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Affiliation |
Engineering educational research section Semiconductor Science and Applied Physics Program |
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Title |
Assistant Professor |
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Related SDGs |
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SUZUKI Hiromasa
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Papers 【 display / non-display 】
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Gas Kinematics and Cosmic-Ray Acceleration in the Gamma-Ray SNRs W41 and G22.7–0.2 Reviewed
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 ) 2026.4
Publishing type：Research paper (scientific journal) Publisher：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 <sup>12</sup>CO(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<sup>−1</sup> for W41 and +76 to +110 km s<sup>−1</sup> 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 × 10<sup>3</sup> cm<sup>−3</sup> for W41 and ∼5.3 × 10<sup>2</sup> cm<sup>−3</sup> 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 × 10<sup>47</sup> erg for W41 and ∼1 × 10<sup>48</sup> 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.
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A fast starburst wind consumes most of the energy from supernovae Reviewed
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 2026.3
Publishing type：Research paper (scientific journal) Publisher：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<sup>1, 2–3</sup>. These winds are primarily powered by supernovae<sup>4, 5–6</sup>, 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 × 10<sup>7</sup> 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<sup>−1</sup> and 4 × 10<sup>42</sup> erg s<sup>−1</sup>, require that most supernova energy is thermalized. These outflow rates provide enough energy to power the ≳30 M<inf>⊙</inf> yr<sup>−1</sup> cool outflow and still transport up to 3 M<inf>⊙</inf> yr<sup>−1</sup> to the intergalactic medium, suggesting that thermal gas pressure is sufficient to power the multiphase wind without additional support from cosmic rays<sup>7</sup>. 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.
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Disentangling multiple gas kinematic drivers in the Perseus galaxy cluster Reviewed
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 2026.2
Publishing type：Research paper (scientific journal) Publisher：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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Amano Y., Ohshiro Y., Suzuki H., Fukushima K., Yamaguchi H.
Publications of the Astronomical Society of Japan 78 ( 1 ) 174 - 184 2026.2
Publishing type：Research paper (scientific journal) Publisher：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
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鈴木 寛大
Publications of the Astronomical Society of Japan 78 ( 1 ) 174 - 184 2026.2
Language：English Publishing type：Research paper (scientific journal) Publisher：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.
MISC 【 display / non-display 】
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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― Reviewed
鈴木寛大
天文月報2025年11月号 2025.11
Authorship：Lead author Publishing type：Article, review, commentary, editorial, etc. (scientific journal)
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30分で分かる超新星残骸のX線精密分光 Invited Reviewed
鈴木寛大
天文教育 37 ( 4 ) 2025.7
Authorship：Lead author Language：Japanese Publishing type：Article, review, commentary, editorial, etc. (scientific journal)
Presentations 【 display / non-display 】
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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
Event date： 2026.3
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(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
Event date： 2026.3
Presentation type：Oral presentation (general)
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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
Event date： 2026.3
Presentation type：Oral presentation (general)
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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
Event date： 2026.3
Presentation type：Oral presentation (general)
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A New Era in Plasma Diagnostics of Supernova Remnants with XRISM Invited International conference
Hiromasa Suzuki
XRISM International Conference 2025
Event date： 2025.10.20 - 2025.10.24
Presentation type：Oral presentation (invited, special)
Grant-in-Aid for Scientific Research 【 display / non-display 】
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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
Grant number：24K17093 2024.04 - 2027.03
独立行政法人日本学術振興会 科学研究費基金 若手研究
Authorship：Principal investigator