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Hot ammonia in the center of the Seyfert 2 galaxy NGC 3079
http://hdl.handle.net/2241/00124679
http://hdl.handle.net/2241/0012467913e884f6-f6e7-41a4-a983-193b880c672e
名前 / ファイル | ライセンス | アクション |
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PASJ_67-1 (2.8 MB)
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Item type | Journal Article(1) | |||||
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公開日 | 2015-06-05 | |||||
タイトル | ||||||
タイトル | Hot ammonia in the center of the Seyfert 2 galaxy NGC 3079 | |||||
言語 | ||||||
言語 | eng | |||||
資源タイプ | ||||||
資源 | http://purl.org/coar/resource_type/c_6501 | |||||
タイプ | journal article | |||||
著者 |
Miyamoto, Yusuke
× Miyamoto, Yusuke× Nakai, Naomasa× Seta, Masumichi× Salak, Dragan× Hagiwara, Kenzaburo× Nagai, Makoto× Ishii, Shun× Yamauchi, Aya |
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著者別名 |
中井, 直正
× 中井, 直正× 永井, 誠 |
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抄録 | ||||||
内容記述タイプ | Abstract | |||||
内容記述 | We present the results of ammonia observations toward the center of NGC 3079. The NH3(J, K) = (1, 1) and (2, 2) inversion lines were detected in absorption with the Tsukuba 32 m telescope, and the NH3(1, 1) through (6, 6) lines with the VLA, although the profile of NH3(3, 3) was in emission in contrast to the other transitions. The background continuum source, whose flux density was ∼ 50 mJy, could not be resolved with the VLA beam of ≲ 0′′.09 × 0′′.08. All ammonia absorption lines have two distinct velocity components: one is at the systemic velocity and the other is blueshifted, and both components are aligned along the nuclear jets. For the systemic components, the relatively low temperature gas is extended more than the high temperature gas. The blueshifted NH3(3, 3) emission can be regarded as ammonia masers associated with shocks by strong winds probably from newly formed massive stars or supernova explosions in dense clouds in the nuclear megamaser disk. Using para-NH3(1, 1), (2, 2), (4, 4), and (5, 5) lines with VLA, we derived the rotational temperature Trot = 120 ± 12 K and 157 ± 19 K for the systemic and blueshifted components, respectively. The total column densities of NH3(0, 0)–(6, 6), assuming Tex ≈ Trot, were (8.85 ± 0.70) × 1016 cm−2 and (4.47 ± 0.78) × 1016 cm−2 for the systemic and blueshifted components, respectively. The fractional abundance of NH3 relative to molecular hydrogen H2 for the systemic and blueshifted was [NH3]/[H2] = 1.3 × 10−7 and 6.5 × 10−8, respectively. We also found the F = 4–4 and F = 5–5 doublet lines of OH 2Π3/2 J = 9/2 in absorption, which could be fitted by two velocity components, systemic and redshifted components. The rotational temperature of OH was estimated to be Trot, OH ≥ 175 K, tracing hot gas associated with the interaction of the fast nuclear outflow with dense molecular material around the nucleus. | |||||
書誌情報 |
PASJ : publications of the Astronomical Society of Japan 巻 67, 号 1, p. 5, 発行日 2015-02 |
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ISSN | ||||||
収録物識別子タイプ | ISSN | |||||
収録物識別子 | 0004-6264 | |||||
書誌レコードID | ||||||
収録物識別子タイプ | NCID | |||||
収録物識別子 | AA1082896X | |||||
DOI | ||||||
識別子タイプ | DOI | |||||
関連識別子 | 10.1093/pasj/psu131 | |||||
権利 | ||||||
権利情報 | © The Author 2015. Published by Oxford University Press on behalf of the Astronomical Society of Japan | |||||
権利 | ||||||
権利情報 | This is a pre-copyedited, author-produced PDF of an article accepted for publication in PASJ : publications of the Astronomical Society of Japan following peer review. The version of record Publ Astron Soc Jpn (February 2015) 67 (1): 5 is available online at: doi: 10.1093/pasj/psu131 | |||||
著者版フラグ | ||||||
値 | author | |||||
出版者 | ||||||
出版者 | Astronomical Society of Japan | |||||
出版者 | ||||||
出版者 | Published online by Oxford University Press |