of Science ID：WOS:000377216300043 - DISCOVERY OF X-RAY EMISSION FROM THE GALACTIC SUPERNOVA REMNANT G32.8-0.1 WITH SUZAKU
Aya Bamba; Yukikatsu Terada; John Hewitt; Robert Petre; Lorella Angelini; Samar Safi-Harb; Ping Zhou; Fabrizio Bocchino; Makoto Sawada
ASTROPHYSICAL JOURNAL, Volume：818, Number：1, Feb. 2016, [Reviewed]
We present the first dedicated X-ray study of the supernova remnant (SNR) G32.8-0.1 (Kes. 78) with Suzaku. X-ray emission from the whole SNR shell has been detected for the first time. The X-ray morphology is well correlated with the emission from the radio shell, while anti-correlated with the molecular cloud found in the SNR field. The X-ray spectrum shows not only conventional low-temperature (kT similar to 0.6 keV) thermal emission in a non-equilibrium ionization state, but also a very high-temperature (kT similar to 3.4 keV) component with a very low ionization timescale (similar to 2.7 x 10(9) cm(-3) s), or a hard nonthermal component with a photon index Gamma similar to 2.3. The average density of the low-temperature plasma is rather low, of the order of 10(-3)-10(-2) cm(-3), implying that this SNR is expanding into a low-density cavity. We discuss the X-ray emission of the SNR, also detected in TeV with H.E.S.S., together with multi-wavelength studies of the remnant and other gamma-ray emitting SNRs, such as W28 and RCW 86. Analysis of a time-variable source, 2XMM J185114.3-000004, found in the northern part of the SNR, is also reported for the first time. Rapid time variability and a heavily absorbed hard-X-ray spectrum suggest that this source could be a new supergiant fast X-ray transient.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.3847/0004-637X/818/1/63
DOI ID：10.3847/0004-637X/818/1/63, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000370370800063 - 21pCD-11 Status of the Soft X-ray Spectrometer (SXS) onboard ASTRO-H
Tashiro M. S.; Mitsuda k.; Yamasaki N.; Takei Y.; Tsujimoto M.; Ogawa M.; Koyama S.; Sakai K.; Sugita H.; Sato Y.; Shinozaki; Okamoto A.; Fujimoto R.; Ohashi T.; Ishisaki Y.; Ezoe Y.; Yamada S.; Seta H.; Terada Y.; Kitamoto S.; Hoshino A.; Tamagawa T.; Ishikawa K.; Noda H.; Sato K.; Ota N.; Sawada M.; Mitsuishi I.; Murakami M.; Murakami H.; Iyomoto N.; Kelley R. L.; Kilbourne C. A.; Porter F. S.; Boyce K. R.; Eckart M. E.; Chiao M. P.; Leutenegger M. A.; Brown G. V.; McCammon D.; Szymkowiak A.; Herder J. -W. den; Haas D.; Vries C. de; Costantini E.; Akamatsu H.; Paltani S.; ASTRO-H SXS team
Meeting Abstracts of the Physical Society of Japan, Volume：71, First page：509, Last page：509, 2016
The Physical Society of Japan (JPS), Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.71.1.0_509
DOI ID：10.11316/jpsgaiyo.71.1.0_509, ISSN：2189-079X, CiNii Articles ID：110010056547, CiNii Books ID：AA12721570 - CTA Report 111: Evaluation results of 7-dynode PMTs for improvement of CTA Large-Sized Telescope
Takahashi M.; Nagayoshi T.; Ishio K.; Inome Y.; Ohoka H.; Okumura A.; Orito R.; Katagiri H.; Kishida S.; Kubo H.; Kushida J.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Takeda J.; Tanaka M.; Tanigawa S.; Tsujimoto S.; Teshima M.; Terada Y.; Tomono Y.; Nakajima D.; Nakamori T.; Nishijima K.; Nozaki S.; Hayashida M.; Bamba A.; Masuda S.; Yamamoto T.; Yoshida T.; Tan Dang Viet; Hadasch Daniela; Mazin Daniel; CTA-Japan consortium
Meeting Abstracts of the Physical Society of Japan, Volume：71, First page：324, Last page：324, 2016CTA大口径望遠鏡はチェレンコフ光密度が低くなる数十GeVのガンマ線を観測するため、高感度かつ低バックグラウンドの光電子増倍管が求められる。2基目以降に向け浜松ホトニクス(株)と共同開発した R12992は、S/N比に影響するパルス幅がダイノードの段数を8段から7段とすることにより初号機用に比べ大きく改善された。また量子効率もピーク値で平均43%にまで上昇した。このR12992の諸特性を測定、評価した結果を報告する。
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.71.2.0_324
DOI ID：10.11316/jpsgaiyo.71.2.0_324, CiNii Articles ID：130006245979 - CTA Report 112: Camera test for the first unit of CTA Large-Sized Telescope
Nozaki S.; Ishio K.; Inome Y.; Ohoka H.; Okumura A.; Orito R.; Katagiri H.; Kishida S.; Kubo H.; Kushida J.; Gunji S.; Koyama S.; Konno Y.; Saito T.; Takahashi M.; Takeda J.; Tanaka M.; Tanigawa S.; Tsujimoto S.; Teshima M.; Terada Y.; Tomono Y.; Nakajima D.; Nakamori T.; Nagayoshi T.; Nishijima K.; Hayashida M.; Bamba A.; Masuda S.; Yamamoto T.; Yoshida T.; Tan Dang Viet; Hadasch Daniela; Mazin Daniel; CTA-Japan Consortium; Ikeno M.; Uchida T.
Meeting Abstracts of the Physical Society of Japan, Volume：71, First page：325, Last page：325, 2016Cherenkov Telescope Array(CTA)計画は、口径の異なる複数の望遠鏡を用いて 20GeVから100TeV 以上のガンマ線を従来よりも10倍高い感度で全天観測する望遠鏡 建設計画である。我々は大口径望遠鏡搭載用カメラの試験・ 開発を行っている。本講演では、初号機で用いるPMT、 波形読出し回路それぞれ133本、19個のモジュールから成る試 験用ミニカメラの構成、動作試験の結果、 及び次号機での搭載に向けた、 新版の波形読出し回路基板の設計の概要、 開発状況について報告する。
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.71.2.0_325
DOI ID：10.11316/jpsgaiyo.71.2.0_325, CiNii Articles ID：130006245978 - In-orbit performance of the Soft X-ray Spectrometer (SXS) onboard ASTRO-H (Hitomi)
Fujimoto R.; Mitsuda K.; Yamasaki N. Y.; Takei Y.; Tsujimoto M.; Ogawa M.; Koyama S.; Ishikawa K.; Sugita H.; Sato Y.; Shinozaki K.; Okamoto A.; Ohashi T.; Ishisaki Y.; Ezoe Y.; Yamada S.; Seta H.; Tashiro M. S.; Terada Y.; Kitamoto S.; Hoshino A.; Tamagawa T.; Sato K.; Sawada M.; Noda H.; Mitsuishi I.; Murakami H.; Ota N.; Iyomoto N.; Murakami M.; Kelley R. L.; Kilbourne C. A.; Porter F. S.; Boyce K. R.; Sneiderman G. A.; DiPirro M. J.; Shirron P. J.; Bialas T.; Eckart M. E.; Chiao M. P.; Leutenegger M. A.; Watanabe T.; Sakai K.; Brown G. V.; McCammon D.; Szymkowiak A.; Herder J. -W. den; Haas D.; Vries C. de; Costantini E.; Akamatsu H.; Paltani S.; ASTRO-H SXS team
Meeting Abstracts of the Physical Society of Japan, Volume：71, First page：367, Last page：367, 20162016年2月17日に打ち上げられたASTRO-H (ひとみ) 衛星に搭載された精密X線分光装置 SXS (Soft X-ray Spectrometer) は，40日弱の限られた期間ではあったが，軌道上において正常に動作し，天体のデータも取得できた．SXS の軌道上での性能について報告する．
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.71.2.0_367
DOI ID：10.11316/jpsgaiyo.71.2.0_367, CiNii Articles ID：130006246130 - Soft Gamma-ray Observation of SN2014J with Suzaku
Yukikatsu Terada; Keiich Maeda; Yasushi Fukazawa; Aya Bamba; Yoshihiro Ueda; Satoru Katsuda; Teruaki Enoto; Tadayuki Takahashi; Toru Tamagawa; Friedrich K. Roepke; Alexander Summa; Roland Diehl
PROCEEDINGS OF THE 14TH INTERNATIONAL SYMPOSIUM ON NUCLEI IN THE COSMOS (NIC2016), 2016
Type Ia Supernovae (SNe Ia) are key objects for the present cosmology as the most mature standard candles. It is important to verify theoretical models of SN Ia explosions observationally. Since emissions from SN Ia are mainly drived by the radioactive sources generated in the explosion, gamma-ray observations are the key for the study. We performed a soft gamma-ray observation of the near-by SN Ia, SN2014J, with the hard X-ray detector (HXD) onboard Suzaku satellite at 77 +/- 2 days after the explosion. After careful treatments of X-ray contaminations from ultra-luminous X-ray source in the M82 galaxy, non X-ray background events, Cosmic X-ray background emission and the Earth's albedo, we found gamma-ray signals are measured from SN2014J at 2 sigma confidence with the flux at (1.2 +/- 0.7)x10(-4) ph s(-1) cm(-2) in the 170 - 250 keV band. The flux ratio between the continuum and the line from Co-56 is sensitive to the ejecta mass and might distinguish progenitor models between single and double degenerate scenarios. Our Suzaku data of continuum emission and line emission reported by INTEGRAL satellite has been examined with this relation but could not distinguish these models. However, thanks to the high sensitivities of the HXD around 200 keV in the shorter exposure than INTEGRAL, the Suzaku observations clearly exclude explosion models with heavier Ni-56 mass than 1 solar mass.
PHYSICAL SOCIETY JAPAN, English, International conference proceedings
DOI：https://doi.org/10.7566/JPSCP.14.010306
DOI ID：10.7566/JPSCP.14.010306, Web of Science ID：WOS:000566261100015 - A broadband X-ray imaging spectroscopy with high-angular resolution: the FORCE mission
Koji Mori; Takeshi Go Tsuru; Kazuhiro Nakazawa; Yoshihiro Ueda; Takashi Okajima; Hiroshi Murakami; Hisamitsu Awaki; Hironori Matsumoto; Yasushi Fukazawa; Hiroshi Tsunemi; Tadayuki Takahashi; William W. Zhang
SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
We are proposing FORCE (Focusing On Relativistic universe and Cosmic Evolution) as a future Japan-lead Xray observatory to be launched in the mid 2020s. Hitomi (ASTRO-H) possesses a suite of sensitive instruments enabling the highest energy-resolution spectroscopy in soft X-ray band, a broadband X-ray imaging spectroscopy in soft and hard X-ray bands, and further high energy coverage up to soft gamma-ray band. FORCE is the direct successor to the broadband X-ray imaging spectroscopy aspect of Hitomi (ASTRO-H) with significantly higher angular resolution. The current design of FORCE defines energy band pass of 1-80 keV with angular resolution of < 15'' in half-power diameter, achieving a 10 times higher sensitivity above 10 keV compared to any previous missions with simultaneous soft X-ray coverage. Our primary scientific objective is to trace the cosmic formation history by searching for "missing black holes" in various mass-scales: "buried supermassive black holes (SMBHs)" (> 10(4) M-circle dot) residing in the center of galaxies in a cosmological distance, "intermediate-mass black holes" (10(2)-10(4) M-circle dot) acting as the possible seeds from which SMBHs grow, and "orphan stellar-mass black holes" (< 10(2) M-circle dot) without companion in our Galaxy. In addition to these missing BHs, hunting for the nature of relativistic particles at various astrophysical shocks is also in our scope, utilizing the broadband X-ray coverage with high angular-resolution. FORCE are going to open a new era in these fields. The satellite is proposed to be launched with the Epsilon vehicle that is a Japanese current solid-fuel rocket. FORCE carries three identical pairs of Super-mirror and wide-band X-ray detector. The focal length is currently planned to be 10 m. The silicon mirror with multi-layer coating is our primary choice to achieve lightweight, good angular optics. The detector is a descendant of hard X-ray imager onboard Hitomi (ASTRO-H) replacing its silicon strip detector with SOI-CMOS silicon pixel detector, allowing an extension of the low energy threshold down to 1 keV or even less.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2231262
DOI ID：10.1117/12.2231262, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000387731500046 - The soft gamma-ray detector (SGD) onboard ASTRO-H
Shin Watanabe; Hiroyasu Tajima; Yasushi Fukazawa; Roger Blandford; Teruaki Enoto; Andrea Goldwurm; Kouichi Hagino; Katsuhiro Hayashi; Yuto Ichinohe; Jun Kataoka; Junichiro Katsuta; Takao Kitaguchi; Motohide Kokubun; Philippe Laurent; Francois Lebrun; Olivier Limousin; Grzegorz M. Madejski; Kazuo Makishima; Tsunefumi Mizunoe; Kunishiro Mori; Takeshi Nakamori; Toshio Nakano; Kazuhiro Nakazawa; Hirofumi Noda; Hirokazu Odaka; Masanori Ohno; Masayuki Ohta; Shinya Saito; Goro Sato; Rie Sato; Shin'ichiro Takeda; Hiromitsu Takahashi; Tadayuki Takahashi; Takaaki Tanaka; Yasuyuki Tanaka; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Kazutaka Yamaoka; Yoichi Yatsu; Daisuke Yonetoku; Takayuki Yuasa
SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
The Soft Gamma-ray Detector (SGD) is one of science instruments onboard ASTRO-H (Hitomi) and features a wide energy band of 60-600 keV with low backgrounds. SGD is an instrument with a novel concept of "Narrow field-of-view" Compton camera where Compton kinematics is utilized to reject backgrounds which are inconsistent with the field-of-view defined by the active shield. After several years of developments, the flight hardware was fabricated and subjected to subsystem tests and satellite system tests. After a successful ASTRO-H (Hitomi) launch on February 17, 2016 and a critical phase operation of satellite and SGD in-orbit commissioning, the SGD operation was moved to the nominal observation mode on March 24, 2016. The Compton cameras and BGO-APD shields of SGD worked properly as designed. On March 25, 2016, the Crab nebula observation was performed, and, the observation data was successfully obtained.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2231962
DOI ID：10.1117/12.2231962, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000387731500028 - The hard X-ray imager (HXI) onboard ASTRO-H
Kazuhiro Nakazawa; Goro Sato; Motohide Kokubun; Teruaki Enoto; Yasushi Fukazawa; Kouichi Hagino; Atsushi Harayama; Katsuhiro Hayashi; Jun Kataoka; Junichiro Katsuta; Philippe Laurent; Francois Lebrung; Olivier Limousin; Kazuo Makishima; Tsunefumi Mizuno; Kunishiro Mori; Takeshi Nakamori; Toshio Nakano; Hirofumi Noda; Hirokazu Odaka; Masanori Ohno; Masayuki Ohta; Shinya Saito; Rie Sato; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin'ichiro Takeda; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Shin Watanabe; Kazutaka Yamaoka; Yoichi Yatsu; Takayuki Yuasa
SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
Hitomi X-ray observatory launched in 17 February 2016 had a hard X-ray imaging spectroscopy system made of two hard X-ray imagers (HXIs) coupled with two hard X-ray telescopes (HXTs). With 12 m focal length, they provide fine (2' half-power diameter; HPD) imaging spectroscopy at 5 to 80 keV. The HXI main imagers are made of 4 layers of Si and a CdTe semiconductor double-sided strip detectors, stacked to enhance detection efficiency as well as to enable photon interaction-depth sensing. Active shield made of 9 BGO scintillators surrounds the imager to provide with low background. Following the deployment of the Extensible Optical Bench (EOB) on 28 February, the HXI was gradually turned on. Two imagers successfully started observation on 14 March, and was operational till the incident lead to Hitomo loss, on 26 March. All detector channels, 1280 ch of imager and 11 channel of active shields and others each, worked well and showed performance consistent with those seen on ground. From the first light observation of G21.5-0.9 and the following Crab observations, 5 80 keV energy coverage and good detection efficiency were confirmed. With blank sky observations, we checked our background level. In some geomagnetic region, strong background continuum, presumably caused by trapped electron with energy similar to 100 keV, is seen. But by cutting the high-background time-intervals, the background became significantly lower, typically with 1-3x10(-4) counts s(-1) keV(-1) cm(-2) (here cm(2) is shown with detector geometrical area). Above 30 keV, line and continuum emission originating from activation of CdTe was significantly seen, though the level of 1-4x10(-4) counts s(-1) keV(-1) cm(-2) is still comparable to those seen in NuSTAR. By comparing the effective area and background rate, preliminary analysis shows that the HXI had a statistical sensitivity similar to NuSTAR for point sources, and more than twice better for largely extended sources.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2231176
DOI ID：10.1117/12.2231176, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000387731500026 - The Astro-H High Resolution Soft X-Ray Spectrometer
Richard L. Kelley; Hiroki Akamatsu; Phillipp Azzarell; Tom Bialas; Kevin R. Boyce; Gregory V. Brown; Edgar Canavan; Meng P. Chiao; Elisa Costantini; Michael J. DiPirro; Megan E. Eckart; Yuichiro Ezoe; Ryuichi Fujimoto; Daniel Haas; Jan-Willem den Herder; Akio Hoshino; Kumi Ishikawa; Yoshitaka Ishisaki; Naoko Iyomoto; Caroline A. Kilbourne; Mark Kimball; Shunji Kitamoto; Saori Konami; Shu Koyama; Maurice A. Leutenegger; Dan McCammon; Joseph Miko; Kazuhisa Mitsuda; Ikuyuki Mitsuishi; Harvey Moseley; Hiroshi Murakami; Masahide Murakami; Hirofumi Noda; Mina Ogawa; Takaya Ohashi; Atsushi Okamoto; Naomi Ota; Stephane Paltani; F. Scott Porter; Kazuhiro Sakai; Kosuke Sato; Yohichi Sato; Makoto Sawada; Hiromi Seta; Keisuke Shinozaki; Peter J. Shirron; Gary A. Sneiderman; Hiroyuki Sugita; Andrew E. Szymkowiak; Yoh Takei; Toni Tamagawa; Makoto Tashiro; Yukikatsu Terada; Masahiro Tsujimoto; Cor P. de Vries; Shinya Yamada; Noriko Y. Yamasaki; Yoichi Yatsu
SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
We present the overall design and performance of the Astro-H (Hitomi) Soft X-Ray Spectrometer (SXS). The instrument uses a 36-pixel array of x-ray microcalorimeters at the focus of a grazing-incidence x-ray mirror Soft X-Ray Telescope (SXT) for high-resolution spectroscopy of celestial x-ray sources. The instrument was designed to achieve an energy resolution better than 7 eV over the 0.3-12 keV energy range and operate for more than 3 years in orbit. The actual energy resolution of the instrument is 4-5 eV as demonstrated during extensive ground testing prior to launch and in orbit. The measured mass flow rate of the liquid helium cryogen and initial fill level at launch predict a lifetime of more than 4 years assuming steady mechanical cooler performance. Cryogen-free operation was successfully demonstrated prior to launch. The successful operation of the SXS in orbit, including the first observations of the velocity structure of the Perseus cluster of galaxies, demonstrates the viability and power of this technology as a tool for astrophysics.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2232509
DOI ID：10.1117/12.2232509, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000387731500020 - In-orbit operation of the ASTRO-H SXS
Masahiro Tsujimoto; Kazuhisa Mitsuda; Richard L. Kelley; Jan-Willem A. den Herder; Hiroki Akamatsu; Thomas G. Bialas; Kevin R. Boyce; Gregory V. Brown; Meng P. Chiao; Elisa Costantini; Cor P. de Vries; Michael J. DiPirro; Megan E. Eckart; Yuichiro Ezoe; Ryuichi Fujimoto; Daniel Haas; Akio Hoshino; Kumi Ishikawa; Yoshitaka Ishisaki; Naoko Iyomoto; Caroline A. Kilbourne; Shunji Kitamoto; Shu Koyama; Maurice A. Leutenegger; Dan McCammon; Ikuyuki Mitsuishi; Hiroshi Murakami; Masahide Murakami; Hirofumi Noda; Mina Ogawa; Naomi Ota; Stephane Paltani; Frederick S. Porter; Kosuke Sato; Yoichi Sato; Makoto Sawada; Hiromi Seta; Keisuke Shinozaki; Peter J. Shirron; Gary A. Sneiderman; Hiroyuki Sugita; Andrew E. Szymkowiak; Yoh Takei; Toru Tamagawa; Makoto S. Tashiro; Yukikatsu Terada; Shinya Yamada; Noriko Y. Yamasaki; Yoichi Yatsu
SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
We summarize all the in-orbit operations of the Soft X-ray Spectrometer (SXS) onboard the ASTRO-H (Hitomi) satellite. The satellite was launched on 2016/02/17 and the communication with the satellite ceased on 2016/03/26. The SXS was still in the commissioning phase, in which the setups were progressively changed. This article is intended to serve as a reference of the events in the orbit to properly interpret the SXS data taken during its short life time, and as a test case for planning the in-orbit operation for future micro-calorimeter missions.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2231784
DOI ID：10.1117/12.2231784, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000387731500023 - Astro-H data analysis, processing and archive
Lorella Angelini; Yukikatsu Terada; Michael Loewenstein; Eric D. Miller; Hiroya Yamaguchi; Tahir Yaqoob; Hans Krimm; Ilana Harrus; Hiromitsu Takahashi; Masayoshi Nobukawa; Makoto Sawada; Michael Witthoeft; Kristin Rutkowski; Andrew Sargent; Robert S. Hill; Michael Dutka; Joseph Eggen
SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
Astro-H (Hitomi) is an X-ray/Gamma-ray mission led by Japan with international participation, launched on February 17, 2016. The payload consists of four different instruments (SXS, SXI, HXI and SGD) that operate simultaneously to cover the energy range from 0.3 keV up to 600 keV. This paper presents the analysis software and the data processing pipeline created to calibrate and analyze the Hitomi science data along with the plan for the archive and user support. These activities have been a collaborative effort shared between scientists and software engineers working in several institutes in Japan and USA.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2234429
DOI ID：10.1117/12.2234429, ISSN：0277-786X, Web of Science ID：WOS:000387731500029 - In-flight performance of pulse processing system of the ASTRO-H soft x-ray spectrometer
Yoshitaka Ishisaki; Shinya Yamada; Hiromi Seta; Makoto S. Tashiro; Sawako Takeda; Yukikatsu Terada; Yuka Kato; Masahiro Tsujimoto; Shu Koyama; Kazuhisa Mitsuda; Makoto Sawada; Kevin R. Boyce; Meng P. Chiao; Tomomi Watanabe; Maurice A. Leutenegger; Megan E. Eckart; F. Scott Porter; Caroline A. Kilbourne; Richard L. Kelley
SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
We summarize results of the initial in-orbit performance of the pulse shape processor (PSP) of the soft x-ray spectrometer instrument onboard ASTRO-H (Hitomi). Event formats, kind of telemetry, and the pulse processing parameters are described, and the parameter settings in orbit are listed. PSP was powered-on two days after launch, and the event threshold was lowered in orbit. PSP worked fine in orbit, and there were no memory error nor SpaceWire communication error until the break-up of spacecraft. Time assignment, electrical crosstalk, and the event screening criteria are studied. It is confirmed that the event processing rate at 100% CPU load is similar to 200 c/s/array, compliant with the requirement on PSP.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2234222
DOI ID：10.1117/12.2234222, ISSN：0277-786X, Web of Science ID：WOS:000387731500114 - The ASTRO-H (Hitomi) X-ray Astronomy Satellite
Takahashi Tadayuki; Kokubun Motohide; Mitsuda Kazuhisa; Kelley Richard; Ohashi Takaya; Aharonian Felix; Akamatsu Hiroki; Akimoto Fumie; Allen Steve; Anabuki Naohisa; Angelini Lorella; Arnaud Keith; Asai Makoto; Audard Marc; Awaki Hisamitsu; Axelsson Magnus; Azzarello Philipp; Baluta Chris; Bamba Aya; Bando Nobutaka; Bautz Marshall; Bialas Thomas; Blandford Roger; Boyce Kevin; Brenneman Laura; Brown Greg; Bulbul Esra; Cackett Edward; Canavan Edgar; Chernyakova Maria; Chiao Meng; Coppi Paolo; Costantini Elisa; de Plaa Jelle; den Herder Jan-Willem; DiPirro Michael; Done Chris; Dotani Tadayasu; Doty John; Ebisawa Ken; Eckart Megan; Enoto Teruaki; Ezoe Yuichiro; Fabian Andrew; Ferrigno Carlo; Foster Adam; Fujimoto Ryuichi; Fukazawa Yasushi; Furuzawa Akihiro; Galeazzi Massimiliano; Gallo Luigi; Gandhi Poshak; Gilmore Kirk; Giustini Margherita; Goldwurm Andrea; Gu Liyi; Guainazzi Matteo; Haas Daniel; Haba Yoshito; Hagino Kouichi; Hamaguchi Kenji; Harayama Atsushi; Harrus Ilana; Hatsukade Isamu; Hayashi Takayuki; Hayashi Katsuhiro; Hayashida Kiyoshi; Hiraga Junko; Hirose Kazuyuki; Hornschemeier Ann; Hoshino Akio; Hughes John; Ichinohe Yuto; Iizuka Ryo; Inoue Yoshiyuki; Inoue Hajime; Ishibashi Kazunori; Ishida Manabu; Ishikawa Kumi; Ishimura Kosei; Ishisaki Yoshitaka; Itoh Masayuki; Iwata Naoko; Iyomoto Naoko; Jewell Chris; Kaastra Jelle; Kallman Timothy; Kamae Tuneyoshi; Kara Erin; Kataoka Jun; Katsuda Satoru; Katsuta Junichiro; Kawaharada Madoka; Kawai Nobuyuki; Kawano Taro; Kawasaki Shigeo; Khangulyan Dmitry; Kilbourne Caroline; Kimball Mark; King Ashley; Kitaguchi Takao; Kitamoto Shunji; Kitayama Tetsu; Kohmura Takayoshi; Kosaka Tatsuro; Koujelev Alex; Koyama Katsuji; Koyama Shu; Kretschmar Peter; Krimm Hans; Kubota Aya; Kunieda Hideyo; Laurent Philippe; Lebrun Francois; Lee Shiu-Hang; Leutenegger Maurice; Limousin Olivier; Loewenstein Michael; Long Knox; Lumb David; Madejski Grzegorz; Maeda Yoshitomo; Maier Daniel; Makishima Kazuo; Markevitch Maxim; Masters Candace; Matsumoto Hironori; Matsushita Kyoko; McCammon Dan; Mcguinness Daniel; McNamara Brian; Mehdipour Missagh; Miko Joseph; Miller Jon; Miller Eric; Mineshige Shin; Minesugi Kenji; Mitsuishi Ikuyuki; Miyazawa Takuya; Mizuno Tsunefumi; Mori Koji; Mori Hideyuki; Moroso Franco; Moseley Harvey; Muench Theodore; Mukai Koji; Murakami Hiroshi; Murakami Toshio; Mushotzky Richard; Nagano Housei; Nagino Ryo; Nakagawa Takao; Nakajima Hiroshi; Nakamori Takeshi; Nakano Toshio; Nakashima Shinya; Nakazawa Kazuhiro; Namba Yoshiharu; Natsukari Chikara; Nishioka Yusuke; Nobukawa Masayoshi; Nobukawa Kumiko; Noda Hirofumi; Nomachi Masaharu; O' Dell Steve; Odaka Hirokazu; Ogawa Hiroyuki; Ogawa Mina; Ogi Keiji; Ohno Masanori; Ohta Masayuki; Okajima Takashi; Okamoto Atsushi; Okazaki Tsuyoshi; Ota Naomi; Ozaki Masanobu; Paerels Frits; Paltani Stephane; Parmar Arvind; Petre Robert; Pinto Ciro; Pohl Martin; Pontius James; Porter F. Scott; Pottschmidt Katja; Ramsey Brian; Reynolds Christopher; Russell Helen; Safi-Harb Samar; Saito Shinya; Sakai Shin-ichiro; Sakai Kazuhiro; Sameshima Hiroaki; Sasaki Toru; Sato Goro; Sato Yoichi; Sato Kosuke; Sato Rie; Sawada Makoto; Schartel Norbert; Serlemitsos Peter; Seta Hiromi; Shibano Yasuko; Shida Maki; Shidatsu Megumi; Shimada Takanobu; Shinozaki Keisuke; Shirron Peter; Simionescu Aurora; Simmons Cynthia; Smith Randall; Sneiderman Gary; Soong Yang; Stawarz Lukasz; Sugawara Yasuharu; Sugita Hiroyuki; Sugita Satoshi; Szymkowiak Andrew; Tajima Hiroyasu; Takahashi Hiromitsu; Takeda Shin'ichiro; Takei Yoh; Tamagawa Toru; Tamura Takayuki; Tamura Keisuke; Tanaka Takaaki; Tanaka Yasuo; Tanaka Yasuyuki; Tashiro Makoto; Tawara Yuzuru; Terada Yukikatsu; Terashima Yuichi; Tombesi Francesco; Tomida Hiroshi; Tsuboi Yohko; Tsujimoto Masahiro; Tsunemi Hiroshi; Tsuru Takeshi; Uchida Hiroyuki; Uchiyama Yasunobu; Uchiyama Hideki; Ueda Yoshihiro; Ueda Shutaro; Ueno Shiro; Uno Shin'ichiro; Urry Meg; Ursino Eugenio; de Vries Cor; Wada Atsushi; Watanabe Shin; Watanabe Tomomi; Werner Norbert; Wik Daniel; Wilkins Dan; Williams Brian; Yamada Takahiro; Yamada Shinya; Yamaguchi Hiroya; Yamaoka Kazutaka; Yamasaki Noriko; Yamauchi Makoto; Yamauchi Shigeo; Yaqoob Tahir; Yatsu Yoichi; Yonetoku Daisuke; Yoshida Atsumasa; Yuasa Takayuki; Zhuravleva Irina; Zoghbi Abderahmen
SPACE TELESCOPES AND INSTRUMENTATION 2016: ULTRAVIOLET TO GAMMA RAY, Volume：9905, 2016, [Reviewed]
DOI：https://doi.org/10.1117/12.2232379
DOI ID：10.1117/12.2232379, ISSN：0277-786X, Web of Science ID：WOS:000387731500019 - THE TRANSIENT ACCRETING X-RAY PULSAR XTE J1946+274: STABILITY OF X-RAY PROPERTIES AT LOW FLUX AND UPDATED ORBITAL SOLUTION
Diana M. Marcu-Cheatham; Katja Pottschmidt; Matthias Kuehnel; Sebastian Mueller; Sebastian Falkner; Isabel Caballero; Mark H. Finger; Peter J. Jenke; Colleen A. Wilson-Hodge; Felix Fuerst; Victoria Grinberg; Paul B. Hemphill; Ingo Kreykenbohm; Dmitry Klochkov; Richard E. Rothschild; Yukikatsu Terada; Teruaki Enoto; Wataru Iwakiri; Michael T. Wolff; Peter A. Becker; Kent S. Wood; Joern Wilms
ASTROPHYSICAL JOURNAL, Volume：815, Number：1, Dec. 2015, [Reviewed]
We present a timing and spectral analysis of the X-ray pulsar XTE J1946+274 observed with Suzaku during an outburst decline in 2010 October and compare with previous results. XTE J1946+274 is a transient X-ray binary consisting of a Be-type star and a neutron star with a 15.75 s pulse period in a 172 days orbit with 2-3 outbursts per orbit during phases of activity. We improve the orbital solution using data from multiple instruments. The X-ray spectrum can be described by an absorbed Fermi-Dirac cut-off power-law model along with a narrow Fe K alpha line at 6.4 keV and a weak Cyclotron Resonance Scattering Feature (CRSF) at similar to 35 keV. The Suzaku data are consistent with the previously observed continuum flux versus iron line flux correlation expected from fluorescence emission along the line of sight. However, the observed iron line flux is slightly higher, indicating the possibility of a higher iron abundance or the presence of non-uniform material. We argue that the source most likely has only been observed in the subcritical (non-radiation dominated) state since its pulse profile is stable over all observed luminosities and the energy of the CRSF is approximately the same at the highest (similar to 5 x 10(37) erg s(-1)) and lowest (similar to 5. x 10(36) erg s(-1)) observed 3-60 keV luminosities.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.1088/0004-637X/815/1/44
DOI ID：10.1088/0004-637X/815/1/44, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000367105000044 - Sub-MeV band observation of a hard burst from AXP 1E 1547.0-5408 with the Suzaku Wide-band All-sky Monitor
Tetsuya Yasuda; Wataru B. Iwakiri; Makoto S. Tashiro; Yukikatsu Terada; Tomomi Kouzu; Teruaki Enoto; Yujin E. Nakagawa; Aya Bamba; Yuji Urata; Kazutaka Yamaoka; Masanori Ohno; Shinpei Shibata; Kazuo Makishima
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：67, Number：3, Jun. 2015, [Reviewed]
The 2.1-s anomalous X-ray pulsar 1E 1547.0-5408 exhibited an X-ray outburst on 2009 January 22, emitting a large number of short bursts. The wide-band all-sky monitor (WAM) on-board Suzaku detected at least 254 bursts in the 160 keV-6.2MeV band over the period of January 22 00: 57-17: 02 UT from the direction of 1E 1547.0-5408. One of these bursts, which occurred at 06: 45: 13, produced the brightest fluence in the 0.5-6.2 MeV range, with an averaged 0.16-6.2 MeV flux and extrapolated 25 keV-2 MeV fluence of about 1x10(-5) erg cm(-2) s(-1) and about 3x10(-4) erg cm(-2), respectively. After pile-up corrections, the time-resolved WAM spectra of this burst were well-fitted in the 0.16-6.2 MeV range by two-component models; specifically, a blackbody plus an optically thin thermal bremsstrahlung or a combination of a blackbody and a power-law component with an exponential cut-off. These results are compared with previous works reporting the persistent emission and weaker short bursts followed by the same outburst.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psv011
DOI ID：10.1093/pasj/psv011, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000356182500012 - Suzaku observation of X-ray variability in soft state LMCX-1
Shu Koyama; Shin'ya Yamada; Aya Kubota; Makoto S. Tashiro; Yukikatsu Terada; Kazuo Makishima
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：67, Number：3, Jun. 2015, [Reviewed]
This paper reports the results of Suzaku observation of the spectral variation of the black hole binary LMCX-1 in the soft state. The observation was carried out in 2009 from July 21 to 24. the obtained net count rate was similar to 30 counts s(-1) in the 0.5-50 keV band with similar to 10% peak-to-peak flux variation. The time-averaged X-ray spectrum cannot be described by a multi-color disk and single Compton component with its reflection, but requires additional Comptonized emissions. This double Compton component model allows a slightly larger inner radius of the multi-color disk, implying a lower spin parameter. Significant spectral evolution was observed above 8 keV along with a flux decrease on a timescale of similar to 10(4)-10(5) s. By spectral fitting, we show that this behavior is well explained by changes in the hard Comptonized emission component in contrast to the maintained disk and soft Comptonized emission.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psv017
DOI ID：10.1093/pasj/psv017, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000356182500017 - 27pSJ-3 CTA Report 98 : Result of characterization of PMTs for the first Large-Sized Telescope of CTA
Takahashi Mitsunari; Inome Yusuke; Umetsu Yohei; Ohoka Hideyuki; Orito Reiko; Katagiri Hideaki; Kushida Junko; Kubo Hidetoshi; Gunji Shuichi; Koyama Shu; Sawada Makoto; Tsujimoto Shimpei; Teshima Masahiro; Terada Yukikatsu; Tomono Yayoi; Nakajima Daisuke; Nagayoshi Tsutomu; Nishijima Kyoshi; Hayashida Masaaki; Bamba Aya; Matsuoka Shunsuke; Yamamoto Tokonatsu; CTA-Japan Consortium
Meeting Abstracts of the Physical Society of Japan, Volume：70, First page：392, Last page：392, 2015
The Physical Society of Japan (JPS), Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.70.2.0_392
DOI ID：10.11316/jpsgaiyo.70.2.0_392, ISSN：2189-079X, CiNii Articles ID：110010030854, CiNii Books ID：AA12721570 - 21pDD-5 CTA Report 90 : High precision measurement of PMTs for the first Large-Sized Telescope of CTA
Takahashi Mitsunari; Inome Yusuke; Umetsu Yohei; Ohoka Hideyuki; Ogino Momoko; Orito Reiko; Katagiri Hideaki; Kushida Junko; Kubo Hidetoshi; Gunji Shuichi; Koyama Shu; Sawada Makoto; Tsujimoto Shimpei; Tsubone Yoshio; Teshima Masahiro; Terada Yukikatsu; Tomono Yayoi; Nakajima Daisuke; Nagayoshi Tsutomu; Nishijima Kyoshi; Hanabata Yoshitaka; Hayashida Masaaki; Bamba Aya; Matsuoka Shunsuke; Yamamoto Tokonatsu; CTA-Japan consortium
Meeting Abstracts of the Physical Society of Japan, Volume：70, First page：410, Last page：410, 2015
The Physical Society of Japan (JPS), Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.70.1.0_410
DOI ID：10.11316/jpsgaiyo.70.1.0_410, ISSN：2189-079X, CiNii Articles ID：110009990600, CiNii Books ID：AA12721570 - 23pDK-4 Development status of Soft X-ray Spectrometer (SXS) onboard ASTRO-H (VI)
Ishisaki K.; Mitsuda K.; Yamasaki N.; Takei Y.; Tsujimoto M.; Ogawa M.; Sugita H.; Sato Y.; Shinozaki K.; Okamoto A.; Fujimoto R.; Ohashi T.; Ezoe Y.; Yamada S.; Konami S.; Tashiro M.; Terada Y.; H. Seta H. Seta; Kitamoto S.; Hoshino A.; Tamagawa T.; Ishikawa K.; Noda H.; Sato K.; Ota N.; Sawada M.; Mitsuishi I.; Murakami M.; Murakami H.; Iyomoto N.; Kelley R.L.; Kilbourne C.A.; Porter F.S.; Boyce K.R.; Eckart M.E.; Chiao M.P.; Leutenegger M.A.; Brown G.V.; McCammon D.; Szymkowiak A.; Herder J.-W. den; Haas D.; de Vries C.; Costantini E.; Akamatsu H.; Paltani S.; ASTRO-H SXS team
Meeting Abstracts of the Physical Society of Japan, Volume：70, First page：471, Last page：471, 2015
The Physical Society of Japan (JPS), Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.70.1.0_471
DOI ID：10.11316/jpsgaiyo.70.1.0_471, ISSN：2189-079X, CiNii Articles ID：110009990627, CiNii Books ID：AA12721570 - Summary of the session, white dwarf pulsars and rotating white dwarf theory
Yukikatsu Terada
The 13th Marcel Grossmann Meeting: On Recent Developments in Theoretical and Experimental General Relativity, Astrophysics and Relativistic Field Theories - Proceedings of the MG13 Meeting on General Relativity, 2012, Number：210699, First page：870, Last page：880, 2015, [Reviewed]
The origin of cosmic rays remains a mystery, even over 100 years since their discovery. Neutron stars (NSs) are considered textbook cases of particle acceleration sites in our Galaxy, but many unresolved numerical problems remain. Searches for new acceleration sites are crucial for astrophysics. The magnetized white dwarfs (MWDs) have the same kind of rotating magnetosphere as NSs, and may be the source of up to 10% of galactic cosmic ray electrons. In the parallel session of the “white dwarf pulsars and rotating white dwarf theory”, we focus on the current observational results on white dwarf pulsars, related theories of the radiation process both in white dwarfs and neutron stars, and the origin and rule of white dwarf pulsars, as well as surveying on the current theories of the internal structure and the equation of state of white dwarfs.
World Scientific, English, International conference proceedings
DOI：https://doi.org/10.1142/9789814623995_0043
DOI ID：10.1142/9789814623995_0043, SCOPUS ID：85045401491 - Search for non-thermal emission from isolated magnetized white dwarfs
Atsushi Harayama; Yukikatsu Terada; Takayuki Hayashi; Manabu Ishida
The 13th Marcel Grossmann Meeting: On Recent Developments in Theoretical and Experimental General Relativity, Astrophysics and Relativistic Field Theories - Proceedings of the MG13 Meeting on General Relativity, 2012, Number：210699, First page：2447, Last page：2449, 2015, [Reviewed]
In order to search for possible non-thermal emission like AE Aquarii, we picked up magnetized isolated white dwarfs (WDs) in addition to binaries including magnetized cataclysmic variables. Recently, many magnetized WDs are found by Sloan Digital Sky Survey project reaching 9000 objects including WDs showing a magnetic field strength of B ∼ 109 G. 82 objects were selected with known magnetic field strength and spin periods in terms of magnetic dipole momentum. The most promising object is EUVE J0317-855, which locates above death line of pulsars and has magnetic dipole radiation Erad ∼ 1.1×1029 erg/s. Then, we researched for non-thermal emission from isolated magnetized WDs with INTEGRAL, MAXI and Suzaku. As a result, no significant emissions were detected from isolated magnetized WDs with these instruments sensitivities.
World Scientific, English, International conference proceedings
DOI：https://doi.org/10.1142/9789814623995_0465
DOI ID：10.1142/9789814623995_0465, SCOPUS ID：85045392263 - The origin of ultrafast outflows in AGN: Monte Carlo simulations of the wind in PDS 456
Kouichi Hagino; Hirokazu Odaka; Chris Done; Poshak Gandhi; Shin Watanabe; Masao Sako; Tadayuki Takahashi
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, Volume：446, Number：1, First page：663, Last page：676, Jan. 2015, [Reviewed]
Ultrafast outflows (UFOs) are seen in many AGN, giving a possible mode for AGN feedback on to the host galaxy. However, the mechanism(s) for the launch and acceleration of these outflows are currently unknown, with UV line driving apparently strongly disfavoured as the material along the line of sight is so highly ionized that it has no UV transitions. We revisit this issue using the Suzaku X-ray data from PDS 456, an AGN with the most powerful UFO seen in the local Universe. We explore conditions in the wind by developing a new 3D Monte Carlo code for radiation transport. The code only handles highly ionized ions, but the data show the ionization state of the wind is high enough that this is appropriate, and this restriction makes it fast enough to explore parameter space. We reproduce the results of earlier work, confirming that the mass-loss rate in the wind is around 30 per cent of the inferred inflow rate through the outer disc. We show for the first time that UV line driving is likely to be a major contribution to the wind acceleration. The mass-loss rate in the wind matches that predicted from a purely line driven system, and this UV absorption can take place out of the line of sight. Continuum driving should also play a role as the source is close to Eddington. This predicts that the most extreme outflows will be produced from the highest mass accretion rate flows on to high-mass black holes, as observed.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/mnras/stu2095
DOI ID：10.1093/mnras/stu2095, ISSN：0035-8711, eISSN：1365-2966, Web of Science ID：WOS:000347518300047 - The Si/CdTe semiconductor Compton camera of the ASTRO-H Soft Gamma-ray Detector (SGD)
Shin Watanabe; Hiroyasu Tajima; Yasushi Fukazawa; Yuto Ichinohe; Shinichiro Takeda; Teruaki Enoto; Taro Fukuyama; Shunya Furui; Kei Genba; Kouichi Hagino; Atsushi Harayama; Yoshikatsu Kuroda; Daisuke Matsuura; Ryo Nakamura; Kazuhiro Nakazawa; Hirofumi Noda; Hirokazu Odaka; Masayuki Ohta; Mitsunobu Onishi; Shinya Saito; Goro Sato; Tamotsu Sato; Tadayuki Takahashi; Takaaki Tanaka; Atsushi Togo; Shinji Tomizuka
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：765, First page：192, Last page：201, Nov. 2014, [Reviewed]
The Soft Gamma-ray Detector (SGD) is one of the instrument payloads onboard ASTRO-H, and will cover a wide energy band (60-600 keV) at a background level 10 times better than instruments currently in orbit. The SGD achieves low background by combining a Compton camera scheme with a narrow field-of-view active shield. The Compton camera in the SGD is realized as a hybrid semiconductor detector system which consists of silicon and cadmium telluride (CdTe) sensors. The design of the SGD Compton camera has been finalized and the final prototype, which has the same configuration as the flight model, has been fabricated for performance evaluation. The Compton camera has overall dimensions of 12 cm×12 cm×12 cm, consisting of 32 layers of Si pixel sensors and 8 layers of CdTe pixel sensors surrounded by 2 layers of CdTe pixel sensors. The detection efficiency of the Compton camera reaches about 15% and 3% for 100 keV and 511 keV gamma rays, respectively. The pixel pitch of the Si and CdTe sensors is 3.2 mm, and the signals from all 13,312 pixels are processed by 208 ASICs developed for the SGD. Good energy resolution is afforded by semiconductor sensors and low noise ASICs, and the obtained energy resolutions with the prototype Si and CdTe pixel sensors are 1.0-2.0 keV (FWHM) at 60 keV and 1.6-2.5 keV (FWHM) at 122 keV, respectively. This results in good background rejection capability due to better constraints on Compton kinematics. Compton camera energy resolutions achieved with the final prototype are 6.3 keV (FWHM) at 356 keV and 10.5 keV (FWHM) at 662 keV, which satisfy the instrument requirements for the SGD Compton camera (better than 2%). Moreover, a low intrinsic background has been confirmed by the background measurement with the final prototype.
Elsevier, English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2014.05.127
DOI ID：10.1016/j.nima.2014.05.127, ISSN：0168-9002, SCOPUS ID：84908346398 - LONG-LASTING X-RAY EMISSION FROM TYPE IIb SUPERNOVA 2011dh AND MASS-LOSS HISTORY OF THE YELLOW SUPERGIANT PROGENITOR
Keiichi Maeda; Satoru Katsuda; Aya Bamba; Yukikatsu Terada; Yasushi Fukazawa
ASTROPHYSICAL JOURNAL, Volume：785, Number：2, Apr. 2014, [Reviewed]
Type IIb supernova (SN) 2011dh, with conclusive detection of an unprecedented yellow supergiant (YSG) progenitor, provides an excellent opportunity to deepen our understanding on the massive star evolution in the final centuries toward the SN explosion. In this paper, we report on detection and analyses of thermal X-ray emission from SN IIb 2011dh at similar to 500 days after the explosion on Chandra archival data, providing a solidly derived mass-loss rate of a YSG progenitor for the first time. We find that the circumstellar media should be dense, more than that expected from a Wolf-Rayet (W-R) star by one order of magnitude. The emission is powered by a reverse shock penetrating into an outer envelope, fully consistent with the YSG progenitor but not with a W-R progenitor. The density distribution at the outermost ejecta is much steeper than that expected from a compact W-R star, and this finding must be taken into account in modeling the early UV/optical emission from SNe IIb. The derived mass-loss rate is similar to 3x10(-6)M(circle dot) yr(-1) for the mass-loss velocity of similar to 20 km s(-1) in the final similar to 1300 yr before the explosion. The derived mass-loss properties are largely consistent with the standard wind mass-loss expected for a giant star. This is not sufficient to be a main driver to expel nearly all the hydrogen envelope. Therefore, the binary interaction, with a huge mass transfer having taken place at similar to 1300 yr before the explosion, is a likely scenario to produce the YSG progenitor.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.1088/0004-637X/785/2/95
DOI ID：10.1088/0004-637X/785/2/95, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000335736800014 - Search for Gravitational Waves Associated with γ-ray Bursts Detected by the Interplanetary Network
Yukikatsu Terada
Physical Review Letters, 2014
Scientific journal
DOI：https://doi.org/10.1103/PHYSREVLETT.113.011102
DOI ID：10.1103/PHYSREVLETT.113.011102, ORCID：67259851, Web of Science ID：WOS:000339091900001 - Development of the camera for the Large Size Telescopes of the Cherenkov Telescope Array
Y. Inome; G. Ambrosi; Y. Awane; H. Baba; A. Bamba; M. Barcelo; U. Barres de Almeida; J. A. Barrio; O. Blanch Bigas; J. Boix; L. Brunetti; E. Carmona; E. Chabanne; M. Chikawa; N. Cho; P. Colin; J. L. Conteras; J. Cortina; F. Dazzi; A. Deangelis; G. Deleglise; C. Delgado; C. Diaz; F. Dubois; A. Fiasson; D. Fink; N. Fouque; L. Freixas; C. Fruck; A. Gadola; R. Garcia; D. Gascon; N. Geffroy; N. Giglietto; F. Giordano; F. Granena; S. Gunji; R. Hagiwara; N. Hamer; Y. Hanabata; T. Hassan; K. Hatanaka; T. Haubold; M. Hayashida; R. Hermel; D. Herranz; K. Hirotani; J. Hose; D. Hugh; S. Inoue; Y. Inoue; K. Ioka; C. Jablonski; M. Kagaya; H. Katagiri; J. Kataoka; H. Kellermann; T. Kishimoto; M. Knoetig; K. Kodani; K. Kohri; T. Kojima; Y. Konno; S. Koyama; H. Kubo; J. Kushida; G. Lamanna; T. Le Flour; M. Lopez-Moya; R. Lopez; E. Lorenz; P. Majumdar; A. Manalaysay; M. Mariotti; G. Martinez; M. Martinez; S. Masuda; S. Matsuoka; D. Mazin; U. Menzel; J. M. Miranda; R. Mirzoyan; I. Monteiro; A. Moralejo; K. Murase; S. Nagataki; T. Nagayoshi; D. Nakajima; T. Nakamori; K. Nishijima; K. Noda; A. Nozato; M. Ogino; Y. Ohira; M. Ohishi; H. Ohoka; A. Okumura; S. Ono; R. Orito; J. L. Panazol; D. Paneque; R. Paoletti; J. M. Paredes; G. Pauletta; S. Podkladkin; J. Prast; R. Rando; O. Reimann; M. Ribo; S. Rosier-Lees; K. Saito; T. Saito; Y. Saito; N. Sakaki; R. Sakonaka; A. Sanuy; M. Sawada; V. Scalzotto; S. Schultz; T. Schweizer; T. Shibata; S. Shu; J. Sieiro; V. Stamatescu; S. Steiner; U. Straumann; R. Sugawara; H. Tajima; H. Takami; M. Takahashi; S. Tanaka; M. Tanaka; L. A. Tejedor; Y. Terada; M. Teshima; Y. Tomono; T. Totani; T. Toyama; Y. Tsubone; Y. Tsuchiya; S. Tsujimoto; H. Ueno; K. Umehara; Y. Umetsu; A. Vollhardt; R. Wagner; H. Wetteskind; T. Yamamoto; R. Yamazaki; A. Yoshida; T. Yoshida; T. Yoshikoshi
ADVANCES IN OPTICAL AND MECHANICAL TECHNOLOGIES FOR TELESCOPES AND INSTRUMENTATION, Volume：9151, First page：914542, Last page：8pp, 2014
The Large Size Telescopes, LSTs, located at the center of the Cherenkov Telescope Array, CTA, will be sensitive for low energy gamma-rays. The camera on the LST focal plane is optimized to detect low energy events based on a high photon detection efficiency and high speed electronics. Also the trigger system is designed to detect low energy showers as much as possible. In addition, the camera is required to work stably without maintenance in a few tens of years. In this contribution we present the design of the camera for the first LST and the status of its development and production.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2054619
DOI ID：10.1117/12.2054619, ISSN：0277-786X, Web of Science ID：WOS:000354525500123 - Development and verification of signal processing system of BGO active shield onboard Astro-H
Masanori Ohno; Shin'ya Tokuda; Takafumi Kawano; Shunya Furui; Ikumi Edahiro; Hiromitsu Takahashi; Kunihiro Goto; Yasushi Fukazawa; Hiroaki Murakami; Syogo Kobayashi; Soki Sakurai; Makoto Sasano; Shunsuke Torii; Toshio Nakano; Ko Ono; Kazuma Miyake; Terukazu Nishida; Kazuhiro Nakazawa; Kazuo Makishima; Kouichi Hagino; Takayuki Yuasa; Hirokazu Odaka; Rie Sato; Shin Watanabe; Motohide Kokubun; Tadayuki Takahashi; Goro Sato; Jun Kataoka; Tatsuhiko Saito; Kazutaka Yamaoka; Hiroyasu Tajima; Yoichi Yatsu; Takeshi Nakamori; Hideki Uchiyama; Daisuke Yonetoku
SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
The hard X-ray imager (HXI) and soft gamma-ray detector (SGD) onboard Astro-H observe astronomical objects with high sensitivity in the hard X-ray (5-80 keV) and soft gamma-ray (40-600 keV) energy bands. To achieve this high sensitivity, background rejection is essential, and these detectors are surrounded by large and thick bismuth germinate scintillators as an active shield. We have developed adequate trigger logic for both the HXI and SGD to process signals from main detector and BGO shield simultaneously and then we optimized the trigger delay and width, with consideration of the trigger latch efficiency. The shield detector system performs well, even after it is assembled as the HXI sensor. The energy threshold maintains the same level as that observed during the prototype development phase, and the experimental room background level of the main detector is successfully reduced by our optimized trigger timing.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2055676
DOI ID：10.1117/12.2055676, ISSN：0277-786X, Web of Science ID：WOS:000354529100166 - Development of the Hard X-ray Monitor onboard WF-MAXI
Makoto Arimoto; Yoichi Yatsu; Nobuyuki Kawai; Hirokazu Ikeda; Atsushi Harayama; Shin'ichiro Takeda; Tadayuki Takahashi; Hiroshi Tomida; Shiro Ueno; Masashi Kimura; Tatehiro Mihara; Motoko Serino; Hiroshi Tsunemi; Atsumasa Yoshida; Takanori Sakamoto; Takayoshi Kohmura; Hitoshi Negoro; Yoshihiro Ueda
SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, First page：91445Z, 2014
WF-MAXI is a mission to detect and localize X-ray transients with short-term variability as gravitational-wave (GW) candidates including gamma-ray bursts, supernovae etc. We are planning on starting observations by WF-MAXI to be ready for the initial operation of the next generation GW telescopes (e.g., KAGRA, Advanced LIGO etc.). WF-MAXI consists of two main instruments, Soft X-ray Large Solid Angle Camera (SLC) and Hard X-ray Monitor (HXM) which totally cover 0.7 keV to 1 MeV band. HXM is a multi-channel array of crystal scintillators coupled with APDs observing photons in the hard X-ray band with an effective area of above 100 cm(2). We have developed an analog application specific integrated circuit (ASIC) dedicated for the readout of 32-channel APDs' signals using 0.35 pm CMOS technology based on Open IP project and an analog amplifier was designed to achieve a low-noise readout. The developed ASIC showed a low-noise performance of 2080 e(-) + 2.3 e(-)/pF at root mean square and with a reverse-type APD coupled to a Ce:GAGG crystal a good FWHM energy resolution of 6.9% for 662 keV gamma-rays.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2054942
DOI ID：10.1117/12.2054942, ISSN：0277-786X, Web of Science ID：WOS:000354529100181 - DISCOVERY OF THE TRANSIENT MAGNETAR 3XMM J185246.6+003317 NEAR SUPERNOVA REMNANT KESTEVEN 79 WITH XMM-NEWTON
Ping Zhou; Yang Chen; Xiang-Dong Li; Samar Safi-Harb; Mariano Mendez; Yukikatsu Terada; Wei Sun; Ming-Yu Ge
ASTROPHYSICAL JOURNAL LETTERS, Volume：781, Number：1, Jan. 2014, [Reviewed]
We report the serendipitous discovery with XMM-Newton that 3XMM J185246.6+003317 is an 11.56 s X-ray pulsar located 1' away from the southern boundary of supernova remnant Kes 79. The spin-down rate of 3XMM J185246.6+003317 is < 1.1 x 10(-13) s s(-1), which, together with the long period P = 11.5587126(4) s, indicates a dipolar surface magnetic field of < 3.6 x 10(13) G, a characteristic age of >1.7 Myr, and a spin-down luminosity of <2.8 x 10(30) erg s(-1). Its X-ray spectrum is best-fitted with a resonant Compton scattering model and also can be adequately described by a blackbody model. The observations covering a seven-month span from 2008 to 2009 show variations in the spectral properties of the source, with the luminosity decreasing from 2.7 x 10(34) erg s(-1) to 4.6 x 10(33) erg s(-1), along with a decrease of the blackbody temperature from kT approximate to 0.8 keV to approximate to 0.6 keV. The X-ray luminosity of the source is higher than its spin-down luminosity, ruling out rotation as a power source. The combined timing and spectral properties, the non-detection of any optical or infrared counterpart, together with the lack of detection of the source in archival X-ray data prior to the 2008 XMM-Newton observation, point to 3XMM J185246.6+003317 being a newly discovered transient low-B magnetar undergoing an outburst decay during the XMM-Newton observations. The non-detection by Chandra in 2001 sets an upper limit of 4x 10(32) erg s(-1) to the quiescent luminosity of 3XMM J185246.6+003317. Its period is the longest among currently known transient magnetars. The foreground absorption toward 3XMM J185246.6+003317 is similar to that of Kes 79, suggesting a similar distance of similar to 7.1 kpc.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.1088/2041-8205/781/1/L16
DOI ID：10.1088/2041-8205/781/1/L16, ISSN：2041-8205, eISSN：2041-8213, Web of Science ID：WOS:000329582400016 - Sub-MeV all sky survey with a compact Si/CdTe Compton telescope
Nakazawa, Kazuhiro; Takahashi, Tadayuki; Watanabe, Shin; Ichinohe, Yuto; Takeda, Shin'ichiro; Enoto, Teruaki; Fukazawa, Yasushi; Kamae, Tuneyoshi; Kokubun, Motohide; Makishima, Kazuo; Mitani, Takefumi; Mizuno, Tsunefumi; Nomachi, Masaharu; Tajima, Hiroyasu; Takashima, Takeshi; Tamagawa, Toru; Terada, Yukikatsu; Tashiro, Makoto; Uchiyama, Yasunobu; Yoshimitsu, Tetsuo
SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
Recent progress in wide field of view or all-sky observations such as Swift/BAT hard X-ray monitor and Fermi GeV gamma-ray observatory has opened up a new era of time-domain high energy astro-physics addressing new insight in, e.g., particle acceleration in the universe. MeV coverage with comparable sensitivity, i.e. 1 similar to 10 mCrab is missing and a new MeV all-sky observatory is needed. These new MeV mission tend to be large, power-consuming and hence expensive, and its realization is yet to come. A compact sub-MeV (0.2-2 MeV) all-sky mission is proposed as a path finder for such mission. It is based on a Si/CdTe semiconductor Compton telescope technology employed in the soft gamma-ray detector onboard ASTRO-H, to be launched in to orbit on late 2015. The mission is kept as small as 0.5 x 0.5 x 0.4 m(3), 150 kg in weight and 200 W in power in place of the band coverage above a few MeV, in favor of early realization as a sub-payload to other large platforms, such as the international space station.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2055422
DOI ID：10.1117/12.2055422, ISSN：0277-786X, Web of Science ID：WOS:000354529100015 - The ASTRO-H X-ray Astronomy Satellite
Takahashi Tadayuki; Mitsuda Kazuhisa; Kelley Richard; Aharonian Felix; Akamatsu Hiroki; Akimoto Fumie; Allen Steve; Anabuki Naohisa; Angelini Lorella; Arnaud Keith; Asai Makoto; Audard Marc; Awaki Hisamitsu; Azzarello Philipp; Baluta Chris; Bamba Aya; Bando Nobutaka; Bautz Marshall; Bialas Thomas; Blandford Roger; Boyce Kevin; Brenneman Laura; Brown Greg; Cackett Edward; Canavan Edgar; Chernyakova Maria; Chiao Meng; Coppi Paolo; Costantini Elisa; de Plaa Jelle; den Herder Jan-Willem; DiPirro Michael; Done Chris; Dotani Tadayasu; Doty John; Ebisawa Ken; Enoto Teruaki; Ezoe Yuichiro; Fabian Andrew; Ferrigno Carlo; Foster Adam; Fujimoto Ryuichi; Fukazawa Yasushi; Funk Stefan; Furuzawa Akihiro; Galeazzi Massimiliano; Gallo Luigi; Gandhi Poshak; Gilmore Kirk; Guainazzi Matteo; Haas Daniel; Haba Yoshito; Hamaguchi Kenji; Harayama Atsushi; Hatsukade Isamu; Hayashi Katsuhiro; Hayashi Takayuki; Hayashida Kiyoshi; Hiraga Junko; Hirose Kazuyuki; Hornschemeier Ann; Hoshino Akio; Hughes John; Hwang Una; Iizuka Ryo; Inoue Yoshiyuki; Ishibashi Kazunori; Ishida Manabu; Ishikawa Kumi; Ishimura Kosei; Ishisaki Yoshitaka; Itoh Masayuki; Iwata Naoko; Iyomoto Naoko; Jewell Chris; Kaastra Jelle; Kallman Timothy; Kamae Tuneyoshi; Kataoka Jun; Katsuda Satoru; Katsuta Junichiro; Kawaharada Madoka; Kawai Nobuyuki; Kawano Taro; Kawasaki Shigeo; Khangaluyan Dmitry; Kilbourne Caroline; Kimball Mark; Kimura Masashi; Kitamoto Shunji; Kitayama Tetsu; Kohmura Takayoshi; Kokubun Motohide; Konami Saori; Kosaka Tatsuro; Koujelev Alexander; Koyama Katsuji; Krimm Hans; Kubota Aya; Kunieda Hideyo; LaMassa Stephanie; Laurent Philippe; Lebrun Francois; Leutenegger Maurice; Limousin Olivier; Loewenstein Michael; Long Knox; Lumb David; Madejski Grzegorz; Maeda Yoshitomo; Makishima Kazuo; Markevitch Maxim; Masters Candace; Matsumoto Hironori; Matsushita Kyoko; McCammon Dan; McGuinness Daniel; McNamara Brian; Miko Joseph; Miller Jon; Miller Eric; Mineshige Shin; Minesugi Kenji; Mitsuishi Ikuyuki; Miyazawa Takuya; Mizuno Tsunefumi; Mori Koji; Mori Hideyuki; Moroso Franco; Muench Theodore; Mukai Koji; Murakami Hiroshi; Murakami Toshio; Mushotzky Richard; Nagano Housei; Nagino Ryo; Nakagawa Takao; Nakajima Hiroshi; Nakamori Takeshi; Nakashima Shinya; Nakazawa Kazuhiro; Namba Yoshiharu; Natsukari Chikara; Nishioka Yusuke; Nobukawa Masayoshi; Noda Hirofumi; Nomachi Masaharu; Dell Steve O; Odaka Hirokazu; Ogawa Hiroyuki; Ogawa Mina; Ogi Keiji; Ohashi Takaya; Ohno Masanori; Ohta Masayuki; Okajima Takashi; Okazaki Tsuyoshi; Ota Naomi; Ozaki Masanobu; Paerels Frits; Paltani Stephane; Parmar Arvind; Petre Robert; Pinto Ciro; Pohl Martin; Pontius James; Porter F. Scott; Pottschmidt Katja; Ramsey Brian; Reis Rubens; Reynolds Christopher; Ricci Claudio; Russell Helen; Safi-Harb Samar; Saito Shinya; Sakai Shin-ichiro; Sameshima Hiroaki; Sato Kosuke; Sato Rie; Sato Goro; Sawada Makoto; Serlemitsos Peter; Seta Hiromi; Shibano Yasuko; Shida Maki; Shimada Takanobu; Shirron Peter; Simionescu Aurora; Simmons Cynthia; Smith Randall; Sneiderman Gary; Soong Yang; Stawarz Lukasz; Sugawara Yasuharu; Sugita Satoshi; Szymkowiak Andrew; Tajima Hiroyasu; Takahashi Hiroaki; Takahashi Hiromitsu; Takeda Shin-ichiro; Takei Yoh; Tamagawa Toru; Tamura Keisuke; Tamura Takayuki; Tanaka Takaaki; Tanaka Yasuyuki; Tanaka Yasuo; Tashiro Makoto; Tawara Yuzuru; Terada Yukikatsu; Terashima Yuichi; Tombesi Francesco; Tomida Hiroshi; Tsuboi Yoko; Tsujimoto Masahiro; Tsunemi Hiroshi; Tsuru Takeshi; Uchida Hiroyuki; Uchiyama Hideki; Uchiyama Yasunobu; Ueda Yoshihiro; Uedag Shutaro; Ueno Shiro; Uno Shinichiro; Urry Meg; Ursino Eugenio; de Vries Cor; Wada Atsushi; Watanabe Shin; Watanabe Tomomi; Werner Norbert; White Nicholas; Wilkins Dan; Yamada Shinya; Yamada Takahiro; Yamaguchi Hiroya; Yamaoka Kazutaka; Yamasaki Noriko; Yamauchi Makoto; Yamauchi Shigeo; Yadoob Tahir; Yatsu Yoichi; Yonetoku Daisuke; Yoshida Atsumasa; Yuasa Takayuki; Zhuravleva Irina; Zoghbi Abderahmen; ZuHone John
SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
DOI：https://doi.org/10.1117/12.2055681
DOI ID：10.1117/12.2055681, ISSN：0277-786X, Web of Science ID：WOS:000354529100065 - The Hard X-ray Imager (HXI) for the ASTRO-H mission
Goro Sato; Motohide Kokubun; Kazuhiro Nakazawa; Teruaki Enoto; Yasushi Fukazawa; Atsushi Harayama; Katsuhiro Hayashi; Jun Kataoka; Junichiro Katsuta; Madoka Kawaharada; Philippe Laurent; Francois Lebrun; Olivier Limousin; Kazuo Makishima; Tsunefumi Mizuno; Kunishiro Mori; Takeshi Nakamori; Hirofumi Noda; Hirokazu Odaka; Masanori Ohno; Masayuki Ohta; Shinya Saito; Rie Sato; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Shin'ichiro Takeda; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Shin Watanabe; Kazutaka Yamaoka; Yoichi Yatsu; Takayuki Yuasa
SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
The 6th Japanese X-ray satellite, ASTRO-H, is scheduled for launch in 2015. The hard X-ray focusing imaging system will observe astronomical objects with the sensitivity for detecting point sources with a brightness of 1/100,000 times fainter than the Crab nebula at > 10 keV. The Hard X-ray Imager (HXI) is a focal plane detector 12 m below the hard X-ray telescope (HXT) covering the energy range from 5 to 80 keV. The HXI is composed of a stacked Si/CdTe semiconductor detector module and surrounding BGO scintillators. The latter work as active shields for efficient reduction of background events caused by cosmic-ray particles, cosmic X-ray background, and in-orbit radiation activation. In this paper, we describe the detector system, and present current status of flight model development, and performance of HXI using an engineering model of HXI.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2055629
DOI ID：10.1117/12.2055629, ISSN：0277-786X, Web of Science ID：WOS:000354529100067 - Soft x-ray spectrometer (SXS): the high-resolution cryogenic spectrometer onboard ASTRO-H
Kazuhisa Mitsuda; Richard L. Kelley; Hiroki Akamatsu; Thomas Bialas; Kevin R. Boyce; Gregory V. Brown; Edgar Canavan; Meng Chiao; Elisa Costantini; Jan-Willem den Herder; Cor de Vries; Michael J. DiPirro; Megan E. Eckart; Yuichiro Ezoe; Ryuichi Fujimoto; Daniel Haas; Akio Hoshino; Kumi Ishikawa; Yoshitaka Ishisaki; Naoko Iyomoto; Caroline A. Kilbourne; Mark Kimball; Shunji Kitamoto; Saori Konami; Maurice A. Leutenegger; Dan McCammon; Joseph Miko; Ikuyuki Mitsuishi; Hiroshi Murakami; Masahide Murakami; Hirofumi Noda; Mina Ogawa; Takaya Ohashi; Atsushi Okamoto; Naomi Ota; Stephane Paltani; F. Scott Porter; Kosuke Sato; Yoichi Sato; Makoto Sawada; Hitomi Seta; Keisuke Shinozaki; Peter J. Shirron; Gary A. Sneiderman; Hiroyuki Sugita; Andrew Szymkowiak; Yoh Takei; Toru Tamagawa; Makoto S. Tashiro; Yukikatsu Terada; Masahiro Tsujimoto; Shinya Yamada; Noriko Y. Yamasaki
SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
We present the development status of the Soft X-ray Spectrometer (SXS) onboard the ASTRO-H mission. The SXS provides the capability of high energy-resolution X-ray spectroscopy of a FWHM energy resolution of < 7eV in the energy range of 0.3 - 10 keV. It utilizes an X-ray micorcalorimeter array operated at 50 mK. The SXS microcalorimeter subsystem is being developed in an EM-FM approach. The EM SXS cryostat was developed and fully tested and, although the design was generally confirmed, several anomalies and problems were found. Among them is the interference of the detector with the micro-vibrations from the mechanical coolers, which is the most difficult one to solve. We have pursued three different countermeasures and two of them seem to be effective. So far we have obtained energy resolutions satisfying the requirement with the FM cryostat.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2057199
DOI ID：10.1117/12.2057199, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000354529100070 - Soft Gamma-ray Detector (SGD) onboard the ASTRO-H
Yasushi Fukazawa; Hiroyasu Tajima; Shin Watanabe; Roger Blandford; Katsuhiro Hayashi; Atsushi Harayama; Jun Kataoka; Madoka Kawaharada; Motohide Kokubun; Philippe Laurent; Francois Lebrun; Olivier Limousin; Grzegorz M. Madejski; Kazuo Makishima; Tsunefumi Mizuno; Kunishiro Mori; Takeshi Nakamori; Kazuhiro Nakazawa; Hirofumi Noda; Hirokazu Odaka; Masanori Ohno; Masayuki Ohta; Shin'ya Saito; Goro Sato; Rie Sato; Shin'ichiro Takeda; Hiromitsu Takahashi; Tadayuki Takahashi; Yasuyuki Tanaka; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Kazutaka Yamaoka; Yoichi Yatsu; Daisuke Yonetoku; Takayuki Yuasa
SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
The Soft Gamma-ray Detector (SGD) is one of observational instruments onboard the ASTRO-H, and will provide 10 times better sensitivity in 60-600 keV than the past and current observatories. The SGD utilizes similar technologies to the Hard X-ray Imager (HXI) onboard the ASTRO-H. The SGD achieves low background by constraining gamma-ray events within a narrow field-of-view by Compton kinematics, in addition to the BGO active shield. In this paper, we will present the results of various tests using engineering models and also report the flight model production and evaluations.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2055292
DOI ID：10.1117/12.2055292, ISSN：0277-786X, Web of Science ID：WOS:000354529100071 - Performance verification and system integration tests of the pulse shape processor for the soft X-ray spectrometer onboard ASTRO-H
Sawako Takeda; Makoto S. Tashiro; Yoshitaka Ishisaki; Masahiro Tsujimoto; Hiromi Seta; Yuya Shimoda; Sunao Yamaguchi; Sho Uehara; Yukikatsu Terada; Ryuichi Fujimoto; Kazuhisa Mitsuda
SPACE TELESCOPES AND INSTRUMENTATION 2014: ULTRAVIOLET TO GAMMA RAY, Volume：9144, 2014, [Reviewed]
The soft X-ray spectrometer (SXS) aboard ASTRO-H is equipped with dedicated digital signal processing units called pulse shape processors (PSPs). The X-ray microcalorimeter system SXS has 36 sensor pixels, which are operated at 50 mK to measure heat input of X-ray photons and realize an energy resolution of 7 eV FWHM in the range 0.3-12.0 keV. Front-end signal processing electronics are used to filter and amplify the electrical pulse output from the sensor and for analog-to-digital conversion. The digitized pulses from the 36 pixels are multiplexed and are sent to the PSP over lowvoltage differential signaling lines. Each of two identical PSP units consists of an FPGA board, which assists the hardware logic, and two CPU boards, which assist the onboard software. The FPGA board triggers at every pixel event and stores the triggering information as a pulse waveform in the installed memory. The CPU boards read the event data to evaluate pulse heights by an optimal filtering algorithm. The evaluated X-ray photon data (including the pixel ID, energy, and arrival time information) are transferred to the satellite data recorder along with event quality information. The PSP units have been developed and tested with the engineering model (EM) and the flight model. Utilizing the EM PSP, we successfully verified the entire hardware system and the basic software design of the PSPs, including their communication capability and signal processing performance. In this paper, we show the key metrics of the EM test, such as accuracy and synchronicity of sampling clocks, event grading capability, and resultant energy resolution.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.2055899
DOI ID：10.1117/12.2055899, ISSN：0277-786X, Web of Science ID：WOS:000354529100162 - Design of the Time assignment System for ASTRO-H and Its Performance before Launch
Yukikatsu Terada; Sunao Yamaguchi; Shigenobu Sugimoto; Taku Inoue; Souhei Nakaya; Mina Ogawa; Tadayasu Dotani; Yoshitaka Ishisaki; Kazuyo Mizushima; Takashi Kominato; Hiroaki Mine; Hiroki Hihara; Kaori Iwase; Tomomi Kouzu; Makoto S. Tashiro; Chikara Natsukari; Masanobu Ozaki; Motohide Kokubun; Tadayuki Takahashi; Satoko Kawakami; Masan. Kasahara; Susumu Kumagai; Lorella Angelini; Michael Witthoeft
2014 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE (NSS/MIC), 2014, [Reviewed]
IEEE, English, International conference proceedings
Web of Science ID：WOS:000392917500464 - Discovery of recombining plasma in the supernova remnant 3C 391
Tamotsu Sato; Katsuji Koyama; Tadayuki Takahashi; Hirokazu Odaka; Shinya Nakashima
Publications of the Astronomical Society of Japan, Volume：66, Number：6, Dec. 2013, [Reviewed]
Recent X-ray study of middle-aged supernova remnants (SNRs) reveals strong radiative recombination continua (RRCs) associated with overionized plasmas, which origin still remains uncertain. We report a discovery of an RRC in the middle-aged SNR 3C∈391. If the X-ray spectrum is fitted with a two-temperature plasma model in collisional ionization equilibrium (CIE), residuals of a Si xiv Lyα line at 2.006 keV, a S xvi Lyα line at 2.623 keV and the edge of a RRC of Si xiii at 2.666 keV are found. In fact, the X-ray spectrum is well described by the composite model consisting of the CIE plasma and a recombining plasma (RP). The abundance pattern suggests that the RP is due to ejecta from core-collapse supernova of the progenitor mass of about 15∈M. There is no significant difference of the recombining parameters between the south-east region and the north-west region surrounded by dense molecular clouds. We also find a hint of a Fe i Kα line at 6.4 keV (2.4∈σ detection) from the south-east region of the SNR.
Oxford University Press, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/psu120
DOI ID：10.1093/pasj/psu120, ISSN：2053-051X, SCOPUS ID：84922562395 - THE INTERPLANETARY NETWORK SUPPLEMENT TO THE FERMI GBM CATALOG OF COSMIC GAMMA-RAY BURSTS
K. Hurley; V. D. Pal'shin; R. L. Aptekar; S. V. Golenetskii; D. D. Frederiks; E. P. Mazets; D. S. Svinkin; M. S. Briggs; V. Connaughton; C. Meegan; J. Goldsten; W. Boynton; C. Fellows; K. Harshman; I. G. Mitrofanov; D. V. Golovin; A. S. Kozyrev; M. L. Litvak; A. B. Sanin; A. Rau; A. von Kienlin; X. Zhang; K. Yamaoka; Y. Fukazawa; Y. Hanabata; M. Ohno; T. Takahashi; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; S. Barthelmy; T. Cline; N. Gehrels; J. Cummings; H. A. Krimm; D. M. Smith; E. Del Monte; M. Feroci; M. Marisaldi
ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES, Volume：207, Number：2, Aug. 2013, [Reviewed]
We present Interplanetary Network (IPN) data for the gamma-ray bursts in the first Fermi Gamma-Ray Burst Monitor (GBM) catalog. Of the 491 bursts in that catalog, covering 2008 July 12 to 2010 July 11, 427 were observed by at least one other instrument in the nine-spacecraft IPN. Of the 427, the localizations of 149 could be improved by arrival time analysis (or "triangulation"). For any given burst observed by the GBM and one other distant spacecraft, triangulation gives an annulus of possible arrival directions whose half-width varies between about 0.'4 and 32 degrees, depending on the intensity, time history, and arrival direction of the burst, as well as the distance between the spacecraft. We find that the IPN localizations intersect the 1 sigma GBM error circles in only 52% of the cases, if no systematic uncertainty is assumed for the latter. If a 6 degrees systematic uncertainty is assumed and added in quadrature, the two localization samples agree about 87% of the time, as would be expected. If we then multiply the resulting error radii by a factor of three, the two samples agree in slightly over 98% of the cases, providing a good estimate of the GBM 3 sigma error radius. The IPN 3 sigma error boxes have areas between about 1 arcmin(2) and 110 deg(2), and are, on the average, a factor of 180 smaller than the corresponding GBM localizations. We identify two bursts in the IPN/GBM sample that did not appear in the GBM catalog. In one case, the GBM triggered on a terrestrial gamma flash, and in the other, its origin was given as "uncertain." We also discuss the sensitivity and calibration of the IPN.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.1088/0067-0049/207/2/39
DOI ID：10.1088/0067-0049/207/2/39, ISSN：0067-0049, eISSN：1538-4365, Web of Science ID：WOS:000322710000021 - Spectral Variation of Hard X-Ray Emission from the Crab Nebula with the Suzaku Hard X-Ray Detector
Tomomi Kouzu; Makoto S. Tashiro; Yukikatsu Terada; Shin'ya Yamada; Aya Bamba; Teruaki Enoto; Koji Mori; Yasushi Fukazawa; Kazuo Makishima
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：65, Number：4, Aug. 2013, [Reviewed]
The Crab Nebula is one of the brightest and most stable sources in the X-ray sky. Year-scale flux variation from the object was recently revealed in the hard X-ray band by four satellites. This marked the first detection of year-scale variability from pulsar wind nebulae in the hard X-ray band. The Crab Nebula has been observed at least once a year for calibration purposes with the Suzaku Hard X-ray Detector (HXD) since its launch in 2005. In order to investigate possible spectral changes as well as flux variation, archival data of the HXD were analyzed. The flux variation reported by other instruments was confirmed in the 25-100 keV band by the HXD at a few percent level, but flux above 100 keV did not follow the trend in variation below 100 keV. The hardness ratios produced utilizing the PIN and GSO sensors installed in the HXD exhibit significant scattering, thereby indicating spectral variations in the hard X-ray band. The spectral changes were quantified by spectral fitting with a broken power-law model. The difference between the two photon indexes of the broken power-law model in harder and softer energy bands is in the range of < 2.54. Taking into account a flux variation of 6.3% and a spectral variation time-scale of a few days, multi components of the broken power-law-shaped synchrotron emission with different cooling times are suggested.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/65.4.74
DOI ID：10.1093/pasj/65.4.74, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000330328300005 - Search for Non-Thermal Emissions from an Isolated Magnetic White Dwarf, EUVE J0317-855, with Suzaku
Atsushi Harayama; Yukikatsu Terada; Manabu Ishida; Takayuki Hayashi; Aya Bamba; Makoto S. Tashiro
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：65, Number：4, Aug. 2013, [Reviewed]
To search for possible non-thermal emissions from magnetic white dwarfs (WDs), we selected the most suitable candidates from among magnetic cataclysmic variables and isolated WDs. After the magnetic cataclysmic variable AE Aquarii, which emits hard X-ray pulses, the isolated WD EUVE J0317-855 is expected to emit the second most powerful magnetic dipole radiation with energies reaching similar to 1.1 x 10(29) erg s(-1). EUVE J0317-855 was observed with Suzaku from 2009 July 16 to 2009 July 17 for about 60 ks. No significant emissions were detected from the object in the 0.5-10 keV band, and the upper limit of the X-ray flux was estimated to be 1.7 x 10(-13) erg cm(-2) s(-1) in the 2-10 keV band. This value corresponds to less than 0.05% of the calculated spin-down energy. It excludes the possibility of explaining soft gamma-ray repeaters and anomalous X-ray pulsars as WDs, but may indicate that the activity in the magnetosphere of WDs is not so different from that occurring in radio pulsars. Curvature radiation, which is one of the suggested mechanism for emissions from the magnetosphere of compact objects, may explain the observed X-ray flux of AE Aquarii, and is consistent with the non-detection of EUVE J0317-855.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/65.4.73
DOI ID：10.1093/pasj/65.4.73, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000330328300004 - An X-Ray Counterpart of HESS J1427-608 Discovered with Suzaku
Takahisa Fujinaga; Koji Mori; Aya Bamba; Shoichi Kimura; Tadayasu Dotani; Masanobu Ozaki; Keiko Matsuta; Gerd Puehlhofer; Hideki Uchiyama; Junko S. Hiraga; Hironori Matsumoto; Yukikatsu Terada
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：65, Number：3, Jun. 2013, [Reviewed]
We report on the discovery of an X-ray counterpart of the unidentified very high-energy gamma-ray source HESS J1427-608. In the sky field coincident with HESS J1427-608, an extended source was found in the 2-8 keV band, and was designated as Suzaku J1427-6051. Its X-ray radial profile has an extension of sigma = 0'.9 +/- 0'.1 if approximated by a Gaussian. The spectrum was well fitted by an absorbed power-law with N-H = (1.1 +/- 0.3) x 10(23) cm(-2), Gamma = 3.1(-0.5)(+0.6), and the unabsorbed flux F-X = (9(-2)(+4)) x 10(-13) erg s(-1) cm(-2) in the 2-10 keV band. Using XMM-Newton archive data, we found seven point sources in the Suzaku source region. However, because their total flux and absorbing column densities are more than an order of magnitude lower than those of Suzaku J1427-6051, we consider that they are unrelated to the Suzaku source. Thus, Suzaku J1427-6051 is considered to be a truly diffuse source and an X-ray counterpart of HESS J1427-608. The possible nature of HESS J1427-608 is discussed based on the observational properties.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/65.3.61
DOI ID：10.1093/pasj/65.3.61, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000321682000018 - Radiation effects on the silicon semiconductor detectors for the ASTRO-H mission
Katsuhiro Hayashi; Inchun Park; Kyohei Dotsu; Issei Ueno; Sho Nishino; Masayuki Matsuoka; Hajimu Yasuda; Yasushi Fukazawa; Takashi Ohsugi; Tsunefumi Mizuno; Hiromitsu Takahashi; Masanori Ohno; Satoru Endo; Takaaki Tanaka; Hiroyasu Tajima; Motohide Kokubun; Shin Watanabe; Tadayuki Takahashi; Kazuhiro Nakazawa; Yukio Uchihori; Hisashi Kitamura
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：699, First page：225, Last page：229, Jan. 2013, [Reviewed]
Hard X-ray Imager (HXI) and Soft Gamma-ray Detector (SGD) onboard the 6th Japanese X-ray satellite, ASTRO-H, utilize double-sided silicon strip detectors (DSSD) and pixel array-type silicon sensors (Si-pad), respectively. The DSSD with a 3.4 cm×3.4 cm area has an imaging capability in the lower energy band for the HXI covering 5-80 keV. The Si-pad consists of 16×16 pixels with a 5.4 cm×5.4 cm area and measures a photon direction with the Compton kinematics in 10-600 keV. Since the ASTRO-H will be operated in a low earth orbit, these detectors will be damaged by irradiation of cosmic-ray protons mainly in the South Atlantic Anomaly. In order to evaluate damage effects of the sensors, we have carried out irradiation tests with 150 MeV proton beams and 60Co gamma-rays with a total dose of 10-20 years irradiation level. In both experiments, the leakage current has increased by ∼0.2 - 1.1nA/ cm2 under an expected operation temperature at -15 °C, which resulted in the noise level within a tolerance of 20 years. In this report, we present a summary of the basic performance of silicon detectors, and radiation effects on them by the irradiation tests. © 2012 Elsevier B.V.
English, International conference proceedings
DOI：https://doi.org/10.1016/j.nima.2012.05.088
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=84870410466&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=84870410466&origin=inward
DOI ID：10.1016/j.nima.2012.05.088, ISSN：0168-9002, SCOPUS ID：84870410466 - X-ray searches for new galactic particle-acceleration sites with Suzaku .
Terada, Y.; Harayama, A.; Hayashi, T.; Dogtani, T.; Ishida, M.; Bamba, A.; Makishima, K.; Mukai, K.; Urata, Y.; Nitta, A.; de Jager, O.; Chadwick, P.; Wagner, S.; Buckley, D.; Tashiro, M. S.; Kouzu, T.; Koyama, S.; Yamazaki, R.
Memorie della Societa Astronomica Italiana, 2013
Origins of cosmic-rays are still mystery for 100 years from the discovery. Neutron stars (NSs) and supernova remnants (SNRs) are considered as textbook cases of particle acceleration sites, but many unresolved problems remain numerically. Searches for new sites are crucial for astrophysics. We focus on two candidates which can contribute a few to ten % of Galactic cosmic-ray electrons: magnetic white dwarfs (MWDs) and runaway O-stars. The former have rotating magnetospheres like NSs, and the latter have termination shocks by fast stellar winds like SNRs. We performed six observations of MWDs in binaries and three single MWDs with Suzaku, and found some evidences of particle acceleration from three. We performed Suzaku observation of a runaway-star BD+43 3654, from where Synchrotron radio emission is reported. The upper limit in X-ray flux indicates low Lorentz factor of electrons, meaning low-turbulent magnetic field in shock....
Scientific journal
ORCID：101134041, Bibcode：2013MmSAI..84..590T - All-sky observations by Suzaku wide-band all-sky monitor .
Ohno, M.; Hanabata, Y.; Kawano, T.; Takaki, K.; Nakamura, R.; Tanaka, Y.; Fukazawa, Y.; Ueno, H.; Tashiro, M.; Terada, Y.; Iwakiri, W.; Yasuda, T.; Asahina, M.; Kobayashi, S.; Sakamoto, A.; Ishida, Y.; Sugimoto, S.; Akiyama, M.; Ohmori, N.; Yamauchi, M.; Nakagawa, Y. E.; Sugita, S.; Yamaoka, K.; Kokubun, M.; Takahashi, T.; Urata, Y.; Tssai, P.; Nakazawa, K.; Makishima, K.; Suzaku-WAM Team
Memorie della Societa Astronomica Italiana, 2013
All-sky observation in wide energy band is important to study bright gamma-ray sources as well as other transient phenomena such as Gamma-ray Bursts (GRBs). Suzaku Wide-band All-sky Monitor (WAM) enables such all-sky observations up to soft gamma-ray band thanks to its wide energy coverage from 50 keV to 5000 keV with very large effective area of 400 cm2 even at 1 MeV. During seven year operations, the WAM has successfully detected more than 1000 GRBs, soft gamma repeaters (SGRs) and solar flares. In addition, long term variability of Crab nebula can be monitored with earth occultation technique. WAM also could provide good information of geomagnetically-trapped charged particles with daily monitoring data....
Scientific journal
ORCID：101134040, Bibcode：2013MmSAI..84..735O - Binaries with the eyes of CTA
Yukikatsu Terada
Astroparticle Physics, 2013
Scientific journal
DOI：https://doi.org/10.1016/J.ASTROPARTPHYS.2012.09.004
DOI ID：10.1016/J.ASTROPARTPHYS.2012.09.004, ORCID：67259932, Web of Science ID：WOS:000318126800022 - Introducing the CTA concept
Yukikatsu Terada
Astroparticle Physics, 2013
Scientific journal
DOI：https://doi.org/10.1016/J.ASTROPARTPHYS.2013.01.007
DOI ID：10.1016/J.ASTROPARTPHYS.2013.01.007, ORCID：67259917, Web of Science ID：WOS:000318126800002 - Search for Diffuse X-Rays from the Bow Shock Region of Runaway Star BD+43 3654 with Suzaku
Yukikatsu Terada; Makoto S. Tashiro; Aya Bamba; Ryo Yamazaki; Tomomi Kouzu; Shu Koyama; Hiromi Seta
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：64, Number：6, Dec. 2012, [Reviewed]
The bow shocks of runaway stars with strong stellar winds of over 2000 km s(-1) can serve as particle acceleration sites. The conversion from stellar wind luminosity into particle acceleration power has an efficiency of the same order of magnitude as those in supernova remnants, based on the radio emission from the bow shock region of runaway star BD +43 3654 (Benaglia et al. 2010, A&A, 517, L10). If this object exhibits typical characteristics, then runaway star systems can contribute a non-negligible fraction of Galactic cosmic-ray electrons. To constrain the maximum energy of accelerated particles from measurements of possible non-thermal emissions in the X-ray band, Suzaku observed BD +43 3654 in 2011 April with an exposure of 99 ks. Because the onboard instruments have a stable and low background level, Suzaku detected a possible enhancement over the background of 7.6 +/- 3.4 counts arcmin(-2) at the bow shock region, where the error represents the 3 a statistics only. However, the excess is not significant within the systematic errors of non-X-ray and cosmic-ray backgrounds of the X-ray Imaging Spectrometer, which are +/- 6.0 and +/- 34 counts arcmin(-2), respectively, and the 3 sigma upper limit in the X-ray luminosity from the shock region, which is 1.1 x 10(32) erg s(-1) per 41.2 arcmin(2) in the 0.5 to 10 keV band. This result leads to three conclusions: (1) a shock-heating process is inefficient on this system; (2) the maximum energy of electrons does not exceed similar to 10 TeV, corresponding to a Lorentz factor of less than 10(7); and (3) the magnetic field in the shock acceleration site might not be as turbulent as those in pulsar wind nebulae and supernova remnants.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/64.6.138
DOI ID：10.1093/pasj/64.6.138, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000313147700024 - The High-Resolution X-Ray Microcalorimeter Spectrometer, SXS, on Astro-H
Kazuhisa Mitsuda; Richard L. Kelley; Kevin R. Boyce; Gregory V. Brown; Elisa Costantini; Michael J. DiPirro; Yuichiro Ezoe; Ryuichi Fujimoto; Keith C. Gendreau; Jan-Willem den Herder; Akio Hoshino; Yoshitaka Ishisaki; Caroline A. Kilbourne; Shunji Kitamoto; Dan McCammon; Masahide Murakami; Hiroshi Murakami; Mina Ogawa; Takaya Ohashi; Atsushi Okamoto; Stephane Paltani; Martin Pohl; F. Scott Porter; Yoichi Sato; Keisuke Shinozaki; Peter J. Shirron; Gary A. Sneiderman; Hiroyuki Sugita; Andrew Szymkowiak; Yoh Takei; Toru Tamagawa; Makoto Tashiro; Yukikatsu Terada; Masahiro Tsujimoto; Cor de Vries; Noriko Y. Yamasaki
JOURNAL OF LOW TEMPERATURE PHYSICS, Volume：167, Number：5-6, First page：795, Last page：802, Jun. 2012, [Reviewed]
The science and an overview of the Soft X-ray Spectrometer onboard the STRO-H mission are presented. The SXS consists of X-ray focusing mirrors and a microcalorimeter array and is developed by international collaboration lead by JAXA and NASA with European participation. The detector is a 6x6 format microcalorimeter array operated at a cryogenic temperature of 50 mK and covers a 3'x3' field of view of the X-ray telescope of 5.6 m focal length. We expect an energy resolution better than 7 eV (FWHM, requirement) with a goal of 4 eV. The effective area of the instrument will be 225 cm(2) at 7 keV; by a factor of about two larger than that of the X-ray microcalorimeter on board Suzaku. One of the main scientific objectives of the SXS is to investigate turbulent and/or macroscopic motions of hot gas in clusters of galaxies.
SPRINGER/PLENUM PUBLISHERS, English, Scientific journal
DOI：https://doi.org/10.1007/s10909-012-0482-1
DOI ID：10.1007/s10909-012-0482-1, ISSN：0022-2291, eISSN：1573-7357, Web of Science ID：WOS:000303461600036 - POSSIBLE DETECTION OF AN EMISSION CYCLOTRON RESONANCE SCATTERING FEATURE FROM THE ACCRETION-POWERED PULSAR 4U 1626-67
W. B. Iwakiri; Y. Terada; T. Mihara; L. Angelini; M. S. Tashiro; T. Enoto; S. Yamada; K. Makishima; M. Nakajima; A. Yoshida
ASTROPHYSICAL JOURNAL, Volume：751, Number：1, First page：35, May 2012, [Reviewed]
We present analysis of 4U 1626-67, a 7.7 s pulsar in a low-mass X-ray binary system, observed with the hard X-ray detector of the Japanese X-ray satellite Suzaku in 2006 March for a net exposure of similar to 88 ks. The source was detected at an average 10-60 keV flux of similar to 4 x 10(-10) erg cm(-2) s(-1). The phase-averaged spectrum is reproduced well by combining a negative and positive power-law times exponential cutoff (NPEX) model modified at similar to 37 keV by a cyclotron resonance scattering feature (CRSF). The phase-resolved analysis shows that the spectra at the bright phases are well fit by the NPEX with CRSF model. On the other hand, the spectrum in the dim phase lacks the NPEX high-energy cutoff component, and the CRSF can be reproduced by either an emission or an absorption profile. When fitting the dim phase spectrum with the NPEX plus Gaussian model, we find that the feature is better described in terms of an emission rather than an absorption profile. The statistical significance of this result, evaluated by means of an F test, is between 2.91 x 10(-3) and 1.53 x 10(-5), taking into account the systematic errors in the background evaluation of HXD-PIN. We find that the emission profile is more feasible than the absorption one for comparing the physical parameters in other phases. Therefore, we have possibly detected an emission line at the cyclotron resonance energy in the dim phase.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.1088/0004-637X/751/1/35
DOI ID：10.1088/0004-637X/751/1/35, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000303814600035 - A spectral study of the black hole candidate XTE J1752-223 in the high/soft state with MAXI, Suzaku, and Swift
Satoshi Nakahira; Shu Koyama; Yoshihiro Ueda; Kazutaka Yamaoka; Mutsumi Sugizaki; Tatehiro Mihara; Masaru Matsuoka; Atsumasa Yoshida; Kazuo Makishima; Ken Ebisawa; Aya Kubota; Shin'ya Yamada; Hitoshi Negoro; Kazuo Hiroi; Masaki Ishikawa; Nobuyuki Kawai; Masashi Kimura; Hiroki Kitayama; Mitsuhiro Kohama; Takanori Matsumura; Mikio Morii; Motoki Nakajima; Motoko Serino; Megumi Shidatsu; Tetsuya Sootome; Kousuke Sugimori; Fumitoshi Suwa; Hiroshi Tomida; Yoko Tsuboi; Hiroshi Tsunemi; Shiro Ueno; Ryuichi Usui; Takayuki Yamamoto; Kyohei Yamazaki; Makoto S. Tashiro; Yukikatsu Terada; Hiromi Seta
Publications of the Astronomical Society of Japan, Volume：64, Number：1, Feb. 2012, [Reviewed]
We report on an X-ray spectral analysis of the black hole candidate XTE J1752-223 in the 2009-2010 outburst, utilizing data obtained with the MAXI/Gas Slit Camera (GSC), the Swift/XRT, and Suzaku, which work comple-mentarily. As already reported by Nakahira et al. (2010, PASJ, 62, L27), MAXI monitored the source continuously throughout the entire outburst for about eight months. All of the MAXI/GSC energy spectra in the high/soft state, lasting for 2 months, are well represented by a multi-color disk plus power-law model. The innermost disk temperature changed from ∼0.7 keV to ∼0.4 keV and the disk flux decreased by an order of magnitude. Nevertheless, the innermost radius is constant at ∼41 D 3.5 (cos i) -1/2 km, where D 3.5 is the source distance in units of 3.5kpc and i the inclination. The multi-color disk parameters obtained with the MAXI/GSC are consistent with those with the Swift/XRT and Suzaku. The Suzaku data also suggest a possibility that the disk emission is slightly Comptonized, which could account for broad iron-K features reported previously. Assuming that the obtained innermost radius represents the innermost stable circular orbit for a non-rotating black hole, we estimate the mass of the black hole to be 5.51 ± 0.28 M ⊙ D 3.5 (cos -1/2 , where the correction for the stress-free inner boundary condition and color hardening factor of 1.7 are taken into account. If the inclination is less than 49°, as suggested from radio monitoring of transient jets, and the soft-to-hard transition in 2010 April occurred at 1%-4% of Eddignton luminosity, the fitting of the Suzaku spectra with a relativistic accretion-disk model derives constraints on the mass and the distance to be 3.1-55M ⊙ and 2.3-22 kpc, respectively. This confirms that the compact object in XTE J1752-223 is a black hole. © 2012. Astronomical Society of Japan.
Scientific journal
DOI：https://doi.org/10.1093/pasj/64.1.13
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=84863287542&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=84863287542&origin=inward
DOI ID：10.1093/pasj/64.1.13, ISSN：0004-6264, SCOPUS ID：84863287542, Web of Science ID：WOS:000301307500013 - Scalable SpaceWire backplane system using μtCA
Takayuki Yuasa; Tadayuki Takahashi; Masaharu Nomachi; Makoto Ioki
2012 18th IEEE-NPSS Real Time Conference, RT 2012, 2012, [Reviewed]
In space instrumentation, a new-generation network interface called SpaceWire has been gaining its momentum following the standardization by the European Space Agency and the European Cooperation for Space Standardization. SpaceWire, providing a high-speed peer-to-peer serial data link and network capability, can be used as an infrastructure of intra-satellite data communication, and replaces a legacy shared-bus type data transfer interface such as MIL-STD-1553B. © 2012 IEEE.
English, International conference proceedings
DOI：https://doi.org/10.1109/RTC.2012.6418177
DOI ID：10.1109/RTC.2012.6418177, SCOPUS ID：84874251812 - First X-ray Detection from a Bow Shock Region of a Runaway Star, BD+43 degrees 3654, with Suzaku
Y. Terada; M. S. Tashiro; A. Bamba; R. Yamazaki; H. Seta; T. Kouzu; S. Koyama
SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND, Volume：1427, 2012, [Reviewed]
Searching for new types of particle-acceleration sites is important. Recently, Synchrotron emission has been reported from a bow shock region from a runway star BD+43 degrees 3654 with a radio observation by VLA. It was the first discovery of a non-thermal emission from a runaway star. In order to search for possible non-thermal tail in the X-ray band, we have performed the observation of the object BD+43 degrees 3654 with Suzaku in April 2011 with the exposure of 105 ksec. As a result, thanks to the stable low-background capability of the XIS, we detected X-rays around the bow shock region. The X-ray luminosity of the diffuse X-rays around the object was about 10(31) erg s(-1) in the 0.5 to 10 keV band. In addition, we also detected X-rays from the object itself, BD+43 degrees 3654, representing a thermal X-ray spectrum with a temperature of 0.6 keV at the luminosity of 1.3x10(31) erg s(-1) in the same band. Detail analyses will be reported in a future paper. The results suggest the conversion efficiency from the momentum of the stellar wind into accelerated electrons would be the same order of magnitudes of those seen in shocks of supernova remnants.
AMER INST PHYSICS, English, International conference proceedings
DOI：https://doi.org/10.1063/1.3696151
DOI ID：10.1063/1.3696151, ISSN：0094-243X, Web of Science ID：WOS:000302776900009 - The ASTRO-H X-ray observatory
Tadayuki Takahashi; Kazuhisa Mitsuda; Richard Kelley; Henri Aarts; Felix Aharonian; Hiroki Akamatsu; Fumie Akimotoe; Steve Allen; Naohisa Anabuki; Lorella Angelini; Keith Arnaud; Makoto Asai; Marc Audard; Hisamitsu Awaki; Philipp Azzarello; Chris Baluta; Aya Bamba; Nobutaka Bando; Mark Bautz; Roger Blandford; Kevin Boyce; Greg Brown; Ed Cackett; Maria Chernyakova; Paolo Coppi; Elisa Costantini; Jelle De Plaa; Jan Willem Den Herder; Michael DiPirro; Chris Done; Tadayasu Dotani; John Doty; Ken Ebisawa; Megan Eckart; Teruaki Enoto; Yuichiro Ezoe; Andrew Fabian; Carlo Ferrigno; Adam Foster; Ryuichi Fujimoto; Yasushi Fukazawa; Stefan Funk; Akihiro Furuzawa; Massimiliano Galeazzi; Luigi Gallo; Poshak Gandhi; Keith Gendreau; Kirk Gilmore; Daniel Haas; Yoshito Haba; Kenji Hamaguchi; Isamu Hatsukade; Takayuki Hayashi; Kiyoshi Hayashida; Junko Hiraga; Kazuyuki Hirose; Ann Hornschemeier; Akio Hoshino; John Hughes; Una Hwang; Ryo Iizuka; Yoshiyuki Inoue; Kazunori Ishibashi; Manabu Ishida; Kosei Ishimura; Yoshitaka Ishisaki; Masayuki Ito; Naoko Iwat; Naoko Iyomoto; Jelle Kaastr; Timothy Kallman; Tuneyoshi Kamae; Jun Kataoka; Satoru Katsuda; Hajime Kawahara; Madoka Kawaharada; Nobuyuki Kawai; Shigeo Kawasaki; Dmitry Khangaluyan; Caroline Kilbourne; Masashi Kimura; Kenzo Kinugasaa; Shunji Kitamoto; Tetsu Kitayama; Takayoshi Kohmura; Motohide Kokubun; Tatsuro Kosaka; Alex Koujelev; Katsuji Koyama; Hans Krimm; Aya Kubota; Hideyo Kunieda; Stephanie LaMass; Philippe Laurent; Francois Lebrun; Maurice Leutenegger; Olivier Limousin; Michael Loewenstein; Knox Long; David Lumb
Proceedings of SPIE - The International Society for Optical Engineering, Volume：8443, 2012, [Reviewed]
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 5 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. © 2012 SPIE.
International conference proceedings
DOI：https://doi.org/10.1117/12.926190
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=84871726495&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=84871726495&origin=inward
DOI ID：10.1117/12.926190, ISSN：0277-786X, SCOPUS ID：84871726495 - The Si/CdTe semiconductor detector for Hard X-ray Imager (HXI) onboard ASTRO-H
Kouichi Hagino; Toshio Nakano; Goro Sato; Shin-ichiro Takeda; Hirokazu Odaka; Shin Watanabe; Kazuhiro Nakazawa; Motohide Kokubun; Tadayuki Takahashi
HIGH ENERGY GAMMA-RAY ASTRONOMY, Volume：1505, First page：809, Last page：812, 2012, [Reviewed]
The hard X-ray imager (HXI) is the focal plane detector onboard ASTRO-H to be launched in 2014. By combining with the hard X-ray telescope, the HXI will realize the focusing imaging in the energy range from 5 up to 80 keV. The sensitivity of the HXI for an isolated point source will be two orders of magnitude better compared with previous missions. The hybrid structure composed of four layers of double-sided silicon strip detectors (DSSD) and one layer of cadmium telluride double-sided strip detector (CdTe-DSD) enables high detection efficiency in the hard X-ray band. The DSSD and CdTe-DSD for ASTRO-H have been developed, and their spectral and imaging performances were evaluated. By using two-strip events for the reconstructions of spectra and images, energy resolution of 1.0 keV at 13.9 keV and 2.0 keV at 59.5 keV, and sub-strip spatial resolution were achieved.
AMER INST PHYSICS, English, International conference proceedings
DOI：https://doi.org/10.1063/1.4772383
DOI ID：10.1063/1.4772383, ISSN：0094-243X, Web of Science ID：WOS:000312503500170 - PROSPECT OF STUDYING HARD X- AND GAMMA-RAYS FROM TYPE Ia SUPERNOVAE
Yukikatsu Terada
The Astrophysical Journal, Volume：760, Number：1, 2012, [Reviewed]
English, Scientific journal
DOI：https://doi.org/10.1088/0004-637X/760/1/54
DOI ID：10.1088/0004-637X/760/1/54, ORCID：67259976, Web of Science ID：WOS:000310922200054 - The time assignment system of ASTRO-H
Tomomi Kouzu; Kaori Iwase; Yuki Mishima; Yukikatsu Terada; Takayuki Yuasa; Yoshitaka Ishisaki; Makoto S. Tashiro; Motohide Kokubun; Masanobu Ozaki; Masaharu Nomachi; Tadayuki Takahashi
IEEE Nuclear Science Symposium Conference Record, First page：163, Last page：166, 2012, [Reviewed]
ASTRO-H is an X-ray astronomy satellite to be launched in 2014. The data acquisition system of this mission is realized with a standard network protocol, SpaceWire. Although the protocol itself is well designed, a new concept to grantee the quality of service will be installed to the ASTRO-H data acquisition system. Therefore, the verification of the design of the concept is essential in the initial phase of the development. The time assignment function is one of the important issues for the SpaceWire development. The accuracy of the absolute time of about 30 μs is required from science goals. The key point of the time assignment with SpaceWire network in the ASTRO-H system is how accurately sharing the time information. In this paper, our design of the time distribution and assignment system for ASTRO-H is shown. The results of our measurements of timing accuracy are also presented to show that the design will fulfill the goal of absolute timing accuracy. © 2011 IEEE.
English, International conference proceedings
DOI：https://doi.org/10.1109/NSSMIC.2011.6154471
DOI ID：10.1109/NSSMIC.2011.6154471, ISSN：1095-7863, SCOPUS ID：84863348846, Web of Science ID：WOS:000304755600030 - Recent Suzaku Studies of the X-ray Emission from Magnetars
Teruaki Enoto; Yujin E. Nakagawa; Toshio Nakano; Hiroyuki Nishioka; Tetsuya Yasuda; Yukikatsu Terada; Takanori Sakamoto; Kazuo Makishima
SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND, Volume：1427, 2012, [Reviewed]
Magnetars are a fascinating subclass of neutrons stars, mainly emerging in the X-ray frequency, with evidence of ultra-strong magnetic field exceeding the critical value, B-c = 4.4 x 10(13) G. So far, soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are believed to be magnetars, based on their slow rotations, high spin-down rates, and burst activities. From its launch, Suzaku has been observed 11 magnetars, and also performed some successful ToO observations of transient sources. Becoming new promising targets in the Suzaku era, the AO-4 Magnetar Key Project has been performed since 2009. Using a best combination of the XIS and the HXD, the hard X-ray tail above 10 keV was clearly detected from 7 of them, including at least two activated sources, together with the soft thermal component from all of them. These Suzaku investigations revealed that a broad-band (0.8-70 keV) spectra of known magnetars systematically change depending on their characteristic age and/or magnetic field. The hard X-rays of magnetars become weaker but harder for older and weak-field objects. In addition, we have been monitoring broad-band persistent X-ray spectra of transient magnetars, together with spectral diagnostics of their weak short bursts. Here we summarize latest Suzaku results on magnetars. Although the emission mechanism of the hard X-rays has not yet been explained by conventional interpretations, the future ASTRO-H mission is expected to provide a more unified understanding of magnetars.
AMER INST PHYSICS, English, International conference proceedings
DOI：https://doi.org/10.1063/1.3696153
DOI ID：10.1063/1.3696153, ISSN：0094-243X, Web of Science ID：WOS:000302776900011 - Suzaku observation of the VHE gamma-ray source HESS J1427-608
Takahisa Fujinaga; Koji Mori; Shoichi Kimura; Aya Bamba; Tadayasu Dotani; Masanobu Ozaki; Hideki Uchiyama; Hironori Matsumoto; Yukikatsu Terada; Gerd Puehlhofer
SUZAKU 2011: EXPLORING THE X-RAY UNIVERSE: SUZAKU AND BEYOND, Volume：1427, 2012, [Reviewed]
We present the analysis results of Suzaku observation of the unidentified very high energy (VHE) gamma-ray source, HESS J1427-608. In the XIS image, we found an extended source (referred as "Suzaku source"), which is positionally coincident with HESS J1427-608. In order to estimate the flux contribution of point sources within the field, we also analyzed the archival data of XMM-Newton. In the EPIC image, four point sources were detected within 4'.5 from the center of the VHE source. However, the flux and N-H are both significantly smaller than those of the Suzaku source. Thus, we consider that the XMM-Newton point sources are not related to the Suzaku source.
AMER INST PHYSICS, English, International conference proceedings
DOI：https://doi.org/10.1063/1.3696203
DOI ID：10.1063/1.3696203, ISSN：0094-243X, Web of Science ID：WOS:000302776900061 - Concept of a small satellite for sub-MeV & MeV all sky survey: the CAST mission
Nakazawa, Kazuhiro; Takahashi, Tadayuki; Ichinohe, Yuto; Takeda, Shin'ichiro; Tajima, Hiroyasu; Kamae, Tuneyoshi; Kokubun, Motohide; Takashima, Takeshi; Tashiro, Makoto; Tamagawa, Toru; Terada, Yukikatsu; Nomachi, Masaharu; Fukazawa, Yasushi; Makishima, Kazuo; Mizuno, Tsunefumi; Mitani, Takefumi; Yoshimitsu, Tetsuo; Watanabe, Shin
SPACE TELESCOPES AND INSTRUMENTATION 2012: ULTRAVIOLET TO GAMMA RAY, Volume：8443, 2012, [Reviewed]
MeV and sub-MeV energy band from similar to 200 keV to similar to 2 MeV contains rich information of high-energy phenomena in the universe. The CAST (Compton Telescope for Astro and Solar Terrestrial) mission is planned to be launched at the end of 2010s, and aims at providing all-sky map in this energy-band for the first time. It is made of a semiconductor Compton telescope utilizing Si as a scatterer and CdTe as an absorber. CAST provides all-sky sub-MeV polarization map for the first time, as well. The Compton telescope technology is based on the design used in the Soft Gamma-ray Detector (SGD) onboard ASTRO-H, characterized by its tightly stacked semiconductor layers to obtain high Compton reconstruction efficiency. The CAST mission is currently planned as a candidate for the small scientific satellite series in ISAS/JAXA, weighting about 500 kg in total. Scalable detector design enables us to consider other options as well. Scientific outcome of CAST is wide. It will provide new information from high-energy sources, such as AGN and/or its jets, supernova remnants, magnetors, black-hole and neutron-star binaries and others. Polarization map will tell us about activities of jets and reflections in these sources, as well. In addition, CAST will simultaneously observe the Sun, and depending on its attitude, the Earth.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.926164
DOI ID：10.1117/12.926164, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000312391600011 - The Hard X-ray Imager (HXI) for the ASTRO-H mission
Motohide Kokubun; Kazuhiro Nakazawa; Teruaki Enoto; Yasushi Fukazawa; Jun Kataoka; Madoka Kawaharada; Philippe Laurent; Francois Lebrun; Olivier Limousin; Kazuo Makishima; Tsunefumi Mizuno; Kunishiro Mori; Takeshi Nakamori; Hirokazu Odaka; Masanori Ohno; Masayuki Ohta; Goro Sato; Rie Sato; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Takaaki Tanaka; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Shin Watanabe; Yoichi Yatsu; Takayuki Yuasa
SPACE TELESCOPES AND INSTRUMENTATION 2012: ULTRAVIOLET TO GAMMA RAY, Volume：8443, 2012, [Reviewed]
The Hard X-ray Imager (HXI) is one of the four detectors on board the ASTRO-H mission (6th Japanese X-ray satellite), which is scheduled to be launched in 2014. Using the hybrid structure composed of double-sided silicon strip detectors and a cadmium telluride double-sided strip detector, both with a high spatial resolution of 250 mu m. Combined with the hard X-ray telescope (HXT), it consists a hard X-ray imaging spectroscopic instrument covering the energy range from 5 to 80 keV with an effective area of >300 cm(2) in total at 30 keV. An energy resolution of 1-2 keV (FWHM) and lower threshold of 5 keV are both achieved with using a low noise front-end ASICs. In addition, the thick BGO active shields surrounding the main detector package is a heritage of the successful performance of the Hard X-ray Detector on board the Suzaku satellite. This feature enables the instrument to achieve an extremely good reduction of background caused by cosmic-ray particles, cosmic X-ray background, and in-orbit radiation activation. In this paper, we present the detector concept, design, latest results of the detector development, and the current status of the hardware.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.925648
DOI ID：10.1117/12.925648, ISSN：0277-786X, Web of Science ID：WOS:000312391600058 - Soft Gamma-ray Detector for the ASTRO-H mission
Shin Watanabe; Hiroyasu Talima; Yasushi Fukazawa; Roger Blandford; Teruaki Enoto; Jun Kataoka; Madoka Kawaharada; Motohide Kokubun; Philippe Laurent; Francois Lebrun; Olivier Limousin; Greg Madejski; Kazuo Makishima; Tsunefumi Mizuno; Takeshi Nakamori; Kazuhiro Nakazawa; Kunishiro Mori; Hirokazu Odaka; Masanori Ohno; Masayuki Ohta; Goro Sato; Rie Sato; Shin'ichiro Takeda; Hiromitsu Takahashi; Tadayuki Takahashi; Takaaki Tanaka; Makoto Tashiro; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Shinya Yamada; Yoichi Yatsu; Daisuke Yonetoku; Takayuki Yuasa
SPACE TELESCOPES AND INSTRUMENTATION 2012: ULTRAVIOLET TO GAMMA RAY, Volume：8443, 2012, [Reviewed]
ASTRO-H is the next generation JAXA X-ray satellite, intended to carry instruments with broad energy coverage and exquisite energy resolution. The Soft Gamma-ray Detector (SGD) is one of ASTRO-H instruments and will feature wide energy band (60-600 keV) at a background level 10 times better than the current instruments on orbit. The SGD is complimentary to ASTRO-H's Hard X-ray Imager covering the energy range of 5-80 keV. The SGD achieves low background by combining a Compton camera scheme with a narrow field-of-view active shield where Compton kinematics is utilized to reject backgrounds. The Compton camera in the SGD is realized as a hybrid semiconductor detector system which consists of silicon and CdTe (cadmium telluride) sensors. Good energy resolution is afforded by semiconductor sensors, and it results in good background rejection capability due to better constraints on Compton kinematics. Utilization of Compton kinematics also makes the SGD sensitive to the gamma-ray polarization, opening up a new window to study properties of gamma-ray emission processes. In this paper, we will present the detailed design of the SGD and the results of the final prototype developments and evaluations. Moreover, we will also present expected performance based on the measurements with prototypes.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.925977
DOI ID：10.1117/12.925977, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000312391600059 - A Monte Carlo simulation framework to study ASTRO-H in-orbit radiation and detector responses based on Geant4 toolkit
Masanobu Ozaki; Hirokazu Odaka; Tamotsu Sato; Tetsuya Yasuda; Makoto Asai; Kazuyoshi Hiragi; Tsunefumi Mizuno; Hideyuki Mori; Yukikatsu Terada; Akihiro Furuzawa
SPACE TELESCOPES AND INSTRUMENTATION 2012: ULTRAVIOLET TO GAMMA RAY, Volume：8443, 2012, [Reviewed]
We are developing an ASTRO-H data analysis framework with the Geant4-based Monte Carlo simulation core, and numerical models of the on-orbit environmental radiation and full-satellite mass structure. The framework uses not only Geant4 but also a traditional X-ray mirror ray-tracing simulator, and a file format compatible with the SimX simulator for input and output of celestial body information. The data exchange between the framework and the external software is based on FITS files, which makes it easy to record and trace the internal steps of the whole simulation framework.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.925879
DOI ID：10.1117/12.925879, ISSN：0277-786X, Web of Science ID：WOS:000312391600147 - In-orbit activation study of ASTRO-H X-ray observatory using Geant4
Tamotsu Sato; Hirokazu Odaka; Kazuyoshi Hiragi; Tsunefumi Mizuno; Masatoshi Ohno; Yasushi Fukazawa; Masayuki Ohta; Yuu Koseki; Shin Watanabe; Motohide Kokubun; Tadayuki Takahashi; Masanobu Ozaki; Makoto Asai; Hiroyasu Tajima; Tetsuya Yasuda; Yukikatsu Terada; Yukio Uchibori; Hisashi Kitamura
IEEE Nuclear Science Symposium Conference Record, First page：1727, Last page：1730, 2012, [Reviewed]
We are developing an integrated simulation framework based on Geant4 to estimate in-orbit performance of instruments onboard ASTRO-H, the international X-ray observatory to be launched in 2014. One of the most important purposes of our simulation is to estimate radiation background of the Hard X-ray Imager (HXI) and the Soft Gamma-ray Detector (SGD), both of which are composed of CdTe and silicon. We developed a new code based on Geant4 to handle the generation and the decay of radioactive nuclei and to estimate the activation of CdTe detector. In addition, to verify simulation results, we performed beam irradiation experiments at NIRS HIMAC using 150 MeV protons, which is typical energy of protons reaching to the CdTe detectors placed in the shielding materials, and measured the activation background spectra for several months. Our simulation results show good agreements with the experimental data. © 2012 IEEE.
English, International conference proceedings
DOI：https://doi.org/10.1109/NSSMIC.2012.6551405
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=84881572872&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=84881572872&origin=inward
DOI ID：10.1109/NSSMIC.2012.6551405, ISSN：1095-7863, SCOPUS ID：84881572872, Web of Science ID：WOS:000326814201176 - Improvements in Calibration of GSO Scintillators in the Suzaku Hard X-Ray Detector
Shin'ya Yamada; Kazuo Makishima; Kazuhiro Nakazawa; Motohide Kokubun; Madoka Kawaharada; Takao Kitaguchi; Shin Watanabe; Hiromitsu Takahashi; Hirofumi Noda; Hiroyuki Nishioka; Kazuyoshi Hiragi; Katsuhiro Hayashi; Kenta Nakajima; Makoto Tashiro; Makoto Sasano; Sho Nishino; Shunsuke Torii; Soki Sakurai; Tadayuki Takahashi; Tsunefumi Mizuno; Teruaki Enoto; Takayuki Yuasa; Takaaki Tanaka; Tomomi Kouzu; Toshio Nakano; Yasushi Fukazawa; Yukikatsu Terada; Yasunobu Uchiyama; Wataru Iwakiri
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：63, First page：S645, Last page：S656, Nov. 2011, [Reviewed]
Improvements of the in-orbit calibration of GSO scintillators in the Hard X-ray Detector aboard Suzaku are reported. To resolve an apparent change in the energy scale of GSO, which appeared across the launch for unknown reasons, consistent and thorough re-analyses of both pre-launch and in-orbit data have been performed. With laboratory experiments using spare hardware, the pulse-height offset, corresponding to zero energy input, was found to change by similar to 0.5% of the full analog voltage scale, depending on the power supply. Furthermore, by carefully calculating all of the light outputs of secondaries from activation lines used in the in-orbit gain determination, their energy deposits in GSO were found to be effectively lower, by several percent, than their nominal energies. Taking both of these effects into account, the in-orbit data agree with the on-ground measurements within similar to 5%, without employing the artificial correction introduced in previous work (Kokubun et al. 2007, PASJ, 59, S53). With this knowledge, we updated the data processing, the response, and the auxiliary files of GSO, and reproduced the HXD-PIN and HXD-GSO spectra of the Crab Nebula over 12-300 keV by a broken power-law with a break energy of similar to 110 keV.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/63.sp3.S645
DOI ID：10.1093/pasj/63.sp3.S645, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000299191800003 - Suzaku Observation of the Intermediate Polar V1223 Sagittarii
Takayuki Hayashi; Manabu Ishida; Yukikatsu Terada; Aya Bamba; Takeshi Shionome
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：63, First page：S739, Last page：S750, Nov. 2011, [Reviewed]
We report on the Suzaku observation of the intermediate polar V1223 Sagittarii. Using a multi-temperature plasma emission model with its reflection from a cold matter, we obtained the shock temperature to be 37.9(-4.6)(+5.1) keV. This constrains the mass and the radius of the white dwarf (WD) in the ranges 0.82(-0.06)(+0.05) M-circle dot and (6.9 +/- 0.4) x 10(8) cm, respectively, with the aid of a WD mass radius relation. The solid angle of the reflector viewed from the post-shock plasma was measured to be Omega/2 pi = 0.91 +/- 0.26. A fluorescent iron K alpha emission line was detected, whose central energy was discovered to be modulated with the WD rotation for the first time in magnetic-CVs. Detailed spectral analysis indicates that the line comprises a stable 6.4 keV component and a red-shifted component, the latter of which appears only around the rotational intensity-minimum phase. The equivalent width (EW) of the former stable component, similar to 80 eV, together with the measured Omega indicates that the major reflector is the WD surface, and the shock height is not more than 7% of the WD radius. Comparing this limitation to the height predicted by the Aizu model (Aizu, 1973, Prog. Theor. Phys., 50, 344), we estimated the fractional area onto which the accretion occurs to be <7 x 10(-3) of the WD radius, which is the most severe constraint in non-eclipsing IPs. The red-shifted iron line component, on the other hand, can be interpreted as emanating from the pre-shock accretion flow via fluorescence. Its EW (28(-13)(+44) eV) and the central energy (6.30(-0.05)(+0.07) keV) at the intensity-minimum phase are consistent with this interpretation.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/63.sp3.S739
DOI ID：10.1093/pasj/63.sp3.S739, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000299191800012 - Search for gravitational wave bursts from six magnetars
J. Abadie; B. P. Abbott; R. Abbott; M. Abernathy; T. Accadia; F. Acernese; C. Adams; R. Adhikari; C. Affeldt; B. Allen; G. S. Allen; E. Amador Ceron; D. Amariutei; R. S. Amin; S. B. Anderson; W. G. Anderson; F. Antonucci; K. Arai; M. A. Arain; M. C. Araya; S. M. Aston; P. Astone; D. Atkinson; P. Aufmuth; C. Aulbert; B. E. Aylott; S. Babak; P. Baker; G. Ballardin; S. Ballmer; D. Barker; S. Barnum; F. Barone; B. Barr; P. Barriga; L. Barsotti; M. Barsuglia; M. A. Barton; I. Bartos; R. Bassiri; M. Bastarrika; A. Basti; J. Bauchrowitz; Th S. Bauer; B. Behnke; M. G. Beker; A. S. Bell; A. Belletoile; I. Belopolski; M. Benacquista; A. Bertolini; J. Betzwieser; N. Beveridge; P. T. Beyersdorf; I. A. Bilenko; G. Billingsley; J. Birch; S. Birindelli; R. Biswas; M. Bitossi; M. A. Bizouard; E. Black; J. K. Blackburn; L. Blackburn; D. Blair; B. Bland; M. Blom; O. Bock; T. P. Bodiya; C. Bogan; R. Bondarescu; F. Bondu; L. Bonelli; R. Bonnand; R. Bork; M. Born; V. Boschi; S. Bose; L. Bosi; B. Bouhou; M. Boyle; S. Braccini; C. Bradaschia; P. R. Brady; V. B. Braginsky; J. E. Brau; J. Breyer; D. O. Bridges; A. Brillet; M. Brinkmann; V. Brisson; M. Britzger; A. F. Brooks; D. A. Brown; A. Brummit; R. Budzyński; T. Bulik; H. J. Bulten; A. Buonanno; J. Burguet-Castell; O. Burmeister; D. Buskulic; C. Buy; R. L. Byer; L. Cadonati; G. Cagnoli; J. Cain; E. Calloni; J. B. Camp; E. Campagna; P. Campsie; J. Cannizzo; K. Cannon; B. Canuel; J. Cao; C. Capano; F. Carbognani; S. Caride; S. Caudill; M. Cavaglià; F. Cavalier; R. Cavalieri; G. Cella; C. Cepeda; E. Cesarini; O. Chaibi; T. Chalermsongsak; E. Chalkley; P. Charlton; E. Chassande-Mottin; S. Chelkowski; Y. Chen; A. Chincarini; N. Christensen; S. S.Y. Chua; C. T.Y. Chung; S. Chung; F. Clara; D. Clark; J. Clark; J. H. Clayton; F. Cleva; E. Coccia; C. N. Colacino; J. Colas; A. Colla; M. Colombini; R. Conte; D. Cook; T. R. Corbitt; N. Cornish; A. Corsi; C. A. Costa; M. Coughlin; J. P. Coulon; D. M. Coward; D. C. Coyne; J. D.E. Creighton; T. D. Creighton; A. M. Cruise; R. M. Culter; A. Cumming; L. Cunningham; E. Cuoco; K. Dahl; S. L. Danilishin; R. Dannenberg; S. D'Antonio; K. Danzmann; K. Das; V. Dattilo; B. Daudert; H. Daveloza; M. Davier; G. Davies; E. J. Daw; R. Day; T. Dayanga; R. De Rosa; D. DeBra; G. Debreczeni; J. Degallaix; M. Del Prete; T. Dent; V. Dergachev; R. DeRosa; R. DeSalvo; S. Dhurandhar; L. Di Fiore; A. Di Lieto; I. Di Palma; M. Di Paolo Emilio; A. Di Virgilio; M. Díaz; A. Dietz; F. Donovan; K. L. Dooley; S. Dorsher; E. S.D. Douglas; M. Drago; R. W.P. Drever; J. C. Driggers; J. C. Dumas; S. Dwyer; T. Eberle; M. Edgar; M. Edwards; A. Effler; P. Ehrens; R. Engel; T. Etzel; M. Evans; T. Evans; M. Factourovich; V. Fafone; S. Fairhurst; Y. Fan; B. F. Farr; D. Fazi; H. Fehrmann; D. Feldbaum; I. Ferrante; F. Fidecaro; L. S. Finn; I. Fiori; R. Flaminio; M. Flanigan; S. Foley; E. Forsi; L. A. Forte; N. Fotopoulos; J. D. Fournier; J. Franc; S. Frasca; F. Frasconi; M. Frede; M. Frei; Z. Frei; A. Freise; R. Frey; T. T. Fricke; D. Friedrich; P. Fritschel; V. V. Frolov; P. Fulda; M. Fyffe; M. Galimberti; L. Gammaitoni; J. Garcia; J. A. Garofoli; F. Garufi; M. E. Gáspár; G. Gemme; E. Genin; A. Gennai; S. Ghosh; J. A. Giaime; S. Giampanis; K. D. Giardina; A. Giazotto; C. Gill; E. Goetz; L. M. Goggin; G. González; M. L. Gorodetsky; S. Goßler; R. Gouaty; C. Graef; M. Granata; A. Grant; S. Gras; C. Gray; R. J.S. Greenhalgh; A. M. Gretarsson; C. Greverie; R. Grosso; H. Grote; S. Grunewald; G. M. Guidi; C. Guido; R. Gupta; E. K. Gustafson; R. Gustafson; B. Hage; J. M. Hallam; D. Hammer; G. Hammond; J. Hanks; C. Hanna; J. Hanson; J. Harms; G. M. Harry; I. W. Harry; E. D. Harstad; M. T. Hartman; K. Haughian; K. Hayama; J. F. Hayau; T. Hayler; J. Heefner; H. Heitmann; P. Hello; M. A. Hendry; I. S. Heng; A. W. Heptonstall; V. Herrera; M. Hewitson; S. Hild; D. Hoak; K. A. Hodge; K. Holt; T. Hong; S. Hooper; D. J. Hosken; J. Hough; E. J. Howell; D. Huet; B. Hughey; S. Husa; S. H. Huttner; D. R. Ingram; R. Inta; T. Isogai; A. Ivanov; P. Jaranowski; W. W. Johnson; D. I. Jones; G. Jones; R. Jones; L. Ju; P. Kalmus; V. Kalogera; S. Kandhasamy; J. B. Kanner; E. Katsavounidis; W. Katzman; K. Kawabe; S. Kawamura; F. Kawazoe; W. Kells; M. Kelner; D. G. Keppel; A. Khalaidovski; F. Y. Khalili; E. A. Khazanov; H. Kim; N. Kim; P. J. King; D. L. Kinzel; J. S. Kissel; S. Klimenko; V. Kondrashov; R. Kopparapu; S. Koranda; W. Z. Korth; I. Kowalska; D. Kozak; V. Kringel; S. Krishnamurthy; B. Krishnan; A. Królak; G. Kuehn; R. Kumar; P. Kwee; M. Landry; B. Lantz; N. Lastzka; A. Lazzarini; P. Leaci; J. Leong; I. Leonor; N. Leroy; N. Letendre; J. Li; T. G.F. Li; N. Liguori; P. E. Lindquist; N. A. Lockerbie; D. Lodhia; M. Lorenzini; V. Loriette; M. Lormand; G. Losurdo; P. Lu; J. Luan; M. Lubinski; H. Lück; A. P. Lundgren; E. Macdonald; B. Machenschalk; M. MacInnis; M. Mageswaran; K. Mailand; E. Majorana; I. Maksimovic; N. Man; I. Mandel; V. Mandic; M. Mantovani; A. Marandi; F. Marchesoni; F. Marion; S. Márka; Z. Márka; E. Maros; J. Marque; F. Martelli; I. W. Martin; R. M. Martin; J. N. Marx; K. Mason; A. Masserot; F. Matichard; L. Matone; R. A. Matzner; N. Mavalvala; R. McCarthy; D. E. McClelland; S. C. McGuire; G. McIntyre; D. J.A. McKechan; G. Meadors; M. Mehmet; T. Meier; A. Melatos; A. C. Melissinos; G. Mendell; R. A. Mercer; L. Merill; S. Meshkov; C. Messenger; M. S. Meyer; H. Miao; C. Michel; L. Milano; J. Miller; Y. Minenkov; Y. Mino; V. P. Mitrofanov; G. Mitselmakher; R. Mittleman; O. Miyakawa; B. Moe; P. Moesta; M. Mohan; S. D. Mohanty; S. R.P. Mohapatra; D. Moraru; G. Moreno; N. Morgado; A. Morgia; S. Mosca; V. Moscatelli; K. Mossavi; B. Mours; C. M. Mow-Lowry; G. Mueller; S. Mukherjee; A. Mullavey; H. Müller-Ebhardt; J. Munch; P. G. Murray; T. Nash; R. Nawrodt; J. Nelson; I. Neri; G. Newton; E. Nishida; A. Nishizawa; F. Nocera; D. Nolting; E. Ochsner; J. O'Dell; G. H. Ogin; R. G. Oldenburg; B. O'Reilly; R. O'Shaughnessy; C. Osthelder; C. D. Ott; D. J. Ottaway; R. S. Ottens; H. Overmier; B. J. Owen; A. Page; G. Pagliaroli; L. Palladino; C. Palomba; Y. Pan; C. Pankow; F. Paoletti; M. A. Papa; A. Parameswaran; S. Pardi; M. Parisi; A. Pasqualetti; R. Passaquieti; D. Passuello; P. Patel; D. Pathak; M. Pedraza; L. Pekowsky; S. Penn; C. Peralta; A. Perreca; G. Persichetti; M. Phelps; M. Pichot; M. Pickenpack; F. Piergiovanni; M. Pietka; L. Pinard; I. M. Pinto; M. Pitkin; H. J. Pletsch; M. V. Plissi; J. Podkaminer; R. Poggiani; J. Pöld; F. Postiglione; M. Prato; V. Predoi; L. R. Price; M. Prijatelj; M. Principe; S. Privitera; R. Prix; G. A. Prodi; L. Prokhorov; O. Puncken; M. Punturo; P. Puppo; V. Quetschke; F. J. Raab; D. S. Rabeling; I. Rácz; H. Radkins; P. Raffai; M. Rakhmanov; C. R. Ramet; B. Rankins; P. Rapagnani; V. Raymond; V. Re; K. Redwine; C. M. Reed; T. Reed; T. Regimbau; S. Reid; D. H. Reitze; F. Ricci; R. Riesen; K. Riles; P. Roberts; N. A. Robertson; F. Robinet; C. Robinson; E. L. Robinson; A. Rocchi; S. Roddy; L. Rolland; J. Rollins; J. D. Romano; R. Romano; J. H. Romie; D. Rosińska; C. Röver; S. Rowan; A. Rüdiger; P. Ruggi; K. Ryan; S. Sakata; M. Sakosky; F. Salemi; M. Salit; L. Sammut; L. Sancho de la Jordana; V. Sandberg; V. Sannibale; L. Santamaría; I. Santiago-Prieto; G. Santostasi; S. Saraf; B. Sassolas; B. S. Sathyaprakash; S. Sato; M. Satterthwaite; P. R. Saulson; R. Savage; R. Schilling; S. Schlamminger; R. Schnabel; R. M.S. Schofield; B. Schulz; B. F. Schutz; P. Schwinberg; J. Scott; S. M. Scott; A. C. Searle; F. Seifert; D. Sellers; A. S. Sengupta; D. Sentenac; A. Sergeev; D. A. Shaddock; M. Shaltev; B. Shapiro; P. Shawhan; T. Shihan Weerathunga; D. H. Shoemaker; A. Sibley; X. Siemens; D. Sigg; A. Singer; L. Singer; A. M. Sintes; G. Skelton; B. J.J. Slagmolen; J. Slutsky; J. R. Smith; M. R. Smith; N. D. Smith; R. Smith; K. Somiya; B. Sorazu; J. Soto; F. C. Speirits; L. Sperandio; M. Stefszky; A. J. Stein; J. Steinlechner; S. Steinlechner; S. Steplewski; A. Stochino; R. Stone; K. A. Strain; S. Strigin; A. S. Stroeer; R. Sturani; A. L. Stuver; T. Z. Summerscales; M. Sung; S. Susmithan; P. J. Sutton; B. Swinkels; G. P. Szokoly; M. Tacca; D. Talukder; D. B. Tanner; S. P. Tarabrin; J. R. Taylor; R. Taylor; P. Thomas; K. A. Thorne; K. S. Thorne; E. Thrane; A. Thüring; C. Titsler; K. V. Tokmakov; A. Toncelli; M. Tonelli; O. Torre; C. Torres; C. I. Torrie; E. Tournefier; F. Travasso; G. Traylor; M. Trias; K. Tseng; L. Turner; D. Ugolini; K. Urbanek; H. Vahlbruch; B. Vaishnav; G. Vajente; M. Vallisneri; J. F.J. Van Den Brand; C. Van Den Broeck; S. Van Der Putten; M. V. Van Der Sluys; A. A. Van Veggel; S. Vass; M. Vasuth; R. Vaulin; M. Vavoulidis; A. Vecchio; G. Vedovato; J. Veitch; P. J. Veitch; C. Veltkamp; D. Verkindt; F. Vetrano; A. Vicere; A. E. Villar; J. Y. Vinet; H. Vocca; C. Vorvick; S. P. Vyachanin; S. J. Waldman; L. Wallace; A. Wanner; R. L. Ward; M. Was; P. Wei; M. Weinert; A. J. Weinstein; R. Weiss; L. Wen; S. Wen; P. Wessels; M. West; T. Westphal; K. Wette; J. T. Whelan; S. E. Whitcomb; D. White; B. F. Whiting; C. Wilkinson; P. A. Willems; H. R. Williams; L. Williams; B. Willke; L. Winkelmann; W. Winkler; C. C. Wipf; A. G. Wiseman; G. Woan; R. Wooley; J. Worden; J. Yablon; I. Yakushin; H. Yamamoto; K. Yamamoto; H. Yang; D. Yeaton-Massey; S. Yoshida; P. Yu; M. Yvert; M. Zanolin; L. Zhang; Z. Zhang; C. Zhao; N. Zotov; M. E. Zucker; J. Zweizig; R. L. Aptekar; W. V. Boynton; M. S. Briggs; T. L. Cline; V. Connaughton; D. D. Frederiks; N. Gehrels; J. O. Goldsten; D. Golovin; A. J. Van Der Horst; K. C. Hurley; Y. Kaneko; A. Von Kienlin; C. Kouveliotou; H. A. Krimm; L. Lin; I. Mitrofanov; M. Ohno; V. D. Pal'shin; A. Rau; A. Sanin; M. S. Tashiro; Y. Terada; K. Yamaoka
Astrophysical Journal Letters, Volume：734, Number：2, Jun. 2011, [Reviewed]
Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are thought to be magnetars: neutron stars powered by extreme magnetic fields. These rare objects are characterized by repeated and sometimes spectacular gamma-ray bursts. The burst mechanism might involve crustal fractures and excitation of non-radial modes which would emit gravitational waves (GWs). We present the results of a search for GW bursts from six galactic magnetars that is sensitive to neutron star f-modes, thought to be the most efficient GW emitting oscillatory modes in compact stars. One of them, SGR 0501+4516, is likely 1kpc from Earth, an order of magnitude closer than magnetars targeted in previous GW searches. A second, AXP 1E 1547.0-5408, gave a burst with an estimated isotropic energy >
1044erg which is comparable to the giant flares. We find no evidence of GWs associated with a sample of 1279 electromagnetic triggers from six magnetars occurring between 2006 November and 2009 June, in GW data from the LIGO, Virgo, and GEO600 detectors. Our lowest model-dependent GW emission energy upper limits for band- and time-limited white noise bursts in the detector sensitive band, and for f-mode ringdowns (at 1090Hz), are 3.0 × 1044 d 2 1erg and 1.4 × 10 47 d 2 1erg, respectively, where and d 0501 is the distance to SGR 0501+4516. These limits on GW emission from f-modes are an order of magnitude lower than any previous, and approach the range of electromagnetic energies seen in SGR giant flares for the first time. © 2011. The American Astronomical Society. All rights reserved.
English, Scientific journal
DOI：https://doi.org/10.1088/2041-8205/734/2/L35
DOI ID：10.1088/2041-8205/734/2/L35, ISSN：2041-8205, ORCID：78692603, SCOPUS ID：79959405183 - SUZAKU OBSERVATIONS OF THE HMXB 1A 1118-61
Slawomir Suchy; Katja Pottschmidt; Richard E. Rothschild; Joern Wilms; Felix Fuerst; Laura Barragan; Isabel Caballero; Victoria Grinberg; Ingo Kreykenbohm; Victor Doroshenko; Andrea Santangelo; Ruediger Staubert; Yukikatsu Terada; Wataru Iwakari; Kazuo Makishima
ASTROPHYSICAL JOURNAL, Volume：733, Number：1, May 2011, [Reviewed]
We present broadband analysis of the Be/X-ray transient 1A 1118-61 by Suzaku at the peak of its third observed outburst in 2009 January and two weeks later when the source flux had decayed by an order of magnitude. The continuum was modeled with a cutoffpl model as well as a compTT model, with both cases requiring an additional blackbody component at lower energies. We confirm the detection of a cyclotron line at similar to 55 keV and discuss the possibility of a first harmonic at similar to 110 keV. Pulse profile comparisons show a change in the profile structure at lower energies, an indication for possible changes in the accretion geometry. Phase-resolved spectroscopy in the outburst data shows a change in the continuum throughout the pulse period. The decrease in the cyclotron resonance scattering feature centroid energy also indicates that the viewing angle on the accretion column is changing throughout the pulse period.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.1088/0004-637X/733/1/15
DOI ID：10.1088/0004-637X/733/1/15, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000290314600015 - Design concepts for the Cherenkov Telescope Array CTA: an advanced facility for ground-based high-energy gamma-ray astronomy
Yukikatsu Terada
Experimental Astronomy, 2011
Scientific journal
DOI：https://doi.org/10.1007/S10686-011-9247-0
DOI ID：10.1007/S10686-011-9247-0, ORCID：67259940, Web of Science ID：WOS:000300769700001 - The international x-ray observatory and other x-ray missions, expectations for pulsar physics
Yukikatsu Terada; Tadayasu Dotani
Astrophysics and Space Science Proceedings, Number：202589, First page：563, Last page：583, 2011, [Reviewed]
Pulsar systems are very good experimental laboratories for the fundamental physics in extreme environments which cannot be achieved on ground. For example, the systems are under conditions of high magnetic field strength, large gravitational potential, and fast rotation, representing highly-ionized hot plasmas with particle acceleration etc. We can test phenomena related to these extreme condition in the X-ray to sub-MeV bands. In future, we will get fantastic capabilities of higher sensitivities, larger effective area, higher energy resolutions, and X-ray imaging capabilities with wider energy band than current missions, in addition to opening new eyes of polarization measurements, and deep all sky monitoring capabilities, with future X-ray missions including ASTRO-H, eRossita, NuSTAR, GEMS, International X-ray Observatory (IXO) and so on. In this paper, we summarize current hot topics on pulsars and discuss expected developments by these future missions, especially by ASTRO-H and IXO, based on the current design parameters.
Springer Netherlands, English, International conference proceedings
DOI：https://doi.org/10.1007/978-3-642-17251-9_47
DOI ID：10.1007/978-3-642-17251-9_47, ISSN：1570-6605, SCOPUS ID：85034624236 - The Time Assignment System of ASTRO-H
Tomomi Kouzu; Kaori Iwase; Yuki Mishima; Yukikatsu Terada; Takayuki Yuasa; Yoshitaka Ishisaki; Makoto S. Tashiro; Motohide Kokubun; Masanobu Ozaki; Masaharu Nomachi; Tadayuki Takahashi
2011 IEEE NUCLEAR SCIENCE SYMPOSIUM AND MEDICAL IMAGING CONFERENCE (NSS/MIC), First page：163, Last page：166, 2011, [Reviewed]
ASTRO-H is an X-ray astronomy satellite to be launched in 2014. The data acquisition system of this mission is realized with a standard network protocol, SpaceWire. Although the protocol itself is well designed, a new concept to grantee the quality of service will be installed to the ASTRO-H data acquisition system. Therefore, the verification of the design of the concept is essential in the initial phase of the development. The time assignment function is one of the important issues for the SpaceWire development. The accuracy of the absolute time of about 30 mu s is required from science goals. The key point of the time assignment with SpaceWire network in the ASTRO-H system is how accurately sharing the time information. In this paper, our design of the time distribution and assignment system for ASTRO-H is shown. The results of our measurements of timing accuracy are also presented to show that the design will fulfill the goal of absolute timing accuracy.
IEEE, English, International conference proceedings
ISSN：1082-3654, Web of Science ID：WOS:000304755600030 - Fine-Pitch Semiconductor Detector for the FOXSI Mission
Yukikatsu Terada
IEEE Transactions on Nuclear Science, Volume：58, Number：4 PART 2, First page：2039, Last page：2046, 2011, [Reviewed]
Scientific journal
DOI：https://doi.org/10.1109/TNS.2011.2154342
DOI ID：10.1109/TNS.2011.2154342, ORCID：67259924, SCOPUS ID：84860389910, Web of Science ID：WOS:000293977200022 - Development of an integrated response generator for Si/CdTe semiconductor Compton cameras
Hirokazu Odaka; Soichiro Sugimoto; Shin-Nosuke Ishikawa; Junichiro Katsuta; Yuu Koseki; Taro Fukuyama; Shinya Saito; Rie Sato; Goro Sato; Shin Watanabe; Motohide Kokubun; Tadayuki Takahashi; Shin'Ichiro Takeda; Yasushi Fukazawa; Takaaki Tanaka; Hiroyasu Tajima
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：624, Number：2, First page：303, Last page：309, Dec. 2010, [Reviewed]
We have developed an integrated response generator based on Monte Carlo simulation for Compton cameras composed of silicon (Si) and cadmium telluride (CdTe) semiconductor detectors. In order to construct an accurate detector response function, the simulation is required to include a comprehensive treatment of the semiconductor detector devices and the data processing system in addition to simulating particle tracking. Although CdTe is an excellent semiconductor material for detection of soft gamma rays, its ineffective charge transport property distorts its spectral response. We investigated the response of CdTe pad detectors in the simulation and present our initial results here. We also performed the full simulation of prototypes of Si/CdTe semiconductor Compton cameras and report on the reproducibility of detection efficiencies and angular resolutions of the cameras, both of which are essential performance parameters of astrophysical instruments. © 2010 Elsevier B.V. All rights reserved.
English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2009.11.052
DOI ID：10.1016/j.nima.2009.11.052, ISSN：0168-9002, SCOPUS ID：78649291432 - EXPANSION VELOCITY OF EJECTA IN TYCHO's SUPERNOVA REMNANT MEASURED BY DOPPLER BROADENED X-RAY LINE EMISSION
Asami Hayato; Hiroya Yamaguchi; Toru Tamagawa; Satoru Katsuda; Una Hwang; John P. Hughes; Midori Ozawa; Aya Bamba; Kenzo Kinugasa; Yukikatsu Terada; Akihiro Furuzawa; Hideyo Kunieda; Kazuo Makishima
ASTROPHYSICAL JOURNAL, Volume：725, Number：1, First page：894, Last page：903, Dec. 2010, [Reviewed]
We show that the expansion of ejecta in Tycho's supernova remnant (SNR) is consistent with a spherically symmetric shell, based on Suzaku measurements of the Doppler broadened X-ray emission lines. All of the strong K alpha line emissions show broader widths at the center than at the rim, while the centroid energies are constant across the remnant (except for Ca). This is the pattern expected for Doppler broadening due to expansion of the SNR ejecta in a spherical shell. To determine the expansion velocities of the ejecta, we applied a model for each emission-line feature having two Gaussian components separately representing red-and blueshifted gas, and inferred the Doppler velocity difference between these two components directly from the fitted centroid energy difference. Taking into account the effect of projecting a three-dimensional shell to the plane of the detector, we derived average spherical expansion velocities independently for the K alpha emission of Si, S, Ar, and Fe, and K beta of Si. We found that the expansion velocities of Si, S, and Ar ejecta of 4700 +/- 100 km s(-1) are distinctly higher than that obtained from Fe K alpha emission, 4000 +/- 300 km s(-1), which is consistent with segregation of the Fe in the inner ejecta. Combining the observed ejecta velocities with the ejecta proper-motion measurements by Chandra, we derived a distance to Tycho's SNR of 4 +/- 1 kpc.
IOP PUBLISHING LTD, English, Scientific journal
DOI：https://doi.org/10.1088/0004-637X/725/1/894
DOI ID：10.1088/0004-637X/725/1/894, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000284576700097 - Suzaku Observation of the Anomalous X-Ray Pulsar 1E 1841-045
Mikio Morii; Shunji Ktamoto; Noriaki Shibazaki; Nobuyuki Kawai; Makoto Arimoto; Masaru Ueno; Takayoshi Kohmura; Yukikatsu Terada; Shigeo Yamauchi; Hiromitsu Takahashi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：62, Number：5, First page：1249, Last page：1259, Oct. 2010, [Reviewed]
We report on the results of a Suzaku observation of the anomalous X-ray pulsar (AXP) IE 1841-045 at the center of the supernova remnant Kes 73. We confirmed that the energy-dependent spectral models obtained by previous separate observations were also satisfied over a wide energy range from 0.4 to similar to 70 keV, simultaneously. Here, the models below similar to 10 keV were a combination of blackbody (BB) and power-law (PL) functions, or of two BBs with different temperatures at 0.6-7.0 keV (Morii et al. 2003. PASJ, 55, L45), and that above similar to 20 keV was a PL function (Kuiper et al. 2004, ApJ, 613, 1173). The combination BB + PL + PL was found to best represent the phase-averaged spectrum. Phase-resolved spectroscopy indicated the existence of two emission regions, one with a thermal and the other with a non-thermal nature. The combination BB + BB + PL was also found to represent the phase-averaged spectrum well. However, we found that this model is physically unacceptable due to an excessively large area of the emission region of the blackbody. Nonetheless, we found that the temperatures and radii of the two blackbody components showed moderate correlations in the phase-resolved spectra. The fact that the same correlations have been observed between the phase-averaged spectra of various magnetars (Nakagawa et al. 2009, PASJ, 61, 109) suggests that a self-similar function can approximate the intrinsic energy spectra of magnetars below similar to 10 keV.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/62.5.1249
DOI ID：10.1093/pasj/62.5.1249, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000283885700017 - A Catalog of Suzaku/WAM Hard X-Ray Solar Flares
Akira Endo; Takashi Minoshima; Kouichi Morigami; Masanobu Suzuki; Atsushi Shimamori; Yumi Sato; Yukikatsu Terada; Makoto S. Tashiro; Yuji Urata; Eri Sonoda; Kazutaka Yamaoka; Satoshi Sugita; Kyoko Watanabe
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：62, Number：5, First page：1341, Last page：1349, Oct. 2010, [Reviewed]
We developed a catalog of solar flares in the hard X-ray band observed with the Wide-band All-sky Monitor (WAM) onboard the Suzaku satellite between 2005 July and 2009 November. During this period, 105 solar flares (GOES class X: 13, M: 29, C: 47, B: 16) were detected with WAM, including 10% of GOES-class C events reported during the same period. The observed photon flux ranged between 9 x 10(-5) and 9 x 10(-1) photons s(-1) cm(-2) keV(-1) at 100 keV. The averaged hard X-ray spectrum for each solar flare was evaluated for 70 of the 105 events, and 43 of them were well fitted with a single power-law model with a photon index ranging between -7 and -3. We observed a weak trend where events with longer durations exhibited harder spectral slopes.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/62.5.1341
DOI ID：10.1093/pasj/62.5.1341, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000283885700024 - Time-Resolved Spectral Variability of the Prompt Emission from GRB 070125 Observed with Suzaku/WAM
Kaori Onda; Makoto S. Tashiro; Yujin E. Nakagawa; Kazutaka Yamaoka; Yukikatsu Terada; Masanori Ohno; Satoshi Sugita; Takanori Sakamoto; Kenji Toma; Poshak Gandhi; Natsuki Kodaka; Wataru Iwakiri; Yuji Urata; Makoto Yamauchi; Yasushi Fukazawa
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：62, Number：3, First page：547, Last page：556, Jun. 2010, [Reviewed]
Time-resolved spectral analyses of GRB 070125 with significant photon detections over the MeV regime using Suzaku/WAM data are reported. The prompt emission interval was divided into 10 time regions, and their spectra were reproduced by a Band function or a cutoff power-law model. The spectra show a complex evolution; a soft-hard-soft trend is seen, rather than a typical hard-to-soft monotonic variation. In addition, a flat spectral slope in the low-energy band exceeding the slope expected from a simple synchrotron emission model is suggested in one of the time regions. These results imply that the internal shocks in the relativistic jet of GRB 070125 have different physical conditions. There is a possible excess at similar to 2.2 MeV in the spectrum of 33 seconds after the trigger at a significant level of approximate to 98.5%, where the continuum spectrum is not reproduced by the Band function. These properties are only shown during the short prompt time interval of the prompt emission, and emphasize the utility of the Suzaku/WAM for the study of gamma-ray bursts.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/62.3.547
DOI ID：10.1093/pasj/62.3.547, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000279835200005 - Suzaku Discovery of a Hard X-Ray Tail in the Persistent Spectra from the Magnetar 1E 1547.0-5408 during its 2009 Activity
Teruaki Enoto; Kazuhiro Nakazawa; Kazuo Makishima; Yujin E. Nakagawa; Takanori Sakamoto; Masanori Ohno; Tadayuki Takahashi; Yukikatsu Terada; Kazutaka Yamaoka; Toshio Murakami; Hiromitsu Takahashi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：62, Number：2, First page：475, Last page：485, Apr. 2010, [Reviewed]
The fastest-rotating magnetar IE 1547.0-5408 was observed in broad-band X-rays with Suzaku for 33 ks on 2009 January 28-29, 7d after the onset of its latest bursting activity. After removing burst events, the absorption-uncorrected 2-10 keV flux of the persistent emission was measured with the XIS as 5.7 x 10(-11)erg cm(-2) s(-1), which is 1-2 orders of magnitude higher than was measured in 2006 and 2007 when the source was less active. This persistent emission was also detected significantly with the HXD in > 10 keV up to at least similar to 110 keV, with an even higher flux of 1.3 x 10(-10) erg cm(-2) s(-1) in 20-100 keV. The pulsation was detected at least up to 70 keV for a period of 2.072135 +/- 0.00005 s, with a deeper modulation than was measured in a fainter state. The phase-averaged 0.7-114 keV spectrum was reproduced by an absorbed blackbody emission with a temperature of 0.65 +/- 0.02 keV, plus a hard power-law with a photon index of similar to 1.5. At a distance of 9 kpc, the bolometric luminosity of the blackbody and the 2-100 keV luminosity of the hard power-law are estimated to be (6.2 +/- 1.2) x 10(35) erg s(-1) and 1.9 x 10(36) erg s(-1), respectively, while the blackbody radius becomes similar to 5 km. Although the source has not been detected significantly in hard X-rays during the past fainter states, a comparison of the present and past spectra at energies below 10 keV suggests that the hard component is more enhanced than the soft X-ray component during the period of persistent activity.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/62.2.475
DOI ID：10.1093/pasj/62.2.475, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000279834900024 - Possible keV-TeV correlation in the reverse shock in Cassiopeia A
Maeda, Yoshitomo; Uchiyama, Yasunobu; Bamba, Aya; Kosugi, Hiroko; Tsunemi, Hiroshi; Helder, Eveline A; Vink, Jacco; Kodaka, Natsuki; Terada, Yukikatsu; Fukazawa, Yasushi; Hiraga, Junko; Hughes, John P; Kokubun, Motohide; Kouzu, Tomomi; Matsumoto, Hironori; Miyata, Emi; Nakamura, Ryoko; Okada, Shunsaku; Someya, Kentaro; Tamagawa, Toru; Tamura, Keisuke; Totsuka, Kohta; Tsuboi, Yohko; Ezoe, Yuichiro; Holt, Stephen S; Ishida, Manabu; Kamae, Tsuneyoshi; Petre, Robert; Takahashi, Tadayuki
Proceedings of the 3rd Suzaku Conference, First page：42, Last page：43, Feb. 2010
English, International conference proceedings
ISSN：1349-113X - Repeated administration of methamphetamine blocked cholecystokinin-octapeptide injection-induced c-fos mRNA expression without change in capsaicin-induced junD mRNA expression in rat cerebellum
Yukikatsu Terada
Journal of Neural Transmission, 2010
Scientific journal
DOI：https://doi.org/10.1007/S00702-010-0444-1
DOI ID：10.1007/S00702-010-0444-1, ORCID：67259928, Web of Science ID：WOS:000281397200003 - Development of BGO active shield for the ASTRO-H soft Gamma-ray Detector
Y. Hanabata; Y. Fukazawa; K. Yamaoka; H. Tajima; J. Kataoka; K. Nakazawa; H. Takahashi; T. Mizuno; M. Ohno; M. Kokubun; T. Takahashi; S. Watanabe; M. Tashiro; Y. Terada; C. Sasaki; K. Nakajima; T. Mizushima
Proceedings of SPIE - The International Society for Optical Engineering, Volume：7732, 2010
Soft Gamma-ray Detector (SGD:40-600 keV) will be mounted on the 6th Japanese X-ray observatory ASTRO-H to be launched in 2014. The main part of the SGD is a Compton camera with a narrow field of view and surrounded by BGO active shields (SGD-BGO). Via this combination, the SGD can achieve sensitivity more than ten times superior to the Suzaku/HXD. The BGO active shield will also function as a gamma-ray burst monitor as proven by the wide-band all-sky monitor (WAM) of the Suzaku/HXD. Avalanche Photodiodes (APDs) are used to read out scintillation lights from the BGO. The size of the former also means we need to focus on collecting light from large, complex-shaped BGO blocks. The significant leakage current of the APD means a lower temperature is preferred to minimize the noise while a higher temperature is preferred to simplify the cooling system. To optimize the BGO shape and the operating temperature, we tested the performance of the BGO readout system with various BGO shapes under different operating temperatures. We also apply waveform sampling by flash-ADC and digital filter instead of a conventional analog filter and ADC scheme to reduce the space and power of the circuit with increased flexibilities. As an active shield, we need to achieve a threshold level of 50-100 keV. Here, we report on the studies of threshold energy of active shield under various conditions and signal processings. © 2010 SPIE.
International conference proceedings
DOI：https://doi.org/10.1117/12.856745
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=77957916088&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=77957916088&origin=inward
DOI ID：10.1117/12.856745, ISSN：0277-786X, SCOPUS ID：77957916088 - The third interplanetary network
K. Hurley; S. Golenetskii; R. Aptekar; E. Mazets; V. Pal'shin; D. Frederiks; I. G. Mitrofanov; D. Golovin; M. L. Litvak; A. B. Sanin; W. Boynton; C. Fellows; K. Harshman; R. Starr; D. M. Smith; C. Wigger; W. Hajdas; A. Von Kienlin; A. Rau; K. Yamaoka; M. Ohno; T. Takahashi; Y. Fukazawa; M. Tashiro; Y. Terada; T. Murakami; K. Makishima; S. Barthelmy; T. Cline; J. Cummings; N. Gehrels; H. Krimm; J. Goldsten; E. Del Monte; M. Feroci; M. Marisaldi; M. Briggs; V. Connaughton; C. Meegan
AIP Conference Proceedings, Volume：1279, First page：330, Last page：333, 2010, [Reviewed]
The 3rd interplanetary network (IPN), which has been in operation since 1990, presently consists of 9 spacecraft: AGILE, Fermi, RHESSI, Suzaku, and Swift, in low Earth orbit
INTEGRAL, in eccentric Earth orbit with apogee 0.5 light-seconds
Wind, up to ∼7 light-seconds from Earth
MESSENGER, en route to Mercury
and Mars Odyssey, in orbit around Mars. The IPN operates as a full-time, all-sky monitor for transients down to a threshold of about 6 × 10-7 erg cm-2 or 1 photoncm-2 s-1. It detects ∼346 cosmic gamma-ray bursts per year. These events are generally not the same ones detected by narrower field of view instruments such as Swift, INTEGRAL IBIS, and SuperAGILE
the localization accuracy is in the several arcminute and above range. The uses of the IPN data are described. © 2010 American Institute of Physics.
English, International conference proceedings
DOI：https://doi.org/10.1063/1.3509301
DOI ID：10.1063/1.3509301, ISSN：0094-243X, SCOPUS ID：78649890599 - Timing analysis of unusual GRB 090709A observed by Suzaku Wide-band All sky Monitor
W. Iwakiri; M. Ohno; T. Kamae; Y. E. Nakagawa; Y. Terada; M. S. Tashiro; A. Yoshida; K. Yamaoka; K. Makishima
AIP Conference Proceedings, Volume：1279, First page：89, Last page：92, 2010, [Reviewed]
A result of a joint timing analysis is presented for prompt emission of long-duration (T90 = 81 s) GRB 090709A with Swift Burst Alert Telescope (Swift/BAT), Suzaku Wide-band All-sky Monitor (Suzaku/WAM) and Konus-Wind over an energy range from 15 keV to 5 MeV. It was reported that multi-peaked GRB 090709A exhibited a possible periodic behavior with a period of about 8 s which is comparable to typical time scale of soft gamma-ray repeaters. However, the periodicity is still marginal in detailed analysis with Swift/BAT and GRB090709A exhibited a typical afterglow [1] [2]. To investigate significance of the periodicity more quantitatively, we performed a detailed timing analysis on all the lightcurves obtained with Suzaku/WAM, Swift/BAT, and Konus-Wind evaluating their underlying trend, red noise and white noise. © 2010 American Institute of Physics.
English, International conference proceedings
DOI：https://doi.org/10.1063/1.3509358
DOI ID：10.1063/1.3509358, ISSN：0094-243X, SCOPUS ID：78649876025 - Hard X-ray and gamma-ray detector for ASTRO-H based on Si and CdTe imaging sensors
Yukikatsu Terada
Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：623, Number：1, First page：425, Last page：427, 2010, [Reviewed]
Scientific journal
DOI：https://doi.org/10.1016/J.NIMA.2010.03.024
DOI ID：10.1016/J.NIMA.2010.03.024, ORCID：67259972, SCOPUS ID：77957846499, Web of Science ID：WOS:000283954800131 - Monte Carlo simulation study of in-orbit background for the soft Gamma-ray Detector onboard ASTRO-H
T. Mizuno; K. Hiragi; Y. Fukazawa; Y. Umeki; H. Odaka; S. Watanabe; M. Kokubun; T. Takahashi; K. Nakajima; K. Nakazawa; K. Makishima; S. Nakahira; Y. Terada; H. Tajima
Proceedings of SPIE - The International Society for Optical Engineering, Volume：7732, 2010, [Reviewed]
The Soft Gamma-ray Detector onboard the ASTRO-H satellite, scheduled for launch in 2014, is a Si/CdTe Compton telescope surrounded by a thick BGO active shield. The SGD covers the energy range from 40 to 600 keV and studies non-thermal phenomena in the universe with high sensitivity. For the success of the SGD mission, careful examination of the expected performance, particularly the instrumental background in orbit, and optimization of the detector configuration are essential. We are developing a Geant4-based Monte Carlo simulation framework on the ANL++ platform, employing the MGGPOD software suite to predict the radioactivation in orbit. A detailed validation of the simulator through the comparison with literature and the beam test data is summarized. Our system will be integrated into the ASTRO-H simulation framework. © 2010 SPIE.
International conference proceedings
DOI：https://doi.org/10.1117/12.856753
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=77957869026&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=77957869026&origin=inward
DOI ID：10.1117/12.856753, ISSN：0277-786X, SCOPUS ID：77957869026 - Systematic surveys of the non thermal emission from white dwarfs with Suzaku and INTEGRAL
Yukikatsu Terada; Atsushi Harayama; Kouichi Morigami; Manabu Ishida; Aya Bamba; Tadayasu Dotani; Takayuki Hayashi; Shunsaku Okada; Ryoko Nakamura; Kazuo Makishima; Koji Mukai; Sachindra Naik
X-RAY ASTRONOMY-2009: PRESENT STATUS, MULTI-WAVELENGTH APPROACH AND FUTURE PERSPECTIVES, PROCEEDINGS, Volume：1248, First page：215, Last page：+, 2010, [Reviewed]
Continuous searches for other possible white dwarf (WD) pulsars like AE Aquarii[l 2] with Suzaku and INTEGRAL have been performed. After picking up WDs with known magnetic field strengths and spin periods from catalogs of CVs and isolated WDs, objects whose induced electric potentials exceed 10(12) volts and dipole radiations over 10(29) erg s(-1) are selected; AM Her, EUVE J0317-85, P01031+234, LHS1734, PG1015+014 etc. Their X-rays were studied with INTEGRAL archive data and/or Suzaku follow-up observations. A promising non-thermal emission from an object, AM Her in a very low state, has been found with Suzaku at the X-ray luminosity of 6.6 x 10(29) erg s(-1).
AMER INST PHYSICS, English, International conference proceedings
DOI：https://doi.org/10.1063/1.3475212
DOI ID：10.1063/1.3475212, ISSN：0094-243X, Web of Science ID：WOS:000284017700074 - Development of double-sided silicon strip detectors for solar hard X-ray observation
Shinya Saito; Shin-nosuke Ishikawa; Shin Watanabe; Hirokazu Odaka; Soichiro Sugimoto; Taro Fukuyama; Motohide Kokubun; Tadayuki Takahashi; Yukikatsu Terada; Hiroyasu Tajima; Takaaki Tanaka; Saem Krucker; Steven Christe; Steve McBride; Lindsay Glesener
SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY, Volume：7732, 2010, [Reviewed]
The Focusing Optics X-ray Solar Imager (FOXSI) is a rocket experiment scheduled for January 2011 launch. FOXSI observes 5 - 15 keV hard X-ray emission from quiet-region solar flares in order to study the acceleration process of electrons and the mechanism of coronal heating. For observing faint hard X-ray emission, FOXSI uses focusing optics for the first time in solar hard X-ray observation, and attains 100 times higher sensitivity than RHESSI, which is the present solar hard X-ray observing satellite. Now our group is working on developments of both Double-sided Silicon Strip Detector (DSSD) and read-out analog ASIC "VATA451" used for FOXSI. Our DSSD has a very fine strip pitch of 75 mu m, which has sufficient position resolution for FOXSI mirrors with angular resolution (FWHM) of 12 arcseconds. DSSD also has high spectral resolution and efficiency in the FOXSI's energy range of 5 - 15 keV, when it is read out by our 64-channel analog ASIC. In advance of the FOXSI launch, we have established and tested a setup of 75 mu m pitch DSSD bonded with "VATA451" ASICs. We successfully read out from almost all the channels of the detector, and proved ability to make a shadow image of tungsten plate. We also confirmed that our DSSD has energy resolution (FWHM) of 0.5 keV, lower threshold of 5 keV, and position resolution less than 63 mu m. These performance satisfy FOXSI's requirements.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.857235
DOI ID：10.1117/12.857235, ISSN：0277-786X, Web of Science ID：WOS:000285506200019 - The High-Resolution X-ray Microcalorimeter Spectrometer System for the SXS on ASTRO-H
Kazuhisa Mitsuda; Richard L. Kelley; Kevin R. Boyce; Gregory V. Brown; Elisa Costantini; Michael J. DiPirro; Yuichiro Ezoe; Ryuichi Fujimoto; Keith C. Gendreau; Jan-Willem den Herder; Akio Hoshino; Yoshitaka Ishisaki; Caroline A. Kilbourne; Shunji Kitamoto; Dan McCammon; Masahide Murakami; Hiroshi Murakami; Mina Ogawa; Takaya Ohashi; Atsushi Okamoto; Stephane Paltani; Martin Pohl; F. Scott Porter; Yoichi Sato; Keisuke Shinozaki; Peter J. Shirron; Gary A. Sneiderman; Hiroyuki Sugita; Andrew Szymkowiak; Yoh Takei; Toru Tamagawa; Makoto Tashiro; Yukikatsu Terada; Masahiro Tsujimoto; Cor de Vries; Hiroya Yamaguchi; Noriko Y. Yamasaki
SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY, Volume：7732, 2010, [Reviewed]
We present the science and an overview of the Soft X-ray Spectrometer onboard the ASTRO-H mission with emphasis on the detector system. The SXS consists of X-ray focusing mirrors and a microcalorimeter array and is developed by international collaboration lead by JAXA and NASA with European participation. The detector is a 6 x 6 format microcalorimeter array operated at a cryogenic temperature of 50 mK and covers a 3' x 3' filed of view of the X-ray telescope of 5.6 m focal length. We expect an energy resolution better than 7 eV (FWHM, requirement) with a goal of 4 eV. The effective area of the instrument will be 225 cm(2) at 7 keV; by a factor of about two larger than that of the X-ray microcalorimeter on board Suzaku. One of the main scientific objectives of the SXS is to investigate turbulent and/or macroscopic motions of hot gas in clusters of galaxies.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.856778
DOI ID：10.1117/12.856778, ISSN：0277-786X, Web of Science ID：WOS:000285506200029 - The ASTRO-H Mission
Takahashi Tadayuki; Mitsuda Kazuhisa; Kelley Richard; Aharonian Felix; Akimoto Fumie; Allen Steve; Anabuki Naohisa; Angelini Lorella; Arnaud Keith; Awaki Hisamitsu; Bamba Aya; Bando Nobutaka; Bautz Mark; Blandford Roger; Boyce Kevin; Brown Greg; Chernyakova Maria; Coppi Paolo; Costantini Elisa; Cottam Jean; Crow John; de Plaa Jelle; de Vries Cor; den Herder Jan-Willem; DiPirro Michael; Done Chris; Dotani Tadayasu; Ebisawa Ken; Enoto Teruaki; Ezoe Yuichiro; Fabian Andrew; Fujimoto Ryuichi; Fukazawa Yasushi; Funk Stefan; Furuzawa Akihiro; Galeazzi Massimiliano; Gandhi Poshak; Gendreau Keith; Gilmore Kirk; Haba Yoshito; Hamaguchi Kenji; Hatsukade Isamu; Hayashida Kiyoshi; Hiraga J; Hirose Kazuyuki; Hornschemeier Ann; Hughes John; Hwang Una; Iizuka Ryo; Ishibashi Kazunori; Ishida Manabu; Ishimura Kosei; Ishisaki Yoshitaka; Isobe Naoki; Ito Masayuki; Iwata Naoko; Kaastra Jelle; Kallman Timothy; Kamae Tuneyoshi; Katagiri Hideaki; Kataoka Jun; Katsuda Satoru; Kawaharada Madoka; Kawai Nobuyuki; Kawasaki Shigeo; Khangaluyan Dmitry; Kilbourne Caroline; Kinugasa Kenzo; Kitamoto Shunji; Kitayama Tetsu; Kohmura Takayoshi; Kokubun Motohide; Kosaka Tatsuro; Kotani Taro; Koyama Katsuji; Kubota Aya; Kunieda Hideyo; Laurent Philippe; Lebrun Francois; Limousin Olivier; Loewenstein Michael; Long Knox; Madejski Grzegorz; Maeda Yoshitomo; Makishima Kazuo; Markevitch Maxim; Matsumoto Hironori; Matsushita Kyoko; McCammon Dan; Miller Jon; Mineshige Shin; Minesugi Kenji; Miyazawa Takuya; Mizuno Tsunefumi; Mori Koji; Mori Hideyuki; Mukai Koji; Murakami Hiroshi; Murakami Toshio; Mushotzky Richard; Nakagawa Yujin; Nakagawa Takao; Nakajima Hiroshi; Nakamori Takeshi; Nakazawa Kazuhiro; Namba Yoshiharu; Nomachi Masaharu; Dell Steve O; Ogawa Hiroyuki; Ogawa Mina; Ogi Keiji; Ohashi Takaya; Ohno Masanori; Ohta Masayuki; Okajima Takashi; Ota Naomi; Ozaki Masanobu; Paerels Frits; Paltani Stephane; Parmer Arvind; Petre Robert; Pohl Martin; Porter Scott; Ramsey Brian; Reynolds Christopher; Sakai Shin-ichiro; Sambruna Rita; Sato Goro; Sato Yoichi; Serlemitsos Peter; Shida Maki; Shimada Takanobu; Shinozaki Keisuke; Shirron Peter; Smith Randall; Sneiderman Gary; Soong Yang; Stawarz Lukasz; Sugita Hiroyuki; Szymkowiak Andrew; Tajima Hiroyasu; Takahashi Hiromitsu; Takei Yoh; Tamagawa Toru; Tamura Takayuki; Tamura Keisuke; Tanaka Takaaki; Tanaka Yasuo; Tanaka Yasuyuki; Tashiro Makoto; Tawara Yuzuru; Terada Yukikatsu; Terashima Yuichi; Tombesi Francesco; Tomida Hiroshi; Tozuka Miyako; Tsuboi Yoko; Tsujimoto Masahiro; Tsunemi Hiroshi; Tsuru Takeshi; Uchida Hiroyuki; Uchiyama Yasunobu; Uchiyama Hideki; Ueda Yoshihiro; Uno Shinichiro; Urry Meg; Watanabe Shin; White Nicholas; Yamada Takahiro; Yamaguchi Hiroya; Yamaoka Kazutaka; Yamasaki Noriko; Yamauchi Makoto; Yamauchi Shigeo; Yatsu Yoichi; Yonetoku Daisuke; Yoshida Atsumasa
SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY, Volume：7732, 2010, [Reviewed]
DOI：https://doi.org/10.1117/12.857875
DOI ID：10.1117/12.857875, ISSN：0277-786X, Web of Science ID：WOS:000285506200027 - Soft Gamma-ray Detector for the ASTRO-H Mission
Hiroyasu Tajima; Roger Blandford; Teruaki Enoto; Yasushi Fukazawa; Kirk Gilmore; Tuneyoshi Kamae; Jun Kataoka; Madoka Kawaharada; Motohide Kokubun; Philippe Laurent; Francois Lebrun; Olivier Limousin; Greg Madejski; Kazuo Makishima; Tsunefumi Mizuno; Kazuhiro Nakazawa; Masanori Ohno; Masayuki Ohta; Goro Sato; Rie Sato; Hiromitsu Takahashi; Tadayuki Takahashi; Takaaki Tanaka; Makoto Tashiro; Yukikatsu Terada; Yasunobu Uchiyama; Shin Watanabe; Kazutaka Yamaoka; Daisuke Yonetoku
SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY, Volume：7732, 2010, [Reviewed]
ASTRO-H is the next generation JAXA X-ray satellite, intended to carry instruments with broad energy coverage and exquisite energy resolution. The Soft Gamma-ray Detector (SGD) is one of ASTRO-H instruments and will feature wide energy band (40-600 keV) at a background level 10 times better than the current instruments on orbit. SGD is complimentary to ASTRO-H's Hard X-ray Imager covering the energy range of 5-80 keV. The SGD achieves low background by combining a Compton camera scheme with a narrow field-of-view active shield where Compton kinematics is utilized to reject backgrounds. The Compton camera in the SGD is realized as a hybrid semiconductor detector system which consists of silicon and CdTe (cadmium telluride) sensors. Good energy resolution is afforded by semiconductor sensors, and it results in good background rejection capability due to better constraints on Compton kinematics. Utilization of Compton kinematics also makes the SGD sensitive to the gamma-ray polarization, opening up a new window to study properties of gamma-ray emission processes. The ASTRO-H mission is approved by ISAS/JAXA to proceed to a detailed design phase with an expected launch in 2014. In this paper, we present science drivers and concept of the SGD instrument followed by detailed description of the instrument and expected performance.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.857531
DOI ID：10.1117/12.857531, ISSN：0277-786X, Web of Science ID：WOS:000285506200034 - Hard X-ray Imager (HXI) for the ASTRO-H mission
Motohide Kokubun; Kazuhiro Nakazawa; Teruaki Enoto; Yasushi Fukazawa; Kirk Gilmore; Jun Kataoka; Madoka Kawaharada; Philippe Laurent; Francois Lebrun; Olivier Limousin; Kazuo Makishima; Tsunefumi Mizuno; Kunishiro Mori; Takeshi Nakamori; Masanori Ohno; Masayuki Ohta; Goro Sato; Hiroyasu Tajima; Hiromitsu Takahashi; Tadayuki Takahashi; Takaaki Tanaka; Yukikatsu Terada; Hideki Uchiyama; Yasunobu Uchiyama; Shin Watanabe; Yoichi Yatsu; Kazutaka Yamaoka
SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY, Volume：7732, 2010, [Reviewed]
The Hard X-ray Imager (HXI) is one of four detectors on board the ASTRO-H mission (6th Japanese X-ray satellite), which is scheduled to be launched in 2014. Using the hybrid structure composed of double-sided silicon strip detectors and a cadmium telluride double-sided strip detector, the instrument fully covers the energy range of photons collected with the hard X-ray telescope up to 80 keV with a high quantum efficiency. High spatial resolution of 250 mu m and an energy resolution of 1-2 keV (FWHM) are both achieved with low noise front-end ASICs. In addition, the thick BGO active shields surrounding the main detector package is a heritage of the successful performance of the Hard X-ray Detector on board the Suzaku satellite. This feature enables the instrument to achieve an extremely high background reduction caused by cosmic-ray particles, cosmic X-ray background, and in-orbit radiation activation. In this paper, we present the detector concept, design, latest results of the detector development, and the current status of the hardware.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.857933
DOI ID：10.1117/12.857933, ISSN：0277-786X, Web of Science ID：WOS:000285506200033 - The Monte Carlo simulation framework of the ASTRO-H X-ray observatory
Masanobu Ozaki; Masanori Ohno; Yukikatsu Terada; Shin Watanabe; Tsunefumi Mizuno; Tadayuki Takahashi; Motohide Kokubun; Masahiro Tsujimoto; Noriko Y. Yamasaki; Hirokazu Odaka; Yoh Takei; Takayuki Yuasa; Akihiro Furuzawa; Hideyuki Mori; Hironori Matsumoto; Takashi Okajima; Caroline A. Kilbourne; Hiroyasu Tajima; Yoshitaka Ishisaki
SPACE TELESCOPES AND INSTRUMENTATION 2010: ULTRAVIOLET TO GAMMA RAY, Volume：7732, 2010, [Reviewed]
We are developing an ASTRO-H data analysis framework with the Geant4-based Monte Carlo simulation core, and numerical models of the on-orbit environmental radiation and full-satellite mass structure. In addition, the framework also includes a mechanism to connect and control data processing modules that are developed independently and data communication channels among them, which has been technically proven by simulations and analysis of the Suzaku HXD, many other detectors and astrophysical issues.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.856126
DOI ID：10.1117/12.856126, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000285506200102 - Development of a cadmium telluride pixel detector for astrophysical applications
Hiromasa Miyasaka; Fiona A. Harrison; Walter R. Cook; Peter H. Mao; Vikram R. Rana; Shin-Nosuke Ishikawa; Masayoshi Ushio; Hiroyuki Aono; Shin Watanabe; Goro Sato; Motohide Kokubun; Tadayuki Takahashi
Proceedings of SPIE - The International Society for Optical Engineering, Volume：7435, 2009, [Reviewed]
We are developing imaging Cadmium Telluride (CdTe) pixel detectors optimized for astrophysical hard X-ray applications. Our hybrid detector consist of a CdTe crystal 1mm thick and 2cm × 2cm in area with segmented anode contacts directly bonded to a custom low-noise application specific integrated circuit (ASIC). The CdTe sensor, fabricated by ACRORAD (Okinawa, Japan), has Schottky blocking contacts on a 605 micron pitch in a 32 × 32 array, providing low leakage current and enabling readout of the anode side. The detector is bonded using epoxy-gold stud interconnects to a custom low noise, low power ASIC circuit developed by Caltech's Space Radiation Laboratory. We have achieved very good energy resolution over a wide energy range (0.62keV FWHM @ 60keV, 10.8keV FWHM @ 662keV). We observe polarization effects at room temperature, but they are suppressed if we operate the detector at or below 0°C degree. These detectors have potential application for future missions such as the International X-ray Observatory (IXO). © 2009 Copyright SPIE - The International Society for Optical Engineering.
English, International conference proceedings
DOI：https://doi.org/10.1117/12.825711
DOI ID：10.1117/12.825711, ISSN：0277-786X, SCOPUS ID：78049398174 - Long-term stability of nonthermal X-ray modulation in the gamma-ray binary LS 5039
Tetsuichi Kishishita; Takaaki Tanaka; Yasunobu Uchiyama; Tadayuki Takahashi
Astrophysical Journal, Volume：697, Number：1, First page：L1, Last page：L5, 2009, [Reviewed]
We report on long-term stability of X-ray modulation apparently synchronized with an orbital period of 3.9days in the γ-ray binary LS 5039. Recent observations with the Suzaku satellite in the year 2007, which continuously covered more than one orbital period, have provided us with detailed characterization of X-ray flux and spectral shape as a function of orbital phase. Motivated by the results from Suzaku, we have re-analyzed the X-ray data obtained with ASCA, XMM-Newton, and Chandra between 1999 and 2005, to investigate long-term behavior of LS 5039 in the X-ray band. We found that the modulation curves in 1999-2007 are surprisingly stable. Even fine structures in the light curves such as spikes and dips are found to be quite similar from one orbit to another. The spectral characteristics observed in the past are consistent with those seen with Suzaku for some orbital phase segments. We suggest that magnetohydrodynamical collisions between the relativistic outflow from a compact object and the stellar wind from the O star explain the clock-like nonthermal X-ray emission over eight years through remarkably stable production of high-energy particles near the binary system. © 2009. The American Astronomical Society. All rights reserved.
Institute of Physics Publishing, English, Scientific journal
DOI：https://doi.org/10.1088/0004-637X/697/1/L1
DOI ID：10.1088/0004-637X/697/1/L1, ISSN：1538-4357, SCOPUS ID：67649188341 - Suzaku observations of PSR B1259-63: A new manifestation of relativistic pulsar wind
Yasunobu Uchiyama; Takaaki Tanaka; Tadayuki Takahashi; Koji Mori; Kazuhiro Nakazawa
Astrophysical Journal, Volume：698, Number：1, First page：911, Last page：921, 2009, [Reviewed]
We observed PSR B1259-63, a young nonaccreting pulsar orbiting around a Be star SS 2883, eight times with the Suzaku satellite from 2007 July to September, to characterize the X-ray emission arising from the interaction between a pulsar relativistic wind and Be star outflows. The X-ray spectra showed a featureless continuum in 0.6-10 keV, modeled by a power law with a wide range of photon indices 1.3-1.8. When combined with the Suzaku PIN detector which allowed spectral analysis in the hard 15-50 keV band, X-ray spectra do show a break at 5 keV in a certain epoch. Regarding the PSR B1259-63 system as a compactified pulsar wind nebula (PWN), in which e ± pairs are assumed to be accelerated at the inner shock front of the pulsar wind, we attribute the X-ray spectral break to the low-energy cutoff of the synchrotron radiation associated with the Lorentz factor of the relativistic pulsar wind γ1 4 × 105. Our result indicates that Comptonization of stellar photons by the unshocked pulsar wind will be accessible (or tightly constrained) by observations with the Fermi Gamma-ray Space Telescope during the next periastron passage. The PSR B1259-63 system allows us to probe the fundamental properties of the pulsar wind by a direct means, being complementary to the study of large-scale PWNe. © 2009. The American Astronomical Society. All rights reserved.
Institute of Physics Publishing, English, Scientific journal
DOI：https://doi.org/10.1088/0004-637X/698/1/911
DOI ID：10.1088/0004-637X/698/1/911, ISSN：1538-4357, SCOPUS ID：66649130232 - Current Status of the Suzaku Wide-band All-sky Monitor (WAM)
Kazutaka Yamaoka; Satoshi Sugita; Makoto Tashiro; Yukikatsu Terada; Yuji Urata; Akira Endo; Kaori Onda; Kouichi Morigami; Natsuki Kodaka; Takako Sugasawara; Wataru Iwakiri; Yasushi Fukazawa; Takeshi Uehara; Chie Kira; Yoshitaka Hanabata; Makoto Yamauchi; Eri Sonoda; Hiroki Tanaka; Ryuji Hara; Norisuke Ohmori; Hidenori Hayashi; Kenta Kono; Soojing Hong; Kazuo Makishima; Kazuhiro Nakazawa; Teruaki Enoto; Hiroyasu Tajima; Tadayuki Takahashi; Motohide Kokubun; Masanori Ohno; Yujin E. Nakagawa; Tohru Tamagawa; Toshio Murakami; Kevin Hurley
GAMMA-RAY BUSTS, Volume：1133, First page：91, Last page：93, 2009, [Reviewed]
The Suzaku Wide-band All-sky Monitor (WAM) consists of 20 BGO anti-coincidence scintillators for the Hard X-ray Detector (HXD), The WAM has a wide field of view (FOV), about half of the whole sky, a large collecting area, 800 cm(2), and broad-band energy coverage from 50 to 5000 keV. Thus it has been designed to work as a gamma-ray burst detector. For the three years since Suzaku launch in July 2005, the WAM has been working very well. About 500 GRBs have been detected through the end of 2008, corresponding to a detection rate of similar to 140 GRBs per year. The current status of the WAM is presented in this paper.
AMER INST PHYSICS, English, International conference proceedings
ISSN：0094-243X, Web of Science ID：WOS:000267717300026 - Suzaku Observation of a White Dwarf as a new Candidate of Cosmic-ray Origin
Yukikatsu Terada; T. Hayashi; M. Ishida; K. Mukai; T. Dotani; A. Bamba; S. Okada; R. Nakamura; K. Makishima; K. Morigami; A. Harayama
HIGH ENERGY GAMMA-RAY ASTRONOMY, Volume：1085, First page：689, Last page：+, 2009, [Reviewed]
Strongly magnetized white dwarfs (WDs) are able to accelerate particles like rotating neutron-star pulsars. If magnetized WDs are a new Cosmic-ray origin, they should be a quiet but numerous accelerators, giving important contributions of low-energy cosmic-rays. We performed a high sensitive search for possible hard X-ray emission from the fast rotating WD, AE Aquarii with Suzaku. The object has a magnetic field with 10(5) Gauss and a rapid spin period of 33 sec. From 100 ksec dataset of Suzaku XIS and HXD, we have discovered spiky pulsations like pulsars in the hard X-ray band of over 4 keV, in addition to the well-known thermal modulation in the softer band. In order to account for the hard X-ray signals with the HXD, the X-ray spectrum requires an additional hard X-ray component on the well-known thermal emissions with temperatures of 0.5 and 2.9 keV. Combined with results from timing analyses, spectral shapes and flux, we concluded that the hard X-ray pulsations should be a non-thermal origin, for example, possible Synchrotron emission with sub MeV electrons. Thus, the object must be a first discovery of a WD equivalent of a neutron star pulsar.
AMER INST PHYSICS, English, International conference proceedings
ISSN：0094-243X, Web of Science ID：WOS:000263556300146 - The Focusing Optics x-ray Solar Imager: FOXSI
Saem Krucker; Steven Christe; Lindsay Glesener; Steve McBride; Paul Turin; David Glaser; Pascal Saint-Hilaire; Gregory Delory; R. P. Lin; Mikhail Gubarev; Brian Ramsey; Yukikatsu Terada; Shin-nosuke Ishikawa; Motohide Kokubun; Shinya Saito; Tadayuki Takahashi; Shin Watanabe; Kazuhiro Nakazawa; Hiroyasu Tajima; Satoshi Masuda; Takashi Minoshima; Masumi Shomojo
OPTICS FOR EUV, X-RAY, AND GAMMA-RAY ASTRONOMY IV, Volume：7437, 2009, [Reviewed]
The Focusing Optics x-ray Solar Imager (FOXSI) is a sounding rocket payload funded under the NASA Low Cost Access to Space program to test hard x-ray focusing optics and position-sensitive solid state detectors for solar observations. Today's leading solar hard x-ray instrument, the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) provides excellent spatial (2 arcseconds) and spectral (1 keV) resolution. Yet, due to its use of indirect imaging, the derived images have a low dynamic range (< 30) and sensitivity. These limitations make it difficult to study faint x-ray sources in the solar corona which are crucial for understanding the solar flare acceleration process. Grazing-incidence x-ray focusing optics combined with position-sensitive solid state detectors can overcome both of these limitations enabling the next breakthrough in understanding particle acceleration in solar flares. The FOXSI project is led by the Space Science Laboratory at the University of California. The NASA Marshall Space Flight Center, with experience from the HERO balloon project, is responsible for the grazing-incidence optics, while the Astro H team (JAXA/ISAS) will provide double-sided silicon strip detectors. FOXSI will be a pathfinder for the next generation of solar hard x-ray spectroscopic imagers. Such observatories will be able to image the non-thermal electrons within the solar flare acceleration region, trace their paths through the corona, and provide essential quantitative measurements such as energy spectra, density, and energy content in accelerated electrons.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.827950
DOI ID：10.1117/12.827950, ISSN：0277-786X, Web of Science ID：WOS:000283842600004 - Development of a Digital Signal Processing System for the X-ray Microcalorimeter onboard ASTRO-H
Hiromi Seta; Makoto S. Tashiro; Yukikatsu Terada; Yuya Shimoda; Kaori Onda; Yoshitaka Ishisaki; Masahiro Tsujimoto; Toshishige Hagihara; Yoh Takei; Kazuhisa Mitsuda; Kevin R. Boyce; Andrew E. Szymkowiak
LOW TEMPERATURE DETECTORS LTD 13, Volume：1185, First page：278, Last page：+, 2009, [Reviewed]
A digital signal processing system for the X-ray microcalorimeter array (SXS) is being developed for the next Japanese X-ray astronomy satellite, ASTRO-H. The SXS digital signal processing system evaluates each pulse by an optimal filtering process. For the ASTRO-H project, we decided to employ digital electronics hardware, which includes a digital I/O board based upon FPGAs, and a separate CPU board. It is crucially important for the FPGA to be able to detect the presence of an "secondary" pulses on the tail of an initial pulse. In order to detect the contaminating pulses, we have developed a new finite impulse response filter, to compensate for the undershoot in the derivative. By employing the filter it is possible for FPGA to detect the secondary pulse very close the first pulse, and to reduce the load of the CPU in the secondary pulse searching process.
AMER INST PHYSICS, English, International conference proceedings
DOI：https://doi.org/10.1063/1.3292332
DOI ID：10.1063/1.3292332, ISSN：0094-243X, Web of Science ID：WOS:000281588500061 - Study of nonthermal emission from SNR RX J1713.7-3946 with Suzaku
Takaaki Tanaka; Yasunobu Uchiyama; Felix A. Aharonian; Tadayuki Takahashi; A. Y.A. Bamba; Junko S. Hiraga; Jun Kataoka; Tetsuichi Kishishita; Motohide Kokubun; Koji Mori; Kazuhiro Nakazawa; Robert Petre; Hiroyasu Tajima; Shin Watanabe
Astrophysical Journal, Volume：685, Number：2, First page：988, Last page：1004, Oct. 2008, [Reviewed]
We present results obtained from a series of observations of the supernova remnant RX J1713.7-3946 by Suzaku. Hard X-rays have been detected up to ∼40 keV. The hard X-ray spectra are described by a power law with photon indices of ∼3.0, which is larger than those below 10 keV. The combination of the spatially integrated XIS and HXD spectra clearly reveals a spectral cutoff which is linked to the maximum energy of accelerated electrons. The broad-band coverage of Suzaku allows us to derive, for the first time, the energy spectrum of parent electrons in the cutoff region. The cutoff energy in the X-ray spectrum indicates that the electron acceleration in the remnant proceeds close to the Bohm diffusion limit. We discuss the implications of the spectral and morphological properties of the Suzaku data in the context of the origin of nonthermal emission. The Suzaku X-ray and H.E.S.S. gamma-ray data together hardly can be explained within a pure leptonic scenario. Moreover, the leptonic models require a weak magnetic field, which is inconsistent with the recently discovered X-ray filamentary structures and their short-term variability. The hadronic models with strong magnetic fields provide reasonable fits to the observed spectra, but require special arrangements of parameters to explain the lack of thermal X-ray emission. For morphology studies, we compare the X-ray and TeV gamma-ray surface brightness. We confirm the previously reported strong correlation between X-rays and TeV gamma rays. At the same time, the Suzaku data reveal a deviation from the general tendency, namely, the X-ray emission in the western rims appears brighter than expected from the average X-ray to gamma-ray ratio. © 2008. The American Astronomical Society. All rights reserved.
Institute of Physics Publishing, English, Scientific journal
DOI：https://doi.org/10.1086/591020
DOI ID：10.1086/591020, ISSN：1538-4357, SCOPUS ID：53549103010 - White Dwarf Equivalent of Pulsars, Discovered with Suzaku
Terada, Yukikatsu
Astronomical Herald, Sep. 2008
Strongly magnetized white dwarfs have the potential to be a new particle acceleration site of a cosmic-ray origin. Since white dwarfs are common objects, they should become quiet but numerous accelerators giving important contributions to low-energy cosmic rays. Suzaku observed one of the most promising objects as accelerators, AE Aquarii, which has a magnetic field of 105 gauss and a rapid spin period of 33 seconds. The author discovered spiky pulsations like neutron star pulsars in the hard X-ray band of over 4 keV, in addition to the well-known thermal modulation in the softer band. From the timing features, spectral shapes and fluxes, he concludes that AE Aquarii is a white dwarf equivalent of neutron star pulsars....
Scientific journal
ORCID：101133876, Bibcode：2008AstHe.101..526T - PoGOLite - A high sensitivity balloon-borne soft gamma-ray polarimeter
Tuneyoshi Kamae; Viktor Andersson; Makoto Arimoto; Magnus Axelsson; Cecilia Marini Bettolo; Claes-Ingvar Bjornsson; Gilles Bogaert; Per Carlson; William Craig; Tomas Ekeberg; Olle Engdegdrd; Yasushi Fukazawa; Shuichi Gunji; Linnea Hjalmarsdotter; Bianca Iwan; Yoshikazu Kanai; Jun Kataoka; Nobuyuki Kawai; Jaroslav Kazejev; Mozsi Kiss; Wlodzimierz Klamra; Stefan Larsson; Grzegorz Madejski; Tsunefumi Mizuno; Johnny Ng; Mark Pearce; Felix Ryde; Markus Suhonen; Hiroyasu TaJima; Hiromitsu Takahashi; Tadayuki Takahashi; Takuya Tanaka; Timothy Thurston; Masaru Ueno; Gary Varneri; Kazuhide Yamamoto; Yuichiro Yamashita; Tomi Ylinen; Hiroaki Yoshida
ASTROPARTICLE PHYSICS, Volume：30, Number：2, First page：72, Last page：84, Sep. 2008, [Reviewed]
We describe a new balloon-borne instrument (PoGOLite) capable of detecting 10% polarisation from 200 mCrab point-like sources between 25 and 80 keV in one 6-h flight. Polarisation measurements in the soft gamma-ray band are expected to provide a powerful probe into high energy emission mechanisms as well as the distribution of magnetic fields, radiation fields and interstellar matter. Synchrotron radiation, inverse Compton scattering and propagation through high magnetic fields are likely to produce high degrees of polarisation in the energy band of the instrument. We demonstrate, through tests at accelerators, with radioactive sources and through computer simulations, that PoGOLite will be able to detect degrees of polarisation as predicted by models for several classes of high energy sources. At present, only exploratory polarisation measurements have been carried out in the soft gamma-ray band. Reduction of the large background produced by cosmic-ray particles while securing a large effective area has been the greatest challenge. PoGOLite uses Compton scattering and photo-absorption in an array of 217 well-type phoswich detector cells made of plastic and BGO scintillators surrounded by a BGO anticoincidence shield and a thick polyethylene neutron shield. The narrow Held of view (FWHM = 1.25 msr, 2.0 deg x 2.0 deg) obtained with detector cells and the use of thick background shields warrant a large effective area for polarisation measurements (similar to 228 cm(2) at E = 40 keV) without sacrificing the signal-to-noise ratio. Simulation studies for an atmospheric overburden of 3-4 g/cm(2) indicate that neutrons and gamma-rays entering the PDC assembly through the shields are dominant backgrounds. Off-line event selection based on recorded phototube waveforms and Compton kinematics reduce the background to that expected for a similar to 100 mCrab source between 25 and 50 keV. A 6-h observation of the Crab pulsar will differentiate between the Polar Cap/Slot Gap, Outer Gap, and Caustic models with greater than 5 sigma significance; and also cleanly identify the Compton reflection component in the Cygnus X-1 hard state. Long-duration flights will measure the dependence of the polarisation across the cyclotron absorption line in Hercules X-1. A scaled-down instrument will be flown as a pathfinder mission from the north of Sweden in 2010. The first science flight is planned to take place shortly thereafter. (C) 2008 Elsevier B.V. All rights reserved.
ELSEVIER SCIENCE BV, English, Scientific journal
DOI：https://doi.org/10.1016/j.astropartphys.2008.07.004
DOI ID：10.1016/j.astropartphys.2008.07.004, ISSN：0927-6505, eISSN：1873-2852, Web of Science ID：WOS:000260023500005 - Suzaku-WAM soft gamma-ray all-sky monitor by the earth occultation technique
Chie Kira; Yasushi Fukazawa; Tetsuya Asano; Hiromitsu Takahashi; Takuya Takahashi; Takeshi Uehara; Yoshitaka Hanabata; Kazutaka Yamaoka; Makoto Tashiro; Yukikatsu Terada; Masanori Ohno
Proceedings of Science, 2008
Suzaku Wide-band All-sky Monitor (WAM), which is the BGO Active Shield surrounding the Hard X-ray Detector (HXD) on-board Suzaku, has detected many gamma-ray bursts, soft gamma-ray repeaters, and solar flares. In addition, thanks to its large field of view (2π str), WAM can monitor bright soft gamma-ray sources with the earth occultation technique, as CGRO/BATSE. We have constructed the analysis system of the WAM earth occultation, calibrated the obtained spectra and flux by the Crab nebula, and found that the response uncertainty is around 20%. Therefore, WAM is an important all-sky monitor in the unique 50 keV - 1 MeV band against RXTE/ASM (1-10 keV) and Swift/BAT (10-100 keV), and enables us to monitor objects in wide energy band from 1 keV to 700 keV by utilizing these three instruments, as well as INTEGRAL. This is a great advantage to observe the hard tail of black hole binaries and search non-thermal components and 511 keV lines associated with the jet ejection. Here, we introduce preliminary results on Galactic black hole binaries. The long-term light curve of Cyg X-1 is successfully obtained around 100-600 keV with WAM. Together with light curves of RXTE/ASM and Swift/BAT, we can clearly see the different behavior between them. Noticeably, the bright phase in 2006 September is coincident with a detection at 0.1-1 TeV energies by MAGIC telescope. This event was also reported by RXTE/ASM, Swift/BAT and INTEGRAL/IBIS and SPI. In the average spectrum up to 700 keV of Cyg X-1, high energy cut-off is clearly seen. Furthermore, we obtained a monthly light curve and spectrum of GRS 1915+105, GX 339-4 and average spectra of some X-ray binaries. Many gamma-ray flares from black hole binaries are expected to be found by Fermi, and simultaneous X-ray monitoring with RXTE, Swift, INTEGRAL, and Suzaku is very important to constrain the emission mechanism.
English, International conference proceedings
ISSN：1824-8039, SCOPUS ID：84883630708 - Suzaku observation of AXP 1E 1841-045 in SNR Kes 73
M. Morii; S. Kitamoto; N. Shibazaki; D. Takei; N. Kawai; M. Arimoto; M. Ueno; Y. Terada; T. Kohmura; S. Yamauchi
AIP Conference Proceedings, Volume：983, First page：268, Last page：270, 2008, [Reviewed]
Anomalous X-ray pulsars (AXPs) are thought to be magnetars, which are neutron stars with ultra strong magnetic field of 1014-10 15G. Their energy spectra below ∼10keV are modeled well by two components consisting of a blackbody (BB) (∼0.4keV) and rather steep power-law (POW) function (photon index ∼2-4). Kuiper et al. (2004) discovered hard X-ray component above ∼10keV from some AXPs. Here, we present the Suzaku observation of the AXP 1E 1841-045 at the center of supernova remnant Kes 73. By this observation, we could analyze the spectrum from 0.4 to 50 keV at the same time. Then, we could test whether the spectral model above was valid or not in this wide energy range. We found that there were residual in the spectral fits when fit by the model of BB + POW. Fits were improved by adding another BB or POW component. But the meaning of each component became ambiguous in the phase-resolved spectroscopy. Alternatively we found that NPEX model fit well for both phase-averaged spectrum and phase-resolved spectra. In this case, the photon indices were constant during all phase, and spectral variation seemed to be very clear. This fact suggests somewhat fundamental meaning for the emission from magnetars. © 2008 American Institute of Physics.
English, International conference proceedings
DOI：https://doi.org/10.1063/1.2900159
DOI ID：10.1063/1.2900159, ISSN：0094-243X, SCOPUS ID：40749109743 - The spectral properties of the GRB prompt gamma-ray emission observed by the Suzaku Wide-band All-sky Monitor
Ohno M; Uehara T; Takahashi T; Fukazawa Y; Kira C; Hanabata Y; Yamaoka K; Nakagawa Y.E; Sugita S; Tamagawa T; Terada Y; Urata Y; Onda K; Kodaka N; Endo A; Suzuki M; Morigami K; Tashiro M.S; Enoto T; Miyawamki R; Nakazawa K; Makishima K; Sonoda E; Yamauchi M; Maeno S; Tanaka H; Hara R; Kokubun M; Suzuki M; Takahashi T; Hong S; Murakami T; Tajima H
AIP Conference Proceedings, Volume：1000, First page：101, Last page：104, 2008, [Reviewed]
DOI：https://doi.org/10.1063/1.2943418
DOI ID：10.1063/1.2943418, ORCID：34407232, SCOPUS ID：78649806841 - The X-ray micro calorimeter on the NeXT mission
Kazuhisa Mitsuda; Noriko Y. Yarnasaki; Keisuke Shinozaki; Yoh Takei; Takao Nakagawai; Hiroyuki Sugitai; Yohichi Satoh; Ryuichi Fujimoto; Takaya Ohashi; Yoshitaka Ishisaki; Yuichiro Ezoe; Masahide Murakami; Makoto Tashiro; Yukikatsu Terada; Shunji Kitarnoto; Torn Tarnagawa; Madoka Kawaharada; Tatehiro Mihara; Richard L. Kelley; Caroline A. Kilbourne; F. Scott Porter; Peter J. Shirron; Michael J. DiPirro; Dan McCanunon; Jan-Willem den Herderk
SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2, Volume：7011, 2008, [Reviewed]
The Soft, X-ray Spectrometer (SXS) onboard the NeXT (New exploration X-ray Telescope) is an X-ray spectrometer utilizing all X-ray microcalorimeter array. Combined with the soft, X-ray telescope of 6 m focal length, the instrument will have a similar to 290cm(2) effective at; 6.7 keV. With the large effective area and the energy resolution as good as 6 eV (FWHM), the instrument is very suited for the high-resolution spectroscopy of iron K emission line. One of the major scientific objectives of SXS is to determine turbulent and/or macroscopic motions of L-he hot gas in clusters of galaxies of up to z similar to 1. The instruments will use 6 x 6 or 8 x 8 format microcalorimeter array which is similar to that of Suzaku XRS. The detector will be cooled to a, cryogenic temperature of 50 mK by multi-stage cooling system consisting of adiabatic demagnetization refrigerator, super fluid He, a 3 He Joule Thomson cooler, and double-stage stirling cycle cooler.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.787952
DOI ID：10.1117/12.787952, ISSN：0277-786X, Web of Science ID：WOS:000259563700072 - Hard X-ray imager (HXI) for the NeXT mission
SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2, Volume：7011, 2008, [Reviewed]
DOI：https://doi.org/10.1117/12.788290
DOI ID：10.1117/12.788290, ISSN：0277-786X, Web of Science ID：WOS:000259563700020 - The NeXT mission
Tadayuki Takahashi; Richard Kelley; Kazuhisa Mitsuda; Hideyo Kunleda; Robert Petre; Nicholas White; Tadayasu Dotani; Ryuichi Fujimoto; Yasushi Fukazawa; Kiyoshi Hayashida; Manabu Ishida; Yoshitaka Ishisaki; Motohide Kokubun; Kazuo Makishima; Katsuji Koyama; Greg M. Madejski; Koji Mori; Richard Mushotzky; Kazuhiro Nakazawa; Yasushi Ogasaka; Takaya Ohashi; Masanobu Ozaki; Hiroyasu Tajima; Makoto Tashiro; Yukikatsu Terada; Hiroshi Tsunemi; Takeshi Go Tsuru; Yoshihiro Ueda; Noriko Yamasaki; Shin Watanabe
SPACE TELESCOPES AND INSTRUMENTATION 2008: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2, Volume：7011, 2008, [Reviewed]
The NeXT (New exploration X-ray Telescope). the new Japanese X-ray Astronomy Satellite following Suzaku, is all international X-ray mission which is currently planed for launch in 2013. NeXT is a combination of wide band X-ray spectroscopy (3-80 keV) provided by multi-layer coating, focusing hard X-ray mirror and hard X-ray imaging detectors, and high energy-resolution soft X-ray spectroscopy (0.3-10 keV) provided by thin-foil X-ray optics and a micro-calorimeter array. The mission will also carry an X-ray CCD camera as a focal plane detector for a soft, X-ray telescope and a non-focusing soft, gamma-ray detector. With these instruments, NeXT Covers very wide energy range from 0.3 keV to 600 keV. The micro-calorimeter system will be developed by international collaboration lead ISAS/JAXA and NASA. The simultaneous broad bandpass, coupled with high spectral resolution of Delta E similar to 7 eV by the micro-calorimeter will enable a wide variety of important, science themes to be pursued.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.789640
DOI ID：10.1117/12.789640, ISSN：0277-786X, Web of Science ID：WOS:000259563700017 - Effects of compton scattering on the gamma-ray spectra of solar flares
Jun'ichi Kotoku; Kazuo Makishima; Yukari Matsumoto; Mitsuhiro Kohama; Yukikatsu Terada; Toru Tamagawa
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, Number：6, First page：1161, Last page：1174, Dec. 2007, [Reviewed]
Using the fully relativistic GEANT4 simulation toolkit, Monte Carlo simulation was applied to the transport of energetic electrons generated in solar flares, and resultant bremsstrahlung gamma-ray spectra were calculated. The solar atmosphere was approximated by 10 vertically stacked zones. The simulation took into account two important physical processes: that the bremsstrahlung photons emitted by precipitating relativistic electrons are strongly forward beamed toward the photosphere, and that the majority of these gamma-rays must be Compton backscattered by the solar atmosphere in order to reach the observer. Then, the Compton degradation was found to make the observable gamma-ray spectra much softer than predicted by simple analytic calculations. The gamma-ray signals were found to be enhanced by several conditions, including a broad pitch-angle distribution of the electrons, a near-limb flare longitude, and a significant tilt in the magnetic field lines if the flare longitude is rather small. These results successfully explain several important flare properties observed in the range of hard X-ray to gamma-ray, in particular including those obtained with Yohkoh. A comparison of the Yohkoh spectrum, from a GOES X3.7 class limb flare on 1998 November 22, with a simulation assuming a broad electron pitch-angle distribution suggests that gamma-rays from this particular solar flare were a mixture of direct bremsstrahlung photons and their Comptonization.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/59.6.1161
DOI ID：10.1093/pasj/59.6.1161, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000252640900014 - Extremely fast acceleration of cosmic rays in a supernova remnant
Yasunobu Uchiyama; Felix A. Aharonian; Takaaki Tanaka; Tadayuki Takahashi; Yoshitomo Maeda
Nature, Volume：449, Number：7162, First page：576, Last page：578, Oct. 2007, [Reviewed]
Galactic cosmic rays (CRs) are widely believed to be accelerated by shock waves associated with the expansion of supernova ejecta into the interstellar medium. A key issue in this long-standing conjecture is a theoretical prediction that the interstellar magnetic field can be substantially amplified at the shock of a young supernova remnant (SNR) through magnetohydrodynamic waves generated by cosmic rays. Here we report a discovery of the brightening and decay of X-ray hot spots in the shell of the SNR RX J1713.7-3946 on a one-year timescale. This rapid variability shows that the X-rays are produced by ultrarelativistic electrons through a synchrotron process and that electron acceleration does indeed take place in a strongly magnetized environment, indicating amplification of the magnetic field by a factor of more than 100. The X-ray variability also implies that we have witnessed the ongoing shock-acceleration of electrons in real time. Independently, broadband X-ray spectrometric measurements of RX J1713.7-3946 indicate that electron acceleration proceeds in the most effective ('Bohm-diffusion') regime. Taken together, these two results provide a strong argument for acceleration of protons and nuclei to energies of 1 PeV (1015 eV) and beyond in young supernova remnants. ©2007 Nature Publishing Group.
Nature Publishing Group, English, Scientific journal
DOI：https://doi.org/10.1038/nature06210
DOI ID：10.1038/nature06210, ISSN：1476-4687, SCOPUS ID：34948879712 - Performance study of Si/CdTe semiconductor Compton telescopes with Monte Carlo simulation
Hirokazu Odaka; Shin'ichiro Takeda; Shin Watanabe; Shin-nosuke Ishikawa; Masayoshi Ushio; Takaaki Tanaka; Kazuhiro Nakazawa; Tadayuki Takahashi; Hiroyasu Tajima; Yasushi Fukazawa
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：579, Number：2, First page：878, Last page：885, Sep. 2007, [Reviewed]
A Compton telescope with high angular resolution and high energy resolution is a promising detector for the next generation of astrophysics space missions aiming at hard X-rays and sub-MeV/MeV gamma-rays. We have been working on a semiconductor Compton camera based on silicon and cadmium telluride (Si/CdTe Compton telescope). The soft gamma-ray detector (SGD) employs a Si/CdTe Compton camera combined with a well-type active shield. It will be mounted on the NeXT mission, proposed to be launched around 2012. One Compton camera module in the SGD will consist of 24 layers of double-sided silicon strip detectors and four layers of CdTe pixel detectors. We carried out Monte Carlo simulations to investigate the basic performance of the detector. Design parameters of devices required in the simulation, such as energy resolution and position resolution of the detector, are based on the results from our prototype detector. From the simulation using current design parameters, the detection efficiency is found to be higher than 10% at ∼100 keV and the angular resolution to be 9° and 4.4° at 120 keV and 330 keV, respectively. The effects of changing the design parameters are also discussed. © 2007.
English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2007.05.293
DOI ID：10.1016/j.nima.2007.05.293, ISSN：0168-9002, SCOPUS ID：34547809985 - Development of double-sided silicon strip detectors (DSSD) for a Compton telescope
Shin'ichiro Takeda; Shin Watanabe; Takaaki Tanaka; Kazuhiro Nakazawa; Tadayuki Takahashi; Yasushi Fukazawa; Hajimu Yasuda; Hiroyasu Tajima; Yoshikatsu Kuroda; Mitsunobu Onishi; Kei Genba
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：579, Number：2, First page：859, Last page：865, Sep. 2007, [Reviewed]
The low noise double-sided silicon strip detector (DSSD) technology is used to construct a next generation Compton telescope which is required to have both high-energy resolution and high-Compton reconstruction efficiency. In this paper, we present the result of a newly designed stacked DSSD module with high-energy resolution in highly packed mechanical structure. The system is designed to obtain good P-side and N-side noise performance by means of DC-coupled read-out. Since there are no decoupling capacitors in front-end electronics before the read-out ASICs, a high density stacked module with a pitch of 2 mm can be constructed. By using a prototype with four-layer of DSSDs with an area of 2.56 cm × 2.56 cm, we have succeeded to operate the system. The energy resolution at 59.5 keV is measured to be 1.6 keV (FWHM) for the P-side and 2.8 keV (FWHM) for the N-side, respectively. In addition to the DSSD used in the prototype, a 4 cm wide DSSD with a thickness of 300 μ m is also developed. With this device, an energy resolution of 1.5 keV (FWHM) was obtained. A method to model the detector energy response to properly handle split events is also discussed. © 2007.
English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2007.05.305
DOI ID：10.1016/j.nima.2007.05.305, ISSN：0168-9002, SCOPUS ID：34547790338 - Development of semiconductor imaging detectors for a Si/CdTe Compton camera
Shin Watanabe; Shin'ichiro Takeda; Shin-nosuke Ishikawa; Hirokazu Odaka; Masayoshi Ushio; Takaaki Tanaka; Kazuhiro Nakazawa; Tadayuki Takahashi; Hiroyasu Tajima; Yasushi Fukazawa; Yoshikatsu Kuroda; Mitsunobu Onishi
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：579, Number：2, First page：871, Last page：877, Sep. 2007, [Reviewed]
Si and CdTe semiconductor imaging detectors have been developed for use in a Si/CdTe Compton camera. Based on a previous study using the first prototype of a Si/CdTe Compton camera, new detector modules have been designed to upgrade the performance of the Compton camera. As the scatter detector of the Compton camera, a stack of double-sided Si strip detector (DSSD) modules, which has four layers with a stack pitch of 2 mm, was constructed. By using the stack DSSDs, an energy resolution of 1.5 keV (FWHM) was achieved. For the absorber detector, the CdTe pixel detector modules were built and a CdTe pixel detector stack using these modules was also constructed. A high energy resolution (Δ E / E ∼ 1 %) was achieved. The improvement of the detection efficiency by stacking the modules has been confirmed by tests of the CdTe stack. Additionally, a large area CdTe imager is introduced as one application of the CdTe pixel detector module. © 2007 Elsevier B.V. All rights reserved.
English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2007.05.306
DOI ID：10.1016/j.nima.2007.05.306, ISSN：0168-9002, SCOPUS ID：34547789853 - A 1-dimensional γ-ray position sensor based on GSO:Ce scintillators coupled to a Si strip detector
Takeshi Itoh; Takayuki Yanagida; Motohide Kokubun; Mitsuhiro Sato; Ryohei Miyawaki; Kazuo Makishima; Takeshi Takashima; Takaaki Tanaka; Kazuhiro Nakazawa; Tadayuki Takahashi; Naoaki Shimura; Hiroyuki Ishibashi
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：579, Number：1, First page：239, Last page：242, Aug. 2007, [Reviewed]
In order to improve a detection efficiency of the improved Fourier Synthesis imaging telescope, we are developing a one-dimensional γ-ray position sensor using crystal scintillators coupled to a silicon strip detector (SSD). We have manufactured thin Gd2 SiO5:Ce (GSO) scintillator plates with a dimension of 10 mm × 5 mm × 0.3 mm. Twenty scintillator plates, with a light reflective sheet between adjacent plates, have been stacked into a block (stacked GSO). The SSD has 32 strip electrodes of 400 μ m pitch on its p-side, while its n-side common electrode is not metallic. The pulse height of the 32 channels are read out simultaneously by an analog ASIC. We coupled the stacked GSO to the n-side of the SSD with the GSO plates running parallel to the SSD strips. By irradiating the coupled device with γ-rays from 137Cs and 22Na, we successfully obtained their spectra, and achieved a position resolution significantly finer than 1 mm. © 2007 Elsevier B.V. All rights reserved.
English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2007.04.144
DOI ID：10.1016/j.nima.2007.04.144, ISSN：0168-9002, SCOPUS ID：34547671032 - A high-energy resolution 4 cm-wide double-sided silicon strip detector
Kazuhiro Nakazawa; Shin'ichiro Takeda; Takaaki Tanaka; Tadayuki Takahashi; Shin Watanabe; Yasushi Fukazawa; Naoyuki Sawamoto; Hiroyasu Tajima; Takeshi Itoh; Motohide Kokubun
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：573, Number：1-2, First page：44, Last page：47, Apr. 2007, [Reviewed]
Double-sided silicon strip detectors (DSSD) with an energy resolution of 1-2 keV full-width at half-maximum (FWHM) are attractive devices for future hard X-ray and soft γ-ray applications. For example, they are well suited as scatterer detectors for semiconductor Compton telescopes working in the sub-MeV to MeV band, as well as imaging spectrometers in the hard X-ray band. In this paper, the performance of newly developed 4-cm-wide DSSDs is presented.This DSSD has an active area of 38.4 mm times 38.4 mm, with a thickness of 300 μm. The stip pitch is 400 μm. The detector shows an average energy resolution of 1.5 keV (FWHM) for 59.5 keV γ-rays, operated at -20 °C with a bias of 100 V. A 22 keV hard X-ray image is also obtained with 400 μm resolution. © 2006 Elsevier B.V. All rights reserved.
English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2006.10.265
DOI ID：10.1016/j.nima.2006.10.265, ISSN：0168-9002, SCOPUS ID：33847658440 - A stacked CdTe pixel detector for a compton camera
Kousuke Oonuki; Takaaki Tanaka; Shin Watanabe; Shin'ichiro Takeda; Kazuhiro Nakazawa; Masayoshi Ushio; Takefumi Mitani; Tadayuki Takahashi; Hiroyasu Tajima
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：573, Number：1-2, First page：57, Last page：60, Apr. 2007, [Reviewed]
We are developing a semiconductor Compton telescope to explore the universe in the energy band from several tens of keV to a few MeV. A detector material of combined Si strip and CdTe pixel is used to cover the energy range around 60 keV. For energies above several hundred keV, in contrast, the higher detection efficiency of CdTe semiconductor in comparison with Si is expected to play an important role as both an absorber and a scatterer. In order to demonstrate the spectral and imaging capability of a CdTe-based Compton camera, we developed a Compton telescope consisting of a stack of CdTe pixel detectors as a small scale prototype. With this prototype, we succeeded in reconstructing images and spectra by solving the Compton kinematics within the energy band from 122 to 662 keV. The energy resolution (FWHM) of reconstructed spectra is 7.3 keV at 511 keV. The angular resolution obtained at 511 keV is measured to be 12 . 2{ring operator} (FWHM). © 2006.
English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2006.10.251
DOI ID：10.1016/j.nima.2006.10.251, ISSN：0168-9002, SCOPUS ID：33847628074 - Probing the disk-jet connection of the radio galaxy 3C 120 observed with Suzaku
Jun Kataoka; James N. Reeves; Kazushi Iwasawa; Alex G. Markowitz; Richard F. Mushotzky; Makoto Arimoto; Tadayuki Takahashi; Yoshihiro Tsubuku; Masayoshi Ushio; Shin Watanabe; Luigi C. Gallo; Greg M. Madejski; Yuichi Terashima; Naoki Isobe; Makoto S. Tashiro; Takayoshi Kohmura
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, Number：2, First page：279, Last page：297, Apr. 2007, [Reviewed]
We report on deep (40 ks x 4) observations of the bright broad line radio galaxy 3C 120 using Suzaku. The observations were spaced one week apart, and sampled a range of continuum fluxes. An excellent broadband spectrum was obtained over two decades of frequency (0.6 to 50 keV) within each 40 ks exposure. We clearly resolved the iron K emission-line complex, finding that it consists of a narrow K alpha core (sigma similar or equal to 110 eV or an EW of 60 eV), a 6.9 keV line, and an underlying broad iron line. Our confirmation of the broad line contrasts with the XMM-Newton observation in 2003, where the broad line was not required. The most natural interpretation of the broadline is iron Kline emission from a face-on accretion disk that is truncated at similar to 10 r(g). Above 10 keV, a relatively weak Compton hump was detected (reflection fraction of R similar or equal to 0.6), superposed on the primary X-ray continuum of Gamma similar or equal to 1.75. Thanks to the good photon statistics and low background of the Suzaku data, we clearly confirm the spectral evolution of 3C 120, whereby the variability amplitude decreases with increasing energy. More strikingly, we discovered that the variability is caused by a steep power-law component of Gamma similar or equal to 2.7, possibly related to non-thermal jet emission. We discuss our findings in the context of similarities and differences between radio-loud/quiet objects.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/59.2.279
DOI ID：10.1093/pasj/59.2.279, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000246404000003 - Strategy of the Suzaku gamma-ray burst observations
Yukikatsu Terada
Advances in Space Research, 2007
Scientific journal
DOI：https://doi.org/10.1016/J.ASR.2007.02.081
DOI ID：10.1016/J.ASR.2007.02.081, ORCID：67259966, Web of Science ID：WOS:000253589900013 - Suzaku observation of TeV SNR RX J1713.7-3946
Tadayuki Takahashi; Takaaki Tanaka; Yasunobu Uchiyama; Junko S. Hiraga; Kazuhiro Nakazawa; Shin Watanabe; Aya Bamba; John P. Hughes; Hideaki Katagiri; Jun Kataoka; Motohide Kokubun; Katsuji Koyama; Koji Mori; Robert Petre; Hiromitsu Takahashi; Yoko Tsuboi
Progress of Theoretical Physics Supplement, Number：169, First page：157, Last page：161, 2007, [Reviewed]
We report on results from Suzaku broadband X-ray observations of the Galactic supernova remnant (SNR) RX J1713.7-3946 with an energy coverage of 0.4-40 keV. With a sensitive hard X-ray measurement from the HXD PIN on board Suzaku, we determine the hard X-ray spectrum in the 12-40 keV range to be described by a power law with photon index Γ = 3.2 ± 0.2, significantly steeper than the soft X-ray index of Γ = 2.4 ± 0.05 measured previously with ASCA and other missions. We find that a simple power law fails to describe the full spectral range of 0.4-40 keV and instead a cutoff power law with hard index Γ = 1.96 ± 0.05 and high energy cutoff εc = 9 ± 1 keV provides an excellent fit over the full bandpass.
Yukawa Institute for Theoretical Physics, English, International conference proceedings
DOI：https://doi.org/10.1143/PTPS.169.157
DOI ID：10.1143/PTPS.169.157, ISSN：1347-4081, SCOPUS ID：41149104072 - Wide-band study of X-ray pulsars with Suzaku
T. Enoto; R. Miyawaki; M. Kokubun; K. Makishima; Y. Terada; T. Mihara; M. Nakajima; M. Suzuki; A. Bamba; A. Senda; K. Makishima; Y. Ishisaki; H. Takahashi; K. Tamura; S. Naik; K. Ebisawa; F. Nagase; S. Kitamoto; K. Sudoh; A. Yoshida; Y. Nakagawa; S. Sugita; T. Kohmura; T. Kotani; N. Kawai; D. Yonetoku; K. Mori
6TH INTEGRAL WORKSHOP: THE OBSCURED UNIVERSE, Volume：622, First page：453, Last page：+, 2007, [Reviewed]
A summary is given on the timing accuracy verifications of the Hard X-ray Detector (HXD) on board the Suzaku satellite. Suzaku has so far observed several Xray pulsars, such as the Crab pulsar, PSR 1509-58, and A0535+26, partially for the purpose of calibrating the HXD timing accuracy and energy responses. Through standard barycentric corrections and temperature compensations of the oscilator in the central data processing unit, the relative and absolute timing accuracies were confirmed using the HXD data of the Crab pulsar. Some initial Suzaku results on X-ray pulsars are also presented.
ESA PUBLICATIONS DIVISION C/O ESTEC, English, International conference proceedings
ISSN：0379-6566, Web of Science ID：WOS:000253876500084 - In orbit timing calibration of the Suzaku hard X-ray detector
Yukikatsu Terada; Teruaki Enoto; Ryouhei Miyawaki; Yasushi Fukazawa; Madoka Kawaharada; Tsuneyoshi Kamae; Motohide Kokubun; Kazuo Makishima; Tsunefumi Mizuno; Toshio Murakami; Kazuhiro Nakazawa; Masaharu Nomach; Tadayuki Takahashi; Hiromitsu Takahashi; Makoto S. Tashiro; Toru Tamagawa; Shin Watanabe; Kazutaka Yamaoka; Daisuke Yonetoku
IEEE Nuclear Science Symposium Conference Record, Volume：2, First page：783, Last page：787, 2007, [Reviewed]
Suzaku is the fifth Japanese astrophysical satellite, devoted to study high energy phenomena in the X-ray band of 0.5 - 600 keV. It was successfully launched from Uchinoura Space Center in Japan on 10th July 2005. The HXD on board Suzaku covers 10 - 600 keV band with a high sensitivity of about 10 -5 cnt/s/cm2/keV level. The sensor consists of 16 identical GSO/BGO well-type-phoswich counters incorporating 2 mm-thick silicon PIN diodes, and 20 surrounding-BGO-shield counters to remove residual non X-ray backgrounds through anti-coincidence rejection. The present paper is particularly focused on timing system of the HXD and in-orbit verifications with pulsars. © 2006 IEEE.
English, International conference proceedings
DOI：https://doi.org/10.1109/NSSMIC.2006.355968
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=38649105205&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=38649105205&origin=inward
DOI ID：10.1109/NSSMIC.2006.355968, ISSN：1095-7863, SCOPUS ID：38649105205, Web of Science ID：WOS:000288875600156 - Suzaku observations of the local and distant hot ISM
Randall K. Smith; Mark W. Bautz; Richard J. Edgar; Ryuichi Fujimoto; Kenji Hamaguchi; John R. Hughes; Manabu Ishida; Richard Kelley; Caroline A. Kilbourne; K. D. Kuntz; Dan McCammon; Eric Miller; Kazuhisa Mitsuda; Koji Mukai; Paul P. Plucinsky; F. Scott Porter; Steve L. Snowden; Yoh Takei; Yukikatsu Terada; Yohko Tsuboi; Noriko Y. Yamasaki
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S141, Last page：S150, Jan. 2007, [Reviewed]
Suzaku observed the molecular cloud MBM 12 and a blank field less than 3 degrees away to separate the local and distant components of the diffuse soft X-ray background. Towards MBM 12, a local (D less than or similar to 275 pc) O VII emission line was clearly detected with an intensity of 3.5 photons cm(-2) s(-1) sr(-1) (or line units, LU), and the O VIII flux was < 0.34 LU. The origin of this O VII emission could be hot gas in the Local Hot Bubble (LHB), charge exchange within the heliosphere with oxygen ions from the solar wind (SWCX), or both. If entirely from the LHB, the emission could be explained by a region with emission measure of 0.0075 cm(-6) pc and a temperature of 1.2 x 10(6) K. However, this temperature and emission measure implies 1/4 keV emission in excess of observations. There is no evidence in the X-ray light curve or solar wind data for a significant contribution from geocoronal SWCX, although interplanetary SWCX is still possible. In any case, the observed O VII flux represents an upper limit to both the LHB emission and interplanetary SWCX in this direction. The blank field was observed immediately afterwards. The net off-cloud O VII and O VIII intensities were (respectively) 2.34 +/- 0.33 and 0.77 +/- 0.16 LU, after subtracting the on-cloud foreground emission. If this more distant O VII and O VIII emission is from a thermal plasma in collisional equilibrium beyond the Galactic disk, we infer it has a temperature of (2.1 +/- 0.1) x 10(6) K with an emission measure of (4 +/- 0.6) x 10(-3) cm(-6) pc.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/59.sp1.S141
DOI ID：10.1093/pasj/59.sp1.S141, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000244441700009 - In-orbit performance of the hard X-ray Detector on board Suzaku
Motohide Kokubun; Kazuo Makishima; Tadayuki Takahashi; Toshio Murakami; Makoto Tashiro; Yasushi Fukazawa; Tuneyoshi Kamae; Greg M. Madejski; Kazuhiro Nakazawa; Kazutaka Yamaoka; Yukikatsu Terada; Daisuke Yonetoku; Shin Watanabe; Toru Tamagawa; Tsunefumi Mizuno; Aya Kubota; Naoki Isobe; Isao Takahashi; Goro Sato; Hiromitsu Takahashi; Soojing Hong; Madoka Kawaharada; Naomi Kawano; Takefumi Mitani; Mio Murashima; Masaya Suzuki; Keiichi Abe; Ryouhei Miyawaki; Masanori Ohno; Takaaki Tanaka; Takayuki Yanagida; Takeshi Itoh; Kousuke Ohnuki; Ken-ichi Tamura; Yasuhiko Endo; Shinya Hirakuri; Tatsuro Hiruta; Takao Kitaguchi; Tetsuichi Kishishita; Satoshi Sugita; Takuya Takahashi; Shin'ichiro Takeda; Teruaki Enoto; Ayumi Hirasawa; Jun'ichiro Katsuta; Satoshi Matsumura; Kaori Onda; Mitsuhiro Sato; Masayoshi Ushio; Shin-nosuke Ishikawa; Koichi Murase; Hirokazu Odaka; Masanobu Suzuki; Yuichi Yaji; Shinya Yamada; Tomonori Yamasaki; Takayuki Yuasa
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S53, Last page：S76, Jan. 2007, [Reviewed]
The in-orbit performance and calibration of the Hard X-ray Detector (HXD) on board the X-ray astronomy satellite Suzaku are described. Its basic performances, including a wide energy bandpass of 10-600keV, energy resolutions of similar to 4 keV (FWHM) at 40 keV and similar to 11% at 511 keV, and a high background rejection efficiency, have been confirmed by extensive in-orbit calibrations. The long-term gains of PIN-Si diodes have been stable within 1% for half a year, and those of scintillators have decreased by 5-20%. The residual non-X-ray background of the HXD is the lowest among past non-imaging hard X-ray instruments in energy ranges of 15-70 and 150-500 keV. We provide accurate calibrations of energy responses, angular responses, timing accuracy of the HXD, and relative normalizations to the X-ray CCD cameras using multiple observations of the Crab Nebula.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/59.sp1.S53
DOI ID：10.1093/pasj/59.sp1.S53, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000244441700005 - The X-ray observatory Suzaku
Kazuhisa Mitsuda; Mark Bautz; Hajime Inoue; Richard L. Kelley; Katsuji Koyama; Hideyo Kunieda; Kazuo Makshima; Yoshiaki Ogawara; Robert Petre; Tadayuki Takahashi; Hiroshi Tsunemi; Nicholas E. White; Naohisa Anabuki; Lorella Angelini; Keith Arnaud; Hisamitsu Awaki; Aya Bamba; Kevin Boyce; Gregory V. Brown; Kai-Wing Chan; Jean Cottam; Tadayasu Dotanli; John Doty; Ken Ebisawa; Yuichiro Ezoe; Andrew C. Fabian; Enectali Figueroa; Ryuichi Fujimoto; Yasushi Fukazawa; Tae Furusho; Akihiro Furuzawa; Keith Gendreau; Richard E. Griffiths; Yoshito Haba; Kenji Hamaguchi; Ilana Harrus; Gunther Hasinger; Isamu Hatsukade; Kiyoshi Hayashida; Patrick J. Henry; Junko S. Hiraga; Stephen S. Holt; Ann Hornschemeier; John P. Hughes; Una Hwang; Manabu Ishida; Yoshitaka Ishisaki; Naoki Isobe; Masayuki Itoh; Naoko Iyomoto; Steven M. Kahn; Tuneyoshi Kamae; Hideaki Katagiri; Jun Kataoka; Haruyoshi Katayama; Nobuyuki Kawai; Caroline Kilbourne; Kenzo Kinugasa; Steve Kissel; Shunji Kitamoto; Mitsuhiro Kohama; Takayoshi Kohmura; Motohide Kokubun; Taro Kotani; Jun'ichi Kotoku; Aya Kubota; Greg M. Madejski; Yoshitomo Maeda; Fumiyoshi Makino; Alex Markowitz; Chiho Matsumoto; Hironori Matsumoto; Masaru Matsuoka; Kyoko Matsushita; Dan McCammon; Tatehiko Mihara; Kazutami Misaki; Emi Miyata; Tsunefumi Mizuno; Koji Mori; Hideyuki Mori; Mikio Morii; Harvey Moseley; Koji Mukai; Hiroshi Murakami; Toshio Murakami; Richard Mushotzky; Fumiaki Nagase; Masaaki Namiki; Hitoshi Negoro; Kazubiro Nakazawa; John A. Nousek; Takashi Okajima; Yasushi Ogasaka; Takaya Ohashi; Tai Oshima; Naomi Ota; Masanobu Ozaki; Hideki Ozawa; Arvind N. Parmar; William D. Pence; F. Scott Porter; James N. Reeves; George R. Ricker; Ikuya Sakurai; Wilton T. Sanders; Atsushi Senda; Peter Serlemitsos; Ryo Shibata; Yang Soong; Randall Smith; Motoko Suzuki; Andrew E. Szymkowiak; Hiromitsu Takahashi; Torn Tamagawa; Keisuke Tamura; Takayuki Tamura; Yasuo Tanaka; Makoto Tashiro; Yuzuru Tawara; Yukikatsu Terada; Yuichi Terashima; Hiroshi Tomida; Ken'ichi Torii; Yohko Tsuboi; Masahiro Tsujimoto; Takeshi Go Tsuru; Martin J. L. Turner; Yoshihiro Ueda; Shiro Ueno; Masaru Ueno; Shin'ichiro Uno; Yuji Urata; Shin Watanabe; Norimasa Yamamoto; Kazutaka Yamaoka; Noriko Y. Yamasaki; Koujun Yamashita; Makoto Yamauchi; Shigeo Yamauchi; Tahir Yaqoob; Daisuke Yonetoku; Atsumasa Yoshida
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S1, Last page：S7, Jan. 2007, [Reviewed]
High-sensitivity wide-band X-ray spectroscopy is the key feature of the Suzaku X-ray observatory, launched on 2005 July 10. This paper summarizes the spacecraft, in-orbit performance, operations, and data processing that are related to observations. The scientific instruments, the high-throughput X-ray telescopes, X-ray CCD cameras, non-imaging hard X-ray detector are also described.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/59.sp1.S1
DOI ID：10.1093/pasj/59.sp1.S1, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000244441700001 - Hard X-ray Detector (HXD) on board Suzaku
Tadayuki Takahashi; Keiichi Abe; Manabu Endo; Yasuhiko Endo; Yuuichiro Ezoe; Yasushi Fukazawa; Masahito Hamaya; Shinya Hirakuri; Soojing Hong; Michihiro Horii; Hokuto Inoue; Naoki Isobe; Takeshi Itoh; Naoko Iyomoto; Tuneyoshi Kamae; Daisuke Kasama; Jun Kataoka; Hiroshi Kato; Madoka Kawaharada; Naomi Kawano; Kengo Kawashima; Satoshi Kawasoe; Tetsuichi Kishishita; Takao Kitaguch; Yoshihito Kobayashi; Motohide Kokubun; Jun'ichi Kotoku; Manabu Kouda; Aya Kubota; Yoshikatsu Kuroda; Greg Madejski; Kazuo Makishima; Kazunori Masukama; Yukari Matsumoto; Takefumi Mitani; Ryohei Miyawaki; Tsunefumi Mizuno; Kunishiro Mori; Masanori Mori; Mio Murashima; Toshio Murakami; Kazuhiro Nakazawa; Hisako Niko; Masaharu Nomachi; Yuu Okada; Masanori Ohno; Kousuke Oonuki; Naomi Ota; Hideki Ozawa; Goro Sato; Shingo Shinoda; Masahiko Sugiho; Masaya Suzuki; Koji Taguchi; Hiromitsu Takahashi; Isao Takahashi; Shin'ichiro Takeda; Ken-ichi Tamura; Takayuki Tamura; Takaaki Tanaka; Chiharu Tanihata; Makoto Tashiro; Yukikatsu Terada; Shin'ya Tominaga; Yasunobu Uchiyama; Shin Watanabe; Kazutaka Yamaoka; Takayuki Yanagida; Daisuke Yonetoku
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S35, Last page：S51, Jan. 2007, [Reviewed]
The Hard X-ray Detector (HXD) on board Suzaku covers a wide energy range from 10 keV to 600 keV by the combination of silicon PIN diodes and GSO scintillators. The HXD is designed to achieve an extremely low in-orbit background based on a combination of new techniques, including the concept of a well-type active shield counter. With an effective area of 142 cm(2) at 20 keV and 273 cm(2) at 150 keV, the background level at sea level reached similar to 1 X 10(-5) cts s(-1) cm(-2) keV(-1) at 30 keV for the PIN diodes, and similar to 2 X 10(-5) cts s(-1) cm(-2) keV(-1) at 100 keV, and similar to 7 X 10(-6) cts s(-1) cm(-2) keV(-1) at 200 keV for the phoswich counter. Tight active shielding of the HXD results in a large array of guard counters surrounding the main detector parts. These anti-coincidence counters, made of similar to 4 cm thick BGO crystals, have a large effective area for sub-MeV to MeV gamma-rays. They work as an excellent gamma-ray burst monitor with limited angular resolution (similar to 5 degrees). The on-board signal-processing system and the data transmitted to the ground are also described.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/59.sp1.S35
DOI ID：10.1093/pasj/59.sp1.S35, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000244441700004 - An apparent hard X-ray decline of CH Cygni
Koji Mukai; Manabu Ishida; Caroline Kilbourne; Hideyuki Mori; Yukikatsu Terada; Kai-Wing Chan; Yang Soong
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S177, Last page：S183, Jan. 2007, [Reviewed]
CH Cygni is a symbiotic star consisting of an M giant and an accreting white dwarf, which is known to be a highly variable X-ray source with a complex, two-component, spectra. Here, we report on two Suzaku observations of CH Cyg, taken in 2006 January and May, during which the system was seen to be in a soft X-ray bright, hard X-ray faint state. Based on the extraordinary strength of the 6.4 keV fluorescent Fe K alpha line, we show that the hard X-rays observed with Suzaku are dominated by scattering.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/59.sp1.S177
DOI ID：10.1093/pasj/59.sp1.S177, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000244441700013 - Millenium study of SN 1006 with suzaku
Aya Bamba; Hiroya Yamaguchi; Katsuji Koyama; Junko S. Hiraga; Steve Holt; John P. Hughes; Hideaki Katagiri; Jun Kataoka; Shunji Kitamoto; Motohide Kokubun; Hironori Matumoto; Emi Miyata; Koji Mori; Hiroshi Nakajima; Masanobu Ozaki; Robert Petre; Akiko Sekiguchi; Tadayuki Takahashi; Takaaki Tanaka; Yukikatsu Terada; Hiroshi Tomida; Hiroshi Tsunemi; Yohko Tsub; Masahiro Tsujimoto; Yasunobu Uchiyama; Masaru Ueno; Shin Watanabe
PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT, Number：169, First page：142, Last page：145, 2007, [Reviewed]
SN 1006 is the milestone of understanding the acceleration mechanism of cosmic rays, and this year is the millennium year for the remnant. We carried out SN 1006 mapping observations with the X-ray Imaging Spectrometers (XIS) onboard Suzaku satellite. Thanks to the excellent spectral response of XIS, K emission lines from highly ionized oxygen were clearly resolved. The intensity maps of these lines have been made additional to the intensity and photon index maps of the nonthermal component. We discovered that regions with strong and hard nonthermal component has weak thermal emission. The north rim of the SNR has the hardest nonthermal component. These facts might have information of efficient cosmic ray acceleration and background plasma.
PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE, English, Scientific journal
ISSN：0375-9687, Web of Science ID：WOS:000252207900034 - Suzaku observations of the dwarf nova SS Cyg in quiescence and outburst
Manabu Ishida; Shunsaku Okada; Ryoko Nakamura; Yukikatsu Terada; Takayuki Hayashi; Koji Mukai; Kenji Hamaguchi
PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT, Number：169, First page：178, Last page：181, 2007, [Reviewed]
We present the results from the Suzaku observations of SS Cyg in quiescence and outburst carried out in November, 2005. Owing to an excellent energy-resolving power of the XIS, we resolved the 6.4 keV iron K alpha line into a narrow component and a broad tail in quiescence, which probably originate from the white dwarf and inner accretion disk, respectively. The 6.4 keV line in outburst is dominated by an extremely broad component. These 6.4 keV line features are first recognized by Suzaku this time. Using the iron abundance of 0.30 +/- 0.03Z(circle dot) obtained from our analysis of the outburst spectra, we set the upper limit of the radial extent of the BL to be < 0.15R(WD) in quiescence.
PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE, English, Scientific journal
ISSN：0375-9687, Web of Science ID：WOS:000252207900042 - Cyclotron observations of binary X-ray pulsars
Tatehiro Mihara; Yukikatsu Terada; Motoki Nakajima; Motoko Suzuki; Teruaki Enoto; Kazuo Makishima; Fumiaki Nagase; Keisuke Sudoh
PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT, Number：169, First page：191, Last page：195, 2007, [Reviewed]
Suzaku has observed some cyclotron X-ray pulsars in the SWG (Science working group) phase. Suzaku detected the cyclotron feature in the lowest luminosity from A0535+26. In Her X-1, Suzaku measured new data points in the year-long trend of cyclotron resonance energy, and searched for the second harmonic structure. The RXTE observations of X0331+53 gave the second example on changing the resonance energy and indicated that the energy ratio of the 2nd and 1st cyclotron energies is apart from two.
PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE, English, Scientific journal
ISSN：0375-9687, Web of Science ID：WOS:000252207900045 - The 7-steps of the data analysis
Yukikatsu Terada; Aya Bamba; Junko S. Hiraga; Naoki Isobe; Aya Kubota; Naomi Ota; Piero Ranalli; Atsushi Senda; Motoko Suzuki; Toru Tamagawa; Yuji Urata; Masanobu Ozaki; Ken Ebisawa; Yoshitaka Ishisaki; Hironori Matsumoto; Izumi Yamagishi; Takayuki Tamura; Koji Mukai; Lorella Angellini; Kenji Hamaguchi
PROGRESS OF THEORETICAL PHYSICS SUPPLEMENT, Number：169, First page：312, Last page：315, 2007, [Reviewed]
It may seem to be difficult to analyze the Suzaku data, but the data structure and the tools are rather simple. We have constructed the way to process Suzaku FITS data and ftools for over ten years. We have prepared three kinds of manuals to analyze the data; Seven step manual of the XIS and the HXD for beginners, first step manual to walk through the analyses, and the ABC guide as a full manual. In the actual analyses, we have to be careful about events in operation and the limitations in the calibration of instruments. In this paper, the data structure, tools, and manuals with activities of help desks, current status of processing are summarized.
PROGRESS THEORETICAL PHYSICS PUBLICATION OFFICE, English, Scientific journal
ISSN：0375-9687, Web of Science ID：WOS:000252207900071 - Recent results from a Si/CdTe semiconductor Compton telescope
Takaaki Tanaka; Shin Watanabe; Shin'ichiro Takeda; Kousuke Oonuki; Takefumi Mitani; Kazuhiro Nakazawa; Takeshi Takashima; Tadayuki Takahashi; Hiroyasu Tajima; Naoyuki Sawamoto; Yasushi Fukazawa; Masaharu Nomachi
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：568, Number：1, First page：375, Last page：381, Nov. 2006, [Reviewed]
We are developing a Compton telescope based on high-resolution Si and CdTe detectors for astrophysical observations in sub-MeV/MeV gamma-ray region. Recently, we constructed a prototype Compton telescope which consists of six layers of double-sided Si strip detectors (DSSDs) and CdTe pixel detectors to demonstrate the basic performance of this new technology. By irradiating the detector with gamma rays from radio isotope sources, we have succeeded in Compton reconstruction of images and spectra. The obtained angular resolution is 3.9°(FWHM) at 511 keV, and the energy resolution is 14 keV (FWHM) at the same energy. In addition to the conventional Compton reconstruction, i.e., drawing cones in the sky, we also demonstrated a full reconstruction by tracking Compton recoil electrons using the signals detected in successive Si layers. By irradiating 137Cs source, we successfully obtained an image and a spectrum of 662 keV line emission with this method. As a next step, development of larger DSSDs with a size of 4 cm × 4 cm is under way to improve the effective area of the Compton telescope. We are also developing a new low-noise analog ASIC to handle the increasing number of channels. Initial results from these two new technologies are presented in this paper as well. © 2006 Elsevier B.V. All rights reserved.
English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2006.06.014
DOI ID：10.1016/j.nima.2006.06.014, ISSN：0168-9002, SCOPUS ID：33750393686 - Development of CdTe pixel detectors for Compton cameras
Shin Watanabe; Takaaki Tanaka; Kousuke Oonuki; Takefumi Mitani; Shin'ichiro Takeda; Tetsuichi Kishishita; Kazuhiro Nakazawa; Tadayuki Takahashi; Yoshikatsu Kuroda; Mitsunobu Onishi
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：567, Number：1, First page：150, Last page：153, Nov. 2006, [Reviewed]
We report our development of CdTe pixel detectors for Si/CdTe semiconductor Compton cameras. We have constructed a prototype of a Si/CdTe Compton camera, consisting of six layered double-sided silicon strip detectors and three CdTe pixel detectors. By using this prototype, we have demonstrated the concept of the Si/CdTe Compton cameras. We have successfully obtained Compton reconstructed images for 80-662 keV gamma-rays. The achieved angular resolution is about 4 degrees for 511 keV gamma-rays. The energy resolution is 14 keV (FWHM) at 511 keV. In order to improve the performance of the Compton camera, we have evaluated all CdTe pixel detectors we have constructed. We found that the I-V curve is helpful to select good detectors. © 2006 Elsevier B.V. All rights reserved.
English, Scientific journal
DOI：https://doi.org/10.1016/j.nima.2006.05.164
DOI ID：10.1016/j.nima.2006.05.164, ISSN：0168-9002, SCOPUS ID：33749359609 - Developments of a new 1-dimensional γ-ray position sensor using scintillators coupled to a Si strip detector
Takeshi Itoh; Motohide Kokubun; Takeshi Takashima; Tsuneo Honda; Kazuo Makishima; Takaaki Tanaka; Takayuki Yanagida; Shinya Hirakuri; Ryohei Miyawaki; Hiromitsu Takahashi; Kazuhiro Nakazawa; Tadayuki Takahashi
IEEE Transactions on Nuclear Science, Volume：53, Number：5, First page：2983, Last page：2990, Oct. 2006, [Reviewed]
In order to operate an "improved" Fourier synthesis imager at higher photon energies than are accessible with solidstate detectors, we developed a new one-dimensional γ-ray position sensor consisting of inorganic scintillators whose light is read out by a silicon strip detector (SSD). The SSD is read out through stripped p-electrodes (DC-coupled, 32 channels at 400 μm pitch). The n-side of the SSD does not have a metallic surface, and has a relatively good optical transparancy. A stack of optically isolated thin CsI(Tl) scintillator plates (10 mm × 10 mm in area and 0.3 mm thick) is attached, edge-on, to the n-side of the SSD. When a γ-ray photon hits the stacked scintillator, the generated scintillation light is detected by the SSD, with the signal pulse-height largest in the p-electrode which is just beneath the CsI plate hit by the γ-ray. The 32-channel outputs from the SSD are acquired simultaneously for each event with a low-noise analog ASIC. The γ-ray position can be calculated as a weighted mean of pulse heights. Using this system, we have obtained a position resolution significantly finer than 1 mm for γ-rays with energies greater than ∼500 keV up to ∼ 1300 keV. © 2006 IEEE.
English, Scientific journal
DOI：https://doi.org/10.1109/TNS.2006.879760
DOI ID：10.1109/TNS.2006.879760, ISSN：0018-9499, SCOPUS ID：33750416039 - Suzaku observations of the hard X-ray variability of MCG-6-30-15: the effects of strong gravity around a Kerr black hole
Giovanni Miniutti; Andrew C. Fabian; Naohisa Anabuki; Jamie Crummy; Yasushi Fukazawa; Luigi Gallo; Yoshito Haba; Kiyoshi Hayashida; Steve Holt; Hideyo Kunieda; Josefin Larsson; Alex Markowitz; Chiho Matsumoto; Masanori Ohno; James N. Reeves; Tadayuki Takahashi; Yasuo Tanaka; Yuichi Terashima; Ken'ichi Torii; Yoshihiro Ueda; Masayoshi Ushio; Shin Watanabe; Makoto Yamauchi; Tahir Yaqoob
Publications of the Astronomical Society of Japan, Volume：59, Number：1 SPEC. ISS., Sep. 2006
Suzaku has, for the first time, enabled the hard X-ray variability of the
Seyfert 1 galaxy MCG-6-30-15 to be measured. The variability in the 14-45 keV
band, which is dominated by a strong reflection hump, is quenched relative to
that at a few keV. This directly demonstrates that the whole reflection
spectrum is much less variable than the power-law continuum. The broadband
spectral variability can be decomposed into two components - a highly variable
power-law and constant reflection - as previously inferred from other
observations in the 2-10 keV band. The strong reflection and high iron
abundance give rise to a strong broad iron line, which requires the inner disc
radius to be at about 2 gravitational radii. Our results are consistent with
the predictions of the light bending model which invokes the very strong
gravitational effects expected very close to a rapidly spinning black hole.
DOI：https://doi.org/10.1093/pasj/59.sp1.S315
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=34047095269&origin=inward
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DOI ID：10.1093/pasj/59.sp1.S315, ISSN：0004-6264, arXiv ID：astro-ph/0609521, SCOPUS ID：34047095269 - Framework for a Geant4-based simulator of the radiation background and detector-responses of the space X-ray observatory Suzaku (Astro-E2)
Masanobu Ozaki; Shin Watanabe; Yukikatsu Terada; Takeshi Jim; Masaki Kitsunezuka; Tetsuichi Kishishita; Yoshitaka Ishisakil; Tadayuki Takahashi
IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：53, Number：3, First page：1310, Last page：1316, Jun. 2006, [Reviewed]
We have constructed a Monte Carlo simulation base for the radiation environment of the Suzaku X-ray observatory satellite. The system consists of an object-oriented analysis framework used for real-data analysis, the Geant4 toolkit, an interface that allows the users a transparent usage of Geant4 components through the framework and classes that are used to build the simulation by a collaboration among different geometry maintainer and detector developer groups. As a demonstration, the geometry of the Hard X-ray Detector, which is one of the Suzaku detectors, is constructed using the framework and a comparison between the simulation output with the actual data is shown.
IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English, Scientific journal
DOI：https://doi.org/10.1109/TNS.2006.875197
DOI ID：10.1109/TNS.2006.875197, ISSN：0018-9499, eISSN：1558-1578, Web of Science ID：WOS:000238582300008 - In Orbit Timing Calibration of the Suzaku Hard X-ray Detector
Yukikatsu Terada; Teruaki Enoto; Ryouhei Miyawaki; Yasushi Fukazawa; Madoka Kawaharada; Tsuneyoshi Kamae; Motohide Kokubun; Kazuo Makishima; Tsunefumi Mizuno; Toshio Murakami; Kazuhiro Nakazawa; Masaharu Nomach; Tadayuki Takahashi; Hiromitsu Takahashi; Makoto S. Tashiro; Toru Tamagawa; Shin Watanabe; Kazutaka Yamaoka; Daisuke Yonetoku
2006 IEEE NUCLEAR SCIENCE SYMPOSIUM CONFERENCE RECORD, VOL 1-6, First page：783, Last page：787, 2006, [Reviewed]
Suzaku is the fifth Japanese astrophysical satellite, devoted to study high energy phenomena in the X-ray band of 0.5 - 600 keV. It was successfully launched from Uchinoura Space Center in Japan on 10th July 2005. The HXD on board Suzaku covers 10 - 600 keV band with a high sensitivity of about 10(-5) cnt/s/cm(2)/keV level. The sensor consists of 16 identical GSO/BGO well-type-phoswich counters incorporating 2 mm-thick silicon PIN diodes, and 20 surrounding-BGO-shield counters to remove residual non X-ray backgrounds through anti-coincidence rejection. The present paper is particularly focused on timing system of the HXD and in-orbit verifications with pulsars.
IEEE, English, International conference proceedings
DOI：https://doi.org/10.1109/NSSMIC.2006.355968
DOI ID：10.1109/NSSMIC.2006.355968, ISSN：1082-3654, Web of Science ID：WOS:000288875600156 - Soft-gamma-ray observations of GRB prompt emission with Suzaku Wideband All-Sky Monitor
Yukikatsu Terada
Nuovo Cimento Della Societa Italiana di Fisica B-basic Topics in Physics, Volume：121, Number：10-11, First page：1127, Last page：1131, 2006, [Reviewed]
Scientific journal
DOI：https://doi.org/10.1393/NCB/I2007-10233-X
DOI ID：10.1393/NCB/I2007-10233-X, ORCID：67259992, SCOPUS ID：34548294278, Web of Science ID：WOS:000250824300015 - Cyclotron resonance energies at a low X-ray luminosity:: A0535+262 observed with Suzaku
Yukikatsu Terada
The Astrophysical Journal, Volume：648, Number：2 II, 2006, [Reviewed]
Scientific journal
DOI：https://doi.org/10.1086/508018
DOI ID：10.1086/508018, ORCID：67259922, SCOPUS ID：33750559838, Web of Science ID：WOS:000240403800014 - Suzaku Wide-Band All-Sky Monitor observations of GRB prompt emissions
Kazutaka Yamaoka; Satoshi Sugita; Masanori Ohno; Takuya Takahashi; Yasushi Fukazawa; Yukikatsu Terada; Yasuhiko Endo; Soojing Hong; Keiichi Abe; Kaori Onda; Makoto Tashiro; Teruaki Enoto; Ryohei Miyawaki; Motohide Kokubun; Kazuo Makishima; Goro Sato; Kazuhiro Nakazawa; Tadayuki Takahashi
GAMMA-RAY BURSTS IN THE SWIFT ERA, Volume：836, First page：201, Last page：+, 2006, [Reviewed]
The Suzaku Wide-band All-sky Monitor (WAM), realized by large thick anti-coincidence shields of the Hard X-ray Detector (HXD), can be powerful gamma-ray burst (GRB) detector which is sensitive to 50-5000 keV gamma-rays. The WAM is now in a full operational phase, and we have already detected some GRBs simultaneously with other satellites (Swift, Konus-Wind, HETE2 and INTEGRAL SPI/ACS). The most impressive event among detected GRBs is GRB051008, which was detected up to 2 MeV with the WAM. In this paper, we report on the WAM in-flight performance as a GRB monitor from initial three-months operations, focusing on the GRB trigger status and spectral analysis of GRB051008 and GRB051111 combined with Swift.
AMER INST PHYSICS, English, International conference proceedings
ISSN：0094-243X, Web of Science ID：WOS:000238125000040 - In-orbit performance of the Suzaku wide-band all-sky monitor - art. no. 626643
Kazutaka Yamaoka; Satoshi Sugita; Masanori Ohno; Takuya Takahashi; Yasushi Fukazawa; Yukikatsu Terada; Tohru Tamagawa; Keiichi Abe; Yasuhiko Endo; Kaori Onda; Satoshi Matsumura; Makoto Tashiro; Hong Soojing; Goro Sato; Kazuhiro Nakazawa; Tadayuki Takahashi; Ryohei Miyawaki; Teruaki Enoto; Motohide Kokubun; Kazuo Makishima; Toshio Murakami
Space Telescopes and Instrumentation II: Ultraviolet to Gamma Ray, Pts 1 and 2, Volume：6266, First page：26643, Last page：26643, 2006, [Reviewed]
The X-ray astronomical satellite Suzaku was successfully launched in July 2005. The onboard Wideband All-sky Monitor (WAM) is designed as the second function of the large, thick BGO anti-coincidence shields of the Hard X-ray Detectors (HXD). It views about half of the whole sky and has a geometrical area of 800 cm(2) per side, with a large effective area of 400 cm(2) even at 1 MeV. Hence, the WAM is expected to provide unique opportunities to detect high energy emission from GRBs and solar flares in the MeV range. In fact, the WAM has detected at least 47 GRBs, although the fine-tuning of the GRB functions is still in progress. The most impressive GRB result is the bright, hard spectrum GRB 051008, which was detected up to 1 MeV with the WAM. We will present here the in-flight performance of the HXD/WAM during the initial eight-months of operations. The in-flight energy response, spectral and timing capabilities, and in-orbit background are described in this paper.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.671994
DOI ID：10.1117/12.671994, ISSN：0277-786X, eISSN：1996-756X, Web of Science ID：WOS:000240015400124 - Hard X-ray Imager for the NeXT Mission
Kazuhiro Nakazawa; Yasushi Fukazawa; Tuneyoshi Kamae; Jun Kataoka; Motohide Kokubun; Kazuo Makishima; Tsunefumi Mizuno; Toshio Murakami; Masaharu Nomachi; Hiroyasu Tajima; Tadayuki Takahashi; Makoto Tashiro; Toru Tamagawa; Yukikatsu Terada; Shin Watanabe; Kazutaka Yamaoka; Daisuke Yonetoku
SPACE TELESCOPES AND INSTRUMENTATION II: ULTRAVIOLET TO GAMMA RAY, PTS 1 AND 2, Volume：6266, 2006, [Reviewed]
The hard X-ray imager (HXI) is the primary detector of the NeXT mission, proposed to explore high-energy non-thermal phenomena in the universe. Combined with a novel hard X-ray mirror optics, the HXI is designed to provide better than arc-minutes imaging capability with 1 keV level spectroscopy, and more than 30 times higher sensitivity compared with any existing hard X-ray instruments. The base-line design of the HXI is improving to secure high sensitivity. The key is to reduce the detector background as far as possible. Based on the experience of the Suzaku satellite launched in July 2005, the current design has a well-type tight active shield and multi layered, multi material imaging detector made of Si and CdTe. Technology has been under development for a few years so that we have reached the level where a basic detector performance is satisfied. Design tuning to further improve the sensitivity and reliability is on-going.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
DOI：https://doi.org/10.1117/12.670674
DOI ID：10.1117/12.670674, ISSN：0277-786X, Web of Science ID：WOS:000240015400075 - Design and performance of the soft gamma-ray detector for the NeXT mission
H. Tajima; T. Kamae; G. Madejski; T. Mitani; K. Nakazawa; T. Tanaka; T. Takahashi; S. Watanabe; Y. Fukazawa; T. Ikagawa; J. Kataoka; M. Kokubun; K. Makishima; Y. Terada; M. Nomachi; M. Tashiro
IEEE Transactions on Nuclear Science, Volume：52, First page：2749, Last page：2757, Dec. 2005
The soft gamma-ray detector (SGD) onboard the Japanese future high energy astrophysics mission (NeXT) is a Compton telescope with narrow field of view, which utilizes Compton kinematics to enhance its background rejection capabilities. It is realized as a hybrid semiconductor gamma-ray detector which consists of silicon and cadmium telluride (CdTe) detectors. It can detect photons in a wide energy band (0.05-1 MeV) at a background level of 5 × 10-7 counts/s/cm2/keV; the silicon layers are required to improve the performance at a lower energy band (<0.3 MeV). Excellent energy resolution is the key feature of the SGD, allowing it to achieve both high angular resolution and good background rejection capability. An additional capability of the SGD, its ability to measure gamma-ray polarization, opens up a new window to study properties of astronomical objects. We will present the development of key technologies to realize the SGD: high quality CdTe, low noise front-end application-specific integrated circuit, and bump bonding technology. Energy resolutions of 1.7 keV (full-width at half-maximum) for CdTe pixel detectors and 1.1 keV for Si strip detectors have been measured. We also present the validation of Monte Carlo simulation used to evaluate the performance of the SGD. © 2005 IEEE.
DOI：https://doi.org/10.1109/TNS.2005.862776
DOI ID：10.1109/TNS.2005.862776, ISSN：0018-9499, CiNii Articles ID：10017263925, SCOPUS ID：33144458024 - Development of the HXD-II wide-band all-sky monitor onboard Astro-E2
Yukikatsu Terada
IEEE Transactions on Nuclear Science, Volume：52, First page：2765, Last page：2772, Dec. 2005
The hard X-ray detector (HXD-II) is one of the three scientific instruments onboard Japanese X-ray astronomy satellite Astro-E2 scheduled to be launched in 2005. This mission is very unique in a point of having a lower background than any other past missions in the 10-600 keV range. In the HXD-II, the large and thick BGO crystals are used as active shields for particle and gamma-ray background to the main detector. They have a wide field of view of ∼2π and a large effective area of 400 cm2 even at 1 MeV. Hence, the BGO shields have been developed as a wide-band all-sky monitor (WAM) with a broadband coverage of 50-5000 keV. In this paper, overall design and performance of the HXD-II/WAM based on the results of preflight calibration tests carried out in June 2004 are described. By irradiating various radio isotopes with the WAM flight model, we verified that it had comparable capabilities with other gamma-ray burst detectors. © 2005 IEEE.
Scientific journal
DOI：https://doi.org/10.1109/TNS.2005.862778
DOI ID：10.1109/TNS.2005.862778, ISSN：0018-9499, ORCID：67259926, SCOPUS ID：33144482172, Web of Science ID：WOS:000235371900008 - A Si/CdTe semiconductor Compton camera
Shin Watanabe; Takaaki Tanaka; Kazuhiro Nakazawa; Takefumi Mitani; Kousuke Oonuki; Tadayuki Takahashi; Takeshi Takashima; Hiroyasu Tajima; Yasushi Fukazawa; Masaharu Nomachi; Shin Kubo; Mitsunobu Onishi; Yoshikatsu Kuroda
IEEE Transactions on Nuclear Science, Volume：52, Number：5, First page：2045, Last page：2051, Oct. 2005, [Reviewed]
We are developing a Compton camera based on Si and CdTe semiconductor imaging devices with high energy resolution. In this paper, results from the most recent prototype are reported. The Compton camera consists of six layered double-sided Si Strip detectors and CdTe pixel detectors, which are read out with low noise analog ASICs, VA32TAs. We obtained Compton reconstructed images and spectra of line gamma-rays from 122 keV to 662 keV. The energy resolution is 9.1 keV and 14 keV at 356 keV and 511 keV, respectively. © 2005 IEEE.
English, Scientific journal
DOI：https://doi.org/10.1109/TNS.2005.856995
DOI ID：10.1109/TNS.2005.856995, ISSN：0018-9499, SCOPUS ID：29144439813 - High resolution Fourier synthesis hard X-ray imaging based on CdTe strip detectors
Yukikatsu Terada
IEEE Transactions on Nuclear Science, Volume：52, First page：2052, Last page：2057, Oct. 2005
Employing Fourier-synthesis optics and one-dimensional position-sensitive detectors, we are developing a novel hard X-ray imager which can work in the ∼ 10 keV to ∼ 200 keV range either as a telescope or a microscope. As the detection part of our imager, we have developed a strip detector made of Schottky CdTe diode, with its cathode divided into 64 channels of 150 urn pitch. Electrodes of all channels are gold-stud bonded to a fanout board, and connected to low noise analog ASIC. We read out signals from all channels simultaneously. As the grid optics elements, one-dimensional "modulation collimator" grids of 1 mm thick tungsten have been manufactured, with 10 grid pitches ranging from 0.2 mm to 2 mm with harmonic ratios. Combining the CdTe strip detector and the grids, we have verified hard X-ray imaging performance of this system. Using an241Am source, we have successfully obtained an image in the 10-70 keV range with a spatial resolution of ∼ 0.5 mm. © 2005 IEEE.
Scientific journal
DOI：https://doi.org/10.1109/TNS.2005.856885
DOI ID：10.1109/TNS.2005.856885, ISSN：0018-9499, ORCID：67259923, SCOPUS ID：29144494846, Web of Science ID：WOS:000233781700085 - Hard X-ray response of CdZnTe detectors in the Swift burst alert telescope
Masaya Suzuki; Makoto Tashiro; Goro Sato; Shin Watanabe; Kazuhiro Nakazawa; Tadayuki Takahashi; Yuu Okada; Hiromitsu Takahashi; Ann Parsons; Scott Barthelmy; Jay Cummings; Neil Gehrels; Derek Hullinger; Hans Krimm; Jack Tueller
IEEE Transactions on Nuclear Science, Volume：52, Number：4, First page：1033, Last page：1035, Aug. 2005, [Reviewed]
The Burst Alert Telescope (BAT) onboard the Swift gamma-ray burst explorer has a coded aperture mask and a detector array of 32 K CdZnTe semiconductor devices. Due to the small mobility and short lifetime of carriers, the electron-hole pairs generated by gamma-ray irradiation cannot be fully collected. Hence the shape of the measured spectra has a broad low-energy tail. We have developed a method to model the spectral response by taking into account the charge transport properties which depend on the depth of the photon interaction [1]. The mobility-lifetime products for detectors derived from our method vary by more than one order of magnitude among detectors. In this paper, we focus on the nonuniformity of the mobility at the millimeter scale by employing a scanning experiment for a single detector. We reveal almost an order of magnitude variance in the mobility-lifetime product of holes within a single detector, while those of electrons remains fairly uniform. © 2005 IEEE.
English, Scientific journal
DOI：https://doi.org/10.1109/TNS.2005.852968
DOI ID：10.1109/TNS.2005.852968, ISSN：0018-9499, SCOPUS ID：27644555260 - Development of a Monte Carlo simulator for the Astro-E2 Hard X-ray Detector (HXD-II)
Yukikatsu Terada
IEEE Transactions on Nuclear Science, Volume：52, Number：4, First page：902, Last page：909, Aug. 2005, [Reviewed]
The Hard X-ray Detector (HXD-II) is one of the scientific payloads on board the fifth Japanese cosmic X-ray satellite Astro-E2, scheduled for launch in 2005. The HXD-II is designed to cover a wide energy range of 10-600 keV with a high sensitivity of about 10(-5) cnt/s/cm(2) /keV. In order to derive the energy response of the sensor and to estimate the background, a Monte Carlo simulator based on the Geant4 toolkit is currently being developed. This paper describes the design concept of the HXD-II software package, including the analysis tools and the Monte Carlo simulator, and its verification through a comparison with actual data taken by pre-flight radio-isotope irradiation experiments, together with calculated outputs that can demonstrate the in-orbit performance of the HXD-II.
IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, Scientific journal
DOI：https://doi.org/10.1109/TNS.2005.852681
DOI ID：10.1109/TNS.2005.852681, ISSN：0018-9499, ORCID：67259915, Web of Science ID：WOS:000231436700014 - Development of a spectral model based on charge transport for the Swift/BAT 32K CdZnTe detector array
Goro Sato; Ann Parsons; Derek Hullinger; Masaya Suzuki; Tadayuki Takahashi; Makoto Tashiro; Kazuhiro Nakazawa; Yuu Okada; Hiromitsu Takahashi; Shin Watanabe; Scott Barthelmy; Jay Cummings; Neil Gehrels; Hans Krimm; Craig Markwardt; Jack Tueller; Ed Fenimore; David Palmer
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：541, Number：1-2, First page：372, Last page：384, Apr. 2005, [Reviewed]
The properties of 32K CdZnTe (4×4mm2 large, 2 mm thick) detectors have been studied in the pre-flight calibration of the Burst Alert Telescope (BAT) on-board the Swift Gamma-ray Burst Explorer (scheduled for launch in November 2004). In order to understand the energy response of the BAT CdZnTe array, we first quantify the mobility-lifetime (μτ) products of carriers in individual CdZnTe detectors, which produce a position dependency in the charge induction efficiency and results in a low-energy tail in the energy spectrum. Based on a new method utilizing 57Co spectra obtained at different bias voltages, the μτ for electrons ranges from 5.0×10-4 to 1.0×10-2cm2V-1 while the μτ for holes ranges from 1.3×10-5 to 1.8×10-4cm2V-1. We find that this wide distribution of μτ products explains the large diversity in spectral shapes between CdZnTe detectors well. We also find that the variation of μτ products can be attributed to the difference of crystal ingots or manufacturing harness. We utilize the 32K sets of extracted μτ products to develop a spectral model of the detector. In combination with Monte Carlo simulations, we can construct a spectral model for any photon energy or any incident angle. © 2005 Elsevier B.V. All rights reserved.
English, International conference proceedings
DOI：https://doi.org/10.1016/j.nima.2005.01.078
DOI ID：10.1016/j.nima.2005.01.078, ISSN：0168-9002, SCOPUS ID：20144378089 - Application of CdTe for the NeXT mission
Yukikatsu Terada
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, Volume：541, First page：332, Last page：341, Apr. 2005
Cadmium telluride (CdTe) and cadmium zinc telluride (CdZnTe) have been regarded as promising semiconductor materials for hard X-ray and γ-ray detection. The high-atomic number of the materials (ZCd=48,ZTe=52) gives a high quantum efficiency in comparison with Si. The large band-gap energy (Eg=1.5eV) allows to operate the detector at room temperature. Based on recent achievements in high-resolution CdTe detectors, in the technology of ASICs and in bump-bonding, we have proposed the novel hard X-ray and γ-ray detectors for the NeXT mission in Japan. The high-energy response of the super mirror onboard NeXT will enable us to perform the first sensitive imaging observations up to 80 keV. The focal plane detector, which combines a fully depleted X-ray CCD and a pixellated CdTe detector, will provide spectra and images in the wide energy range from 0.5 to 80 keV. In the soft γ-ray band up to ∼1MeV, a narrow field-of-view Compton γ-ray telescope utilizing several tens of layers of thin Si or CdTe detector will provide precise spectra with much higher sensitivity than present instruments. The continuum sensitivity will reach several ×10-8photons-1keV-1cm-2 in the hard X-ray region and a few ×10-7photons-1keV-1cm-2 in the soft γ-ray region. © 2005 Elsevier B.V. All rights reserved.
Scientific journal
DOI：https://doi.org/10.1016/j.nima.2005.01.073
DOI ID：10.1016/j.nima.2005.01.073, ISSN：0168-9002, ORCID：5294779, SCOPUS ID：20144366718 - The search for optical emission on and before the GRB trigger with the WIDGET telescope
T. Tamagawa; F. Usui; Y. Urata; K. Abe; K. Onda; M. Tashiro; Y. Terada; H. Fujiwara; N. Miura; S. Hirose; N. Kawai; A. Yoshida; M. Mori; K. Makishima
Nuovo Cimento della Societa Italiana di Fisica C, Volume：28, Number：4-5, First page：771, Last page：774, 2005
WIDGET is a robotic telescope for monitoring the HETE-2 field-of-view to detect Gamma-Ray Burst optical flashes or possible optical precursors. The system has 62° × 62° wide field-of-view which covers about 80% of HETE-2 one with a 2k×2k Apogee U10 CCD camera and a Canon EF 24 mm f/1.4 wide-angle lens without a bandpass filter. WIDGET has been in operation since June 2004 at Akeno observing site where is about 200 km apart from Tokyo. Typical limiting magnitude with S/N = 3 at the site is V = 10mag for 5 seconds exposure and V = 11mag for 30 seconds exposure. We had already six coincident observations with HETE-2 position alerts. It was, however, cloudy for all cases due to rainy season in Japan. The expected number of coincident observations under clear sky is about 5 events per year. We will extend the system in early 2005 for Swift era to monitor optical transients in wider field-of-view, multi-color or polarization modes. © Società Italiana di Fisica.
Editrice Compositori s.r.l., English, Scientific journal
ISSN：1826-9885, SCOPUS ID：29344451956 - R&D of a new 1-dimensional γ-ray position sensor using scintillators coupled to a Si strip detector
Takeshi Itoh; Motohide Kokubun; Takeshi Takashima; Takayuki Yanagida; Shinya Hirakuri; Ryohei Miyawaki; Hiromitsu Takahashi; Kazuo Makishima; Takaaki Tanaka; Kazuhiro Nakazawa; Tadayuki Takahashi; Tsuneo Honda
IEEE Nuclear Science Symposium Conference Record, Volume：1, First page：186, Last page：190, 2005, [Reviewed]
As the detection part of an improved Fourier Synthesis imager, we developed a new one-dimensional γ-ray position sensor consisting of inorganic scintillators whose lights are read out by a silicon strip detector (SSD). The employed SSD has no metal anode, with its Al-cathode divided into 32 channels of 400 μm pitch. Electrodes of all channels are Albonded to a low noise analog ASIC, so that signals can be read out from all channels simultaneously. We fabricated a "stacked CsI scintillator", consisting of 20 CsI(Tl) scintillator plates each having a dimension of 10 mm × 10 mm × 0.3 mm, and 0.07 mm-thick light reflective sheets inserted between adjacent CsI plates. Coupling the scintillator and the SSD, γ-ray with energies ≳ 500 keV were successfully detected, with a position resolution of ∼0.37 mm. © 2005 IEEE.
English, International conference proceedings
DOI：https://doi.org/10.1109/NSSMIC.2005.1596233
DOI ID：10.1109/NSSMIC.2005.1596233, ISSN：1095-7863, SCOPUS ID：33846598372 - Preflight calibration and performance of the Astro-E2/HXD-II wide-band all-sky monitor
Yukikatsu Terada
IEEE Transactions on Nuclear Science, Volume：52, Number：6, First page：2758, Last page：2764, 2005, [Reviewed]
Scientific journal
DOI：https://doi.org/10.1109/TNS.2005.860172
DOI ID：10.1109/TNS.2005.860172, ORCID：67259921, SCOPUS ID：33144456539, Web of Science ID：WOS:000235371900007 - Performance of GRB monitor with Astro-E2 Hard X-ray Detector (HXD-II)
Yukikatsu Terada
Nuovo Cimento Della Societa Italiana di Fisica C, Volume：28, Number：4-5, First page：821, Last page：824, 2005, [Reviewed]
Scientific journal
DOI：https://doi.org/10.1393/NCC/I2005-10164-7
DOI ID：10.1393/NCC/I2005-10164-7, ORCID：67259989, SCOPUS ID：29344457423, Web of Science ID：WOS:000234266300074 - A prototype Si/CdTe compton camera and the polarization measurement
Takefumi Mitani; Takaaki Tanaka; Kazuhiro Nakazawa; Tadayuki Takahashi; Takeshi Takashima; Hiroyasu Tajima; Hidehito Nakamura; Masaharu Nomachi; Tatsuya Nakamoto; Yasushi Fukazawa
IEEE Transactions on Nuclear Science, Volume：51, Number：5 I, First page：2432, Last page：2436, Oct. 2004, [Reviewed]
Compton camera is the most promising approach for gamma-ray detection in the energy region from several hundred kiloelectronvolts to megaelectronvolts, especially for application in high energy astrophysics. In order to obtain good angular resolution, semiconductor detectors such as silicon, germanium and cadmium telluride(CdTe) have several advantages over scintillation detectors, which have been used so far. Based on the recent advances of high resolution CdTe and silicon imaging detectors, we are working on a Si/CdTe Compton camera. We have developed 64-pixel CdTe detectors with a pixel size of 2 mm × 2 mm and double-sided Si strip detectors(DSSDs) with a position resolution of 800 μm. As a prototype Si/CdTe Compton camera, we use a DSSD as a scatterer and two CdTe pixel detectors as an absorber. In order to verify its performance, we irradiate the camera with 100% linearly polarized 170 keV γ-rays and demonstrate the system works properly as a Compton camera. The resolution of the reconstructed scattering angle is 22° (full-width at half-maximum). Measurement of polarization is also reported. The polarimetric modulation factor is obtained to be 43%, which is consistent with the prediction of Monte Carlo simulations.
English, Scientific journal
DOI：https://doi.org/10.1109/TNS.2004.835653
DOI ID：10.1109/TNS.2004.835653, ISSN：0018-9499, SCOPUS ID：8344280452 - Improvement of the CdTe diode detectors using a guard-ring electrode
Kazuhiro Nakazawa; Kousuke Oonuki; Takaaki Tanaka; Yoshihito Kobayashi; Ken'ichi Tamura; Takefumi Mitani; Goro Sato; Shin Watanabe; Tadayuki Takahashi; Ryoichi Ohno; Akihito Kitajima; Yoshikatsu Kuroda; Mitsunobu Onishi
IEEE Transactions on Nuclear Science, Volume：51, Number：4 I, First page：1881, Last page：1885, Aug. 2004, [Reviewed]
Recent results from the Schottky CdTe diode detectors employing a guard-ring (GR) electrode are reported. A cathode electrode, made of platinum, was separated into an active electrode(s) and a surrounding GR. Typical leakage current of a device with active area of 2 × 2 mm2 and 0.5 mm thickness surrounded by a GR, is 7 and 20 pA at a bias of 100 and 500 V, respectively, operated at 20°C. Spectral resolution of this device is 0.93 and 1.2 keV (FWHM) at 59.5 and 122 keV, respectively, operated at 20°C with a bias of 800 V. Detailed study of the characteristics of these devices working as a gamma-ray detector is presented.
English, International conference proceedings
DOI：https://doi.org/10.1109/TNS.2004.832684
DOI ID：10.1109/TNS.2004.832684, ISSN：0018-9499, SCOPUS ID：4444338347 - Performance of a low noise front-end ASIC for Si/CdTe detectors in compton gamma-ray telescope
Hiroyasu Tajima; Tatsuya Nakamoto; Takaaki Tanaka; Shingo Uno; Takefumi Mitani; Eduardo Do Couto e Silva; Yasushi Fukazawa; Tuneyoshi Kamae; Grzegorz Madejski; Daniel Marlow; Kazuhiro Nakazawa; Masaharu Nomachi; Yu Okada; Tadayuki Takahashi
IEEE Transactions on Nuclear Science, Volume：51, Number：3, First page：842, Last page：847, Jun. 2004, [Reviewed]
Compton telescopes based on semiconductor technologies are being developed to explore the gamma-ray universe in an energy band 0.1-20 MeV, which is not well covered by the present or near-future gamma-ray telescopes. The key feature of such Compton telescopes is the high energy resolution that is crucial for high angular resolution and high background rejection capability. The energy resolution around 1 keV is required to approach physical limit of the angular resolution due to Doppler broadening. We have developed a low noise front-end ASIC (application-specific integrated circuit), VA32TA, to realize this goal for the readout of double-sided silicon strip detector (DSSD) and cadmium telluride (CdTe) pixel detector which are essential elements of the semiconductor Compton telescope. We report on the design and test results of the VA32TA. We have reached an energy resolution of 1.3 keV [full-width at half-maximum (FWHM)] for 60 and 122 keV at 0°C with a DSSD and 1.7 keV (FWHM) with a CdTe detector.
English, International conference proceedings
DOI：https://doi.org/10.1109/TNS.2004.829394
DOI ID：10.1109/TNS.2004.829394, ISSN：0018-9499, SCOPUS ID：3342890652 - Evolution of the synchrotron spectrum in Markarian 421 during the 1998 campaign
Chiharu Tanihata; Jun Kataoka; Tadayuki Takahashi; Greg M. Madejski
Astrophysical Journal, Volume：601, Number：2 I, First page：759, Last page：770, Feb. 2004, [Reviewed]
The uninterrupted 7 day ASCA observations of the TeV blazar Mrk 421 in 1998 have clearly revealed that X-ray flares occur repeatedly. In this paper, we present the results of the time-resolved spectral analysis of the combined data taken by ASCA, RXTE, BeppoSAX, and the Extreme Ultraviolet Explorer (EUVE). In this object - and in many other TeV blazars - the precise measurement of the shape of the X-ray spectrum, which reflects the high-energy portion of the synchrotron component, is crucial in determining the high-energy cutoff of the accelerated electrons in the jet. Thanks to the simultaneous broadband coverage, we measured the 0.1-25 keV spectrum resolved on timescales as short as several hours, providing a great opportunity to investigate the detailed spectral evolution at the flares. By analyzing the time-subdivided observations, we parameterize the evolution of the synchrotron peak, where the radiation power dominates, by fitting the combined spectra with a quadratic form [where the νFν flux at the energy E obeys logνFnu
(E) = log (νFν,peak) - const (log E-log Epeak)2]. In this case, we show that there is an overall trend that the peak energy E peak and peak flux νFν,peak increase or decrease together. The relation of the two parameters is best described as E peak ∝ νFν,peak0.7 for the 1998 campaign. Similar results were derived for the 1997 observations, while the relation gave a smaller index when both 1997 and 1998 data were included. On the other hand, we show that this relation, and also the detailed spectral variations, differs from flare to flare within the 1998 campaign. We suggest that the observed features are consistent with the idea that flares are due to the appearance of a new spectral component. With the availability of the simultaneous TeV data, we also show that there exists a clear correlation between the synchrotron peak flux and the TeV flux.
Institute of Physics Publishing, English, Scientific journal
DOI：https://doi.org/10.1086/380779
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=1842480987&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=1842480987&origin=inward
DOI ID：10.1086/380779, ISSN：1538-4357, eISSN：1538-4357, SCOPUS ID：1842480987 - Recent achievements of the high resolution Schottky CdTe diode for gamma-ray detectors
T Tanaka; Y Kobayashi; T Mitani; K Nakazawa; K Oonuki; G Sato; T Takahashi; S Watanabe
NEW ASTRONOMY REVIEWS, Volume：48, Number：1-4, First page：309, Last page：313, Feb. 2004
We describe the recent progress on the use of Schottky Cadmium telluride (CdTe) diode detectors for gamma-ray spectroscopy. The extremely low leakage current of the newly developed CdTe diode allows us to apply a much higher bias voltage in comparison with the previous CdTe detectors. Both the improved charge-collection efficiency and the low leakage current lead to a good energy resolution even at room temperature. Large-area CdTe diode detectors with dimensions of 21.5 x 21.5 mm(2) are now available. By stacking 40 layers of these large-area devices, we have achieved a good energy resolution of several keV (FWHM) for MeV gamma-rays. (C) 2003 Elsevier B.V. All rights reserved.
ELSEVIER SCI LTD, English, Scientific journal
DOI：https://doi.org/10.1016/j.newar.2003.11.036
DOI ID：10.1016/j.newar.2003.11.036, ISSN：1387-6473, SCOPUS ID：0742267935, Web of Science ID：WOS:000189181600055 - Hard X-ray and γ-ray detectors for the NeXT mission
Yukikatsu Terada
New Astronomy Reviews, Volume：48, Number：1-4, First page：269, Last page：273, Feb. 2004, [Reviewed]
Scientific journal
DOI：https://doi.org/10.1016/j.newar.2003.11.047
DOI ID：10.1016/j.newar.2003.11.047, ORCID：5294785, SCOPUS ID：0742302536 - A search for cyclotron resonance features with integral
Y Okada; H Niko; M Kokubun; K Makishima; M Nakajima; T Mihara; T Terada; Y Terada; F Nagase; Y Tanaka
PROCEEDINGS OF THE 5TH INTEGRAL WORKSHOP ON THE INTEGRAL UNIVERSE, Volume：552, Number：552, First page：467, Last page：470, 2004, [Reviewed]
We present an INTEGRAL observation of the Cen-Crux region in order to search the electron cyclotron resonance scattering features from the X-ray binary pulsars. During the AO1 200 ks observation, we clearly detected 4 bright X-ray binaries, 1 Seyfert Galaxy, and 4 new sources in the Field of view. Especially from GX301-2, the cyclotron resonance feature is detected at about similar to 37 keV, and width of 3-4 keV. In addition, the depth of the resonance feature strongly depends on the X-ray luminoscity. This is the first detection of luminosity dependence of the resonance depth. The well-known twin pulsars are spatially separated by JEM-X and IBIS/ISGRI, and pulse periods are measured individually; 296.90 sec for 1E1145-6141 and 292.5 sec for 4U1145-619. The cyclotron resonance feature is marginally detected from 1E1145.1-6141. Cen X-3 was very dim during, the observation and poor statistics disable its to detect the resonance features.
EUROPEAN SPACE AGENCY, English, International conference proceedings
ISSN：0379-6566, ORCID：34407078, SCOPUS ID：23844488725, Web of Science ID：WOS:000227471700085 - Radiation physics simulator for space X-ray observatory Astro-E2
Masanobu Ozaki; Shin Watanabe; Yukikatsu Terada; Takeshi Itoh; Masaki Kitsunezuka; Yoshitaka Ishisaki; Tadayuki Takahashi
IEEE Nuclear Science Symposium Conference Record, Volume：4, First page：2174, Last page：2177, 2004
We constructed a Monte-Carlo simulator framework for the radiation environment of Astro-E2, the Japanese 5th X-ray astronomy satellite. We used Geant4 as the simulator engine, and embedded it into the analysis framework derived from what has been used for other Astro-E2 software development. The entire architecture is designed to make the learning cost of the framework programming as low as possible for not only end users but developers, and we implemented some software mechanisms to register Geant4 components such as physics processes and geometry builder into the framework without using the Geant4's run manager explicitly. © 2004 IEEE.
International conference proceedings
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ISSN：1095-7863, SCOPUS ID：23844517159 - Development of a Si/CdTe semiconductor Compton telescope
Takaaki Tanaka; Takefumi Mitani; Shin Watanabe; Kazuhiro Nakazawa; Kousuke Oonuki; Goro Sato; Tadayuki Takahashi; Ken'ichi Tamura; Hiroyasu Tajima; Hidehito Nakamura; Masaharu Nomachi; Tatsuya Nakamoto; Yasushi Fukazawa
Proceedings of SPIE - The International Society for Optical Engineering, Volume：5501, First page：229, Last page：240, 2004, [Reviewed]
We are developing a Compton telescope based on high resolution Si and CdTe imaging devices in order to obtain a high sensitivity astrophysical observation in sub-MeV gamma-ray region. In this paper, recent results from the prototype Si/CdTe semiconductor Compton telescope are reported. The Compton telescope consists of a double-sided Si strip detector (DSSD) and CdTe pixel detectors, combined with low noise analog LSI, VA32TA. With this detector, we obtained Compton reconstructed images and spectra from line gamma-rays ranging from 81 keV up to 356 keV. The energy resolution is 3.8 keV and 7.9 keV at 122 keV and 356 keV, respectively, and the angular resolution is 9.9° and 5.7° at 122 keV and 356 keV, respectively.
English, International conference proceedings
DOI：https://doi.org/10.1117/12.552600
DOI ID：10.1117/12.552600, ISSN：0277-786X, SCOPUS ID：19944391308 - Spectral evolution of an ultraluminous compact X-ray source in NGC 253
Takaaki Tanaka; Masahiko Sugiho; Aya Kubota; Kazuo Makishima; Tadayuki Takahashi
Progress of Theoretical Physics Supplement, Volume：155, First page：427, Last page：428, 2004, [Reviewed]
We report an observational result for a ULX in NGC253. We find that the spectral evolution is well consistent with the standard behavior. That is, the source satisfies the relation Ldisk ∝ Tin 4 as established for black hole binaries. By comparing with black hole binaries, we estimate black hole mass of this ULX as 7M⊙.
Yukawa Institute for Theoretical Physics, English, Scientific journal
DOI：https://doi.org/10.1143/PTPS.155.427
DOI ID：10.1143/PTPS.155.427, ISSN：0375-9687, SCOPUS ID：11044230657 - Swift status
Makoto Tashiro; Tadayuki Takahashi
Progress of Theoretical Physics Supplement, Volume：155, First page：429, Last page：430, 2004, [Reviewed]
The gamma-ray burst (GRB) observatory Swift is now on the final stage of the pre-launch calibration to be launched in 2004. Swift is designed to observe GRBs and their afterglows with the burst alert telescope (BAT) and two multiwavelength telescopes (XRT and UVOT). The BAT, a coded mask hard X-ray telescope equipped with newly designed CdZnTe detectors, covers 1/6 sky to detect and determine the GRB position onboard. With its sensitivity, it is calculated for the BAT to be able to detect more than 200 GRBs during its nominal two year mission life. The spacecraft maneuvers within about a minute to aim XRT and UVOT afterglows with their fine space and spectral resolutions. Swift is one of the ideal observatory to improve our knowledge by its capability of the continuous and multiwavelength observation. This paper also describes possible collaborations with X-ray and gamma-ray observatories including the coming ASTRO-E2.
Yukawa Institute for Theoretical Physics, English, Scientific journal
DOI：https://doi.org/10.1143/PTPS.155.429
DOI ID：10.1143/PTPS.155.429, ISSN：0375-9687, SCOPUS ID：11044228708 - Development of uniform CdTe pixel detectors based on caltech ASIC
Kousuke Oonuki; Hokuto Inoue; Kazuhiro Nakazawa; Takefumi Mitani; Takaaki Tanaka; Tadayuki Takahashi; C.M. Hubert Chen; Walter R. Cook; Fiona A. Harrison
Proceedings of SPIE - The International Society for Optical Engineering, Volume：5501, First page：218, Last page：228, 2004, [Reviewed]
We have developed a large CdTe pixel detector with dimensions of 23.7 × 13.0 mm2 and a pixel size of 448 × 448 μm 2. The detector is based on recent technologies of an uniform CdTe single crystal, a two-dimensional ASIC, and stud bump-bonding to connect pixel electrodes on the CdTe surface to the ASIC. Good spectra are obtained from 1051 pixels out of total 1056 pixels. When we operate the detector at -50°C, the energy resolution is 0.67 keV and 0.99 keV at 14 keV and 60 keV, respectively. Week-long stability of the detector is confirmed at operating temperatures of both -50°C and -20°C. The detector also shows high uniformity: the peak positions for all pixels agree to within 0.82 %, and the average of the energy resolution is 1.04 keV at a temperature of -50°C. When we normalized the peak area by the total counts detected by each pixel, a variation of 2.1 % is obtained.
English, International conference proceedings
DOI：https://doi.org/10.1117/12.552598
DOI ID：10.1117/12.552598, ISSN：0277-786X, SCOPUS ID：10044263921 - Gamma-ray polarimetry with Compton telescope
Hiroyasu Tajima; Grzegorz Madejski; Takefumi Mitani; Takaaki Tanaka; Hidehito Nakamura; Kazuhiro Nakazawa; Tadayuki Takahashi; Yasushi Fukazawa; Tuneyoshi Kamae; Motohide Kokubun; Daniel Marlow; Masaharu Nomachi; Eduardo Do Couto e Silva
Proceedings of SPIE - The International Society for Optical Engineering, Volume：5488, Number：2, First page：561, Last page：571, 2004, [Reviewed]
Compton telescope is a promising technology to achieve very high sensitivity in the soft gamma-ray band (0.1-10 MeV) by utilizing Compton kinematics. Compton kinematics also enables polarization measurement which will open new windows to study gamma-ray production mechanism in the universe. CdTe and Si semiconductor technologies are key technologies to realize the Compton telescope in which their high energy resolution is crucial for high angular resolution and background rejection capability. We have assembled a prototype module using a double-sided silicon strip detector and CdTe pixel detectors. In this paper, we present expected polarization performance of a proposed mission (NeXT/SGD). We also report results from polarization measurements using polarized synchrotron light and validation of EGS4 MC simulation.
English, International conference proceedings
DOI：https://doi.org/10.1117/12.552487
DOI ID：10.1117/12.552487, ISSN：0277-786X, SCOPUS ID：10044223534 - Activation properties of schottky CdTe diodes irradiated by 150 MeV protons
Mio M. Murakami; Yoshihito Kobayashi; Motohide Kokubun; Isao Takahashi; Yuu Okada; Madoka Kawaharada; Kazuhiro Nakazawa; Shin Watanabe; Goro Sato; Manabu Kouda; Takefumi Mitani; Tadayuki Takahashi; Masaya Suzuki; Makoto Tashiro; Satoshi Kawasoe; Masaharu Nomachi; Kazuo Makishima
IEEE Transactions on Nuclear Science, Volume：50, First page：1013, Last page：1019, Aug. 2003
Cadmium Telluride (CdTe), with its high photon absorption efficiency, has been regarded as a promising semiconductor material for the next generation X/γ-ray detectors. In order to apply this device to astrophysics, it is essential to investigate the radiation hardness and background properties induced by cosmic-ray protons in orbit. We irradiated Schottky CdTe diodes and a CdTe block with a beam of mono-energetic (150 MeV) protons. The induced activation in CdTe was measured externally with a germanium detector, and internally with the irradiated CdTe diode itself. We successfully identified most of radioactive isotopes induced mainly via (p, xn) reactions, and confirmed that the activation background level of CdTe diode is sufficiently low in orbit. We compared energy resolution and leakage current before and after the irradiation and also monitored the signals from a calibration source during the irradiation. There have been no significant degradation. CdTe diodes are tolerant enough to radioactivity in low earth orbit.
DOI：https://doi.org/10.1109/TNS.2003.815120
DOI ID：10.1109/TNS.2003.815120, ISSN：0018-9499, SCOPUS ID：0041424939 - Fourier Synthesis Image Reconstruction by Use of One-Dimensional Position-Sensitive Detectors
Yukikatsu Terada
Applied optics, Volume：42, First page：4176, Last page：4185, Jul. 2003, [Reviewed]
20, Scientific journal
DOI：https://doi.org/10.1364/AO.42.004176
DOI ID：10.1364/AO.42.004176, ISSN：0003-6935, ORCID：5294784, PubMed ID：12856730 - Changes in local structure during electrochemical Li insertion into A-site deficient perovskite oxides, La1/3NbO3
Yukikatsu Terada
The Journal of Physical Chemistry B, 2003
Scientific journal
DOI：https://doi.org/10.1021/JP034262+
DOI ID：10.1021/JP034262+, ORCID：67259836, Web of Science ID：WOS:000185609600007 - Neutronics experiments for DEMO blanket at JAERI/FNS
Yukikatsu Terada
Nuclear Fusion, 2003
Scientific journal
DOI：https://doi.org/10.1088/0029-5515/43/7/303
DOI ID：10.1088/0029-5515/43/7/303, ORCID：67259784, Web of Science ID：WOS:000184430400003 - Observational evidence for a high-energy Compton cloud in GRO J1655-40 under a high accretion rate
Yoshihito Kobayashi; Aya Kubota; Kazuhiro Nakazawa; Tadayuki Takahashi; Kazuo Makishima
Publications of the Astronomical Society of Japan, Volume：55, Number：1, First page：273, Last page：279, 2003, [Reviewed]
Observational results on GRO J1655-40 are reported, based on the X-ray spectra obtained with the PCA and the HEXTE on-board RXTE during its 1996-1997 outburst. By referring to the 40-150 keV X-ray luminosity, L40-150. six typical spectra were selected and analyzed. When L40-150 is sufficiently below ∼ 5 × 1036erg s-1 (assuming a distance of 3.2 kpc and an isotropic emission), the 3-150 keV PCA/HEXTE spectra are well described by a standard spectral model consisting of an optically-thick disk spectrum and a power-law tail. When L40-150 exceeds 5 × 1036 erg s-1, the standard model fails to reproduce the joint spectrum, due to a mild turn-over in the HEXTE spectrum. Successful fits are recovered when the power-law component is replaced by a broken power-law model with the break energy at ∼ 40 keV, or by an exponentially cutoff power-law model with the cutoff energy at 190-300 keV. The fits are further improved by employing a thermal Comptonization component, wherein the electron temperature and optical depth of the Compton cloud are estimated to be 70-85 keV and 0.45-0.65, respectively. These results provide strong evidence for the existence of thermal high-energy electrons, and reconfirm the picture of strong disk Comptonization.
Astronomical Society of Japan, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/55.1.273
DOI ID：10.1093/pasj/55.1.273, ISSN：0004-6264, SCOPUS ID：0038066594 - Mystery of strong iron lines from magnetic cataclysmic variables
Terada, Yukikatsu
Astronomical Herald, Dec. 2002
Extremely strong ionized iron emission lines were discovered with ASCA from a few Galactic objects. They are thought to be polar systems, or binary systems containing magnetic white dwarfs. We think the line intensities of these objects are unphysical, because they are 2 or 3 times higher than those of other polars. In other words, we consider that the iron line emission may be somehow enhanced by an unknown yet universal mechanism, rather than that indicating a truly high metallicity of those systems. In this paper, we propose a new possible interpretation that the iron line is collimated in the accretion plasma due to resonance scattering, and demonstrate the solution of the mystery....
Scientific journal
ORCID：101134211, Bibcode：2002AstHe..95..581T - Performance of the ASTRO-E hard X-ray detector
M. Tashiro; T. Kamae; K. Makishima; T. Takahashi; T. Murakami; Y. Fukazawa; M. Kokubun; K. Nakazawa; M. Nomachi; A. Yoshida; Y. Ezoe; N. Isobe; N. Iyomoto; J. Kataoka; J. Kotoku; M. Kouda; S. Kubo; A. Kubota; Y. Matsumoto; T. Mizuno; G. M. Madejski; Y. Okada; N. Ota; H. Ozawa; G. Sato; M. Sugiho; M. Sugizaki; I. Takahashi; H. Takahashi; T. Tamura; C. Tanihata; Y. Terada; Y. Uchiyama; S. Watanabe; K. Yamaoka; D. Yonetoku
IEEE Transactions on Nuclear Science, Volume：49 I, Number：4, First page：1893, Last page：1897, Aug. 2002
This paper summarizes the design and performance of the hard X-ray detector constructed for the ASTRO-E satellite. The detector utilizes the GSO/BGO well-type phoswich counters in a compound-eye configuration to achieve an extremely low background level of a few × 10-5counts s-1 cm-2keV-1 [1]. The GSO scintillators installed in the BGO active shield wells are sensitive to 30-600 kev photons, while the 2-mm-thick silicon PIN diodes, placed in front of each GSO crystal, cover the 10-60 kev energy band with a spectral resolution of ∼3.5-keV full-width at half-maximum. The design goals, of both low background and high energy resolution, in the hard X-ray bands were verified through the preflight calibration experiments.
Scientific journal
DOI：https://doi.org/10.1109/TNS.2002.801491
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DOI ID：10.1109/TNS.2002.801491, ISSN：0018-9499, SCOPUS ID：0036703265 - CdTe and CdZnTe detectors for timing measurements
Yuu Okada; Tadayuki Takahashi; Goro Sato; Shin Watanabe; Kazuhiro Nakazawa; Kunishiro Mori; Kazuo Makishima
IEEE Transactions on Nuclear Science, Volume：49, Number：4, First page：1986, Last page：1992, Aug. 2002, [Reviewed]
We measured timing properties of CdTe and CdZnTe semiconductor detectors with planar configuration. We developed a new method to evaluate their performance in timing resolution utilizing an 241Am-doped plastic scintillator. We confirmed that the low mobility and short lifetime of holes are major obstacles to their timing resolution. However, their timing properties can be very much improved, either by applying a high electric field that increases the carrier speed or by selecting those events which are dominated by the electron signal. We demonstrated the latter through a pulse-shape discrimination technique using two different integration time constants. In conjunction with a newly developed CdTe diode, we obtained a superior timing resolution of 5.8 ns. We also discussed the application of CdTe to positron emission tomography (PET), employing the standard 511 keV gamma-gamma coincidence method. We confirmed that a geometrical configuration in which the electrodes are parallel to the incident γ-rays gives about three times better timing response than a geometry when the electrodes are perpendicular to the γ-ray beam.
English, Scientific journal
DOI：https://doi.org/10.1109/TNS.2002.801709
DOI ID：10.1109/TNS.2002.801709, ISSN：0018-9499, SCOPUS ID：0036702981 - CdTe stacked detectors for gamma-ray detection
Shin Watanabe; Tadayuki Takahashi; Yuu Okada; Goro Sato; Manabu Kouda; Takefumi Mitani; Yoshihito Kobayashi; Kazuhiro Nakazawa; Yoshikatsu Kuroda; Mitsunobu Onishi
IEEE Transactions on Nuclear Science, Volume：49, Number：3, First page：1292, Last page：1296, Jun. 2002, [Reviewed]
We describe a stacked detector made of thin cadmium telluride (CdTe) diode detectors. By using a thin CdTe device, we can overcome the charge loss problem due to the small mobility and short lifetime of holes in CdTe or cadmium zinc telluride (CdZnTe) detectors. However, a CdTe detector with a thickness of more than 5 mm is needed for adequate detection efficiency for gamma-rays of several hundred keV. Good energy resolution and good peak detection efficiency are difficult to obtain using such a thick CdTe detector. The stacked detector enabled us to realize a detector with both high-energy resolution and good efficiencies for gamma rays up to several hundred keV. In order to verify this concept, we constructed a prototype made of ten layers of a 0.5-mm-thick CdTe diode detectors with a surface area of 21.5 mm × 21.5 mm. With this, we have achieved 5.3-keV and 7.9-keV energy resolution [full width at half maximum (FWHM)] at 356 keV and 662 keV, respectively, at the temperature of -20°C.
English, Scientific journal
DOI：https://doi.org/10.1109/TNS.2002.1039654
DOI ID：10.1109/TNS.2002.1039654, ISSN：0018-9499, SCOPUS ID：0036624389 - Broad band X-ray imaging mission "NeXT"
Yuzuru Tawara; Hideyo Kunieda; Hajime Inoue; Kazuhisa Mitsuda; Yasushi Ogasaka; Tadayuki Takahashi
Proceedings of SPIE - The International Society for Optical Engineering, Volume：4851, Number：1, First page：324, Last page：330, 2002, [Reviewed]
One of the major fields to be explored in the 21st century is the hard X-ray sky up to 50 keV or 100 keV. Above 10 keV, thermal components start to decay rapidly and then non-thermal power law continua become dominant. For example, some of SNR and Cluster of Galaxies exhibit substantial non-thermal components, which suggest high energy electrons. We would like to investigate acceleration mechanisms of such high energy particles by observing hard X-ray images and their spectra. In order to perform imaging observations in hard X-ray range up to 50 keV, supermirror hard X-ray telescopes are most promising. We have studied to put Pt/C supermirror on the mirror shells of a high throughput X-ray telescope. The first satellite mission proposed with the supermirror hard X-ray telescope is our New X-ray Telescope mission (NeXT) in Japan to be launched 2010. 6-7 supermirror telescopes will be installed at the top of an extensible optical bench. The hybrid X-ray imager will be placed on the focal plane to observe hard X-ray images up to 50 keV with CdTe pixel detector underneath a thin CCD for soft X-ray imaging. For high resolution spectroscopy, TES type calorimeters are considered without cryogen. Non-imaging hard X-ray and soft gamma ray detector is studied to achieve unprecedented sensitivity between 50 and 300 keV. NeXT will be a sort of pathfinder of hard X-ray astronomy not only technically but also scientifically.
English, International conference proceedings
DOI：https://doi.org/10.1117/12.461508
DOI ID：10.1117/12.461508, ISSN：0277-786X, SCOPUS ID：0038295794 - High resolution CdTe detectors for the next generation multi-compton gamma-ray telescope
Tadayuki Takahashi; Kazuhiro Nakazawa; Tuneyoshi Kamae; Hiroyasu Tajima; Yasushi Fukazawa; Masaharu Nomachi; Motohide Kokubun
Proceedings of SPIE - The International Society for Optical Engineering, Volume：4851, Number：2, First page：1228, Last page：1235, 2002, [Reviewed]
A multi-Compton gamma-ray telescope based on high resolution semiconductor materials (Semiconductor Multi-Compton Telescope (SMCT) or Advanced Compton Telescope (ACT)) is a promising approach to achieve high sensitivity for gamma-rays with energies from several hundred keV up to several MeV. A SMCT utilizing several tens of layers of thin CdTe (Cadmium Telluride) detector is an attractive concept to obtain higher detection efficiency in comparison with Si-based SMCT. Recently we have developed high energy-resolution CdTe diode detectors. A large-area detector with dimensions of 2.15 × 2.15 cm2 with a thickness of 0.5 mm shows an energy resolution of better than 3 keV (FWHM) at 60 keV. In order to extend the application of CdTe diodes to the detection of MeV gamma-rays, we have constructed a stacked detector consisting of 40 layers of large CdTe diodes. Here we report the recent progress on the high-resolution CdTe diode and describe the conceptual design of new Multi-Compton Gamma-ray telescopes based on Monte Carlo simulation. An idea of active pair production telescope is briefly described.
English, International conference proceedings
DOI：https://doi.org/10.1117/12.461287
DOI ID：10.1117/12.461287, ISSN：0277-786X, SCOPUS ID：0037957111 - CdTe and CdZnTe detectors for timing measurements
Yuu Okada; Tadayuki Takahashi; Goro Sato; Shin Watanabe; Kazuhiro Nakazawa; Kunishiro Mori; Kazuo Makishima
IEEE Nuclear Science Symposium and Medical Imaging Conference, Volume：4, First page：2429, Last page：2433, 2002, [Reviewed]
We report the timing properties of CdTe and CdZnTe detectors in planar configuration. By utilizing 241Am doped scintilator, we have developed a new method to evaluate the timing performance of the semiconductor detector. We confirm that the slow mobility and short life time of holes significantly degrades the timing performance. To achieve high carrier speed, either by applying a high electric field or by selecting only electrons, is very important for obtaining a detector with fast, ∼ nsec timing capability. To select only the electron events, we adopt the pulse height selection with a fast-slow shaping amplifier. In conjunction with a newly developed CdTe diode, we obtain a superior performance of 5.8 nsec. We also discuss the application for Positron Emission Tomography with 511 keV gamma-gamma coincidence method, and found that a geometrical arrangement in which electrodes are parallel to the incident γ-rays gives about 3 time better timing response than is available when the electrodes are perpendicular to the γ-ray beam.
English, Scientific journal
DOI：https://doi.org/10.1109/NSSMIC.2001.1009310
DOI ID：10.1109/NSSMIC.2001.1009310, ISSN：1095-7863, SCOPUS ID：0035555033 - Variability timescales of TeV blazars observed in the ASCA continuous long-look X-ray monitoring
Chiharu Tanihata; C. Megan Urry; Tadayuki Takahashi; Jun Kataoka; Stefan J. Wagner; Greg M. Madejski; Makoto Tashiro; Manabu Kouda
Astrophysical Journal, Volume：563, Number：2, First page：569, Last page：581, Dec. 2001, [Reviewed]
Three uninterrupted, long (lasting respectively 7, 10, and 10 days) ASCA observations of the well-studied TeV-bright blazars Mrk 421, Mrk 501, and PKS 2155-304 all show continuous strong X-ray flaring. Despite the relatively faint intensity states in two of the three sources, there was no identifiable quiescent period in any of the observations. Structure function analysis shows that all blazars have a characteristic timescale of ∼1 day, comparable to the recurrence time and to the timescale of the stronger flares. On the other hand, examination of these flares in more detail reveals that each of the strong flares is not a smooth increase and decrease but exhibits substructures of shorter flares having timescales of ∼10 ks. We verify via simulations that in order to explain the observed structure function, these shorter flares ("shots") are unlikely to be fully random, but in some way are correlated with each other. The energy dependent cross-correlation analysis shows that interband lags are not universal in TeV blazars. This is important since in the past only positive detections of lags were reported. In this work, we determine that the sign of a lag may differ from flare to flare
significant lags of both signs were detected from several flares, while no significant lag was detected from others. However, we also argue that the nature of the underlying component can affect these values. The facts that all flares are nearly symmetric and that fast variability shorter than the characteristic timescale is strongly suppressed, support the scenario where the light crossing time dominates the variability timescales of the day-scale flares.
Institute of Physics Publishing, English, Scientific journal
DOI：https://doi.org/10.1086/323960
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DOI ID：10.1086/323960, ISSN：1538-4357, eISSN：1538-4357, SCOPUS ID：18044402878 - X-ray beaming caused by resonance scattering in the accretion column of magnetic cataclysmic variables
Y. Terada; M. Ishida; K. Makishima; T. Imanari; R. Fujimoto; K. Matsuzaki; H. Kaneda
Monthly Notices of the Royal Astronomical Society, Volume：328, Number：1, First page：112, Last page：126, Nov. 2001, [Reviewed]
Extremely strong ionized Fe emission lines, with equivalent widths reaching ∼4000 eV, were discovered by ASCA from a few Galactic compact objects, including AX J2315-0592, RX J1802.1 + 1804 and AX J1842.8-0423. These objects are thought to be binary systems containing magnetized white dwarfs (WDs). A possible interpretation of the strong Fe K line is the line-photon collimation in the WD accretion column, as a result of resonance scattering of line photons. The collimation occurs when the accretion column has a flat shape, and the effect is augmented by the vertical velocity gradient, which reduces the resonant trapping of resonant photons along the magnetic field lines. This effect was quantitatively confirmed with Monte Carlo simulations. Furthermore, with ASCA observations of the polar V834 Centauri, this collimation effect was clearly detected as a rotational modulation of the equivalent width of the Fe K emission line. The extremely strong emission lines mentioned above can be explained consistently by our interpretation. Combining this effect with other X-ray information, the geometry and plasma parameters in the accretion column were determined.
English, Scientific journal
DOI：https://doi.org/10.1046/j.1365-8711.2001.04878.x
DOI ID：10.1046/j.1365-8711.2001.04878.x, ISSN：0035-8711, SCOPUS ID：0042869774 - Spatially dependent response of thick and large area p-i-n diode for ASTRO-E hard X-ray detector
Yukikatsu Terada
IEEE Transactions on Nuclear Science, Volume：48, First page：426, Last page：429, Jun. 2001
The ASTRO-E hard X-ray detector utilizes GSO(Gd2SiO5:Ce 0.5% mol)-BGO(Bi4Ge3O12) well-type phoswich counters [1] in compound-eye configuration to achieve an extremely low background level of about a few times 10-5 counts s-1 cm-2 keV-1. The GSO scintillators placed at the bottom of the BGO well observe photons in the energy range 30-600 keV. To cover the lower energy range of 10-60 keV, silicon p-i-n diodes of 2 mm in thickness and 21.5×21.5 mm2 in size were newly developed and placed in front of the GSO scintillators. The p-i-n diode exhibits complex spectral responses, including subpeak and low energy tail components. To examine the origin of these components, we measured the spatially resolved response of the p-i-n diode and confirmed that the subpeak and the low energy tail are related to the electrode structures and electric fields in the p-i-n diode, respectively.
Scientific journal
DOI：https://doi.org/10.1109/23.940093
DOI ID：10.1109/23.940093, ISSN：0018-9499, ORCID：67259998, SCOPUS ID：17944364085, Web of Science ID：WOS:000170576200038 - X-ray beaming due to resonance scattering in the accretion column of magnetic cataclysmic variables
Yukikatsu Terada
New Century of X-ray Astronomy, 2001
Scientific journal
ORCID：67259826, Web of Science ID：WOS:000176731500136 - Achievements of the ASTRO-E hard X-ray detector development
M. Tashiro; K. Makishima; T. Kamae; T. Murakami; T. Takahashi; Y. Fukazawa; M. Kokubun; K. Nakazawa; M. Nomachi; A. Yoshida; Y. Ezoe; N. Isobe; N. Iyomoto; J. Kataoka; J. Kotoku; M. Kouda; S. Kubo; A. Kubota; Y. Matsumoto; T. Mizuno; Y. Okada; N. Ota; H. Ozawa; G. Sato; M. Sugiho; M. Sugizaki; I. Takahashi; H. Takahashi; T. Tamura; C. Tanihata; Y. Terada; Y. Uchiyama; S. Watanabe; K. Yamaoka; D. Yonetoku
IEEE Nuclear Science Symposium and Medical Imaging Conference, Volume：1, First page：483, Last page：486, 2001
The ASTRO-E Hard X-ray Detector utilized GSO/BGO well-type phoswich counters in compound-eye configuration [1], to achieve an extremely low background level of a few ×10-5 counts s-1cm-2keV-1. The GSO scintillators installed in the BGO active shield wells observes 30-600 keV photons, while silicon PIN diodes of 2 mm thick placed in front of each GSO crystal covers 10 - 60 keV photons with energy resolution of ∼3.5 keV FWHM. The design goals both of low background and high energy resolution in the hard X-ray bands were confirmed to be achieved through the preflight calibration experiments.
International conference proceedings
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=0035553511&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=0035553511&origin=inward
SCOPUS ID：0035553511 - Spatially dependent response of thick and large area PIN diode developed for ASTRO-E hard x-ray detector
M. Sugiho; T. Kamae; K. Makishima; T. Takahashi; T. Murakami; M. Tashiro; Y. Fukazawa; M. Kaneda; T. Tamura; N. Iyomoto; M. Sugizaki; H. Ozawa; A. Kubota; K. Nakazawa; K. Yamaoka; M. Kokubun; N. Ota; C. Tanihata; N. Isobe; S. Kubo; Y. Terada; Y. Matsumoto; Y. Uchiyama; D. Yonetoku; I. Takahashi; J. Kotoku; S. Watanabe; Y. Ezoe
IEEE Nuclear Science Symposium and Medical Imaging Conference, Volume：1, 2000
The ASTRO-E Hard X-ray Detector utilizes GSO/BGO well-type phoswich counters in compound-eye configuration, to achieve an extremely low background level of about a few times 10-5 counts s-1 cm-2 keV-1. The GSO scintillators placed at the bottom of the BGO well observe photons in the energy range 30-600 keV. To cover the lower energy range of 10-60 keV, silicon PIN diodes of 2 mm in thickness and 21.5 × 21.5mm2 in size were newly developed, and placed in front of the GSO scintillators. The PIN diode exhibits complex spectral responses, including subpeak and low energy tail components. To examine the origin of these components, we measured spatially-resolved response of the PIN diode, and confirmed that the subpeak and the low energy tail are related to the electrode structures and electric fields in the PIN diode, respectively.
International conference proceedings
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=0034593751&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=0034593751&origin=inward
SCOPUS ID：0034593751 - A peculiar X-ray transient source, AX J1842.8-0423, discovered with ASCA
Y Terada; H Kaneda; K Makishima; M Ishida; K Matsuzaki; F Nagase; T Kotani
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：51, Number：1, First page：39, Last page：44, Feb. 1999, [Reviewed]
A new transient X-ray source, AX J1842.8-0423, was discovered with ASCA in 1996 October in the Scutum arm region. The source exhibited an absorption-corrected 2-10 keV flux of 5.2 x 10(-12) erg s(-1) cm(-2) with insignificant intensity variability. The continuous spectrum is approximated by a power-law of photon index 2.9, absorbed by a hydrogen column of NH similar to 5 X 10(22) Cm-2 The spectrum also exhibits the Fe-K emission line with an extremely large equivalent width of similar to 4000 eV, of which the centroid energy is similar to 6.8 keV. The overall spectrum can be reproduced by a thin-thermal plasma-emission model having a temperature of similar to 5.1 keV, on the condition that the heavy-element abundance is allowed to increase to 3.0(-0.9)(+4.3) solar abundance. The source was undetectable in a previous observation in 1993 October, as well as in a subsequent observation in 1996 April. The overall source behavior is thus quite peculiar, but may be explained in terms of a close binary involving a magnetized white dwarf viewed from pole-on inclination, where the unusually strong Fe-K line may be the result of resonant scattering of line photons.
OXFORD UNIV PRESS, English, Scientific journal
DOI：https://doi.org/10.1093/pasj/51.1.39
DOI ID：10.1093/pasj/51.1.39, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000079030200004 - Fabrication of the ASTRO-E Hard X-ray Detector
K Nakazawa; T Kamae; K Makishima; T Takahashi; T Murakami; M Tashiro; Y Fukazawa; T Tamura; N Iyomoto; K Ebisawa; Y Ezoe; M Hamaya; M Horii; N Isobe; M Kokubun; J Kotoku; A Kubota; Y Matsumoto; T Mizuno; Y Mizuno; K Mori; T Onishi; N Ota; S Shinoda; M Sugiho; K Taguchi; Takahasi, I; M Tanaka; C Tanihata; Y Terada; Y Uchiyama; S Watanabe; K Yamaoka; D Yonetoku
EUV, X-RAY, AND GAMMA-RAY INSTRUMENTATION FOR ASTRONOMY X, Volume：3765, First page：148, Last page：159, 1999, [Reviewed]
The Bard X-ray Detector (HXD) is one of the three instruments on the fifth Japanese cosmic X-ray satellite ASTROE , scheduled for launch in January, 2000. The HXD covers a wide energy range of 10-600 keV, using 16 identical GSO/BGO phoswich-counter modules, of which the low-energy efficiency is greatly improved by adding 2 mm-thick silicon PIN diodes. Production of the HXD between completed and pre-flight calibration is now in progress. The design concept of the HXD sensor, detail of the production process, and a brief summary of the measured performance is reported.
SPIE-INT SOC OPTICAL ENGINEERING, English, International conference proceedings
ISSN：0277-786X, ORCID：34407116, SCOPUS ID：0033354596, Web of Science ID：WOS:000084180500015 - Thick and large area PIN diodes for hard X-ray astronomy
Yukikatsu Terada
Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 1999
Scientific journal
DOI：https://doi.org/10.1016/S0168-9002(99)00636-1
DOI ID：10.1016/S0168-9002(99)00636-1, ORCID：67259822, Web of Science ID：WOS:000082897900046 - The digital data processing system of the ASTRO-E hard X-ray detector
Y Terada; M Tashiro; T Takahashi; Y Fukazawa; G Kawaguchi; K Matsuzaki; Odagi, I; Y Tanaka; K Makishima; T Kamae
ASTRONOMISCHE NACHRICHTEN, Volume：320, Number：4-5, First page：377, Last page：377, 1999, [Reviewed]
WILEY-V C H VERLAG GMBH, English, Scientific journal
ISSN：0004-6337, Web of Science ID：WOS:000084277700139 - Verification of the Astro-E Hard X-ray Detector based on newly developed Ground Support Equipment
J. Kataoka; M. Nomachi; T. Takahashi; G. Kawaguchi; Y. Terada; T. Murakami; C. Tanihata; Y. Uchiyama; K. Yamaoka; Y. Fukazawa; T. Kamae; K. Makishima; M. Tashiro; H. Kubo
Proceedings of SPIE - The International Society for Optical Engineering, Volume：3445, First page：143, Last page：154, 1998, [Reviewed]
English
- XRISM Science Performance and Data Analysis Workshop in Swiss
12 Feb. 2024
欧州第一回XRISM科学データ解析ワークショップ 開催主催 - The 2nd XRISM Community Workshop in USA Meryland, SOC
17 Jan. 2024
米国第二回XRISMコミュニティ研究会 開催主催 - X線分光撮像衛星XRISMの科学運用の現状(2)
吉田鉄生; 林克洋; 金丸善朗; 小川翔司; 福島光太郎; 寺田幸功; 田代信; 高橋弘充; 水野恒史; 深沢泰司; 阪本菜月; 信川正順; 宇野伸一郎; 中澤知洋; 大宮悠希; 大熊佳吾; 内山秀樹; 久保田あや; 勝田哲; 塩入匠; 本上侑吾; 寺島雄一; 志達めぐみ; 新居田祐基; 高木利紘; 山内茂雄; 太田直美; 白木天音; 鈴木那梨; 北口貴雄; 山田智史; 坪井陽子; 米山友景; 根本登; 内田悠介; 江口智士; 谷本敦; 善本真梨那; 内田和海; 海老沢研; 渡辺伸; 飯塚亮; HOLLAND Matt; YAQOOB Tahir; BALUTA Chris; LOEWENSTEIN Michael; LOEWENSTEIN Michael; MILLER Eric
Volume：2024, 2024
ISSN：1347-0639, J-Global ID：202402236287409494 - Current Status of the XRISM Science Operations: II
林克洋; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 中澤知洋; 内山秀樹; 久保田あや; 寺島雄一; 深澤泰司; 山内茂雄; 太田直美; 北口貴雄; 勝田哲; 坪井陽子; 志達めぐみ; 海老沢研; 内田悠介; 江口智士; 谷本敦; 米山友景; 山田智史; 内田和海; 吉田鉄生; 金丸善朗; 小川翔司; 福島光太郎; 渡辺伸; 飯塚亮; HOLLAND Matt; LOEWENSTEIN Michael; LOEWENSTEIN Michael; MILLER Eric; YAQOOB Tahir; BALUTA Chris; 白木天音; 新居田祐基; 根本登; 大宮悠希; 鈴木那梨; 善本真梨那; 大熊佳吾; 本上侑吾; 高木利紘
日本物理学会講演概要集(CD-ROM), Volume：79, Number：2, 2024
ISSN：2189-079X, J-Global ID：202502277995798054 - CTA report 223: Study of the probalitity of afterpulse of the Camera for the CTA Large-Sized Telescope
清本拓人; 高橋光成; 山本常夏; 小林志鳳; 小林志鳳; 武石隆治; 齊藤隆之; 立石大; 寺田幸功; 糸川拓海; 猪目祐介; 大岡秀行; 岡知彦; 奥村曉; 奥村曉; 折戸玲子; 片桐秀明; 櫛田淳子; 窪秀利; 郡司修一; 櫻井駿介; 田島宏康; 田中真伸; 手嶋政廣; 手嶋政廣; 寺内健太; 門叶冬樹; 中森健之; 西嶋恭司; 野崎誠也; 野崎誠也; 野田浩司; 野田浩司; 橋山和明; HADASCH Daniela; MAZIN Daniel; MAZIN Daniel; 溝手雅也
日本物理学会講演概要集(CD-ROM), Volume：79, Number：1, 2024
ISSN：2189-079X, J-Global ID：202402282580510821 - X線分光撮像衛星XRISMの科学運用の現状
小川翔司; 寺田幸功; 田代信; 高橋弘充; 水野恒史; 深沢泰司; 阪本菜月; 信川正順; 宇野伸一郎; 中澤知洋; 大宮悠希; 大熊佳吾; 内山秀樹; 久保田あや; 勝田哲; 塩入匠; 寺島雄一; 志達めぐみ; 新居田祐基; 山内茂雄; 太田直美; 白木天音; 鈴木那梨; 北口貴雄; 山田智史; 坪井陽子; 米山友景; 根本登; 内田悠介; 江口智士; 谷本敦; 善本真梨那; 海老沢研; 渡辺伸; 飯塚亮; 林克洋; 内田和海; 金丸善朗; 星野晶夫; 吉田鉄生; HOLLAND Matt; YAQOOB Tahir; BALUTA Chris; LOEWENSTEIN Michael; LOEWENSTEIN Michael; MILLER Eric
Volume：2024, 2024
ISSN：1347-0639, J-Global ID：202402268559182117 - Current Status of the XRISM Science Operations
林克洋; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 中澤知洋; 内山秀樹; 久保田あや; 寺島雄一; 深澤泰司; 山内茂雄; 太田直美; 北口貴雄; 勝田哲; 坪井陽子; 志達めぐみ; 海老沢研; 内田悠介; 江口智士; 谷本敦; 米山友景; 山田智史; 内田和海; 吉田鉄生; 金丸善朗; 小川翔司; 星野晶夫; 渡辺伸; 飯塚亮; HOLLAND Matt; LOEWENSTEIN Michael; LOEWENSTEIN Michael; MILLER Eric; YAQOOB Tahir; BALUTA Chris; 塩入匠; 阪本菜月; 白木天音; 新居田祐基; 根本登; 大宮悠希; 鈴木那梨; 善本真梨那; 大熊佳吾
日本物理学会講演概要集(CD-ROM), Volume：79, Number：1, 2024
ISSN：2189-079X, J-Global ID：202402253520919847 - XRISM Timing System and in-orbit Verification
寺田幸功; 寺田幸功; 志達めぐみ; 塩入匠; 新居田祐基; 澤田真理; 小湊隆; 田代信; 田代信; 戸田謙一; 前島弘則; 夏苅権; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 中澤知洋; 内山秀樹; 久保田あや; 寺島雄一; 深沢泰司; 山内茂雄; 太田直美; 北口貴雄; 勝田哲; 坪井陽子; 海老沢研; 内田悠介; 江口智士; 林克洋; 谷本敦; 米山友景; 山田智史; 内田和海; 吉田鉄生; 金丸善朗; 小川翔司; 星野晶夫; 渡辺伸; 飯塚亮; HOLLAND M; LOEWENSTEIN M; LOEWENSTEIN M; MILLER E; YAQOOB T; BALUTA C
日本物理学会講演概要集(CD-ROM), Volume：79, Number：1, 2024
ISSN：2189-079X, J-Global ID：202402277873851601 - JSPS core-to-core XRISM Team Meeting #6, Local Organization Committee
15 Dec. 2023
JSPS事業 XRISMチーム会議#6 開催主催 - The 15th International Astrophysical Consortium for High Energy Calibration Meeting 2023 Workshop, Science Organization Committee
23 Apr. 2023
国際衛星較正コンソーシアム (IACHEC)会議 2023 開催委員 - X線分光撮像衛星XRISMの科学運用に向けての模擬試験
林克洋; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 米山友景; 吉田鉄生; BALUTA Chris; 海老沢研; 江口智士; 深澤泰司; 橋口葵; 勝田哲; 北口貴雄; 小高裕和; 大野雅功; 太田直美; 阪間美南; 阪本菜月; 志達めぐみ; 塩入匠; 丹波翼; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内田悠介; 内山秀樹; 山田智史; 山内茂雄
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302210598711687 - X線分光撮像衛星XRISMの観測データ処理ツールの開発状況
山田智史; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 林克洋; 米山友景; 吉田鉄生; BALUTA Chris; 海老沢研; 江口智士; 深澤泰司; 橋口葵; 勝田哲; 北口貴雄; 小高裕和; 大野雅功; 太田直美; 阪間美南; 阪本菜月; 志達めぐみ; 塩入匠; 丹波翼; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内田悠介; 内山秀樹; 山内茂雄
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302249250042517 - X線分光撮像衛星XRISMの科学運用準備の現状(2)
米山友景; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 林克洋; 吉田鉄生; BALUTA Chris; 海老沢研; 江口智士; 深澤泰司; 橋口葵; 勝田哲; 北口貴雄; 小高裕和; 大野雅功; 太田直美; 阪間美南; 阪本菜月; 志達めぐみ; 塩入匠; 丹波翼; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内田悠介; 内山秀樹; 山田智史; 山内茂雄
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302258897086050 - 軟X線から硬X線の広帯域を高感度で撮像分光する衛星計画FORCEの現状(15)
森浩二; 武田彩希; 村上弘志; 寺田幸功; 久保田あや; 山田智史; 馬場彩; 小高裕和; 谷津陽一; 小林翔悟; 幸村孝由; 内山泰伸; 佐藤寿紀; 北山哲; 高橋忠幸; 石田学; 渡辺伸; 山口弘悦; 藤田裕; 中嶋大; 萩野浩一; 中澤知洋; 古澤彰浩; 鶴剛; 上田佳宏; 内田裕之; 榎戸輝揚; 水本岬希; 田中孝明; 鈴木寛大; 松本浩典; 野田博文; 常深博; 伊藤真之; 信川正順; 信川久実子; 太田直美; 粟木久光; 寺島雄一; 志達めぐみ; 深沢泰司; 水野恒史; 高橋弘充; 谷本敦; 赤松弘規; HORNSCHEMEIER Ann.E; OKAJIMA Takashi; ZHANG W.William; VENTERS Tonia; YUKITA Mihoko
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302262717458170 - Status report of the XRISM science operation
内田悠介; 田代信; 田代信; 寺田幸功; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 米山友景; 吉田鉄生; BALUTA Chris; 海老沢研; 江口智士; 深澤泰司; 橋口葵; 林克洋; 勝田哲; 北口貴雄; 小高裕和; 大野雅功; 太田直美; 阪間美南; 阪本菜月; 志達めぐみ; 塩入匠; 丹波翼; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内山秀樹; 山田智史; 山内茂雄
日本物理学会講演概要集(CD-ROM), Volume：78, Number：1, 2023
ISSN：2189-079X, J-Global ID：202302211107124079 - A wide-band X-ray observatory FORCE: proposal status as of March 2023
中澤知洋; 森浩二; 村上弘志; 赤松弘規; 久保田あや; 幸村孝由; 小林翔悟; 高橋忠幸; 馬場彩; 萩野浩一; 寺田幸功; 内山泰伸; 佐藤寿紀; 石村康生; 北山哲; 谷津陽一; 藤田裕; 石田学; 渡辺伸; 山口弘悦; 中嶋大; 古澤彰浩; 信川正順; 太田直美; 鶴剛; 上田佳宏; 榎戸輝揚; 内田裕之; 水本岬希; 信川久実子; 松本浩典; 小高裕和; 野田博文; 常深博; 田中孝明; 鈴木寛大; 伊藤真之; 粟木久光; 寺島雄一; 志達めぐみ; 深沢泰司; 水野恒史; 高橋弘充; 武田彩希; 谷本敦; HORNSCHEMEIER A.E.; 岡島崇; ZHANG W.W.
日本物理学会講演概要集(CD-ROM), Volume：78, Number：1, 2023
ISSN：2189-079X, J-Global ID：202302253684665724 - X線分光撮像衛星XRISMの科学運用準備の現状(3)
林克洋; 田代信; 寺田幸功; 高橋弘充; 信川正順; 水野恒史; 宇野伸一郎; 久保田あや; 中澤知洋; 渡辺伸; 飯塚亮; 佐藤理江; 星野晶夫; 吉田鉄生; 小川翔司; 金丸善朗; BALUTA Chris; 海老沢研; 江口智士; 小高裕和; 勝田哲; 北口貴雄; 新居田祐基; 太田直美; 阪本菜月; 志達めぐみ; 塩入匠; 白木天音; 谷本敦; 寺島雄一; 坪井陽子; 内田和海; 内田悠介; 内山秀樹; 山田智史; 山内茂雄; 米山友景
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302259844930637 - CTA大口径望遠鏡のためのSiPMモジュールに装着する集光器の開発
溝手雅也; 山本常夏; 奥村曉; 田島宏康; 高橋光成; 齋藤隆之; 猪目祐介; 大岡秀行; 櫻井駿介; 手嶋政廣; 野田浩司; 橋山和明; 窪秀利; 岡知彦; 野崎誠也; HADASCH Daniela; MAZIN Daniel; 片桐秀明; 吉田龍生; 寺内健太; 折戸玲子; 櫛田淳子; 西嶋恭司; 郡司修一; 門叶冬樹; 中森健之; 砂田裕志; 立石大; 寺田幸功; 田中真伸
Volume：2023, 2023
ISSN：1347-0639, J-Global ID：202302219796682291 - JSPS core-to-core XRISM Multiwavelength Workshop 2022, Science Organization Committee & Local Organization Committee Chair
14 Dec. 2022
JSPS事業 第一回XRISM多波長連携ワークショップ 開催委員および開催主宰者 - JSPS core-to-core XRISM Science Meeting #5, Local Organization Committee Chair
12 Dec. 2022
JSPS事業 XRISM科学会議#5 開催主催 - JSPS core-to-core XRISM Science Workshop for Young Researchers 2022, Science Organization Committee & Local Organization Committee Chair
19 Oct. 2022
JSPS事業 第一回XRISM若手科学会議 開催委員および開催主宰者 - International Astrophysical Consortium for High Energy Calibration Meeting 2022 Spring Workshop, Science Organization Committee
23 May 2022
国際衛星較正コンソーシアム (IACHEC)会議 2022 開催委員 - 軟X線から硬X線の広帯域を高感度で撮像分光する衛星計画FORCEの現状(13)
森浩二; 武田彩希; 村上弘志; 寺田幸功; 久保田あや; 榎戸輝揚; 馬場彩; 小高裕和; 谷本敦; 谷津陽一; 小林翔悟; 幸村孝由; 萩野浩一; 内山泰伸; 佐藤寿紀; 北山哲; 高橋忠幸; 石田学; 渡辺伸; 山口弘悦; 藤田裕; 中嶋大; 中澤知洋; 古澤彰浩; 鶴剛; 上田佳宏; 内田裕之; 水本岬希; 田中孝明; 鈴木寛大; 松本浩典; 野田博文; 常深博; 伊藤真之; 信川正順; 信川久実子; 太田直美; 粟木久光; 寺島雄一; 志達めぐみ; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 赤松弘規; HORNSCHEMEIER A. E.; 岡島崇; ZHANG W. W.; VENTERS T.; YUKITA M.
Volume：2022, 2022
ISSN：1347-0639, J-Global ID：202202235960902055 - 軟X線から硬X線の広帯域を高感度で撮像分光する衛星計画FORCEの現状(14)
森浩二; 武田彩希; 村上弘志; 寺田幸功; 久保田あや; 榎戸輝揚; 馬場彩; 小高裕和; 谷本敦; 谷津陽一; 小林翔悟; 幸村孝由; 内山泰伸; 佐藤寿紀; 北山哲; 高橋忠幸; 石田学; 渡辺伸; 山口弘悦; 藤田裕; 中嶋大; 萩野浩一; 中澤知洋; 古澤彰浩; 鶴剛; 上田佳宏; 内田裕之; 水本岬希; 田中孝明; 鈴木寛大; 松本浩典; 野田博文; 常深博; 伊藤真之; 信川正順; 信川久実子; 太田直美; 粟木久光; 寺島雄一; 志達めぐみ; 深沢泰司; 水野恒史; 高橋弘充; 赤松弘規; HORNSCHEMEIER A.E; 岡島崇; ZHANG W.W.; VENTERS T.; YUKITA M.
Volume：2022, 2022
ISSN：1347-0639, J-Global ID：202202259244431957 - 無衝突衝撃波でのイオン加熱機構:XRISMによる宇宙線加速効率の制限
霜田治朗; 大平豊; 馬場彩; 寺田幸功; 寺田幸功; 山崎了; 井上剛志; 田中周太
Volume：2022, 2022
ISSN：1347-0639, J-Global ID：202202223881592777 - International Astrophysical Consortium for High Energy Calibration Meeting 2021 (Spring/Fall Workshops), Science Organization Committee
16 Apr. 2021
国際衛星較正コンソーシアム (IACHEC)会議 開催委員 - 2021年度夢ナビ講義・夢ナビ研究室訪問 講師
Apr. 2021
2021年度夢ナビ講義Video・夢ナビ研究室訪問 講師（視聴 432名・訪問参加数145名） - A wide-band X-ray observatory FORCE: Development status of the Wide-band Hybrid X-ray Imager and its CdTe imager
中澤知洋; 森浩二; 村上弘志; 寺田幸功; 久保田あや; 榎戸輝揚; 馬場彩; 小高裕和; 谷津陽一; 小林翔悟; 幸村孝由; 萩野浩一; 内山泰伸; 佐藤寿紀; 北山哲; 高橋忠幸; 石田学; 渡辺伸; 山口弘悦; 大橋隆哉; 中嶋大; 古澤彰浩; 鶴剛; 上田佳宏; 内田裕之; 松本浩典; 野田博文; 常深博; 信川正順; 太田直美; 信川久実子; 伊藤真之; 田中孝明; 鈴木寛大; 粟木久光; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 武田彩希; 大野雅功; 赤松弘規; HORNSCHEMEIER A.E; 岡島崇; ZHANG W.W.
日本物理学会講演概要集(CD-ROM), Volume：76, Number：2, 2021
ISSN：2189-079X, J-Global ID：202202212428718394 - A wide-band X-ray observatory FORCE: Mission and Spacecraft design study improvements in 2020
中澤知洋; 森浩二; 村上弘志; 寺田幸功; 久保田あや; 榎戸輝揚; 馬場彩; 小高裕和; 谷津陽一; 小林翔悟; 幸村孝由; 萩野浩一; 内山泰伸; 北山哲; 高橋忠幸; 石田学; 渡辺伸; 山口弘悦; 大橋隆哉; 中嶋大; 古澤彰浩; 鶴剛; 上田佳宏; 田中孝明; 内田裕之; 松本浩典; 野田博文; 常深博; 信川正順; 太田直美; 信川久実子; 伊藤真之; 粟木久光; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 武田彩希; 大野雅功; 赤松弘規; HORNSCHEMEIER A.E; 岡島崇; ZHANG W.W.
日本物理学会講演概要集(CD-ROM), Volume：76, Number：1, 2021
ISSN：2189-079X, J-Global ID：202102263502534111 - 軟X線から硬X線の広帯域を高感度で撮像分光する衛星計画FORCEの現状(12)
森浩二; 武田彩希; 村上弘志; 寺田幸功; 久保田あや; 榎戸輝揚; 馬場彩; 小高裕和; 谷津陽一; 小林翔悟; 幸村孝由; 萩野浩一; 内山泰伸; 佐藤寿紀; 北山哲; 高橋忠幸; 高橋忠幸; 石田学; 渡辺伸; 山口弘悦; 藤田裕; 中嶋大; 中澤知洋; 古澤彰浩; 鶴剛; 上田佳宏; 内田裕之; 田中孝明; 鈴木寛大; 松本浩典; 野田博文; 常深博; 伊藤真之; 信川正順; 信川久実子; 太田直美; 粟木久光; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 赤松弘規; HORNSCHEMEIER A.E; 岡島崇; ZHANG W.W.
Volume：2021, 2021
ISSN：1347-0639, J-Global ID：202102213317552845 - 軟X線から硬X線の広帯域を高感度で撮像分光する小型衛生計画FORCEの現状(11)
森浩二; 武田彩希; 村上弘志; 寺田幸功; 久保田あや; 榎戸輝明; 馬場彩; 小高裕和; 谷津陽一; 小林翔悟; 幸村孝由; 萩野浩一; 内山泰伸; 北山哲; 高橋忠幸; 石田学; 渡辺伸; 山口弘悦; 大橋隆哉; 中嶋大; 中澤知洋; 古澤彰浩; 鶴剛; 上田佳宏; 田中孝明; 内田裕之; 松本浩典; 野田博文; 常深博; 伊藤真之; 信川正順; 信川久実子; 太田直美; 粟木久光; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 赤松弘規; HORNSCHEMEIER A.E.; 岡島崇; ZHANG W.W.
Volume：2021, 2021
ISSN：1347-0639, J-Global ID：202102267438113800 - International Astrophysical Consortium for High Energy Calibration Meeting 2020, Science Organization Committee
23 Nov. 2020
国際衛星較正コンソーシアム (IACHEC)会議 開催委員 - CTA Report 163: Assembly and quality control of focal-plane-camera modules for the 2nd to 4th Large-Sized Telescopes of CTA
������������������ ������������������; ���������������� ��������; ���������������� ��������������; Kawashima Shotaro; Kawamura Kiomei; �������������� ����������; �������� ������������������; ���������� ��������������; ������������������ ������������; ���������� ����������������; �������������� ����������������; ���������� ������������; ������������ ������������; ������������ ��������; ������������ ������������; ������������ ����������; �������������� ����������; Tsukamoto Yusuke; �������������� ����������������; ������������ ������������������; �������������� ������������; ���������������� ��������������; Imagawa Kaname; ������������������ ��������������; Nabatame Yasuyuki; ������������������ ������������; ������������ ��������; ������������ ����������; �������� ��������; �������������� ��������������; ������������ ������������; ���������� ������������; ������������ ������; �������������� ��������; ���������������� ������������������; �������������� ������������; ������ ������-���������� ��������������������; ���������� Masahiro; Sasaki Nobuaki; Dettlaff Antonios; ���������� ����������������; ������ ����������������; �������������� ������; �������������� ����������; ���������� ����������
Meeting Abstracts of the Physical Society of Japan, Volume：75, First page：472, Last page：472, 2020
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.75.1.0_472
DOI ID：10.11316/jpsgaiyo.75.1.0_472, CiNii Articles ID：130008157419 - 軟X線から硬X線の広帯域を高感度で撮像分光する小型衛星計画FORCEの現状(10)
森浩二; 武田彩希; 村上弘志; 寺田幸功; 久保田あや; 馬場彩; 小高裕和; 谷津陽一; 幸村孝由; 萩野浩一; 小林翔悟; 内山泰伸; 北山哲; 高橋忠幸; 高橋忠幸; 石田学; 渡辺伸; 飯塚亮; 山口弘悦; 大橋隆哉; 中嶋大; 中澤知洋; 古澤彰浩; 鶴剛; 上田佳宏; 田中孝明; 内田裕之; 松本浩典; 野田博文; 常深博; 伊藤真之; 信川正順; 信川久実子; 太田直美; 粟木久光; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; HORNSCHEMEIER A. E; 岡島崇; ZHANG W. W.; WILLIAMS B. J.
Volume：2020, 2020
ISSN：1347-0639, J-Global ID：202002260841062191 - 超巨大ブラックホールの進化を探る広帯域X線高感度撮像分光衛星FORCE
森浩二; 武田彩希; 村上弘志; 寺田幸功; 久保田あや; 榎戸輝明; 馬場彩; 小高裕和; 谷津陽一; 小林翔悟; 幸村孝由; 萩野浩一; 内山泰伸; 北山哲; 高橋忠幸; 高橋忠幸; 石田学; 渡辺伸; 飯塚亮; 山口弘悦; 大橋隆哉; 中嶋大; 中澤知洋; 古澤彰浩; 鶴剛; 上田佳宏; 田中孝明; 内田裕之; 松本浩典; 野田博文; 常深博; 伊藤真之; 信川正順; 信川久実子; 太田直美; 粟木久光; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 赤松弘規; HORNSCHEMEIER A.E.; 岡島崇; ZHANG W.W.
Volume：2020, 2020
ISSN：1347-0639, J-Global ID：202002231461281151 - X線天文衛星Athena計画の現状
松本浩典; 山崎典子; 満田和久; 篠崎慶亮; 前田良知; 粟木久光; 坪井陽子; 江副祐一郎; 山口弘悦; 佐藤浩介; 中嶋大; 深沢泰司; 大橋隆哉; 上田佳宏; 寺島雄一; 太田直美; 馬場彩; 海老沢研; 寺田幸功; 鶴剛; 常深博
Volume：2020, 2020
ISSN：1347-0639, J-Global ID：202002232041182598 - A wide-band X-ray observatory FORCE: Science study and proposal status update
中澤知洋; 森浩二; 鶴剛; 上田佳宏; 石田学; 松本浩典; 粟木久光; 村上弘志; 寺田幸功; 久保田あや; 榎戸輝揚; 馬場彩; 小高裕和; 谷津陽一; 小林翔悟; 幸村孝由; 萩野浩一; 内山泰伸; 北山哲; 高橋忠幸; 渡辺伸; 飯塚亮; 山口弘悦; 大橋隆哉; 中嶋大; 古澤彰浩; 田中孝明; 内田裕之; 野田博文; 常深博; 伊藤真之; 信川正順; 信川久実子; 太田直美; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 赤松弘規; HORNSCHEMEIER A.E; 岡島崇; ZHANG W.W.
日本物理学会講演概要集(CD-ROM), Volume：75, Number：2, 2020
ISSN：2189-079X, J-Global ID：202102270682518989 - The 14th International Astrophysical Consortium for High Energy Calibration Meeting, SOC & LOC Chair
20 May 2019
第１４回 国際衛星較正コンソーシアム (IACHEC)会議 Science Organization Committee & Local Organization Committee Chair - CTA Report 151: Mass production and performance evaluation of focal plane light concentrators for the first CTA Large-Sized Telescope
Suzuki M.; Yamamoto T.; Inada T.; Inome Y.; Iwamura Y.; Ohoka H.; Okazaki N.; Oka T.; Okumura A.; Orito R.; Kajiwara Y.; Katagiri H.; Kushida J.; Kimura S.; Kubo H.; Gunji S.; Koyama S.; Saito T.; Sakurai S.; Sawada M.; Sunada Y.; Takahashi M.; Tanaka M.; Tamura K.; Choushi Y.; Tujimoto S.; Teshima M.; Terada Y.; Tokanai F.; Nakamori T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Nozaki S.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Furuta T.; Masuda S.; Yoshida T.; Hadasch Daniela; Mazin Daniel; the CTA-Japan consortium
Meeting Abstracts of the Physical Society of Japan, Volume：74.1, Number：1, First page：560, Last page：560, 22 Mar. 2019
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.74.1.0_560
DOI ID：10.11316/jpsgaiyo.74.1.0_560, ISSN：2189-079X, eISSN：2189-0803, J-Global ID：201902289864116161, CiNii Articles ID：130008148550 - The Science Organizing Comittee Chair, 第１８回高エネルギー宇宙物理連絡会研究会「高エネルギー宇宙物理学の最前線と2020/30年代のロードマップ」
18 Mar. 2019
第１８回高エネルギー宇宙物理連絡会研究会の主催者 - CTA Report 149: Development of analysis software for CTA LST-1
Iwamura Yuki; Kubo Hidetoshi; Gunji Shuichi; Kobayashi Yukiho; Saito Takayuki; Sakaki Naoto; Sakurai Shunsuke; Sasai Yoshinori; Sunada Yuji; Takahashi Tomoya; Taneda Yuki; Inada Tomohiro; Chikawa Michiyuki; Choushi Yuuki; Teshima Masahiro; Terada Yukikatsu; Nakamori Takeshi; Nishijima Kyoshi; Nozaki Seiya; Noda Koji; Hayashida Masaaki; Hiroshima Nagisa; Ohishi Michiko; Fukami Satoshi; Fujihara Chikako; Miura Chika; Yamamoto Tokonatsu; Yoshikoshi Takanori; Yoshida Tatsuo; Ri Ken; Zenin Anatolii; the CTA-Japan Consortium; Ohtani Yoshiki; Okumura Akira; Orito Reiko; Katagiri Hideaki; Kamimoto Takumi; Kushida Junko
Meeting Abstracts of the Physical Society of Japan, Volume：74, First page：558, Last page：558, 2019
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.74.1.0_558
DOI ID：10.11316/jpsgaiyo.74.1.0_558, CiNii Articles ID：130008148536 - MAGIC報告66:HESS J1912+101領域のガンマ線放射
永吉勤; 永吉勤; GREEN David; FRUCK Christian; STRZYS Marcel; 井上進; 稲田知大; 岩村由樹; 大谷恵生; 岡知彦; 緒方智之; 神本匠; 梶原由貴; 櫛田淳子; 窪秀利; 久門拓; 小林志鳳; 齋藤隆之; 櫻井駿介; 高橋光成; 種田裕貴; 辻本晋平; 手嶋政廣; 手嶋政廣; 中森健之; 西嶋恭司; 野崎誠也; 野田浩司; HADASCH Daniela; 平子丈; 深見哲志; 古田智也; MAZIN Daniel; MAZIN Daniel; 増田周; 勝田哲; 佐藤浩介; 田代信; 寺田幸功
Volume：74, Number：1, 2019
ISSN：2189-079X, J-Global ID：201902219247405378 - CTA Report 150: Commissioning test of the focal plane camera of the first CTA Large-Sized Telescope.
Nozaki S.; Kajiwara Y.; Katagiri H.; Kushida J.; Kimura S.; Kubo H.; Gunji S.; Koyama S.; Saito T.; Sakurai S.; Sawada M.; Inada T.; Suzuki M.; Sunada Y.; Takahashi M.; Takahara H.; Tanaka M.; Tamura K.; Choushi Y.; Tujimoto S.; Teshima M.; Terada Y.; Inome Y.; Tokanai F.; Nakamori T.; Nagayoshi T.; Nishijima K.; Nishiyama G.; Noda K.; Hayashida M.; Bamba A.; Hirako J.; Fukami S.; Iwamura Y.; Furuta T.; Masuda S.; Yamamoto T.; Yoshida T.; Hadasch Daniela; Mazin Daniel; the CTA-Japan consortium; Ikeno M.; Uchida T.; Ohoka H.; Okazaki N.; Oka T.; Okumura A.; Orito R.
Meeting Abstracts of the Physical Society of Japan, Volume：74, First page：559, Last page：559, 2019
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.74.1.0_559
DOI ID：10.11316/jpsgaiyo.74.1.0_559, CiNii Articles ID：130008148543 - CTA Report 157: Measurement of timing response performance of photomultiplier tube used for CTA large sized telescope
Sunada Yuji; Katagiri Hideaki; Kushida Junko; Kubo Hidetoshi; Gunji Shuichi; Kobayashi Yukiho; Saito Takayuki; Sakurai Shunsuke; Suzuki Megumi; Takahashi Mitsunari; Tanaka Manobu; Inome Yusuke; Tamura Kenji; Choushi Yuuki; Teshima Masahiro; Terada Yukikatsu; Tokanai Fuyuki; Nakamori Takeshi; Nagayoshi Tsutomu; Nishijima Kyoshi; Nogami Yuto; Nozaki Seiya; Iwamura Yuki; Noda Koji; Hadasch Daniela; Hayashida Masaaki; Bamba Aya; Hirako Joe; Furuta Tomoya; Mazin Daniel; Masuda Shu; Yamamoto Tokonatsu; Yoshida Tatsuo; Ohoka Hideyuki; Ikeno Masahiro; Uchida Tomohisa; Oka Tomohiko; Okazaki Nao; Okumura Akira; Orito Reiko; Kajiwara Yuki
Meeting Abstracts of the Physical Society of Japan, Volume：74, First page：360, Last page：360, 2019
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.74.2.0_360
DOI ID：10.11316/jpsgaiyo.74.2.0_360, CiNii Articles ID：130008153483 - 軟X線から硬X線の広帯域を高感度で撮像分光する小型衛星計画FORCEの現状(9)
鶴剛; 上田佳宏; 田中孝明; 内田裕之; 森浩二; 武田彩希; 村上弘志; 寺田幸功; 中島真也; 久保田あや; 馬場彩; 小高裕和; 谷津陽一; 幸村孝由; 萩野浩一; 小林翔悟; 内山泰伸; 北山哲; 高橋忠幸; 石田学; 渡辺伸; 飯塚亮; 山口弘悦; 中嶋大; 中澤知洋; 古澤彰浩; 松本浩典; 常深博; 伊藤真之; 信川正順; 太田直美; 粟木久光; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 岡島崇; 森英之
Volume：2019, 2019
ISSN：1347-0639, J-Global ID：201902272639090319 - 小型衛星計画FORCE用のX線反射鏡開発の現状
松本浩典; 粟木久光; 田村啓輔; 岡島崇; 森英之; 森浩二; 武田彩希; 村上弘志; 寺田幸功; 中島真也; 久保田あや; 馬場彩; 小高裕和; 谷津陽一; 幸村孝由; 萩野浩一; 小林翔悟; 内山泰伸; 北山哲; 高橋忠幸; 石田学; 渡辺伸; 飯塚亮; 山口弘悦; 中嶋大; 中澤知洋; 古澤彰浩; 鶴剛; 上田佳宏; 田中孝明; 内田裕之; 常深博; 伊藤真之; 信川正順; 太田直美; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功
Volume：2019, 2019
ISSN：1347-0639, J-Global ID：201902243140319404 - 軟X線から硬X線の広帯域を高感度で撮像分光する小型衛星計画FORCEの現状(8)
森浩二; 武田彩希; 村上弘志; 寺田幸功; 中島真也; 久保田あや; 馬場彩; 小高裕和; 谷津陽一; 幸村孝由; 萩野浩一; 小林翔悟; 内山泰伸; 北山哲; 高橋忠幸; 石田学; 渡辺伸; 飯塚亮; 山口弘悦; 中嶋大; 中澤知洋; 古澤彰浩; 鶴剛; 上田佳宏; 田中孝明; 内田裕之; 松本浩典; 常深博; 伊藤真之; 信川正順; 太田直美; 粟木久光; 寺島雄一; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 岡島崇; 森英之
Volume：2019, 2019
ISSN：1347-0639, J-Global ID：201902278827319256 - The Science Organizing Comittee Chair of The 1st Japan-China X-ray collaboration Workshop “New eyes on X-ray astrophysical objects with Japanese and Chinese observatories”
19 Nov. 2018
第一回日中X線宇宙物理国際会議の主催者 (SOC chair) - 軟X線から硬X線の広帯域を高感度で撮像分光する小型衛星計画FORCEの現状(7)
中澤知洋; 森浩二; 鶴剛; 上田佳宏; 松本浩典; 粟木久光; 石田学; 寺島雄一; 常深博; 中嶋大; 田中孝明; 内田裕之; 伊藤真之; 寺田幸功; 久保田あや; 馬場彩; 小高裕和; 高橋忠幸; 谷津陽一; 幸村孝由; 萩野浩一; 小林翔悟; 北山哲; 村上弘志; 信川正順; 太田直美; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 古澤彰浩; 武田彩希; 中島真也; 内山泰伸; 渡辺伸; 飯塚亮; 岡島崇; 山口弘悦; 森英之
日本天文学会年会講演予稿集, Volume：2018, First page：220, 20 Aug. 2018
Japanese
ISSN：1347-0639, J-Global ID：201802295703941764 - 「ひとみ」HXIを用いた軌道上中性子バックグラウンドの評価
鈴木寛大; 中澤知洋; 萩野浩一; 国分紀秀; 佐藤悟朗; 高橋忠幸; 渡辺伸; 太田方之; 佐藤理江; 森國城; 村上浩章; 三宅克馬; 古田禄大; 馬場彩; 鶴剛; 田中孝明; 榎戸輝揚; 小林翔悟; 寺田幸功; 内山秀樹; 谷津洋一; 野田博文; 田島宏康; 山岡和貴; 林克洋; 林克洋; 深沢泰司; 水野恒史; 大野雅功; 高橋弘充; 勝田隼一郎; 中森健之; 内山泰伸; 斉藤新也; 牧島一夫; 小高裕和; 湯浅孝行; 中野俊男; 片岡淳; 三村健人; LEBRUN Francois; LIMOUSIN Olivier; LAURENT Philippe; MAIER Daniel; 武田伸一郎; 森浩二
日本天文学会年会講演予稿集, Volume：2018, First page：227, 20 Feb. 2018
Japanese
ISSN：1347-0639, J-Global ID：201802275754345763 - X線衛星代替機XARMにおける科学運用計画
寺田幸功; 田代信; 田代信; 海老沢研; 深沢泰司; 飯塚亮; 勝田哲; 北口貴雄; 久保田あや; 水野恒史; 中島真也; 中澤知洋; 信川正順; 大野雅功; 太田直美; 志達めぐみ; 菅原泰晴; 高橋弘充; 田村隆幸; 田中康之; 寺島雄一; 坪井陽子; 内山秀樹; 宇野伸一郎; 渡辺伸; 山内茂雄
日本天文学会年会講演予稿集, Volume：2018, First page：228, 20 Feb. 2018
Japanese
ISSN：1347-0639, J-Global ID：201802220528606681 - 中性子星合体におけるr-process元素合成のX線診断
井上進; 仏坂健太; 村瀬孔大; 馬場彩; 長瀧重博; 寺田幸功
Volume：2018, 2018
ISSN：1347-0639, J-Global ID：201802267726623210 - X-ray diagnostics of r-process nucleosynthesis in neutron star mergers
Inoue Susumu; Hotokezaka Kenta; Murase Kohta; Bamba Aya; Nagataki Shigehiro; Terada Yukikatsu
Meeting Abstracts of the Physical Society of Japan, Volume：73.1, First page：462, Last page：462, 2018
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.73.1.0_462
DOI ID：10.11316/jpsgaiyo.73.1.0_462, eISSN：2189-0803, CiNii Articles ID：130007648478 - Detecting polarization of gamma rays from Crab Nebula with Hitomi Soft Gamma-ray Detector(SGD)
Watanabe Shin; Ohno Masanori; Odaka Hirokazu; Kataoka Jun; Katsuta Junichiro; Kitaguchi Takao; Kokubun Motohide; Goldwurm Andrea; Saito Shinya; Sato Goro; Sato Rie; Uchida Yusuke; Takahashi Tadayuki; Takahashi Hiromitsu; Takeda Shin'ichiro; Tanaka Takaaki; Tanaka Yasuyuki; Terada Yukikatsu; Nakazawa Kazuhiro; Nakano Toshio; Nakamori Takashi; Noda Hirofumi; Tajima Hiroyasu; Hagino Kouichi; Hayashi Katsuhiro; Blandford Roger; Makishima Kazuo; Madejski Grzegorz; Mizuno Tsunefumi; Mori Kunishiro; Yatsu Yoichi; Yamaoka Kazutaka; Yuasa Takayuki; Fukazawa Yasushi; Yonetoku Daisuke; Laurent Philippe; Limousin Olivier; Lebrun François; the SGD team; Ichinohe Yuto; Uchiyama Hideki; Uchiyama Yasunobu; Enoto Teruaki; Ohta Masayuki
Meeting Abstracts of the Physical Society of Japan, Volume：73, First page：492, Last page：492, 2018
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.73.1.0_492
DOI ID：10.11316/jpsgaiyo.73.1.0_492, CiNii Articles ID：130007648585 - 光電子増倍管の1光電子信号強度分布の精密測定
山本常夏; 猪目祐介; 郡司修一; HADASCH Daniela; 林田将明; 片桐秀明; 今野裕介; 窪秀利; 櫛田淳子; 中森健之; 永吉勤; 西嶋恭司; 野崎誠也; MAZIN Daniel; 増田周; MIRZOYAN Razmik; 大岡秀行; 折戸玲子; 斎藤隆之; 櫻井駿介; 高橋光成; 手嶋政廣; 手嶋政廣; 寺田幸功; 門叶冬樹; 吉田龍生; 吉井柊
日本物理学会講演概要集(CD-ROM), Volume：72, Number：2, First page：ROMBUNNO.12aS35‐2, 25 Sep. 2017
Japanese
ISSN：2189-079X, J-Global ID：201702272415176341 - 1‐80keVの広帯域X線を高感度で撮像分光する次世代の小型科学衛星計画FORCE:2017年のステータス
中澤知洋; 森浩二; 村上弘志; 久保田あや; 寺田幸功; 谷津陽一; 馬場彩; 幸村孝由; 内山泰伸; 斉藤新也; 北山哲; 高橋忠幸; 渡辺伸; 中島真也; 萩野浩一; 松本浩典; 古澤彰浩; 鶴剛; 上田佳宏; 田中孝明; 内田裕之; 武田彩希; 常深博; 中嶋大; 信川正順; 太田直美; 粟木久光; 寺島雄一; 深沢泰司; 高橋弘充; 大野雅功; 岡島崇; 山口弘悦; 森英之; 小高裕和
日本物理学会講演概要集(CD-ROM), Volume：72, Number：1, First page：ROMBUNNO.20aK21‐5, 21 Mar. 2017
Japanese
ISSN：2189-079X, J-Global ID：201702247665760103 - NuSTAR/Suzakuによる最も明るいガンマ線超新星残骸N132Dの観測
馬場彩; 山崎了; 大平豊; 澤田真理; 寺田幸功; 小山勝二; 山口弘悦; 勝田哲
Volume：2017, 2017
ISSN：1347-0639, J-Global ID：201702248935752976 - X線天文衛星「ひとみ」搭載の硬X線撮像検出器(HXI)の軌道上性能
中澤知洋; 高橋忠幸; 国分紀秀; 渡辺伸; 佐藤悟朗; 太田方之; 萩野浩一; 佐藤理江; LEE Herman; 能町正治; 米徳大輔; 田中孝明; 榎戸輝揚; 寺田幸功; 内山秀樹; 谷津洋一; 一戸悠人; 野田博文; 田島宏康; 山岡和貴; 林克洋; 深沢泰司; 水野恒史; 大野雅功; 高橋弘充; 中森健之; 内山泰伸; 斉藤新也; 牧島一夫; 湯浅孝行; 中野俊男; 片岡淳; LEBRUN Francois; GOLDWURM Andrea; LIMOUSIN Olivier; LAURENT Philippe; MAIER Daniel; 小高裕和
日本物理学会講演概要集(CD-ROM), Volume：71, Number：2, First page：ROMBUNNO.24aSP‐6, 23 Sep. 2016
Japanese
ISSN：2189-079X, J-Global ID：201602272459157362 - X線天文衛星「ひとみ(ASTRO‐H)」搭載軟ガンマ線検出器(SGD)の軌道上動作
深沢泰司; 田島宏康; 渡辺伸; 大野雅功; 勝田隼一郎; 北口貴雄; 高橋弘充; 田中康之; 水野恒史; 林克洋; 山岡和貴; 太田方之; 国分紀秀; 佐藤悟朗; 佐藤理江; 高橋忠幸; 萩野浩一; 森國城; 一戸悠人; 内山秀樹; 内山泰伸; 斉藤新也; 榎戸輝揚; 田中孝明; 小高裕和; BLANDFORD Roger; MADEJSKI Grzegorz; 片岡淳; GOLDWURM Andrea; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois; 武田伸一郎; 寺田幸功; 中澤知洋; 中野俊男; 牧島一夫; 湯浅孝行; 中森健之; 野田博文; 谷津陽一; 米徳大輔
日本天文学会年会講演予稿集, Volume：2016, First page：245, 20 Aug. 2016
Japanese
ISSN：1347-0639, J-Global ID：201602289335125998 - X線天文衛星「ひとみ(ASTRO‐H)」搭載硬X線撮像検出器(HXI)の軌道上動作
萩野浩一; 中澤知洋; 国分紀秀; 佐藤悟朗; 高橋忠幸; 渡辺伸; 太田方之; 佐藤理江; LEE Herman; 能町正治; 米徳大輔; 田中孝明; 榎戸輝揚; 寺田幸功; 内山秀樹; 谷津洋一; 一戸悠人; 野田博文; 田島宏康; 山岡和貴; 林克洋; 林克洋; 深沢泰司; 水野恒史; 大野雅功; 高橋弘充; 中森健之; 内山泰伸; 斉藤新也; 牧島一夫; 湯浅孝行; 中野俊男; 片岡淳; LEBRUN Francois; GOLDWURM Andrea; LIMOUSIN Olivier; LAURENT Philippe; MAIER Daniel; 武田伸一郎; 小高裕和
日本天文学会年会講演予稿集, Volume：2016, First page：245, 20 Aug. 2016
Japanese
ISSN：1347-0639, J-Global ID：201602243814162204 - X線天文衛星「すざく」搭載広帯域全天モニターWAMによる2005年から2015年までの太陽フレアの観測
矢部聖也; 田代信; 寺田幸功; 山内誠; 大森法輔; 牧島一夫; 岩切渉; 山岡和貴; 杉田聡司; 深沢泰司; 大野雅功; 河野貴文; 高橋忠幸; 国分紀秀; 中川友進; 浦田裕次; 中澤知洋
日本天文学会年会講演予稿集, Volume：2016, First page：96, 20 Aug. 2016
Japanese
ISSN：1347-0639, J-Global ID：201602246783740824 - ASTRO‐H衛星搭載硬X線撮像検出器(HXI)の現状打ち上げ
中澤知洋; 国分紀秀; 佐藤悟朗; 萩野浩一; 太田方之; 小高裕和; 川原田円; 佐藤理江; 高橋忠幸; 武田伸一郎; 原山淳; 渡辺伸; 榎戸輝揚; 田中孝明; 寺田幸功; 内山秀樹; 谷津陽一; 中野俊男; 田島宏康; 山岡和貴; 大野雅功; 勝田隼一郎; 高橋弘充; 深沢泰司; 水野恒史; 中森健之; 野田博文; 牧島一夫; 湯浅孝行; 内山泰伸; 斉藤新也; 片岡淳; LAURENT Philippe; LEBRUN Francois; LIMOUSIN Okivier
日本天文学会年会講演予稿集, Volume：2016, First page：211, 20 Feb. 2016
Japanese
ISSN：1347-0639, J-Global ID：201602211759134026 - In-orbit performance of Soft Gamma-ray Detector(SGD) onboard Hitomi (ASTRO-H) X-ray satellite
Watanabe Shin; Odaka Hirokazu; Kataoka Jun; Katsuta Junichiro; Kitaguchi Takao; Kokubun Motohide; Goldwurm Andrea; Saito Shinya; Sato Goro; Sato Rie; Takahashi Tadayuki; Tajima Hiroyasu; Takahashi Hiromitsu; Takeda Shin'ichiro; Tanaka Takaaki; Tanaka Yasuyuki; Terada Yukikatsu; Nakazawa Kazuhiro; Nakano Toshio; Nakamori Takashi; Noda Hirofumi; Hagino Kouichi; Fukazawa Yasushi; Hayashi Katsuhiro; Blandford Roger; Makishima Kazuo; Madejski Grzegorz; Mizuno Tsunefumi; Mori Kunishiro; Yatsu Yoichi; Yamaoka Kazutaka; Yuasa Takayuki; Yonetoku Daisuke; Ichinohe Yuto; Laurent Philippe; Limousin Olivier; Lebrun François; the SGD team; Uchiyama Hideki; Uchiyama Yasunobu; Enoto Teruaki; Ohta Masayuki; Ohno Masanori
Meeting Abstracts of the Physical Society of Japan, Volume：71, First page：371, Last page：371, 20162016年2月17日に打ち上げられたX線衛星「ひとみ」(ASTRO-H)に搭載された軟ガンマ線検出器(Soft Gamma-ray Detector:SGD)の軌道動作実績について報告する。SGDは、3月15日より順次、センサーの立ち上げを行い、通信途絶となった3月26日まで、機能的には正常に動作させることができた。一部の天体からのガンマ線信号の取得に成功し、高感度ガンマ線観測を行う上で重要となる軌道上バックグランドのデータを得た。SGDで初めて実現したSi/CdTe半導体コンプトンカメラで得られたこれらのデータについて、報告を行う。
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.71.2.0_371
DOI ID：10.11316/jpsgaiyo.71.2.0_371, CiNii Articles ID：130006246129 - X線天文衛星「ひとみ(ASTRO-H)」搭載機器の解析ソフトウェアの開発
寺田幸功; 高橋弘充; 信川正順; 澤田真理; BALUTA C.; 高橋忠幸; ANGELINI L.; 山口弘悦; 山口弘悦; MILLER E.; KRIMM H.; YAQOOB T.; LOWENSTEIN M.; HARRUS I.; 中島真也; 上田周太朗; 佐藤悟朗; 佐藤理江; 飯塚亮; 竹井洋; 前田良知; 辻本匡弘; 山崎典子; 夏苅権; 石田学; 海老沢研; 田村隆幸; 尾崎正伸; 石崎欣尚
Volume：2016, 2016
ISSN：1347-0639, J-Global ID：201602279553317978 - Radioactive decay products in neutron star merger ejecta: heating efficiency and γ-ray emission
Yukikatsu Terada
Monthly Notices of the Royal Astronomical Society, 2016
The radioactive decay of the freshly synthesized $r$-process nuclei ejected
in compact binary mergers power optical/infrared macronovae (kilonovae) that
follow these events. The light curves depend critically on the energy partition
among the different products of the radioactive decay and this plays an
important role in estimates of the amount of ejected $r$-process elements from
a given observed signal. We study the energy partition and $\gamma$-ray
emission of the radioactive decay. We show that $20$-$50\%$ of the total
radioactive energy is released in $\gamma$-rays on timescales from hours to a
month. The number of emitted $\gamma$-rays per unit energy interval has roughly
a flat spectrum between a few dozen keV and $1$ MeV so that most of this energy
is carried by $\sim 1$ MeV $\gamma$-rays. However at the peak of macronova
emission the optical depth of the $\gamma$-rays is $\sim 0.02$ and most of the
$\gamma$-rays escape. The loss of these $\gamma$-rays reduces the heat
deposition into the ejecta and hence reduces the expected macronova signals if
those are lanthanides dominated. This implies that the ejected mass is larger
by a factor of $2$-$3$ than what was previously estimated. Spontaneous fission
heats up the ejecta and the heating rate can increase if a sufficient amount of
transuranic nuclei are synthesized. Direct measurements of these escaping
$\gamma$-rays may provide the ultimate proof for the macronova mechanisms and
an identification of the $r$-process nucleosynthesis sites. However, the
chances to detect these signals are slim with current X-ray and $\gamma$-ray
missions. New detectors, more sensitive by at least a factor of ten, are needed
for a realistic detection rate.
Technical report
DOI：https://doi.org/10.1093/MNRAS/STW404
DOI ID：10.1093/MNRAS/STW404, ORCID put code：67259871, arXiv ID：arXiv:1511.05580, Web of Science ID：WOS:000376386600004 - ASTRO‐H搭載硬X線撮像検出器(HXI)の地上試験における最終性能
小林翔悟; 佐藤悟朗; 萩野浩一; 中野俊男; 中澤知洋; 湯浅孝行; 牧島一夫; 榎戸輝揚; 佐藤理江; 渡辺伸; 国分紀秀; 高橋忠幸; 斉藤新也; 内山泰伸; 片岡淳; 谷津陽一; 北口貴雄; 大野雅功; 高橋弘充; 水野恒史; 深沢泰司; 田島宏康; 寺田幸功; 中森健之; LIMOUSIN Olivier; LAURENT Philippe; LEBRUN Francois
日本物理学会講演概要集(CD-ROM), Volume：70, Number：2, First page：ROMBUNNO.25PSJ-4, 24 Sep. 2015
Japanese
ISSN：2189-079X, J-Global ID：201602219700360309 - CTAで探る宇宙線の起源:RX J1713.7‐3946のガンマ線シミュレーション
佐野栄俊; 福井康雄; 田島宏康; 奥村暁; 中森健之; 郡司修一; 片桐秀明; 柳田昭平; 吉田龍生; 山崎了; 大平豊; 馬場彩; 澤田真理; 森浩二; 李兆衡; 藤田裕; 井上剛志; 花畑義隆; 林田将明; 吉越貴紀; 窪秀利; 斎藤隆之; 田中孝明; 櫛田淳子; 井上進; 井岡邦仁; 郡和範; 村瀬孔大; 長瀧重博; 内藤統也; 寺田幸功; 内山泰伸; GABICI Stefano
日本天文学会年会講演予稿集, Volume：2015, First page：48, 20 Aug. 2015
Japanese
ISSN：1347-0639, J-Global ID：201502216722627221 - CTA大口径望遠鏡 カメラの開発状況
山本常夏; 猪目祐介; 掃部寛隆; 大岡秀行; 高橋光成; 手嶋政廣; 中嶋大輔; 花畑義隆; 林田将明; 窪秀利; 今野裕介; 斎藤隆行; 土屋優吾; 畑中謙一郎; 増田周; 寺田幸功; 松岡俊介; 永吉勤; 郡司修一; 武田淳希; 門叶冬樹; 中森健之; 澤田真理; 坪根善雄; 馬場彩; 折戸玲子; 片桐秀明; 梅津陽平; 櫛田淳子; 辻本晋平; 友野弥生; 西嶋恭司; 小山志勇
日本天文学会年会講演予稿集, Volume：2015, First page：258, 20 Aug. 2015
Japanese
ISSN：1347-0639, J-Global ID：201502206186823289 - CTA計画大口径望遠鏡初号機用PMTの性能と品質管理
永吉勤; 寺田幸功; 松岡俊介; 猪目祐介; 掃部寛隆; 山本常夏; 大岡秀行; 高橋光成; 手嶋政廣; 中嶋大輔; 花畑義隆; 林田将明; 窪秀利; 今野裕介; 斎藤隆行; 土屋優吾; 畑中謙一; 増田周; 郡司修一; 武田淳希; 門叶冬樹; 中森健之; 澤田真理; 坪根善雄; 馬場彩; 折戸玲子; 片桐秀明; 梅津陽平; 櫛田淳子; 辻本晋平; 友野弥生; 西嶋恭司; 小山志勇
日本天文学会年会講演予稿集, Volume：2015, First page：54, 20 Aug. 2015
Japanese
ISSN：1347-0639, J-Global ID：201502216636844317 - CTA大口径望遠鏡 焦点面検出器の構造
掃部寛隆; 猪目祐介; 山本常夏; 大岡秀行; 高橋光成; 手嶋政廣; 中嶋大輔; 花畑義隆; 林田将明; 窪秀利; 今野裕介; 斎藤隆行; 土屋優吾; 畑中謙一郎; 増田周; 寺田幸功; 松岡俊介; 永吉勤; 郡司修一; 武田淳希; 門叶冬樹; 中森健之; 澤田真理; 坪根善雄; 馬場彩; 折戸玲子; 片桐秀明; 梅津陽平; 櫛田淳子; 辻本晋平; 友野弥生; 西嶋恭司; 小山志勇
日本天文学会年会講演予稿集, Volume：2015, First page：54, 20 Aug. 2015
Japanese
ISSN：1347-0639, J-Global ID：201502217127990033 - ASTRO‐H衛星搭載軟ガンマ線検出器の現状と解析ソフトウェアについて
高橋弘充; 田島宏康; 深沢泰司; 渡辺伸; 渡辺伸; 大野雅功; 北口貴雄; 田中康之; 水野恒史; 太田方之; 小高裕和; 国分紀秀; 佐藤悟朗; 佐藤理江; 武田伸一郎; 林克洋; 原山淳; 森國城; 高橋忠幸; 高橋忠幸; 中澤知洋; 牧島一夫; 田中孝明; 榎戸輝揚; 片岡淳; 谷津陽一; 内山泰伸; 内山秀樹; 中森健之; 山岡和貴; BLANDFORD Roger; MADEJSKI Grzegorz; 田代信; 寺田幸功; 山田真也; 湯浅孝行; 米徳大輔; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois
日本天文学会年会講演予稿集, Volume：2015, First page：256, 20 Aug. 2015
Japanese
ISSN：1347-0639, J-Global ID：201502208558523514 - ASTRO‐H衛星搭載硬X線撮像検出器(HXI)の現状打上げに向けて
中澤知洋; 国分紀秀; 佐藤悟朗; 萩野浩一; 太田方之; 小高裕和; 川原田円; 佐藤理江; 高橋忠幸; 武田伸一郎; 原山淳; 渡辺伸; 榎戸輝揚; 田中孝明; 寺田幸功; 内山秀樹; 谷津陽一; 中野俊男; 牧島一夫; 田島宏康; 山岡和貴; 大野雅功; 勝田隼一郎; 高橋弘充; 深沢泰司; 水野恒史; 中森健之; 野田博文; 湯浅孝行; 内山泰伸; 斉藤新也; 片岡淳; LAURENT Philippe; LEBRUN Francois; LIMOUSIN Olivier
日本天文学会年会講演予稿集, Volume：2015, First page：255, 20 Aug. 2015
Japanese
ISSN：1347-0639, J-Global ID：201502209587792610 - The 14th Marcel Grossmann Meeting, BN4 session, “End of white dwarfs; Observations and Theories of type Ia Supernova explorations and White Dwarfs near the Chandrasekhar limit”, Rome Italy, SOC session chair
12 Jul. 2015
国際会議、第14回 Marcel Grossmann Meeting で開催された BN4セッションの Session Chair - Session Chair of The 15th Marcel Grossmann Meeting, Session "End of white dwarfs an type Ia Supernova"
12 Jul. 2015
国際会議、第15回 Marcel Grossmann Meeting で開催された BN4セッションの Session Chair - ASTRO‐H衛星搭載硬X線撮影検出器(HXI)の現状FMの完成
中澤知洋; 国分紀秀; 佐藤悟朗; 川原田円; 佐藤理江; 渡辺伸; 高橋忠幸; 太田方之; 小高裕和; 武田伸一郎; 原山淳; 斉藤新也; 湯浅孝行; 谷津陽一; 内山秀樹; 田島宏康; 山岡和貴; 深沢泰司; 水野恒史; 大野雅功; 高橋弘充; 勝田隼一郎; 寺田幸功; 牧島一夫; 片岡淳; 野田博文; 榎戸輝揚; 田中孝明; 内山泰伸; 中森健之; LIMOUSIN Olivier; LAURENT Philippe; LEBRUN Francois; 櫻井壮希; 笹野理; 中野俊男; 小林翔悟; 村上浩章; 小野光; 加藤佑一
日本天文学会年会講演予稿集, Volume：2015, First page：262, 20 Feb. 2015
Japanese
ISSN：1347-0639, J-Global ID：201502250152467376 - 23pDK-3 Test results of flight models for Soft Gamma-ray Detector on board ASTRO-H
Tajima Hiroyasu; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Francois; SGD team
Meeting Abstracts of the Physical Society of Japan, Volume：70, First page：470, Last page：470, 2015
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.70.1.0_470
DOI ID：10.11316/jpsgaiyo.70.1.0_470, ISSN：2189-079X, CiNii Articles ID：110009990626, CiNii Books ID：AA12721570 - 25pSJ-3 Results of ight integration test for Soft Gamma-ray Detector on board ASTRO-H
Hayashi K.; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Francois; SGD team
Meeting Abstracts of the Physical Society of Japan, Volume：70, First page：351, Last page：351, 2015
The Physical Society of Japan, Japanese
DOI：https://doi.org/10.11316/jpsgaiyo.70.2.0_351
DOI ID：10.11316/jpsgaiyo.70.2.0_351, ISSN：2189-079X, CiNii Articles ID：110010028590, CiNii Books ID：AA12721570 - A COSPAR Capacity Building Workshop (メキシコ) 講師
16 Nov. 2014
国際宇宙空間研究委員会（COSPAR)主催の Workshop で、海外大学院生・PDを対象にした講義の講師 - 18pSB-8 CTA Report 80 : Calibration of PMTs for the CTA Large-Sized Telescopes
Takahashi Mitsunari; Inome Yusuke; Umetsu Yohei; Ohoka Hideyuki; Ogino Momoko; Orito Reiko; Katagiri Hideaki; Kushida Junko; Kubo Hidetoshi; Gunji Shuichi; Koyama Shu; Sawada Makoto; Tsujimoto Shimpei; Tsubone Yoshio; Teshima Masahiro; Terada Yukikatsu; Tomono Yayoi; Nakajima Daisuke; Nagayoshi Tsutomu; Nishijima Kyoshi; Hanabata Yoshitaka; Hayashida Masaaki; Bamba Aya; Matsuoka Shunsuke; Yamamoto Tokonatsu; CTA-Japan Consortium
Meeting abstracts of the Physical Society of Japan, Volume：69, Number：2, First page：33, Last page：33, 22 Aug. 2014
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110009873412, CiNii Books ID：AA11439205 - ASTRO‐H衛星搭載硬X線撮像検出器(HXI)開発の現状
佐藤悟朗; 国分紀秀; 中澤知洋; 高橋忠幸; 渡辺伸; 川原田円; 太田方之; 佐藤理江; 武田伸一郎; 小高裕和; 湯浅孝行; 林克洋; 原山淳; 牧島一夫; 野田博文; 片岡淳; 谷津陽一; 中森健之; 内山秀樹; 田島宏康; 山岡和貴; 深沢泰司; 水野恒史; 高橋弘充; 大野雅功; 寺田幸功; 榎戸輝揚; 田中孝明; 内山泰伸; LIMOUSIN Olivier; LAURENT Philippe; LEBRUN Francois
日本天文学会年会講演予稿集, Volume：2014, First page：275, 20 Feb. 2014
Japanese
ISSN：1347-0639, J-Global ID：201402254053457030 - ASTRO‐H衛星搭載軟ガンマ線検出器(SGD)開発の現状
大野雅功; 田島宏康; 深沢泰司; 渡辺伸; 高橋弘充; 田中康之; 水野恒史; 太田方之; 小高裕和; 川原田円; 国分紀秀; 佐藤理江; 高橋忠幸; 武田伸一郎; 原山淳; 林克洋; 森國城; 湯浅孝行; 佐藤悟朗; 中澤知洋; 野田博文; 牧島一夫; 田中孝明; 榎戸輝揚; 山田真也; 片岡淳; 谷津陽一; 内山泰伸; 内山秀樹; 中森健之; 山岡和貴; BLANDFORD Roger; MADEJSKI Grzegorz; 田代信; 寺田幸功; 米徳大輔; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois
日本天文学会年会講演予稿集, Volume：2014, First page：276, 20 Feb. 2014
Japanese
ISSN：1347-0639, J-Global ID：201402294281184585 - Si/CdTe半導体コンプトンカメラによるsub‐MeV全天観測構想
中澤知洋; 高橋忠幸; 渡辺伸; 国分紀秀; 一戸悠人; 武田伸一郎; 高島健; 三谷烈史; 田代信; 寺田幸功; 玉川徹; 榎戸輝揚; 能町正治; 羽島宏康; 深沢泰司; 水野恒史; 内山泰伸
日本天文学会年会講演予稿集, Volume：2014, First page：277, 20 Feb. 2014
Japanese
ISSN：1347-0639, J-Global ID：201402231095448228 - Expected Hard X-Ray and Soft Gamma-Ray from Supernovae
Keiichi Maeda; Yukikatsu Terada; Aya Bamba
16 Feb. 2014
High energy emissions from supernovae (SNe), originated from newly formed
radioactive species, provide direct evidence of nucleosynthesis at SN
explosions. However, observational difficulties in the MeV range have so far
allowed the signal detected only from the extremely nearby core-collapse SN
1987A. No solid detection has been reported for thermonuclear SNe Ia, despite
the importance of the direct confirmation of the formation of 56Ni, which is
believed to be a key ingredient in their nature as distance indicators. In this
paper, we show that the new generation hard X-ray and soft gamma-ray
instruments, on board Astro-H and NuStar, are capable of detecting the signal,
at least at a pace of once in a few years, opening up this new window for
studying SN explosion and nucleosynthesis.
Technical report
DOI：https://doi.org/10.14311/APP.2014.01.0205
DOI ID：10.14311/APP.2014.01.0205, arXiv ID：arXiv:1402.3759 - 29pTK-6 Development status of the Hard X-ray Imager (HXI) onboard ASTRO-H
Kawaharada Madoka; Odaka Hirokazu; Kataoka Jun; Sato Rie; Harayama Atsushi; Takahashi Tadayuki; Takahashi Hiromitsu; Takeda Shin'ichiro; Tajima Hiroyasu; Tanaka Takaaki; Terada Yukikatsu; Kokubun Motohide; Fukazawa Yasushi; Makishima Kazuo; Mizuno Tsunefumi; Yatsu Yoichi; Yamaoka Kazutaka; Yuasa Takayuki; Watanabe Shin; Laurent Philippe; Lebrun Francois; Limousin Olivier; Nakazawa Kazuhiro; the HXI team; Sato Goro; Uchiyama Hideki; Uchiyama Yasunobu; Enoto Teruaki; Ohta Masayuki; Ohno Masanori
Meeting Abstracts of the Physical Society of Japan, Volume：69, Number：1, First page：129, Last page：129, 2014
The Physical Society of Japan, Japanese
DOI ID：10.11316/jpsgaiyo.69.1.1.0_129_2, ISSN：1342-8349, CiNii Articles ID：110009834029, CiNii Books ID：AA11439205 - The Astro-H mission
Yoshitomo Maeda; Tadayuki Takahashi; Kazuhisa Mitsuda; Richard Kelley
Acta Polytechnica, Volume：53, First page：803, Last page：806, 01 Dec. 2013
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 ΔE~4÷7eV of SXS. Using the unique powers of these instruments, ASTRO-H will address unresolved issues in high-energy astrophysics. © Czech Technical University in Prague, 2013.
DOI：https://doi.org/10.14311/AP.2013.53.0803
DOI ID：10.14311/AP.2013.53.0803, ISSN：1210-2709, SCOPUS ID：84896805246 - Local Organizing Comittee of the 66th Fujiwara seminor, X-raying the Gamma-ray Universe
04 Nov. 2013
国際会議LOC。参加者 80名(半数国外)。 - A COSPAR Capacity Building Workshop (中国) 講師
02 Sep. 2013
国際宇宙空間研究委員会（COSPAR)主催の Workshop で、海外大学院生・PDを対象にした講義の講師 - CTA60 : Developing of the photon detector of LST camera
Nagayoshi T; Inome Y; Ueno H; Ohoka H; Ogino M; Orito R; Katagiri H; Kusida J; Kubo H; Gunji S; Koyama S; Sasaki H; Sawada M; Takahashi M; Tanaka S; Teshima M; Tsujimoto S; Tsubone Y; Terada Y; Nakajima D; Nishijima K; Hanabata Y; Hayashida M; Bamba A; Yamamoto T; CTA-Japan Consortium
Meeting abstracts of the Physical Society of Japan, Volume：68, Number：2, First page：104, Last page：104, 26 Aug. 2013
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110009754498, CiNii Books ID：AA11439205 - ASTRO‐H衛星搭載硬X線撮像検出器(HXI)の現状~FM製造の現状と予想性能~
中澤知洋; 国分紀秀; 川原田円; 佐藤悟朗; 牧島一夫; 渡辺伸; 高橋忠幸; 佐藤理江; 太田方之; 小高裕和; 武田伸一郎; 湯浅孝行; 中森健之; 片岡淳; 谷津陽一; 内山秀樹; 田島宏康; 山岡和貴; 深沢泰司; 水野恒史; 大野雅功; 高橋弘充; 寺田幸功; 榎戸輝揚; 田中孝明; 内山泰伸; LIMOUSIN Olivier; LAURENT Philippe; LEBRUN Francois
日本天文学会年会講演予稿集, Volume：2013, First page：293, 20 Aug. 2013
Japanese
ISSN：1347-0639, J-Global ID：201302255232876258 - すざく衛星搭載広帯域全天モニタによる太陽フレア観測
大野雅功; 高木勝俊; 河野貴文; 中村竜; 古井俊也; 深沢泰司; 安田哲也; 石田勇介; 上野遥; 杉本樹信; 遠藤輝; 坂本明弘; 丸谷美恵; 寺田幸功; 田代信; 石川真之介; 大森法輔; 秋山満; 山内誠; 山岡和貴; 杉田聡司; 中川友進; 国分紀秀; 高橋忠幸; 岩切渉; 花畑義隆; 浦田裕次; 中澤知洋; 牧島一夫
日本天文学会年会講演予稿集, Volume：2013, First page：115, 20 Aug. 2013
Japanese
ISSN：1347-0639, J-Global ID：201302239855201540 - 27pBE-5 Development of the Soft Gamma-ray Detector on board ASTRO-H (2^
harf of 2012)
Mizuno Tsunefumi; Blandford Rogor; Madojski Grzogorz; Laurent Philippe; Limousin Olivier; Lobrun Franoois; SGD team
Meeting Abstracts of the Physical Society of Japan, Volume：68, Number：1, First page：134, Last page：134, 2013
The Physical Society of Japan, Japanese
DOI ID：10.11316/jpsgaiyo.68.1.1.0_134_2, ISSN：1342-8349, CiNii Articles ID：110009642912, CiNii Books ID：AA11439205 - Development of Flight Model for Soft Gamma-ray Detector onboard ASTRO-H
Tajima Hiroyasu; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Frangois; the SGD team
Meeting Abstracts of the Physical Society of Japan, Volume：68, Number：2, First page：110, Last page：110, 2013
The Physical Society of Japan, Japanese
DOI ID：10.11316/jpsgaiyo.68.2.1.0_110_1, ISSN：1342-8349, CiNii Articles ID：110009754521, CiNii Books ID：AA11439205 - Development Status of the Hard X-ray Imager(HXI)for ASTRO-H
Sato G; Kataoka J; Kawaharada M; Sato R; Takahashi T; Takahashi H; Takeda S; Tajima H; Tanaka T; Terada Y; Fukazawa Y; Kokubun M; Makishima K; Mizuno T; Yatsu Y; Yamaoka K; Yuasa T; Watanabe S; Limousin O; Laurent P; Lebrun F; the HXI team; Nakazawa K; Uchiyama H; Uchiyama Y; Enoto T; Ohta M; Ohno M; Odaka H
Meeting Abstracts of the Physical Society of Japan, Volume：68, Number：2, First page：110, Last page：110, 2013
The Physical Society of Japan, Japanese
DOI ID：10.11316/jpsgaiyo.68.2.1.0_110_4, ISSN：1342-8349, CiNii Articles ID：110009754524, CiNii Books ID：AA11439205 - ASTRO‐H衛星搭載軟ガンマ線検出器(SGD)の開発現状
渡辺伸; 田島宏康; 深沢泰司; 太田方之; 小高裕和; 川原田円; 国分紀秀; 佐藤悟朗; 佐藤理江; 高橋忠幸; 武田伸一郎; 森國城; 湯浅孝行; 水野恒史; 高橋弘充; 大野雅功; 内山秀樹; 中澤知洋; 牧島一夫; 田中孝明; 榎戸輝揚; 山田真也; 片岡淳; 中森健之; 谷津陽一; 内山泰伸; BLANDFORD Roger; MADEJSKI Grzegorz; 田代信; 寺田幸功; 米徳大輔; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois
日本天文学会年会講演予稿集, Volume：2012, First page：275, 20 Aug. 2012
Japanese
ISSN：1347-0639, J-Global ID：201202250025785383 - The 13th Marcel Grossmann Meeting, BN4 session, “White Dwarf Pulsars and Rotating White Dwarf Theory”, Stockholm, SOC session chair
01 Jul. 2012
国際会議、第13回 Marcel Grossmann Meeting で開催された BN4セッションの Session Chair - The Digital Processing System for the Soft X-Ray Spectrometer Onboard ASTRO-H - The Design and the Performance
Yukikatsu Terada
IEEE Transactions on Nuclear Science, Volume：59, First page：366, Last page：372, 01 Apr. 2012
We report the design and the performance of the engineering model of the digital signal processing system called the Pulse Shape Processor (PSP) for the Soft X-ray Spectrometer (SXS) onboard the ASTRO-H satellite. The SXS employs an X-ray microcalorimeter system, in which X-ray photons are detected as a heat pulse due to photoelectric absorption. The pixelized HgTe absorbers are cooled down to 50 mK. The required energy resolution is 7 eV (FWHM) at 6 keV. Since the data link to the satellite data recorder is limited to 200 kbit s -1, the onboard digital processor PSP plays a critical role in achieving the required resolution. The PSP is also the rate-limiting factor for other performance of the SXS, such as maximum count rate and energy range. In this paper, we show the design of the PSP, and show the performance based on a series of laboratory tests performed with the engineering models of the detector and the analog readout electronics. We found that (1) the PSP can register energy in the 0.07-18 keV band [energy range], (2) the energy resolution of the engineering model system, including the detector, analog electronics, and the PSP, is 4.8-5.7 eV at 5.9 keV [energy resolution], and (3) the PSP has sufficient processing power to handle a point-like source fainter than 0.3 Crab [maximum count rate]. These results are expected to be quite similar to those with the flight model, thus the results will be useful for the observation planning using the SXS. © 2012 IEEE.
DOI：https://doi.org/10.1109/TNS.2011.2179671
DOI ID：10.1109/TNS.2011.2179671, ISSN：0018-9499, ORCID put code：67259950, SCOPUS ID：84859897783, Web of Science ID：WOS:000302953700015 - ASTRO‐H:衛星搭載軟ガンマ線検出器(SGD)の開発現状
渡辺伸; 田島宏康; 深沢泰司; 太田方之; 小高裕和; 川原田円; 国分紀秀; 佐藤悟朗; 高橋忠幸; 武田伸一郎; 森國城; 湯浅孝行; 水野恒史; 高橋弘充; 大野雅功; 内山泰伸; 榎戸輝揚; 田中孝明; BLANDFORD Roger; MADEJSKI Grzegarz; 内山秀樹; 中澤知洋; 牧島一夫; 片岡淳; 中森健之; 谷津陽一; 田代信; 寺田幸功; 山岡和貴; 山田真也; 米徳大輔; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois
日本天文学会年会講演予稿集, Volume：2012, First page：282, 20 Feb. 2012
Japanese
ISSN：1347-0639, J-Global ID：201202214865199942 - ASTRO‐H衛星搭載HXI/SGDの電源制御回路部(CPMU)の開発
原山淳; 川原田円; 渡辺伸; 太田方之; 国分紀秀; 高橋忠幸; 田島宏康; 深沢泰司; 中澤知洋; 片岡淳; 寺田幸功
日本天文学会年会講演予稿集, Volume：2012, First page：284, 20 Feb. 2012
Japanese
ISSN：1347-0639, J-Global ID：201202237729654180 - 14aSP-9 Developement and Status of the Soft Gamma-ray Detector onboard ASTRO-H
Fukazawa Y.; Kataoka J.; Kawaharada M.; Kokubun M.; Sato G.; Sato R.; Takahashi T; Takahashi H.; Takeda S.; Tashiro M.; Tanaka T.; Tajima H.; Terada Y.; Nakazawa K.; Nakamori T.; Makishima K.; Mizuno T.; Mori K.; Yatsu Y.; Yamada S.; Yuasa T.; Yonetoku D.; Watanabe S.; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Francois; the SGD team; Uchiyama H.; Uchiyama Y.; Enoto T.; Ohta M.; Ohno M.; Odaka H.
Meeting Abstracts of the Physical Society of Japan, Volume：67, Number：2, First page：119, Last page：119, 2012
The Physical Society of Japan, Japanese
DOI ID：10.11316/jpsgaiyo.67.2.1.0_119_1, ISSN：1342-8349, CiNii Articles ID：110009599801, CiNii Books ID：AA11439205 - 26pGJ-8 Development of Soft Gamma-ray Detector onboard ASTRO-H
Tajima Hiroyasu; Blandford Roger; Madejski Grzegorz; Laurent Philippe; Limousin Olivier; Lebrun Francois
Meeting Abstracts of the Physical Society of Japan, Volume：67, Number：1, First page：139, Last page：139, 2012
The Physical Society of Japan, Japanese
DOI ID：10.11316/jpsgaiyo.67.1.1.0_139_4, ISSN：1342-8349, CiNii Articles ID：110009565334, CiNii Books ID：AA11439205 - 26pGJ-3 Development status of the Hard X-ray Imager (HXI) onboard ASTRO-H
Kawaharada Madoka; Nakazawa Kazuhiro; Uchiyama Hideki; Makishima Kazuo; Mizuno Tsunefumi; Takahashi Hiromitsu; Ohno Masanori; Kataoka Jun; Nakamori Takeshi; Terada Yukikatsu; Kokubun Motohide; Yatsu Yoichi; Yamaoka Kazutaka; Tajima Hiroyasu; Tanaka Takaaki; Enoto Teruaki; Philippe Laurent; Francois Lebrun; Olivier Limousin; Sato Goro; Watanabe Shin; Tanaka Yasayuki; Ohta Masayuki; Yuasa Takayuki; Odaka Hirokazu; Takahashi Tadayuki
Meeting Abstracts of the Physical Society of Japan, Volume：67, Number：1, First page：138, Last page：138, 2012
The Physical Society of Japan, Japanese
DOI ID：10.11316/jpsgaiyo.67.1.1.0_138_4, ISSN：1342-8349, CiNii Articles ID：110009565330, CiNii Books ID：AA11439205 - Development of a Digital Signal Processing System for the X-Ray Microcalorimeter Onboard ASTRO-H (II)
Yukikatsu Terada
Journal of Low Temperature Physics, Volume：167, First page：575, Last page：581, 01 Jan. 2012
The Pulse Shape Processor is a digital signal processing electronics for the microcalorimeter instrument onboard ASTRO-H. Receiving digitized waveform (14 bit, 12.5 kHz sample) from 2×18 channels, two identical units of PSP-A and -B trigger X-ray events, assign five kinds of event grade, and perform optimal filtering to measure energy deposit on the 6 × 6 microcalorimeter pixels. One unit of PSP is composed of one FPGA board and two CPU boards. This paper describes the event processing algorithm to fulfill requirements for the signal processing, and task sharing between FPGA and CPU. © Springer Science+Business Media, LLC 2012.
DOI：https://doi.org/10.1007/S10909-012-0483-0
DOI ID：10.1007/S10909-012-0483-0, ISSN：0022-2291, ORCID put code：67259913, SCOPUS ID：84871778888, Web of Science ID：WOS:000303461600003 - ASTRO‐H搭載軟ガンマ線検出器(SGD)の開発現状
深沢泰司; 田島宏康; 渡辺伸; 水野恒史; 高橋弘充; 大野雅功; 内山泰伸; 榎戸輝揚; 田中孝明; 太田方之; 小高裕和; 川原田円; 国分紀秀; 佐藤悟朗; 高橋忠幸; 湯浅孝行; 武田伸一郎; 森國城; 内山秀樹; 中澤知洋; 牧島一夫; 片岡淳; 中森健之; 谷津陽一; 田代信; 寺田幸功; 山岡和貴; 米徳大輔; BLANDFORD Roger; MADEJSKI Grzegorz; LAURENT Philippe; LIMOUSIN Olivier; LEBRUN Francois
日本天文学会年会講演予稿集, Volume：2011, First page：303, 20 Aug. 2011
Japanese
ISSN：1347-0639, J-Global ID：201102207189370087 - モンテカルロシミュレーションを用いたASTRO‐H半導体コンプトンカメラの放射化バックグラウンドの評価(2)
平木一至; 水野恒史; 深沢泰司; 小高裕和; 佐藤有; 渡辺伸; 国分紀秀; 高橋忠幸; 中澤知洋; 下浦享; 中平聡志; 寺田幸功; 田島宏康
日本天文学会年会講演予稿集, Volume：2011, First page：304, 20 Aug. 2011
Japanese
ISSN：1347-0639, J-Global ID：201102220670117901 - ASTRO‐H HXI/SGD検出器搭載の高電圧電源部の開発
原山淳; 川原田円; 渡辺伸; 太田方之; 国分紀秀; 高橋忠幸; 田島宏康; 深沢泰司; 中澤知洋; 片岡淳; 寺田幸功
日本天文学会年会講演予稿集, Volume：2011, First page：303, 20 Aug. 2011
Japanese
ISSN：1347-0639, J-Global ID：201102287247725153 - 26aGS-11 X-ray Search for non-thermal emission from magnetic white dwarfs with hard spectra
Terada Y.; Harayama A.; Ishida M.; Dotani T.; Bamba A.; Hayashi T.; Urata Y.; Lin H.
Meeting abstracts of the Physical Society of Japan, Volume：66, Number：1, First page：110, Last page：110, 03 Mar. 2011
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110008610127, CiNii Books ID：AA11439205 - 27pGS-6 The status of development of the digital waveform processing system PSP in the soft X-ray spectrometer SXS onboard ASTRO-H
Shimoda Y.; Seta H.; Tashiro M.; Terada Y.; Yasuda T.; Takeda S.; Ishisaki Y.; Abe Y.; Tsujimoto M.; Mitsuda K.; Boyce Kevin; Matsuda K.; Masukawa K.
Meeting abstracts of the Physical Society of Japan, Volume：66, Number：1, First page：121, Last page：121, 03 Mar. 2011
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110008610164, CiNii Books ID：AA11439205 - 27pGS-7 Quantitivity of timing accuracy in the time distribution system on board ASTRO-H (2)
Kouzu T.; Iwase K.; Terada Y.; Mishima Y.; Tashiro M. S.; Ishisaki Y.; Yuasa T.; Nomachi M.; Takahashi T.; Kokubun M.; Ozaki M.; ASTRO-H collaborations
Meeting abstracts of the Physical Society of Japan, Volume：66, Number：1, First page：121, Last page：121, 03 Mar. 2011
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110008610165, CiNii Books ID：AA11439205 - ASTRO‐H衛星硬X線・軟ガンマ線検出器アクティブシールドの構造設計
中島健太; 中野俊男; 中澤知洋; 牧島一夫; 花畑義隆; 深沢泰司; 山岡和貴; 田島宏康; 片岡淳; 高橋弘充; 水野恒史; 大野雅功; 国分紀秀; 高橋忠幸; 渡辺伸; 田代信; 寺田幸功
日本物理学会講演概要集, Volume：66, Number：1, First page：122, 03 Mar. 2011
Japanese
ISSN：1342-8349, J-Global ID：201102253748599164 - ASTRO‐H衛星搭載軟ガンマ線検出器によるガンマ線バーストの観測
大野雅功; 渡辺伸; 川原田円; 太田方之; 佐藤有; 国分紀秀; 高橋忠幸; 田島宏康; 田中孝明; 榎戸輝揚; 深沢泰司; 高橋弘充; 花畑義隆; 松岡正之; 中澤知洋; 湯浅孝行; 中島健太; 西岡博之; 牧島一夫; 山岡和貴; 片岡淳; 中森健之; 吉野将生; 齋藤龍彦; 米徳大輔; 寺田幸功
日本物理学会講演概要集, Volume：66, Number：1, First page：34, 03 Mar. 2011
Japanese
ISSN：1342-8349, J-Global ID：201102271914408966 - CTA計画とCTA Japanの活動報告
井岡邦仁; 青野正裕; 浅野勝晃; 井上進; 井上芳幸; 榎本良治; 大石理子; 大岡秀行; 大平豊; 奥村曉; 折戸玲子; 格和純; 片桐秀明; 株木重人; 川中宣太; 木舟正; 窪秀利; 郡司修一; 郡和範; 榊直人; 柴田徹; 高橋慶太郎; 高橋弘充; 田島宏康; 田中真伸; 谷森達; 千川道幸; 千葉順成; 手嶋政廣; 寺田幸功; 当真賢二; 門叶冬樹; 戸谷友則; 内藤統也; 長滝重博; 中森健之; 西嶋恭司; 萩原亮太; 林田将明; 原敏
日本天文学会年会講演予稿集, Volume：2011, First page：230, 20 Feb. 2011
Japanese
ISSN：1347-0639, J-Global ID：201102204072428026 - 27pGS-8 R&D Status of the Soft Gamma-ray Detector (SGD) for ASTRO-H
Tanaka Takaaki; Takahashi Tadayuki; Takahashi Hiromitsu; Tajima Hiroyasu; Tashiro Makoto; Terada yukikatsu; Nakazawa Kazuhiro; Nakamori Takeshi; Fukazawa Yasushi; Blandford Roger; Makishima Kazuo; Uchiyama Yasunobu; Madejski Grzegorz; Mizuno Tsunefumi; Mori Kunishiro; Yatsu Yoichi; Yamaoka Kazutaka; Laurent Philippe; Limousin Olivier; Lebrun Francois; Watanabe Shin; Enoto Teruaki; Ohta Masayuki; Ohno Masanori; Kataoka Jun; Kawaharada Madoka; Kokubun Motohide; Sato Goro
Meeting Abstracts of the Physical Society of Japan, Volume：66, Number：1, First page：122, Last page：122, 2011
The Physical Society of Japan, Japanese
DOI ID：10.11316/jpsgaiyo.66.1.1.0_122_1, ISSN：1342-8349, CiNii Articles ID：110008610166, CiNii Books ID：AA11439205 - 18pSX-7 Developments of Soft Gamma-ray Detector on board the ASTRO-H satellite
Watanabe Shin; Kataoka Jun; Kawaharada Madoka; Kokubun Motohide; Sato Goro; Takahashi Hiromitsu; Takahashi Tadayuki; Tashiro Makoto; Tanaka Takaaki; Terada Yukikatsu; Nakazawa Kazuhiro; Tajima Hiroyasu; Nakamori Takeshi; Blandford Roger; Makishima Kazuo; Madeiski Grzegorz; Mizuno Tsunefumi; Mori Kunishiro; Yatsu Yoichi; Yuasa Takayuki; Laurent Philippe; Limousin Olivier; Fukazawa Yasushi; Lebrun Francois; ASTRO-H SGD team; Uchiyama Hideki; Uchiyama Yasunobu; Enoto Teruaki; Ohta Masayuki; Ohno Masanori; Odaka Hirokazu
Meeting Abstracts of the Physical Society of Japan, Volume：66, Number：2, First page：112, Last page：112, 2011
The Physical Society of Japan, Japanese
DOI ID：10.11316/jpsgaiyo.66.2.1.0_112_4, ISSN：1342-8349, CiNii Articles ID：110008757637, CiNii Books ID：AA11439205 - 26aGS-8 Suzaku observation of black hole candidate XTE J1752-223
Koyama S; Tashiro M. S; Terada Y; Seta H; Kubota A; Yamaoka K
Meeting Abstracts of the Physical Society of Japan, Volume：66, Number：0, 2011
一般社団法人 日本物理学会, Japanese
CiNii Articles ID：110008610124 - ASTRO‐H衛星硬X線・軟ガンマ線検出器アクティブシールドの機構開発
中島健太; 中澤知洋; 中野俊男; 西岡博之; 牧島一夫; 花畑義隆; 高橋弘充; 水野恒史; 深沢泰司; 山岡和貴; 田島宏康; 片岡淳; 大野雅功; 国分紀秀; 高橋忠幸; 渡辺伸; 田代信; 寺田幸功
日本天文学会年会講演予稿集, Volume：2010, First page：226, 20 Aug. 2010
Japanese
ISSN：1347-0639, J-Global ID：201002297490938422 - ASTRO‐H搭載半導体コンプトンカメラシステムのトリガーロジック及び信号処理ファームウェアの開発
大野雅功; 佐藤有; 渡辺伸; 川原田円; 太田方之; 田中康之; 小高裕和; 斉藤新也; 佐々木智香子; 福山太郎; 萩野浩一; 国分紀秀; 高橋忠幸; 田島宏康; 田中孝明; 榎戸輝揚; 深沢泰司; 高橋弘充; 花畑義隆; 中澤知洋; 湯浅孝行; 中島健太; 西岡博之; 牧島一夫; 山岡和貴; 片岡淳; 吉野将生; 米徳大輔; 寺田幸功
日本物理学会講演概要集, Volume：65, Number：2, First page：17, 18 Aug. 2010
Japanese
ISSN：1342-8349, J-Global ID：201002264320819598 - ASTRO‐H半導体コンプトンカメラの放射化バックグラウンド・モンテカルロシミュレータの開発とその評価
平木一至; 水野恒史; 深沢泰司; 小高裕和; 渡辺伸; 国分紀秀; 高橋忠幸; 中澤知洋; 下浦享; 中平聡志; 寺田幸功; 田島宏康
日本物理学会講演概要集, Volume：65, Number：2, First page：82, 18 Aug. 2010
Japanese
ISSN：1342-8349, J-Global ID：201002280860716521 - Response to the cosmic-ray heavy ion particles of hard X-ray and gamma-ray detectors on board the ASTRO-H satellite
国分紀秀; 渡辺伸; 太田方之; 佐藤悟郎; 岸下徹一; 勝田隼一郎; 小高裕和; 石川真之介; 古関優; 佐々木智香子; 斎藤新也; 福山太郎; 中澤知洋; 奥村暁; 山田真也; 鳥井俊輔; 中島健太; 片岡淳; 吉野将生; 三浦大陽; 寺田幸功; 原山淳; 中嶋大; 出原寿紘; 内堀幸夫; 北村尚
NIRS-M (Natl Inst Radiol Sci), Number：234, First page：270, Last page：271, Jun. 2010
Japanese
J-Global ID：201302245403129000 - 20pBP-13 Particle Acceleration mechanism in White Dwarfs via Multi-wave Simultaneous Campaign with Optical, X-ray, and TeV gamma-rays
Terada Y.; Harayama A.; Bamba A.; Ishida M.; Dotani T.; Hayashi T.; Nakamura R.; Makishima K.; Mukai K.; Nitta A.; Jager Okkie de; Chadwick Paula; Wagner Stefan; Buckley David
Meeting abstracts of the Physical Society of Japan, Volume：65, Number：1, First page：106, Last page：106, 01 Mar. 2010
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110007654206, CiNii Books ID：AA11439205 - 20aBP-1 Suzaku Observations of Magnetars-Neutron Stars with Ultra-Strong Magnetic Fields
Makishima K.; Enoto T.; Nakagawa Y.; Hayato A.; Terada Y.; Kouzu T.; Yamaoka K.; Yoshida A.; Ohno M.; Sakamoto T.; Suzaku Magnetar Team
Meeting abstracts of the Physical Society of Japan, Volume：65, Number：1, First page：102, Last page：102, 01 Mar. 2010
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110007654188, CiNii Books ID：AA11439205 - 20aBP-7 Quantitivity of timing accuracy in the time distribution system on board ASTRO-H
Kouzu T.; Terada Y.; Tashiro M. S.; Iwase K.; Yuasa T.; Nomachi M.; Ishisaki Y.; Takahashi T.; Kokubun M.; Ozaki M.; ASTRO-H collaborations
Meeting abstracts of the Physical Society of Japan, Volume：65, Number：1, First page：103, Last page：103, 01 Mar. 2010
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110007654192, CiNii Books ID：AA11439205 - ASTRO‐H衛星搭載硬X線・軟ガンマ線検出器アクティブシールドの開発(I):光読み出し
花畑義隆; 深沢泰司; 山岡和貴; 田島宏康; 片岡淳; 中澤知洋; 高橋弘充; 水野恒史; 大野雅功; 国分紀秀; 高橋忠幸; 渡辺伸; 田代信; 寺田幸功; 佐々木智香子; 中島健太; 水島翼
日本物理学会講演概要集, Volume：65, Number：1, First page：103, 01 Mar. 2010
Japanese
ISSN：1342-8349, J-Global ID：201002201347165644 - ASTRO‐H衛星搭載硬X線撮影検出器(HXI)の開発
国分紀秀; 渡辺伸; 太田方之; 佐藤理江; 大野雅功; 田中康之; 高橋忠幸; 中澤知洋; 牧島一夫; 深沢泰司; 水野恒史; 高橋弘充; 片岡淳; 寺田幸功; 山岡和貴; 田島宏康; 田中孝明
日本物理学会講演概要集, Volume：65, Number：1, First page：104, 01 Mar. 2010
Japanese
ISSN：1342-8349, J-Global ID：201002216547252883 - ASTRO‐H衛星硬X線・軟ガンマ線検出器アクティブシールドの開発(II):機構開発
中島健太; 中澤知洋; 西岡博之; 牧島一夫; 花畑義隆; 深沢泰司; 山崎和貴; 田島宏康; 片岡淳; 高橋弘充; 水野恒史; 大野雅功; 国分紀秀; 高橋忠幸; 渡辺伸; 田代信; 寺田幸功; 佐々木智香子; 水島翼
日本物理学会講演概要集, Volume：65, Number：1, First page：103, 01 Mar. 2010
Japanese
ISSN：1342-8349, J-Global ID：201002297783303073 - 次期X線天文衛星ASTRO‐H(ex‐NeXT)搭載硬X線イメージャ(HXI)の開発の現状(IV)
中澤知洋; 牧島一夫; 国分紀秀; 渡辺伸; 高橋忠幸; 深沢泰司; 片岡淳; 寺田幸功; 山岡和貴; 玉川徹; 田島宏康; OLIVIER Limousin; LAURENT Philippe; LEBRUN Francois
日本天文学会年会講演予稿集, Volume：2010, First page：252, 20 Feb. 2010
Japanese
ISSN：1347-0639, J-Global ID：201002200360947523 - モンテカルロシミュレーションを用いた次期X線天文衛星ASTRO‐H搭載軟ガンマ線検出器SGDの放射化バックグラウンドの評価
平木一至; 水野恒史; 深沢泰司; 梅木勇大; 小高裕和; 渡辺伸; 国分紀秀; 高橋忠幸; 中澤知洋; 中平聡志; 寺田幸功; 田島宏康
日本天文学会年会講演予稿集, Volume：2010, First page：255, 20 Feb. 2010
Japanese
ISSN：1347-0639, J-Global ID：201002206033454414 - 「すざく」衛星搭載硬X線検出器(HXD)主検出部の現状(IV)
西野翔; 深沢泰司; 高橋弘充; 水野恒史; 林克洋; 平木一至; 国分紀秀; 渡辺伸; 田中孝明; 中澤知洋; 山田真也; 川原田円; 寺田幸功
日本天文学会年会講演予稿集, Volume：2010, First page：264, 20 Feb. 2010
Japanese
ISSN：1347-0639, J-Global ID：201002224721077649 - 「すざく」衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状(IX)
山岡和貴; 田代信; 寺田幸功; 恩田香織; 遠藤輝; 岩切渉; 菅佐原たか子; 大野雅功; 鈴木素子; 国分紀秀; 高橋忠幸; 杉田聡司; 深沢泰司; 高橋拓也; 上原岳士; 花畑義隆; 山内誠; 園田絵里; 大森法輔; 河野健太; 林秀憲; 野田和宏; 大休寺新; 西岡祐介; 中澤知洋; 榎戸輝揚; 牧島一夫; 玉川徹; 中川友進; 浦田裕次; 林紅妙; VASQUEZ Nicolas; 洪秀徴; 村上敏夫; 田島宏康
日本天文学会年会講演予稿集, Volume：2010, First page：264, 20 Feb. 2010
Japanese
ISSN：1347-0639, J-Global ID：201002225747874004 - 「すざく」衛星搭載WAM検出器による太陽フレアに伴う硬X線の系統的解析
遠藤輝; 嶋森篤史; 田代信; 寺田幸功; 浦田裕次; 浦田裕次; 園田絵里; 山内誠; 山岡和貴; 深沢泰司; 大野雅功; 渡邉恭子; 杉田聡司; 簑島敬
Volume：2010, 2010
ISSN：1347-0639, J-Global ID：201002270585130109 - Suzaku X-Ray Imaging and Spectroscopy of Cassiopeia A
Yoshitomo Maeda; Yasunobu Uchiyama; Aya Bamba; Hiroko Kosugi; Hiroshi Tsunemi; Eveline A. Helder; Jacco Vink; Natsuki Kodaka; Yukikatsu Terada; Yasushi Fukazawa; Junko Hiraga; John P. Hughes; Motohide Kokubun; Tomomi Kouzu; Hironori Matsumoto; Emi Miyata; Ryoko Nakamura; Shunsaku Okada; Kentaro Someya; Toru Tamagawa; Keisuke Tamura; Kohta Totsuka; Yohko Tsuboi; Yuichiro Ezoe; Stephen S. Holt; Manabu Ishida; Tsuneyoshi Kamae; Robert Petre; Tadayuki Takahashi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, Number：6, First page：1217, Last page：1228, Dec. 2009
Suzaku X-ray observations of a young supernova remnant, Cassiopeia A, were carried out. K-shell transition lines from highly ionized ions of various elements were detected, including Chromium (Cr-K alpha at 5.61 keV). The X-ray continuum spectra were modeled in the 3.4-40keV band, summed over the entire remnant, and were fitted with a simplest combination of the thermal bremsstrahlung and the non-thermal cut-off power-law models. The spectral fits with this assumption indicate that the continuum emission is likely to be dominated by non-thermal emission with a cut-off energy at > 1 keV. The thermal-to-non thermal fraction of the continuum flux in the 4-10 keV band is best estimated as similar to 0.1. Non-thermal-dominated continuum images in the 4-14 keV band were made. The peak of the non-thermal X-rays appears at the western part. The peak position of the TeV gamma-rays measured with HEGRA and MAGIC is also shifted at the western part with the I-sigma confidence. Since the location of the X-ray continuum emission was known to be presumably identified with the reverse shock region, the possible keV-TeV correlations give a hint that the accelerated multi-TeV hadrons in Cassiopeia A are dominated by heavy elements in the reverse shock region.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/61.6.1217
DOI ID：10.1093/pasj/61.6.1217, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000273306300004 - Local Organizing Comittee of the 3rd Suzaku conference, entitled "the Energetic Cosmos, from Suzaku to ASTRO-H "
Sep. 2009
北海道小樽市にて開催した第三回「すざく」国際会議のLOC。300名参加、うち海外100名。LOC 主要メンバー代表として ISAS news (JAXA発行)にて報告。 - マグネター天体1E1547.0‐5408の「すざく」ToO観測
榎戸輝揚; 牧島一夫; 坂本貴紀; 中川友進; 山岡和貴; 大野雅功; 高橋忠幸; 中澤知洋; 高橋弘充; 村上敏夫; 寺田幸功
日本天文学会年会講演予稿集, Volume：2009, First page：74, 20 Aug. 2009
Japanese
ISSN：1347-0639, J-Global ID：200902208021437931 - 10aSD-11 Development status of the Soft X-ray Spectrometer (SXS) onboard Astro-H (II)
Fujimoto Ryuichi; Sato Kosuke; Mitsuda Kazuhisa; Yamasaki Noriko; Takei Yoh; Tsujimoto Masahiro; Sugita Hiroyuki; Sato Yoichi; Shinozaki Keisuke; Ohashi Takaya; Ishisaki Yoshitaka; Ezoe Yuichiro; Murakami Masahide; Tashiro Makoto; Terada Yukikatsu; Tamagawa Toru; Mihara Tatehiro; Kawaharada Madoka; Yamaguchi Hiroya; Kitamoto Shunji; Murakami Hiroshi; Kelley R.L; Kilbourne C.A; Porter F.S; McCammon D; den Herder J.-W
Meeting abstracts of the Physical Society of Japan, Volume：64, Number：2, 18 Aug. 2009
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110007501526 - Broad-band properties of the hard X-ray cataclysmic variables IGR J00234+6141 and 1RXS J213344.1+510725
G. Anzolin; D. de Martino; M. Falanga; K. Mukai; J. -M. Bonnet-Bidaud; M. Mouchet; Y. Terada; M. Ishida
ASTRONOMY & ASTROPHYSICS, Volume：501, Number：3, First page：1047, Last page：1058, Jul. 2009
Context. A significant number of cataclysmic variables have been detected as hard X-ray sources in the INTEGRAL survey, most of them of the magnetic intermediate polar type.
Aims. We present a detailed X-ray broad-band study of two new sources, IGR J00234+6141 and 1RXS J213344.1+510725, that allow us to classify them as secure members of the intermediate polar class.
Methods. Timing and spectral analysis of IGR J00234+6141 are based on an XMM-Newton observation and INTEGRAL publicly available data. For 1RXS J213344.1+510725, we use XMM-Newton and Suzaku observations at different epochs, as well as INTEGRAL publicly available data.
Results. We determine a spin period of 561.64 +/- 0.56 s for the white dwarf in IGR J00234+6141. The X-ray pulses are observed up to similar to 2 keV. From XMM-Newton and Suzaku observations of 1RXS J213344.1+510725, we find a rotational period of 570.862 +/- 0.034 s. The observations span three epochs where the pulsation is observed to change at different energies both in amplitude and shape. In both objects, the spectral analysis spanned over a wide energy range, from 0.3 to 100 keV, shows the presence of multiple emission components absorbed by dense material. The X-ray spectrum of IGR J00234+6141 is consistent with a multi-temperature plasma with a maximum temperature of similar to 50 keV. In 1RXS J213344.1+510725, multiple optically thin components are inferred, as well as an optically thick (blackbody) soft X-ray emission with a temperature of similar to 100 eV. This adds 1RXS J213344.1+510725 to the growing group of soft X-ray intermediate polars.
Conclusions. Though showing similar rotational periods and being hard X-ray sources, these two intermediate polars appear different in several respects, among which the presence of a soft X-ray component in 1RXS J213344.1+510725. This source also emits circularly polarized light in the optical band, thus joining the group of soft and polarized intermediate polars as a fifth member. How the hard X-ray and polarized emission are thermalized in these systems is a timely question.
EDP SCIENCES S A, English
DOI：https://doi.org/10.1051/0004-6361/200911816
DOI ID：10.1051/0004-6361/200911816, ISSN：1432-0746, Web of Science ID：WOS:000268292200019 - Search for Sc-K Line Emission from RX J0852.0-4622 Supernova Remnant with Suzaku
Junko S. Hiraga; Yusuke Kobayashi; Toru Tamagawa; Asami Hayato; Aya Bamba; Yukikatsu Terada; Robert Petre; Hideaki Katagiri; Hiroshi Tsunemi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, Number：2, First page：275, Last page：281, Apr. 2009
We searched for evidence of line emission around 4 keV from the northwestern rim of the supernova remnant RX J0852.0-4622 using Suzaku XIS data. Several papers have reported on the detection of an emission line around 4.1 keV from this region of the sky. This line Would arise from K-band fluorescence by Sc-44, the immediate decay product of Ti-44. We performed spectral analysis for the entire portion of the NW rim of the remnant within the XIS field of view, as well as various regions corresponding to regions of published claims of line emission. We found no line emission around 4.1 keV anywhere, and are able to set a restrictive Upper limit to the X-ray flux: 1.1 x 10(-6) s(-1) cm(-2) for the entire field. For every region, our flux upper limit falls below that of the previously claimed detection. Therefore, we conclude that, to date, no definite X-ray line feature from Sc-K emission has been detected in the NW rim of RX J0852.0-4622. Our negative-detection supports the recent claim that RX J0852-4622 is neither young (1700-4000 yr) nor nearby (similar to 750 pc).
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/61.2.275
DOI ID：10.1093/pasj/61.2.275, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000266228300012 - Search for Sc-K Line Emission from RX J0852.0-4622 Supernova Remnant with Suzaku
Junko S. Hiraga; Yusuke Kobayashi; Toru Tamagawa; Asami Hayato; Aya Bamba; Yukikatsu Terada; Robert Petre; Hideaki Katagiri; Hiroshi Tsunemi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, Number：2, First page：275, Last page：281, Apr. 2009
We searched for evidence of line emission around 4 keV from the northwestern rim of the supernova remnant RX J0852.0-4622 using Suzaku XIS data. Several papers have reported on the detection of an emission line around 4.1 keV from this region of the sky. This line Would arise from K-band fluorescence by Sc-44, the immediate decay product of Ti-44. We performed spectral analysis for the entire portion of the NW rim of the remnant within the XIS field of view, as well as various regions corresponding to regions of published claims of line emission. We found no line emission around 4.1 keV anywhere, and are able to set a restrictive Upper limit to the X-ray flux: 1.1 x 10(-6) s(-1) cm(-2) for the entire field. For every region, our flux upper limit falls below that of the previously claimed detection. Therefore, we conclude that, to date, no definite X-ray line feature from Sc-K emission has been detected in the NW rim of RX J0852.0-4622. Our negative-detection supports the recent claim that RX J0852-4622 is neither young (1700-4000 yr) nor nearby (similar to 750 pc).
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/61.2.275
DOI ID：10.1093/pasj/61.2.275, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000266228300012 - 28pSH-6 Development of the signal processing system for the X-ray microcalorimeter onboard ASTRO-H
Seta Hiromi; Tashiro Makoto; Terada Yukikatsu; Onda Kaori; Shimoda Yuuya; Ishisaki Yoshitaka; Takei Yoh; Mitsuda Kazuhisa; ASTRO-H SXS team
Meeting abstracts of the Physical Society of Japan, Volume：64, Number：1, First page：93, Last page：93, 03 Mar. 2009
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110007370071, CiNii Books ID：AA11439205 - 28pSH-5 Development of mirocalorimeter SXS designed for ASTRO-H
Takei Y; Mitsuda K; Yamasaki N; Tsujimoto M; Shinozaki K; Sugita H; Sato Y; Fujimoto R; Sato K; Ohashi T; Ishisaki Y; Ezoe Y; Murakami M; Tashiro M. S; Terada Y; Tamagawa T; Mihara T; Kawaharada M; Yamaguchi H; Kitamoto S; Murakami H; Kelley Richard L; Kilbourne C. A; Porter F. S; Shirron P. J; DiPirro M. J; Sneiderman Gary A; McCammon D; Herder J.-W. den; ASTRO-H SXS tea
Meeting abstracts of the Physical Society of Japan, Volume：64, Number：1, 03 Mar. 2009
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110007370070 - SpaceWire I/Fを用いた衛星内時刻配信の検証
湯浅孝行; 中澤知洋; 牧島一夫; 高橋忠幸; 能町正治; 高島健; 国分紀秀; 小高裕和; 寺田幸功; 藤代巌; 程島文夫; 田苗明; 遠山正明
日本物理学会講演概要集, Volume：64, Number：1, First page：93, 03 Mar. 2009
Japanese
ISSN：1342-8349, J-Global ID：200902286009410484 - 次期X線天文衛星ASTRO‐H(ex‐NeXT)搭載硬X線イメージャ(HXI)の開発の現状(III)
中澤知洋; 牧島一夫; 国分紀秀; 渡辺伸; 高橋忠幸; 深沢泰司; 片岡淳; 寺田幸功; 山岡和貴; 玉川徹; 田島宏康
日本天文学会年会講演予稿集, Volume：2009, First page：260, 20 Feb. 2009
Japanese
ISSN：1347-0639, J-Global ID：200902276984213570 - 「すざく」衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状(VII)
大野雅功; 国分紀秀; 鈴木素子; 高橋忠幸; 田代信; 寺田幸功; 浦田裕次; 恩田香織; 遠藤輝; 小高夏来; 守上浩市; 岩切渉; 菅佐原たか子; 山岡和貴; 杉田聡司; 玉川徹; 中川友進; 深沢泰司; 高橋拓也; 上原岳士; 吉良知恵; 花畑義隆; 中澤知洋; 榎戸輝揚; 牧島一夫; 洪秀徴; 山内誠; 園田絵里; 田中裕基; 原龍児; 大森法輔; 河野健太; 林秀憲; 田島宏康
日本天文学会年会講演予稿集, Volume：2009, First page：253, 20 Feb. 2009
Japanese
ISSN：1347-0639, J-Global ID：200902296985521636 - Design and In-Orbit Performance of the Suzaku Wide-Band All-Sky Monitor
Kazutaka Yamaoka; Akira Endo; Teruaki Enoto; Yasushi Fukazawa; Ryuji Hara; Yoshitaka Hanabata; Soojing Hong; Tsuneyoshi Kamae; Chie Kira; Natsuki Kodaka; Motohide Kokubun; Shouta Maeno; Kazuo Makishima; Ryohei Miyawaki; Kouichi Morigami; Toshio Murakami; Yujin E. Nakagawa; Kazuhiro Nakazawa; Norisuke Ohmori; Masanori Ohno; Kaori Onda; Goro Sato; Eri Sonoda; Satoshi Sugita; Masanobu Suzuki; Motoko Suzuki; Hiroyasu Tajima; Tadayuki Takahashi; Takuya Takahashi; Hiroki Tanaka; Tohru Tamagawa; Makoto S. Tashiro; Yukikatsu Terada; Takeshi Uehara; Yuji Urata; Makoto Yamauchi; Atsumasa Yoshida; Kevin Hurley; Valentin PaL'Shin; Takanori Sakamoto; Jay Cummings
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, First page：S35, Last page：S53, Jan. 2009
The Suzaku Wide-band All-sky Monitor (WAM) consists of thick BGO anti-coincidence shields of the Hard X-ray Detectors (HXD). It views about half of the sky and has a geometrical area of 800 cm(2) per side and an effective area of 400 cm(2), even at 1 MeV. Hence, the WAM can provide unique opportunities to detect high-energy emission from GRBs and solar flares in the sub-MeV to MeV range. The WAM has detected more than 400 GRBs and 100 solar flares since its launch. This paper describes the in-flight performance of the HXD/WAM during the initial two years of operations, including the in-flight energy response, spectral and timing capabilities, and in-orbit background.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/61.sp1.S35
DOI ID：10.1093/pasj/61.sp1.S35, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000264418100004 - Suzaku Observations of Tycho's Supernova Remnant
T. Tamagawa; A. Hayato; S. Nakamura; Y.Terada; A. Bamba; J. S. Hiraga; J. P.Hughes; U. Hwang; J. Kataoka; K. Kinugasa; H. Kunieda; T. Tanaka; H. Tsunemi; M. Ueno; S. S. Holt; M. Kokubun; E. Miyata; A. Szymkowiak; T. Takahashi; K. Tamura; D. Ueno
Volume：61, Number：Sp. Iss. 1, First page：S167-172, 2009 - Suzaku Observations of SS Cygni in Quiescence and Outburst
Manabu Ishida; Shunsaku Okada; Takayuki Hayashi; Ryoko Nakamura; Yukikatsu Terada; Koji Mukai; Kenji Hamaguchi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, First page：S77, Last page：S91, Jan. 2009
We present results from the Suzaku observations of the dwarf nova SS Cyg in quiescence and outburst in 2005 November. The high sensitivity of the HXD PIN and the high spectral resolution of the XIS enabled us to determine the plasma parameters with unprecedented precision. The maximum temperature of the plasma in quiescence, 20.4(-2.6)(+4.0) (stat) +/- 3.0 (sys) keV, is significantly higher than that in outburst, 6.0(-1.3)(+0.2) keV. The elemental abundances are close to the solar ones for medium-Z elements (Si, S, Ar), whereas they decline both in lighter and heavier elements, except for that of carbon, which is 2 solar, at least. The solid angle of the reflector subtending over an optically thin thermal plasma is Omega(Q)/(2 pi) = 1.7 +/- 0.2 (stat) +/- 0.1 (sys) in quiescence. A 6.4 keV iron K alpha line is resolved into narrow and broad components. These facts indicate that both the white dwarf and the accretion disk contribute to the reflection. We consider the standard optically thin boundary layer as being the most plausible picture for the plasma configuration in quiescence. The solid angle of the reflector in outburst, Omega(O) (2 pi) = 0.9(-0.4)(+0.5), and a broad 6.4 keV iron line indicate that the reflection in outburst originates from the accretion disk and an equatorial accretion belt. The broad 6.4 keV line suggests that the optically thin thermal plasma is distributed on the accretion disk like solar corona.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/61.sp1.S77
DOI ID：10.1093/pasj/61.sp1.S77, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000264418100007 - Design and In-Orbit Performance of the Suzaku Wide-Band All-Sky Monitor
Kazutaka Yamaoka; Akira Endo; Teruaki Enoto; Yasushi Fukazawa; Ryuji Hara; Yoshitaka Hanabata; Soojing Hong; Tsuneyoshi Kamae; Chie Kira; Natsuki Kodaka; Motohide Kokubun; Shouta Maeno; Kazuo Makishima; Ryohei Miyawaki; Kouichi Morigami; Toshio Murakami; Yujin E. Nakagawa; Kazuhiro Nakazawa; Norisuke Ohmori; Masanori Ohno; Kaori Onda; Goro Sato; Eri Sonoda; Satoshi Sugita; Masanobu Suzuki; Motoko Suzuki; Hiroyasu Tajima; Tadayuki Takahashi; Takuya Takahashi; Hiroki Tanaka; Tohru Tamagawa; Makoto S. Tashiro; Yukikatsu Terada; Takeshi Uehara; Yuji Urata; Makoto Yamauchi; Atsumasa Yoshida; Kevin Hurley; Valentin PaL'Shin; Takanori Sakamoto; Jay Cummings
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, First page：S35, Last page：S53, Jan. 2009
The Suzaku Wide-band All-sky Monitor (WAM) consists of thick BGO anti-coincidence shields of the Hard X-ray Detectors (HXD). It views about half of the sky and has a geometrical area of 800 cm(2) per side and an effective area of 400 cm(2), even at 1 MeV. Hence, the WAM can provide unique opportunities to detect high-energy emission from GRBs and solar flares in the sub-MeV to MeV range. The WAM has detected more than 400 GRBs and 100 solar flares since its launch. This paper describes the in-flight performance of the HXD/WAM during the initial two years of operations, including the in-flight energy response, spectral and timing capabilities, and in-orbit background.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/61.sp1.S35
DOI ID：10.1093/pasj/61.sp1.S35, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000264418100004 - The Nature of a Cosmic-Ray Accelerator, CTB 37 B, Observed with Suzaku and Chandra
Ryoko Nakamura; Aya Bamba; Manabu Ishida; Hiroshi Nakajima; Ryo Yamazaki; Yukikatsu Terada; Gerd Puehlhofer; Stefan J. Wagner
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, First page：S197, Last page：S207, Jan. 2009
We report on Suzaku and Chandra observations of the young supernova remnant CTB 37 B, from which TeV gamma-rays were detected by the H.E.S.S. Cherenkov telescope. The 80 ks Suzaku observation provided us with a clear image of diffuse emission and high-quality spectra. The spectra revealed that the diffuse emission is comprised of thermal and non-thermal components. The thermal component can be represented by an NEI model with a temperature, a pre-shock electron density and an age of 0.9 +/- 0.2 keV, 0.4 +/- 0.1 cm(-3), and 650(-300)(+2500) yr, respectively. This suggests that the explosion of CTB 37 B occurred ill a low-density space. A non-thermal power-law component was found from the southern region of CTB 37 B. Its photon index of similar to 1.5 and a high roll-off energy (greater than or similar to 15 keV) indicate efficient cosmic-ray acceleration. A comparison of this X-ray spectrum with the TeV gamma-ray spectrum leads us to conclude that the TeV gamma-ray emission seems to be powered by either multi-zone Inverse Compton scattering or the decay of neutral pions. The point source resolved by Chandra near the shell is probably associated with CTB 37 B, because of the common hydrogen column density with the diffuse thermal emission. Spectral and temporal characteristics Suggest that this source is a new anomalous X-ray pulsar.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/61.sp1.S197
DOI ID：10.1093/pasj/61.sp1.S197, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000264418100020 - Modeling and Reproducibility of Suzaku HXD PIN/GSO Background
Yasushi Fukazawa; Tsunefumi Mizuno; Shin Watanabe; Motohide Kokubun; Hiromitsu Takahashi; Naomi Kawano; Sho Nishino; Mahito Sasada; Hirohisa Shirai; Takuya Takahashi; Yudai Umeki; Tomonori Yamasaki; Tomonori Yasuda; Aya Bamba; Masanori Ohno; Tadayuki Takahashi; Masayoshi Ushio; Teruaki Enoto; Takao Kitaguchi; Kazuo Makishima; Kazuhiro Nakazawa; Yuichi Uehara; Shin'ya Yamada; Takayuki Yuasa; Naoki Isobe; Madoka Kawaharada; Takaaki Tanaka; Makoto S. Tashiro; Yukikatsu Terada; Kazutaka Yamaoka
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, First page：S17, Last page：S33, Jan. 2009
Suzaku Hard X-ray Detector (HXD) achieved the lowest background level than any other previously or currently operational missions sensitive in the energy range of 10-600 keV, by utilizing PIN photodiodes and GSO scintillators; mounted in BGO active shields to reject particle background and Compton-scattered events as much as possible. Because it does not have an imaging capability nor rocking mode for the background monitor, the sensitivity is limited by the reproducibility of the non X-ray background (NXB) model. We modeled the HXD NXB, which varies with time as well as other satellites with a low-Earth orbit, by utilizing several parameters, including particle monitor counts and satellite orbital/attitude information, The model background is supplied as an event file in which the background events are generated by random numbers, and can be analyzed in the same way as the real data. The reproducibility of the NXB model depends on the event selection criteria (such as cut-off rigidity and energy band) and the integration time, and the 1 sigma systematic error is estimated to be less than 3% (PIN 15-40 keV) and 1% (GSO 50-100 keV) for more than 10 ks exposure.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/61.sp1.S17
DOI ID：10.1093/pasj/61.sp1.S17, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000264418100003 - Suzaku Observations of Tycho's Supernova Remnant
Toru Tamagawa; Asami Hayato; Satoshi Nakamura; Yukikatsu Terada; Aya Bamba; Junko S. Hiraga; John P. Hughes; Una Hwang; Jun Kataoka; Kenzo Kinugasa; Hideyo Kunieda; Takaaki Tanaka; Hiroshi Tsunemi; Masaru Ueno; Stephen S. Holt; Motohide Kokubun; Emi Miyata; Andrew Szymkowiak; Tadayuki Takahashi; Keisuke Tamura; Daisuke Ueno; Kazuo Makishima
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：61, Number：Sp. Iss. 1, First page：S167, Last page：S174, Jan. 2009
Tycho's supernova remnant was observed by the XIS and HXD instruments onboard the Suzaku satellite on 2006 June 26-29 for 92 ks. The spectrum up to 30 keV was well fitted with a two-component model, consisting of a power-law with a photon index of 2.7 and a thermal bremsstrahlung model with a temperature of 4.7 keV. The former component can alternatively be modeled as synchrotron emission from a population of relativistic electrons with an estimated roll-off energy of around 1 keV. In the XIS spectra, in addition to the prominent Fe K alpha line (6.445 keV), we observed for the first time significant K alpha line emission from trace species Cr and Mn at energies of 5.48 keV and 5.95 keV, respectively. Faint K beta lines from Ca (4.56 keV) and Fe (7.11 keV) were also seen. The ionization states of Cr and Mn, based on their line centroids, Lire estimated to be similar to that of Fe K alpha (Fe XV or XVI).
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/61.sp1.S167
DOI ID：10.1093/pasj/61.sp1.S167, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000264418100016 - 22pSH-4 Soft gamma-ray long-term earth occultation observations of black hole sources with Suzaku-WAM
Kira Chie; Fukazawa Yasushi; Takahashi Hiromitsu; Takahashi Takuya; Uehara Takeshi; Hanabata Yoshitaka; Yamaoka Kazuki; Tashiro Makoto; Ohno Masanori; Tamagawa Tohru; Terada Yukinori
Meeting abstracts of the Physical Society of Japan, Volume：63, Number：2, First page：89, Last page：89, 25 Aug. 2008
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110006982710, CiNii Books ID：AA11439205 - FOXSIロケット実験計画の概要
増田智; 簑島敬; 下条圭美; 寺田幸功; 高橋忠幸; 石川真之介; 国分紀秀; 渡辺伸; 田島宏康; 中澤知洋; 奥山翔; KRUCKER S; LIN R; CHRISTE S; RAMSEY B; GUBAREV M
日本天文学会年会講演予稿集, Volume：2008, First page：139, 20 Aug. 2008
Japanese
ISSN：1347-0639, J-Global ID：200902208961420131 - すざく衛星搭載WAMによるガンマ線バーストの広帯域高感度観測
大野雅功; 国分紀秀; 鈴木素子; 高橋忠幸; 山岡和貴; 杉田聡司; 田代信; 寺田幸功; 浦田裕次; 恩田香織; 遠藤輝; 鈴木正信; 小高夏来; 守上浩市; 岩切渉; 菅佐原たか子; 玉川徹; 中川友進; 深沢泰司; 高橋拓也; 上原岳士; 吉良知恵; 花畑義隆; 中澤知洋; 榎戸輝揚; 牧島一夫; 洪秀徴; 山内誠; 園田絵里; 田中裕基; 原龍児; 大森法輔; 田島宏康
日本天文学会年会講演予稿集, Volume：2008, First page：75, 20 Aug. 2008
Japanese
ISSN：1347-0639, J-Global ID：200902270078743858 - 「すざく」衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状(VI)
田代信; 寺田幸功; 浦田裕次; 恩田香織; 遠藤輝; 小高夏来; 守上浩市; 岩切渉; 菅佐原たか子; 大野雅功; 国分紀秀; 鈴木素子; 高橋忠幸; 山岡和貴; 杉田聡司; 玉川徹; 中川友進; 深沢泰司; 高橋拓也; 上原岳士; 吉良知恵; 花畑義隆; 中澤知洋; 榎戸輝揚; 牧島一夫; 洪秀徴; 山内誠; 園田絵里; 田中裕基; 原龍児; 大森法輔; 河野健太; 林秀憲; 田島宏康
日本天文学会年会講演予稿集, Volume：2008, First page：257, 20 Aug. 2008
Japanese
ISSN：1347-0639, J-Global ID：200902291725275290 - Suzaku discovery of hard X-ray pulsations from a rotating magnetized white dwarf, AE Aquarii
Yukikatsu Terada; Takayuki Hayashi; Manabu Ishida; Koji Mukai; Tadayasu Dotani; Shunsaku Okada; Ryoko Nakamura; Sachindra Naik; Aya Bamba; Kazuo Makishima
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, Number：2, First page：387, Last page：397, Apr. 2008
A fast rotating magnetized white dwarf, AE Aquarii, was observed with Suzaku, in 2005 October-November and 2006 October with exposures of 53.1 and 42.4ks, respectively. In addition to clear spin modulation in the 0.5-10 keV band of the XIS data at the barycentric period of 33.0769 +/- 0.0001 s, the 10-30 keV HXD data in the second half of the 2005 observation also showed statistically significant periodic signals at a consistent period. On that occasion, the spin-folded HXD light curve exhibited two sharp spikes separated by similar to 0.2 cycles in phase, in contrast to approximately sinusoidal profiles observed at energies below similar to 4 keV. The folded 4-10 keV XIS light curves are understood to be a superposition of those two types of pulse profiles. The phase-averaged 1.5-10 keV spectra can be reproduced by two thermal components with temperatures of 2.0(-0.16)(+0.20) keV and 0.53(-0.13)(+0.14) keV but the 12-25 keV HXD data show a significant excess above the extrapolated model. This excess can be explained by either a power-law model with a photon index of 1.12(-0.62)(+0.63) or a third thermal component with a temperature of 54(-47)(+26) keV. At a distance of 102pc, the 4-30keV luminosities of the thermal and the additional components become 1.7(-0.6)(+1.3) and 5.3(-0.3)(+15.3) X 10(29) erg s(-1), respectively. The latter corresponds to 0.09% of the spin-down energy of the object. Possible emission mechanisms of the hard pulsations are discussed, including non-thermal ones, in particular.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/60.2.387
DOI ID：10.1093/pasj/60.2.387, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000255818400025 - Suzaku observation of the anomalous X-ray pulsar CXOU J164710.2-455216
Sachindra Naik; Tadayasu Dotani; Nobuyuki Kawai; Motohide Kokubun; Takayasu Anada; Mikio Morii; Tatehiro Mihara; Teruaki Enoto; Madoka Kawaharada; Toshio Murakami; Yujin E. Nakagawa; Hiromitsu Takahashi; Yukikatsu Terada; Atsumasa Yoshida
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, Number：2, First page：237, Last page：244, Apr. 2008
A Suzaku TOO observation of CXOU J164710.2-455216 was performed on 2006 September 23-24 for a net exposure of 38.8 ks. Pulsations were clearly detected in the XIS light curves with a pulse period of 10.61063(2) s. The XIS pulse profile is found to be highly non-sinusoidal. It shows 3 peaks of different amplitudes with an RMS fractional amplitude of similar to 11% in the 0.2-6.0 keV energy band. The 1 -10 keV XIS spectra were well fitted by two different models consisting of a power-law and a blackbody component and two blackbody components, respectively. Although both the models are statistically acceptable, a difference in the pulse profiles at soft (0.2-6.0 keV) and hard (6-12keV) X-rays favors the model consisting of two blackbody components. The temperatures of two blackbody components are found to be 0.61 +/- 0.01 keV and 1.22 +/- 0.06 keV, and the value of the absorption column density is 1.73 +/- 0.03 x 10(22) atoms cm(-2). Pulse phase resolved spectroscopy shows that the flux of the soft blackbody component consists of three narrow peaks, whereas the flux of the other component shows a single peak over the pulse period of the AXP. The blackbody radii change between 2.2-2.7 km and 0.28-0.38 km (assuming the source distance to be 5 kpc) over the pulse phases for the soft and hard components, respectively. The details of the results obtained from the timing and spectral analyses are presented.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/60.2.237
DOI ID：10.1093/pasj/60.2.237, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000255818400011 - 「すざく」衛星による2006年12月5日のX9太陽フレアからの中性子検出の可能性 II
北口貴雄; 江戸輝揚; 中澤知洋; 牧島一夫; 馬場彩; 国分紀秀; 川原田円; 遠藤輝; 浦田裕次; 寺田幸功; 田代信; 山岡和貴; HONG S; 土屋晴文; LOEWENSTEIN Michael
日本物理学会講演概要集, Volume：63, Number：1, First page：105, 29 Feb. 2008
Japanese
ISSN：1342-8349, J-Global ID：200902239349446957 - 「すざく」およびRXTE衛星で探るX線パルサーのサイクロトロン吸収線
牧島一夫; 榎戸輝揚; 中島基樹; 三原建弘; 寺田幸功; 鈴木素子; 岩切渉; 上田剛; 北口貴雄; 中澤知洋; 国分紀秀
日本物理学会講演概要集, Volume：63, Number：1, First page：104, 29 Feb. 2008
Japanese
ISSN：1342-8349, J-Global ID：200902296698025288 - 次期X線天文衛星NeXT搭載硬X線撮像検出器(HXI)の開発(II)
国分紀秀; 渡辺伸; 佐藤理江; 武田伸一郎; 石川真之介; 小高裕和; 青野博之; 高橋忠幸; 深沢泰司; 中澤知洋; 片岡淳; 寺田幸功; 山岡和貴; 玉川徹
日本天文学会年会講演予稿集, Volume：2008, First page：247, 20 Feb. 2008
Japanese
ISSN：1347-0639, J-Global ID：200902228121785350 - 「すざく」衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状(V)
寺田幸功; 田代信; 浦田裕次; 恩田香織; 遠藤輝; 鈴木正信; 小高夏来; 守上浩市; 深沢泰司; 大野雅功; 高橋拓也; 上原岳士; 吉良知恵; 花畑義隆; 山岡和貴; 中川友進; 杉田聡司; 玉川徹; 中澤知洋; 榎戸輝揚; 洪秀徴; 牧島一夫; 高橋忠幸; 国分紀秀; 鈴木素子; 山内誠; 園田絵里; 前野将太; 田中裕基; 原龍児; 田島宏康
日本天文学会年会講演予稿集, Volume：2008, First page：246, 20 Feb. 2008
Japanese
ISSN：1347-0639, J-Global ID：200902276515426857 - In-orbit timing calibration of the hard X-ray detector on board Suzaku
Yukikatsu Terada; Teruaki Enoto; Ryouhei Miyawaki; Yoshitaka Ishisaki; Tadayasu Dotani; Ken Ebisawa; Masanobu Ozaki; Yoshihiro Ueda; Lucien Kuiper; Manabu Endo; Yasushi Fukazawa; Tsuneyoshi Kamae; Madoka Kawaharada; Motohide Kokubun; Yoshikatsu Kuroda; Kazuo Makishinia; Kazunori Masukawa; Tsunefumi Mizuno; Toshio Murakami; Kazuhiro Nakazawa; Atsushi Nakajima; Masaharu Nomach; Naoki Shibayama; Tadayuki Takahash; Hiromitsu Takahashi; Makoto S. Tashiro; Toru Tamagawa; Shin Watanabe; Makio Yamaguchi; Kazutaka Yamaoka; Daisuke Yonetoku
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, Number：Sp. Iss. 1, First page：S25, Last page：S33, Feb. 2008
The hard X-ray detector (HXD) aboard the X-ray satellite Suzaku is designed to have a good timing capability with a 61 its time resolution. In addition to detailed descriptions of the HXD timing system, results of in-orbit timing calibration and the performance of the HXD are summarized. The relative accuracy of time measurements of the HXD event was confirmed to have an accuracy of 1.9 x 10(-9) s s(-1) per day, and the absolute timing was confirmed to be accurate to 360 mu s or better. The results were achieved mainly through observations of the Crab pulsar, including simultaneous ones with RXTE, INTEGRAL, and Swift.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/60.sp1.S25
DOI ID：10.1093/pasj/60.sp1.S25, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000255818700003 - Suzaku observations of Hercules X-1: Measurements of the two cyclotron harmonics
Teruaki Enoto; Kazuo Makishima; Yukikatsu Terada; Tatehiro Mihara; Kazuhiro Nakazawa; Tsuyoshi Ueda; Tadayasu Dotani; Motohide Kokubun; Fumiaki Nagase; Sachindra Naik; Motoko Suzuki; Motoki Nakajinia; Hiromitsu Takahashi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, Number：Sp. Iss. 1, First page：S57, Last page：S68, Feb. 2008
The accretion-powered pulsar Her X-1 was observed with Suzaku twice in its main-on state, on 2005 October 5-6 and 2006 March 29-30, for a net exposure of 30.5 ks and 34.4 ks, respectively. In the 2005 and 2006 observations, the source was detected at an average 10-30 keV intensity of 290 mCrab and 230 mCrab, respectively. The intrinsic pulse period was measured on both occasions at 1.23776 s by HXD-PIN, after barycentric and binary corrections. The pulse phase-averaged spectra in the energy range above 10 keV were well fitted by the "Negative and Positive power-law times EXponential" (NPEX) model, multiplied by a fundamental cyclotron resonance scattering feature at similar to 36 keV, which appears very significantly in the HXD-PIN data. The resonance profiles were successfully reproduced by a Lorentzian-type scattering cross section, rather than by a Gaussian-type alternative. The pulse phase-averaged HXD-GSO data, covering 50-120 keV, are featureless. However, in a differential spectrum between the pulse-decay phase and off-pulse phase, the second-harmonic cyclotron resonance was detected in the GSO data at similar to 73 keV, with a depth of 1.6(-0.7)(+0.9) This makes Her X-1 a 6th pulsar with established second-harmonic resonance. The implications of these results are briefly discussed.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/60.sp1.S57
DOI ID：10.1093/pasj/60.sp1.S57, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000255818700007 - Spectral properties of prompt emission of four short gamma-ray bursts observed by the Suzaku-WAM and the Konus-wind
Masanori Ohno; Yasushi Fukazawa; Takuya Takahashi; Kazutaka Yamaoka; Satoshi Sugita; Valentin Pal'shin; Dmitry Frederiks; Philipp Oleynik; Mikhail Ulanov; Takanori Sakamoto; Goro Sato; Kevin Hurley; Makoto S. Tashiro; Yuji Urata; Kaori Onda; Toru Tamagawa; Yukikatsu Terada; Motoko Suzuki; Hong Soojing
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, Number：Sp. Iss. 1, First page：S361, Last page：S373, Feb. 2008
We have performed a joint analysis of prompt emission from four bright short gamma-ray bursts (GRBs) with the Suzaku-WAM and the Konus-Wind experiments. This joint analysis allows us to investigate the spectral properties of short-duration bursts over a wider energy band with a higher accuracy. We find that these bursts have a high E-peak, around 1 MeV and have a harder power-law component than that of long GRBs. However, we can not determine whether these spectra follow the cut-off power-law model or the Band model. We also investigated the spectral lag, hardness ratio, inferred isotropic radiation energy and existence of a soft emission hump, in order to classify them into short or long GRBs using several criteria, in addition to the burst duration. We find that all criteria, except for the existence of the soft hump, support the fact that our four GRB samples are correctly classified as belonging to the short class. In addition, our broad-band analysis revealed that there is no evidence of GRBs with a very large hardness ratio, as seen in the BATSE short GRB sample, and that the spectral lag of our four short GRBs is consistent with zero, even in the MeV energy band, unlike long GRBs. Although our short GRB samples are still limited, these results suggest that the spectral hardness of short GRBs might not differ significantly from that of long GRBs, and also that the spectral lag at high energies could be a strong criterion for burst classification.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/60.sp1.S361
DOI ID：10.1093/pasj/60.sp1.S361, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000255818700035 - Suzaku detection of extended/diffuse hard X-ray emission from the galactic center
Takayuki Yuasa; Ken-Ichi Tamura; Kazuhiro Nakazawa; Motohide Kokubun; Kazuo Makishima; Aya Bamba; Yoshitomo Maeda; Tadayuki Takahashi; Ken Ebisawa; Atsushi Senda; Yoshiaki Hyd; Takeshi Go Tsuru; Katsuji Koyama; Shigeo Yamauchi; Hiromitsu Takahashi
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, First page：S207, Last page：S221, Feb. 2008
Five on-plane regions within +/-0.degrees 8 of the galactic center were observed with the Hard X-ray Detector (HXD) and the X-ray Imaging Spectrometer (XIS) aboard Suzaku. From all regions, significant hard X-ray emission was detected with HXD-PIN up to 40 keV, in addition to the extended plasma emission which is dominant in the XIS band. The hard X-ray signals are inferred to come primarily from a spatially extended source, rather than from a small number of bright discrete objects. Contributions to the HXD data from catalogued X-ray sources, typically brighter than 1 mCrab, were estimated and removed using information from Suzaku and other satellites. Even after this removal, the hard X-ray signals remained significant, exhibiting a typical 12-40keV surface brightness of 4 x 10(-10) erg cm(-2) s(-1) deg(-2) and power-law-like spectra with a photon index of 1.8. Combined fittings to the XIS and HXD-PIN spectra confirm that a separate hard tail component is superposed onto the hot thermal emission, confirming a previous report based on the XIS data. Over the 5-40 keV band, the hard tail is spectrally approximated by a power law of photon index similar to 2, but better by those with somewhat convex shapes. Possible origins of the extended hard X-ray emission are discussed.
OXFORD UNIV PRESS, English, Technical report
DOI：https://doi.org/10.1093/pasj/60.sp1.S207
DOI ID：10.1093/pasj/60.sp1.S207, ISSN：0004-6264, eISSN：2053-051X, arXiv ID：arXiv:0709.1580, Web of Science ID：WOS:000255818700022 - 報道公開: 「すざく」、白色矮星パルサーを発見！
17 Jan. 2008
研究業績を報道公開。NHK, さいたまTVで放映されたほか、産経新聞、毎日新聞をはじめとする全国２４社の新聞に掲載 - 報道公開: (米国) White Dwarf like a Pulsar
02 Jan. 2008
研究業績を、共同研究機関である NASA Goddard Space Flight Center よりプレスリリース。(http://www.nasa.gov/centers/goddard/news/topstory/2007/whitedwarf_pulsar.html) - Suzaku Observations of Hercules X-1 : Measurements of the Two Cyclotron Harmonics
T. Enoto; K. Makishima; Y.Terada; T. Mihara; K. Nakazawa; T. Ueda; T. Dotani; M. Kokubun; F. Nagase; S. Naik; M. Suzuki; M. Nakajima; H. Takahashi
Volume：60, Number：Sp. Iss. 1, First page：S57-S68, 2008 - Spectral properties of prompt emission of four short gamma-ray bursts observed by the Suzaku-WAM and the Konus-wind
M. Ohno; Y. Fukazawa; T. Takahashi; K. Yamaoka; S. Sugita; V. Pal’shin; T. Sakamoto; G. Sato; K. Hurley; D. Frederiks; P. Oleynik; M. Ulanov; M. Tashiro; Y. Urata; K. Onda; T. Tamagawa; Y.Terada; M. Suzuki; S. Hong
Volume：60, Number：Sp. Iss. 1, First page：S361-S373, 2008 - Suzaku wide-band observations of SN 1006
Aya Bamba; Yasushi Fukazawa; Junko S. Hiraga; John P. Hughes; Hideaki Katagiri; Motohide Kokubun; Katsuji Koyama; Emi Miyata; Tsunefumi Mizuno; Koji Mori; Hiroshi Nakajima; Masanobu Ozaki; Rob Petre; Hiromitsu Takahashi; Tadayuki Takahashi; Takaaki Tanaka; Yukikatsu Terada; Yasunobu Uchiyama; Shin Watanabe; Hiroya Yamaguch
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：60, Number：Sp. Iss. 1, First page：S153-S161, Last page：S161, 2008
We report on the wide-band spectra of SN 1006, as observed by Suzaku. Thermal and nonthermal emissions were successfully resolved thanks to the excellent spectral response of Suzaku's X-ray CCD XIS. The nonthermal emission could not be reproduced by a simple power-law model, but needed a roll-off at 5.7 x 10(16) Hz = 0.23 keV. The roll-off frequency is significantly higher in the northeastern rim than in the southwestern rim. We also placed the most stringent upper limit of the flux above 10 keV using the Hard X-ray Detector.
OXFORD UNIV PRESS, English
DOI：https://doi.org/10.1093/pasj/60.sp1.S153
DOI ID：10.1093/pasj/60.sp1.S153, ISSN：0004-6264, eISSN：2053-051X, Web of Science ID：WOS:000255818700016 - Broadband X-ray spectroscopy of A0535+262 with Suzaku
S. Naik; T. Dotani; Y. Terada; M. Nakajima; T. Mihara; M. Suzuki; K. Makishima; K. Sudoh; S. Kitamoto; F. Nagase; T. Enoto; H. Takahashi
ASTROPHYSICAL JOURNAL, Volume：672, Number：1, First page：516, Last page：523, Jan. 2008
The transient X-ray binary pulsar A0535+262 was observed with Suzaku on 2005 September 14 when the source was in the declining phase of the August-September minor outburst. The similar to 103 s X-ray pulse profile was strongly energy dependent, with a double-peaked profile in the soft X-ray energy band (< 3 keV) and a single-peaked smooth profile in hard X-rays. The width of the primary dip is found to increase with energy. The broadband energy spectrum of the pulsar is well described with a negative and positive power law with exponential (NPEX) continuum model, along with a blackbody component for soft excess. A weak iron K alpha emission line with an equivalent width similar to 25 eV was detected in the source spectrum. The blackbody component is found to be pulsating over the pulse phase, implying that the accretion column and/or the inner edge of the accretion disk may be the possible emission site of the soft excess in A0535+262. The higher value of the column density is believed to be the cause of the secondary dip in the soft X-ray energy band. The iron line equivalent width is found to be constant (within errors) over the pulse phase. However, a sinusoidal type of flux variation of the iron emission line, in phase with the hard X-ray flux, suggests that the inner accretion disk is the possible emission region of the iron fluorescence line.
IOP PUBLISHING LTD, English
DOI：https://doi.org/10.1086/523295
DOI ID：10.1086/523295, ISSN：0004-637X, eISSN：1538-4357, Web of Science ID：WOS:000253454000046 - In-orbit timing calibration of the hard X-ray detector on board Suzaku
Y.Terada; T. Enoto; R. Miyawaki; Y. Ishisaki; T. Dotani; K. Ebisawa; M. Ozaki; Y. Ueda; L. Kuiper; M. Endo; Y. Fukazawa; T. Kamae; M. Kawaharada; M. Kokubun; Y. Kuroda; K. Makishima; K. Masukawa; T. Mizuno; T. Murakami; K. Nakazawa; A. Nakajima; M. Nomach; N. Shibayama; T. Takahashi; H. Takahashi; M.S.Tashiro; T. Tamagawa; S. Watanabe; M. Yamaguchi; K. Yamaoka; D. Yonetoku
Publications of the Astronomical Society of Japan, Volume：60, Number：Sp. Iss. 1, First page：S25-S33, 2008 - Suzaku wide-band observations of SN 1006
A. Bamba; Y. Fukazawa; J. Hiraga; J. Huges; H. Katagiri; M. Kokubun; K. Koyama; E. Miyata; T. Mizuno; K. Mori; H. Nakajima; M. Ozaki; R. Petre; H. Takahashi; T. Takahashi; T. Tanaka; Y.Terada; Y. Uchiyama; S. Watanabe; H. Yamaguchi
Publications of the Astronomical Society of Japan, Volume：60, Number：Sp. Iss. 1, First page：S153-S161, 2008 - Possible Suzaku detection of non-thermal X-ray signals from a rotating magnetized white dwarf
Y. Terada; M. Ishida; K. Mukai; T. Dotani; K. Makishima; S. Naik; T. Hayashi; S. Okada; R. Nakamura; T. Enoto
ADVANCES IN SPACE RESEARCH, Volume：41, Number：3, First page：512, Last page：517, 2008
Although rotating neutron stars (NSs) have been regarded as being textbook examples of astrophysical particle acceleration sites for decades, details of the acceleration mechanism remain a mystery; for example, we cannot yet observationally distinguish "polar cap" models from "outer gap" models. To solve the model degeneracy, it is useful to study similar systems with much different physical parameters. Strongly magnetized white dwarfs (WDs) are ideal for this purpose, because they have essentially the same system geometry as NSs, but differ largely from NSs in the system parameters, including the size, magnetic field, and the rotation velocity, with the induced electric field expected to reach 10(13)-10(14) eV. Based on this idea, the best candidate among WDs, AE Aquarii, was observed with the fifth Japaneses X-ray satellite, Suzaku. The hard X-ray detector (HXD) on-board Suzaku has the highest sensitivity in the hard X-ray band over 10 keV. A marginal detection in the hard X-ray band was achieved with the HXD, and was separated from the thermal emission. The flux corresponds to about 0.02% of its spin-down energy. If the signal is real, this observation must be a first case of the detection of non-thermal emission from WDs. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved.
ELSEVIER SCI LTD, English
DOI：https://doi.org/10.1016/j.asr.2007.05.076
DOI ID：10.1016/j.asr.2007.05.076, ISSN：0273-1177, Web of Science ID：WOS:000253590600017 - Oxygen line mapping of SN 1006 with Suzaku
Aya Bamba; Hiroya Yamaguchi; KatsuJi Koyama; Junko S. Hiraga; Steve Holt; John P. Hughes; Hideaki Katagiri; Jun Kataoka; Satoru Katsuda; Shunji Kitamoto; Motohide Kokubun; Hironori Matsumoto; Emi Miyata; Koji Mori; Hiroshi Nakajima; Masanobu Ozaki; Rob Petre; Akiko Sekiguchi; Tadayuki Takahashi; Takaaki Tanaka; Yukikatsu Terada; Hiroshi Tomida; Yohko Tsuboi; Masahiro Tsujimoto; Hiroshi Tsunemi; Yasunobu Uchiyama; Masaru Ueno; Shin Watanabe
ADVANCES IN SPACE RESEARCH, Volume：41, Number：3, First page：411, Last page：415, 2008
SN 1006 is one of the supernova remnants (SNRs) with relatively low-temperature electrons, considering the young age of just 1000 years. We carried out SN 1006 mapping observations with the X-ray Imaging Spectrometers (XIS) and the Hard X-ray Detector (HXD) onboard Suzaku, the fifth Japanese X-ray satellite. Thanks to the excellent spectral resolution of XIS in the soft X-ray band, H-like and He-like oxygen emission lines were clearly detected, and we could make a map of the line intensity, and as well as a flux and the photon index of nonthermal component. We found that these parameters have spatial dependences from region to region in the SNR; the north region is bright in nonthermal, while dim in thermal; the east region is bright in both nonthermal and thermal; the inner region shows dim nonthermal and bright thermal emission. The photon index is the smallest in the north region. (C) 2007 Published by Elsevier Ltd on behalf of COSPAR.
ELSEVIER SCI LTD, English
DOI：https://doi.org/10.1016/j.asr.2007.03.055
DOI ID：10.1016/j.asr.2007.03.055, ISSN：0273-1177, Web of Science ID：WOS:000253590600006 - Initial results from suzaku
Tadayuki Takahashi; Kazuhisa Mitsuda; Hideyo Kunieda
Energy Budget in the High Energy Universe - Proceedings of the International Workshop, First page：217, Last page：225, 01 Dec. 2007
Suzaku is the fifth in the series of Japanese astronomy satellites devoted to observations of celestial X-ray sources launched on a Japanese M-V rocket on July 10, 2005. Suzaku features the excellent X-ray sensitivity, with high throughput over a broad-band energy range of 0.2 to 600 keV. Suzaku's broad bandpass, low background, and good CCD resolution makes it a unique tool capable of addressing a variety of outstanding problems in astrophysics. Copyright © 2007 by World Scientific Publishing Co. Pvt. Ltd.
SCOPUS ID：84894291835 - 「すざく」衛星によるHer X‐1のサイクロトロン共鳴線の観測
榎戸輝揚; 牧島一夫; 寺田幸功; 三原建弘; 上田剛; 中澤知洋; 鈴木素子; 国分紀秀; 長瀬文昭; 中島基樹; 高橋弘充
日本物理学会講演概要集, Volume：62, Number：2, First page：106, 21 Aug. 2007
Japanese
ISSN：1342-8349, J-Global ID：200902207999863421 - 「すざく」衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状(III)
HONG S; 田代信; 浦田裕次; 恩田香織; 鈴木正信; 小高夏来; 守上浩市; 寺田幸功; 玉川徹; 山岡和貴; 中川友進; 杉田聡司; 国分紀秀; 渡辺伸; 鈴木素子; 深沢泰司; 水野恒史; 大野雅功; 高橋拓也; 上原岳士; 吉良知恵; 中澤知洋; 榎戸輝揚; 山内誠; 園田絵里; 前野将太; 田中裕基; 原龍児
日本物理学会講演概要集, Volume：62, Number：2, First page：106, 21 Aug. 2007
Japanese
ISSN：1342-8349, J-Global ID：200902269950824922 - 「すざく」衛星搭載硬X線検出器広帯域全天モニタ部(HXD‐WAM)の現状(IV)
杉田聡司; 山岡和貴; 中川友進; 田代信; 浦田裕次; 恩田香織; 遠藤輝; 鈴木正信; 小高夏来; 守上浩市; 玉川徹; 寺田幸功; 深沢泰司; 大野雅功; 高橋拓也; 上原岳士; 吉良知恵; 中澤知洋; 宮脇良平; 榎戸輝揚; 牧島一夫; 高橋忠幸; 国分紀秀; 鈴木素子; 洪秀徴; 山内誠; 園田絵里; 前野将太; 田中裕基; 原龍児; 田島宏康
日本天文学会年会講演予稿集, Volume：2007, First page：293, 20 Aug. 2007
Japanese
ISSN：1347-0639, J-Global ID：200902240112462310 - すざく衛星によるHer X‐1サイクロトロン共鳴吸収の観測
榎戸輝揚; 牧島一夫; 三原建弘; 寺田幸功; 中澤知洋; 上田剛; 中島基樹; 鈴木素子; 長瀬文昭
日本天文学会年会講演予稿集, Volume：2007, First page：127, 20 Aug. 2007
Japanese
ISSN：1347-0639, J-Global ID：200902209510157255 - 次世代X線天文衛星NeXT搭載,硬X線撮像検出器(HXI)に向けた開発の現状
渡辺伸; 国分紀秀; 佐藤理江; 武田伸一郎; 石川真之介; 小高裕和; 青野博之; 高橋忠幸; 深沢泰司; 安田創; 田中琢也; 西野翔; 中澤知洋; 奥山翔; 田島宏康; 田中孝明; 片岡淳; 寺田幸功; 玉川徹
日本天文学会年会講演予稿集, Volume：2007, First page：300, 20 Aug. 2007
Japanese
ISSN：1347-0639, J-Global ID：200902222912573766 - すざく衛星搭載HXD‐PIN検出器のノイズイベント経年変化の調査
西野翔; 梅木勇大; 深沢泰司; 水野恒史; 高橋弘充; 牛尾雅佳; 渡辺伸; 国分紀秀; 田中孝明; 北口貴雄; 中澤知洋; 山田真也; 湯浅孝行; 川原田円; 寺田幸功
日本天文学会年会講演予稿集, Volume：2007, First page：293, 20 Aug. 2007
Japanese
ISSN：1347-0639, J-Global ID：200902270439376545 - 26aSF-6 X線観測衛星「すざく」搭載広帯域全天モニター(WAM)を用いた太陽フレアの観測と性能評価(26aSF X線・γ線,宇宙線・宇宙物理領域)
鈴木 正信; 佐藤 優美; 浦田 裕次; 田代 信; 寺田 幸功; 山岡 和貴; 簑島 敬; 横山 央明; 牧島 一夫; 高橋 忠幸; HXD-WAMチーム
Volume：62, Number：1, First page：95, Last page：95, 28 Feb. 2007
Japanese
ISSN：1342-8349, CiNii Articles ID：110007140777, CiNii Books ID：AA11439205 - 26aSF-4 Background Simulation of Hard X-ray Detector onboard Suzaku
Kitaguchi T.; Kawaharada M.; Kokubun M.; Odaka H.; T. Tadayuki; Ozaki M.; Terada Y.; Ishisaki Y.; Makishima K.; HXD team
Meeting abstracts of the Physical Society of Japan, Volume：62, Number：1, First page：94, Last page：94, 28 Feb. 2007
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110007140779, CiNii Books ID：AA11439205 - Suzaku observations of cyclotron resonances in binary X-ray pulsars
Y. Terada; T. Mihara; F. Nagase; L. Angelini; T. Dotani; T. Enoto; S. Kitamoto; T. Kohmura; M. Kokubun; T. Kotani; K. Makishima; S. Naik; M. Nakajima; S. Sugita; K. Sudoh; M. Suzuki; H. Takahashi; D. Yonetoku; A. Yoshida
ADVANCES IN SPACE RESEARCH, Volume：40, Number：10, First page：1485, Last page：1490, 2007
Since the typical magnetic field strengths of neutron stars reach 1012 Gauss, the cyclotron resonance produced by a transition between Landau levels appears in the X-ray band. Systematic measurements of cyclotron absorption features in bright sources have been carried out extensively with Ginga, RXTE, BeppoSAX, and INTEGRAL. The cyclotron resonance phenomena can now be studied with a higher sensitivity over a wider hard X-ray band than before, thanks to the Hard X-ray Detector onboard the fifth Japanese X-ray satellite, Suzaku, launched in July, 2005. Suzaku observed Hercules X-1 mainly for calibration purposes, and successfully confirmed its well-known cyclotron absorption feature. Furthermore, the transient pulsar A0535+262 was observed with Suzaku on 14 September, 2005, in the decay phase of its minor outburst (Finger, M.F. Renewed Activity from A0535+26. The Astronomer's Telegram, vol. 595, 2005). The cyclotron resonance of A0535+262 was successfully detected in absorption at about 45 keV (Inoue, H., Kunieda, H., White, N., Kelley, R., Nlihara, T., Terada, Y., Takahashi, H., Kokubun, M., Makishima, K. Suzaku detection of cyclotron line near 50 keV for A0535+26. The Astronomer's Telegram vol. 595, 2005; Terada, Y., Mihara, T., Nakajima, M., et al. Cyclotron resonance energies at a low X-ray luminosity: A0535+262 observed with Suzaku. ApJL 648, L139-LI42, 2006), even though the object was as dim as 30 mCrab at 20 keV. Compared with previous measurements of the same feature achieved at much brighter phases (e.g., Kretschmar, P., Kreykenbohm, I., Pottschmidt, et al. Integral observes possible cyclotron line at 47 keV for 1A0535+262. The Astronomer's Telegram, vol. 601, 2005; Wilson, C.A., Finger, M.H. RXTE confirms cyclotron line near 50 keV for A0535+26. The Astronomer's Telegram 605, 2005), the Suzaku results give a new constraint to luminosity-related changes in the resonance energy that are observed in other binary pulsars (Nakajima, M., Mihara, T., Makishima, K., Niko, H. A further study of the luminosity-dependent cyclotron resonance energies of the binary X-ray pulsar 4U 0115+63 with the Rossi X-ray timing explorer. ApJ 646, 1125-1138, 2006). (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved.
ELSEVIER SCI LTD, English
DOI：https://doi.org/10.1016/j.asr.2007.02.020
DOI ID：10.1016/j.asr.2007.02.020, ISSN：0273-1177, Web of Science ID：WOS:000253590100010 - Discovery of a possible X-ray counterpart to HESS J1804-216
Aya Bamba; Katsuji Koyama; Junko S. Hiraga; John P. Hughes; Takayoshi Kohmura; Motohide Kokubun; Yoshitomo Maeda; Hironori Matsumoto; Atsushi Senda; Tadayuki Takahashi; Yohko Tsuboi; Shigeo Yamauchi; Takayuki Yuasa
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN, Volume：59, First page：S209, Last page：S214, Jan. 2007
Suzaku deep observations have discovered two highly significant nonthermal X-ray sources, Suzaku J1804-2142 (Src 1) and Suzaku J1804-2140 (Src 2), positionally coincident with the unidentified TeV gamma-ray source, HESS J1804-216. The X-ray sources are not time variable and show no Counterpart in other wavebands, except for the TeV source. Src 1 is unresolved at Suzaku spatial resolution, whereas Src 2 is extended or composed of multiple sources. The X-ray spectra are highly absorbed, hard, and featureless, and are well fitted by absorbed power-law models with best-fit photon indices and absorption columns of -0.3(-0.5)(+0.5) and 0.2(-0.2)(+2.0) x 10(22) cm(-2) for Src 1, and 1.7(-1.0)(+1.4) and 1.1(-0.6)(+1.0) x 10(23) cm(-2) for Src 2. The measured X-ray absorption to the latter source is signif icantly larger than the total Galactic neutral hydrogen column in that direction. The unabsorbed 2-10 keV band luminosities are 7.5 x 10(32) (d/5 kpc)(2) erg s(-1) (Src 1) and 1.3 x 10(33) (d/5 kpc)(2) erg s(-1) (Src 2), where d is the source distance. Among the handful of TeV sources with known X-ray counterparts, HESS J1804-216 has the largest ratio of TeV gamma-ray to hard X-ray fluxes. We discuss the nature of the emission and propose the Suzaku sources as plausible counterparts to the TeV source, although further observations are necessary to confirm this.
OXFORD UNIV PRESS, English, Technical report
DOI：https://doi.org/10.1093/pasj/59.sp1.S209
DOI ID：10.1093/pasj/59.sp1.S209, ISSN：0004-6264, eISSN：2053-051X, arXiv ID：astro-ph/0608310, Web of Science ID：WOS:000244441700016 - 22aZJ-3 In orbit timing calibration of the Suzaku Hard X-ray Detector with X-ray pulsars (II)
Terada Yukikatsu; Enoto T; Ishizaki Y; Ebisawa K; Ozaki M; Dotani T; Kokubun M; Makishima K; the Suzaku; HXD team
Meeting Abstracts of the Physical Society of Japan, Volume：62, Number：0, 2007
The Physical Society of Japan, Japanese
CiNii Articles ID：110007194126 - 26aSF-3 Current Status of the Suzaku Hard X-ray Detector (III)
Kokubun M; Fukazawa Y; Mizuno T; Takahashi H; Tashiro S; Yamaoka K; Murakami T; Yonetoku D; Suzaku HXD team; Takahashi T; Nakazawa K; Watanabe S; Kawaharada M; Makishima K; Terada Y; Tamagawa T; Kubota A
Meeting Abstracts of the Physical Society of Japan, Volume：62, Number：0, 2007
一般社団法人 日本物理学会, Japanese
CiNii Articles ID：110007140780 - 「すざく」衛星搭載硬X線検出器(HXD/PIN)の軌道上バックグラウンドの系統的評価
牛尾雅佳; 高橋忠幸; 田中孝明; 田村健一; 中澤知洋; 渡辺伸; 国分紀秀; 川埜直美; 深沢泰司; 磯部直樹; 寺田幸功
日本天文学会年会講演予稿集, Volume：2006, First page：264, 20 Aug. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302240685242929 - 「すざく」衛星搭載広帯域全天モニタ(HXD/WAM)によるGRB観測の現状
大野雅功; 高橋拓也; 深沢泰司; 山岡和貴; 杉田聡司; 玉川徹; 寺田幸功; 鈴木素子; 田代信; 浦田裕次; 阿部圭一; 恩田香織; 鈴木正信; 洪秀徴; 国分紀秀; 榎戸輝揚; 牧島一夫; 佐藤悟朗; 中澤知洋; 高橋忠幸
日本天文学会年会講演予稿集, Volume：2006, First page：70, 20 Aug. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302243200014620 - 「すざく」衛星搭載硬X線検出器(HXD)主検出部の現状(II)
国分紀秀; 川原田円; 牧島一夫; 寺田幸功; 山岡和貴; 高橋忠幸; 中澤知洋; 渡辺伸; 深沢泰司; 水野恒史; 高橋弘充; 田代信; 米徳大輔; 村上敏夫
日本天文学会年会講演予稿集, Volume：2006, First page：264, 20 Aug. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302286233674929 - 「すざく」搭載硬X線検出器GSOシンチレータのゲイン履歴補正およびバックグラウンドモデル化の現状
山崎智紀; 平澤歩; 高橋弘充; 深沢泰司; 山田真也; 伊藤健; 北口貴雄; 国分紀秀; 牧島一夫; 鈴木正信; 田代信; 磯部直樹; 寺田幸功; 中澤知洋; 高橋忠幸
日本天文学会年会講演予稿集, Volume：2006, First page：265, 20 Aug. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302289337226889 - X線天文衛星「すざく」による観測速報(4)
伊藤 真之; 馬場 彩; 寺田 幸功; 鶴 剛; 小澤 碧; 松下 恭子; 大橋 隆哉; 太田 直美; 深沢 泰司; 中澤 和洋
Volume：99, Number：6, First page：332, Last page：333, 20 May 2006
Japanese
ISSN：0374-2466, CiNii Articles ID：10017508663 - X線天文衛星「すざく」による観測速報(3)
田代 信; 山岡 和貴; 大野 雅功; 村上 敏夫; 中澤 知洋; 中川 友進; 河合 誠之; 高橋 忠幸; 寺田 幸功
Volume：99, Number：5, First page：282, Last page：283, 20 Apr. 2006
Japanese
ISSN：0374-2466, CiNii Articles ID：10018138467, CiNii Books ID：AN00154555 - 28aTF-1 In-Orbit Calibration of the HXD-II onboard Suzaku
Kitaguchi T.; Kokubun M.; Hirakuri S.; Miyawaki R.; Makishima K.; Terada Y.; Kishishita T.; Nakazawa K.; Takahashi T.; Endo Y.; Tashiro M.; Fukazawa Y.; the HXD team
Meeting abstracts of the Physical Society of Japan, Volume：61, Number：1, First page：92, Last page：92, 04 Mar. 2006
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110007179582, CiNii Books ID：AA11439205 - 28aTF-2 Current Status of the Suzaku Hard X-ray Detector
Kokubun M.; Takahashi H.; Makishima K.; Terada Y.; Tamagawa T.; Kubota A.; Takahashi T.; Nakazawa K.; Watanabe S.; Fukazawa Y.; Mizuno T.; Tashiro S.; Murakami T.; Yonetoku D.; Yamaoka K.; Kamae T.; Madjeski Greg; Nomachi M.
Meeting abstracts of the Physical Society of Japan, Volume：61, Number：1, First page：92, Last page：92, 04 Mar. 2006
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110007177174, CiNii Books ID：AA11439205 - 28pTF-14 超広視野可視光カメラ(WIDGET)の改良とガンマ線バースト観測結果(28pTF X線・γ線,宇宙線・宇宙物理領域)
桑原 允; 吾妻 洋樹; 玉川 徹; 浦田 裕次; 寺田 幸功; 田代 信; 阿部 圭一; 恩田 香織; 臼井 文彦; WIDGETチーム
Volume：61, Number：1, First page：99, Last page：99, 04 Mar. 2006
Japanese
ISSN：1342-8349, CiNii Articles ID：110007177186, CiNii Books ID：AA11439205 - 「すざく」衛星による銀河中心,および銀河面からの硬X線放射の観測
大貫宏祐; 中澤知洋; 田村健一; 渡辺伸; 高橋忠幸; 村上弘志; 寺田幸功; 千田篤史; 国分紀秀; 深沢泰司; 小山勝二
日本天文学会年会講演予稿集, Volume：2006, First page：146, 20 Feb. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302215605008551 - 「すざく」ファーストライト:硬X線検出器(HXD‐II)
国分紀秀; 高橋弘充; 牧島一夫; 山岡和貴; 高橋忠幸; 中澤知洋; 渡辺伸; 深沢泰司; 水野恒史; 寺田幸功; 田代信; 米徳大輔; 村上敏夫; 能町正治; 釜江常好; MADEJSKI Greg
日本天文学会年会講演予稿集, Volume：2006, First page：280, 20 Feb. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302217149968532 - すざく衛星搭載PIN型シリコン検出器の軌道上較正及び性能評価
岸下徹一; 高橋忠幸; 中澤知洋; 渡辺伸; 田中孝明; 田村健一; 牧島一夫; 国分紀秀; 宮脇良平; 北口貴雄; 平栗慎也; 寺田幸功; 田代信; 遠藤康彦; 深沢泰司; 川埜直美; 平澤歩
日本天文学会年会講演予稿集, Volume：2006, First page：249, 20 Feb. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302223073460950 - 「すざく」硬X線検出器(HXD)のバックグラウンド差引の現状
深沢泰司; 川埜直美; 山崎智紀; 牧島一夫; 国分紀秀; 北口貴雄; 高橋忠幸; 中澤知洋; 渡辺伸; 寺田幸功; 山岡和貴
日本天文学会年会講演予稿集, Volume：2006, First page：250, 20 Feb. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302241557996909 - 「すざく」衛星搭載の硬X線検出器HXD主検出部の現状
中澤知洋; 釜江常好; 久保田あや; 国分紀秀; 高橋忠幸; 高橋弘充; 田代信; 玉川徹; 寺田幸功; 能町正治; 深沢泰司; 牧島一夫; 水野恒史; 村上敏夫; 山岡和貴; 米徳大輔; 渡辺伸; MADEJSKI Greg
日本天文学会年会講演予稿集, Volume：2006, First page：248, 20 Feb. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302257447818626 - 「すざく」広帯域全天モニタ(WAM)のバックグラウンド解析
高橋拓也; 大野雅功; 深沢泰司; 杉田聡司; 山岡和貴; 遠藤康彦; 田代信; 榎戸輝揚; 宮脇良平; 国分紀秀; 佐藤悟朗; 中澤知洋; 高橋忠幸; 寺田幸功; 玉川徹; 牧島一夫
日本天文学会年会講演予稿集, Volume：2006, First page：250, 20 Feb. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302274687309054 - 「すざく」衛星搭載 硬X線検出器 広帯域全天モニタ部(HXD‐II/WAM)の現状(I)
田代信; 山岡和貴; 寺田幸功; 玉川徹; 久保田あや; 牧島一夫; 国分紀秀; 高橋弘充; 釜江常好; MADJESKI Greg; 深沢泰司; 水野恒史; 高橋忠幸; 中澤知洋; 渡辺伸; 村上敏夫; 米徳大輔; 能町正治
日本天文学会年会講演予稿集, Volume：2006, First page：249, 20 Feb. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302284920725310 - すざく衛星搭載広帯域全天モニタ(WAM)によるGRBの観測
杉田聡司; 山岡和貴; 大野雅功; 高橋拓也; 深沢泰司; 洪秀徴; 阿部圭一; 遠藤康彦; 恩田香織; 田代信; 榎戸輝揚; 宮脇良平; 国分紀秀; 佐藤悟朗; 中澤知洋; 寺田幸功; 玉川徹; 高橋忠幸; 牧島一夫
日本天文学会年会講演予稿集, Volume：2006, First page：56, 20 Feb. 2006
Japanese
ISSN：1347-0639, J-Global ID：201302293406120122 - 28aTF-3 GRB observation with Suzaku Wideband All-sky Monitor (HXD-WAM)
Ohno Masanori; Abe Keiichi; Endo Yasuhiko; Onda Kaori; Sato Goro; Nakazawa Kazuhiro; Takahashi Tadayuki; Enoto Teruaki; Miyawaki Ryouhei; Kokubun Motohide; Makishima Kazuo; Fukazawa Yasushi; Suzaku HXD-II team; Takahashi Takuya; Yamaoka Kazutaka; Sugita Satoshi; Terada Yukikatsu; Tamagawa Toru; Tashiro Makoto; Hong Soojing
Meeting Abstracts of the Physical Society of Japan, Volume：61, Number：0, 2006
The Physical Society of Japan, Japanese
CiNii Articles ID：110007177175 - 23pSH-9 The Suzaku Hard X-ray Detector timing calibration using the X-ray pulsars
Enoto T; Terada Y; Ishisaki Y; Miyawaki R; Senda A; Ebisawa K; Kokubun M; Makishima K; the Suzaku team
Meeting Abstracts of the Physical Society of Japan, Volume：61, Number：0, 2006
The Physical Society of Japan, Japanese
CiNii Articles ID：110007178487 - 23aSH-9 Current Status of the Suzaku Hard X-ray Detactor Wide-band All-sky Monitor (II)
Terada Y; Suzuki M; Nakazawa K; Watanabe S; Sato G; Fukazawa Y; Mizuno T; Ohno M; Takahashi T; Kokubun M; Enoto T; Tamagawa T; Hong S; the Suzaku; HXD team; Suzuki M; Yamaoka K; Sugita S; Tashiro M; Urata Y; Abe K; Onda K
Meeting Abstracts of the Physical Society of Japan, Volume：61, Number：0, 2006
The Physical Society of Japan, Japanese
CiNii Articles ID：110007179786 - 23aSH-8 Current Status of the Suzaku Hard X-ray Detector (II)
Kokubun M; Fukazawa Y; Mizuno T; Takahashi H; Tashiro S; Yamaoka K; Murakami T; Yonetoku D; the Suzaku; HXD team; Kawaharada M; Makishima K; Takahashi T; Nakazawa K; Watanabe S; Terada Y; Tamagawa T; Kubota A
Meeting Abstracts of the Physical Society of Japan, Volume：61, Number：0, 2006
一般社団法人 日本物理学会, Japanese
CiNii Articles ID：110007183543 - 23pSH-6 Evaluation of the background models of HXD/PIN detector on board "SUZAKU" satellite and their reproducibility in the orbit
Ushio M; Takahashi T; Tanaka T; Nakazawa K; Watanabe S; Kokubun M; Fukazawa Y; Terada Y; the SUZAKU; HXD team
Meeting Abstracts of the Physical Society of Japan, Volume：61, Number：0, 2006
The Physical Society of Japan, Japanese
CiNii Articles ID：110007183662 - Results of a Si/CdTe compton telescope
Kousuke Oonuki; Takaaki Tanaka; Shin Watanabe; Shin'ichiro Takeda; Kazuhiro Nakazawa; Takefumi Mitani; Tadayuki Takahashi; Hiroyasu Tajima; Yasushi Fukazawa; Masaharu Nomachi
Proceedings of SPIE - The International Society for Optical Engineering, Volume：5922, First page：1, Last page：11, 01 Dec. 2005
We have been developed Si/CdTe semiconductor Compton telescope to explore the universe in the energy band from several 10 keV to a few MeV. In our Si/CdTe Compton telescope, a stacked thin CdTe pixel detector is a key component to achieve higher detection efficiency for MeV gamma-rays maintaining high energy resolution. In this paper, results from a prototype stacked CdTe pixel detector are reported, which consists of three layers of CdTe pixel detectors and one CdTe pixel detector at their side. With this prototype detector, we succeeded in Compton reconstruction of images and spectra in the energy band from 122 keV to 662 keV. The energy resolution (FWHM) of reconstructed spectra is 7.3 keV at 511 keV and 3.1 keV at 122 keV, respectively.
DOI：https://doi.org/10.1117/12.621809
DOI ID：10.1117/12.621809, ISSN：0277-786X, SCOPUS ID：31844455683 - Astro‐E2衛星の現状:硬X線検出器HXD
中澤知洋; 釜江常好; 国分紀秀; 高橋忠幸; 高橋弘充; 田代信; 寺田幸功; 能町正治; 深沢泰司; 牧島一夫; 水野恒史; 村上敏夫; 山岡和貴; 米徳大輔; 渡辺伸; MADEJSKI Greg
日本天文学会年会講演予稿集, Volume：2005, First page：312, 20 Aug. 2005
Japanese
ISSN：1347-0639, J-Global ID：201302294454175180 - 15aSA-13 Status report of the Hard X-ray detector(HXD-II) onboard Astro-E2 satellite III : Wideband All-sky Monitor(WAM) part
Yamaoka Kazutaka; Kamae Tsuneyoshi; Kokubun Norihide; Takahashi Tadayuki; Takahashi Hiromitsu; Tashiro Makoto; Terada Yukikatsu; Nakazawa Kazuhiro; Nomachi Masaharu; Fukazawa Yasushi; Makishima Kazuo; Mizuno Tsunefumi; Murakami Toshio; Watanabe Shin; Madejski Greg; on behalf of Astro-E2 HXD-II team
Meeting abstracts of the Physical Society of Japan, Volume：60, Number：2, First page：37, Last page：37, 19 Aug. 2005
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110004558749, CiNii Books ID：AA11439205 - 14aSF-9 WIDGET(WIDe-field telescope GRB for Early Timing) STATUS
Abe K.; Tamagawa T.; Usui F.; Terada Y.; Urata Y.; Onda K.; Tashiro M.; Azuma H.; Kuwahara M.; the WIDGET team
Meeting abstracts of the Physical Society of Japan, Volume：60, Number：2, First page：29, Last page：29, 19 Aug. 2005
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110004558724, CiNii Books ID：AA11439205 - 15aSA-11 Current Status of the Astro-E2 Hard X-ray Detector : I
Kokubun N.; Kamae T.; Takahashi T.; Takahashi H.; Tashiro S.; Terada Y.; Nakazawa K.; Nomachi M.; Fukaawa Y.; Makishima K.; Mizuno T.; Murakami T.; Yamaoka K.; Watanabe S.; Yonetoku D.; Madejski Greg; and HXD-II team
Meeting abstracts of the Physical Society of Japan, Volume：60, Number：2, First page：37, Last page：37, 19 Aug. 2005
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110004558748, CiNii Books ID：AA11439205 - The search for optical emission on and before the GRB trigger with the WIDGET telescope
T Tamagawa; F Usui; Y Urata; K Abe; K Onda; M Tashiro; Y Terada; H Fujiwara; N Miura; S Hirose; N Kawai; A Yoshida; M Mori; K Makishima
NUOVO CIMENTO DELLA SOCIETA ITALIANA DI FISICA C-COLLOQUIA ON PHYSICS, Volume：28, Number：4-5, First page：771, Last page：774, Jul. 2005
WIDGET is a robotic telescope for rnonitoring the HETE-2 field-of-view to detect Gamma-Ray Burst optical flashes or possible optical precursors. The system has 62 degrees x 62 degrees wide field-of-view which covers about 80% of HETE-2 one with a, 2kx2k Apogee U10 CCD camera and a Canon EF 24 mm f/1.4 wide-angle lens without a bandpass filter. WIDGET has been in operation since June 2004 at Akeno observing site where is about 200 kin apart from Tokyo. Typical limiting magnitude with S/N=3 at the site is V = 10(mag) for 5 seconds exposure and V = 11(mag) for 30 seconds exposure. We had already six coincident observations with HETE-2 position alerts. It was, however, cloudy for all cases due to rainy season in Japan. The expected number of coincident observations under clear sky is about 5 events per year. We will extend the system in early 2005 for Swift era to monitor optical transients in wider field-of-view, multi-color or polarization modes.
SOC ITALIANA FISICA, English
DOI：https://doi.org/10.1393/ncc/i2005-10150-1
DOI ID：10.1393/ncc/i2005-10150-1, ISSN：1124-1896, Web of Science ID：WOS:000234266300063 - 27aWH-5 Investigation on the activation background of γ-ray detector device by cosmic-ray particles
Kokubun M.; Murashima M.; Takahashi I.; Terada Y.; Watanabe S.; Takahashi T.; Makishima K.
Meeting abstracts of the Physical Society of Japan, Volume：60, Number：1, First page：81, Last page：81, 04 Mar. 2005
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110004534503, CiNii Books ID：AA11439205 - 25pWJ-12 Final verification of the data acquisition system of the HXD-II onboard Astro-E2
Kitaguchi T.; Kokubun M.; Takahashi I.; Kawaharada M.; Murashima M.; Miyawaki R.; Yanagida T.; Itoh T.; Niko H.; Hirakuri S.; Makishima K.; Nakazawa K.; Takahashi T.; Fukazawa Y.; Terada Y.; Nohmachi M.
Meeting abstracts of the Physical Society of Japan, Volume：60, Number：1, First page：28, Last page：28, 04 Mar. 2005
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110004534315, CiNii Books ID：AA11439205 - ASTRO‐E2衛星搭載PIN型シリコン検出器の応答特性
岸下徹一; 高橋忠幸; 田中孝明; 中澤知洋; 三谷烈史; 渡辺伸; 寺田幸功; 川原田円; 国分紀秀; 高橋勲; 二河久子; 宮脇良平
日本天文学会年会講演予稿集, Volume：2005, First page：251, 20 Feb. 2005
Japanese
ISSN：1347-0639, J-Global ID：201302262369009990 - Astro‐E2衛星硬X線検出器(HXD‐II)のソフトウェア開発の現状
寺田幸功; 渡辺伸; 尾崎正伸; 大野雅功; 鈴木雅也; 伊藤健; 内山泰伸; 久保信; 佐藤悟朗; 高橋勲; 川原田円; 村島未生; 宮脇良平; 柳田健之; 三谷烈史; 田中孝明; 川埜直美; 洪秀徴; 牧島一夫; 高橋忠幸; 村上敏夫; 田代信; 深沢泰司; 国分紀秀; 中澤知洋; 山岡和貴; 米徳大輔
日本天文学会年会講演予稿集, Volume：2005, First page：251, 20 Feb. 2005
Japanese
ISSN：1347-0639, J-Global ID：201302296356632096 - Development and qualification of the HXD-II onboard Astro-E2
Madoka Kawaharada; Soojing Hong; Mio M. Murashima; Motohide Kokubun; Takeshi Itoh; Kazuo Makishima; Ryouhei Miyawaki; Hisako Niko; Takayuki Yanagida; Takefumi Mitani; Kazuhiro Nakazawa; Kousuke Oonuki; Tadayuki Takahashi; Ken'ichi Tamura; Takaaki Tanaka; Yukikatsu Terada; Yasushi Fukazawa; Naomi Kawano; Kengo Kawashima; Masanori Ohno; Kazutaka Yamaoka; Keiichi Abe; Masaya Suzuki; Makoto Tashiro; Daisuke Yonetoku; Toshio Murakami
Proceedings of SPIE - The International Society for Optical Engineering, Volume：5501, First page：286, Last page：295, 01 Dec. 2004
The Hard X-ray Detector (HXD-II), one of instruments onboard the Astro-E2 satellite to be launched in February 2005, is in the final stage of its development. The HXD-II probes the universe in the energy range of 10-600 keV with a sensitivity by an order of magnitude better than those of previous missions. The assembly of the HXD-II completed in January 2004, followed by a series of pre-launch qualification tests. As a result, the design goals of the HXD-II have been met. These include; a background level of 5 × 10 -6 counts/s/keV/cm 2 at 200 keV for GSO and 1 × 10 -5 counts/s/keV/cm 2 at 30 keV for PIN; energy resolutions of 2.9 keV (PIN diode, at 59.5 keV) and 10 % (GSO scintillator, at 662 keV); and low energy thresholds of 10 keV for PIN diodes and 30 keV for GSO scintillators. The measured background predicts a continuum sensitivity of a few ×10 -6 photons/s/keV/cm 2 . Anti-Counter units surrounding the HXD-II provide 50 keV-5 MeV information on gamma-ray bursts and bright X-ray transients.
DOI：https://doi.org/10.1117/12.551051
DOI ID：10.1117/12.551051, ISSN：0277-786X, SCOPUS ID：19944367586 - High resolution fourier synthesis hard X-ray imaging based on CdTe strip detectors
Ryohei Miyawaki; Hisako Niko; Yuu Okada; Motohide Kokubun; Kazuo Makishima; Hitoshi Negoro; Jun'ichi Kotoku; Yukikatsu Terada; Takaaki Tanaka; Takefumi Mitani; Kazuhiro Nakazawa; Tadayuki Takahashi; Ryoichi Ohno; Minoru Funaki; Yoshikatsu Kuroda; Kei Genba; Mitsunobu Onishi
IEEE Nuclear Science Symposium Conference Record, Volume：7, First page：4392, Last page：4396, 01 Dec. 2004
Employing Fourier-synthesis optics and one-dimensional position-sensitive detectors, we are developing a novel hard X-ray imager which can work in the ∼10 keV to ∼200 keV range either as a telescope or a microscope. As the detection part of our imager, we have developed a strip detector made of Schottky CdTe diode, with its cathode divided into 64 channels of 150 μm pitch. Electrodes of all channels are gold-stud bonded to a fanout board, and connected to low noise analog ASIC. We read out signals from all channels simultaneously. As the grid optics elements, one-dimensional modulation collimator grids of 1 mm thick tungsten have been manufactured, with 10 grid pitches ranging from 0.2 mm to 2 mm with harmonic ratios. Combining the CdTe strip detector and the modulation collimators, we have verified hard X-ray imaging performance of this system. Specifically, by observing an241Am source, we have successfully obtained an image in the 10-70 keV range. © 2004 IEEE.
ISSN：1095-7863, SCOPUS ID：23844467438 - Design and performance of soft Gamma-ray detector for NeXT mission
H. Tajima; T. Kamae; G. Madejski; T. Mitani; K. Nakazawa; T. Tanaka; T. Takahashi; S. Watanabe; Y. Fukazawa; T. Ikagawa; J. Kataoka; M. Kokubun; K. Makishima; Y. Terada; M. Nomachi; M. Tashiro
IEEE Nuclear Science Symposium Conference Record, Volume：1, First page：314, Last page：321, 01 Dec. 2004
The Soft Gamma-ray Detector (SGD) on board NeXT (Japanese future high energy astrophysics mission) is a Compton telescope with narrow field of view (FOV), which utilizes Compton kinematics to enhance its background rejection capabilities. It is realized as a hybrid semiconductor gamma-ray detector which consists of silicon and CdTe (Cadmium Telluride) detectors. It can detect photons in a wide energy band (0.05-1 MeV) at a background level of 5 × 10-7counts/s/cm2/keV; the silicon layers are required to improve the performance at a lower energy band (<0.3 MeV). Excellent energy resolution is the key feature of the SGD, allowing to achieve both high angular resolution and good background rejection capability. An additional capability of the SGD, its ability to measure gamma-ray polarization opens up a new window to study properties of astronomical objects. We will present the development of key technologies to realize the SGD; high quality CdTe, low noise front-end ASIC and bump bonding tecnology. Energy resolutions of 1.7 keV (FWHM) for CdTe pixel detectors and 1.1 keV for Si strip detectors have been measured. We also present the validation of MC simulation used to evaluate the performance of the SGD. © 2004 IEEE.
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=23844483540&origin=inward
ISSN：1095-7863, SCOPUS ID：23844483540 - Activation Background of the Hard X‐ray Detector II (HXD‐II) Onboard Astro‐E2
村島未生; 川原田円; 国分紀秀; 岡田祐; 牧島一夫; 井上北斗; 小林謙仁; 三谷烈史; 中沢知洋; 高橋忠幸; HONG Soojing; 寺田幸功; 宮坂浩正; 山岡和貴; 川添哲志
宇宙航空研究開発機構研究開発報告 JAXA-RR-, Number：04-004, First page：26P, 01 Dec. 2004
Japanese
ISSN：1349-1113, J-Global ID：200902237717110104 - Improvements of the Astro-E2 Hard X-ray Detector (HXD-II)
M Kokubun; K Abe; Y Ezoe; Y Fukazawa; S Hong; H Inoue; T Itoh; T Kamae; D Kasama; M Kawaharada; N Kawano; K Kawashima; S Kawasoe; Y Kobayashi; J Kotoku; M Kouda; A Kubota; GM Madejski; K Makishima; T Mitani; H Miyasaka; R Miyawaki; K Mori; M Mori; T Murakami; MM Murashima; K Nakazawa; H Niko; M Nomachi; M Ohno; Y Okada; K Oonuki; G Sato; M Suzuki; H Takahashi; Takahashi, I; T Takahashi; K Tamura; T Tanaka; M Tashiro; Y Terada; S Tominaga; S Watanabe; K Yamaoka; T Yanagida; D Yonetoku
IEEE TRANSACTIONS ON NUCLEAR SCIENCE, Volume：51, Number：5, First page：1991, Last page：1996, Oct. 2004
We summarize significant improvements which have been achived in the development of Astro-E2 Hard X-ray Detector (HXD-II). An expanded energy range and better energy resolution have been achieved from progresses in device materials and redesigning of the front-end electronics. An improved estimation for the detector background in orbit has also been conducted based upon results from our proton irradiation experiment. The sensitivity of HXD-II can be expected to reach an order of 10(-6) [c s(-1) keV(-1) cm(-2)].
IEEE-INST ELECTRICAL ELECTRONICS ENGINEERS INC, English
DOI：https://doi.org/10.1109/TNS.2004.832921
DOI ID：10.1109/TNS.2004.832921, ISSN：0018-9499, SCOPUS ID：8344229310, Web of Science ID：WOS:000224490900011 - 28aSD-8 PreFlight Calibration and Performance of the Astro-E2/HXD-II Anti Counter as the All Sky Monitor
Ohno Masanori; Fukazawa Yasushi; Yamaoka Kazutaka; Tsutsui Akihito; Makishima Kazuo; Kokubun Motohide; Terada Yukikatsu; Kotoku Junichi; Tashiro Makoto; Hong Soojing; Mori Masanori; Murakami Toshio; Takahashi Tadayuki; Nakazawa Kazuhiro
Meeting abstracts of the Physical Society of Japan, Volume：59, Number：2, First page：76, Last page：76, 25 Aug. 2004
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002050716, CiNii Books ID：AA11439205 - 28pSD-11 The search for optical emission on and before the GRB with the WIDGET
Abe K; Tamagawa T; Usui F; Terada Y; Urata Y; Onda K; Tashiro M; Fujiwara H; Miura N; Hirose S; Makishima K; Mori M; Kawai N; Yoshida A
Meeting abstracts of the Physical Society of Japan, Volume：59, Number：2, First page：80, Last page：80, 25 Aug. 2004
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002050772, CiNii Books ID：AA11439205 - 27aZE-2 A search for cyclotron resonance features with the INTEGRAL observatory
Okada Yuu; Niko Hisako; Kokubun Motohide; Makishima Kazuo; Mihara Takehiro; Nakajima Motoki; Terada Yukikatsu
Meeting abstracts of the Physical Society of Japan, Volume：59, Number：1, First page：78, Last page：78, 03 Mar. 2004
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002184478, CiNii Books ID：AA11439205 - 28aZK-10 Verification of Fourier Synthesis Hard X-ray Imager using one-dimensional CdTe detector
Miyawaki R; Niko H; Okada Y; Kotoku J; Kokubun M; Makishima K; Tanaka T; Mitani T; Nakazawa K; Takahashi T; Negoro H; Terada Y
Meeting abstracts of the Physical Society of Japan, Volume：59, Number：1, First page：89, Last page：89, 03 Mar. 2004
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002184671, CiNii Books ID：AA11439205 - NeXTによる核γ線観測でひらく新しい物理
寺田 幸功; 望月 優子; 玉川 徹
Volume：4, First page：51, Last page：54, 08 Jan. 2004
Japanese
CiNii Articles ID：40007259372, CiNii Books ID：AA11571712 - Si/CdTe semiconductor Compton camera
Shin Watanabe; Takaaki Tanaka; Kazuhiro Nakazawa; Takefumi Mitani; Kousuke Oonuki; Tadayuki Takahashi; Takeshi Takashima; Hiroyasu Tajima; Yasushi Fukazawa; Masaharu Nomachi; Shin Kubo; Mitsunobu Onishi; Yoshikatsu Kuroda
IEEE Nuclear Science Symposium Conference Record, Volume：7, First page：4286, Last page：4290, 2004
We are developing a Compton camera based on Si and CdTe semiconductor imaging devices with high energy resolution. In this paper, results from the most recent prototype are reported. The Compton camera consists of six stacked double-sided Si Strip detectors and CdTe pixel detectors, which are read out with low noise analog ASICs, VA32TAs. We obtained Compton reconstructed images and spectra of line gamma-rays from 80 keV to 662 keV. The energy resolution (FWHM) is 10 keV and 16 keV at 356 keV and 511 keV, respectively. © 2004 IEEE.
Scopus：https://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=23844451402&origin=inward
Scopus Citedby：https://www.scopus.com/inward/citedby.uri?partnerID=HzOxMe3b&scp=23844451402&origin=inward
ISSN：1095-7863, SCOPUS ID：23844451402 - 太陽フレアにおける磁気ループ根元からのガンマ線放射
古徳純一; 古徳純一; 牧島一夫; 牧島一夫; 小浜光洋; 寺田幸功; 玉川徹
Volume：2004, 2004
ISSN：1347-0639, J-Global ID：201302241298530017 - Astro‐E2衛星搭載硬X線検出器(HXD‐II)主検出部の打ち上げ前較正試験
村島未生; 川原田円; 二河久子; 宮脇良平; 高橋勲; 国分紀秀; 牧島一夫; 三谷烈史; 渡辺伸; 中澤知洋; 川埜直美; 鈴木雅也; 田代信; 寺田幸功
日本天文学会年会講演予稿集, Volume：2004, First page：248, 2004
Japanese
ISSN：1347-0639, J-Global ID：201302236760898021 - Performance of a low noise front-end ASIC for Si/CdTe detectors in compton gamma-ray telescope
Hiroyasu Tajima; Tatsuya Nakamoto; Takaaki Tanaka; Shingo Uno; Takefumi Mitani; Eduardo Do Couto; E. Silva; Yasushi Fukazawa; Tuneyoshi Kamae; Grzegorz Madejski; Daniel Marlow; Kazuhiro Nakazawa; Masaharu Nomachi; Yu Okada; Tadayuki Takahashi
IEEE Nuclear Science Symposium Conference Record, Volume：1, First page：396, Last page：401, 01 Dec. 2003
Compton telescopes based on semiconductor technologies are being developed to explore the gamma-ray universe in an energy band 0.1-20 MeV, which is not well covered by the present or near-future gamma-ray telescopes. The key feature of such Compton telescopes is the high energy resolution that is crucial for high angular resolution and high background rejection capability. The energy resolution around 1 keV is required to approach physical limit of the angular resolution due to Doppler broadening. We have developed a low noise front-end ASIC, VA32TA, to realize this goal for the readout of Double-sided Silicon Strip Detector (DSSD) and Cadmium Telluride (CdTe) pixel detector which are essential elements of the semiconductor Compton telescope. We report on the design and test results of the VA32TA. We have reached an energy resolution of 1.3 keV (FWHM) for 60 keV and 122 keV at 0̊ Cwith a DSSD and 1.7 keV (FWHM) with a CdTe detector.
ISSN：1095-7863, SCOPUS ID：19944426961 - Prototype of Compton Camera using high resolution Si/CdTe detectors - Si/CdTe Compton Camera as a polarimeter
Takefumi Mitani; Takaaki Tanaka; Kazuhiro Nakazawa; Tadayuki Takahashi; Takeshi Takashima; Hiroyasu Tajima; Hidehito Nakamura; Masaharu Nomachi; Tatsuya Nakamoto; Yasushi Fukazawa
IEEE Nuclear Science Symposium Conference Record, Volume：5, First page：3588, Last page：3592, 01 Dec. 2003
To bring a breakthrough in the observation of the gamma-ray universe, we are working on the development of Semiconductor Multi-Compton Telescope(SMCT). In the SMCT, all the energy, positional and timing resolution must be high to ensure high sensitivity. The imaging device based on the high resolution CdTe diode and Si, such as CdTe pixel detectors and Double-sided Si Strip Detectors (DSSDs), are promising candidates for the components of the SMCT. Here we report the results of a CdTe pixel detector connected with a low noise analog ASIC. We obtained an energy resolution of 2.5 keV(FWHM) at 122 keV, with a positional resolution of 2 mm. Performance of the first prototype Compton Camera using a DSSD and two CdTe pixel detectors is also described. We irradiated 100% linearly polarised 170 keV γ-ray line to the system and obtained the polarimetric modulation factor of 43%.
ISSN：1095-7863, SCOPUS ID：19944428930 - Design and Performance of Digital Electronics of HXD-II
Takahashi Hiromitsu; Kokubun Motohide; Makishima Kazuo; Tashiro Makoto; Suzuki Masaya; Terada Yukikatsu; Takahashi Tadayuki; Nakazawa Kazuhiro; Fukazawa Yasushi; HXD team
Meeting abstracts of the Physical Society of Japan, Volume：58, Number：2, First page：13, Last page：13, 15 Aug. 2003
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002058382, CiNii Books ID：AA11439205 - Gurrent status of the Astro-E2 Hard X-ray Detector (2)
Kokubun M.; Makishima K.; Nakazawa K.; Takabashi T.; Fukazawa Y.; Tashiro S.; Yamaoka K.; Terada Y.; Yonetoku D.; Murakami T.; Nomachi M.; Kamae T.; HXD-H team
Meeting abstracts of the Physical Society of Japan, Volume：58, Number：2, First page：80, Last page：80, 15 Aug. 2003
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002058831, CiNii Books ID：AA11439205 - The response of the HXD-II onboard Astro-E2 to cosmic particles
Kawaharada M.; Kokubun M.; Makishima K.; Kou H.; Terada Y.; Miyasaka H.; Yamaoka K.; Ohno M.; Fukazawa Y.; Inoue H.; Takahashi T.; HXD members
Meeting abstracts of the Physical Society of Japan, Volume：58, Number：1, First page：68, Last page：68, 06 Mar. 2003
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002211866, CiNii Books ID：AA11439205 - Activation Background of the Astro-E2 Hard X-ray Detector II
Murakami Mio M.; Kawasoe S.; Kawaharada M.; Hong S. J.; Kobayashi Y.; Mitani T.; Inoue H.; Ohno M.; Mori M.; Okada Y.; Kotoku J.; Terada Y.; Kokubun M.; Nakazawa K.; Yamaoka K.; Miyasaka H.; Fukazawa Y.; Takahashi T.; Makishima K.; HXD team
Meeting abstracts of the Physical Society of Japan, Volume：58, Number：1, First page：68, Last page：68, 06 Mar. 2003
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002211870, CiNii Books ID：AA11439205 - Development of cosmic X-ray imaging system with CdTe strip detector and Fourier synthesis optics
Okada Yuu; Miyawaki Ryouhei; Kotoku Junnichi; Kokubun Motohide; Makishima Kazuo; Takahashi Tadayuki; Terada Yukikatsu; Negoro Hitoshi
Meeting abstracts of the Physical Society of Japan, Volume：58, Number：1, First page：93, Last page：93, 06 Mar. 2003
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002212240, CiNii Books ID：AA11439205 - 28pSL-2 Astro-E2 衛星で狙う硬 X 線物理学
牧島 一夫; 国分 紀秀; 高橋 忠幸; 中澤 知洋; 深沢 泰司; 田代 信; 山岡 和貴; 寺田 幸功; 村上 敏夫; 米徳 大輔; 能町 正治; 釜江 常好; HXD team
Volume：58, Number：1, First page：89, Last page：89, 06 Mar. 2003
Japanese
ISSN：1342-8349, CiNii Articles ID：110002212169, CiNii Books ID：AA11439205 - 太陽フレアで加速された粒子のエネルギースペクトルの推定
古徳純一; 玉川徹; 小浜光洋; 寺田幸功; 牧島一夫
Volume：2003, 2003
ISSN：1347-0639, J-Global ID：201302216893673129 - 一次元半導体検出器とフーリエ光学系を用いた高空間分解能ガンマ線イメージャーの開発
岡田祐; 宮脇良平; 古徳純一; 国分紀秀; 牧島一夫; 高橋忠幸; 寺田幸功; 根来均
Volume：2003, 2003
ISSN：1347-0639, J-Global ID：201302233377438590 - 狭視野型軟γ線コンプトンカメラの感度の見積もり
川埜直美; 阿部由紀子; 中本達也; 川添哲志; 深沢泰司; 三谷烈史; 中澤知洋; 高橋忠幸; 寺田幸功; 田代信; 国分紀秀; 牧島一夫
日本天文学会年会講演予稿集, Volume：2003, First page：249, 2003
Japanese
ISSN：1347-0639, J-Global ID：201302251523318842 - Low noise double-sided silicon strip detector for multiple-compton gamma-ray telescope
Hiroyasu Tajima; Tuneyoshi Kamae; Shingo Uno; Tatsuya Nakamoto; Yasushi Fukazawa; Takefumi Mitani; Tadayuki Takahashi; Kazuhiro Nakazawa; Yu Okada; Masaharu Nomachi
Proceedings of SPIE - The International Society for Optical Engineering, Volume：4851, First page：875, Last page：884, 01 Dec. 2002
A Semiconductor Multiple-Compton Telescope (SMCT) is being developed to explore the gamma-ray universe in an energy band 0.1-20 MeV, which is not well covered by the present or near-future gamma-ray telescopes. The key feature of the SMCT is the high energy resolution that is crucial for high angular resolution and high background rejection capability. We have developed prototype modules for a low noise Double-sided Silicon Strip Detector (DSSD) system which is an essential element of the SMCT. The geometry of the DSSD is optimized to achieve the lowest noise possible. A new front-end VLSI device optimized for low noise operation is also developed. We report on the design and test results of the prototype system. We have reached an energy resolution of 1.3 keV (FWHM) for 60 keV and 122 keV at 0°C.
DOI：https://doi.org/10.1117/12.461511
DOI ID：10.1117/12.461511, ISSN：0277-786X, SCOPUS ID：0038633543 - Development of Digital Electronics of Hard X-ray Detector on board Astro-E2(HXD2)
Terada Y.; Tashiro S.; Ezoe Y.; Takahashi H.; Suzuki M.; Mitani T.; Kokubun M.; Nakazawa K.; Yamaoka K.; Takahashi T.; Makishima K.; HXDteam
Meeting abstracts of the Physical Society of Japan, Volume：57, Number：2, First page：80, Last page：80, 13 Aug. 2002
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110009718131, CiNii Books ID：AA11439205 - Development of All-Sky-Monitor of Astro-E2HXD-II(2)
Hong S.; Yamaoka K.; Terada Y.; Kotoku J.; Mori M.; Tashiro M.; Fukazawa Y.; Kawasoe S.; Ohno M.; Takahashi T.; Kokubun M.; Makishima K.
Meeting abstracts of the Physical Society of Japan, Volume：57, Number：2, First page：80, Last page：80, 13 Aug. 2002
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110009718129, CiNii Books ID：AA11439205 - Astro-E2衛星硬X線検出器(HXD-11)のシールド部の開発
洪秀徴; 洪秀徴; 山岡和貴; 寺田幸功; 深沢泰司; 川添哲志; 大野雅功; 森正統; 田代信; 高橋忠幸; 古徳純一; 国分紀秀; 牧島一夫
Volume：2002, 2002
ISSN：1347-0639, J-Global ID：201402168858119006 - フーリエ・ベッセル合成を用いた宇宙硬X線撮像光学系の基礎研究
古徳純一; 寺田幸功; 牧島一夫
Volume：2001, 2001
ISSN：1347-0639, J-Global ID：201402110318375056 - ASTRO-E衛星硬X線検出器(HXD)アンチカウンタの応答関数の構築
古徳純一; 山岡和貴; 寺田幸功; 国分紀秀; 牧島一夫; 釜江常好; 高橋忠幸; 村上敏夫
Volume：2000, 2000
ISSN：1347-0639, J-Global ID：201402111141331165 - Measurement of the Response of the ASTRO-E Hare X-ray Detecto
ISOBE N.; TERADA Y.; MATSUMOTO Y.; TANIHATA T.; MAKISHIMA K.; KAMAE T.; TAKAHASHI T.; TASHIRO M.; FUKAZAWA Y.; KOKUBUN M.; YAMAOKA K.; NAKAZAWA K.; HXD TEAM
Meeting abstracts of the Physical Society of Japan, Volume：53, Number：2, First page：82, Last page：82, 05 Sep. 1998
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110001988592, CiNii Books ID：AA11439205 - Evaluation Test of Photomultiplier Tube for Hard Xray Detector on bord ASTRO-E
TERADA Y.; MIZUNO T.; FUKAZAWA Y.; MAKISHIMA K.; KAMAE T.; TAKAHASHI T.; KATAOKA J.; TANIHATA T.; HXD TEAM
Meeting abstracts of the Physical Society of Japan, Volume：53, Number：1, First page：56, Last page：56, 10 Mar. 1998
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110002173783, CiNii Books ID：AA11439205 - Monte Carlo evaluation of the ASTRO-E Hard X-ray Detector
KOKUBUN M; FUKAZAWA Y; MAKISHIMA K; MATSUZAKI K; MATSUMOTO Y; YAMAOKA K; HXD TEAM; ISOBE N; KAMAE T; KUBOTA A; TAKAHASHI T; TANIHATA C; TASHIRO M; TERADA Y; NAKAZAWA K
Meeting Abstracts of the Physical Society of Japan, Volume：53, Number：0, 1998
一般社団法人 日本物理学会, Japanese
CiNii Articles ID：110001988591 - 23p-J-5 The performance test of Photomultiplier Tube for Hard X-ray Detector(HXD) on bord ASTRO-E
Mizuno T.; Terada Y.; Fukazawa Y.; Makishima K; Kamae T.; Takahashi T.; HXD Team
Meeting abstracts of the Physical Society of Japan, Volume：52, Number：2, First page：82, Last page：82, 02 Sep. 1997
The Physical Society of Japan (JPS), Japanese
ISSN：1342-8349, CiNii Articles ID：110001981299, CiNii Books ID：AA11439205
- 宇宙物理学ハンドブック
高原文郎,家正則,小玉英雄, 高橋忠幸 他
朝倉書店, Jan. 2020
Total pages：912
ISBN：9784254131277 - Science with the Cherenkov Telescope Array
CTA Consortium
World Scientific Publishing Co. Pte. Ltd.,, Jan. 2019
Total pages：365
ISBN：9789813270091 - High Energy Emission from Pulsars and their Systems
Nanda Rea and Diego F.Torres (Edittors), Y.Terada ほか 97名
Springer, 2010
Total pages：641 - High Energy Emission from Pulsars and their Systems
Nanda Rea and Diego F.Torres (Edittors), Y.Terada ほか 97名
Springer Press
Total pages：641
- X線分光撮像衛星XRISMの時刻システム構築および軌道上精度評価
寺田幸功ほか
Mar. 2024, [Domestic conference] - Latest status and expectations for the recently born X-ray observatory XRISM (the X-Ray Imaging and Spectroscopy Mission)
Terada, Yukikatsu
Feb. 2024, [International conference] - XRISM衛星アーカイブに向けた地上高次データ処理の開発
寺田幸功
Feb. 2024, [Domestic conference] - IACHEC Timing Working Group Status
Terada, Yukikatsu et. al.
Apr. 2023, [International conference] - XRISM Timing System Design and Timing Accuracy
Terada Yukikatsu et. al.
Apr. 2023, [International conference] - Current status of the XRISM
Terada, Yukikatsu et. al.
Apr. 2023, [International conference] - XRISM 衛星科学運用に向けた準備進捗２０２２年度
寺田幸功、田代信、ほか 35名
Jan. 2023, [Domestic conference] - 高感度核ガンマ線観測で拓く宇宙r-process 重元素合成
寺田 幸功 (埼玉大)
Nov. 2022, [Domestic conference] - 銀河系内中性子星連星合体残骸からの核ガンマ線放射診断
寺田幸功(埼玉大,JAXA), 三輪祐也(埼玉大), 大住隼人(埼玉大), 藤本信一郎(熊本高専), 勝田哲(埼 玉大), 馬場彩(東大), 山崎了(青山学院大)
日本天文学会2022年秋季年会講演予稿集, Sep. 2022, [Domestic conference] - Gamma-ray Diagnostics of r-process Nucleosynthesis in the Remnants of Galactic Binary Neutron-Star Mergers
Y.Terada, Y.Miwa, H.Ohsumi, S.Fujimoto, S.Katsuda, A.Bamba, R.Yamazaki
Jul. 2022, [International conference] - Timing Working Group Report
Yukikatsu Terada et al
May 2022, [International conference] - 線分光撮像衛星XRISM 時刻システムの地上評価検証
寺田幸功(埼大, ISAS/JAXA), 高橋弘充(広大), 飯塚亮(ISAS/JAXA), 林克洋(ISAS/JAXA), 志達 めぐみ(愛媛大), 加藤颯(埼大), 佐藤諒平(埼大), 他XRISM Mission Operation Preparation Team, 小湊隆(日本電気)
日本天文学会春季年会2022年会予稿集, Mar. 2022, [Domestic conference] - XRISM 衛星科学運用に向けた準備進捗２０２１年度
寺田幸功 ほか33名
Jan. 2022, [Domestic conference] - Timing Working Group Status
Yukikatsu Terada et al.
Nov. 2021, [International conference] - 中性子星連星合体イベントのガンマ線残光の探査
寺田幸功
Aug. 2021, [Domestic conference] - 核ガンマ線を用いた銀河系内中性子星連星合体残骸の探査
寺田幸功
Aug. 2021, [Domestic conference] - Timing Working Group Status
Yukikatsu Terada et al.
May 2021, [International conference] - Theoretical Estimations and Observational Systematic Survey of R-process Gamma-rays from Galactic Kilonova Remnants
Terada Yukikatsu , Miwa Yuya , Fujimoto Sihichiro , Katsuda Satoru , Bamba Aya , Yamazaki Ryo
Jan. 2021, [International conference] - XRISM 衛星科学運用に向けた準備進捗２０２０年度
寺田幸功, 田代信, 高橋弘充, 信川正順, 水野恒史, 宇野伸一郎, 久保田あや, 中澤知洋, 渡辺伸, 飯塚亮, 佐藤理江, 林克洋, Baluta Chris, 海老沢研, 江口智士, 深沢泰司, 勝田哲, 北口貴雄, 小高裕和, 大野雅功, 太田直美, 志達めぐみ, 菅原泰晴, 谷本敦, 寺島雄一, 坪井陽子, 内田悠介, 内山秀樹, 山内茂雄
Jan. 2021, [Domestic conference] - Detail plans and preparations for the science operations of the XRISM mission
Terada Y., Holland M., Loewenstein M., Tashiro M., and other 34 authors
Proceedings of the SPIE, Dec. 2020, [International conference] - 連星中性子星合体残骸の核ガンマ線探査
寺田幸功, 三輪祐也, 藤本信一郎, 勝田哲, 馬場彩, 山崎了
Mar. 2020, [Domestic conference] - Numerical Estimation and Observational Searches for Nuclear Gamma-rays from Galactic Kilonova Remnants
Yukikatsu Terada
Feb. 2020, [International conference] - XRISM 衛星の科学運用計画とその準備進捗
寺田幸功, 田代信, 高橋弘充, 信川正順, 水野恒史, 田村隆幸, 宇野伸一郎, 久保田あや, 中澤知洋, 渡辺伸, 飯塚亮, 佐藤理江, 海老沢研, 深沢泰司, 勝田哲, 北口貴雄, 中島真也, 大野雅功, 太田直美, 志達めぐみ, 菅原泰晴, 寺島雄一, 坪井陽子, 内田悠介, 内山秀樹, 山内茂雄
Jan. 2020, [Domestic conference] - Systematic Survey of Nuclear Gamma-rays from Galactic Kilonova Remnants
Yukikatsu Terada
Oct. 2019, [International conference] - Science Operations Team Responsibility and Status Report
Y. Terada, M. Holland, M. Loewenstein
Oct. 2019, [International conference] - 超高精度分光で探る将来X線宇宙物理と太陽物理研究とのシナジー
寺田幸功
Sep. 2019, [Domestic conference] - XRISM Science Operations Plan
Yukikatsu Terada
May 2019, [International conference] - PhoENiXへの期待：白色矮星での非熱的X線の観測
寺田幸功
Nov. 2018, [Domestic conference] - Search for Possible Gamma-rays from Galactic Kilonova Remnants
Yukikatsu Terada
Nov. 2018, [International conference] - Suzaku/Hitomi Science Operations
Yukikatsu Terada
Nov. 2018, [International conference] - Suzaku/Hitomi Analyses school
Yukikatsu Terada
Nov. 2018, [International conference] - 高エネルギー宇宙物理連絡会が関与する飛翔体将来計画概要
寺田幸功
Sep. 2018, [Domestic conference] - Observational approaches on the nature of Type Ia Supernovae with near Future X-ray Missions
Yukikatsu Terada
Proceeding of 15th Marcel Grossmann Meeting, Jul. 2018, [International conference] - X線ガンマ線による中性子星連星合体からの核ガンマ線の探査計画
寺田幸功,
Jun. 2018, [Domestic conference] - Systematic survey of Galactic Kilonova Remnant in Soft gamma-rays
Yukikatsu Terada
Jun. 2018, [International conference] - Science Operations Team
Y.Terada, S.Watanabe, H.Takahashi, T.Mizuno, Y.Terashima, S. Uno, M Loewenstein, M. Holland, K. Mukai, E.Miller et al.
May 2018, [International conference] - Introduction of the 14th IACHEC meeting
Y. Terada, M.Tsujimoto, K.Mori, H.Nakajima
Apr. 2018, [International conference] - Timing calibration Session chair report
Yukikatsu Terada
Apr. 2018, [International conference] - The XARM mission status and science operations plan
Yukikatsu Terada
Apr. 2018, [International conference] - X 線衛星代替機XARM における科学運用計画
寺田幸功ほか24名
日本天文学会 2018年春季年会予稿集, Mar. 2018, [Domestic conference] - ひとみ」電波 Crab 同時観測による Giant radio pulse に同期したX線増光の探査
寺田幸功
Mar. 2018, [Domestic conference] - X線衛星代替機における科学運用の計画概要
寺田幸功、ほか24名
第18回宇宙科学シンポジウム, Jan. 2018, [Domestic conference] - Science and Mission Operations team status
寺田幸功ほか
Dec. 2017, [Domestic conference] - 「ひとみ」衛星による Crab Giant radio pulse のX線電波同時観測
Yukikatsu Terada
Nov. 2017, [Domestic conference] - Status of the X-ray Astronomy Recovery Mission (XARM)
Terada, Y, and Tashiro M.
Mar. 2017, [International conference] - Time assignment anomalies of Suzaku
S.Koyama, Y.Terada, et al,
Mar. 2017, [International conference] - Verification of GPS synchronization function for the time assignment of Hitomi
K.Oshimizu, Y.Terada, et al
Mar. 2017, [International conference] - Summary of Hitomi Timing calibration
Terada, Yukikatsu et al
Mar. 2017, [International conference] - Short burst from AXP 1E1547.0-5408, (review of PhD thesis by T. Yasuda)
Y.Terada and T.Yasuda
Mar. 2017, [International conference] - Ｘ線天文衛星「ひとみ」と電波の同時観測による 「かに星雲」パルサーからの Giant radio pulse のX 線特性
寺田幸功ほか
Mar. 2017, [Domestic conference] - Ia型超新星 SN2014Jの「すざく」sub MeV 観測レビューと将来 MeV観測
寺田幸功ほか
Feb. 2017, [Domestic conference] - Timing analyses and calibrations of Crab pulsar with Hitomi
Terada, Yukikatsu et al
Feb. 2017, [International conference] - Hitomi Software/Calibration Team: Report on Recent Activities
Terada Yukikatsu, Angelini Lorella, et al.
Feb. 2017, [International conference] - Future high-sensitive gamma-ray observations of nucleosynthesis nuclei in neutron star mergers
Terada, Yukikatsu et al
Dec. 2016, [International conference] - 「すざく」衛星による宇宙エックス線背景放射の軟ガンマ線観測
寺田幸功ほか
Sep. 2016, [Domestic conference] - X線天文衛星「ひとみ(ASTRO-H)」塔載機器の解析ソフトウェアの開発
寺田幸功ほか
Sep. 2016, [Domestic conference] - Soft gamma-ray Observation of SN2014J with Suzaku
Yukikatsu Terada, Keiich Maeda, Yasushi Fukazawa, Aya Bamba, Yoshihiro Ueda, Satoru Katsuda, Teruaki Enoto, Tadayuki Takahashi, Toru Tamagawa, Friedrich Ropke, S, Alexander Summa, Roland Diehl
Jun. 2016, [International conference] - Hitomi software status, data distribution plan, analysis procedure & limitations
Y. Terada, L. Angelini , E. Miller H. Takahashi T. Yaqoob M. Lowenstein H. Yamaguchi H. Krimms M.Nobukawa M.Sawada,
May 2016, [International conference] - Hitomi SXS simulators
Terada, Yukikatsu
May 2016, [International conference] - MeV Gamma-ray Studies of Neutron Star Merger
Terada, Yukikatsu
Feb. 2016, [International conference] - White Dwarf Pulsars and Rotating White Dwarfs
Terada, Yukikatsu
Sep. 2015, [International conference] - Verification of Time assignment system for ASTRO-H with Function Detail data
Terada, Yukikatsu
Jul. 2015, [International conference] - Status and updates on pre-pipeline process for ASTRO-H mission
Yukikatsu Terada, ASTRO-H Software/Calibration team
Jul. 2015, [International conference] - Soft gamma-ray Continuum emission from SN2014J with Suzaku HXD
Terada, Yukikatsu
Jul. 2015, [International conference] - Review on the soft Gamma-ray observational studies of Supernovae as Nucleaosynthesis Sites
Terada, Yukikatsu
Jun. 2015, [International conference] - "「すざく」を用いたIa 型超新星SN2014J の硬エックス線観測"
寺田幸功(埼玉大)、前田啓一(京大)、玉川徹(理研)、馬場彩(青学)、高橋忠幸(ISAS)、深沢泰 司(広大)、榎戸輝揚(理研)、勝田哲(ISAS)
Mar. 2015, [Domestic conference] - ASTRO-H software/calibration, Status and updates on pre-pipeline process
Yukikatsu Terada, ASTRO-H Software/Calibration team
Mar. 2015, [International conference] - 「すざく」によるIa型超新星 SN2014J のToO硬X線観測
寺田幸功(埼玉大)、前田啓一(京大)、玉川徹(理研)、馬場彩(青学)、高橋忠幸(ISAS)、深沢泰 司(広大)、榎戸輝揚(理研)、勝田哲(ISAS)
Jan. 2015, [Domestic conference] - Suzaku spacecraft and instruments & ftools and Suzaku dedicated softwares
Y.Terada
Nov. 2014, [International conference] - Suzaku spacecraft and instruments & ftools and Suzaku dedicated softwares
Y.Terada
Nov. 2014, [International conference] - Design of the Time Assignment System for ASTRO-H and Its Performance Before Launch
Yukikatsu Terada∗, Sunao Yamaguchi∗, Shigenobu Sugimoto∗, Taku Inoue∗, Souhei Nakaya∗, Mina Ogawa† , Tadayasu Dotani†, Yoshitaka Ishisaki‡, Kazuyo Mizushima§, Takashi Kominato§, Hiroaki Mine§, Hiroki Hihara¶, Kaori Iwase¶, Tomomi Kouzu∗¶, Makoto S. Tashiro∗, Chikara Natsukari†, Masanobu Ozaki†, Motohide Kokubun†, Tadayuki Takahashi†, Satoko Kawakami¶, Masaru Kasahara¶, Susumu Kumagai¶, Lorella Angelini, Michael Witthoeft
IEEE Conference Record, Nov. 2014, [International conference] - ASTRO-H software/calibration, Software review & organization meetings on Science Operation
Yukikatsu Terada, ASTRO-H Software/Calibration team
Jul. 2014, [International conference] - ASTRO-H software/calibration, Current status of Pre-pipeline and the data distribution plan
Yukikatsu Terada, ASTRO-H Software/Calibration team
Jul. 2014, [International conference] - Summary of working group activity and status, Timing
Y.Terada, M.Nobukawa, K.Nobukawa, S.Koyama, H. Hamaguchi, K. Mukai, J. Kennea, L. Natalucci, C. Markwardt, B. LaMarr
May 2014, [International conference] - Calibration and software for the ASTRO-H Time assignment
Yukikatsu Terada et al.
May 2014, [International conference] - Suzaku Operations and Calibration Status
Y.Terada, E.Miller, and Suzaku team
May 2014, [International conference] - ASTRO-H衛星用時刻付けシステムの構築
寺田幸功, 山口直, 杉本樹信, 井上拓, 中谷創平, 小川美奈, 堂谷忠靖, 夏苅権, 尾崎正伸, 国分紀秀, 高橋忠幸,石崎欣尚,水島和代, 小湊隆, 峯弘昭, 檜原弘樹,岩瀬かほり
Mar. 2014, [Domestic conference] - Gamma-rays from supernovae and their remnants
Yukikatsu Terada
Feb. 2014, [International conference] - Systematic surveys of non-thermal emission from white dwarfs with Suzaku
Y.Terada, M.Asahina, T.Hayashi, A. Harayama, T.Dotani, M.Ishida, A.Bamba, K. Makishima, K.Mukai, Y.Urata, A. Nitta, O. de Jager, P.Chadwick, S. Wagner, D. Buckley
Feb. 2014, [International conference] - ASTRO-H Ground calibration status and software for time assignment
Yukikatsu Terada et al.
Feb. 2014, [Domestic conference] - ASTRO-H software/calibration, pre-pipeline and pipeline process
Yukikatsu Terada
Feb. 2014, [International conference] - 将来計画に関する検討会：めざすサイエンス
寺田幸功
Jan. 2014, [Domestic conference] - Cataclysmic Variables, Novae, and white dwarfs
Yukikatsu Terada
Sep. 2013, [International conference] - Suzaku spacecraft and instruments & ftools and Suzaku dedicated softwares
Yukikatsu Terada
Sep. 2013, [International conference] - ASTRO-H software and calibration: progress in time assignment and coordinate
Yukikatsu Terada et al.
Jul. 2013, [International conference] - ASTRO-H pre-pipeline process
Yukikatsu Terada et al.
Jul. 2013, [International conference] - Status of ASTRO-H
Ota N., Terada Y., et al.
International Astronomical Consortium for High Energy Calibration, Mar. 2013, [International conference] - Calibration status of Suzaku satellite
Miller E., Terada Y., et al.
International Astronomical Consortium for High Energy Calibration, Mar. 2013, [International conference] - すざく」による逃亡星 BD+43 3654 における粒子加速の探査
寺田幸功、馬場彩、山崎了、田代信、神頭知美、小山志勇
日本天文学会 春季年会, Mar. 2013, [Domestic conference] - What has been done and is missing on Time assignment software
Terada Y., Angelini L., et al.
the 9th ASTRO-H Science Meeting, Feb. 2013, [International conference] - What has been done and is missing on Pre Pipe line processing software
Terada Y., Angelini L., et al.
the 9th ASTRO-H Science Meeting, Feb. 2013, [International conference] - X-ray searches for new Galactic Particle-Acceleration sites with Suzaku
Terada Y., Harayama A., Hayashi T., and other 15 authors
X-ray astronomy, towards the next 50 years!, Sep. 2012, [International conference] - ASTRO-H衛星の科学解析用時刻づけソフトウェアの開発
寺田幸功、Lorella Angelini、神頭知美、上野遥、田代信、ほか9名
日本天文学会 秋季年会, Sep. 2012, [Domestic conference] - Summary of time assignment tool
Terada Y., Angelini L., et al.
the 8th ASTRO-H Science Meeting, Jul. 2012, [International conference] - Status and plan of the Software and Calibration Team activities
Terada Y., Angelini L., et al.
the 8th ASTRO-H Science Meeting, Jul. 2012, [International conference] - Review on High Energy observations in searches for Non-thermal emissions from Accelerated particles in Magnetic White Dwarfs
Terada Yukikatsu
the 13th Marcel Grossmann Meeting, Jul. 2012, [Invited], [International conference] - ASTRO-H 衛星と次世代ガンマ線望遠鏡 CTA で切り拓くガンマ線連星
寺田幸功(埼玉大), Josep M. Paredes, Pere Munar Adrover, Marc Ribo(バルセロナ大, スペイン), 長滝 重博 (京都大), 内藤 統也 (山梨学院大)
日本天文学会 春季年会, Mar. 2012, [Domestic conference] - ASTRO-H Time assignment system
Y.Terada, L.Angelini, R.Petre, Jan-Willem den Herder, K.Ishibashi, U.Hwang, H.Krimm, N.Ota, K.Mori, Y.Haba, H.Takahashi, M.Nobukawa, S.Yamada, T.Takahashi
the 7th Astro-H Science Meeting, Feb. 2012, [International conference] - ASTRO-H 衛星用の科学解析用ソフトウェア・キャリブレーション
Y.Terada, L.Angelini, R.Petre, Jan-Willem den Herder, K.Ishibashi, U.Hwang, H.Krimm, N.Ota, K.Mori, Y.Haba, H.Takahashi, M.Nobukawa, S.Yamada, T.Takahashi
第12回宇宙科学シンポジウム, Jan. 2012, [Domestic conference] - 「すざく」による逃亡星 BD+43~3654 からのエックス線検出
Y.Terada, M.Tashiro, A.Bamba, R.Yamazaki, T.Kozu, S.Koyama, H.Seta
日本天文学会 秋季年会, Sep. 2011, [Domestic conference] - 白色矮星パルサーのアイディアと X線γ線 観測現状
Y.Terada
研究会High Energy Observation of Pulsar Systems for Future Missions, Sep. 2011, [Domestic conference] - "First X-ray Detection from a Bow Shock Region of a Runaway Star, BD+43 3654, with Suzaku"
"Y.Terada, M.Tashiro, A.Bamba, R.Yamazaki, T.Kozu, S.Koyama, H.Seta"
"第四回「すざく」国際会議, Exploring the X-ray Universe: Suzaku and Beyond", Jul. 2011 - First X-ray Detection from a Bow Shock Region of a Runaway Star, BD+43 3654, with Suzaku
Y.Terada, M.Tashiro, A.Bamba, R.Yamazaki, T.Kozu, S.Koyama, H.Seta
第四回「すざく」国際会議, Exploring the X-ray Universe: Suzaku and Beyond, Jul. 2011, [International conference] - ASTRO-H Software/Calibration Documents
Y.Terada, L.Angelini, R.Petre, Jan-Willem den Herder, K.Ishibashi, U.Hwang, H.Krimm, N.Ota, K.Mori, Y.Haba, H.Takahashi, M.Nobukawa, S.Yamada, T.Takahashi
the 6th Astro-H Science Meeting, Jul. 2011, [International conference] - ASTRO-H Timing Analyses of a Fast-rotating Pulsars
Y.Terada, T.Kozu, S.Mineshige et al.
the 6th Astro-H Science Meeting, Jul. 2011, [International conference] - Challenges on ASTRO-H Data Analyses and Software: from Suzaku Lessons
Y.Terada, L.Angelini, R.Petre, J.W.denHerder
第６回International Astronomical Consortium for High Energy Calibration国際会議, Apr. 2011, [International conference] - ハードな強磁場白色矮星からの非熱的放射探査
寺田幸功、原山淳、堂谷忠靖、石田学、馬場彩、林多佳由、浦田裕次、玉川徹
Mar. 2011, [Domestic conference] - すざく」による強磁場激変星 V2487 OphとIGR~J00234+6141の観測
寺田幸功、原山淳、堂谷忠靖、石田学、馬場彩、林多佳由、浦田裕次
Mar. 2011, [Domestic conference] - Future with Astro-H, Data Processing
Y.Terada
the 5th Astro-H Science Meeting, Feb. 2011, [International conference] - Astro-H Calibration and Software
Y.Terada, L.Angelini, R.Petre, J.W.denHerder
the 5th Astro-H Science Meeting, Feb. 2011, [International conference] - 強磁場激変星 AM Her における降着プラズマ温度のX 線光度依存性の発見
寺田幸功, 石田学,馬場彩,向井浩二,林多佳由,原山淳
Sep. 2010, [Domestic conference] - Astro-H Mission: overview of Instruments and Science
Y.Terada
Harvard CfA seminor, Aug. 2010, [Invited], [International conference] - Astro-H calibration
Y.Terada
the 4th Astro-H Science Meeting, Aug. 2010, [International conference] - The International X-ray Observatory and other X-ray missions, expectations for pulsar physics
Y.Terada
High-energy emission from pulsars and their systems, Apr. 2010, [Invited], [International conference] - 可視・X線・TeV多波長同時観測を通じた白色矮星における粒子加速の検証
寺田幸功,原山淳,馬場彩,石田学,堂谷忠靖,林多佳由,中村良子,牧島一夫,向井浩二,新田敦子,Okkie de Jager,Paula Chadwick,Stefan Wagner,David Buckley
2010 - 「すざく」、H.E.S.S.、可視光による白色矮星パルサーの多波長同時観測
寺田幸功,原山淳,馬場彩,石田学,堂谷忠靖,林多佳由,中村良子,牧島一夫,向井浩二,新田敦子,Okkie de Jager,Paula Chadwick,Stefan Wagner,David Buckley
2010 - 可視・X線・TeV多波長同時観測を通じた白色矮星における粒子加速の検証
2010 - 「すざく」、H.E.S.S.、可視光による白色矮星パルサーの多波長同時観測
2010 - 「すざく」、 第二の白色矮星パルサー発見か?
寺田幸功、原山淳(埼玉大)、石田学、馬場彩(宇宙研)、林多佳由、塩野目雄(宇宙研・首都大)、向井浩二(NASA)、牧島一夫(東大・理研)
2009 - Systematic surveys of the non thermal emission from white dwarfs with Suzaku and INTEGRAL
2009
Poster presentation - Discovery of possible non-thermal emission from AM Hercules in the very low state with Suzaku — The second white dwarf pulsar ?? —
2009
Poster presentation - 「すざく」ヘルプデスク、ゲスト観測者サポートの三年
寺田幸功、ほか13名
2009
Poster presentation - 「すざく」、 第二の白色矮星パルサー発見か?
2009 - Systematic surveys of the non thermal emission from white dwarfs with Suzaku and INTEGRAL
Y.Terada, M.Ishida, K.Makishima, K.Mukai, T.Dotani, A.Bamba. T.Hayashi, A.Harayama, K.Morigami, S. Okada, R.Nakamura, and S.Naik
2009
Poster presentation - Discovery of possible non-thermal emission from AM Hercules in the very low state with Suzaku — The second white dwarf pulsar ?? —
Y.Terada, M.Ishida, A.Bamba,K.Mukai, K.Makishima, A.Harayama, T.Hayashi, T.Shionome, and K. Morigami
2009
Poster presentation - 「すざく」ヘルプデスク、ゲスト観測者サポートの三年
2009
Poster presentation - H.E.S.S. and Suzaku collaboration, White Dwarfs
2008 - 強磁場激変星みずがめ座AE星の降着流変動
寺田幸功、ほか10名
2008 - Suzaku Observation of a White Dwarf as a new Candidate of Cosmic-ray Origin
2008
Poster presentation - Suzaku Observation of a White Dwarf as a new Candidate of Cosmic-ray Origin
2008 - Suzaku observation of spinning white-dwarfs
2008 - Suzaku Discovery of Hard X-ray Pulsations from the Rotating Magnetized White Dwarf, AE Aquarii
2008
Poster presentation - 「すざく」衛星搭載硬X線検出器(HXD) 広帯域全天モニタ部の現状 (V)
寺田幸功、ほか30名
2008 - H.E.S.S. and Suzaku collaboration, White Dwarfs
寺田幸功
2008 - 強磁場激変星みずがめ座AE星の降着流変動
2008 - Suzaku Observation of a White Dwarf as a new Candidate of Cosmic-ray Origin
2008
Poster presentation - Suzaku Observation of a White Dwarf as a new Candidate of Cosmic-ray Origin
寺田幸功、ほか10名
2008 - Suzaku observation of spinning white-dwarfs
寺田幸功、ほか10名
2008 - Suzaku Discovery of Hard X-ray Pulsations from the Rotating Magnetized White Dwarf, AE Aquarii
寺田幸功、ほか9名
2008
Poster presentation - 「すざく」衛星搭載硬X線検出器(HXD) 広帯域全天モニタ部の現状 (V)
2008 - The current status, performance, and calibration plan of the HXD onboard Suzaku
2007 - Suzaku Discovery of Hard X-ray Pulsation from the Rotating Magnetized White Dwarf, AE Aquarii
2007
Poster presentation - 「すざく」による白色矮星からの非熱的パルス放射の発見
寺田幸功、ほか9名
2007 - X 線パルサーを用いた「すざく」衛星 硬X線検出器の時刻較正 (II)
寺田幸功、ほか30名
2007 - Timing Calibration of Suzaku HXD on the simultaneouscampain of Crab
2007 - The current status, performance, and calibration plan of the HXD onboard Suzaku
寺田幸功
2007, [Domestic conference] - Suzaku Discovery of Hard X-ray Pulsation from the Rotating Magnetized White Dwarf, AE Aquarii
寺田幸功、ほか9名
2007
Poster presentation - 「すざく」による白色矮星からの非熱的パルス放射の発見
2007 - X 線パルサーを用いた「すざく」衛星 硬X線検出器の時刻較正 (II)
2007 - Timing Calibration of Suzaku HXD on the simultaneouscampain of Crab
寺田幸功
2007, [Domestic conference]
- Exercises on Experimental Physics III"", 実習・実験
- Exercises on Experimental Physics II"", 実習・実験
- Seminars on Physics I"", 演習
- Topics Space Experiments for Astrophysics, 講義
- Special Theory of Relativity, 講義
- Topics of Astrophysic I
- Exercises on Experimental Physics Ⅲ, 実習・実験
- Exercises on Experimental Physics Ⅱ, 実習・実験
- Progress in Modern Physics, 講義
- Special Theory of Relativity, 講義
- Seminars on Physics II, 講義
- Seminars on Physics I, 講義
- Topics of Astrophysics II, 講義
- Topics Space Experiments for Astrophysics, 講義
- Seminars on Physics II"", 実習・実験
- Seminars on Physics I"", 実習・実験
- Topics of Astrophysics I, 講義
- Topics Space Experiments for Astrophysics, 講義
- Progress in Modern Physics, 講義
- Physics Experiment III, 実習・実験
- Physics Experiment II, 実習・実験
- Special Theory of Relativity, 講義
- Seminars on Physics II"", 実習・実験
- Seminars on Physics I"", 実習・実験
- Topics of Astrophysics II"", 講義
- Topics Space Experiments for Astrophysics, 講義
- Seminars on Physics II"", 実習・実験
- Seminars on Physics I"", 実習・実験
- Topics of Astrophysics I, 講義
- Topics Space Experiments for Astrophysics, 講義
- Seminars on Physics II"", 実習・実験
- Seminars on Physics I"", 実習・実験
- Topics of Astrophysics II"", 講義
- Topics Space Experiments for Astrophysics, 講義
- Progress in Modern Physics, 講義
- Physics Experiment III, 実習・実験
- Physics Experiment II, 実習・実験
- Special Theory of Relativity, 講義
- Basic Physics, 講義
- Progress in Modern Physics, 講義
- Physics Experiment III, 実習・実験
- Physics Experiment II, 実習・実験
- Special Theory of Relativity, 講義
- Topics of Physics I / II, 講義
- Topics Space Experiments for Astrophysics, 講義
- Topics of Astrophysics I, 講義
- Topics of Physics I / II, 実習・実験
- Physics Experiment II, 実習・実験
- Topics Space Experiments for Astrophysics, 講義
- Topics of Astrophysics II, 講義
- Physics Experiment II, 実習・実験
- Astrophysics, 講義
- Topics of Astrophysics I, 講義
■ Affiliated academic society
- Feb. 2011, COSMIC RAY RESEARCHERS CONGRESS
- Nov. 2006
- Oct. 2002, High Energy AstroPhysics Association in Japan
- Sep. 1998
- Sep. 1998
- -
- International Astronomical Union
- Toward understanding progenitors and explosion physics of core-collapse supernovae by mutual studies between observations and numerical simulations
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Scientific Research (B), 01 Apr. 2021 - 31 Mar. 2026
Saitama University
Grant amount(Total)：17030000, Direct funding：13100000, Indirect funding：3930000
Grant number：21H01121 - Study of the origin of the diversity of Type Ia Supernovae with high energy-resolution X-ray spectroscopy
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Scientific Research (C), 01 Apr. 2020 - 31 Mar. 2025
Saitama University
Grant amount(Total)：4420000, Direct funding：3400000, Indirect funding：1020000
Grant number：20K04009 - Systematic searches for soft-gamma-ray remnants of gravitational-wave astronomical objects in our Galaxy
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Scientific Research on Innovative Areas (Research in a proposed research area), 01 Apr. 2018 - 31 Mar. 2020
Saitama University
Grant amount(Total)：2600000, Direct funding：2000000, Indirect funding：600000
Grant number：18H04571 - 高感度軟ガンマ線観測による重力波天体キロノバでの重元素合成の探査
01 Apr. 2015 - 31 Mar. 2017
寺田幸功
Grant amount(Total)：4290000, Direct funding：3300000, Indirect funding：990000
Grant number：15H00773 - High sensitive searches for the non-thermal emission from white dwarfs to verify a new Cosmic-ray origin
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Scientific Research (B), 01 Apr. 2011 - 31 Mar. 2016
TERADA Yukikatsu; ISHIDA Manabu; BAMBA Aya, Saitama University
Grant amount(Total)：15860000, Direct funding：12200000, Indirect funding：3660000
The origin of Cosmic-rays, which are high energy particles from the universe, is a long standing mystery for hundred years since its discovery. Before this research, theoretical and observational approaches for the Cosmic-ray origins are achieved mainly on very energetic sites. Our approach is on the magnetic white dwarfs, which may show the same kind of non-thermal activities in the magnetosphere of neutron stars. As a result, a possibility that magnetic white dwarfs can generate Cosmic-rays is shown observationally from the X-ray and gamma-ray observations. In addition, basic studies to use future X-ray high sensitive missions and/or high energy gamma-ray telescopes are also performed.
Grant number：23340055 - Multiwavelength observational study on ultra-relativistic jets
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Scientific Research (B), 01 Apr. 2010 - 31 Mar. 2015
TASHIRO Makoto; TERADA Yukikatsu; TAMAGAWA Toru, Saitama University
Grant amount(Total)：15080000, Direct funding：11600000, Indirect funding：3480000
Gamma-Ray Bursts (GRBs) and Active Galactic Nuclei (AGNs) are the two archetypical phenomena among astrophysical jets. This study consists of multi-wavelength observational study of these objects to investigate (A) the life of the jets, (B) physics of radiation region, and (C) circumstances including intergalactic warm-hot plasma. Through this study we realized that: the life time of AGN jets is up to 100 Myears with a fairly constant energy ejection; the radiation of the GRB prompt emission consists both of non-thermal synchrotron and thermal blackbody like emissions. We also developed X-ray micro-calorimeter system for the next generation X-ray observatory ASTRO-H and made observation plan to reveal warm-hot intergalactic medium irradiated by GRB or relativistically beamed AGN jets.
Grant number：22340039 - High sensitive study of Cosmic X-ray Background with Suzaku
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Young Scientists (B), 2007 - 2009
TERADA Yukikatsu, Saitama University
Grant amount(Total)：3570000, Direct funding：3000000, Indirect funding：570000
The main purpose of this research is to search for an origin of the Cosmic X-ray background emission (CXB), which comes from everywhere in the universe. The origin is a long standing mystery. We have observed the CXB emission in the hard X-ray band, where the energy density of the CXB becomes at peak. We used the hard X-ray detector, HXD, onboard Suzaku, which has the highest sensitivity in the world. With this research, the systematic errors of estimation of the noise events of the HXD were reduced to make the best use of its sensitivity. We have successfully measured the hard X-ray spectra of the CXB, and tested the model of the active-galactic-nuclei origin.
Grant number：19740168 - Theoretical Research for Synthesis of Uranium Elements in Supernovas
Japan Society for the Promotion of Science, Grants-in-Aid for Scientific Research, Grant-in-Aid for Scientific Research (C), 2004 - 2006
YUKO Motizuki; MADOKORO Hideki; SHIMIZU Tetsuya; TAMAGAWA Toru; TERADA Yukikatsu, The Institute of Physical and Chemical Research
Grant amount(Total)：3100000, Direct funding：3100000
The origin of heavy elements from iron to uranium is a mystery. It is believed that such heavy elements were created by the rapid neutron capture process (the r-process), in which seed nuclei captures many neutrons very rapidly in a very short time. Core-collapse supernovae have been suggested for the last 50 years to be the first candidate to host the r-process nucleosynthesis. The biggest problem here is that, except a few cases, hydrodynamical simulations could not have produced high-enough entropy to lead to a successful r-process up to its 3rd peak. In this research, we have demonstrated that a 2-Dimensional hydrodynamical simulation can naturally attain such a high entropy required for the r-process. In addition, our models have features of neutron richness and a fast expansion. All of these are essential requirements for a successful supernova model to give an environment for the r-process nucleosynthesis. It is thus very promising to study the r-process nucleosyntheis based on our hydrodynamical simulations of core-collapse supernovae. In this research, we have also developed the base of nuclear reaction network supercomputing calculations, and have investigated the detection possibilities of nuclear gamma-rays from the r-process nuclides and electron-capture decay X-rays from titanium and nickel isotopes, with future Japanese X-ray satellites, NeXT and Suzaku, respectively.
Grant number：16540277 - 軟γ線観測による太陽での粒子の加速機構の解明
2004 - 2005
寺田幸功
Grant amount(Total)：3400000, Direct funding：3400000
Grant number：16740160 - 硬X線観測による超新星残骸での粒子加速の研究
1999 - 2001
Grant amount(Total)：2700000, Direct funding：2700000
Grant number：99J09908 - －
Competitive research funding - -
Competitive research funding