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  1. 数理物質系 (Faculty of Pure and Applied Sciences)
  2. 中井 直正 (Nakai Naomasa)
  1. コンテンツタイプ (Contents Type)
  2. 雑誌発表論文等 (Journal article, etc.)
  3. A~
  4. Astronomy and astrophysics

Detection of ammonia in M 51

http://hdl.handle.net/2241/119357
cb8fe56d-905e-4757-9ef8-99c9a4bea8a9
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AA_552.pdf AA_552.pdf (341.6 kB)
item type Journal Article(1)
公開日 2013-06-12
タイトル
タイトル Detection of ammonia in M 51
言語
言語 eng
資源タイプ
タイプ journal article
著者 Takano, Shuro

× Takano, Shuro

WEKO 100587

Takano, Shuro

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Takano, Toshiaki

× Takano, Toshiaki

WEKO 100588

Takano, Toshiaki

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Nakai, Naomasa

× Nakai, Naomasa

WEKO 100589

Nakai, Naomasa

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Kawaguchi, Kentaro

× Kawaguchi, Kentaro

WEKO 100590

Kawaguchi, Kentaro

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Schilke, Peter

× Schilke, Peter

WEKO 100591

Schilke, Peter

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著者別名 中井, 直正

× 中井, 直正

WEKO 566
e-Rad 80192665
筑波大学研究者総覧 0000000585

中井, 直正

Search repository
抄録
内容記述 Aims. To study the abundance and temperature of ammonia in the center of a nearby galaxy M 51 and to compare them with those in other nearby galaxies, we observed its (J,K) = (1, 1), (2, 2), (3, 3), and (4, 4) inversion transitions at the wavelength of 1.3 cm.

Methods. The observations were carried out with the Effelsberg 100-m radio telescope.

Results. The (1, 1), (2, 2), and (3, 3) transitions are clearly detected, but the (4, 4) transition is barely detected. The rotational temperature obtained from the (1, 1) and (2, 2) transitions of para-ammonia is 25 ± 2 K, which is similar to those of M 82 and the Large Magellanic Cloud (N 159 W), but significantly lower than those of IC 342 and NGC 1068 among the nearby galaxies. The column density of ammonia is (8.1 ± 2.4) × 1013 cm-2, and the abundance relative to H2 is ~4.5 × 10-9. The abundance in M 51 is about a factor of 5 lower than those of NGC 253 and IC 342, but about one order of magnitude higher than those of M 82 and the Large Magellanic Cloud. The addition of the data of M 51 further supports the exceptionally low abundances of ammonia reported previously in these two galaxies. For understanding the abundance of ammonia in M 51 and other nearby galaxies, their temperatures were compared. As a result, we found that the galaxies with low temperature tend to have low abundance of ammonia. In addition, the photodissociation rate of ammonia was compared to those of related molecules detected in the nearby galaxies to discuss the effect of photodissociation. We found that the low abundance of ammonia in some galaxies cannot be explained only by the effect of photodissociation.
書誌情報 Astronomy and astrophysics

巻 552, p. A34, 発行日 2013-04
ISSN
収録物識別子 0004-6361
書誌レコードID
収録物識別子 AA00553195
DOI
関連識別子
関連識別子 10.1051/0004-6361/201118593
権利
権利情報 © ESO, 2013
権利
権利情報 Reproduced with permission from Astronomy & Astrophysics, © ESO
著者版フラグ
値 publisher
出版者
出版者 EDP Sciences
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