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工学教育研究部 工学科情報通信プログラム担当 |
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Disentangling multiple gas kinematic drivers in the Perseus galaxy cluster 査読あり
Bellomi E., Zhuravleva I., Heinrich A., Zhang C., ZuHone J., Vigneron B., Ueda S., Truong N., Stancil P.C., Shefler L., Migkas K., Meunier J., Hlavacek-Larrondo J., Drury I., Yukita M., Yoshida T., Yoneyama T., Yaqoob T., Yamauchi S., Yamauchi M., Yamasaki N., 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., Tümer A., Tsuru T.G., Tsunemi H., Tsujimoto M., Tsuboi Y., 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.
Nature 650 ( 8101 ) 309 - 313 2026年2月
掲載種別：研究論文（学術雑誌） 出版者・発行元：Nature
Galaxy clusters, the Universe’s largest halo structures, are filled with an X-ray-emitting gas with a temperature between 10 million and 100 million degrees. Their evolution is shaped by energetic processes such as feedback from supermassive black holes (SMBHs) and mergers with other cosmic structures<sup>1, 2–3</sup>. The imprints of these processes on gas kinematics remain largely unknown, restricting our understanding of energy conversion within clusters<sup>4</sup>. High-resolution spectral mapping with the X-Ray Imaging and Spectroscopy Mission (XRISM) observatory<sup>5</sup> offers a way forward<sup>6,7</sup>. Here we present XRISM kinematic measurements of the Perseus cluster, radially covering the extent of its cool core. We find direct evidence for at least two dominant drivers of gas motions operating on distinct physical scales: a small-scale driver in the inner approximately 60 kpc, probably associated with the SMBH feedback; and a large-scale driver in the outer core, powered by mergers. This finding suggests that, during the active phase, SMBH feedback drives gas motions, which, if fully dissipated into heat, could have a substantial role in offsetting radiative cooling losses in the Perseus core. Our study underscores the necessity of kinematic mapping observations of extended sources to robustly characterize the velocity fields and their role in the evolution of massive halos. It further offers a kinematic diagnostic for SMBH feedback models.
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Chemical composition and enrichment of the Centaurus cluster core seen by XRISM /Resolve 査読あり
Mernier F., Fukushima K., Simionescu A., Kondo M., Majumder A., Plšek T., Werner N., Fujita Y., Sato K., Matsushita K., Loewenstein M., Mushotzky R., Breuer J.P., Fujimoto R., Fukazawa Y., Hatsukade I., Nakazawa K., Urata M., Yamasaki N.
Astronomy and Astrophysics 706 2026年2月
掲載種別：研究論文（学術雑誌） 出版者・発行元：Astronomy and Astrophysics
Context. Hot, X-ray emitting atmospheres pervading galaxy clusters (and groups) are rich in metals, which have been synthesised and released by asymptotic giant branch (AGB) stars, core-collapse supernovae (SNcc), and Type Ia supernovae (SNIa) over cosmic history. This makes the intracluster medium (ICM) an ideal astrophysical system to constrain its chemical composition, and hence ultimately understand metal production and enrichment on megaparsec scales. Aims. In this work, we take advantage of the unprecedented ∼5 eV resolution offered by the Resolve instrument on board the XRISM observatory to measure the chemical composition of the core of the bright, nearby, and metal-rich Centaurus cluster with unprecedented accuracy. We use these measurements to provide constraints on the stellar populations having enriched the cluster core. Methods. Through a deep (287 ks) Resolve full-array spectral analysis of Centaurus, we derived the Fe abundance and its relative Si/Fe, S/Fe, Ar/Fe, Ca/Fe, Cr/Fe, Mn/Fe, and Ni/Fe ratios. We completed this high-resolution view with N/Fe, O/Fe, Ne/Fe, and Mg/Fe ratios obtained with XMM-Newton/RGS archival data. This abundance pattern was then fitted with various combinations of AGBs, SNcc and SNIa nucleosynthesis yields with the aim of constraining their explosion and/or progenitor models. Results. Similarly to the core of Perseus (from previous Hitomi/SXS results), we find that nine out of our 11 measured abundance ratios are formally consistent with the chemical composition of our Solar System (within uncertainties of the latter). However, the (super-solar) N/Fe and (half-solar) Mg/Fe ratios significantly differ from Perseus and/or other systems, and thus they provide tension with the picture of a fully solar composition ubiquitous to all systems. In addition, possible uncertainties in O/Fe and Ne/Fe with atomic codes highlight the need for studying more systems at high spectral resolution to assess (or rule out) the universality of the ICM composition in clusters’ cool cores. Combinations of (AGB+)SNcc+SNIa yield models can reproduce our observed X/Fe ratios in all cases. However, whether two distinct populations of SNIa are needed depends on the weight of our RGS measurements. We also briefly discuss the possibility of a multi-metallicity gas phase in this respect.
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XRISM Observations of the Prototypical Cold Front in A3667 査読あり
Omiya Y., Ichinohe Y., Nakazawa K., Awaki H., Eckert D., Fujita Y., Hatsukade I., Markevitch M., Mernier F., Mitsuishi I., Ota N., Simionescu A., Uchida Y., Ueda S., Zhuravleva I., Zuhone J.
Astrophysical Journal Letters 996 ( 1 ) 2026年1月
掲載種別：研究論文（学術雑誌） 出版者・発行元：Astrophysical Journal Letters
We present high-resolution X-ray spectroscopy of the merging galaxy cluster A3667 with XRISM/Resolve. Two observations, targeting the cluster X-ray core and the prototypical cold front, were performed with exposures of 105 and 276 ks, respectively. We find that the gas in the core is blueshifted by v<inf>z</inf> ∼ −200 km s<sup>−1</sup> relative to the brightest cluster galaxy, while the low-entropy gas inside the cold front is redshifted by v<inf>z</inf> ∼ 200 km s<sup>−1</sup>. As one moves further off-center across the front, the line-of-sight (LoS) velocity changes significantly, by Δ v z = 53 5 − 154 + 167 km s<sup>−1</sup>, back to the value similar to that in the core. There are no significant LoS velocity gradients perpendicular to the cluster symmetry axis. These features suggest that the gas forming the cold front is flowing in the plane oriented along the LoS, supporting an offset merger scenario in which the main cluster has passed in front of the subcluster and induced rotation of the core gas in the plane perpendicular to the sky. The region just inside the front exhibits the largest LoS velocity dispersion seen across two pointings, σ<inf>z</inf> ∼ 420 km s<sup>−1</sup>, which can be interpreted as a developing turbulence or a projection of the LoS velocity shear within the front. The large LoS velocity jump across the cold front, combined with the lack of Kelvin-Helmholtz instability on the surface of the front, suggests some mechanism to suppress it. For example, a magnetic field with B > 5 μG is required if the cold front is stabilized by magnetic draping.
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Chlorine and potassium enrichment in the Cassiopeia A supernova remnant 査読あり
Agarwal M., Matsunaga K., Fujimoto S.I., Zhuravleva I., Yukita M., Yoshida T., Yoneyama T., Yaqoob T., Yamauchi S., Yamauchi M., Yamasaki N., 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., 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., Ishi D., Ichinohe Y., Hornschemeier A., Hodges-Kluck E., Hell N., Hayashi T.
Nature Astronomy 10 ( 1 ) 144 - 153 2026年1月
掲載種別：研究論文（学術雑誌） 出版者・発行元：Nature Astronomy
The elements in the Universe are synthesized primarily in stars and supernovae, where nuclear fusion favours the production of even-Z elements. In contrast, odd-Z elements are less abundant and their yields are highly dependent on detailed stellar physics, making theoretical predictions of their cosmic abundance uncertain. In particular, the origin of odd-Z elements such as phosphorus (P), chlorine (Cl) and potassium (K), which are important for planet formation and life, is poorly understood. While the abundances of these elements in Milky Way stars are close to solar values, supernova explosion models systematically underestimate their production by up to an order of magnitude, indicating that key mechanisms for odd-Z nucleosynthesis are currently missing from theoretical models. Here we report the observation of P, Cl and K in the Cassiopeia A supernova remnant using high-resolution X-ray spectroscopy with X-Ray Imaging and Spectroscopy Mission data, with the detection of K at above the 6σ level being the most significant finding. Supernova explosion models of normal massive stars cannot explain the element abundance pattern, especially the high abundances of Cl and K, while models that include stellar rotation, binary interactions or shell mergers agree closely with the observations. Our observations suggest that such stellar activity plays an important role in supplying these elements to the Universe.
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XRISM/Resolve view of Abell 2319: Turbulence, sloshing, and ICM dynamics 査読あり
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., Gu L., Guainazzi M., Hagino K., Hamaguchi K., Hatsukade I., Hayashi K., Hayashi T., Hell N., Hodges-Kluck E., Hornschemeier A., Ichinohe Y., Ishi D., Ishida M., Ishikawa K., Ishisaki Y., Kaastra J., Kallman T., Kara E., Katsuda S., Kanemaru Y., Kelley R., Kilbourne C., Kitamoto S., Kobayashi S.B., Kohmura T., Kubota A., Leutenegger M., Loewenstein M., Maeda Y., Markevitch M., Matsumoto H., Matsushita K., McCammon D., McNamara B., Mernier F., Miller E., Miller J., 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., 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.
Publications of the Astronomical Society of Japan 77 ( 6 ) 1278 - 1289 2025年12月
掲載種別：研究論文（学術雑誌） 出版者・発行元：Publications of the Astronomical Society of Japan
We present results from XRISM/Resolve observations of the core of the galaxy cluster Abell 2319, focusing on its kinematic properties. The intracluster medium (ICM) exhibits temperatures of approximately 8 keV across the core, with a prominent cold front and a high-temperature region (11 keV) in the north-west. The average gas velocity in the region around the brightest cluster galaxy (BCG) covered by two Resolve pointings is consistent with that of the BCG to within 40 km s and we found modest average velocity dispersion of 230-250 km s. On the other hand, spatially resolved spectroscopy reveals interesting variations. A blueshift of up to 230 km s is observed around the east edge of the cold front, where the gas with the lowest specific entropy is found. The region further south inside the cold front shows only a small velocity difference from the BCG; however, its velocity dispersion is enhanced to 400 km s, implying the development of turbulence. These characteristics indicate that we are observing sloshing motion with some inclination angle following BCG and that gas phases with different specific entropy participate in sloshing with their own velocities, as expected from simulations. No significant evidence for a high-redshift ICM component associated with the subcluster Abell 2319B was found in the region covered by the current Resolve pointings. These results highlight the importance of sloshing and turbulence in shaping the internal structure of Abell 2319. Further deep observations are necessary to better understand the mixing and turbulent processes within the cluster.
DOI： 10.1093/pasj/psaf109
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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年3月
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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年3月
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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年8月
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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年8月
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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年6月
講演・口頭発表等 【 表示 ／ 非表示 】
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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 (5) 国際共著
野田博文、小林翔悟,森浩二、中嶋大、冨田洋、廿日出勇、他
日本物理学会 2026年春季大会 2026年3月26日
開催年月日： 2026年3月23日 - 2026年3月26日
記述言語：日本語 会議種別：口頭発表（一般）
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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(5) 国際共著
小林翔悟、森浩二、中嶋大、冨田洋、廿日出勇、他
日本天文学会2026年春季年会 2026年3月5日
開催年月日： 2026年3月4日 - 2026年3月7日
記述言語：日本語 会議種別：口頭発表（一般）
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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 (4) 国際共著
内田裕之,、鈴木寛大、米山友景、森浩二、廿日出勇、他
日本物理学会 第80回年次大会（2025年） 2025年9月18日
開催年月日： 2025年9月16日 - 2025年9月19日
記述言語：日本語 会議種別：口頭発表（一般）
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XRISM 衛星による合体銀河団 Abell 3667 におけるガスの乱流および大規模運動の探査 国際共著
大宮悠希,、一戸悠人、中澤知洋、粟木久光、廿日出勇、他
日本物理学会 第80回年次大会（2025年） 2025年9月18日
開催年月日： 2025年9月16日 - 2025年9月19日
記述言語：日本語 会議種別：口頭発表（一般）
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Ｘ線分光撮像衛星XRISM 搭載軟Ｘ線分光装置Resolve によるケプラー超新星残骸の親星調査 国際共著
金丸善朗、勝田哲、秋田桜佑、森浩二、廿日出勇、他
日本天文学会2025年秋季年会 2025年9月11日
開催年月日： 2025年9月9日 - 2025年9月11日
記述言語：日本語 会議種別：口頭発表（一般）
科研費（文科省・学振・厚労省）獲得実績 【 表示 ／ 非表示 】
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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
研究課題/領域番号：17540261 2007年04月 - 2008年03月
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
研究課題/領域番号：16540217 2006年04月 - 2007年03月
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
研究課題/領域番号：17540261 2006年04月 - 2007年03月
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
研究課題/領域番号：17540261 2005年04月 - 2006年03月
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
研究課題/領域番号：16540217 2005年04月 - 2006年03月
科学研究費補助金 基盤研究(C)