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DO CIRCUMNUCLEAR DENSE GAS DISKS DRIVE MASS ACCRETION ONTO SUPERMASSIVE BLACK HOLES
http://hdl.handle.net/2261/60925
http://hdl.handle.net/2261/60925f00b4d72-e8d5-4393-9b9f-63e5e16991e8
| 名前 / ファイル | ライセンス | アクション |
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Izumi_2016_ApJ_827_81.pdf (2.4 MB)
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| Item type | 学術雑誌論文 / Journal Article(1) | |||||
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| 公開日 | 2017-01-10 | |||||
| タイトル | ||||||
| タイトル | DO CIRCUMNUCLEAR DENSE GAS DISKS DRIVE MASS ACCRETION ONTO SUPERMASSIVE BLACK HOLES | |||||
| 言語 | ||||||
| 言語 | eng | |||||
| キーワード | ||||||
| 主題Scheme | Other | |||||
| 主題 | galaxies: active | |||||
| キーワード | ||||||
| 主題Scheme | Other | |||||
| 主題 | galaxies: ISM | |||||
| キーワード | ||||||
| 主題Scheme | Other | |||||
| 主題 | ISM: molecules | |||||
| 資源タイプ | ||||||
| 資源 | http://purl.org/coar/resource_type/c_6501 | |||||
| タイプ | journal article | |||||
| 著者 |
Izumi, Takuma
× Izumi, Takuma× Kawakatu, Nozomu× Kohno, Kotaro |
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| 著者所属 | ||||||
| 著者所属 | Institute of Astronomy, School of Science, The University of Tokyo | |||||
| 著者所属 | ||||||
| 著者所属 | Faculty of Natural Sciences, National Institute of Technology, Kure College | |||||
| 著者所属 | ||||||
| 著者所属 | Research Center for the Early Universe, The University of Tokyo | |||||
| 抄録 | ||||||
| 内容記述タイプ | Abstract | |||||
| 内容記述 | We present a positive correlation between the mass of dense molecular gas (Mdense) of ~ 100 pc scale circumnuclear disks (CNDs) and the black hole mass accretion rate (M_ BH) in total 10 Seyfert galaxies, based on data compiled from the literature and an archive (median aperture θmed = 220 pc). A typical Mdense of CNDs is 107-8 M⊙, estimated from the luminosity of the dense gas tracer, the HCN(1 -0) emission line. Because dense molecular gas is the site of star formation, this correlation is virtually equivalent to the one between nuclear star formation rate and M_ BH revealed previously. Moreover, the Mdense -M_ BH correlation was tighter for CND-scale gas than for the gas on kpc or larger scales. This indicates that CNDs likely play an important role in fueling black holes, whereas >kpc scale gas does not. To demonstrate a possible approach for studying the CND-scale accretion process with the Atacama Large Millimeter/submillimeter Array (ALMA), we used a mass accretion model where angular momentum loss due to supernova explosions is vital. Based on the model prediction, we suggest that only the partial fraction of the mass accreted from the CND (M_ acc) is consumed as M_ BH. However, M_ acc agrees well with the total nuclear mass flow rate (i.e., M_ BH + outflow rate). Although these results are still tentative with large uncertainties, they support the view that star formation in CNDs can drive mass accretion onto supermassive black holes in Seyfert galaxies. | |||||
| 内容記述 | ||||||
| 内容記述タイプ | Other | |||||
| 内容記述 | UTokyo Research掲載「銀河中心にある高い密度の分子ガス円盤が超巨大ブラックホールを育てる」 URI: http://www.u-tokyo.ac.jp/ja/utokyo-research/research-news/dense-molecular-gas-disks-drive-the-growth-of-supermassive-black-holes.html | |||||
| 内容記述 | ||||||
| 内容記述タイプ | Other | |||||
| 内容記述 | UTokyo Research "Dense molecular gas disks drive the growth of supermassive black holes" URI: http://www.u-tokyo.ac.jp/en/utokyo-research/research-news/dense-molecular-gas-disks-drive-the-growth-of-supermassive-black-holes.html | |||||
| 書誌情報 |
The Astrophysical Journal Online Edition 巻 827, 号 1, 発行日 2016-08-10 |
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| DOI | ||||||
| 識別子タイプ | DOI | |||||
| 関連識別子 | info:doi/10.3847/0004-637X/827/1/81 | |||||
| 権利 | ||||||
| 権利情報 | © 2016. The American Astronomical Society. All rights reserved. | |||||
| 著者版フラグ | ||||||
| 値 | publisher | |||||
| 出版者 | ||||||
| 出版者 | IOP Publishing | |||||
| 関係URI | ||||||
| 識別子タイプ | URI | |||||
| 関連識別子 | http://www.u-tokyo.ac.jp/ja/utokyo-research/research-news/dense-molecular-gas-disks-drive-the-growth-of-supermassive-black-holes.html | |||||
| 関係URI | ||||||
| 識別子タイプ | URI | |||||
| 関連識別子 | http://www.u-tokyo.ac.jp/en/utokyo-research/research-news/dense-molecular-gas-disks-drive-the-growth-of-supermassive-black-holes.html | |||||
| 異版である | ||||||
| 関連タイプ | isVersionOf | |||||
| 識別子タイプ | URI | |||||
| 関連識別子 | http://dx.doi.org/10.3847/0004-637X/827/1/81 | |||||
