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Star Formation in the Molecular Cloud Associated with the Monkey Head Nebula: Sequential or Spontaneous?
http://hdl.handle.net/10232/18781
http://hdl.handle.net/10232/187812cd7ac48-1a2c-4e54-8cad-c317c1702462
| 名前 / ファイル | ライセンス | アクション |
|---|---|---|
HANDA_0004-637X_762_1_17.pdf (1.7 MB)
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| Item type | 学術雑誌論文 / Journal Article(1) | |||||
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| 公開日 | 2014-12-22 | |||||
| タイトル | ||||||
| タイトル | Star Formation in the Molecular Cloud Associated with the Monkey Head Nebula: Sequential or Spontaneous? | |||||
| タイトル言語 | en | |||||
| 著者 |
Chibueze, James O.
× Chibueze, James O.× 井村, 健二× 面高, 俊宏× 半田, 利弘× 永山, 匠× 藤沢, 健太× 砂田, 和良× 仲野, 誠× 亀﨑, 達矢× 山口, 善之× 関戸, 衛 |
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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 | H II regions | |||||
| 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: individual objects (Gemini OB1) | |||||
| キーワード | ||||||
| 主題言語 | en | |||||
| 主題Scheme | Other | |||||
| 主題 | ISM: molecules | |||||
| 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 | |||||
| アクセス権 | ||||||
| アクセス権 | open access | |||||
| アクセス権URI | http://purl.org/coar/access_right/c_abf2 | |||||
| 要約 | ||||||
| 内容記述タイプ | Other | |||||
| 内容記述 | We mapped the (1,1), (2,2), and (3,3) lines of NH3 toward the molecular cloud associated with the Monkey Head Nebula (MHN) with a 1.'6 angular resolution using a Kashima 34 m telescope operated by the National Institute of Information and Communications Technology (NICT). The kinetic temperature of the molecular gas is 15-30 K in the eastern part and 30-50 K in the western part. The warmer gas is confined to a small region close to the compact H II region S252A. The cooler gas is extended over the cloud even near the extended H II region, the MHN. We made radio continuum observations at 8.4 GHz using the Yamaguchi 32 m radio telescope. The resultant map shows no significant extension from the Hα image. This means that the molecular cloud is less affected by the MHN, suggesting that the molecular cloud did not form by the expanding shock of the MHN. Although the spatial distribution of the Wide-field Infrared Survey Explorer and Two Micron All Sky Survey point sources suggests that triggered low- and intermediate-mass star formation took place locally around S252A, but the exciting star associated with it should be formed spontaneously in the molecular cloud. | |||||
| 内容記述言語 | en | |||||
| 収録雑誌名 |
en : The Astrophysical Journal 巻 762, 号 1, 発行日 2012 |
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| 作成日 | ||||||
| 日付 | 2012-12-11 | |||||
| 日付タイプ | Issued | |||||
| ISSN | ||||||
| 収録物識別子タイプ | PISSN | |||||
| ISSN | 0004637X | |||||
| DOI | ||||||
| 識別子タイプ | DOI | |||||
| DOI | https://doi.org/10.1088/0004-637X/762/1/17 | |||||
| 権利 | ||||||
| 権利情報の言語 | en | |||||
| 権利情報 | American Astronomical Society | |||||
| 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 | IOP Publishing/American Astronomical Society | |||||
| 出版者言語 | en | |||||
