|
Affiliation |
Engineering educational research section Semiconductor Science and Applied Physics Program |
|
Title |
Professor |
|
External Link |
|
|
Related SDGs |
|
MORI Koji
|
|
|
Degree 【 display / non-display 】
-
Doctor (Science) ( 2002.6 Osaka University )
Research Areas 【 display / non-display 】
-
Natural Science / Astronomy / X-ray and Gamma-ray astrophysics
Papers 【 display / non-display 】
-
Yukumoto M., Mori K., Takeda A., Nishioka Y., Kimura M., Fuchita Y., Yoshida T., Tsuru T.G., Kurachi I., Hagino K., Arai Y., Kohmura T., Tanaka T., Nobukawa K.K.
Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment 1072 2025.3
Language：English Publishing type：Research paper (scientific journal) Publisher：Nuclear Instruments and Methods in Physics Research, Section A: Accelerators, Spectrometers, Detectors and Associated Equipment
We have been developing silicon-on-insulator (SOI) pixel detectors with a pinned depleted diode (PDD) structure, named “XRPIX”, for X-ray astronomy. In our previous study, we successfully optimized the design of the PDD structure, achieving both the suppression of large leakage current and satisfactory X-ray spectroscopic performance. Here, we report a detailed study on the X-ray spectroscopic performance of the XRPIX with the optimized PDD structure. The data were obtained at −60 °C with the “event-driven readout mode”, in which only a triggering pixel and its surroundings are read out. The energy resolutions in full width at half maximum at 6.4 keV are 178±1eV and 291±1eV for single-pixel and all-pixel event spectra, respectively. The all-pixel events include charge-sharing pixel events as well as the single-pixel events. These values are the best achieved in the history of our development. We argue that the gain non-linearity in the low energy side due to excessive charge injection to the charge-sensitive amplifier is a major factor to limit the current spectroscopic performance. Optimization of the amount of the charge injection is expected to lead to further improvement in the spectroscopic performance of XRPIX, especially for the all-pixel event spectrum.
-
XRISM Reveals Low Nonthermal Pressure in the Core of the Hot, Relaxed Galaxy Cluster A2029 Reviewed International coauthorship
Audard M., Awaki H., Ballhausen R., Bamba A., Behar E., Boissay-Malaquin R., Brenneman L., Brown G.V., Corrales L., Costantini E., Cumbee R., Trigo M.D., Done C., Dotani T., Ebisawa K., Eckart M.E., Eckert D., Eguchi S., Enoto T., Ezoe Y., Foster A., Fujimoto R., Fujita Y., Fukazawa Y., Fukushima K., Furuzawa A., Gallo L., García J.A., Gu L., Guainazzi M., Hagino K., Hamaguchi K., Hatsukade I., Hayashi K., Hayashi T., Hell N., Hodges-Kluck E., Hornschemeier A., Ichinohe Y., Ishida M., Ishikawa K., Ishisaki Y., Kaastra J., Kallman T., Kara E., Katsuda S., Kanemaru Y., Kelley R., Kilbourne C., Kitamoto S., Kobayashi S., Kohmura T., Kubota A., Leutenegger M., Loewenstein M., Maeda Y., Markevitch M., Matsumoto H., Matsushita K., McCammon D., McNamara B., Mernier F., Miller E.D., Miller J.M., Mitsuishi I., Mizumoto M., Mizuno T., Mori K., Mukai K., Murakami H., Mushotzky R., Nakajima H., Nakazawa K., Ness J.U., Nobukawa K., Nobukawa M., Noda H., Odaka H., Ogawa S., Ogorzalek A., Okajima T., Ota N., Paltani S., Petre R., Plucinsky P., Porter F.S., Pottschmidt K., Sato K., Sato T., Sawada M., Seta H., Shidatsu M., Simionescu A., Smith R., Suzuki H., Szymkowiak A., Takahashi H., Takeo M., Tamagawa T., Tamura K.
Astrophysical Journal Letters 982 ( 1 ) 2025.3
Language：English Publishing type：Research paper (scientific journal) Publisher：Astrophysical Journal Letters
The X-ray binary system Cygnus X-3 (4U 2030+40, V1521 Cyg) is luminous but enigmatic owing to the high intervening absorption. High-resolution X-ray spectroscopy uniquely probes the dynamics of the photoionized gas in the system. In this Letter, we report on an observation of Cyg X-3 with the XRISM/Resolve spectrometer, which provides unprecedented spectral resolution and sensitivity in the 2-10 keV band. We detect multiple kinematic and ionization components in absorption and emission whose superposition leads to complex line profiles, including strong P Cygni profiles on resonance lines. The prominent Fe XXV Hea and Fe XXVI Lya emission complexes are clearly resolved into their characteristic fine-structure transitions. Self-consistent photoionization modeling allows us to disentangle the absorption and emission components and measure the Doppler velocity of these components as a function of binary orbital phase. We find a significantly higher velocity amplitude for the emission lines than for the absorption lines. The absorption lines generally appear blueshifted by ∼-500-600 km s-1. We show that the wind decomposes naturally into a relatively smooth and large-scale component, perhaps associated with the background wind itself, plus a turbulent, denser structure located close to the compact object in its orbit.
-
Soft X-ray Imager of the Xtend system on board XRISM Reviewed
Noda, H., Mori, K. et al.
Publications of the Astronomical Society of Japan 2025.3
Authorship：Corresponding author Language：English Publishing type：Research paper (scientific journal) Publisher：Publications of the Astronomical Society of Japan
Sagittarius A East is a supernova remnant with a unique surrounding environment, as it is located in the immediate vicinity of the supermassive black hole at the Galactic center, Sagittarius A∗. The X-ray emission of the remnant is suspected to show features of overionized plasma, which would require peculiar evolutionary paths. We report on the first observation of Sagittarius A East with the X-Ray Imaging and Spectroscopy Mission (XRISM). Equipped with a combination of a high-resolution microcalorimeter spectrometer and a large field-of-view CCD imager, we for the first time resolved the Fe XXV K-shell lines into fine structure lines and measured the forbidden-to-resonance intensity ratio to be 1.39 ± 0.12, which strongly suggests the presence of overionized plasma. We obtained a reliable constraint on the ionization temperature just before the transition into the overionization state, of >4 keV. The recombination timescale was constrained to be <8 × 1011 cm−3 s. The small velocity dispersion of 109 ± 6 km s−1 indicates a low Fe ion temperature <8 keV and a small expansion velocity <200 km s−1. The high initial ionization temperature and small recombination timescale suggest that either rapid cooling of the plasma via adiabatic expansion from dense circumstellar material or intense photoionization by Sagittarius A∗ in the past may have triggered the overionization.
-
The bulk motion of gas in the core of the Centaurus galaxy cluster Reviewed
Majumder A., Hosogi K., Sun M., Plšek T., Werner N., Kondo M., Zhuravleva I., Yukita M., Yoshida T., Yoneyama T., Yaqoob T., Yamauchi S., Yamauchi M., Yamasaki N.Y., Yamaoka K., Yamaguchi H., Yamada S., Yamada S., Williams B.J., Watanabe S., Vink J., Uno S., Ueda Y., Uchiyama H., Uchida Y., Uchida N., Uchida H., Tsuru T.G., Tsunemi H., Tsujimoto M., Tsuboi Y., Trigo M.D., Terashima Y., Terada Y., Tashiro M., Tanimoto A., Tanaka T., Tamura K., Tamagawa T., Takeo M., Takahashi H., Szymkowiak A., Suzuki H., Smith R., Simionescu A., Shidatsu M., Seta H., Sawada M., Sato T., Sato K., Pottschmidt K., Porter F.S., Plucinsky P., Petre R., Paltani S., Ota N., Okajima T., Ogorzalek A., Ogawa S., Odaka H., Noda H., Nobukawa M., Nobukawa K., Ness J.U., Nakazawa K., Nakajima H., Mushotzky R., Murakami H., Mukai K., Mori K., Mizuno T., Mizumoto M., Mitsuishi I., Miller J.M., Miller E.D., Mernier F., McNamara B., McCammon D., Matsushita K., Matsumoto H., Markevitch M., Maeda Y., Loewenstein M., Leutenegger M., Kubota A., Kohmura T., Kobayashi S., Kitamoto S., Kilbourne C., Kelley R., Kanemaru Y., Katsuda S., Kara E., Kallman T., Kaastra J., Ishisaki Y., Ishikawa K., Ishida M., Ichinohe Y., Hornschemeier A.
Nature 638 ( 8050 ) 365 - 369 2025.2
Publishing type：Research paper (scientific journal) Publisher：Nature
Galaxy clusters contain vast amounts of hot ionized gas known as the intracluster medium (ICM). In relaxed cluster cores, the radiative cooling time of the ICM is shorter than the age of the cluster. However, the absence of line emission associated with cooling suggests heating mechanisms that offset the cooling, with feedback from active galactic nuclei (AGNs) being the most likely source1,2. Turbulence and bulk motions, such as the oscillating (‘sloshing’) motion of the core gas in the cluster potential well, have also been proposed as mechanisms for heat distribution from the outside of the core3,4. Here we present X-ray spectroscopic observations of the Centaurus galaxy cluster with the X-Ray Imaging and Spectroscopy Mission satellite. We find that the hot gas flows along the line of sight relative to the central galaxy, with velocities from 130 km s−1 to 310 km s−1 within about 30 kpc of the centre. This indicates bulk flow consistent with core gas sloshing. Although the bulk flow may prevent excessive accumulation of cooled gas at the centre, it could distribute the heat injected by the AGN and bring in thermal energy from the surrounding ICM. The velocity dispersion of the gas is found to be only ≲120 km s−1 in the core, even within about 10 kpc of the AGN. This suggests that the influence of the AGN on the surrounding ICM motion is limited in the cluster.
-
Overionized plasma in the supernova remnant Sagittarius A East anchored by XRISM observations Reviewed
Audard M., Awaki H., Ballhausen R., Bamba A., Behar E., Boissay-Malaquin R., Brenneman L., Brown G.V., Corrales L., Costantini E., Cumbee R., Diaz-Trigo M., Done C., Dotani T., Ebisawa K., Eckart M., Eckert D., Enoto T., Eguchi S., Ezoe Y., Foster A., Fujimoto R., Fujita Y., Fukazawa Y., Fukushima K., Furuzawa A., Gallo L., García J.A., Gu L., Guainazzi M., Hagino K., Hamaguchi K., Hatsukade I., Hayashi K., Hayashi T., Hell N., Hodges-Kluck E., Hornschemeier A., Ichinohe Y., Ishida M., Ishikawa K., Ishisaki Y., Kaastra J., Kallman T., Kara E., Katsuda S., Kanemaru Y., Kelley R., Kilbourne C., Kitamoto S., Kobayashi S., Kohmura T., Kubota A., Leutenegger M., Loewenstein M., Maeda Y., Markevitch M., Matsumoto H., Matsushita K., McCammon D., McNamara B., Mernier F., Miller E.D., Miller J.M., Mitsuishi I., Mizumoto M., Mizuno T., Mori K., Mukai K., Murakami H., Mushotzky R., Nakajima H., Nakazawa K., Ness J.U., Nobukawa K., Nobukawa M., Noda H., Odaka H., Ogawa S., Ogorzalek A., Okajima T., Ota N., Paltani S., Petre R., Plucinsky P., Scott Porter F., Pottschmidt K., Sato K., Sato T., Sawada M., Seta H., Shidatsu M., Simionescu A., Smith R., Suzuki H., Szymkowiak A., Takahashi H., Takeo M., Tamagawa T., Tamura K.
Publications of the Astronomical Society of Japan 77 ( 1 ) L1 - L8 2025.2
Publishing type：Research paper (scientific journal) Publisher：Publications of the Astronomical Society of Japan
Sagittarius A East is a supernova remnant with a unique surrounding environment, as it is located in the immediate vicinity of the supermassive black hole at the Galactic center, Sagittarius A∗. The X-ray emission of the remnant is suspected to show features of overionized plasma, which would require peculiar evolutionary paths. We report on the first observation of Sagittarius A East with the X-Ray Imaging and Spectroscopy Mission (XRISM). Equipped with a combination of a high-resolution microcalorimeter spectrometer and a large field-of-view CCD imager, we for the first time resolved the Fe XXV K-shell lines into fine structure lines and measured the forbidden-to-resonance intensity ratio to be 1.39 ± 0.12, which strongly suggests the presence of overionized plasma. We obtained a reliable constraint on the ionization temperature just before the transition into the overionization state, of >4 keV. The recombination timescale was constrained to be <8 × 1011 cm−3 s. The small velocity dispersion of 109 ± 6 km s−1 indicates a low Fe ion temperature <8 keV and a small expansion velocity <200 km s−1. The high initial ionization temperature and small recombination timescale suggest that either rapid cooling of the plasma via adiabatic expansion from dense circumstellar material or intense photoionization by Sagittarius A∗ in the past may have triggered the overionization.
DOI： 10.1093/pasj/psae111
MISC 【 display / non-display 】
-
SXS装置によるかに超新星残骸の熱的プラズマ放射探査 Invited
辻本匡弘、森浩二
天文月報 2019.6
Language：Japanese Publishing type：Article, review, commentary, editorial, etc. (scientific journal) Publisher：日本天文学会
-
超新星残骸から探るIa型超新星爆発の親星の金属量
森浩二
天文月報 2014.6
Language：Japanese Publishing type：Article, review, commentary, editorial, etc. (scientific journal) Publisher：日本天文学会
-
宮崎県における高等学校と大学との物理教育に関する連絡会
森浩二、木村英二
大学の物理教育 2013.11
Language：Japanese Publishing type：Research paper, summary (national, other academic conference) Publisher：日本物理学会
-
Ｘ線で見る星座
森浩二
数研出版株式会社サイエンスネット第37号 37 2009.11
Language：Japanese Publishing type：Article, review, commentary, editorial, etc. (other) Publisher：数研出版株式会社
-
Ｘ線天文衛星 Suzaku および Chandra を用いた小マゼラン星雲中の超新星残骸 0103-72.6 の観測的研究
川井田英広, 木村結樹, 森浩二
宮崎大学工学部紀要 ( 37 ) 43 - 50 2008.8
Language：Japanese Publishing type：Article, review, commentary, editorial, etc. (bulletin of university, research institution) Publisher：宮崎大学工学部
Presentations 【 display / non-display 】
-
超高層大気を観測するISS搭載X線SOI-CMOSピクセル検出器カメラの開発 International coauthorship
武田彩希、森浩二、他
日本物理学会2024年春季大会
Event date： 2025.3.18 - 2025.3.21
Language：Japanese Presentation type：Oral presentation (general)
-
CTA報告218：全体報告 International coauthorship
山本常夏、森浩二、他
日本物理学会2024年春季大会
Event date： 2025.3.18 - 2025.3.21
Language：Japanese Presentation type：Oral presentation (general)
-
X線分光撮像衛星XRISM搭載X線望遠鏡(XMA)開発の現状 (9) International coauthorship
石田學、森浩二、他
日本物理学会2024年春季大会
Event date： 2025.3.18 - 2025.3.21
Language：Japanese Presentation type：Oral presentation (general)
-
Ｘ線分光撮像衛星 XRISM 搭載軟Ｘ線撮像装置 Xtend の現状 International coauthorship
鈴木寛大、森浩二、他
日本物理学会2024年春季大会
Event date： 2025.3.18 - 2025.3.21
Language：Japanese Presentation type：Oral presentation (general)
-
XRISM衛星によるSN1987A観測１：爆発噴出物プラズマの膨張構造の測定 International coauthorship
寺田幸功、森浩二、他
日本天文学会2025年春季年会
Event date： 2025.3.17 - 2025.3.20
Language：Japanese Presentation type：Oral presentation (general)
Awards 【 display / non-display 】
-
日本物理学会若手奨励賞
2009.3 日本物理学会
森浩二
Award type：Award from Japanese society, conference, symposium, etc. Country：Japan
-
井上研究奨励賞
2005.2 井上科学振興財団
森浩二
Award type：Award from publisher, newspaper, foundation, etc. Country：Japan
Grant-in-Aid for Scientific Research 【 display / non-display 】
-
終端衝撃波のＸ線撮像分光による銀河系内最強加速器「カニ星雲」の加速機構の解明
Grant number：23K20850 2024.04 - 2026.03
独立行政法人日本学術振興会 科学研究費基金 基盤研究(B)
Authorship：Principal investigator
-
終端衝撃波のＸ線撮像分光による銀河系内最強加速器「カニ星雲」の加速機構の解明
Grant number：21H01095 2021.04 - 2026.03
独立行政法人日本学術振興会 科学研究費補助金 基盤研究(B)
Authorship：Principal investigator
-
カニ星雲のサブ秒角スケールでの精密X線分光による電磁流体加速機構の解明
Grant number：21J10842 2021.04 - 2023.03
独立行政法人日本学術振興会 科学研究費補助金 特別研究員奨励費
Authorship：Principal investigator
-
超新星残骸のＸ線精密撮像分光から探るIa型超新星の親星の起源
Grant number：16H03983 2019.04 - 2020.03
科学研究費補助金 基盤研究(B)
Authorship：Principal investigator
-
超新星残骸のＸ線精密撮像分光から探るIa型超新星の親星の起源
Grant number：16H03983 2018.04 - 2019.03
科学研究費補助金 基盤研究(B)
Authorship：Principal investigator
Other research activities 【 display / non-display 】
-
国立天文台ハワイ観測所 Subaru Seminars
2005.02
国立天文台ハワイ観測所において「Recent progress in X-ray studies of the Crab Pulsar Wind Nebula」というタイトルでセミナーをおこなった。
-
大阪大学理学部X線天文グループセミナー
2004.12
大阪大学理学部X線天文グループに招かれて「パルサー星雲観測の最近の進展」というタイトルでセミナーをおこなった。
Available Technology 【 display / non-display 】
-
Ｘ線天文衛星を用いた高エネルギー天体の観測的研究
Ｘ線に感度を持つ衛星搭載用半導体カメラの開発
地上で動作可能な放射線イメージングカメラの開発Home Page： 高エネルギー宇宙物理学研究室
Related fields where technical consultation is available：・ Ｘ線・ガンマ線・陽子・中性子を含む放射線イメージング
・ 人工衛星に搭載する機器開発一般Message：お手持ちの技術を宇宙開発・放射線測定等に応用したいという場合は、ぜひご連絡ください