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Engineering educational research section Information and Communication Technology Program |
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HATSUKADE Isamu
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Degree 【 display / non-display 】
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Doctor of Science ( 1989.6 Osaka University )
Papers 【 display / non-display 】
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XRISM Reveals Low Nonthermal Pressure in the Core of the Hot, Relaxed Galaxy Cluster A2029 Reviewed
Audard M., Awaki H., Ballhausen R., Bamba A., Behar E., Boissay-Malaquin R., Brenneman L., Brown G.V., Corrales L., Costantini E., Cumbee R., Diaz Trigo M., Done C., Dotani T., Ebisawa K., Eckart M.E., Eckert D., Eguchi S., Enoto T., Ezoe Y., Foster A., Fujimoto R., Fujita Y., Fukazawa Y., Fukushima K., Furuzawa A., Gallo L., García J.A., Gu L., Guainazzi M., Hagino K., Hamaguchi K., Hatsukade I., Hayashi K., Hayashi T., Hell N., Hodges-Kluck E., Hornschemeier A., Ichinohe Y., Ishida M., Ishikawa K., Ishisaki Y., Kaastra J., Kallman T., Kara E., Katsuda S., Kanemaru Y., Kelley R., Kilbourne C., Kitamoto S., Kobayashi S., Kohmura T., Kubota A., Leutenegger M., Loewenstein M., Maeda Y., Markevitch M., Matsumoto H., Matsushita K., McCammon D., McNamara B., Mernier F., Miller E.D., Miller J.M., Mitsuishi I., Mizumoto M., Mizuno T., Mori K., Mukai K., Murakami H., Mushotzky R., Nakajima H., Nakazawa K., Ness J.U., Nobukawa K., Nobukawa M., Noda H., Odaka H., Ogawa S., Ogorzalek A., Okajima T., Ota N., Paltani S., Petre R., Plucinsky P., Porter F.S., Pottschmidt K., Sato T., Sawada M., Seta H., Shidatsu M., Simionescu A., Smith R., Sato K., Suzuki H., Szymkowiak A., Takahashi H., Takeo M., Tamagawa T., Tamura K.
Astrophysical Journal Letters 982 ( 1 ) 2025.3
Publishing type：Research paper (scientific journal) Publisher：Astrophysical Journal Letters
We present XRISM Resolve observations of the core of the hot, relaxed galaxy cluster Abell 2029 (A2029). We find that the line-of-sight bulk velocity of the intracluster medium (ICM) within the central 180 kpc is at rest with respect to the brightest cluster galaxy, with a 3σ upper limit of |vbulk| < 100 km s−1. We robustly measure the field-integrated ICM velocity dispersion to be σv = 169 ± 10 km s−1, obtaining similar results for both single-temperature and two-temperature plasma models to account for the cluster cool core. This result, if ascribed to isotropic turbulence, implies a subsonic ICM with Mach number M3D ≈ 0.22 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.
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Initial operations of the Soft X-ray Imager onboard XRISM Reviewed International coauthorship
Suzuki H., Yoneyama T., Kobayashi S.B., Noda H., Uchida H., Nobukawa K.K., Hagino K., Mori K., Tomida H., Nakajima H., Tanaka T., Murakami H., Uchiyama H., Nobukawa M., Kanemaru Y., Otsuka Y., Yokosu H., Yonemaru W., Nakano H., Ichikawa K., Takemoto R., Matsushima T., Yoshimoto M., Aoyagi M., Shima K., Aoki Y., Ito Y., Fukuda K., Kiyama H., Aoki D., Fujisawa K., Shimizu Y., Higuchi M., Fukuda M., Sakamoto N., Azuma R., Inoue S., Kohmura T., Yamauchi M., Hatsukade I., Matsumoto H., Odaka H., Mizuno T., Yoshida T., Maeda Y., Ishida M., Tsuru T.G., Yamaoka K., Okajima T., Hayashi T., Hiraga J.S., Ozaki M., Dotani T., Tsunemi H., Hayashida K.
Journal of Astronomical Telescopes, Instruments, and Systems 11 ( 4 ) 2025.3
Publishing type：Research paper (scientific journal) Publisher：Proceedings of SPIE - The International Society for Optical Engineering
XRISM (X-Ray Imaging and Spectroscopy Mission) is an astronomical satellite with the capability of high-resolution spectroscopy with the X-ray microcalorimeter, Resolve, and wide field-of-view imaging with the CCD camera, Xtend. The Xtend consists of the mirror assembly (XMA: X-ray Mirror Assembly) and detector (SXI: Soft X-ray Imager). The components of SXI include CCDs, analog and digital electronics, and a mechanical cooler. After the successful launch on September 6th, 2023 (UT) and subsequent critical operations, the mission instruments were turned on and set up. The CCDs have been kept at the designed operating temperature of −110◦C after the electronics and cooling system were successfully set up. During the initial operation phase, which continued for more than a month after the critical operations, we verified the observation procedure, stability of the cooling system, all the observation options with different imaging areas and/or timing resolutions, and operations for protection against South Atlantic Anomaly. We optimized the operation procedure and observation parameters including the cooler settings, imaging areas for the specific modes with higher timing resolutions, and event selection algorithm. We summarize our policy and procedure of the initial operations for SXI. We also report on a couple of issues we faced during the initial operations and lessons learned from them.
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The bulk motion of gas in the core of the Centaurus galaxy cluster Reviewed
Majumder A., Hosogi K., Sun M., Plšek T., Werner N., Kondo M., Zhuravleva I., Yukita M., Yoshida T., Yoneyama T., Yaqoob T., Yamauchi S., Yamauchi M., Yamasaki N.Y., Yamaoka K., Yamaguchi H., Yamada S., Yamada S., Williams B.J., Watanabe S., Vink J., Uno S., Ueda Y., Uchiyama H., Uchida Y., Uchida N., Uchida H., Tsuru T.G., Tsunemi H., Tsujimoto M., Tsuboi Y., Trigo M.D., Terashima Y., Terada Y., Tashiro M., Tanimoto A., Tanaka T., Tamura K., Tamagawa T., Takeo M., Takahashi H., Szymkowiak A., Suzuki H., Smith R., Simionescu A., Shidatsu M., Seta H., Sawada M., Sato T., Sato K., Pottschmidt K., Porter F.S., Plucinsky P., Petre R., Paltani S., Ota N., Okajima T., Ogorzalek A., Ogawa S., Odaka H., Noda H., Nobukawa M., Nobukawa K., Ness J.U., Nakazawa K., Nakajima H., Mushotzky R., Murakami H., Mukai K., Mori K., Mizuno T., Mizumoto M., Mitsuishi I., Miller J.M., Miller E.D., Mernier F., McNamara B., McCammon D., Matsushita K., Matsumoto H., Markevitch M., Maeda Y., Loewenstein M., Leutenegger M., Kubota A., Kohmura T., Kobayashi S., Kitamoto S., Kilbourne C., Kelley R., Kanemaru Y., Katsuda S., Kara E., Kallman T., Kaastra J., Ishisaki Y., Ishikawa K., Ishida M., Ichinohe Y., Hornschemeier A.
Nature 638 ( 8050 ) 365 - 369 2025.2
Publishing type：Research paper (scientific journal) Publisher：Nature
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.
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Overionized plasma in the supernova remnant Sagittarius A East anchored by XRISM observations Reviewed
Audard M., Awaki H., Ballhausen R., Bamba A., Behar E., Boissay-Malaquin R., Brenneman L., Brown G.V., Corrales L., Costantini E., Cumbee R., Diaz-Trigo M., Done C., Dotani T., Ebisawa K., Eckart M., Eckert D., Enoto T., Eguchi S., Ezoe Y., Foster A., Fujimoto R., Fujita Y., Fukazawa Y., Fukushima K., Furuzawa A., Gallo L., García J.A., Gu L., Guainazzi M., Hagino K., Hamaguchi K., Hatsukade I., Hayashi K., Hayashi T., Hell N., Hodges-Kluck E., Hornschemeier A., Ichinohe Y., Ishida M., Ishikawa K., Ishisaki Y., Kaastra J., Kallman T., Kara E., Katsuda S., Kanemaru Y., Kelley R., Kilbourne C., Kitamoto S., Kobayashi S., Kohmura T., Kubota A., Leutenegger M., Loewenstein M., Maeda Y., Markevitch M., Matsumoto H., Matsushita K., McCammon D., McNamara B., Mernier F., Miller E.D., Miller J.M., Mitsuishi I., Mizumoto M., Mizuno T., Mori K., Mukai K., Murakami H., Mushotzky R., Nakajima H., Nakazawa K., Ness J.U., Nobukawa K., Nobukawa M., Noda H., Odaka H., Ogawa S., Ogorzalek A., Okajima T., Ota N., Paltani S., Petre R., Plucinsky P., Scott Porter F., Pottschmidt K., Sato K., Sato T., Sawada M., Seta H., Shidatsu M., Simionescu A., Smith R., Suzuki H., Szymkowiak A., Takahashi H., Takeo M., Tamagawa T., Tamura K.
Publications of the Astronomical Society of Japan 77 ( 1 ) L1 - L8 2025.2
Publishing type：Research paper (scientific journal) Publisher：Publications of the Astronomical Society of Japan
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∗. 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 1.39 ± 0.12, 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 >4 keV. The recombination timescale was constrained to be <8 × 1011 cm−3 s. The small velocity dispersion of 109 ± 6 km s−1 indicates a low Fe ion temperature <8 keV and a small expansion velocity <200 km s−1. 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∗ in the past may have triggered the overionization.
DOI： 10.1093/pasj/psae111
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The XRISM/Resolve View of the Fe K Region of Cyg X-3 Reviewed
Audard M., Awaki H., Ballhausen R., Bamba A., Behar E., Boissay-Malaquin R., Brenneman L., Brown G.V., Corrales L., Costantini E., Cumbee R., Trigo M.D., Done C., Dotani T., Ebisawa K., Eckart M.E., Eckert D., Eguchi S., Enoto T., Ezoe Y., Foster A., Fujimoto R., Fujita Y., Fukazawa Y., Fukushima K., Furuzawa A., Gallo L., García J.A., Gu L., Guainazzi M., Hagino K., Hamaguchi K., Hatsukade I., Hayashi K., Hayashi T., Hell N., Hodges-Kluck E., Hornschemeier A., Ichinohe Y., Ishida M., Ishikawa K., Ishisaki Y., Kaastra J., Kallman T., Kara E., Katsuda S., Kanemaru Y., Kelley R., Kilbourne C., Kitamoto S., Kobayashi S., Kohmura T., Kubota A., Leutenegger M., Loewenstein M., Maeda Y., Markevitch M., Matsumoto H., Matsushita K., McCammon D., McNamara B., Mernier F., Miller E.D., Miller J.M., Mitsuishi I., Mizumoto M., Mizuno T., Mori K., Mukai K., Murakami H., Mushotzky R., Nakajima H., Nakazawa K., Ness J.U., Nobukawa K., Nobukawa M., Noda H., Odaka H., Ogawa S., Ogorzalek A., Okajima T., Ota N., Paltani S., Petre R., Plucinsky P., Porter F.S., Pottschmidt K., Sato K., Sato T., Sawada M., Seta H., Shidatsu M., Simionescu A., Smith R., Suzuki H., Szymkowiak A., Takahashi H., Takeo M., Tamagawa T., Tamura K.
Astrophysical Journal Letters 977 ( 2 ) 2024.12
Publishing type：Research paper (scientific journal) Publisher：Astrophysical Journal Letters
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 Hea and Fe XXVI Lya 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.
MISC 【 display / non-display 】
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ビデオ流星観測システムの開発と流星の自動検出
稲田憲哉、船倉さやか、松本陽子、廿日出勇
情報処理学会九州支部「火の国シンポジウム2003」A-1-4 2003.3
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H_{0} Determination Using X-ray Cluster of Galaxies A773
共著者：M.Matsuura, S.Miyoshi, K.Yamashita, Y.Tawara, A.Furuzawa, A.N.Lasenby, R.Saunders, M.Jones, I.Hatsukade
京都産業大学論集 28巻59-71頁 1997.3
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SS433の時間変動の研究
共著者：松岡宏志、高岸邦夫、廿日出勇
宮崎大学工学部研究報告40号65-69頁 1994.8
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天体観測用CCDカメラ制御、データ処理システム
共著者：高岸邦夫、廿日出勇、黒木隆
宮崎大学工学部研究報告39号39-45頁 1993.8
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Near-nucleus imaging observations of comet Austin
共著者：J.Watanabe, S.Ichikawa, K.Takagishi, I.Hatsukade, M.Sakai, 他5名
Publications of National AstronomicalObservatory of Japan, Vol.2, 267-292 1991.6
Presentations 【 display / non-display 】
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X線分光撮像衛星XRISM搭載軟X線撮像装置Xtendの現状 (3)
鈴木寛大, 米山友景, 森浩二, 中嶋大, 他
日本物理学会2025年春季大会 2025.3.21
Event date： 2025.3.18 - 2025.3.21
Presentation type：Oral presentation (general)
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X線分光撮像衛星(XRISM) 搭載軟X線撮像装置(Xtend) の軌道上運用 (3) International coauthorship
米山友景, 鈴木寛大, 森浩二, 中嶋大 他
日本天文学会2025年春季年会 2025.3.18
Event date： 2025.3.17 - 2025.3.20
Language：Japanese Presentation type：Oral presentation (general)
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XRISM衛星によるAbell 3667銀河団の観測成果 International coauthorship
大宮 悠希, 一戸 悠人, 中澤 知洋, 粟木 久光 他
日本天文学会2025年春季年会 2025.3.17
Event date： 2025.3.17 - 2025.3.20
Language：Japanese Presentation type：Oral presentation (general)
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XRISM/Resolveを用いたケンタウルス座銀河団中心部のガスの温度、速度構造の精密分光観測 International coauthorship
近藤麻里恵, 佐藤浩介, 松下恭子 藤田裕 他
日本天文学会2025年春季年会 2025.3.17
Event date： 2025.3.17 - 2025.3.20
Language：Japanese Presentation type：Oral presentation (general)
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Ｘ線分光撮像衛星 XRISM 搭載軟Ｘ線撮像装置 Xtend の現状 (2)
村上弘志, 小林翔悟, 森浩二, 中嶋大 他
日本物理学会第７９回年次大会（2024年） 2024.9.16
Event date： 2024.9.16 - 2024.9.19
Presentation type：Oral presentation (general)
Grant-in-Aid for Scientific Research 【 display / non-display 】
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人工衛星および地上観測によるガンマ線バースト・X線フラッシュの研究
Grant number：17540261 2007.04 - 2008.03
科学研究費補助金 基盤研究(C)
宮崎大学に設置されたHETE-2に連動する自動制御望遠鏡（RIMOTS）を運用し、γ線バーストの残光観測を行っている。
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広視野・高時間分解能観測システムを用いたγ線バースト閃光の研究
Grant number：16540217 2006.04 - 2007.03
科学研究費補助金 基盤研究(C)
これまで観測が行われていないGRB発生前後の残光観測を行うために、広視野を高時間分解能で常時観測する観測システム、Miyazaki Wide-field Monitor（MWM）を開発した。
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人工衛星および地上観測によるガンマ線バースト・X線フラッシュの研究
Grant number：17540261 2006.04 - 2007.03
科学研究費補助金 基盤研究(C)
宮崎大学に設置されたHETE-2に連動する自動制御望遠鏡（RIMOTS）を運用し、γ線バーストの残光観測を行っている。
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人工衛星および地上観測によるガンマ線バースト・X線フラッシュの研究
Grant number：17540261 2005.04 - 2006.03
科学研究費補助金 基盤研究(C)
宮崎大学に設置されたHETE-2に連動する自動制御望遠鏡（RIMOTS）を運用し、γ線バーストの残光観測を行っている。
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広視野・高時間分解能観測システムを用いたγ線バースト閃光の研究
Grant number：16540217 2005.04 - 2006.03
科学研究費補助金 基盤研究(C)