The mass of the black hole in Centaurus A from SINFONI AO-assisted integral-field observations of stellar kinematics
The mass of the black hole in Centaurus A from SINFONI AO-assisted integral-field observations of stellar kinematics
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半人马座 A 黑洞的质量，来自 SINFONI AO 辅助的恒星运动学积分场观测
DOI：
10.1111/j.1365-2966.2008.14377.x
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发表时间：
2009
影响因子：
4.8
通讯作者：
Cappellari M
中科院分区：
文献类型：
--
作者：
Cappellari M
利用恒星运动学的高分辨率积分场观测，对椭圆星系Centaurus A（Cen A）（NGC 5128）的超大质量黑洞（BH）的质量和核恒星轨道分布进行了测定.这些观测是用欧洲南方天文台甚大望远镜的近红外线（K波段）SINFONI（近红外线综合场观测摄谱仪）获得的，使用自适应光学（AO）校正地球大气层的模糊效应。该数据的空间分辨率为0.17弧秒半高全宽和高信号噪声比（S/N）≥ 80每光谱像素，使恒星的视线速度分布的形状可以可靠地提取。我们探测到清晰的低水平恒星旋转，这是相对于气体的反向旋转。用轴对称三积分动力学模型拟合数据，得到BH质量的最佳拟合值MBH =（5.5 ± 3.0）× 107 M_（？）（3σ误差）和（M/L）K=（0.65 ± 0.15）太阳单位。这些值与以前从气体运动学中确定的值非常一致，特别是与我们自己发表的从相同数据中提取的值非常一致。这提供了一个最干净的气体与恒星比较的MBH测定，由于使用积分场数据的动力示踪剂和由于一个非常好的解决BH球的影响RBH <$0.70弧秒。我们得到一个准确的配置文件的轨道各向异性，并仔细测试其可靠性使用球形牛仔裤模型与径向变化的各向异性。我们发现，在接近BH的切向各向异性的增加，但这种影响的空间范围似乎仅限于RBH的大小，而不是在表面亮度分布的核心ofRb <$3.9弧秒，与目前的模拟详细预测的二元BH冲刷机制。要从这一观察中得出结论，需要进行更现实的模拟。
We present a determination of the mass of the supermassive black hole (BH) and the nuclear stellar orbital distribution of the elliptical galaxy Centaurus A (Cen A) (NGC 5128) using high-resolution integral-field observations of the stellar kinematics. The observations were obtained with SINFONI (Spectrograph for INtegral Field Observations in the Near Infrared) at the European Southern Observatory Very Large Telescope in the near-infrared (IR) (Kband), using adaptive optics (AO) to correct for the blurring effect of the Earth's atmosphere. The data have a spatial resolution of 0.17 arcsec full width at half-maximum and high signal-to-noise ratios (S/N) ≳ 80 per spectral pixel so that the shape of the stellar line-of-sight velocity distribution can be reliably extracted. We detect clear low-level stellar rotation, which is counter-rotating with respect to the gas. We fit axisymmetric three-integral dynamical models to the data to determine the best-fitting values for the BH massMBH= (5.5 ± 3.0) × 107M⊙(3σ errors) and (M/L)K= (0.65 ± 0.15) in solar units. These values are in excellent agreement with previous determinations from the gas kinematics, and in particular with our own published value, extracted from the same data. This provides one of the cleanest gas versus stars comparisons ofMBHdetermination, due to the use of integral-field data for both dynamical tracers and due to a very well-resolved BH sphere of influenceRBH≈ 0.70 arcsec. We derive an accurate profile of the orbital anisotropy, and carefully test its reliability using spherical Jeans models with radially varying anisotropy. We find an increase in the tangential anisotropy close to the BH, but the spatial extent of this effect seems restricted to the size ofRBHinstead of that ofRb≈ 3.9 arcsec of the core in the surface brightness profile, contrary to detailed predictions of current simulations of the binary BH scouring mechanism. More realistic simulations would be required to draw conclusions from this observation.
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DOI：
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发表时间：
2003
期刊：
影响因子：
--
作者：
Julia Silge;K. Gebhardt
通讯作者：
K. Gebhardt
DOI：
10.1111/j.1365-2966.2008.13754.x
发表时间：
2008-05
影响因子：
4.8
作者：
M. Cappellari
通讯作者：
M. Cappellari
DOI：
10.1111/j.1365-2966.2006.09994.x
发表时间：
2006-02
影响因子：
4.8
作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
通讯作者：
D. Croton;G. Kauffmann;V. Springel;S. White;G. Lucia;A. Jenkins;J. Navarro;C. Frenk;Liang Gao-Lian
星系的轴对称三积分模型：NGC 3379 中的大质量黑洞
DOI：
10.1086/301240
发表时间：
1999
期刊：
The Astronomical Journal
影响因子：
--
作者：
K. Gebhardt;D. Richstone;J. Kormendy;T. Lauer;E. Ajhar;R. Bender;A. Dressler;S. Faber;C. Grillmair;J. Magorrian;S. Tremaine
通讯作者：
S. Tremaine
DOI：
10.1111/j.1365-2966.2008.13960.x
发表时间：
2008-09
影响因子：
4.8
作者：
N. Nowak;R. Saglia;J. Thomas;R. Bender;R. Davies;K. G. M. Garching;Usm Munich;U. Austin
通讯作者：
N. Nowak;R. Saglia;J. Thomas;R. Bender;R. Davies;K. G. M. Garching;Usm Munich;U. Austin