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• Gas Kinematics and Cosmic-Ray Acceleration in the Gamma-Ray SNRs W41 and G22.7–0.2 査読あり

  Murase T., Sano H., Matsubara K., Fukui Y., Nishi J., Einecke S., Filipović M.D., Kasai R., Matsusaka R., Rowell G., Sodou H., Suzuki H., Shibata Y., Tsuge K., Takaba H., Handa T.

  Astrophysical Journal   1001 ( 1 )   2026年4月

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  掲載種別：研究論文（学術雑誌）   出版者・発行元：Astrophysical Journal  

  We present a study of the interstellar medium associated with the two middle-aged supernova remnants (SNRs) W41 and G22.7–0.2, both detected in TeV gamma rays. Using high-angular-resolution ¹²CO(J = 1–0) data from the Nobeyama 45 m telescope and H i data from the Very Large Array, we investigated the spatial and kinematic properties of molecular and atomic gas that interact with the SNRs. We identified associated clouds in the velocity ranges of +50 to +80 km s⁻¹ for W41 and +76 to +110 km s⁻¹ for G22.7–0.2. Column density analysis indicates that target protons are dominated by molecular hydrogen, while atomic hydrogen contributes less than ∼10%–15% even after correction for self-absorption. The mean proton densities are ∼1.2 × 10³ cm⁻³ for W41 and ∼5.3 × 10² cm⁻³ for G22.7–0.2. From the gamma-ray luminosities, we estimate the total energy of accelerated cosmic-ray protons as W <inf>p</inf> ∼ 3 × 10⁴⁷ erg for W41 and ∼1 × 10⁴⁸ erg for G22.7–0.2, corresponding to 0.03%–0.1% of the canonical supernova explosion energy. These W <inf>p</inf> values agree with the decreasing trend in W <inf>p</inf> observed in the middle-aged SNRs within the previously reported SNR age–W <inf>p</inf> relation.

  DOI： 10.3847/1538-4357/ae3dd4

  Scopus

• A fast starburst wind consumes most of the energy from supernovae 査読あり

  Scannapieco E., Sasamata S., Kosec P., Grell G., Grayson S., Boettcher E., Ampuku K., 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., Tümer A., Tsuru T., 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.

  Nature   651 ( 8107 )   909 - 913   2026年3月

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  掲載種別：研究論文（学術雑誌）   出版者・発行元：Nature  

  Starburst galaxies often host multiphase, galaxy-scale winds thought to enrich the circumgalactic medium and limit further star formation by disrupting interstellar gas clouds^{1, 2–3}. These winds are primarily powered by supernovae^{4, 5–6}, but it remains unclear how supernova energy forms an organized flow. Here we use the Resolve spectrometer on the X-ray Imaging and Spectroscopy Mission to show that the hot (T = 2 × 10⁷ K) gas in the nucleus of the starburst galaxy M82 is moving quickly, with a line-of-sight velocity dispersion σ=595-128+464kms-1. This is consistent with a hot, nuclear wind generated by thermal pressure. We show that a free-wind model reproduces the measured temperature but underpredicts the velocity. The inferred mass and energy outflow rates from the nucleus, about 7 M<inf>⊙</inf> yr⁻¹ and 4 × 10⁴² erg s⁻¹, require that most supernova energy is thermalized. These outflow rates provide enough energy to power the ≳30 M<inf>⊙</inf> yr⁻¹ cool outflow and still transport up to 3 M<inf>⊙</inf> yr⁻¹ to the intergalactic medium, suggesting that thermal gas pressure is sufficient to power the multiphase wind without additional support from cosmic rays⁷. We also show that the nuclear gas is hotter and faster than the plasma seen on larger scales (kT=0.72-0.08+0.10keV, σ=175-73+86kms-1), suggesting a distinct origin for the latter.

  DOI： 10.1038/s41586-026-10231-1

  Scopus

• 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

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  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^{1, 2–3}. The imprints of these processes on gas kinematics remain largely unknown, restricting our understanding of energy conversion within clusters⁴. High-resolution spectral mapping with the X-Ray Imaging and Spectroscopy Mission (XRISM) observatory⁵ offers a way forward^6,7. 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.

  DOI： 10.1038/s41586-025-10017-x

  Scopus

• Spatially resolved plasma diagnostics of the supernova remnant DEM L71 using the reflection grating spectrometer 査読あり

  Amano Y., Ohshiro Y., Suzuki H., Fukushima K., Yamaguchi H.

  Publications of the Astronomical Society of Japan   78 ( 1 )   174 - 184   2026年2月

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  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 a spatially resolved high-resolution X-ray spectroscopy of the supernova remnant DEM L71 using the Reflection Grating Spectrometer (RGS) aboard XMM-Newton. Because of the large dispersion angle of the RGS, we are able to resolve individual emission lines and examine their spatial distributions within this moderately extended remnant. We derive line fluxes across different regions of DEM L71 and perform quantitative plasma diagnostics. Our analysis reveals that some regions have high forbidden-to-resonance ratios of O VII Heα lines, suggesting a non-negligible contribution from additional physical processes, such as charge exchange and/or resonance scattering. Our results demonstrate that the RGS has potential to serve as an outstanding X-ray imaging spectrometer for moderately diffuse objects.

  DOI： 10.1093/pasj/psaf131

  Scopus

• Spatially resolved plasma diagnostics of the supernova remnant DEM L71 using the reflection grating spectrometer 査読あり

  鈴木 寛大

  Publications of the Astronomical Society of Japan   78 ( 1 )   174 - 184   2026年2月

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  記述言語：英語   掲載種別：研究論文（学術雑誌）   出版者・発行元：Oxford University Press (OUP)  

  We present a spatially resolved high-resolution X-ray spectroscopy of the supernova remnant DEM L71 using the Reflection Grating Spectrometer (RGS) aboard XMM-Newton. Because of the large dispersion angle of the RGS, we are able to resolve individual emission lines and examine their spatial distributions within this moderately extended remnant. We derive line fluxes across different regions of DEM L71 and perform quantitative plasma diagnostics. Our analysis reveals that some regions have high forbidden-to-resonance ratios of O vii He
  lines, suggesting a non-negligible contribution from additional physical processes, such as charge exchange and/or resonance scattering. Our results demonstrate that the RGS has potential to serve as an outstanding X-ray imaging spectrometer for moderately diffuse objects.

  CiNii Research

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• XRISMニュース（5）： 国際相互較正 ―IACHEC年次集会2025開催記録― 査読あり

  鈴木寛大

  天文月報2025年11月号   2025年11月

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  担当区分：筆頭著者   掲載種別：記事・総説・解説・論説等（学術雑誌）  

• 30分で分かる超新星残骸のX線精密分光 招待あり 査読あり

  鈴木寛大

  天文教育   37 ( 4 )   2025年7月

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  担当区分：筆頭著者   記述言語：日本語   掲載種別：記事・総説・解説・論説等（学術雑誌）  

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• XRISM/Xtend observations of diffuse X-ray emission around microquasars

  Hiromasa Suzuki (U. Miyazaki), Naomi Tsuji (ICRR), Megumi Shidatsu (Ehime U.), Hideki Uchiyama (Shizuoka U.), Masayoshi Nobukawa (Nara U. of Edu.), Koji Mori (U. Miyazaki), Takaaki Tanaka (Konan U.), Shinya Yamada, Shogo Kobayashi (Rikkyo U.), Yoshihiro Ueda (Kyoto U.), Robert Petre (NASA/GSFC), Yusuke Sakai (Rikkyo U.), Toshihiro Takagi, Marina Yoshimoto (Ehime U.)

  日本天文学会年会 

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  開催年月日： 2026年3月

  会議種別：口頭発表（一般）  

• X線分光撮像衛星XRISM搭載軟X線撮像装置Xtendの現状(5)

  野田博文, 小林翔悟A, 森浩二B, 中嶋大C, 冨田洋D, Takashi OkajimaE, 鈴木寛大B, 米山友景D, 内田裕之G, 萩野浩一H, 信川久実子I, 田中孝明J, 村上弘志K, 信川正順L, 内山秀樹M, 松本浩典N, 小高裕和N, 鶴剛G, 林多佳由G, 山内誠B, 廿日出勇B, 幸村孝由O, 山岡和貴P, 上田周太郎V, 石田学D, 前田良知D, 田村啓輔Q, R.Boissay-MalaquinQ, 佐藤寿紀R, 金丸善朗D, 伊師大貴D, 水野恒史S, 堂谷忠靖D, 尾崎正伸T, 常深博N, 東竜一J, 朝比奈遥C, 中村彰太郎C, 亀井貴光C, 福田将大C, 善本真梨那U, 袴田知宏N, 青柳美緒N, 島耕平N, 井上峻G, 青木悠馬I, 伊藤耶馬斗I, 樋口茉由O, 伊藤世織O, 中武隼汰O, 市川雄大B, 中野瑛子B, 岳本廉央B, 松島司B, 浦瀬怜香B, 倉嶋順B, 淵琴美B, 林田清N, 他 XRISM/Xtend チーム

  日本物理学会春季大会 

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  開催年月日： 2026年3月

  会議種別：口頭発表（一般）  

• 超高層大気を観測するISS曝露部搭載X線SOI-CMOSカメラSUIMの地上試験

  武田彩希, 鈴木寛大, 黒木瑛介, 田中富貴, 髙本巴瑠乃, 有川玲華, 柴田夢叶, 森浩二, 桒野慧, 信川久実子, 松井怜生, 竹島優人, 佐藤彰太郎, 青木悠馬, 鶴剛, 内田裕之, 勝田哲, 中澤知洋, 信川正順, 幸村孝由

  日本物理学会春季大会 

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  開催年月日： 2026年3月

  会議種別：口頭発表（一般）  

• 超高層大気を観測するISS曝露部搭載X線SOI-CMOSカメラSUIMの開発状況

  鈴木寛大, 武田彩希, 黒木瑛介, 田中富貴, 髙本巴瑠乃, 有川玲華, 柴田夢叶, 森浩二, 桒野慧, 信川久実子, 松井怜生, 竹島優人, 佐藤彰太郎, 青木悠馬, 鶴剛, 内田裕之, 勝田哲, 中澤知洋, 信川正順, 幸村孝由

  日本物理学会春季大会 

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  開催年月日： 2026年3月

  会議種別：口頭発表（一般）  

• A New Era in Plasma Diagnostics of Supernova Remnants with XRISM 招待あり 国際会議

  Hiromasa Suzuki

  XRISM International Conference 2025 

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  開催年月日： 2025年10月20日 - 2025年10月24日

  会議種別：口頭発表（招待・特別）  

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• 観測装置の国際相互較正が可能にするX線精密分光時代の無衝突衝撃波の理解刷新

  研究課題/領域番号：24K17093  2024年04月 - 2027年03月

  独立行政法人日本学術振興会  科学研究費基金  若手研究

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  担当区分：研究代表者 

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• GHzサンプリングが可能にする極低ノイズX線観測による宇宙線の生成源の探索

  2025年04月 - 2026年02月

  日本科学協会  笹川科学研究助成 

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  担当区分：研究代表者