| アイテムタイプ |
学術雑誌論文 / Journal Article(1) |
| 公開日 |
2025-10-22 |
| タイトル |
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タイトル |
Mapping Cassiopeia A’s silicon/sulfur Doppler velocities with XRISM/Resolve |
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言語 |
en |
| 言語 |
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言語 |
eng |
| キーワード |
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言語 |
en |
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キーワード |
ISM: individual objects (Cassiopeia A) |
| キーワード |
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言語 |
en |
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キーワード |
ISM: jets and outflows |
| キーワード |
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言語 |
en |
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キーワード |
ISM: supernova remnants |
| キーワード |
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言語 |
en |
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キーワード |
X-rays: ISM |
| 資源タイプ |
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資源タイプ |
journal article |
| アクセス権 |
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アクセス権 |
open access |
| 著者 |
Vink, Jacco
| en |
Vink, Jacco（Personal）
Anton Pannekoek Instituut voor Sterrenkunde
|
Search repository
Agarwal, Manan
| en |
Agarwal, Manan（Personal）
Anton Pannekoek Instituut voor Sterrenkunde
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Search repository
Bamba, Aya
Gu, Liyi
| en |
Gu, Liyi（Personal）
SRON Netherlands Institute for Space Research
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Search repository
Plucinsky, Paul
| en |
Plucinsky, Paul（Personal）
Harvard-Smithsonian Center for Astrophysics
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Search repository
Behar, Ehud
Corrales, Lia
Foster, Adam
| en |
Foster, Adam（Personal）
Harvard-Smithsonian Center for Astrophysics
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Search repository
Fujimoto, Shin Ichiro
| en |
Fujimoto, Shin Ichiro（Personal）
National Institute of Technology, Kumamoto College
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Search repository
Ichihashi, Masahiro
Ichikawa, Kazuhiro
Katsuda, Satoru
Matsumoto, Hironori
Matsunaga, Kai
Mizuno, Tsunefumi
森, 浩二
Murakami, Hiroshi
Nakajima, Hiroshi
Sato, Toshiki
Sawada, Makoto
Sonoda, Haruto
Suzuki, Shunsuke
Tateishi, Dai
Terada, Yukikatsu
Uchida, Hiroyuki
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| 抄録 |
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内容記述タイプ |
Abstract |
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内容記述 |
Young supernova remnants (SNRs) provide crucial insights into explosive nucleosynthesis products and their velocity distribution soon after the explosion. However, these velocities are influenced by the dynamics of the circumstellar medium (CSM), which in young core-collapse SNRs originates from the progenitor’s late-phase mass loss. Cassiopeia A (Cas A), the youngest known Galactic core-collapse SNR, was studied to analyze the spatial distribution of silicon and sulfur radial velocities using two high-spectral-resolution observations from the XRISM/Resolve imaging spectrometer. Resolve’s capabilities enabled the detailed characterization of Sixiii, Sixiv, Sxv, and Sxvi lines, whose line shapes can be resolved and modeled using Gaussian radial velocity components. The radial velocities measured generally align with previous CCD-based results, confirming that they were not artifacts caused by blended lines or ionization variations. Modeling line profiles with two-component Gaussians improved fits in some regions, revealing distinct redshifted (back side) and blueshifted (front side) components only in a few specific areas. In most regions, however, both components were either both redshifted (north-west) or both blueshifted (south-east), consistent with the patchy ejecta shell morphology seen in optically emitting fast-moving knots. The individual line components revealed line broadening ranging from σv ≈ 200 to σv ≈ 2000 km s-1. Components with 1000 ≲ σv> ≲ 2000 km s-1 are consistent with previously determined reverse-shock velocities, suggesting non-equilibrated or partially equilibrated ion temperatures. Narrow components with small radial velocities found near Cas A’s projected center likely originate from shocked CSM plasma. But the low radial velocity and small σ<inf>v</inf> poses a challenge to identify these components with either the front side or back side of the SNR, or a blend of both sides. |
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言語 |
en |
| 書誌情報 |
en : Publications of the Astronomical Society of Japan
巻 77,
号 Supplement_1,
p. 154-170,
発行日 2025-09
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| 出版者 |
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出版者 |
Oxford University Press (OUP) |
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言語 |
en |
| ISSN |
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収録物識別子タイプ |
EISSN |
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収録物識別子 |
2053051X |
| ISSN |
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収録物識別子タイプ |
ISSN |
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収録物識別子 |
00046264 |
| DOI |
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関連タイプ |
isVersionOf |
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識別子タイプ |
DOI |
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関連識別子 |
https://doi.org/10.1093/pasj/psaf053 |
| 著者版フラグ |
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出版タイプ |
VoR |
fulltext (4.6 MB)
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