東北大学研究者紹介

研究者詳細

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ヤマダ　サトシ

山田　智史

Satoshi Yamada

所属

高等研究機構学際科学フロンティア研究所　新領域創成研究部学際基盤研究分野　先端基礎科学研究領域

職名

助教

学位

博士(理学) （京都大学）

researchmap

https://researchmap.jp/styamada

J-GLOBAL ID

202401005419318857

e-Rad 研究者番号

90963520

ORCID

https://orcid.org/0000-0002-9754-3081

経歴 4

2025年12月～継続中

ジュネーヴ大学/スイス: University of Geneva (Switzerland)　JSPS　Overseas Research Fellowships
2025年4月～継続中

東北大学　学際科学フロンティア研究所新領域創成研究部
2022年4月～ 2025年3月

理化学研究所　開拓研究本部　基礎科学特別研究員 (SPDR)
2019年4月～ 2022年3月

日本学術振興会, 特別研究員 (DC1)

学歴 3

京都大学大学院　理学研究科　物理学・宇宙物理学専攻 (博士課程)

2019年4月～ 2022年3月
京都大学大学院　理学研究科　物理学・宇宙物理学専攻 (修士課程)

2017年4月～ 2019年3月
京都大学　理学部　理学科

2013年4月～ 2017年3月

所属学協会 2

高エネルギー宇宙物理連絡会
日本天文学会

研究キーワード 7

衛星開発
X線マイクロカロリメータ
多波長天文学
赤外線天文学
X線天文学
活動銀河核
ブラックホール

研究分野 1

自然科学一般 / 天文学 /

受賞 7

理事長感謝状

2024年2月　理化学研究所 (衛星開発の活躍に対する贈呈)
JAXA 感謝状

2024年2月　宇宙科学研究所
井上研究奨励賞

2024年2月　井上科学振興財団
OUTSTANDING CONTRIBUTION AWARD for young researchers (2度目)

2024年9月　JAXA 宇宙科学研究所
理事長感謝状

2024年2月　理化学研究所 (観測研究の活躍に対する贈呈)
OUTSTANDING CONTRIBUTION AWARD for young researchers

2023年6月　JAXA 宇宙科学研究所
オーラルアワード受賞

2019年8月　天文・天体物理若手の会

︎全件表示 ︎最初の5件までを表示

論文 90

Vigorous turbulence driven by quasar-mode feedback in a cluster core 国際共著査読有り

Satoshi Yamada, Shutaro Ueda, Hirofumi Noda, Yutaka Fujita, Misaki Mizumoto, Kentaro Nagamine, Claudio Ricci, Shoji Ogawa, Taiki Kawamuro, Shinya Yamada, Yuichi Terashima, Yoshihiro Ueda

Nature Astronomy　2026年7月28日
出版者・発行元： Springer Science and Business Media LLC
DOI： 10.1038/s41550-026-02939-x 　

eISSN：2397-3366

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Abstract Quasars are among the most luminous objects. They are powered by accretion onto supermassive black holes. They are thought to impact cosmological evolution primarily through energetic winds, known as quasar-mode feedback, yet the efficiency and spatial extent of this process remain poorly constrained. Here we present X-Ray Imaging and Spectroscopy Mission (XRISM) observations of H1821+643—the nearest galaxy cluster with a central quasar (redshift z = 0.297)—which was a rare opportunity to directly probe quasar-mode feedback in the intracluster medium. High-resolution spectroscopy reveals exceptionally broadened Fe XXV emission lines from the intracluster medium, with a velocity dispersion of approximately 300 km s ⁻¹ , far exceeding values observed in nearby cluster cores. These lines originate predominantly at radii of 20–100 kpc from the centre. Assuming that turbulence from a quasar-driven shock led to the broadening of the lines, the energy injected by the quasar beyond galactic scales (≳20 kpc) is estimated to be ≳1–10% of its radiative energy. Notably, this feedback efficiency exceeds previous multiwavelength estimates by orders of magnitude (≲0.01%) and reaches the levels required by the latest cosmological hydrodynamical simulations. This finding of vigorous turbulence indicates that quasar-mode feedback plays a central role in regulating galaxy and cluster evolution at high redshift.
XRISM Time-resolved Fe Kα Spectroscopy of NGC 4395: Time-variable Inner-disk Emission 査読有り

Taiki Kawamuro, Satoshi Yamada, Hirofumi Noda, Yoshiyuki Inoue, Shoji Ogawa, Misaki Mizumoto

The Astrophysical Journal Letters　1005　(2)　L62-L62　2026年7月8日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ae796e 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract We report the first XRISM observation of the low-mass AGN in the nearby dwarf galaxy NGC 4395 ( M _BH ∼ 10 ⁴⁻⁵ M _⊙ ), complemented by a simultaneous NuSTAR observation. We constrained the continuum by jointly fitting the XRISM/Resolve (2–12 keV) and NuSTAR (3–30 keV) spectra while excluding the Fe K band (5.5–7.5 keV). Relative to this baseline continuum, the time-averaged Resolve spectrum revealed an unresolved neutral Fe K α core with a velocity width of ≲110 km s ⁻¹ and an adjacent redward wing. The red wing was well reproduced by an additional relativistically broadened Fe K component. Furthermore, time-resolved spectroscopy with ≈87 ks bins showed that the diskline profile varied significantly over the ∼400 ks observation. This evolution can be interpreted in terms of changes in the inner radius of the line-emitting region, together with a possible inclination modulation with a period of ≈210 ks. If interpreted as Lense–Thirring precession of a tilted inner flow, the observed period would favor the low end of the black hole mass estimates ( M _BH ≈ 9 × 10 ³ M _⊙ ) and imply a moderate spin ( a ≳ 0.6). These results highlight the capability of XRISM to track relativistic disk dynamics in AGNs.
Discovery of Powerful Multivelocity Ultrafast Outflows in the Starburst Merger Galaxy IRAS 05189–2524 with XRISM 査読有り

Hirofumi Noda, Satoshi Yamada, Shoji Ogawa, Kouichi Hagino, Ehud Behar, Omer Reich, Anna Ogorzalek, Laura Brenneman, Yuichi Terashima, Misaki Mizumoto, Francesco Tombesi, Pierpaolo Condò, Alfredo Luminari, Atsushi Tanimoto, Megan E. Eckart, Erin Kara, Takashi Okajima, Yoshihiro Ueda, Yuki Aiso, Makoto Tashiro

The Astrophysical Journal Letters　993　(2)　L53-L53　2025年11月6日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ae14e8 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract We observed the X-ray-bright ultraluminous infrared galaxy IRAS 05189−2524 with XRISM during its performance verification phase. The unprecedented energy resolution of the onboard X-ray microcalorimeter revealed complex spectral features at ∼7–9 keV, which can be interpreted as blueshifted Fe XXV / XXVI absorption lines with various velocity dispersions, originating from ultrafast outflow (UFO) components with multiple bulk velocities of ∼0.076 c , ∼0.101 c , and ∼0.143 c . In addition, a broad Fe–K emission line was detected around ∼7 keV, forming a P Cygni profile together with the absorption lines. The onboard X-ray CCD camera revealed a 0.4–12 keV broadband spectrum characterized by a neutrally absorbed power-law continuum with a photon index of ∼2.3 and intrinsic flare-like variability on timescales of ∼10 ks, both of which are likely associated with near-Eddington accretion. We also found potential variability of the UFO parameters on a timescale of ∼140 ks. Using these properties, we propose new constraints on the outflow structure and suggest the presence of multiple outflowing regions on scales of about tens to 100 Schwarzschild radii, located within roughly 2000 Schwarzschild radii. Since both the estimated momentum and energy outflow rates of the UFOs exceed those of galactic molecular outflows, our results indicate that powerful, multivelocity UFOs are already well developed during a short-lived evolutionary phase following a major galaxy merger, characterized by intense starburst activity and likely preceding the quasar phase. This system is expected to evolve into a quasar, sustaining strong UFO activity and suppressing star formation in the host galaxy.
X-Ray Winds in Nearby-to-distant Galaxies (X-WING). I. Legacy Surveys of Galaxies with Ultrafast Outflows and Warm Absorbers in z ∼ 0–4 査読有り

Satoshi Yamada, Taiki Kawamuro, Misaki Mizumoto, Claudio Ricci, Shoji Ogawa, Hirofumi Noda, Yoshihiro Ueda, Teruaki Enoto, Mitsuru Kokubo, Takeo Minezaki, Hiroaki Sameshima, Takashi Horiuchi, Shoichiro Mizukoshi

The Astrophysical Journal Supplement Series　274　(1)　8-8　2024年8月22日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4365/ad5961 　

ISSN：0067-0049

eISSN：1538-4365

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Abstract As an inaugural investigation under the X-ray Winds In Nearby-to-distant Galaxies (X-WING) program, we assembled a data set comprising 132 active galactic nuclei (AGNs) spanning redshifts z ∼ 0–4 characterized by blueshifted absorption lines indicative of X-ray winds. Through an exhaustive review of previous research, we compiled the outflow parameters for 583 X-ray winds, encompassing key attributes such as outflow velocities (V _out), ionization parameters (ξ), and hydrogen column densities. By leveraging the parameters V _out and ξ, we systematically categorized the winds into three distinct groups: ultrafast outflows (UFOs), low-ionization parameter (low-IP) UFOs, and warm absorbers (WAs). Strikingly, a discernible absence of linear correlations in the outflow parameters, coupled with distributions approaching instrumental detection limits, was observed. Another notable finding was the identification of a velocity gap around V _out ∼ 10,000 km s⁻¹. This gap was particularly evident in the winds detected via absorption lines within the ≲2 keV band, indicating disparate origins for low-IP UFOs and WAs. In cases involving Fe xxv/Fe xxvi lines, where the gap might be attributed to potential confusion between emission/absorption lines and the Fe K-edge, the possibility of UFOs and galactic-scale WAs being disconnected is considered. An examination of the outflow and dust sublimation radii revealed a distinction: UFOs appear to consist of dust-free material, whereas WAs likely comprise dusty gas. From 2024, the X-Ray Imaging and Spectroscopy Mission is poised to alleviate observational biases, providing insights into the authenticity of the identified gap, a pivotal question in comprehending AGN feedback from UFOs.
[O iv]- and [Ne v]-weak Active Galactic Nuclei Hidden by Compton-thick Material in Late Mergers 査読有り

Satoshi Yamada, Yoshihiro Ueda, Taiki Kawamuro, Claudio Ricci, Yoshiki Toba, Masatoshi Imanishi, Takamitsu Miyaji, Atsushi Tanimoto, Kohei Ichikawa, Martín Herrera-Endoqui, Shoji Ogawa, Ryosuke Uematsu, Keiichi Wada

The Astrophysical Journal　2024年4月1日

DOI： 10.3847/1538-4357/ad2936 　
Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in the GOALS Sample with a Self-consistent AGN Model including a Polar-dust Component 査読有り

Satoshi Yamada, Yoshihiro Ueda, Martín Herrera-Endoqui, Yoshiki Toba, Takamitsu Miyaji, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Masatoshi Imanishi, Claudio Ricci

The Astrophysical Journal Supplement Series　2023年4月1日

DOI： 10.3847/1538-4365/acb349 　
Comprehensive Broadband X-Ray and Multiwavelength Study of Active Galactic Nuclei in 57 Local Luminous and Ultraluminous Infrared Galaxies Observed with NuSTAR and/or Swift/BAT 査読有り

Satoshi Yamada, Yoshihiro Ueda, Atsushi Tanimoto, Masatoshi Imanishi, Yoshiki Toba, Claudio Ricci, George C. Privon

The Astrophysical Journal Supplement Series　2021年12月1日

DOI： 10.3847/1538-4365/ac17f5 　
Nature of Compton-thick Active Galactic Nuclei in “Nonmerging” Luminous Infrared Galaxies UGC 2608 and NGC 5135 Revealed with Broadband X-Ray Spectroscopy 査読有り

Satoshi Yamada, Yoshihiro Ueda, Atsushi Tanimoto, Saeko Oda, Masatoshi Imanishi, Yoshiki Toba, Claudio Ricci

The Astrophysical Journal　2020年7月1日

DOI： 10.3847/1538-4357/ab94b1 　
Luminosity Ratio between [O iv] 25.89 μm Line and Nuclear Continuum 12 μm as a Diagnostic for “Buried” AGNs 査読有り

Satoshi Yamada, Yoshihiro Ueda, Atsushi Tanimoto, Taiki Kawamuro, Masatoshi Imanishi, Yoshiki Toba

The Astrophysical Journal　876　(2)　96-96　2019年5月8日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ab14f0 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract We propose new diagnostics that utilize the [O iv] 25.89 μm and nuclear (subarcsecond scale) 12 μm luminosity ratios for identifying whether an active galactic nucleus (AGN) is deeply “buried” in their surrounding materials. Utilizing a sample of 16 absorbed AGNs at redshifts lower than 0.03 in the Swift/BAT catalog observed with Suzaku, we find that AGNs with small scattering fractions (<0.5%) tend to show weaker [O iv]-to-12 μm luminosity ratios than the average of Seyfert 2 galaxies. This suggests that this ratio is a good indicator for identifying buried AGNs. Then, we apply this criterion to 23 local luminous and ultraluminous infrared galaxies (U/LIRGs) in various merger stages hosting AGNs. We find that AGNs in most mid- to late-stage mergers are buried, while those in earlier-stage ones (including nonmerger) are not. This result suggests that the fraction of buried AGNs in U/LIRGs increases as the galaxy–galaxy interaction becomes more significant.
Broadband X-Ray Spectral Analysis of the Double-nucleus Luminous Infrared Galaxy Mrk 463 査読有り

Satoshi Yamada, Yoshihiro Ueda, Saeko Oda, Atsushi Tanimoto, Masatoshi Imanishi, Yuichi Terashima, Claudio Ricci

The Astrophysical Journal　858　(2)　106-106　2018年5月10日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/aabacb 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract We present a broadband (0.4–70 keV) X-ray spectral analysis of the luminous infrared galaxy (LIRG) system Mrk 463 observed with Nuclear Spectroscopic Telescope Array (NuSTAR), Chandra, and XMM-Newton, which contains double active galactic nuclei (AGNs; Mrk 463E and Mrk 463W) with a separation of ∼3.8 kpc. Detecting their transmitted hard X-ray >10 keV continua with NuSTAR, we confirm that Mrk 463E and Mrk 463W have AGNs with intrinsic luminosities of (1.6–2.2) × 10⁴³ and (0.5–0.6) × 10⁴³ erg s⁻¹ (2–10 keV) obscured by hydrogen column densities of 8 × 10²³ and 3 × 10²³ cm⁻², respectively. Both nuclei show strong reflection components from cold matter. The luminosity ratio between X-ray (2–10 keV) and [O iv] 25.89 μm of Mrk 463E is ∼5 times smaller than those of normal Seyfert galaxies, suggesting that the intrinsic SED is X-ray weak relative to the UV luminosity. In fact, the bolometric AGN luminosity of Mrk 463E estimated from L′-band (3.8 μm), [O iv] 25.89 μm, and [Ne v] 14.32 μm lines indicate a large bolometric-to-X-ray luminosity ratio, κ_{2–10 keV} ≈ 110–410, and a high Eddington ratio, λ_Edd ∼ 0.4–0.8. We suggest that the merger triggered a rapid growth of the black hole in Mrk 463E, which is not yet deeply “buried” by circumnuclear dust. By contrast, the L′-band luminosity of Mrk 463W is unusually small relative to the X-ray luminosity, suggesting that the Eddington ratio is low (<10⁻³) and it might be still in an early phase of merger-driven AGN activity.
Kinetic structure of the intracluster medium across nearby clusters observed with XRISM 国際共著査読有り

Naomi Ota, Erwin T. Lau, Satoshi Yamada, Yuki Omiya, and Hiroya Yamaguchi

PASJ Letter (accepted)　2026年8月
The Geometry of Ultra-Fast Outflows Probed by Soft X-ray Variability in PDS 456 国際共著査読有り

Sato et a

PASJ (accepted)　2026年8月
Decoupled Kinematics and Excitation in the Compton-thick AGN NGC 6552: Spatially Resolved KOOLS-IFU Observations 国際共著査読有り

Kyuseok Oh, Yoshihiro Ueda, Kanta Fujiwara, Keisuke Isogai, Satoshi Yamada, Keito Shimoda, Yoshiki Toba, Kazuya Matsubayashi, Shoji Ogawa, Yuya Nakatani

The Astrophysical Journal　1005　(2)　185-185　2026年7月6日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae7c66 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract Hard-X-ray-selected Compton-thick active galactic nuclei (AGNs) provide a relatively obscuration-resistant census of accretion, but optical line diagnostics can be strongly shaped by extinction and geometry. Spatially resolved integral-field spectroscopy can mitigate these effects and provide direct constraints on outflow kinematics and ionization state on kiloparsec scales. We present Kyoto Okayama Optical Low-dispersion Spectrograph fiber integral field unit (IFU) instrument optical integral-field spectroscopy of NGC 6552 obtained on the 3.8 m Seimei Telescope. Using spatially resolved emission-line ratios and nonparametric [O iii ] λ 5007 kinematics over the central ∼2 kpc, we test whether ionized-gas kinematics are locally coupled to excitation. The [O iii ] λ 5007 width W ₈₀ is broadly elevated across the inner region (∼530–830 km s ⁻¹ ) and declines monotonically with projected galactocentric distance, consistent with a centrally concentrated outflow that decelerates at larger radii. Despite this clear kinematic structure, neither W ₈₀ nor the velocity asymmetry parameter Δ v shows a statistically significant correlation with [O iii ] λ 5007/H β . Order-of-magnitude outflow energetics yield –0.28% (for assumed n _e = 50–1000 cm ⁻³ ), consistent with [O iii ]-based estimates tracing only the ionized phase of a multiphase outflow. We conclude that in NGC 6552, both the total line broadening traced by W ₈₀ and Δ v are consistent with being governed primarily by spatial dynamical structure and line-of-sight superposition of multiple kinematic components, with no statistically significant coupling to excitation-driven processes detected at our sensitivity level. A positive W ₈₀ –[O iii ] λ 5007/H β coupling does emerge in the small subset of bins for which the two-component fit is most strongly favored statistically, and deeper observations will be needed to confirm.
The Dynamic Central Environment of NGC 3516 Revealed by XRISM 国際共著査読有り

Anna Juráňová, Erin Kara, Ehud Behar, Elisa Costantini, Jon M. Miller, Daniele Rogantini, James N. Reeves, Valentina Braito, Jacobo Ebrero, Luigi Gallo, Noa Keshet, Gerard A. Kriss, Missagh Mehdipour, Hirofumi Noda, Atsushi Tanimoto, Francesco Tombesi, Tracey J. Turner, Satoshi Yamada

The Astrophysical Journal　1005　(1)　27-27　2026年6月22日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae6b79 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract We present a detailed, time-resolved analysis of the Fe K band of the Seyfert 1.5 galaxy NGC 3516 observed with XRISM. The 249 ks observation spanning ∼310 ks in elapsed time reveals an exceptionally rich and time-variable absorption spectrum. Six distinct absorption components are detected across multiple ionization states, spanning more than an order of magnitude in ionization parameter and a wide range of systemic velocities, from a potential inflow (+4300 km s ⁻¹ ) to an ultrafast outflow (−9800 km s ⁻¹ ), the latter detected at >3 σ for the first time in this source. Despite their diversity, the components exhibit relatively small broadening (≲420 km s ⁻¹ ), suggesting similar internal dynamics within a medium that has a complex structure. Time-resolved spectroscopy reveals pronounced variability in three highly ionized absorbers, with Fe xxv –Fe xxvi features that appear and disappear on timescales of tens of kiloseconds. This behavior likely reflects a combination of geometrical transits of clumpy gas and ionization-state changes driven by continuum variability. An additional temporary absorption feature in the red wing of the Fe K α line, consistent with Fe xxv absorption, indicates a possible transient ultrafast inflow at ∼15,000 km s ⁻¹ (∼5% c ). Finally, the continuum light curve exhibits a tentative ∼40 ks oscillatory pattern, accompanied by correlated shifts of a weak, narrow Fe K α emission feature, suggesting dynamic coupling between the continuum and the line-emitting region. Together, these results reveal an environment dominated by rapidly evolving, multiphase gas flows, where accretion, ejection, and ionization processes are tightly coupled on subparsec scales.
Blackbody Quasar and Radio Source (BBQSORS): A Candidate of Transitional Little Red Dots with a T ∼ 10 ⁴ K Blackbody Spectrum 国際共著査読有り

Yuxing 宇星 Zhong 仲, Xiaoyang Chen, Kohei Ichikawa, Youwen Kong, Kentaro Aoki, Satoshi Yamada, Tohru Nagao, Daisaburo Kido, Toshihiro Kawaguchi, Yoshiki Matsuoka, Toru Misawa, Shoichiro Mizukoshi, Masafusa Onoue, Ayumi Takahashi, Yoshiki Toba

The Astrophysical Journal Letters　1004　(1)　L2-L2　2026年6月2日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ae633b 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract JWST surveys have identified a new class of active galactic nuclei (AGNs) called little red dots (LRDs). Their observational properties challenge the canonical AGN paradigm and provide key insights into the early growth phase of the supermassive black holes (SMBHs). We report Subaru/PFS spectroscopic follow-up of a radio-loud quasar at z = 1.715 from the UNVEIL radio AGN catalog, including X-ray detections. The spectrum displays broad C iii ] λ 1909 and Mg ii λ 2800 emission lines with FWHM ≳4000 km s ⁻¹ , accompanied by narrow absorption features. The spectrum reveals a characteristic Λ-shape over the rest-frame wavelength ranging ∼1500–3500 Å. The underlying continuum cannot be reproduced by simply applying dust extinction to typical unobscured quasars. Alternatively, it is well described by a blackbody spectrum with a temperature of T ∼ 10 ⁴ K. This result agrees well with its UV to MIR photometry, which can be well modeled by three blackbody components representing the BH envelope ( T ≈ 9700 K), dust torus ( T ≈ 1500 K), and host galaxy dust ( T ∼ 80 K). The source is marginally detected in the GALEX NUV, revealing a potential V-shaped spectral energy distribution around 1400 Å, reminiscent of the spectral feature reported for LRDs whose V-shapes occur around 3000–4000 Å. This wavelength shift is broadly consistent with the temperature contrast between our blackbody component ( T ∼ 10 ⁴ K) and the lower effective temperature of T ∼ 5000 K expected for the BH envelope of LRDs. These properties suggest that this source might be caught in an evolutionary phase in which the dense gas envelope characteristic of LRD has begun to fragment, allowing us to witness the emergence of a quasar from an LRD-like state.
High-spectral-resolution X-Ray Observations of the Evolved Supermassive Stellar Binary System η Carinae: Fe K α Band Profile Revealed with XRISM 国際共著査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Michael F. Corcoran, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Emi Goto, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Shun Inoue, Daiki Ishi, Manabu Ishida, Yukiko Ishihara, Kumi Ishikawa, Yoshitaka Ishisaki, Francisco Junqueira, Jelle Kaastra, Timothy Kallman, Yoshiaki Kanemaru, Erin Kara, Satoru Katsuda, Richard L. Kelley, Caroline A. Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Bert Vander Meulen, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Asca Miyamoto, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva

The Astrophysical Journal　1003　(2)　156-156　2026年5月22日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae3a80 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract The supermassive binary system, η Carinae, is experiencing enormous wind-driven mass loss at a rate unparalleled in the rest of the Galaxy. Their wind–wind collision (WWC) continuously produces shock heated, X-ray-emitting plasmas. The XRISM X-ray observatory observed the system in 2023 and 2024 when the X-ray emission began to increase toward periastron passage in 2025. This paper reports unprecedentedly high-resolution X-ray spectra in the Fe K α band between 6.2 and 7.1 keV, obtained with the Resolve X-ray microcalorimeter. The hydrogen-like (Ly α ) and helium-like (He α ) lines reveal three velocity components. Two of them are broadened with maximum velocities of 2000–3000 km s ⁻¹ , likely originating from the postshock companion wind. The other is relatively narrow, with a Gaussian broadening of only ∼290 km s ⁻¹ in 1 σ , which may originate from the postshock companion wind at the WWC stagnation point or penetrating the primary wind. The Fe fluorescent lines exhibit a moderate blueshift and broadening with velocities at 100–200 km s ⁻¹ , consistent with the primary wind’s velocity field. The spectra also confirm a Compton shoulder of the He α line complex for the first time. Both fluorescing and scattering spectral profiles indicate that the binary system is seen from the companion side during these observations. The flux ratio of the Compton-scattering emission to the fluorescent line suggests substantial hydrogen depletion of the primary wind, expected from CNO-cycled hydrogen nuclear fusion gas.
Complex Nuclear Structure in Seyfert 2 Galaxy NGC 4388 Revealed by XRISM Observation 国際共著査読有り

Kanta Fujiwara, Yoshihiro Ueda, Shoji Ogawa, Yuya Nakatani, Jon M. Miller, Takashi Okajima, Taiki Kawamuro, Peter G Boorman, Luigi Gallo, Misaki Mizumoto, Richard Mushotzky, Hirofumi Noda, Yuichi Terashima, Francesco Tombesi, Bert Vander Meulen, Satoshi Yamada

The Astrophysical Journal　1003　(1)　6-6　2026年5月11日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae5e5c 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract We report results from the simultaneous XRISM (183 ks) and NuSTAR (62 ks) observations of the Seyfert 2 galaxy NGC 4388. This active galactic nucleus has the brightest Fe K α line among Compton-thin, obscured sources. To model the reflection continuum and fluorescent lines, we employ an updated version of XCLUMPY and a broad-line region (BLR) model with a disk-like geometry. The profile of the neutral Fe K fluorescent line is well described as the sum of three components convolved with Gaussians with FWHM values of ∼290 km s ⁻¹ , ∼1470 km s ⁻¹ , and ∼11,100 km s ⁻¹ . These line widths correspond to radii of 1.5 pc, 0.060 pc, and 1.0 × 10 ⁻³ pc by assuming Keplerian motion, which we interpret as the dusty torus, its inner edge region, and the BLR, respectively. The data suggest that the Fe K α BLR component is larger than that of H α (FWHM of 4500 km s ⁻¹ ) in the polarized optical spectrum, implying that the velocity field of the BLR is dominated by that parallel to the equatorial plane. In addition, Fe XXVI Ly α and Fe XXV absorption lines are detected, characterized by , , v _out ∼ 40 km s ⁻¹ , and σ _v ∼ 160 km s ⁻¹ . We infer that the absorber is gravitationally bound and is possibly associated with a failed wind, consistent with a radiation-driven fountain flow.
A XRISM study of highly ionized iron emission lines from the low-Eddington-ratio AGN in NGC 7213 国際共著査読有り

Kaito Murakami, Taiki Kawamuro, Ryota Tomaru, Hirokazu Odaka, Elias Kammoun, Shoji Ogawa, Stefano Bianchi, Hirofumi Noda, Claudio Ricci, Yuichi Terashima, Yoshihiro Ueda, Satoshi Yamada, Hironori Matsumoto

Publications of the Astronomical Society of Japan　2026年5月1日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psag049 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract We present an analysis of XRISM and NuSTAR data obtained for the nearby low-Eddington active galactic nucleus NGC 7213. Our goal is to examine whether its He-like and H-like iron emission lines can be reproduced by photoionization or collisional ionization processes. Using the broad-band energy coverage of our data (2–60 keV), we first constrained the continuum shape. Then, we focused on the iron-K band in the Resolve spectrum. Gaussian fits to Fe xxv He$\alpha$ and Fe xxvi Ly$\alpha$ lines suggest that they may have different velocity widths: $v_\sigma =790^{+370}_{-240}$ km s$^{-1}$ for Fe xxv and $v_\sigma =2610^{+1700}_{-1580}$ km s$^{-1}$ for Fe xxvi. In this case, the He$\alpha$ resonance line (w) and forbidden line (z) have similar intensities of ${\approx }0.5$–$0.6\times 10^{-5}$ ph s$^{-1}$ cm$^{-2}$, while the intercombination lines (x + y) are not significantly detected with upper limits of ${\lesssim }0.2\times 10^{-5}$ ph s$^{-1}$ cm$^{-2}$. Motivated by the possible difference in the line widths, we tested one- and two-zone photoionized and collisionally ionized models. Our results show that the additional ionized component is not significantly required, and the current data cannot uniquely determine whether photoionization or collisional ionization dominates. Moreover, if the Fe xxv He$\alpha$ complex implies that the weak x + y lines are suppressed relative to the w and z lines, such a structure is difficult to reproduce with either ionization model adopted. Finally, by comparing NGC 7213 with M 81$^\ast$, accreting at a much lower Eddington ratio of $\lambda _{\rm Edd}\sim 10^{-5}$, we found a decrease in the density of the gas responsible for highly ionized iron emission, which may imply that the density decreases with decreasing $\lambda _{\rm Edd}$.
Winds of Change: XRISM Resolve X-Ray Spectroscopy of NGC 4051 国際共著査読有り

James N. Reeves, Shoji Ogawa, Tracey J. Turner, Valentina Braito, Satoshi Yamada, Steven B. Kraemer, Hirofumi Noda, Anna Trindade Falcão, Martin Elvis, Giuseppina Fabbiano

The Astrophysical Journal　1001　(2)　137-137　2026年4月13日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae5527 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract NGC 4051 is a nearby (16.7 Mpc), Narrow Line Seyfert 1 galaxy (NLS1), which has a low black hole mass of 10 ⁶ M _⊙ . It is also known for its rapid X-ray variability, on timescales of kiloseconds, and has a complex, multicomponent wind in both the soft X-ray and Fe K bands. Here we present the first high-resolution XRISM Resolve spectrum of NGC 4051, which was captured in a historically bright state for a 150 ks exposure. XRISM resolves two blueshifted Fe K shell absorption troughs in the mean spectrum, which can be ascribed to H-like iron and arises from two outflow components with outflow velocities of 0.025 c and 0.04 c . A time-dependent spectral analysis shows that the iron K absorption is variable on timescales of less than a day, increasing in velocity over the duration of the observation. The velocity changes may be explained either by the passage of two separate transiting absorbers, of different velocities, or by a single accelerating outflow of approximately constant column density. In the latter case, the wind acceleration is likely to be too large to be caused by radiation pressure, and instead, magnetic driving is favored to accelerate the wind up to 0.04 c . The outflow can originate from an accretion disk wind, whose kinetic power is sub-Eddington, in contrast to recent examples of winds from powerful, luminous quasars observed by XRISM.
Accurate determination of chemical abundances near a supermassive black hole 国際共著査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. Garcia, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick Scott Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi G. Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Kanta Fujiwara, Takuma Izumi, Taiki Kawamuro, Keiichi Maeda, Yuya Nakatani, Frits Paerels, Ryosuke Uematsu, Bert Vander Meulen

Nature Astronomy　10　(6)　880-891　2026年3月31日
出版者・発行元： Springer Science and Business Media LLC
DOI： 10.1038/s41550-026-02817-6 　

eISSN：2397-3366
A fast starburst wind consumes most of the energy from supernovae 国際共著査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Kazuki Ampuku, Erin Boettcher, Skylar Grayson, Gabriel Grell, Peter Kosec, Seiya Sasamata, Evan Scannapieco

Nature　651　(8107)　909-913　2026年3月25日
出版者・発行元： Springer Science and Business Media LLC
DOI： 10.1038/s41586-026-10231-1 　

ISSN：0028-0836

eISSN：1476-4687
Resolving the Multiple Component Outflows in PG 1211+143. II. The Soft X-Ray View of the Ultrafast Outflow 国際共著査読有り

James N. Reeves, Valentina Braito, Misaki Mizumoto, Steven B. Kraemer, Ehud Behar, Chris Done, Kouichi Hagino, Gabriele A. Matzeu, Hirofumi Noda, Mariko Nomura, Shoji Ogawa, Ken Ohsuga, Atsushi Tanimoto, Tracey J. Turner, Yoshihiro Ueda, Satoshi Yamada, Sreeparna Ganguly, Paolo Somenzi, Omer Reich

The Astrophysical Journal　1000　(2)　170-170　2026年3月20日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae47e8 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract The nearby quasar PG 1211+143 hosts one of the prototypical examples of an ultrafast outflow (UFO), as seen in several past XMM-Newton and Chandra observations. In 2024 December, PG 1211+143 was observed simultaneously with XRISM Resolve and XMM-Newton, allowing both the Fe K and soft X-ray outflows to be examined at high resolution simultaneously. The Resolve spectrum revealed a forest of Fe K absorption lines from the UFO, comprising up to six discrete velocity components ranging from v / c = −0.074 to v / c = −0.40. Here, we present the simultaneous XMM-Newton Reflection Grating Spectrometer (RGS) spectrum, where three lower-ionization counterparts of the Fe K velocity zones are observed, at v / c = –0.074, −0.12, and −0.33. The soft X-ray absorbers tend to be less ionized than their Fe K counterparts, with their opacity arising mainly from Fe L-shell lines and highly ionized oxygen. By comparing the Resolve and RGS absorbers, we show that the outflow can be parameterized with a density profile varying with radius as r ^−5/3 , while the lower-ionization zones likely originate from denser clumps of gas. Pure electron scattering appears insufficient to provide the thrust needed to power the wind, unless sufficient low-ionization gas capable of radiative line driving exists outside of the line of sight. Overall, PG 1211+143 provides further evidence for the clumpy nature of accretion disk winds, as was recently revealed in the quasar PDS 456 with XRISM.
Diverse Origins of Broad H α Lines in Heavily Obscured Active Galactic Nuclei Revealed by Multiepoch Spectroscopy 国際共著査読有り

Shoichiro Mizukoshi, Takeo Minezaki, Subaru Ubukata, Kazuya Matsubayashi, Hiroaki Sameshima, Mitsuru Kokubo, Takashi Horiuchi, Hirofumi Noda, Satoshi Yamada, Bovornpratch Vijarnwannaluk, Chian-Chou Chen

The Astrophysical Journal　999　(2)　229-229　2026年3月6日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae38d9 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract According to the classical active galactic nucleus (AGN) model, broad emission lines originate from the broad-line region (BLR) and are observable only when the attenuation by the dusty torus is small. However, we recently found several heavily obscured ( A _V > 50 mag) AGNs with broad H α detections: MCG -3-34-64, UGC 5101, and Mrk 268. To investigate the origin of the observed broad line in these AGNs, we performed multiepoch optical spectroscopic observations to search for flux variability of the broad H α line. For MCG -3-34-64 and UGC 5101, no significant variability was detected, suggesting that the broad line of these AGNs may arise from sources other than the BLR. Spectral fitting analysis suggests a possible large contribution of ionized outflows to the observed broad component of MCG -3-34-64, while both the outflow and scattering by polar material can explain that of UGC 5101. For Mrk 268, we detected a significant (4.3 σ ) flux variation of the broad H α line by using the flux ratio of the H α complex and the [S ii ] λλ 6716, 6731 doublet, indicating that the broad line originates directly from the BLR. The lack of significant flux variation in the optical continuum implies that the line of sight to the nucleus of Mrk 268 is mildly obscured. Our results demonstrate that the observed broad H α lines in obscured AGNs likely have multiple origins. Such complexity may introduce additional uncertainties in black hole mass measurements of distant AGNs revealed by, e.g., JWST.
A XRISM/Resolve View of the Dynamics in the Hot Gaseous Atmosphere of M87 国際共著査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Matthew Charbonneau, Neo Dizdar, Masashi Fujita, Daisuke Ito, Jessica Martin, Hannah McCall, Helen Russell, John ZuHone

The Astrophysical Journal　998　(2)　210-210　2026年2月11日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae2c5c 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract The XRISM/Resolve microcalorimeter directly measured the gas velocities in the core of the Virgo Cluster, the closest example of active galactic nucleus (AGN) feedback in a cluster. This proximity allows us to resolve the kinematic impact of feedback on scales down to 5 kpc. Our spectral analysis reveals a high velocity dispersion of km s ⁻¹ near the AGN, which steeply declines to ∼60 km s ⁻¹ between 5 and 25 kpc in the northwest direction. The observed line-of-sight bulk velocity in all regions is broadly consistent with the central galaxy, M87, with a mild trend toward blueshifted motions at larger radii. Systematic uncertainties have been carefully assessed and do not affect the measurements. The central velocities, if attributed entirely to isotropic turbulence, correspond to a transonic intracluster medium at sub-6 kpc scales with 3D Mach number and a nonthermal pressure fraction of . Simple models of weak shocks and sound waves and calculations assuming isotropic turbulence both support the hypothesis that the velocity field reflects a mix of shock-driven expansion and turbulence. Compared to other clusters observed by XRISM to date, M87’s central region stands out as the most kinematically disturbed, exhibiting both the highest velocity dispersion and the largest 3D Mach number, concentrated at the smallest physical scales.
Disentangling multiple gas kinematic drivers in the Perseus galaxy cluster 国際共著査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi G. Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Ian Drury, Julie Hlavacek-Larrondo, Julian Meunier, Kostas Migkas, Lior Shefler, Phillip C. Stancil, Nhut Truong, Shutaro Ueda, Benjamin Vigneron, John ZuHone, Congyao Zhang, Annie Heinrich, Irina Zhuravleva, Elena Bellomi

Nature　2026年1月28日
出版者・発行元： Springer Science and Business Media LLC
DOI： 10.1038/s41586-025-10017-x 　

ISSN：0028-0836

eISSN：1476-4687
Resolving the Multiple Component Outflows in PG 1211+143. I. The Fe–K Absorption Structure and UFO Forest 国際共著査読有り

Misaki Mizumoto, James N. Reeves, Valentina Braito, Ehud Behar, Chris Done, Kouichi Hagino, Steven B. Kraemer, Gabriele A. Matzeu, Hirofumi Noda, Mariko Nomura, Shoji Ogawa, Ken Ohsuga, Atsushi Tanimoto, Tracey J. Turner, Yoshihiro Ueda, Satoshi Yamada, Sreeparna Ganguly, Paolo Somenzi

The Astrophysical Journal　997　(2)　219-219　2026年1月23日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae2853 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract We present the initial high-resolution X-ray spectroscopic observations of the Fe–K absorption structure in the luminous nearby quasar PG 1211+143, utilizing the X-ray Imaging and Spectroscopy Mission (XRISM). The primary objective is to characterize the Fe–K absorption features due to ultra-fast outflow (UFO) in this Eddington-luminosity source. Observations were conducted with XRISM’s Resolve and Xtend instruments, complemented by simultaneous data from XMM-Newton and NuSTAR. A historically bright phase was captured. The Resolve spectra clearly reveal a prominent P Cygni profile and resolves the Fe–K absorption into six distinct velocity components, ranging from v = −0.074 to −0.405 c . A similar superposition of multiple UFOs has been reported in PDS 456, suggesting that such a “UFO forest” structure may be a common feature of near Eddington-luminosity sources. Some UFO components exhibit narrow line widths of approximately σ ∼ 200 km s ⁻¹ , which may indicate that the outflows have reached their terminal velocities, thereby resulting in a smaller velocity shear. The mass outflow rate is estimated to be , which is of the order of the Eddington accretion rate. This suggests a physically plausible scenario where the outflow is a significant channel for mass ejection.
Discovery of an X-Ray Luminous Radio-loud Quasar at z = 3.4: A Possible Transitional Super-Eddington Phase 国際共著査読有り

Sakiko Obuchi, Kohei Ichikawa, Satoshi Yamada, Nozomu Kawakatu, Teng Liu, Naoki Matsumoto, Andrea Merloni, Kosuke Takahashi, Ingyin Zaw, Xiaoyang Chen, Kazuhiro Hada, Zsofi Igo, Hyewon Suh, Julien Wolf

The Astrophysical Journal　997　(2)　156-156　2026年1月21日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ae1d6d 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract We report the multiwavelength properties of eROSITA Final Equatorial Depth Survey (eFEDS) J084222.9+001000 (hereafter ID830), a quasar at z = 3.4351, identified as the most X-ray luminous radio-loud quasar in the eFEDS field. ID830 shows a rest-frame 0.5–2 keV luminosity of , with a steep X-ray photon index (Γ = 2.43 ± 0.21), and a significant radio counterpart detected with the Very Large Array FIRST 1.4 GHz and Very Large Array Sky Survey 3 GHz bands. The rest-frame UV to optical spectra from Sloan Digital Sky Survey and Subaru/MOIRCS J band show a dust-reddened quasar feature with A _V = 0.39 ± 0.08 mag, and the expected bolometric active galactic nuclei luminosity from the dust-extinction-corrected UV luminosity reaches L _bol,3000Å = (7.62 ± 0.31) × 10 ⁴⁶ erg s ⁻¹ . We estimate a black hole mass of M _BH = (4.40 ± 0.72) × 10 ⁸ M _⊙ based on the Mg II λ 2800 emission-line width, and Eddington ratios from the dust-extinction-corrected UV continuum luminosity and X-ray luminosity that reach λ _Edd,UV = 1.44 ± 0.24 and λ _Edd,X = 12.8 ± 3.9, respectively, both indicating super-Eddington accretion. ID830 shows a high ratio of UV to X-ray luminosities, α _OX = −1.20 ± 0.07 (or α _OX = −1.42 ± 0.07 after correcting for jet-linked X-ray excess), higher than quasars and little red dots in the super-Eddington phase with similar UV luminosities, with α _OX < −1.8. Such a high α _OX suggests the coexistence of a prominent radio jet and X-ray corona in this high-Eddington-accretion phase. We propose that ID830 may be in a transitional phase after an accretion burst, evolving from a super-Eddington to a sub-Eddington state, which could naturally describe the high α _OX .
XRISM Finds the Changing-look Active Galactic Nucleus NGC 1365 in an Extended Low State: A Dense, Highly Ionized Outflow Obscures the Central Source 国際共著査読有り

Fatima Zaidouni, Erin Kara, Peter Kosec, Ehud Behar, Richard Mushotzky, Michael Koss, A. Juráňová, Elias Kammoun, Laura W. Brenneman, Joheen Chakraborty, Ken Ebisawa, Megan E. Eckart, Andrew C. Fabian, Yasushi Fukazawa, Javier A. García, Liyi Gu, Megan Masterson, Shoji Ogawa, Takashi Okajima, Stéphane Paltani, Daniele Rogantini, Yuichi Terashima, Brian J. Williams, Satoshi Yamada

The Astrophysical Journal Letters　997　(1)　L26-L26　2026年1月19日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ae307d 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract We present the first XRISM/Resolve observations of the active galactic nucleus NGC 1365, obtained in 2024 February and July. NGC 1365 is known for rapid transitions between Compton-thick and Compton-thin states, along with strong absorption from a highly ionized wind. During our observations, the source was found in a persistent low-flux state, characterized by a decrease in hard-X-ray luminosity and significant line-of-sight obscuration. In this state, XRISM/Resolve reveals clear Fe xxv and Fe xxvi absorption lines together with, for the first time in this source, corresponding emission lines. These features may arise either from reemission from a photoionized wind (P Cygni profile) or from collisionally ionized gas associated with outflow-driven shocks in the interstellar medium. We estimate the wind launch radius to be approximately 10 ¹⁶ cm (∼10 ⁴ R _g ), consistent with the location of the X-ray broadline region. We also resolve a broadened Fe K α line by σ ∼ 1300 km s ⁻¹ , placing it at similar scales to the wind, consistent with radii inferred from disk-broadening models and the variability of the Fe K α broad line. The similarity of the Fe K α profile to the H β wing and broad Pa α width indicates that the X-ray-emitting region is likely cospatial with the optical/infrared broadline region and originates from the same gas.
Evaluation of the pointing accuracy of the X-Ray Imaging and Spectroscopy Mission during the first year 国際共著査読有り

Yoshiaki Kanemaru, Ryo Iizuka, Yoshitomo Maeda, Takashi Okajima, Takayuki Hayashi, Kazuhiro Kiyokane, Yuto Nihei, Takashi Kominato, Manabu Ishida, Chikara Natsukari, Shin Watanabe, Kousuke 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, Matthew P. Holland, Michael Loewenstein, Eric D. Miller, Tahir Yaqoob, Robert S. Hill, Morgan D. Waddy, Mark M. Mekosh, Joseph B. Fox, Isabella S. Brewer, Emily Aldoretta, Makoto Tashiro, Kenichi Toda, Hironori Maejima

Journal of Astronomical Telescopes, Instruments, and Systems　11　(04)　2025年12月18日
出版者・発行元： SPIE-Intl Soc Optical Eng
DOI： 10.1117/1.jatis.11.4.042025 　

ISSN：2329-4124
Delving into the depths of NGC 3783 with XRISM: III. Birth of an ultrafast outflow during a soft flare 査読有り

Liyi Gu, Keigo Fukumura, Jelle Kaastra, Megan Eckart, Ralf Ballhausen, Ehud Behar, Camille Diez, Matteo Guainazzi, Timothy Kallman, Erin Kara, Chen Li, Missagh Mehdipour, Misaki Mizumoto, Shoji Ogawa, Christos Panagiotou, Matilde Signorini, Atsushi Tanimoto, Keqin Zhao, Hirofumi Noda, Jon Miller, Satoshi Yamada

Astronomy & Astrophysics　704　A146-A146　2025年12月9日
出版者・発行元： EDP Sciences
DOI： 10.1051/0004-6361/202557189 　

ISSN：0004-6361

eISSN：1432-0746

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The 2024 X-ray/UV observation campaign of NGC 3783, led by XRISM, revealed the launch of an ultrafast outflow (UFO) with a radial velocity of 0.19 c (57 000 km s ⁻¹ ). This event is synchronized with the sharp decay, within less than half a day, of a prominent soft X-ray/UV flare. Accounting for the look-elsewhere effect, the XRISM Resolve data alone indicate a low probability of 2 × 10 ⁻⁵ that this UFO detection is due to random chance. The UFO features narrow H-like and He-like Fe lines with a velocity dispersion of ∼1000 km s ⁻¹ , suggesting that it originates from a dense clump. Beyond this primary detection, there are hints of weaker outflow signatures throughout the rise and fall phases of the soft flare. Their velocities increase from 0.05 c to 0.3 c over approximately three days, and they may be associated with a larger stream in which the clump is embedded. The radiation pressure is insufficient to drive the acceleration of this rapidly evolving outflow. The observed evolution of the outflow kinematics instead closely resembles that of solar coronal mass ejections, implying magnetic driving and, conceivably, reconnection near the accretion disk as the likely mechanisms behind both the UFO launch and the associated soft flare.
Chlorine and potassium enrichment in the Cassiopeia A supernova remnant 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz-Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. Garcia, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick Scott Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi G. Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Shin-ichiro Fujimoto, Kai Matsunaga, Manan Agarwal

Nature Astronomy　2025年12月4日
出版者・発行元： Springer Science and Business Media LLC
DOI： 10.1038/s41550-025-02714-4 　

eISSN：2397-3366
XRISM Constraints on Unidentified X-Ray Emission Lines, Including the 3.5 keV Line, in the Stacked Spectrum of 10 Galaxy Clusters 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Jean-Paul Breuer, Priyanka Chakraborty, Stefano Ettori, Andrew Fabian, Annie Heinrich, Marie Kondo, Julie HLavacek-Larrondo, Hannah McCall, Paul Nulsen, Tom Rose, Helen Russell, Arnab Sarkar, Evan Scannapieco, Kazunori Suda, Ming Sun, Prathamesh Tamhane, Nhut Truong, Norbert Werner, Congyao Zhang

The Astrophysical Journal Letters　994　(1)　L28-L28　2025年11月18日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ae17ad 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract We stack 3.75 Ms of early XRISM Resolve observations of 10 galaxy clusters to search for unidentified spectral lines in the E = 2.5–15 keV band (rest frame), including the E = 3.5 keV line reported in earlier low spectral resolution studies of cluster samples. Such an emission line may originate from the decay of the sterile neutrino, a warm dark matter (DM) candidate. No unidentified lines are detected in our stacked cluster spectrum, with the 3 σ upper limit on the m _s ∼ 7.1 keV DM particle decay rate (which corresponds to an E = 3.55 keV emission line) of Γ ∼ 1.0 × 10 ⁻²⁷ s ⁻¹ . This upper limit is 3–4 times lower than the one derived by Hitomi Collaboration from the Perseus observation but still 5 times higher than the XMM-Newton detection reported by E. Bulbul et al. in the stacked cluster sample. XRISM Resolve, with its high spectral resolution but small field of view, may reach the sensitivity needed to test the XMM-Newton cluster sample detection by combining several years worth of future cluster observations.
XRISM/Resolve view of Abell 2319: Turbulence, sloshing, and ICM dynamics 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo B Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, Francois Mernier, Eric Miller, Jon Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Riccardo Seppi, Itsuki Aihara, Yuki Omiya

Publications of the Astronomical Society of Japan　77　(6)　1278-1289　2025年11月17日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psaf109 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract 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 ($\sim$11 keV) in the north-west. The average gas velocity in the $3{^{\prime } } \times$ $4 {^{\prime } }$ region around the brightest cluster galaxy (BCG) covered by two Resolve pointings is consistent with that of the BCG to within 40 km s$^{-1}$ and we found modest average velocity dispersion of 230–250 km s$^{-1}$. On the other hand, spatially resolved spectroscopy reveals interesting variations. A blueshift of up to $\sim$230 km s$^{-1}$ 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 $\sim$400 km s$^{-1}$, 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.
XRISM/Resolve Reveals the Complex Iron Structure of NGC 7213: Evidence for Radial Stratification between Inner Disk and Broad-line Region 査読有り

E. Kammoun, T. Kawamuro, K. Murakami, S. Bianchi, F. Nicastro, A. Luminari, E. Aydi, M. Eracleous, O. K. Adegoke, E. Bertola, P. G. Boorman, V. Braito, G. Bruni, A. Comastri, P. Condò, M. Dadina, T. Enoto, J. A. García, V. E. Gianolli, F. A. Harrison, G. Lanzuisi, M. Laurenti, A. Marinucci, G. Mastroserio, H. Matsumoto, G. Matt, G. Matzeu, R. Middei, E. Nardini, H. Noda, H. Odaka, S. Ogawa, F. Panessa, E. Piconcelli, C. Pinto, J. M. Piotrowska, G. Ponti, C. Ricci, R. Ricci, R. Serafinelli, F. Shi, D. Stern, A. Tanimoto, Y. Terashima, R. Tomaru, F. Tombesi, A. Tortosa, Y. Ueda, F. Ursini, C. Vignali, S. Yamada, S. Yamada

The Astrophysical Journal Letters　994　(1)　L13-L13　2025年11月13日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ae18c2 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract We present the first high-resolution X-ray spectrum of NGC 7213 obtained with XRISM/Resolve, supported by simultaneous XMM-Newton, NuSTAR, and SOAR optical data. The XRISM spectrum resolves the neutral Fe K α into two components: a narrow core ( ), consistent with emission at the dust sublimation radius, and a broader asymmetric line, best described by disklike emission from ∼100 R _g . This disk component mirrors the profile of the double-peaked H α line observed in the optical. In addition, we detect broadened Fe xxv and Fe xxvi emission lines, whose inferred locations bridge the gap between the inner disk and the optical broad-line region. The weak narrow Fe K α equivalent width (EW = 32 ± 6 eV) and the absence of a Compton hump imply a low-covering-fraction, Compton-thin torus. Together, these results reveal a radially stratified structure in NGC 7213, spanning nearly 4 orders of magnitude in radius, and place the source in an intermediate-accretion state ( λ _Edd = 0.1%–1%), where the inner disk and broad-line region remain, while the torus shows signs of dissipation.
Comparing XRISM Cluster Velocity Dispersions with Predictions from Cosmological Simulations: Are Feedback Models Too Ejective? 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Weiguang Cui, Stefano Ettori, Skylar Grayson, Annie Heinrich, Hannah McCall, Dylan Nelson, Nobuhiro Okabe, Yuki Omiya, Arnab Sarkar, Evan Scannapieco, Ming Sun, Keita Tanaka, Nhut Truong, Daniel R. Wik, Congyao Zhang, John ZuHone

The Astrophysical Journal Letters　993　(1)　L11-L11　2025年10月24日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ae100c 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract The dynamics of the intracluster medium (ICM), the hot plasma that fills galaxy clusters, are shaped by gravity-driven cluster mergers and feedback from supermassive black holes (SMBHs) in the cluster cores. XRISM measurements of ICM velocities in several clusters offer insights into these processes. We compare XRISM measurements for nine galaxy clusters (Virgo, Perseus, Centaurus, Hydra-A, PKS 0745–19, A2029, Coma, A2319, and Ophiuchus) with predictions from three state-of-the-art cosmological simulation suites, TNG-Cluster, the Three Hundred Project GADGET-X, and GIZMO-SIMBA, that employ different models of feedback. In cool cores, XRISM reveals systematically lower velocity dispersions than the simulations predict, with all 10 measurements below the median simulated values by a factor of 1.5–1.7 on average and all falling within the bottom 10% of the predicted distributions. The observed kinetic-to-total pressure ratio is also lower, with a median value of 2.2%, compared to the predicted 5.0%–6.5% for the three simulations. Outside the cool cores and in non-cool-core (NCC) clusters, simulations show better agreement with XRISM measurements, except for the outskirts of the relaxed, cool-core cluster A2029, which exhibits an exceptionally low kinetic pressure support (<1%), with none of the simulated systems in either of the three suites reaching such low levels. The NCC Coma and A2319 exhibit dispersions at the lower end but within the simulated spread. Our comparison suggests that the three numerical models may overestimate the kinetic effects of SMBH feedback in cluster cores. Additional XRISM observations of NCC clusters will clarify if there is a systematic tension in the gravity-dominated regime as well.
Delving into the depths of NGC 3783 with XRISM: II. Cross-calibration of X-ray instruments used in the large, multi-mission observational campaign 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Yoshiaki Kanemaru, Erin Kara, Satoru Katsuda, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Camille Diez, Keigo Fukumura, Chen Li, Missagh Mehdipour, Christos Panagiotou, Matilde Signorini, Keqin Zhao

Astronomy & Astrophysics　702　A147-A147　2025年10月15日
出版者・発行元： EDP Sciences
DOI： 10.1051/0004-6361/202556000 　

ISSN：0004-6361

eISSN：1432-0746

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Context. Accurate X-ray spectroscopic measurements are fundamental for deriving basic physical parameters of the most abundant baryon components in the Universe. The plethora of X-ray observatories currently operational enables a panchromatic view of the high-energy emission of celestial sources. However, uncertainties in the energy-dependent calibration of the instrument transfer functions (e.g. the effective area, energy redistribution, or gain) can limit - and historically, did limit - the accuracy of X-ray spectroscopic measurements. Aims. We revised the status of the cross-calibration among the scientific payload on board four operation missions: Chandra, NuSTAR, XMM-Newton, and the recently launched XRISM. XRISM carries the micro-calorimeter Resolve, which yields the best energy resolution at energies ≥2 keV. For this purpose, we used the data from a 10-day-long observational campaign targeting the nearby active galactic nucleus NGC 3783, carried out in July 2024. Methods. We present a novel model-independent method for assessing the cross-calibration status that is based on a multi-node spline of the spectra with the highest-resolving power (XRISM/Resolve in our campaign). We also estimated the impact of the intrinsic variability of NGC 3783 on the cross-calibration status due to the different time coverages of participating observatories and performed an empirical reassessment of the Resolve throughput at low energies. Results. Based on this analysis, we derived a set of energy-dependent correction factors of the observed responses, enabling a statistically robust analysis of the whole spectral dataset. They will be employed in subsequent papers describing the astrophysical results of the campaign.
Stratified wind from a super-Eddington X-ray binary is slower than expected 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick Scott Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi G. Tsuru, Aysegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Joey Neilsen, Ryota Tomaru, Missagh Mehdipour

Nature　646　(8083)　57-61　2025年9月17日
出版者・発行元： Springer Science and Business Media LLC
DOI： 10.1038/s41586-025-09495-w 　

ISSN：0028-0836

eISSN：1476-4687

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Abstract Accretion disks in strong gravity ubiquitously produce winds, seen as blueshifted absorption lines in the X-ray band of both stellar mass X-ray binaries (black holes and neutron stars)^1–4 and supermassive black holes⁵. Some of the most powerful winds (termed Eddington winds) are expected to arise from systems in which radiation pressure is sufficient to unbind material from the inner disk (L ≳ L _Edd). These winds should be extremely fast and carry a large amount of kinetic power, which, when associated with supermassive black holes, would make them a prime contender for the feedback mechanism linking the growth of those black holes with their host galaxies⁶. Here we show the XRISM Resolve spectrum of the galactic neutron star X-ray binary, GX 13+1, which reveals one of the densest winds ever seen in absorption lines. This Compton-thick wind significantly attenuates the flux, making it appear faint, although it is intrinsically more luminous than usual (L ≳ L _Edd). However, the wind is extremely slow, more consistent with the predictions of thermal-radiative winds launched by X-ray irradiation of the outer disk than with the expected Eddington wind driven by radiation pressure from the inner disk. This puts new constraints on the origin of winds from bright accretion flows in binaries, but also highlights the very different origin required for the ultrafast (v ~ 0.3c) winds seen in recent Resolve observations of a supermassive black hole at a similarly high Eddington ratio⁷.
In-orbit science operations for the X-Ray Imaging and Spectroscopy Mission 国際共著査読有り

Katsuhiro Hayashi, Makoto Tashiro, Yukikatsu Terada, Tessei Yoshida, Shoji Ogawa, Yoshiaki Kanemaru, Kotaro Fukushima, Akio Hoshino, Chris Baluta, Hiromitsu Takahashi, Masayoshi Nobukawa, Tsunefumi Mizuno, Kazuhiro Nakazawa, Shin’ichiro Uno, Shin Watanabe, Ryo Iizuka, Rie Sato, Matthew P. Holland, Michael Loewenstein, Koji Mukai, Jan-Uwe Ness, Guillaume Belanger, Matteo Guainazzi, 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, Eric D. Miller, Tahir Yaqoob, Robert S. Hill, Morgan D. Waddy, Mark M. Mekosh, Joseph B. Fox, Emily Aldoretta, Isabella S. Brewer, Kenji Hamaguchi, François Mernier, Anna Ogorzalek, Katja Pottschmidt, Mihoko Yukita, Ayşegül Tümer, Edward J. Sabol, 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, Taichi Nakamoto, Chulsoo Kang, Hironori Maejima, Ken’ichi Toda, Chikara Natsukari

Journal of Astronomical Telescopes, Instruments, and Systems　11　(04)　2025年9月8日
出版者・発行元： SPIE-Intl Soc Optical Eng
DOI： 10.1117/1.jatis.11.4.042017 　

ISSN：2329-4124
Constraining gas motion and non-thermal pressure beyond the core of the Abell 2029 galaxy cluster with XRISM 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi C Gallo, Javier A García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice A Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric Miller, Jon M Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Tommaso Bartalesi, Stefano Ettori, Roman Kosarzycki, Lorenzo Lovisari, Tom Rose, Arnab Sarkar, Ming Sun, Prathamesh Tamhane

Publications of the Astronomical Society of Japan　77　(Supplement_1)　S242-S253　2025年8月18日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psaf055 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract We report on a detailed spectroscopic study of the gas dynamics and hydrostatic mass bias of the galaxy cluster Abell 2029, utilizing high-resolution observations from XRISM Resolve. Abell 2029, known for its cool core and relaxed X-ray morphology, provides an excellent opportunity to investigate the influence of gas motions beyond the central region. Expanding upon prior studies that revealed low turbulence and bulk motions within the core, our analysis covers regions out to the scale radius $R_{2500}$ (670 kpc) based on three radial pointings extending from the cluster center toward the northern side. We obtain accurate measurements of bulk and turbulent velocities along the line of sight. The results indicate that non-thermal pressure accounts for no more than 2% of the total pressure at all radii, with a gradual decrease outward. The observed radial trend differs from many numerical simulations, which often predict an increase in non-thermal pressure fraction at larger radii. These findings suggest that deviations from hydrostatic equilibrium are small, leading to a hydrostatic mass bias of around 2% across the observed area.
Thermal and kinematic properties of ejecta in SN1987A revealed by XRISM 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi C Gallo, Javier A García, Liyi Gu, Matteo Guainazzi, Roberta Giuffrida, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Ryunosuke Kikuchi, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice A Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Tsukasa Matsushima, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D Miller, Jon M Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick Scott Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Jiro Shimoda, Aurora Simionescu, Randall K Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Go Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Marco Miceli, Vincenzo Sapienza

Publications of the Astronomical Society of Japan　77　(Supplement_1)　S193-S208　2025年8月18日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psaf056 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract We present an analysis of high-resolution spectra from the shock-heated plasmas in SN 1987A, based on an observation using the Resolve instrument onboard the X-Ray Imaging and Spectroscopy Mission (XRISM). The 1.7–10 keV Resolve spectra are accurately represented by a single-component, plane-parallel shock plasma model, with a temperature of $2.84_{-0.08}^{+0.09}$ keV and an ionization parameter of $2.64_{-0.45}^{+0.58}$ × $10^{11}\,\,{\rm s\,\, cm}^{-3}$. The Resolve spectra are also well reproduced by the 3D magneto-hydrodynamic simulation presented by Orlando et al. (2020, A&A, 636, A22) suggesting substantial contribution from the ejecta. The metal abundances obtained with Resolve align with the Large Magellanic Cloud value, indicating that the X-rays in 2024 originate from “non-metal-rich” shock-heated ejecta and the reverse shock has not reached the inner metal-rich region of ejecta. Doppler widths of the atomic lines from Si, S, and Fe correspond to velocities of 1500–1700 km s$^{-1}$, where the thermal broadening effects in this non-metal-rich plasma are negligible. Therefore, the line broadening seen in Resolve spectra is determined by the large bulk motion of ejecta. For reference, we determined a $90\%$ upper limit on non-thermal emission from a pulsar wind nebula at $4.3 \times 10^{-13}$ erg cm$^{-2}$ s$^{-1}$ in the 2–10 keV range, aligning with NuSTAR findings by Greco et al. (2022, ApJ, 931, 132). Additionally, we searched for the $^{44}$Sc K line feature and found a $1\sigma$ upper limit of $1.0 \times 10^{-6}$ photons cm$^{-2}$ s$^{-1}$, which translates to an initial $^{44}$Ti mass of approximately $2 \times 10^{-4}\, M_{\odot }$, consistent with previous X-ray to soft gamma-ray observations (Boggs et al. 2015, Science, 348, 670; Grebenev et al. 2012, Nature, 490, 373; Leising 2006, ApJ, 651, 1019).
Kinematic Evidence for Bipolar Ejecta Flows in the Galactic Supernova Remnant W49B 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard L. Kelley, Caroline A. Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice A. Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Hidetoshi Sano, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi G. Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Yuki Amano, Amy Gall, Sharon Mitrani, Kaito Murakami, Roi Rahin, Nari Suzuki

The Astrophysical Journal Letters　988　(2)　L58-L58　2025年7月28日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ade138 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract W49B is a unique Galactic supernova remnant with centrally peaked, “bar”-like ejecta distribution, which was once considered evidence for a hypernova origin that resulted in a bipolar ejection of the stellar core. However, chemical abundance measurements contradict this interpretation. Closely connected to the morphology of the ejecta is its velocity distribution, which provides critical details for understanding the explosion mechanism. We report the first ever observational constraint on the kinematics of the ejecta in W49B using the Resolve microcalorimeter spectrometer on the X-ray Imaging and Spectroscopy Mission (XRISM). Using XRISM/Resolve, we measured the line-of-sight velocity traced by the Fe Heα emission, which is the brightest feature in the Resolve spectrum, to vary by ±300 km s⁻¹ with a smooth east-to-west gradient of a few tens of kilometers per second per parsec along the major axis. Similar trends in the line-of-sight velocity structure were found for other Fe-group elements Cr and Mn, traced by the Heα emission, and also for intermediate-mass elements Si, S, Ar, and Ca, traced by the Lyα emission. The discovery of the east–west gradient in the line-of-sight velocity, together with the absence of a twin-peaked line profile or enhanced broadening in the central region, clearly rejects the equatorially expanding disk model. In contrast, the observed velocity structure suggests bipolar flows reminiscent of a bipolar explosion scenario. An alternative scenario would be a collimation of the ejecta by an elongated cavity sculpted by bipolar stellar winds.
Quantum Machine Learning for Identifying Transient Events in X-Ray Light Curves 査読有り

Taiki Kawamuro, Shinya Yamada, Shigehiro Nagataki, Shunji Matsuura, Yusuke Sakai, Satoshi Yamada

The Astrophysical Journal　2025年7月10日

DOI： 10.3847/1538-4357/adda43 　
Unraveling the structure of the stratified ultra-fast outflows in PDS 456 with XRISM 査読有り

Yerong Xu, Luigi C Gallo, Kouichi Hagino, James N Reeves, Francesco Tombesi, Misaki Mizumoto, Alfredo Luminari, Adam G Gonzalez, Ehud Behar, Rozenn Boissay-Malaquin, Valentina Braito, Pierpaolo Condó, Chris Done, Aiko Miyamoto, Ryuki Mizukawa, Hirokazu Odaka, Riki Sato, Atsushi Tanimoto, Makoto Tashiro, Tahir Yaqoob, Satoshi Yamada

Publications of the Astronomical Society of Japan　77　(Supplement_1)　S223-S241　2025年7月8日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psaf070 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract Multiple clumpy wind components ($v_\mathrm{out}\sim 0.2\!-\!0.3c$) in the luminous quasar PDS 456 have recently been resolved in the Fe K band for the first time, thanks to the high-resolution X-ray spectrometer Resolve onboard XRISM. In this paper, we investigate the structure of ultra-fast outflows (UFOs) using coordinated observations from XRISM, XMM–Newton, and NuSTAR, along with the self-consistently calculated photoionization model PION. Our results reveal a stratified ionization structure, characterized by a scaling relation between wind velocity and ionization parameter $v_\mathrm{out}\propto \xi ^{(0.14\pm 0.04)}$. To evaluate the screening effect in photoionization modeling, we tested all possible order permutations of six PION components. We find that highly ionized UFOs ($\log \xi &gt;4.5$) are insensitive to their relative positions, whereas the soft X-ray UFO ($\log \xi \sim 3$ and $v_\mathrm{out}\sim 0.27c$) and the lowest-ionized hard X-ray UFO ($\log \xi \sim 4.1$ and $v_\mathrm{out}\sim 0.23c$) are statistically favored—based on the evidence from both the C-statistic and Bayesian analysis—to occupy the middle and innermost layers, respectively. This suggests a possible trend where slower UFOs are launched from regions closer to the supermassive black hole. The soft X-ray UFO is found to be thermally unstable, regardless of its relative position. However, its location remains unclear. Our sequence analysis and its similarity to hard X-ray UFOs suggest that they may be co-spatial, while variability constraints support its location within the broad-line region at sub-parsec scales. Simulations with XRISM with an open gate valve show that high-resolution soft X-ray data can enhance the reliability of our results. Furthermore, simulations with the future X-ray mission NewAthena demonstrate its capability to resolve the absorber sequence and spatial distributions, enabling the determination of UFO structures and their roles in active galactic nucleus feedback.
Verification of the timing system for the X-ray Imaging and Spectroscopy Mission in the GPS unsynchronized mode 国際共著査読有り

Megumi Shidatsu, Yukikatsu Terada, Takashi Kominato, So Kato, Ryohei Sato, Minami Sakama, Takumi Shioiri, Yugo Motogami, Yuuki Niida, Chulsoo Kang, Toshihiro Takagi, Taichi Nakamoto, 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, Tahir Yaqoob, Eric D. Miller, Robert S. Hill, Efrain C. Perez-Solis, Morgan D. Waddy, Mark Mekosh, Joseph B. Fox, Isabella S. Brewer, Emily Aldoretta, Koji Mukai, Kenji Hamaguchi, François Mernier, Anna Ogorzalek, Katja Pottschmidt, Mihoko Yukita

Journal of Astronomical Telescopes, Instruments, and Systems　11　(04)　2025年6月3日
出版者・発行元： SPIE-Intl Soc Optical Eng
DOI： 10.1117/1.jatis.11.4.042012 　

ISSN：2329-4124
XRISM Forecast for the Coma Cluster: Stormy, with a Steep Power Spectrum 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Daiki Ishi, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzałek, Takashi Okajima, Naomi Ota, Stéphane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Ayşegül Tümer, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shutaro Ueda, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Andrew Fabian, Dylan Nelson, Nobuhiro Okabe, Annalisa Pillepich, Cicely Potter, Manon Regamey, Kosei Sakai, Mona Shishido, Nhut Truong, Daniel R. Wik, John ZuHone

The Astrophysical Journal Letters　985　(1)　L20-L20　2025年5月19日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/add2f6 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract The XRISM Resolve microcalorimeter array measured the velocities of hot intracluster gas at two positions in the Coma galaxy cluster: squares at the center and at 6 (170 kpc) to the south. We find the line-of-sight velocity dispersions in those regions to be σ _z = 208 ± 12 km s⁻¹ and 202 ± 24 km s⁻¹, respectively. The central value corresponds to a 3D Mach number of M = 0.24 ± 0.015 and a ratio of the kinetic pressure of small-scale motions to thermal pressure in the intracluster plasma of only 3.1% ± 0.4%, at the lower end of predictions from cosmological simulations for merging clusters like Coma, and similar to that observed in the cool core of the relaxed cluster A2029. Meanwhile, the gas in both regions exhibits high line-of-sight velocity differences from the mean velocity of the cluster galaxies, Δv _z = 450 ± 15 km s⁻¹ and 730 ± 30 km s⁻¹, respectively. A small contribution from an additional gas velocity component, consistent with the cluster optical mean, is detected along a sight line near the cluster center. The combination of the observed velocity dispersions and bulk velocities is not described by a Kolmogorov velocity power spectrum of steady-state turbulence; instead, the data imply a much steeper effective slope (i.e., relatively more power at larger linear scales). This may indicate either a very large dissipation scale, resulting in the suppression of small-scale motions, or a transient dynamic state of the cluster, where large-scale gas flows generated by an ongoing merger have not yet cascaded down to small scales.
Structured ionized winds shooting out from a quasar at relativistic speeds 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick Scott Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi G. Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Valentina Braito, Pierpaolo Condò, Keigo Fukumura, Adam Gonzalez, Alfredo Luminari, Aiko Miyamoto, Ryuki Mizukawa, James Reeves, Riki Sato, Francesco Tombesi, Yerong Xu

Nature　641　(8065)　1132-1136　2025年5月14日
出版者・発行元： Springer Science and Business Media LLC
DOI： 10.1038/s41586-025-08968-2 　

ISSN：0028-0836

eISSN：1476-4687
X-Ray Imaging and Spectroscopy Mission 査読有り

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
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psaf023 　

ISSN：0004-6264

eISSN：2053-051X

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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.
AGN outflows and their properties in Mrk 766 as revealed by KOOLS-IFU on the Seimei Telescope 査読有り

Kyuseok Oh, Yoshihiro Ueda, Satoshi Yamada, Yoshiki Toba, Keisuke Isogai, Atsushi Tanimoto, Shoji Ogawa, Ryosuke Uematsu, Yuya Nakatani, Kanta Fujiwara, Yuta Okada, Kazuya Matsubayashi, Kenta Setoguchi

Publications of the Astronomical Society of Japan　2025年4月9日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psaf025 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract We present the emission-line flux distributions and their ratios, as well as the gas outflow features, of the innermost 2 kpc region of the type 1 Seyfert galaxy Mrk 766, using the Kyoto Okayama Optical Low-dispersion Spectrograph with an optical-fiber integral field unit on the Seimei Telescope. We find that the central region of Mrk 766 is kinematically disturbed, exhibiting asymmetric and radially distributed active galactic nucleus (AGN)-driven ionized gas outflows traced by [O iii]$\lambda 5007$ with velocities exceeding 500 ${\rm km}~{\rm s}^{-1}$. The mass of the ionized gas outflow is estimated to be $10^{4.65-5.95}\, M_{\odot }$, and the mass outflow rate is 0.14–2.73 $M_{\odot }$ yr$^{-1}$. This corresponds to a kinetic power, $\dot{E}_{\rm K}$, of $4.31 \times 10^{40} \ {\rm erg} \ {\rm s^{-1 } }&lt; \dot{E}_{\rm K} &lt; 8.62 \times 10^{41} \ {\rm erg} \ {\rm s^{-1 } }$, which is equivalent to 0.08%–1.53% of the bolometric luminosity, $L_{\rm bol}$. This result is consistent with other observed properties of ionized gas outflows, although it is lower than the theoretical predictions in AGN feedback models ($\sim$5%), implying that ionized gas outflows traced by [O iii]$\lambda 5007$ represent only a minor fraction of the total outflows ejected from the host galaxy. Given the asymmetric and radially distributed outflow signatures observed across the host galaxy within the limited field of view, the maximum distance that the outflowing gas has traveled remains an open question.
Development of the timing system for the X-ray imaging and spectroscopy mission 査読有り

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, Morgan D. Waddy, Mark Mekosh, Joseph B. Fox, Emily Aldoretta, Isabella Brewer, Koji Mukai, Kenji Hamaguchi, François Mernier, Anna Ogorzalek, Katja Pottschmidt, Mihoko Yukita, Toshihiro Takagi, Yugo Motogami, Teruaki Enoto, Takaaki Tanaka, Taichi Nakamoto, Chulsoo Kang, Tsuyoshi Miyazaki

Journal of Astronomical Telescopes, Instruments, and Systems　11　(04)　2025年4月7日
出版者・発行元： SPIE-Intl Soc Optical Eng
DOI： 10.1117/1.jatis.11.4.042007 　

ISSN：2329-4124
XRISM Reveals Low Nonthermal Pressure in the Core of the Hot, Relaxed Galaxy Cluster A2029 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Tommaso Bartalesi, Stefano Ettori, Roman Kosarzycki, Lorenzo Lovisari, Tom Rose, Arnab Sarkar, Ming Sun, Prathamesh Tamhane

The Astrophysical Journal Letters　982　(1)　L5-L5　2025年3月12日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ada7cd 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract 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 ∣v _bulk∣ < 100 km s⁻¹. We robustly measure the field-integrated ICM velocity dispersion to be σ _v = 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 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.
The bulk motion of gas in the core of the Centaurus galaxy cluster 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick Scott Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, María Díaz Trigo, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi G. Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Y. Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Marie Kondo, Norbert Werner, Tomáš Plšek, Ming Sun, Kokoro Hosogi, Anwesh Majumder

Nature　638　(8050)　365-369　2025年2月12日
出版者・発行元： Springer Science and Business Media LLC
DOI： 10.1038/s41586-024-08561-z 　

ISSN：0028-0836

eISSN：1476-4687
Overionized plasma in the supernova remnant Sagittarius A East anchored by XRISM observations 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz-Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D Miller, Jon M Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick Scott Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi G Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Q Daniel Wang, Yuki Amano, Kojiro Tanaka, Takuto Narita, Yuken Ohshiro, Anje Yoshimoto, Yuma Aoki, Mayura Balakrishnan

Publications of the Astronomical Society of Japan　77　(1)　L1-L8　2024年12月26日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psae111 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract 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 $1.39 \pm 0.12$, 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 $\gt\! 4\:$keV. The recombination timescale was constrained to be $\lt\! 8 \times 10^{11} \:$cm$^{-3}\:$s. The small velocity dispersion of $109 \pm 6\:$km$\:$s$^{-1}$ indicates a low Fe ion temperature $\lt\! 8\:$keV and a small expansion velocity $\lt\! 200\:$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.
The XRISM/Resolve View of the Fe K Region of Cyg X-3 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, María Díaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Satoshi Eguchi, Teruaki Enoto, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Ryota Tomaru, Tasuku Hayashi, Tomohiro Hakamata, Daiki Miura, Karri Koljonen, Mike McCollough

The Astrophysical Journal Letters　977　(2)　L34-L34　2024年12月11日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ad8ed0 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract 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.
The XRISM first-light observation: Velocity structure and thermal properties of the supernova remnant N 132D 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz-Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D Miller, Jon M Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick Scott Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi G Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Manan Agarwal, Yuken Ohshiro

Publications of the Astronomical Society of Japan　76　(6)　1186-1201　2024年10月10日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psae080 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract 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 $\sigma _v \sim 450$ km s$^{-1}$. However, the Fe He$\alpha$ lines are substantially broadened with $\sigma _v \sim 1670$ km s$^{-1}$. 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$\alpha$ 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 $-1000 \lesssim V_{\rm rs}$ (km s$^{-1}$) $\lesssim 3300$ (in the observer frame). We also find that Fe Ly$\alpha$ emission is redshifted with a bulk velocity of $\sim 890$ km s$^{-1}$, 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.
Discovery of a hyperluminous quasar at z = 1.62 with Eddington ratio &gt;3 in the eFEDS field confirmed by KOOLS-IFU on Seimei Telescope 査読有り

Yoshiki Toba, Keito Masu, Naomi Ota, Zhen-Kai Gao, Masatoshi Imanishi, Anri Yanagawa, Satoshi Yamada, Itsuki Dosaka, Takumi Kakimoto, Seira Kobayashi, Neiro Kurokawa, Aika Oki, Sorami Soga, Kohei Shibata, Sayaka Takeuchi, Yukana Tsujita, Tohru Nagao, Masayuki Tanaka, Yoshihiro Ueda, Wei-Hao Wang

Publications of the Astronomical Society of Japan　76　(6)　1173-1180　2024年9月20日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psae078 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract We report the discovery of a hyperluminous type 1 quasar (eFEDS J082826.9-013911; eFEDS J0828-0139) at $z_{\rm spec} = 1.622$ with a super-Eddington ratio ($\lambda _{\rm Edd}$). We perform the optical spectroscopic observations with KOOLS-IFU (the Kyoto Okayama Optical Low-dispersion Spectrograph with optical fiber) on the Seimei Telescope. The black hole mass ($M_{\rm BH}$) based on the single-epoch method with Mg ii$\lambda$2798 is estimated to be $M_{\rm BH} = {(6.2 \pm 1.2) }\times 10^8\, M_{\odot }$. To measure the precise infrared luminosity ($L_{\rm IR}$), we obtain submillimeter data taken by SCUBA-2 on the James Clerk Maxwell Telescope and conduct the spectral energy distribution analysis with X-ray to submillimeter data. We find that $L_{\rm IR}$ of eFEDS J0828-0139 is $L_{\rm IR} = {(6.8 \pm 1.8)} \times 10^{13}\, L_{\odot }$, confirming the existence of a hypeluminous infrared galaxy. $\lambda _{\rm Edd}$ is estimated to be $\lambda _{\rm Edd} = {3.6 \pm 0.7}$, making it a quasar with one of the highest BH mass accretion rates at cosmic noon.
XRISM Spectroscopy of the Fe Kα Emission Line in the Seyfert Active Galactic Nucleus NGC 4151 Reveals the Disk, Broad-line Region, and Torus 査読有り

Marc Audard, Hisamitsu Awaki, Ralf Ballhausen, Aya Bamba, Ehud Behar, Rozenn Boissay-Malaquin, Laura Brenneman, Gregory V. Brown, Lia Corrales, Elisa Costantini, Renata Cumbee, Maria Diaz Trigo, Chris Done, Tadayasu Dotani, Ken Ebisawa, Megan E. Eckart, Dominique Eckert, Teruaki Enoto, Satoshi Eguchi, Yuichiro Ezoe, Adam Foster, Ryuichi Fujimoto, Yutaka Fujita, Yasushi Fukazawa, Kotaro Fukushima, Akihiro Furuzawa, Luigi Gallo, Javier A. García, Liyi Gu, Matteo Guainazzi, Kouichi Hagino, Kenji Hamaguchi, Isamu Hatsukade, Katsuhiro Hayashi, Takayuki Hayashi, Natalie Hell, Edmund Hodges-Kluck, Ann Hornschemeier, Yuto Ichinohe, Manabu Ishida, Kumi Ishikawa, Yoshitaka Ishisaki, Jelle Kaastra, Timothy Kallman, Erin Kara, Satoru Katsuda, Yoshiaki Kanemaru, Richard Kelley, Caroline Kilbourne, Shunji Kitamoto, Shogo Kobayashi, Takayoshi Kohmura, Aya Kubota, Maurice Leutenegger, Michael Loewenstein, Yoshitomo Maeda, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, François Mernier, Eric D. Miller, Jon M. Miller, Ikuyuki Mitsuishi, Misaki Mizumoto, Tsunefumi Mizuno, Koji Mori, Koji Mukai, Hiroshi Murakami, Richard Mushotzky, Hiroshi Nakajima, Kazuhiro Nakazawa, Jan-Uwe Ness, Kumiko Nobukawa, Masayoshi Nobukawa, Hirofumi Noda, Hirokazu Odaka, Shoji Ogawa, Anna Ogorzalek, Takashi Okajima, Naomi Ota, Stephane Paltani, Robert Petre, Paul Plucinsky, Frederick S. Porter, Katja Pottschmidt, Kosuke Sato, Toshiki Sato, Makoto Sawada, Hiromi Seta, Megumi Shidatsu, Aurora Simionescu, Randall Smith, Hiromasa Suzuki, Andrew Szymkowiak, Hiromitsu Takahashi, Mai Takeo, Toru Tamagawa, Keisuke Tamura, Takaaki Tanaka, Atsushi Tanimoto, Makoto Tashiro, Yukikatsu Terada, Yuichi Terashima, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Yoshihiro Ueda, Shinichiro Uno, Jacco Vink, Shin Watanabe, Brian J. Williams, Satoshi Yamada, Shinya Yamada, Hiroya Yamaguchi, Kazutaka Yamaoka, Noriko Yamasaki, Makoto Yamauchi, Shigeo Yamauchi, Tahir Yaqoob, Tomokage Yoneyama, Tessei Yoshida, Mihoko Yukita, Irina Zhuravleva, Xin Xiang, Takeo Minezaki, Margaret Buhariwalla, Dimitra Gerolymatou, Scott Hagen

The Astrophysical Journal Letters　973　(1)　L25-L25　2024年9月1日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/ad7397 　

ISSN：2041-8205

eISSN：2041-8213

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Abstract 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 . 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.
Development and operation status of X-Ray Imaging and Spectroscopy Mission (XRISM)

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
出版者・発行元： SPIE
DOI： 10.1117/12.3019325 　
The in-orbit XRISM science operations

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
出版者・発行元： SPIE
DOI： 10.1117/12.3018908 　
Detail design of the XRISM Timing System and its verification in the nominal operation mode

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
出版者・発行元： SPIE
DOI： 10.1117/12.3019329 　
Verification of the XRISM timing system in the GPS unsynchronized mode

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
出版者・発行元： SPIE
DOI： 10.1117/12.3019651 　
Evaluation of the initial pointing accuracy of XRISM

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
出版者・発行元： SPIE
DOI： 10.1117/12.3016594 　
Wide-band x-ray observatory for the time domain astronomy era: CHRONOS

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
出版者・発行元： SPIE
DOI： 10.1117/12.3018366 　
Updated picture of the active galactic nuclei with dusty/dust-free gas structures and effects of the radiation pressure 査読有り

Shoichiro Mizukoshi, Takeo Minezaki, Hiroaki Sameshima, Mitsuru Kokubo, Hirofumi Noda, Taiki Kawamuro, Satoshi Yamada, Takashi Horiuchi

Monthly Notices of the Royal Astronomical Society　532　(1)　666-680　2024年6月13日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/mnras/stae1482 　

ISSN：0035-8711

eISSN：1365-2966

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ABSTRACT This study investigates the properties of two gas structures of X-ray selected active galactic nuclei (AGNs), that is, dusty and dust-free gas components, by separating them with the line-of-sight dust extinction ($A_V$) and the neutral gas column density ($N_{\mathrm{H } }$). The typical column density of the dusty and dust-free gas differs depending on the Seyfert type, indicating that both structures have anisotropic column density distributions. The number of targets with the dusty gas column density ($N_{\mathrm{H,d } }$) of $\log N_{\mathrm{H,d } }\ [\mathrm{cm^{-2 } }]\gt 23$ is much smaller than that with the same column density of the dust-free gas. This result indicates that the optically thick part of the dusty gas structure is very thin. There are very few targets with a larger Eddington ratio ($f_{\mathrm{Edd } }$) than the effective Eddington limit of the dusty gas and the covering factor of the dusty gas with $22\le \log N_{\mathrm{H,d } }\ [\mathrm{cm^{-2 } }]\lt 24$ exhibits a clear drop at the effective Eddington limit. These results support the scenario wherein the covering factor of the dusty torus decreases in a high Eddington ratio owing to the radiation-driven dusty gas outflow. The covering factor of the dust-free gas with the column density ($N_{\mathrm{H,df } }$) of $22\le \log N_{\mathrm{H,df } }\ [\mathrm{cm^{-2 } }]\lt 24$ similarly exhibits the decrease in high Eddington ratio, although it may be owing to the dust-free gas outflow driven by certain other mechanisms than the radiation pressure. Finally, we propose an updated picture of the AGN gas structure based on our results and the literature.
ALMA Lensing Cluster Survey: Full Spectral Energy Distribution Analysis of z ∼ 0.5–6 Lensed Galaxies Detected with millimeter Observations 査読有り

Ryosuke Uematsu, Yoshihiro Ueda, Kotaro Kohno, Yoshiki Toba, Satoshi Yamada, Ian Smail, Hideki Umehata, Seiji Fujimoto, Bunyo Hatsukade, Yiping Ao, Franz Erik Bauer, Gabriel Brammer, Miroslava Dessauges-Zavadsky, Daniel Espada, Jean-Baptiste Jolly, Anton M. Koekemoer, Vasily Kokorev, Georgios E. Magdis, Masamune Oguri, Fengwu Sun

The Astrophysical Journal　2024年4月1日

DOI： 10.3847/1538-4357/ad26f7 　
Probing the origin of the two-component structure of broad-line region by reverberation mapping of an extremely variable quasar 査読有り

Shumpei Nagoshi, Fumihide Iwamuro, Satoshi Yamada, Yoshihiro Ueda, Yuto Oikawa, Masaaki Otsuka, Keisuke Isogai, Shin Mineshige

Monthly Notices of the Royal Astronomical Society　2024年2月27日

DOI： 10.1093/mnras/stae319 　
Coevolution and Nuclear Structure in the Dwarf Galaxy POX 52 Studied by Multiwavelength Data from Radio to X-Ray 査読有り

Taiki Kawamuro, Claudio Ricci, Satoshi Yamada, Hirofumi Noda, Ruancun Li, Matthew J. Temple, Alessia Tortosa

The Astrophysical Journal　2024年1月1日

DOI： 10.3847/1538-4357/ad0972 　
BASS. XLII. The Relation between the Covering Factor of Dusty Gas and the Eddington Ratio in Nearby Active Galactic Nuclei 査読有り

C. Ricci, K. Ichikawa, M. Stalevski, T. Kawamuro, S. Yamada, Y. Ueda, R. Mushotzky, G. C. Privon, M. J. Koss, B. Trakhtenbrot, A. C. Fabian, L. C. Ho, D. Asmus, F. E. Bauer, C. S. Chang, K. K. Gupta, K. Oh, M. Powell, R. W. Pfeifle, A. Rojas, F. Ricci, M. J. Temple, Y. Toba, A. Tortosa, E. Treister, F. Harrison, D. Stern, C. M. Urry

The Astrophysical Journal　2023年12月1日

DOI： 10.3847/1538-4357/ad0733 　
AGN number fraction in galaxy groups and clusters atz&lt; 1.4 from the Subaru Hyper Suprime-Cam survey 査読有り

Aoi Hashiguchi, Yoshiki Toba, Naomi Ota, Masamune Oguri, Nobuhiro Okabe, Yoshihiro Ueda, Masatoshi Imanishi, Satoshi Yamada, Tomotsugu Goto, Shuhei Koyama, Kianhong Lee, Ikuyuki Mitsuishi, Tohru Nagao, Atsushi J Nishizawa, Akatoki Noboriguchi, Taira Oogi, Koki Sakuta, Malte Schramm, Mio Shibata, Yuichi Terashima, Takuji Yamashita, Anri Yanagawa, Anje Yoshimoto

Publications of the Astronomical Society of Japan　75　(6)　1246-1261　2023年9月29日
出版者・発行元： Oxford University Press (OUP)
DOI： 10.1093/pasj/psad066 　

ISSN：0004-6264

eISSN：2053-051X

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Abstract One of the key questions on active galactic nuclei (AGN) in galaxy clusters is how AGN could affect the formation and evolution of member galaxies and galaxy clusters in the history of the Universe. To address this issue, we investigate the dependence of AGN number fraction (fAGN) on cluster redshift (zcl) and distance from the cluster center (R$/$R200). We focus on more than 27000 galaxy groups and clusters at 0.1 &lt; zcl &lt; 1.4 with more than 1 million member galaxies selected from the Subaru Hyper Suprime-Cam. By combining various AGN selection methods based on infrared (IR), radio, and X-ray data, we identify 2688 AGN. We find that (i) fAGN increases with zcl and (ii) fAGN decreases with R$/$R200. The main contributors to the rapid increase of fAGN towards high-z and cluster center are IR- and radio-selected AGN, respectively. These results indicate that the emergence of the AGN population depends on the environment and redshift, and galaxy groups and clusters at high z play an important role in AGN evolution. We also find that cluster–cluster mergers may not drive AGN activity in at least the cluster center, while we have tentative evidence that cluster–cluster mergers could enhance AGN activity in the outskirts of (particularly massive) galaxy clusters.
Broad-band X-ray spectral study of nuclear structure in local obscured radio galaxies 査読有り

Yuya Nakatani, Yoshihiro Ueda, Claudio Ricci, Koki Inaba, Shoji Ogawa, Kenta Setoguchi, Ryosuke Uematsu, Satoshi Yamada, Tomohiro Yoshitake

Monthly Notices of the Royal Astronomical Society　2023年6月22日

DOI： 10.1093/mnras/stad1836 　
MAXI/GSC detection of X-ray rebrightening of GRS 1915+105

Yamada, S., Nakajima, M., Negoro, H., Kobayashi, K., Tanaka, M., Soejima, Y., Mihara, T., Kawamuro, T., Tamagawa, T., Matsuoka, M., Sakamoto, T., Serino, M., Sugita, S., Hiramatsu, H., Nishikawa, H., Yoshida, A., Tsuboi, Y., Kohara, J., Urabe, S., Nawa, S., Nemoto, N., Shidatsu, M., Iwasaki, M., Kawai, N., Niwano, M., Hosokawa, R., Imai, Y., Ito, N., Takamatsu, Y., Nakahira, S., Ueno, S., Tomida, H., Ishikawa, M., Kurihara, T., Ueda, Y., Ogawa, S., Setoguchi, K., Yoshitake, T., Inaba, K., Nakatani, Y., Yamauchi, M., Sato, T., Hatsuda, R., Fukuoka, R., Hagiwara, Y., Umeki, Y., Yamaoka, K., Kawakubo, Y., Sugizaki, M., Iwakiri, W.

The Astronomer's Telegram　15968　1-1　2023年3月
ALMA Lensing Cluster Survey: Properties of Millimeter Galaxies Hosting X-Ray-detected Active Galactic Nuclei 査読有り

Ryosuke Uematsu, Yoshihiro Ueda, Kotaro Kohno, Satoshi Yamada, Yoshiki Toba, Seiji Fujimoto, Bunyo Hatsukade, Hideki Umehata, Daniel Espada, Fengwu Sun, Georgios E. Magdis, Vasily Kokorev, Yiping Ao

The Astrophysical Journal　2023年3月1日

DOI： 10.3847/1538-4357/acb4e9 　
X線分光撮像衛星XRISMの科学運用への準備状況

内田悠介, 田代信, 寺田幸功, 高橋弘充, 信川正順, 水野恒史, 宇野伸一郎, 久保田あや, 中澤知洋, 渡辺伸, 飯塚亮, 佐藤理江, 米山友景, 吉田鉄生, 海老沢研, 江口智士, 深澤泰司, 橋口葵, 林克洋, 勝田哲, 北口貴雄, 小高裕和, 大野雅功, 太田直美, 阪間美南, 阪本菜月, 志達めぐみ, 塩入匠, 丹波翼, 谷本敦, 寺島雄一, 坪井陽子, 内田和海, 内山秀樹, 山田智史, 山内茂雄

日本物理学会講演概要集　78.1　666-666　2023年
出版者・発行元：一般社団法人日本物理学会
DOI： 10.11316/jpsgaiyo.78.1.0_666 　

eISSN：2189-0803
Narrow Fe–Kα Reverberation Mapping Unveils the Deactivated Broad-line Region in a Changing-look Active Galactic Nucleus 査読有り

Hirofumi Noda, Taisei Mineta, Takeo Minezaki, Hiroaki Sameshima, Mitsuru Kokubo, Taiki Kawamuro, Satoshi Yamada, Takashi Horiuchi, Hironori Matsumoto, Makoto Watanabe, Kumiko Morihana, Yoichi Itoh, Koji S. Kawabata, Yasushi Fukazawa

The Astrophysical Journal　2023年1月1日

DOI： 10.3847/1538-4357/aca963 　
Optical IFU observations of GOALS sample with KOOLS-IFU on Seimei Telescope: Initial results of nine U/LIRGs at z < 0.04 査読有り

Yoshiki Toba, Satoshi Yamada, Kazuya Matsubayashi, Koki Terao, Aoi Moriya, Yoshihiro Ueda, Kouji Ohta, Aoi Hashiguchi, Kazuharu G Himoto, Hideyuki Izumiura, Kazuma Joh, Nanako Kato, Shuhei Koyama, Hiroyuki Maehara, Rana Misato, Akatoki Noboriguchi, Shoji Ogawa, Naomi Ota, Mio Shibata, Nozomu Tamada, Anri Yanagawa, Naoki Yonekura, Tohru Nagao, Masayuki Akiyama, Masaru Kajisawa, Yoshiki Matsuoka

Publications of the Astronomical Society of Japan　74　(6)　1356-1367　2022年12月1日
出版者・発行元： Oxford University Press ({OUP})
DOI： 10.1093/pasj/psac073 　

ISSN：0004-6264 2053-051X

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<jats:title>Abstract</jats:title> <jats:p>We present ionized gas properties of nine local ultra/luminous infrared galaxies (U/LIRGs) at z &lt; 0.04 through Integral Field Unit (IFU) observations with KOOLS-IFU on the Seimei Telescope. The observed targets are drawn from the Great Observatories All-sky LIRG Survey (GOALS), covering a wide range of merger stages. We successfully detect emission lines such as Hβ, [O iii]λ5007, Hα, [N ii]λλ6549, 6583, and [S ii]λλ6717, 6731 with a spectral resolution of R = 1500–2000, which provides (i) a spatially resolved (∼200–700 pc) moment map of ionized gas and (ii) diagnostics for an active galactic nucleus (AGN) within the central ∼3–11 kpc in diameter for our sample. We find that the [O iii] outflow that is expected to be driven by an AGN tends to be stronger (i) towards the galactic center and (ii) as a sequence of the merger stage. In particular, the outflow strength in the late-stage (stage D) mergers is about 1.5 times stronger than that in the early-state (stage B) mergers, which indicates that galaxy mergers could induce AGN-driven outflow and play an important role in the co-evolution of galaxies and supermassive black holes.</jats:p>
Broadband X-Ray Spectral Analysis of the Dual AGN System Mrk 739 査読有り

Koki Inaba, Yoshihiro Ueda, Satoshi Yamada, Shoji Ogawa, Ryosuke Uematsu, Atsushi Tanimoto, Claudio Ricci

The Astrophysical Journal　2022年11月1日

DOI： 10.3847/1538-4357/ac97ec 　
Xappl: software framework for the XRISM pre-pipeline

Satoshi Eguchi, Makoto Tashiro, Yukikatsu Terada, Hiromitsu Takahashi, Masayoshi Nobukawa, Tsunefumi Mizuno, Shin'ichiro Uno, Aya Kubota, Kazuhiro Nakazawa, Shin Watanabe, Ryo Iizuka, Rie Sato, Tomokage Yoneyama, Chris Baluta, Ken Ebisawa, Yasushi Fukazawa, Katsuhiro Hayashi, So Kato, Satoru Katsuda, Takao Kitaguchi, Hirokazu Odaka, Masanori Ohno, Naomi Ota, Minami Sakama, Ryohei Sato, Megumi Shidatsu, Yasuharu Sugawara, Tsubasa Tamba, Atsushi Tanimoto, Yuichi Terashima, Yohko Tsuboi, Nagomi Uchida, Yuusuke Uchida, Hideki Uchiyama, Shigeo Yamauchi, Masaaki Sakano, Tessei Yoshida, Satoshi Yamada

Space Telescopes and Instrumentation 2022: Ultraviolet to Gamma Ray　266-266　2022年8月31日
出版者・発行元： SPIE
DOI： 10.1117/12.2629316 　
NuSTAR Observations of 52 Compton-thick Active Galactic Nuclei Selected by the Swift/Burst Alert Telescope All-sky Hard X-Ray Survey 査読有り

Atsushi Tanimoto, Yoshihiro Ueda, Hirokazu Odaka, Satoshi Yamada, Claudio Ricci

The Astrophysical Journal Supplement Series　2022年6月1日

DOI： 10.3847/1538-4365/ac5f59 　
A hard X-ray view of luminous and ultra-luminous infrared galaxies in GOALS – I. AGN obscuration along the merger sequence 査読有り

C Ricci, G C Privon, R W Pfeifle, L Armus, K Iwasawa, N Torres-Alb{\`{a } }, S Satyapal, F E Bauer, E Treister, L C Ho, S Aalto, P Ar{\'{e } }valo, L Barcos-Mu{\~{n } }oz, V Charm, aris, T Diaz-Santos, A S Evans, T Gao, H Inami, M J Koss, G Lansbury, S T Linden, A Medling, D B S, ers, Y Song, D Stern, V U, Y Ueda, S Yamada

Monthly Notices of the Royal Astronomical Society　506　(4)　5935-5950　2021年8月13日
出版者・発行元： Oxford University Press ({OUP})
DOI： 10.1093/mnras/stab2052 　

ISSN：0035-8711 1365-2966

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<jats:title>ABSTRACT</jats:title> <jats:p>The merger of two or more galaxies can enhance the inflow of material from galactic scales into the close environments of active galactic nuclei (AGNs), obscuring and feeding the supermassive black hole (SMBH). Both recent simulations and observations of AGN in mergers have confirmed that mergers are related to strong nuclear obscuration. However, it is still unclear how AGN obscuration evolves in the last phases of the merger process. We study a sample of 60 luminous and ultra-luminous IR galaxies (U/LIRGs) from the GOALS sample observed by NuSTAR. We find that the fraction of AGNs that are Compton thick (CT; $N_{\rm H}\ge 10^{24}\rm \, cm^{-2}$) peaks at $74_{-19}^{+14}{ { \ \rm per\ cent } }$ at a late merger stage, prior to coalescence, when the nuclei have projected separations (dsep) of 0.4–6 kpc. A similar peak is also observed in the median NH [$(1.6\pm 0.5)\times 10^{24}\rm \, cm^{-2}$]. The vast majority ($85^{+7}_{-9}{ { \ \rm per\ cent } }$) of the AGNs in the final merger stages (dsep ≲ 10 kpc) are heavily obscured ($N_{\rm H}\ge 10^{23}\rm \, cm^{-2}$), and the median NH of the accreting SMBHs in our sample is systematically higher than that of local hard X-ray-selected AGN, regardless of the merger stage. This implies that these objects have very obscured nuclear environments, with the $N_{\rm H}\ge 10^{23}\rm \, cm^{-2}$ gas almost completely covering the AGN in late mergers. CT AGNs tend to have systematically higher absorption-corrected X-ray luminosities than less obscured sources. This could either be due to an evolutionary effect, with more obscured sources accreting more rapidly because they have more gas available in their surroundings, or to a selection bias. The latter scenario would imply that we are still missing a large fraction of heavily obscured, lower luminosity ($L_{2-10}\lesssim 10^{43}\rm \, erg\, s^{-1}$) AGNs in U/LIRGs.</jats:p>
X-Ray Constraint on the Location of the AGN Torus in the Circinus Galaxy 査読有り

Ryosuke Uematsu, Yoshihiro Ueda, Atsushi Tanimoto, Taiki Kawamuro, Kenta Setoguchi, Shoji Ogawa, Satoshi Yamada, Hirokazu Odaka

The Astrophysical Journal　913　(1)　17-17　2021年5月1日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/abf0a2 　
GRB 210110A: MAXI/GSC detection

Yamada, S., Negoro, H., Serino, M., Nakajima, M., Aoki, M., Kobayashi, K., Takagi, R., Asakura, Seino, Mihara, T., Tamagawa, T., Matsuoka, M., Sakamoto, T., Sugita, S., Nishida, H., Komachi, K., Yoshida, A., Tsuboi, Y., Iwakiri, W., Sasaki, R., Kawai, H., Okamoto, Y., Kitakoga, S., Shidatsu, M., Kawai, N., Adachi, R., Niwano, M., Hosokawa, R., Nakahira, S., Sugawara, Y., Ueno, S., Tomida, H., Ishikawa, M., Tominaga, M., Nagatsuka, T., Ueda, Y., Ogawa, S., Setoguchi, K., Yoshitake, T., Goto, U., Uematsu, R., Tsunemi, H., Yamauchi, M., Kurogi, K., Miike, K., Kawamuro, T., Yamaoka, K., Kawakubo, Y., Sugizaki, M., MAXI Team

GRB Coordinates Network　29284　1-1　2021年1月
Systematic Study of AGN Clumpy Tori with Broadband X-Ray Spectroscopy: Updated Unified Picture of AGN Structure 査読有り

Shoji Ogawa, Yoshihiro Ueda, Atsushi Tanimoto, Satoshi Yamada

The Astrophysical Journal　2021年1月1日

DOI： 10.3847/1538-4357/abccce 　
Application of an X-Ray Clumpy Torus Model (XCLUMPY) to 10 Obscured Active Galactic Nuclei Observed with Suzaku and NuSTAR 査読有り

Atsushi Tanimoto, Yoshihiro Ueda, Hirokazu Odaka, Shoji Ogawa, Satoshi Yamada, Toshihiro Kawaguchi, Kohei Ichikawa

The Astrophysical Journal　2020年7月1日

DOI： 10.3847/1538-4357/ab96bc 　
NuSTAR Discovery of a Compton-thick, Dust-obscured Galaxy: WISE J0825+3002 査読有り

Yoshiki Toba, Satoshi Yamada, Yoshihiro Ueda, Claudio Ricci, Yuichi Terashima, Tohru Nagao, Wei-Hao Wang, Atsushi Tanimoto, Taiki Kawamuro

The Astrophysical Journal　888　(1)　8-8　2019年12月27日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ab5718 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract We report the discovery of a Compton-thick (CT), dust-obscured galaxy at z = 0.89, WISE J082501.48+300257.2 (WISE 0825+3002), observed by the Nuclear Spectroscopic Telescope Array. X-ray analysis with the XCLUMPY model revealed that hard X-ray luminosity in the rest-frame 2–10 keV band of WISE 0825+3002 is L_X (2–10 keV) = ${4.2}_{-1.6}^{+2.8}\times {10}^{44}$ erg s⁻¹ while its hydrogen column density is N_H = ${1.0}_{-0.4}^{+0.8}\times {10}^{24}$ cm⁻², indicating that WISE 0825+3002 is a mildly CT active galactic nucleus (AGN). We performed spectral energy distribution (SED) fitting with CIGALE to derive its stellar mass, star formation rate, and infrared luminosity. The estimated Eddington ratio based on stellar mass and integration of the best-fit SED of the AGN component is λ_Edd = 0.70, which suggests that WISE 0825+3002 harbors an actively growing black hole behind a large amount of gas and dust. We found that the relationship between the luminosity ratio of X-ray and 6 μm, and Eddington ratio, follows an empirical relation for AGNs reported by Toba et al.
Application of Clumpy Torus Model to Broadband X-Ray Spectra of Two Seyfert 1 Galaxies: IC 4329A and NGC 7469 査読有り

Shoji Ogawa, Yoshihiro Ueda, Satoshi Yamada, Atsushi Tanimoto, Toshihiro Kawaguchi

The Astrophysical Journal　875　(2)　115-115　2019年4月20日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/ab0e08 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract We apply a new X-ray clumpy torus model, XCLUMPY, in which the clump distribution is assumed to be the same as that in the infrared clumpy torus model (CLUMPY) by Nenkova et al., to the broadband X-ray spectra of type-1 active galactic nuclei (AGNs) for the first time. We analyze the archival data of IC 4329A and NGC 7469 observed with NuSTAR/Suzaku and NuSTAR/XMM-Newton, respectively, whose infrared spectra were studied with CLUMPY by Ichikawa et al. and optical extinctions (A_V) of the tori were estimated. We consider two models, invoking (Model 1) a relativistic reflection component from the accretion disk and (Model 2) a partial absorber. Assuming that the narrow Fe Kα emission line at 6.4 keV originates from the torus, we separate the contribution of the torus reflection components in the total spectra. Our models yield equatorial hydrogen column densities of the tori to be ${N}_{ { \rm{H } } }^{\mathrm{Equ } }\,=$ (0.53–1.43) × 10²³ cm⁻² and ${N}_{ { \rm{H } } }^{\mathrm{Equ } }\,=$ (0.84–1.43) × 10²⁴ cm⁻², for IC 4329A and NGC 7469, respectively. We find that the N_H/A_V ratios in the tori are by factors of 25–68 (IC 4329A) and 2.4–3.9 (NGC 7469) smaller than that in the Galactic interstellar medium (ISM). These results suggest that a non-negligible fraction of AGNs are “dust-rich” compared with the Galactic ISM, as opposite to the general trend previously reported in many obscured AGNs.
GRB 140404C: MAXI/GSC detection.

Yamada, S., Negoro, H., Nakajima, M., Iwakiri, W., Maruyama, W., Aoki, M., Kobayashi, K., Mihara, T., Nakahira, S., Matsuoka, M., Sakamoto, T., Serino, M., Sugita, S., Hashimoto, T., Yoshida, A., Tsuboi, Y., Sasaki, R., Kawai, H., Sato, T., Kawai, N., Sugizaki, M., Tachibana, Y., Morita, K., Oeda, M., Shiraishi, K., Ueno, S., Tomida, H., Ishikawa, M., Sugawara, Y., Isobe, N., Shimomukai, R., Tominaga, M., Ueda, Y., Tanimoto, A., Morita, T., Ogawa, S., Tsunemi, H., Yoneyama, T., Asakura, K., Ide, S., Yamauchi, M., Iwahori, S., Kurihara, Y., Kawamuro, T., Yamaoka, K., Shidatsu, M., Kawakubo, Y.

GRB Coordinates Network　24049　1-1　2019年1月
X-Ray, Optical, and Near-infrared Monitoring of the New X-Ray Transient MAXI J1820+070 in the Low/Hard State 査読有り

Megumi Shidatsu, Satoshi Nakahira, Satoshi Yamada, Taiki Kawamuro, Yoshihiro Ueda, Hitoshi Negoro, Katsuhiro L. Murata, Ryosuke Itoh, Yutaro Tachibana, Ryo Adachi, Yoichi Yatsu, Nobuyuki Kawai, Hidekazu Hanayama, Takashi Horiuchi, Hiroshi Akitaya, Tomoki Saito, Masaki Takayama, Tomohito Ohshima, Noriyuki Katoh, Jun Takahashi, Takahiro Nagayama, Masayuki Yamanaka, Miho Kawabata, Tatsuya Nakaoka, Seiko Takagi, Tomoki Morokuma, Kumiko Morihana, Hiroyuki Maehara, Kazuhiro Sekiguchi

The Astrophysical Journal　868　(1)　54-54　2018年11月20日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4357/aae929 　

ISSN：0004-637X

eISSN：1538-4357

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Abstract We report X-ray, optical, and near-infrared monitoring of the new X-ray transient MAXI J1820+070 discovered with MAXI on 2018 March 11. Its X-ray intensity reached ∼2 crab at 2–20 keV at the end of March, and then gradually decreased until the middle of June. In this period, the X-ray spectrum was described by Comptonization of the disk emission, with a photon index of ∼1.5 and an electron temperature of ∼50 keV, which is consistent with a black hole X-ray binary in the low/hard state. The electron temperature was slightly decreased, and the photon index increased, with increasing flux. The source showed significant X-ray flux variation on a timescale of seconds. This short-term variation was found to be associated with changes in the spectral shape, and the photon index became slightly harder at higher fluxes. This suggests that the variation was produced by a change in the properties of the hot electron cloud responsible for the strong Comptonization. Modeling a multi-wavelength spectral energy distribution around the X-ray flux peak at the end of March, covering the near-infrared to X-ray bands, we found that the optical and near-infrared fluxes were likely contributed substantially by the jet emission. Before this outburst, the source was never detected in the X-ray band with MAXI (with a 3σ upper limit of ∼0.2 mcrab at 4–10 keV, obtained from seven years of data from 2009 to 2016), whereas weak optical and infrared activity was found at flux levels ∼3 orders of magnitude lower than the peak fluxes in the outburst.
The 7-year MAXI/GSC X-Ray Source Catalog in the High Galactic Latitude Sky (3MAXI) 査読有り

T. Kawamuro, Y. Ueda, M. Shidatsu, T. Hori, M. Morii, S. Nakahira, N. Isobe, N. Kawai, T. Mihara, M. Matsuoka, T. Morita, M. Nakajima, H. Negoro, S. Oda, T. Sakamoto, M. Serino, M. Sugizaki, A. Tanimoto, H. Tomida, Y. Tsuboi, H. Tsunemi, S. Ueno, K. Yamaoka, S. Yamada, A. Yoshida, W. Iwakiri, Y. Kawakubo, Y. Sugawara, S. Sugita, Y. Tachibana, T. Yoshii

The Astrophysical Journal Supplement Series　238　(2)　32-32　2018年10月15日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4365/aad1ef 　

eISSN：1538-4365
The 7-year MAXI /GSC Source Catalog of the Low-Galactic-latitude Sky (3MAXI) 査読有り

T. Hori, M. Shidatsu, Y. Ueda, T. Kawamuro, M. Morii, S. Nakahira, N. Isobe, N. Kawai, T. Mihara, M. Matsuoka, T. Morita, M. Nakajima, H. Negoro, S. Oda, T. Sakamoto, M. Serino, M. Sugizaki, A. Tanimoto, H. Tomida, Y. Tsuboi, H. Tsunemi, S. Ueno, K. Yamaoka, S. Yamada, A. Yoshida, W. Iwakiri, Y. Kawakubo, Y. Sugawara, S. Sugita, Y. Tachibana, T. Yoshii

The Astrophysical Journal Supplement Series　235　(1)　7-7　2018年2月26日
出版者・発行元： American Astronomical Society
DOI： 10.3847/1538-4365/aaa89c 　

eISSN：1538-4365
GRB 180829A/MAXI J0406-019: MAXI/GSC detection.

Yamada, S., Negoro, H., Serino, M., Nakajima, M., Sakamaki, A., Maruyama, W., Mihara, T., Nakahira, S., Yatabe, F., Takao, Y., Matsuoka, M., Sakamoto, T., Sugita, S., Kawakubo, Y., Hashimoto, T., Yoshida, A., Kawai, N., Sugizaki, M., Tachibana, Y., Morita, K., Ueno, S., Tomida, H., Ishikawa, M., Sugawara, Y., Isobe, N., Shimomukai, R., Ueda, Y., Tanimoto, A., Morita, T., Tsuboi, Y., Iwakiri, W., Sasaki, R., Kawai, H., Sato, T., Tsunemi, H., Yoneyama, T., Asakura, K., Ide, S., Yamauchi, M., Hidaka, K., Iwahori, S., Kawamuro, T., Yamaoka, K., Shidatsu, M.

GRB Coordinates Network　23186　1-1　2018年1月
Multi-messenger Observations of a Binary Neutron Star Merger^* 査読有り

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Conceição, G. Consolati, F. Contreras, M. J. Cooper, S. Coutu, C. E. Covault, J. Cronin, S. D’Amico, B. Daniel, S. Dasso, K. Daumiller, B. R. Dawson, J. A. Day, R. M. de Almeida, S. J. de Jong, G. De Mauro, J. R. T. de Mello Neto, I. De Mitri, J. de Oliveira, V. de Souza, J. Debatin, O. Deligny, M. L. Díaz Castro, F. Diogo, C. Dobrigkeit, J. C. D’Olivo, Q. Dorosti, R. C. Dos Anjos, M. T. Dova, A. Dundovic, J. Ebr, R. Engel, M. Erdmann, M. Erfani, C. O. Escobar, J. Espadanal, A. Etchegoyen, H. Falcke, J. Farmer, G. Farrar, A. C. Fauth, N. Fazzini, F. Feldbusch, F. Fenu, B. Fick, J. M. Figueira, A. Filipčič, M. M. Freire, T. Fujii, A. Fuster, R. Gaïor, B. García, F. Gaté, H. Gemmeke, A. Gherghel-Lascu, P. L. Ghia, U. Giaccari, M. Giammarchi, M. Giller, D. Głas, C. Glaser, G. Golup, M. Gómez Berisso, P. F. Gómez Vitale, N. González, A. Gorgi, M. Gottowik, A. F. Grillo, T. D. Grubb, F. Guarino, G. P. Guedes, R. Halliday, M. R. Hampel, P. Hansen, D. Harari, T. A. Harrison, V. M. Harvey, A. Haungs, T. Hebbeker, D. Heck, P. Heimann, A. E. Herve, G. C. Hill, C. Hojvat, E. Holt, P. Homola, J. R. Hörandel, P. Horvath, M. Hrabovský, T. Huege, J. Hulsman, A. Insolia, P. G. Isar, I. Jandt, J. A. Johnsen, M. Josebachuili, J. Jurysek, A. Kääpä, K. H. Kampert, B. Keilhauer, N. Kemmerich, J. Kemp, R. M. Kieckhafer, H. O. Klages, M. Kleifges, J. Kleinfeller, R. Krause, N. Krohm, D. Kuempel, G. Kukec Mezek, N. Kunka, A. Kuotb Awad, B. L. Lago, D. LaHurd, R. G. Lang, M. Lauscher, R. Legumina, M. A. Leigui de Oliveira, A. Letessier-Selvon, I. Lhenry-Yvon, K. Link, D. Lo Presti, L. Lopes, R. López, A. López Casado, R. Lorek, Q. Luce, A. Lucero, M. Malacari, M. Mallamaci, D. Mandat, P. Mantsch, A. G. Mariazzi, I. C. Maris, G. Marsella, D. Martello, H. Martinez, O. Martínez Bravo, J. J. Masías Meza, H. J. Mathes, S. Mathys, J. Matthews, G. Matthiae, E. Mayotte, P. O. Mazur, C. Medina, G. Medina-Tanco, D. Melo, A. Menshikov, K.-D. Merenda, S. Michal, M. I. Micheletti, L. Middendorf, L. Miramonti, B. Mitrica, D. Mockler, S. Mollerach, F. Montanet, C. Morello, G. Morlino, A. L. Müller, G. Müller, M. A. Muller, S. Müller, R. Mussa, I. Naranjo, P. H. Nguyen, M. Niculescu-Oglinzanu, M. Niechciol, L. Niemietz, T. Niggemann, D. Nitz, D. Nosek, V. Novotny, L. Nožka, L. A. Núñez, F. Oikonomou, A. Olinto, M. Palatka, J. Pallotta, P. Papenbreer, G. Parente, A. Parra, T. Paul, M. Pech, F. Pedreira, J. Pȩkala, J. Peña-Rodriguez, L. A. S. Pereira, M. Perlin, L. Perrone, C. Peters, S. Petrera, J. Phuntsok, T. Pierog, M. Pimenta, V. Pirronello, M. Platino, M. Plum, J. Poh, C. Porowski, R. R. Prado, P. Privitera, M. Prouza, E. J. Quel, S. Querchfeld, S. Quinn, R. Ramos-Pollan, J. Rautenberg, D. Ravignani, J. Ridky, F. Riehn, M. Risse, P. Ristori, V. Rizi, W. Rodrigues de Carvalho, G. Rodriguez Fernandez, J. Rodriguez Rojo, M. J. Roncoroni, M. Roth, E. Roulet, A. C. Rovero, P. Ruehl, S. J. Saffi, A. Saftoiu, F. Salamida, H. Salazar, A. Saleh, G. Salina, F. Sánchez, P. Sanchez-Lucas, E. M. Santos, E. Santos, F. Sarazin, R. Sarmento, C. Sarmiento-Cano, R. Sato, M. Schauer, V. Scherini, H. Schieler, M. Schimp, D. Schmidt, O. Scholten, P. Schovánek, F. G. Schröder, S. Schröder, A. Schulz, J. Schumacher, S. J. Sciutto, A. Segreto, A. Shadkam, R. C. Shellard, G. Sigl, G. Silli, R. Šmída, G. R. Snow, P. Sommers, S. Sonntag, J. F. Soriano, R. Squartini, D. Stanca, S. Stanič, J. Stasielak, P. Stassi, M. Stolpovskiy, F. Strafella, A. Streich, F. Suarez, M. Suarez-Durán, T. Sudholz, T. Suomijärvi, A. D. Supanitsky, J. Šupík, J. Swain, Z. Szadkowski, A. Taboada, O. A. Taborda, C. Timmermans, C. J. Todero Peixoto, L. Tomankova, B. Tomé, G. Torralba Elipe, P. Travnicek, M. Trini, M. Tueros, R. Ulrich, M. Unger, M. Urban, J. F. Valdés Galicia, I. Valiño, L. Valore, G. van Aar, P. van Bodegom, A. M. van den Berg, A. van Vliet, E. Varela, B. Vargas Cárdenas, R. A. Vázquez, D. Veberič, C. Ventura, I. D. Vergara Quispe, V. Verzi, J. Vicha, L. Villaseñor, S. Vorobiov, H. Wahlberg, O. Wainberg, D. Walz, A. A. Watson, M. Weber, A. Weindl, M. Wiedeński, L. Wiencke, H. Wilczyński, M. Wirtz, D. Wittkowski, B. Wundheiler, L. Yang, A. Yushkov, E. Zas, D. Zavrtanik, M. Zavrtanik, A. Zepeda, B. Zimmermann, M. Ziolkowski, Z. Zong, F. Zuccarello, S. Kim, S. Schulze, F. E. Bauer, J. M. Corral-Santana, I. de Gregorio-Monsalvo, J. González-López, D. H. Hartmann, C. H. Ishwara-Chandra, S. Martín, A. Mehner, K. Misra, M. J. Michałowski, L. Resmi, Z. Paragi, I. Agudo, T. An, R. Beswick, C. Casadio, S. Frey, P. Jonker, M. Kettenis, B. Marcote, J. Moldon, A. Szomoru, H. J. van Langevelde, J. Yang, A. Cwiek, M. Cwiok, H. Czyrkowski, R. Dabrowski, G. Kasprowicz, L. Mankiewicz, K. Nawrocki, R. Opiela, L. W. Piotrowski, G. Wrochna, M. Zaremba, A. F. Żarnecki, D. Haggard, M. Nynka, J. J. Ruan, P. A. Bland, T. Booler, H. A. R. Devillepoix, J. S. de Gois, P. J. Hancock, R. M. Howie, J. Paxman, E. K. Sansom, M. C. Towner, J. Tonry, M. Coughlin, C. W. Stubbs, L. Denneau, A. Heinze, B. Stalder, H. Weiland, R. P. Eatough, M. Kramer, A. Kraus, E. Troja, L. Piro, J. Becerra González, N. R. Butler, O. D. Fox, H. G. Khandrika, A. Kutyrev, W. H. Lee, R. Ricci, R. E. Ryan Jr., R. Sánchez-Ramírez, S. Veilleux, A. M. Watson, M. H. Wieringa, J. M. Burgess, H. van Eerten, C. J. Fontes, C. L. Fryer, O. Korobkin, R. T. Wollaeger, F. Camilo, A. R. Foley, S. Goedhart, S. Makhathini, N. Oozeer, O. M. Smirnov, R. P. Fender, P. A. Woudt

The Astrophysical Journal Letters　848　(2)　L12-L12　2017年10月16日
出版者・発行元： American Astronomical Society
DOI： 10.3847/2041-8213/aa91c9 　

ISSN：2041-8205

eISSN：2041-8213

詳細を見る詳細を閉じる

Abstract On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s } }$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg² at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc } }$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.

︎全件表示 ︎最初の5件までを表示

MISC 4

せいめい望遠鏡KOOLS-IFU可視面分光観測で探るNGC7674のAGN活動

鳥羽儀樹, 鳥羽儀樹, 守屋碧, 太田直美, 山田智史, 城知磨, 松林和也, 橋口葵, 柴田実桜, 美里らな, 上田佳宏

日本天文学会年会講演予稿集　2021　2021年

ISSN： 1347-0639
X線分光撮像衛星XRISMの科学運用における地上高次データ処理の開発

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ISSN： 2433-2216
ALMA Lensing Cluster Survey:暗いサブミリ波銀河中における埋もれたAGNの評価

植松亮祐, 上田佳宏, 河野孝太郎, 鳥羽儀樹, 山田智史, 梅畑豪紀, 藤本征史, 廿日出文洋

日本天文学会年会講演予稿集　2024　2024年

ISSN： 1347-0639
ALMAレンズ群サーベイ:ミリ波観測で検出された遠方銀河の完全なSED解析

植松亮祐, 上田佳宏, 河野孝太郎, 鳥羽儀樹, 山田智史, 藤本征史, 廿日出文洋, 梅畑豪紀

日本天文学会年会講演予稿集　2022　2022年

ISSN： 1347-0639

書籍等出版物 4

量子× AI で宇宙の突発的な異常エネルギー解放現象を検出

川室太希、山田真也、山田智史、長瀧重博、松浦俊司、酒井優輔

Isotope News 2026年6月号 No.806 (公益社団法人日本アイソトープ協会)：https://www.jrias.or.jp/books/cat3/list.html　2026年6月
多波長観測で探る合体銀河中の銀河ーブラックホール共進化機構

山田智史

天文月報 116(1) 5-14 2023年1月
XRISM Science Book (Section 3.2.2)

Satoshi Yamada

2027年
PRIMA Investigation of Obscured Active Galactic Nuclei in Star-Forming Galaxies at Cosmic Noon

Y. Ueda, S. Yamada, Y. Toba, T. Nagao, (PRIMA General Observer Science Book Volume 2, pp.252-257)

2025年12月

講演・口頭発表等 82

From Ultrafast Outflows to Cluster-scale Feedback: Insights from XRISM 国際会議

Satoshi Yamada

Cospar 2026 (Italy)　2026年8月
Direct Measurement of Quasar-mode Feedback on Cluster Scales 国際会議

Satoshi Yamada

The X-ray Universe 2026 (Spain)　2026年6月
Huge impact of quasar-mode feedback from accretion disk to cluster-core scales 国際会議

Satoshi Yamada

Breaking the limits 2026-Super Eddington Accretion onto Compact Objects (Italy)　2026年6月
Latest Astronomical Results: Coevolution of Black Holes and Us 国際会議

Satoshi Yamada

FRIS-KKU Joint Symposium 2025 (Korea)　2025年7月
Accretion and Multi-scale Ejection Resolved by X-ray Observations from 1999 to 2025 国際会議

Satoshi Yamada

Vasto Accretion Meeting 2025 (Italy)　2025年6月
X-ray Winds In Nearby-to-distant Galaxies (X-WING). I: Legacy Surveys of Galaxies with Warm Absorbers and Ultrafast Outflows in z ~ 0-4

Satoshi Yamada

AGN Feedback and Star Formation Across Cosmic Scales and Time (Italy)　2024年9月
Multiwavelength View of AGN Feedback from Accretion Disk to Cluster Scales 招待有り

Satoshi Yamada

Kyoto Torus Workshop 2026 (Kyoto)　2026年5月
Variability of complex Fe lines (XRISM AO1-3)

山田智史

第4回XRISM衛星 AGNワークショップ　2026年1月
XRISM衛星による銀河団スケールのQuasar-mode Feedbackの直接観測

山田智史

高エネルギー宇宙物理学研究会2025　2025年12月
クールコア銀河団のXRISM観測によるQuasar-mode Feedbackで駆動された激しい乱流の発見

山田智史

ALMA Workshop 2025: Addressing the cooling flow problem with ALMA: cooling, cooled, and/or cold gas in the centers of galaxy clusters?　2025年11月
Direct measurement of quasar feedback beyond galactic scales 国際会議

Satoshi Yamada

XRISM International Conference 2025　2025年10月
X線天文学の立場から微細構造輝線観測への期待招待有り

山田智史

銀河微細構造輝線勉強会2025　2025年8月
Exploring the obscured AGNs in the Cosmic Noon with PRIMA 国際会議

Satoshi Yamada

PRIMA-J Science Workshop 2025　2025年7月
Accretion and Multi-scale Ejection Resolved by X-ray Observations from 1999 to 2025 招待有り

Satoshi Yamada

Astro Colloquium　2025年4月
XRISM First Results: From BH to Galaxy Cluster 国際会議

Satoshi Yamada

Revealing the Nature of Supermassive Black Hole Coronae with Synergy of XRISM and ALMA　2025年3月
XRISM AO1: H1821+643の観測成果

山田智史

第3回XRISM衛星 AGNワークショップ　2025年2月
XRISMの初期成果: 巨大ブラックホール近傍から銀河団まで招待有り

山田智史

大阪大学X線セミナー　2025年1月
Role of Mergers in Evolution of Galaxies and Supermassive Black Holes Revealed with Ultrahigh-spatial-resolution Infrared and Multiwavelength Observations

Satoshi Yamada

SPDR FY2024　2025年1月
Latest observational results of bright AGNs

Satoshi Yamada

The History and Future of X-ray Astronomy　2024年12月
XRISM AO1: H1821+643の観測結果

山田智史

第2回XRISM衛星 AGNワークショップ　2024年10月
X線で観た合体銀河中の巨大ブラックホール進化招待有り

山田智史

The Violent Universe　2024年9月
X-WING Project:1999年から現在までに検出された z=0-4の全X線アウトフローとXRISMが開拓するAGN Feedbackの研究

山田智史

日本天文学会2023年秋季年会　2024年9月
[O IV] and [Ne V]-weak AGNs Hidden by Compton-thick Material in Late Mergers

Satoshi Yamada

AGN across the sky: new windows opened by HSC and other wide-field surveys　2024年8月
X-ray Winds In Nearby-to-distant Galaxies (X-WING) - I: Legacy Surveys of Galaxies with Warm Absorbers and Ultrafast Outflows in z ~ 0-4

Satoshi Yamada

10th GALAXLY EVOLUTION WORKSHOP (Taiwan)　2024年8月
X-ray Winds In Nearby-to-distant Galaxies (X-WING) Project

山田智史

最先端の観測装置と理論の両輪で探る降着現象の物理　2024年5月
XRISM衛星で観る宇宙形成の姿

山田智史

学変(A):申請へ向けて「宇宙線学」の共創:宇宙線でつなぐ天体と生命の共進化の多角的探究　2024年5月
[O IV] and [Ne v]-weak AGNs Hidden by Compton-thick Material in Late Mergers

山田智史

日本天文学会2024年春季年会　2024年3月
X-ray Winds in Nearby-to-distant Galaxies (X-WING) – I: Legacy Surveys of Galaxies with Warm Absorbers and UFOs in z~ 0-4

Satoshi Yamada

The 2nd XRISM Community Workshop (USA)　2024年1月
X-ray Weak AGNs Hosting Rapidly Growing Black Holes and Massive Outflows in Late-stage Mergers

Satoshi Yamada

East-Asia AGN Workshop 2023　2023年9月
多波長放射を用いたU/LIRGが持つAGNの探査法

山田智史

日本天文学会2023年秋季年会　2023年9月
AGN Outflow の多スケール構造とFeedback

山田智史

微細構造線研究会2023　2023年9月
合体末期の銀河が持つ[O IV]/[Ne V]-weak AGNの構造

山田智史

基盤Aミニワークショップ　2023年8月
合体銀河中で急成長する塵に埋もれた巨大ブラックホール

山田智史

山田研究会「宇宙における降着現象〜活動性・多様性の源〜」　2023年6月
ポーラーダストを考慮した多波長データ解析で探る合体銀河中の共進化過程

山田智史

日本天文学会2023年春季年会　2023年3月
X線分光撮像衛星XRISMの観測データ処理ツールの開発状況

山田智史

日本天文学会2023年春季年会　2023年3月
JEDI Strategy: Obscured AGNs and dual AGNs

山田智史

AGN/コンパクト（広帯域）SG ミーティング　2023年3月
JEDI Deep Survey of high-z AGNs

山田智史

AGN/コンパクト（広帯域）SG ミーティング　2023年3月
Hard X-ray to Radio Multiwavelength SED Analysis of Local U/LIRGs with Self-consistent AGN Model Including Polar-dust Component

Satoshi Yamada

The 9th Galaxy Evolution Workshop　2023年2月
Latest Picture of Torus and Polar Dust in Merging Galaxies Revealed by Hard X-ray to Radio Multiwavelength Analysis

Satoshi Yamada

Torus 2022 Workshop Smoke and Mirrors (Netherlands)　2022年12月
Hard X-Ray to Radio Multiwavelength SED Analysis of Local U/LIRGs in GOALS Sample with Self-consistent AGN Model Including Polar-dust Component

Satoshi Yamada

Tracing the SMBH growth: outlook beyond the HSC-SSP, and future collaborations　2022年11月
Comprehensive Multiwavelength Studies of Local U/LIRGs observed with NuSTAR and/or Swift/BAT

Satoshi Yamada

What drives the growth of black holes: a decade of reflection (Iceland)　2022年9月
多波長観測による超/高光度赤外線銀河が持つX 線で暗い活動銀河核の調査

山田智史

日本天文学会2022年秋季年会　2022年9月
Multiwavelength Study of Galaxy and Supermassive Black Hole Growth in Galaxy Mergers 招待有り

Satoshi Yamada

RIKEN Monthly Seminar　2022年8月
ポーラーダスト成分を含めたAGNモデルによる超/高光度赤外線銀河の多波長SED解析

山田智史

AGNミニワークショップ　2022年8月
Multiwavelength Study of Galaxy-Supermassive Black Hole Coevolution in Galaxy Mergers 招待有り

Satoshi Yamada

ISAS Astrophysics Colloquia　2022年7月
多波長SED解析で解明する合体銀河中の活動銀河核とポーラーダストの構造

山田智史

日本天文学会2022年春季年会　2022年3月
Comprehensive Broadband X-ray and Multiwavelength Study of AGNs in 57 Local U/LIRGs Observed with NuSTAR and/or Swift/BAT

Satoshi Yamada

Galaxy Evolution Workshop 2021　2022年2月
硬 X 線による近傍 U/LIRG 中の埋もれた AGN の観測招待有り

山田智史

第 5 回 FORCE 研究会　2021年12月
Comprehensive Broadband X-ray and Multiwavelength Study of AGNs in 57 Local U/LIRGs Observed with NuSTAR and/or Swift/BAT

Satoshi Yamada

East-Asia AGN Workshop 2021　2021年10月
巨大ブラックホール連星候補を持つ合体銀河NGC 7674の可視面分光観測

山田智史

2021年度せいめいユーザーズミーティング　2021年8月
硬X線と多波長観測で探る合体銀河中の超巨大ブラックホールの進化

山田智史

多重AGNサイエンスワークショップ　2021年7月
多波長観測で探る合体銀河での星形成と超巨大ブラックホールの成長

山田智史

様々なスケールの衝突流による誘発的星形成〜大質量星から超大質量星団まで〜　2021年7月
硬X線観測で探る超/高光度赤外線銀河中のAGNの構造と降着機構の進化

山田智史

日本天文学会2021年春季年会　2021年3月
Structure of AGN Tori in Ultra-/luminous Infrared Galaxies Unveiled by Mid-infrared and X-ray Spectroscopy

Satoshi Yamada

Galaxy Evolution Workshop 2020　2021年2月
Torus Properties and Supermassive Black Hole Growth in Ultra-/luminous Infrared Galaxies Revealed by X-ray and Mid-infrared Spectroscopy

Satoshi Yamada

Supermassive Black Holes, online conference　2020年12月
中間赤外線とX線で探る超/高光度赤外線銀河が持つトーラス構造と巨大ブラックホールの進化招待有り

山田智史

RCSCE 129-th Seminar　2020年9月
Nature of Obscured AGNs in Ultra-/luminous Infrared Galaxies

Satoshi Yamada

Kyoto Black Hole Accretion Workshop 2020 ~ Link between Theories and Observations ~　2020年3月
超/高光度赤外線銀河が持つ活動銀河核の広帯域X線スペクトル解析

山田智史

日本天文学会2020年春季年会　2020年3月
Nature of Compton-thick AGNs in “Non-merging” Luminous Infrared Galaxies UGC 2608 and NGC 5135 Revealed with Broadband X-ray Spectroscopy

Satoshi Yamada

HSC-AGN face-to-face meeting 2020　2020年1月
Revealing Torus Structure in Ultra/luminous Infrared Galaxies with Mid-infrared and Hard X-ray Observations

山田智史

理論天文学ミニワークショップ 2019　2019年12月
Revealing Torus Properties of Ultra-/luminous Infrared Galaxies with NuSTAR Observations

Satoshi Yamada

The 2nd Keihan Black Hole Workshop　2019年11月
Revealing the Compton-thick Active Galactic Nuclei in the Two “Non-merging” Luminous Infrared Galaxies with Broadband X-ray Observations (NGC 5135 and UGC 2608)

Satoshi Yamada

X-ray Astronomy 2019 (Italy)　2019年9月
Exploring “Buried” Active Galactic Nuclei in Merging Galaxies with Subarcsecond Mid-infrared Observations

Satoshi Yamada

Mid-infrared Astronomy, --Past 20 years and Future 20 years　2019年8月
[O IV] 25.89 μm と nuclear 12 μm の光度比を用いた合体銀河中のAGNトーラス構造の解明

山田智史

サマースクール “コンパクト天体基礎講座”　2019年8月
中間赤外線とX線観測による合体銀河中のAGNトーラス構造の解明招待有り

山田智史

AGN seminar, ISAS/JAXA　2019年7月
[O IV] 25.89 μm と nuclear 12 μm の光度比を用いた “塵に埋もれた” 活動銀河核の診断法

山田智史

2019年度天文・天体物理若手夏の学校　2019年7月
Structure of AGN Tori in Merging Galaxies Revealed by Mid-infrared and X-ray Observations

Satoshi Yamada

Galaxy Evolution Workshop 2019　2019年6月
合体の兆候のない高光度赤外線銀河が持つ活動銀河核のトーラス構造

山田智史

第1回京大・阪大ブラックホール勉強会　2019年6月
中間赤外線とX線観測による合体銀河中のAGNトーラス構造の解明

山田智史

「超巨大ブラックホール研究推進連絡会」第6回ワークショップ　2019年5月
[O IV] 25.89 μm と nuclear 12 μm の光度比を用いた “塵に埋もれた” 活動銀河核の診断法

山田智史

日本天文学会2019年春季年会　2019年3月
X線と中間赤外線による合体銀河の隠された活動銀河核の研究

山田智史

高感度・広帯域X線観測で探るブラックホール降着現象の物理　2019年3月
Buried AGN Fraction in U/LIRGs Revealed by Luminous Ratio between [O IV] 25.89 μm and Nuclear 12 μm Continuum

Satoshi Yamada

East-Asia AGN Workshop 2019 (Taiwan)　2019年1月
Rapidly Growing Supermassive Black Hole in the Merging Galaxy Mrk 463

Satoshi Yamada

HSC-AGN face-to-face meeting 2018　2018年11月
Torus Properties of “Non-merging” Luminous Infrared Galaxy NGC 5135

Satoshi Yamada

IAU Symposium 341　2018年11月
高光度赤外線銀河 NGC 5135 が持つ隠された活動銀河核の広帯域X線観測

山田智史

2018年度天文・天体物理若手夏の学校　2018年7月
2つの核を持つ高光度赤外線銀河 Mrk 463 の広帯域X線スペクトル解析

山田智史

2018年度天文・天体物理若手夏の学校　2018年7月
高光度赤外線銀河が持つ隠された活動銀河核の広帯域X線観測

山田智史

AGN トーラスミニ研究会　2018年6月
合体の兆候のない高光度赤外線銀河 NGC 5135 が持つ活動銀河核の広帯域X線スペクトル解析

山田智史

日本天文学会2018年秋季年会　2018年3月
二重AGNを持つ高光度赤外線銀河 Mrk 463 の広帯域X線スペクトル解析

山田智史

日本天文学会2018年春季年会　2018年3月
On the Nature of the double active galactic nuclei in the merging galaxy Mrk 463

Satoshi Yamada

Zurich AGN workshop program　2017年12月
Broadband X-ray spectral analysis of the double-nucleus LIRG Mrk 463

Satoshi Yamada

East-Asia AGN Workshop 2017　2017年12月
Broadband X-ray spectral analysis of the double-nucleus LIRG Mrk 46

Satoshi Yamada

2017 COSMOS Team Meeting　2017年7月

︎全件表示 ︎最初の5件までを表示

共同研究・競争的資金等の研究課題 10

太陽系内外を繋ぐバリオン循環の物理・化学構造と生命の起源の学際研究

山田智史

2025年4月～ 2030年3月
XRISM衛星を主軸とした多波長面分光観測で探る銀河団までのアウトフロー構造

山田智史

2026年4月～ 2029年3月
X線衛星XRISMとTAO赤外線望遠鏡で探る活動銀河核アウトフローの物理機構

山田智史

2025年12月～ 2027年11月
X線衛星XRISMとTAO赤外線望遠鏡による合体銀河中のアウトフロー構造の解明

山田智史

提供機関：Japan Society for the Promotion of Science

制度名：Grants-in-Aid for Scientific Research

研究種目：Grant-in-Aid for Early-Career Scientists

研究機関：Institute of Physical and Chemical Research

2023年4月～ 2026年3月
超高空間分解能の赤外線観測と多波長観測による合体銀河が宇宙進化に果たした役割の解明

山田智史

2022年4月～ 2025年3月
理研内競争枠追加研究費 (SPDR Research Fundと共通)

山田智史

2023年4月～ 2024年3月
X線精密分光観測と赤外線高空間分解能観測で探る合体銀河中のアウトフローの物理機構

山田智史

2022年8月～ 2024年3月

詳細を見る詳細を閉じる

本研究課題は、宇宙に存在する銀河と、その中心に普遍的に存在する超巨大ブラックホールの両者の形成過程の解明が主な目的である。これらは単調に成長するのではなく、銀河同士の合体とそれに伴うブラックホールへの質量降着により急激に成長する。両者の進化過程を知るには、銀河の合体時に起きる物理現象を観測する必要があるが、ガスやダストに深く覆われて観測することが難しい。そこで今年度は、84天体の合体銀河に対し、透過力の高いX線、ダスト吸収により再放射される赤外線、星間物質による電波放射などを考慮し、独自に開発した多波長放射モデルを用いて、波長毎の放射源を網羅的に調査した。その結果、合体段階が進んだ天体ほど両者の成長が活発であることを解明することに成功した。さらにはブラックホールからの強い放射により噴出する「アウトフロー」により、莫大な物質が銀河にまで還元される描像を得た。現状の進捗は総じて順調であり、採択された科研費(スタート支援、早川幸男基金)も活用し、積極的に観測と理論の専門家との密な議論の元で地上望遠鏡観測(せいめい望遠鏡など)や多波長解析モデル開発(Yamada+23, ApJSで出版済み)に加え、論文執筆や国際学会発表も行った。本研究では2023年度に打上げ予定のXRISM衛星の観測も重要となる。予定通りの打上げに向けて、自身が担当する定常運用監視ツールの開発も行い、パイプライン開発チームを代表して日本天文学会の春季年会でも開発状況の進捗を報告した。衛星開発も順調に進んでおり、観測後の対応についても共同研究者と密に議論を進めている。次年度からはXRISM衛星の観測による成果も報告できると期待される。
近傍超/高光度赤外線銀河の包括的な多波長研究と超大質量ブラックホールと銀河の共進化機構への示唆

山田智史

2024年2月～
Comprehensive Multiwavelength Studies of Local U/LIRGs Observed with NuSTAR and/or Swift/BAT

山田智史

2022年9月～ 2022年10月
合体銀河中の活動銀河核の探査と多波長追求観測による銀河ブラックホール共進化の解明

山田智史

2019年4月～ 2022年3月

詳細を見る詳細を閉じる

本研究の目的は、銀河と超巨大ブラックホール (Supermassive Black Hole; SMBH) の共進化の物理的起源の解明である。前年度に続き、銀河同士の合体段階で急速に進化中の種族である超/高光度赤外線銀河84天体に着目し、SMBHへの質量降着機構を調べた。同研究室が開発した最新のX線モデルを適用することに加え、5つのX線衛星による約20年分の観測データを系統的に解析することで、銀河とSMBH間の質量輸送に関わるトーラス構造の物理的描像を得ることに成功した。特に合体末期では、激しい質量降着率によりSMBHが進化するだけでなく、輻射圧による莫大な質量輸送機構（アウトフロー）により銀河進化が制御されることも示唆された。本成果は学術論文として出版されている (Yamada et al. 2021, ApJS, 257, 61)。一方で、現状でのアウトフローの性質を導出する手法が、輝線/吸収線の青方偏移量の測定などに限られており、アウトフローを検出できた例のほとんどは合体末期の銀河のみであった。アウトフローの成長過程を正しく評価するには、新たな手法を開発し、他の合体段階におけるアウトフローも含めて系統的に調査することが不可欠である。そこで我々は、X線解析で使用したトーラスモデルの構造に加え、アウトフローのダスト成分と考えられるポーラーダストの構造も考慮した赤外線放射モデルを開発した。これを多波長放射モデルに実装し、同じ84天体を対象にX線から電波までの多波長データ解析を行い、ポーラーダストの性質に強い制限を与えた。その結果、合体が進むにつれてポーラーダストの光度は増加するが、一方でダストの平均温度は減少する傾向を初めて発見した。この結果は、合体が進むにつれてアウトフローが発達し、銀河スケールにまで広がったポーラーダストを形成していく描像を支持する。本成果も執筆中であり、ApJSに投稿する予定である。

︎全件表示 ︎最初の5件までを表示

担当経験のある科目(授業) 2

力学B (電生)　早稲田大学
物理学実験1　立教大学

メディア報道 27

ブラックホールの「爆風」、30万光年先まで到達東北大など

日本経済新聞 2026年8月15日号

2026年8月

メディア報道種別: 新聞・雑誌
Supermassive Black Hole Winds Span 300,000 Light-Years

Scientific Frontline：https://www.sflorg.com/2026/07/asph07292601.html

2026年7月

メディア報道種別: インターネットメディア
Black hole "blast" reaches 300,000 light years

EurekAlert：https://www.eurekalert.org/news-releases/1137999

2026年7月

メディア報道種別: インターネットメディア
噴き出す「爆風」銀河外までブラックホール世界初観測

静岡新聞 2026年7月29日号：https://www.kusastro.kyoto-u.ac.jp/~styamada/yamada2026a/newspapers/Shizuoka_Shimbun_20260729.pdf

2026年7月

メディア報道種別: 新聞・雑誌
ブラックホール爆風銀河外まで威力従来推定の100倍超

河北新報 2026年7月29日号：https://www.kusastro.kyoto-u.ac.jp/~styamada/yamada2026a/newspapers/Kahoku_Shimpo_20260729.pdf

2026年7月

メディア報道種別: 新聞・雑誌
一般相対性理論が予言する銀河中心ガス円盤の歳差運動の兆候を観測

プレスリリース：https://www.astroarts.co.jp/article/hl/a/14570_ngc4395

2026年7月

メディア報道種別: インターネットメディア
爆発的に星が誕生する合体銀河の中心で暴れ出したモンスター

プレスリリース：https://www.xrism.jaxa.jp/topics/science/1261/

2026年3月

メディア報道種別: インターネットメディア
理学研究科修了の5名が第40回井上研究奨励賞を受賞

京都大学　https://sci.kyoto-u.ac.jp/ja/news-246

2023年12月

メディア報道種別: インターネットメディア
金大など世界初観測ブラックホール銀河外へ「爆風」

北國新聞 2026年7月29日号：https://www.kusastro.kyoto-u.ac.jp/~styamada/yamada2026a/newspapers/Hokkoku_Chokan_20260729.pdf

2026年7月

メディア報道種別: 新聞・雑誌
噴き出す爆風、銀河外までブラックホール高温ガス、世界初観測

茨城新聞 2026年7月29日号：https://www.kusastro.kyoto-u.ac.jp/~styamada/yamada2026a/newspapers/Ibaraki_Shimbun_20260729.pdf

2026年7月

メディア報道種別: 新聞・雑誌
「爆風」銀河の外までブラックホール、世界初観測

福島民報 2026年7月29日号：https://www.kusastro.kyoto-u.ac.jp/~styamada/yamada2026a/newspapers/Fukushima_Minpo_20260729.pdf

2026年7月

メディア報道種別: 新聞・雑誌
噴き出す爆風銀河外側までブラックホールで世界初観測

秋田魁新報 2026年7月29日号：https://www.kusastro.kyoto-u.ac.jp/~styamada/yamada2026a/newspapers/Akita_Sakigake_Shimpo_20260729.pdf

2026年7月

メディア報道種別: 新聞・雑誌
ブラックホールから噴き出す「爆風」銀河の外側まで届く威力

岩手日報 2026年7月29日号：https://www.kusastro.kyoto-u.ac.jp/~styamada/yamada2026a/newspapers/Iwate_Nippo_20260729.pdf

2026年7月

メディア報道種別: 新聞・雑誌
噴き出す「爆風」銀河外までブラックホールから世界初

東奥日報 2026年7月29日号：https://www.kusastro.kyoto-u.ac.jp/~styamada/yamada2026a/newspapers/To-o_Nippo_20260729.jpg

2026年7月

メディア報道種別: 新聞・雑誌
ブラックホール爆風、世界初観測銀河外まで噴き出す

共同通信：https://news.yahoo.co.jp/articles/d1374c129c3908bfaf7f8a53339201cfe3651dc2

2026年7月

メディア報道種別: インターネットメディア
ブラックホールの「爆風」、30万光年先まで到達 ―想定の100倍超のエネルギーを発見―

プレスリリース：https://www.fris.tohoku.ac.jp/feature/topics/detail---id-1753.html

2026年7月

メディア報道種別: インターネットメディア
すばる望遠鏡が発見した特異なクエーサー「バーベキューソース」― 超巨大ブラックホール進化の途中段階か ―

プレスリリース：https://subarutelescope.org/jp/results/2026/06/02/3719.html

2026年6月

メディア報道種別: インターネットメディア
X線で調べる超大質量ブラックホール近傍の化学組成

プレスリリース：https://www.astroarts.co.jp/article/hl/a/14463_circinus

2026年4月

メディア報道種別: インターネットメディア
NASA-JAXA’s XRISM Telescope Clocks Hot Wind of Galaxy M82

プレスリリース：https://science.nasa.gov/missions/xrism/nasa-jaxas-xrism-telescope-clocks-hot-wind-of-galaxy-m82/

2026年3月

メディア報道種別: インターネットメディア
ブラックホールと暗黒物質が引き起こす宇宙の嵐

プレスリリース：https://www.astroarts.co.jp/article/hl/a/14408_perseus

2026年2月

メディア報道種別: インターネットメディア
理論上限の13倍の速さで物質を飲み込む巨大ブラックホール

プレスリリース：https://www.astroarts.co.jp/article/hl/a/14380_quasar

2026年1月

メディア報道種別: インターネットメディア
太陽の爆発にそっくり？超巨大ブラックホールからのガス噴出をXRISMが観測

プレスリリース：https://www.isas.jaxa.jp/topics/004154.html

2025年12月

メディア報道種別: インターネットメディア
Flaring black hole whips up ultra-fast winds (ESO/SRON/JAXA)

プレスリリース：https://www.esa.int/Science_Exploration/Space_Science/XMM-Newton/Flaring_black_hole_whips_up_ultra-fast_winds

2025年12月

メディア報道種別: インターネットメディア
「量子コンピュータxAI」で宇宙の異常変動を捉え、ブラックホールなど宇宙の謎に迫るー東北大学学際科学フロンティア研究所助教山田智史氏に聞く

読売新聞2025年7月25日号　http://www.kusastro.kyoto-u.ac.jp/~styamada/news/yomiuri_20250725.pdf

2025年7月

メディア報道種別: 新聞・雑誌
阪大・立教大・理研・東北大、宇宙のX線変動データから量子機械学習モデルで異常なエネルギー放射現象を捉えることに成功

日本経済新聞　https://www.nikkei.com/article/DGXZRSP693403_S5A700C2000000/

2025年7月

メディア報道種別: 新聞・雑誌
宇宙を読み解く新たな知性：量子×AIで異常なエネルギー放射現象を発見 ―X線宇宙観測データと量子機械学習の融合による世界初の成果―

大阪大学、立教大学、理化学研究所、東北大学　https://www.fris.tohoku.ac.jp/feature/topics/detail---id-1583.html

2025年7月

メディア報道種別: インターネットメディア
超巨大ブラックホールが撃ち出す超高速のガスの弾丸

JAXA　XRISM/PDS456 Team　https://www.xrism.jaxa.jp/topics/science/1140/

2025年5月

メディア報道種別: インターネットメディア

︎全件表示 ︎最初の5件までを表示

学術貢献活動 3

観測提案書の査読委員 (XRISM衛星、Subaru望遠鏡など: 5件)
国際論文の査読 (ApJ, A&A; 計5件)
国内研究会「最先端の観測装置と理論の両輪で探る降着現象の物理」の主催

2024年5月～

学術貢献活動種別: 学会・研究会等

その他 7

次世代X線ExCEED衛星サイエンスチームの所属 (代表機関：JAXA/NASA)
次世代X線NewAthena衛星サイエンスチームの所属 (代表機関：ESA)
次世代遠赤外線PRIMA衛星チームの所属 (代表機関：NASA)
すばる望遠鏡 Prime Focus Spectrograph (PFS) チームの所属 (代表機関：国立天文台)
次世代 X 線 Chronos 衛星チームの所属 (代表機関：JAXA)
XRISM 衛星開発チームの所属 (代表機関：JAXA/NASA)
全天 X 線監視装置 MAXI チームの所属 (代表機関：理化学研究所)

︎全件表示 ︎最初の5件までを表示