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Sagittarius A Molecular Cloud Complex in H13CO+ and Thermal SiO Emission Lines
http://hdl.handle.net/10232/19038
http://hdl.handle.net/10232/1903882b3f550-6be3-44cd-92cf-5e62875a63bc
| 名前 / ファイル | ライセンス | アクション |
|---|---|---|
HANDA_0004-6264_63_763-794.pdf (12.4 MB)
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| Item type | 学術雑誌論文 / Journal Article(1) | |||||
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| 公開日 | 2013-07-31 | |||||
| タイトル | ||||||
| タイトル | Sagittarius A Molecular Cloud Complex in H13CO+ and Thermal SiO Emission Lines | |||||
| タイトル言語 | en | |||||
| 著者 |
坪井, 昌人
× 坪井, 昌人× 但木, 謙一× 宮崎, 敦× 半田, 利弘 |
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| 言語 | ||||||
| 言語 | eng | |||||
| キーワード | ||||||
| 主題言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | Galaxy: center | |||||
| キーワード | ||||||
| 主題言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | ISM: clouds | |||||
| キーワード | ||||||
| 主題言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | ISM: magnetic fileds | |||||
| キーワード | ||||||
| 主題言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | ISM: supernova remnants | |||||
| 資源タイプ | ||||||
| 資源タイプ識別子 | http://purl.org/coar/resource_type/c_6501 | |||||
| 資源タイプ | journal article | |||||
| 要約 | ||||||
| 内容記述タイプ | Other | |||||
| 内容記述 | We present results of a high-resolution wide-field mapping observation of the Sagittarius A (Sgr A) molec-ular cloud complex in H13CO+ J = 1-0 and thermal SiO J = 2-1 emission lines with the 25-beam receiver of the 100 GHz band operating on the Nobeyama Radio Observatory 45-m telescope. The mapping area covers a 0.°5 x × 0.°5 area involving several named molecular clouds, for example GCM -0.02-0.07, GCM -0.13-0.08, GCM 0.11-0.11, the Sickle molecular cloud, the Arched filaments molecular cloud, and so on. The data have an effective angular resolution of 26"". The H13CO+ emission line is a famous tracer of molecular gas mass because the line is optically thin, even in the Galactic center region, and is not emphasized by shock. The emission line presents a clumpy distribution of the molecular cloud. The averaged fractional abundance in the Sgr A complex is N (H13 CO+) /NH2 (1.8±0.4) ×10-11, comparing the LTE mass and the virial theorem mass. The SiO emission line is a famous and reliable tracer of shocked molecular gas. We find many molecular clouds that are remarkable only in the SiO emission line. Such molecular clouds have a large velocity width of up to 60km s-1. The brightness temperature ratio is up to TB(SiO)/ TB(H13CO+) < 8. The features are dominated by shock SiO-enriched gas. In such clouds, the ratio of the fractional abundance of SiO and H13CO+ molecules is X (Si0)/ x(H13CO+)~ 100. The features are presumably made by supernova remnants. We found a prototypical example in GCM -0.02-0.07. It has two distinct structures. One is a ridge-like structure contacting with the Sgr A East shell; another is an expanding shell-like structure. There is a wide-velocity width ridge of SiO-enriched gas in GCM 0.11-0.11, which is adja-cent to Vertical filaments. This suggests that the collision with the molecular cloud accelerates relativistic electrons, which illuminate the Vertical filaments-Polarized Plumes complex. | |||||
| 内容記述言語 | en | |||||
| 収録雑誌名 |
en : Publications of the Astronomical Society of Japan 巻 63, 号 4, p. 763-794, 発行日 2011 |
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| 作成日 | ||||||
| 日付 | 2011-08-25 | |||||
| 日付タイプ | Issued | |||||
| ISSN | ||||||
| 収録物識別子タイプ | PISSN | |||||
| ISSN | 00046264 | |||||
| NII書誌ID（雑誌） | ||||||
| 収録物識別子タイプ | NCID | |||||
| NC ID | AA1082896X | |||||
| DOI | ||||||
| 識別子タイプ | DOI | |||||
| DOI | https://doi.org/10.1093/pasj/63.4.763 | |||||
| 権利 | ||||||
| 権利情報の言語 | en | |||||
| 権利情報 | Astronomical Society of Japan | |||||
| 出版タイプ | ||||||
| 出版タイプ | VoR | |||||
| 出版タイプResource | http://purl.org/coar/version/c_970fb48d4fbd8a85 | |||||
| NDC | ||||||
| 主題Scheme | NDC | |||||
| 主題 | 440 | |||||
| 公開者・出版者 | ||||||
| 出版者 | Astronomical Society of Japan | |||||
| 出版者言語 | en | |||||
| 公開者・出版者 | ||||||
| 出版者 | 日本天文学会 | |||||
| 出版者言語 | ja | |||||
