A cool accretion disk around the Galactic Centre black hole
A cool accretion disk around the Galactic Centre black hole
复制标题
银河中心黑洞周围的酷吸积盘
作者：
E. Murchikova;E. Murchikova;E. Phinney;A. Pancoast;R. Blandford
在银河系的中心有一个质量为4 × 106太阳质量的超大质量黑洞1，2。一个巨大的热（107开尔文）和冷（102至104开尔文）气体库在几个秒差距内包围着它。尽管X射线观测提供了黑洞吸积区中热气量的限制，即在105史瓦西半径（0.04秒差距）内，但较冷气体的质量不受限制。一种可能的方法是通过氢复合光谱线7，8中的发射来检测这种较冷的气体。在这里，我们报告成像的104开尔文电离气体盘在2 × 104史瓦西半径，使用1.3毫米复合线H30α。这条发射线呈双峰状，全速线宽约为每秒2，200公里。辐射集中在射电源人马座A* 上，但红移的一侧向东北方向移动了0.11弧秒（在8千秒差距处为0.004秒差距），蓝移的一侧向西南方向移动了类似的距离。我们用质量为10 - 5至10 - 4太阳质量的旋转圆盘和平均氢密度约为每立方厘米105至106来解释这些观测结果，这些值对假设的几何形状敏感。考虑到氢的Brγ谱线强度的上限，发射比预期的要强。我们认为脉泽辐射增强了H30α跃迁。1.3毫米氢复合线的辐射揭示了我们银河系中心超大质量黑洞周围半径为0.004秒差距的冷气体旋转盘。
There is a supermassive black hole of mass 4 × 106 solar masses at the centre of the Milky Way1,2. A large reservoir of hot (107 kelvin) and cooler (102 to 104 kelvin) gas surrounds it within a few parsecs3. Although constraints on the amount of hot gas in the accretion zone of the black hole—that is, within 105 Schwarzschild radii (0.04 parsecs)—have been provided by X-ray observations4–6, the mass in cooler gas has been unconstrained. One possible way this cooler gas could be detected is by its emission in hydrogen recombination spectral lines7,8. Here we report imaging of a 104-kelvin ionized gas disk within 2 × 104 Schwarzschild radii, using the 1.3-millimetre recombination line H30α. This emission line is double-peaked, with full velocity linewidth of about 2,200 kilometres per second. The emission is centred on the radio source Sagittarius A*, but the redshifted side is displaced 0.11 arcsec (0.004 parsecs at a distance of 8 kiloparsecs) to the northeast and the blueshifted side is displaced a similar distance to the southwest. We interpret these observations in terms of a rotating disk of mass 10−5 to 10−4 solar masses and mean hydrogen density of about 105 to 106 per cubic centimetre, with the values being sensitive to the assumed geometry. The emission is stronger than expected, given the upper limit on the strength of the Brγ spectral line of hydrogen. We suggest that the H30α transition is enhanced by maser emission. Emission from the 1.3-millimetre hydrogen recombination line reveals a rotating disk of cool gas 0.004 parsecs in radius around the supermassive black hole at the centre of our Galaxy.
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DOI：
10.3847/1538-4357/aace62
发表时间：
2018-06
期刊：
The Astrophysical Journal
影响因子：
--
作者：
G. Witzel;G. Martinez;J. Hora;S. Willner;M. Morris;C. Gammie;E. Becklin;M. Ashby;F. Baganoff
通讯作者：
G. Witzel;G. Martinez;J. Hora;S. Willner;M. Morris;C. Gammie;E. Becklin;M. Ashby;F. Baganoff
DOI：
10.3847/1538-4357/aaf4f8
发表时间：
2018-12
期刊：
The Astrophysical Journal
影响因子：
--
作者：
S. Gillessen;P. Plewa;F. Widmann;S. Fellenberg;M. Schartmann;M. Habibi;A. Rosales;M. Bauböck;J. Dexter;F. Gao;I. Waisberg;F. Eisenhauer;O. Pfuhl;T. Ott;A. Burkert;P. D. Zeeuw;P. D. Zeeuw;R. Genzel;R. Genzel
通讯作者：
S. Gillessen;P. Plewa;F. Widmann;S. Fellenberg;M. Schartmann;M. Habibi;A. Rosales;M. Bauböck;J. Dexter;F. Gao;I. Waisberg;F. Eisenhauer;O. Pfuhl;T. Ott;A. Burkert;P. D. Zeeuw;P. D. Zeeuw;R. Genzel;R. Genzel
DOI：
10.3847/1538-4357/aab3c6
发表时间：
2018-03
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Pancoast;A. Barth;K. Horne;T. Treu;B. Brewer;V. Bennert;G. Canalizo;E. Gates;Weidong Li;M. Malkan;D. Sand;T. Schmidt;S. Valenti;Jong-hak Woo;K. Clubb;M. C. Cooper;S. Crawford;S. Hönig;M. D. Joner;M. Kandrashoff;M. Lazarova;A. Nierenberg;E. Romero-Colmenero;D. Son;E. Tollerud;J. Walsh;H. Winkler
通讯作者：
A. Pancoast;A. Barth;K. Horne;T. Treu;B. Brewer;V. Bennert;G. Canalizo;E. Gates;Weidong Li;M. Malkan;D. Sand;T. Schmidt;S. Valenti;Jong-hak Woo;K. Clubb;M. C. Cooper;S. Crawford;S. Hönig;M. D. Joner;M. Kandrashoff;M. Lazarova;A. Nierenberg;E. Romero-Colmenero;D. Son;E. Tollerud;J. Walsh;H. Winkler
DOI：
10.1088/0004-637x/750/1/58
发表时间：
2012-01
期刊：
The Astrophysical Journal
影响因子：
--
作者：
A. Burkert;M. Schartmann;C. Alig;S. Gillessen;R. Genzel;T. Fritz;F. Eisenhauer
通讯作者：
A. Burkert;M. Schartmann;C. Alig;S. Gillessen;R. Genzel;T. Fritz;F. Eisenhauer