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CO J = 3–2 Emission from the "Water Fountain" Sources IRAS 16342-3814 and IRAS 18286-0959
http://hdl.handle.net/10232/26220
http://hdl.handle.net/10232/262207fa5e17d-f297-4a9b-ae53-c2a9af92cdd5
名前 / ファイル | ライセンス | アクション |
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Item type | 学術雑誌論文 / Journal Article(1) | |||||
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公開日 | 2016-03-15 | |||||
タイトル | ||||||
タイトル | CO J = 3–2 Emission from the "Water Fountain" Sources IRAS 16342-3814 and IRAS 18286-0959 | |||||
著者 |
IMAI, Hiroshi
× IMAI, Hiroshi× HE, Jin-Hua× NAKASHIMA, Jun-ichi× UKITA, Nobuharu× DEGUCHI, Shuji× KONING, Nico |
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別言語の著者 | ||||||
姓名 | 今井, 裕 | |||||
別言語の著者 | ||||||
姓名 | 中島, 淳一 | |||||
別言語の著者 | ||||||
姓名 | 浮田, 信治 | |||||
別言語の著者 | ||||||
姓名 | 出口, 修至 | |||||
言語 | ||||||
言語 | eng | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | stars | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | AGB and post-AGB -- stars | |||||
キーワード | ||||||
主題Scheme | Other | |||||
主題 | individual (IRAS 16342-3814, IRAS 18286-0959) | |||||
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(Abstract) | ||||||
内容記述タイプ | Other | |||||
内容記述 | We observed CO J = 3–2 emission from "water-fountain" sources, which exhibit high-velocity collimated stellar jets traced by H2O maser emission, with the Atacama Submillimeter Telescope Experiment (ASTE) 10m telescope. We detected CO emission from two sources: IRAS 16342-3814 and IRAS 18286-0959. The IRAS 16342-3814 CO emission exhibits a spectrum that could be well fit to a Gaussian profile, rather than to a parabolic profile, with a velocity width (FWHM) of 158±6 km s^-1 and an intensity peak at V_LSR= 50±2 km s^-1. The mass-loss rate of the star is estimated to be ~2.9×10^-5 M yr^-1. Our morpho-kinematic models suggest that the CO emission is optically thin, and associated with a bipolar outflow rather than with a (cold and relatively small) torus. The IRAS 18286-0959 CO emission has a velocity width (FWHM) of 3.0±0.2 km s ^-1, smaller than typically seen in AGB envelopes. The narrow velocity width of the CO emission suggests that it originates from either an interstellar molecular cloud or a slowly-rotating circumstellar envelope that harbors the H2O maser source. | |||||
収録雑誌名 |
Publications of the Astronomical Society of Japan 巻 61, 号 6, p. 1365-1372, 発行日 2009 |
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作成日 | ||||||
日付 | 2009-12-25 | |||||
ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
ISSN | 0004-6264 | |||||
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 | info:doi/10.1093/pasj/61.6.1365 | |||||
権利 | ||||||
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 | |||||
公開者別名 | ||||||
公開者別名 | 日本天文学会 |