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  2. 寺田 幸功

寺田 幸功

テラダ ユキカツ  (Yukikatsu Terada)

基本情報

所属
埼玉大学 大学院理工学研究科 理工学研究科  教授
国立研究開発法人宇宙航空研究開発機構 宇宙科学研究所 特任教授
学位
博士(2002年3月 東京大学)
J-GLOBAL ID
200901062224980497
researchmap会員ID
1000368169
外部リンク

研究キーワード

 14

研究分野

 2

経歴

 8
もっとみる

学歴

 3

委員歴

 2

論文

 372
  • Makoto Tashiro, Richard Kelley, Shin Watanabe, Hironori Maejima, Lillian Reichenthal, Kenichi Toda, Leslie Hartz, Andrea Santovincenzo, Kyoko Matsushita, Hiroya Yamaguchi, Robert Petre, Brian Williams, Matteo Guainazzi, Elisa Costantini, Yoh Takei, Yoshitaka Ishisaki, Ryuichi Fujimoto, Joy Henegar-Leon, Gary Sneiderman, Hiroshi Tomida, Koji Mori, Hiroshi Nakajima, Yukikatsu Terada, Matthew Holland, Michael Loewenstein, Eric Miller, Makoto Sawada, Timothy Kallman, Jelle Kaastra, Chris Done, Teruaki Enoto, Aya Bamba, Lia Corrales, Yoshihiro Ueda, Erin Kara, Irina Zhuravleva, Yutaka Fujita, Yoshitaka Arai, Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Chris Baluta, Nobutaka Bando, Ehud Behar, Thomas Bialas, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V Brown, Meng Chiao, Renata Cumbee, Cor de Vries, Jan-Willem den Herder, María Díaz Trigo, Michael DiPirro, Tadayasu Dotani, Jacobo Ebrero Carrero, Ken Ebisawa, Megan Eckart, Dominique Eckert, Satoshi Eguchi, Yuichiro Ezoe, Carlo Ferrigno, Adam Foster, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier Garcia Martinez, Nathalie Gorter, Martin Grim, Liyi Gu, Kouichi 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, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Keiichi Matsuzaki, Dan McCammon, Brian McLaughlin, Brian McNamara, Francois Mernier, Joseph 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, Anna Ogorzalek, Takashi Okajima, Atsushi Okamoto, Naomi Ota, Masanobu Ozaki, Stephane Paltani, Paul Plucinsky, F Scott Porter, Katja Pottschmidt, Jose Antonio Quero, 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, Yang Soong, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shinichiro Uno, Jacco Vink, Michael Witthoeft, Rob Wolfs, Satoshi Yamada, Shinya Yamada, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Keiichi Yanagase, Tahir Yaqoob, Susumu Yasuda, Tomokage Yoneyama, Tessei Yoshida, Miohoko Yukita
    Publications of the Astronomical Society of Japan 2025年4月11日  査読有り
    Abstract The X-Ray Imaging and Spectroscopy Mission (XRISM) is a joint mission between the Japan Aerospace Exploration Agency (JAXA) and the National Aeronautics and Space Administration (NASA) in collaboration with the European Space Agency (ESA). In addition to the three space agencies, universities and research institutes from Japan, North America, and Europe have joined to contribute to developing satellite and onboard instruments, data-processing software, and the scientific observation program. XRISM is the successor to the ASTRO-H (Hitomi) mission, which ended prematurely in 2016. Its primary science goal is to examine astrophysical problems with precise, high-resolution X-ray spectroscopy. XRISM promises to discover new horizons in X-ray astronomy. It carries a 6 × 6 pixelized X-ray microcalorimeter on the focal plane of an X-ray mirror assembly (Resolve) and a co-aligned X-ray CCD camera (Xtend) that covers the same energy band over a large field of view. XRISM utilizes the Hitomi heritage, but all designs were reviewed. The attitude and orbit control system was improved in hardware and software. The spacecraft was launched from the JAXA Tanegashima Space Center on 2023 September 6 (UTC). During the in-orbit commissioning phase, the onboard components were activated. Although the gate valve protecting the Resolve sensor with a thin beryllium X-ray entrance window was not yet opened, scientific observation started in 2024 February with the planned performance verification observation program. The nominal observation program commenced with the following guest observation program beginning in 2024 September.
  • 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 2025年4月  査読有り
    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....
  • 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.
    2025年3月  
    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....
  • 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.
    2025年3月  
    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)....
  • 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.
    2025年3月  
    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....
  • 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.
    2025年3月  
    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....
  • 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.
    2025年3月  
    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....
  • 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 2025年3月  査読有り
    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....
  • 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 2025年3月  査読有り
    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∣ &lt; 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 <inline-formula> </inline-formula> and a nonthermal pressure fraction of 2.6 ± 0.3%. The turbulent velocity is similar to what was measured in the core of the Perseus cluster by Hitomi, but here in a more massive cluster with an ICM temperature of 7 keV, the limit on the nonthermal pressure fraction is even more stringent. Our result is consistent with expectations from simulations of relaxed clusters, but it is on the low end of the predicted distribution, indicating that A2029 is an exceptionally relaxed cluster with no significant impacts from either a recent minor merger or active galactic nucleus activity....
  • 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
    2025年3月  
    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....
  • 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 2025年2月  査読有り
    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....
  • 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.
    2025年2月  
    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 &amp; sim; 40 arcsec....
  • 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 2025年2月  査読有り
    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<inline-formula><tex-math id="TM0001" notation="LaTeX">$^{*}$</tex-math></inline-formula>. The X-ray emission of the remnant is suspected to show features of overionized plasma, which would require peculiar evolutionary paths. We report on the first observation of Sagittarius A East with the X-Ray Imaging and Spectroscopy Mission (XRISM). Equipped with a combination of a high-resolution microcalorimeter spectrometer and a large field-of-view CCD imager, we for the first time resolved the Fe XXV K-shell lines into fine structure lines and measured the forbidden-to-resonance intensity ratio to be <inline-formula><tex-math id="TM0002" notation="LaTeX">$1.39 \pm 0.12$</tex-math></inline-formula>, which strongly suggests the presence of overionized plasma. We obtained a reliable constraint on the ionization temperature just before the transition into the overionization state, of <inline-formula><tex-math id="TM0003" notation="LaTeX">$\gt\! 4\:$</tex-math></inline-formula>keV. The recombination timescale was constrained to be <inline-formula><tex-math id="TM0004" notation="LaTeX">$\lt\! 8 \times 10^{11} \:$</tex-math></inline-formula>cm<inline-formula><tex-math id="TM0005" notation="LaTeX">$^{-3}\:$</tex-math></inline-formula>s. The small velocity dispersion of <inline-formula><tex-math id="TM0006" notation="LaTeX">$109 \pm 6\:$</tex-math></inline-formula>km<inline-formula><tex-math id="TM0007" notation="LaTeX">$\:$</tex-math></inline-formula>s<inline-formula><tex-math id="TM0008" notation="LaTeX">$^{-1}$</tex-math></inline-formula> indicates a low Fe ion temperature <inline-formula><tex-math id="TM0009" notation="LaTeX">$\lt\! 8\:$</tex-math></inline-formula>keV and a small expansion velocity <inline-formula><tex-math id="TM0010" notation="LaTeX">$\lt\! 200\:$</tex-math></inline-formula>km<inline-formula><tex-math id="TM0011" notation="LaTeX">$\:$</tex-math></inline-formula>s<inline-formula><tex-math id="TM0012" notation="LaTeX">$^{-1}$</tex-math></inline-formula>. The high initial ionization temperature and small recombination timescale suggest that either rapid cooling of the plasma via adiabatic expansion from dense circumstellar material or intense photoionization by Sagittarius A<inline-formula><tex-math id="TM0013" notation="LaTeX">$^{*}$</tex-math></inline-formula> in the past may have triggered the overionization....
  • 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.
    2025年1月  
    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 &amp; sim; 40 arcsec....
  • 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.
    2025年1月  
    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....
  • 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 2024年12月  査読有り
    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 <inline-formula><tex-math id="TM0001" notation="LaTeX">$\sigma _v \sim 450$</tex-math></inline-formula> km s<inline-formula><tex-math id="TM0002" notation="LaTeX">$^{-1}$</tex-math></inline-formula>. However, the Fe He<inline-formula><tex-math id="TM0003" notation="LaTeX">$\alpha$</tex-math></inline-formula> lines are substantially broadened with <inline-formula><tex-math id="TM0004" notation="LaTeX">$\sigma _v \sim 1670$</tex-math></inline-formula> km s<inline-formula><tex-math id="TM0005" notation="LaTeX">$^{-1}$</tex-math></inline-formula>. This broadening can be explained by a combination of the thermal Doppler effect due to the high ion temperature and the kinematic Doppler effect due to the SNR expansion. Assuming that the Fe He<inline-formula><tex-math id="TM0006" notation="LaTeX">$\alpha$</tex-math></inline-formula> emission originates predominantly from the supernova ejecta, we estimate the reverse shock velocity at the time when the bulk of the Fe ejecta were shock heated to be <inline-formula><tex-math id="TM0007" notation="LaTeX">$-1000 \lesssim V_{\rm rs}$</tex-math></inline-formula> (km s<inline-formula><tex-math id="TM0008" notation="LaTeX">$^{-1}$</tex-math></inline-formula>) <inline-formula><tex-math id="TM0009" notation="LaTeX">$\lesssim 3300$</tex-math></inline-formula> (in the observer frame). We also find that Fe Ly<inline-formula><tex-math id="TM0010" notation="LaTeX">$\alpha$</tex-math></inline-formula> emission is redshifted with a bulk velocity of <inline-formula><tex-math id="TM0011" notation="LaTeX">$\sim 890$</tex-math></inline-formula> km s<inline-formula><tex-math id="TM0012" notation="LaTeX">$^{-1}$</tex-math></inline-formula>, substantially larger than the radial velocity of the local interstellar medium surrounding N 132D. These results demonstrate that high-resolution X-ray spectroscopy is capable of providing constraints on the evolutionary stage, geometry, and velocity distribution of SNRs....
  • 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 2024年12月  査読有り
    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....
  • 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.
    2024年12月  
    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 &amp; #8764; 40 arcsec....
  • 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
    2024年12月  
    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....
  • 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 2024年11月  査読有り
    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....
  • 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.
    2024年11月  
    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 &amp; sim; 40 arcsec....
  • 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 2024年10月  査読有り
    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....
  • 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 2024年10月  査読有り
    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 (&gt; 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....
  • 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 2024年9月  査読有り
    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<inline-formula> </inline-formula>. Overall, the resolution and sensitivity of XRISM show that the narrow Fe K line in AGN is an effective probe of all key parts of the accretion flow, as it is currently understood. We discuss the implications of these findings for our understanding of AGN accretion, future studies with XRISM, and X-ray-based black hole mass measurements....
  • 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 227-227 2024年8月21日  
  • 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 52-52 2024年8月21日  
  • 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 236-236 2024年8月21日  
  • 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 224-224 2024年8月21日  
  • 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 235-235 2024年8月21日  
  • 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 61-61 2024年8月21日  
  • 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 60-60 2024年8月21日  
  • 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 92-92 2024年8月21日  
  • 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.
    2024年8月  
    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 &amp; ndash; 40 arcsec....
  • 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.
    2024年8月  
    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 &amp; ndash; 40 arcsec....
  • 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.
    2024年8月  
    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)....
  • 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.
    2024年8月  
    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....
  • 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.
    2024年8月  
    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 &amp; sim; 40 arcsec....
  • 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.
    2024年8月  
    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 &amp; sim; 40 arcsec....
  • Bamba, Aya, Terada, Yukikatsu, Kashiyama, Kazumi, Kisaka, Shota, Minami, Takahiro, Takahashi, Tadayuki
    Publications of the Astronomical Society of Japan 2024年8月  査読有り
    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....
  • 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.
    2024年7月  
    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)....
  • 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.
    2024年7月  
    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....
  • 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.
    2024年7月  
    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....
  • 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.
    2024年7月  
    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 &amp; sim; 40 arcsec....
  • 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.
    2024年7月  
    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....
  • 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.
    2024年6月  
    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....
  • 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 2024年6月  
    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....
  • 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.
    2024年5月  
    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 &amp; ndash; 20:41 TT, is given....
  • 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.
    2024年5月  
    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)....
  • 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.
    2024年4月  
    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....
  • 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.
    2024年3月  
    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....

MISC

 263
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    欧州第一回XRISM科学データ解析ワークショップ 開催主催
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    米国第二回XRISMコミュニティ研究会 開催主催
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