| アイテムタイプ |
default_学術雑誌論文 / Journal Article(1) |
| タイトル |
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タイトル |
The XRISM first-light observation: Velocity structure and thermal properties of the supernova remnant N 132D |
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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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主題Scheme |
Other |
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主題 |
X-rays |
| キーワード |
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言語 |
en |
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主題Scheme |
Other |
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主題 |
ISMISM |
| キーワード |
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言語 |
en |
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主題Scheme |
Other |
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主題 |
individual objects (except planetary nebulae)ISM |
| キーワード |
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言語 |
en |
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主題Scheme |
Other |
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主題 |
supernova remnants |
| 資源タイプ |
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資源タイプ識別子 |
http://purl.org/coar/resource_type/c_6501 |
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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 |
metadata only access |
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アクセス権URI |
http://purl.org/coar/access_right/c_14cb |
| 著者 |
山内 茂雄
粟木 久光
江副 祐一郎
榎戸 輝揚
海老沢 研
勝田 哲
澤田 真理
志達 めぐみ
鈴木 寛大
堂谷 忠靖
中澤 知洋
野田 博文
萩野 浩一
馬場 彩
福島 光太郎
藤田 裕
藤本 龍一
山内 誠
米山 友景
山岡 和貴
鶴 剛
山崎 典子
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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 |
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 σv ∼ 450 km s −1 . However, the Fe He α lines are substantially broadened with σv ∼ 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 α 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 −10 0 0 ≲ Vrs ( km s −1 ) ≲ 3300 ( in the observer frame) . We also find that Fe Ly α emission is redshifted with a bulk velocity of ∼ 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. |
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言語 |
en |
| 書誌情報 |
en : Publications of the Astronomical Society of Japan (PASJ)
巻 76,
号 6,
p. 1186-1201,
発行日 2024
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| 出版者 |
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出版者 |
日本天文学会 |
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言語 |
ja |
| 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 |
2053-051X |
| DOI |
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識別子タイプ |
DOI |
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関連識別子 |
10.1093/pasj/psae080 |
| 権利 |
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権利情報 |
© The Author(s) |
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言語 |
en |
https://academic.oup.com/pasj/article/76/6/1186/7817719
