半人马座A的中心秒差距：高激发气体、分子盘和黑洞的质量
The central parsecs of Centaurus A: High Excitation Gas, a Molecular Disk, and the Mass of the Black Hole
摘要：
我们提出了半人马座A中心区域的二维气体运动学图。VLT的自适应光学（AO）辅助SINFONI数据在K波段的分辨率为0.12”。电离气体物种（Br_gamma，[Fe II]，[SiVI]）显示出旋转模式，该模式越来越多地被Cen A射电喷流方向上的更高激发线的非旋转运动所覆盖。氢分子（H_2）的发射谱线显示出规则的旋转，没有因喷流而产生畸变。分子气体似乎在恒星和中心超大质量黑洞的引力势中得到了很好的解决，因此我们用它作为示踪剂来模拟中心+/-1.5”的质量。这是第一个AO积分场观测的核心岑A，使我们能够研究的规律性的旋转周围的黑洞，以及内半径的影响，并确定倾斜角的气体盘在一个强大的方式。气体运动学最好通过描述翘曲气体盘的倾斜环模型来建模;其平均倾角为~ 34度，长轴的平均位置角为~ 155度。最适合的黑洞质量是M_BH~4.5x10^7 Msolar，这是基于一个“运动学热”盘模型，其中速度色散通过Jeans方程包含在内。这个黑洞的质量估计值比以前从电离气体运动学中得出的质量值要低一些，但与之一致。这也是一致的恒星动力学测量从相同的AO观测，我们在一个单独的文件。这使Cen A与M_BH-σ关系式一致。
英文摘要：
We present two-dimensional gas-kinematic maps of the central region in Centaurus A. The adaptive optics (AO) assisted SINFONI data from the VLT have a resolution of 0.12" in K-band. The ionized gas species (Br_gamma, [FeII], [SiVI]) show a rotational pattern that is increasingly overlaid by non-rotational motion for higher excitation lines in direction of Cen A's radio jet. The emission lines of molecular hydrogen (H_2) show regular rotation and no distortion due to the jet. The molecular gas seems to be well settled in the gravitational potential of the stars and the central supermassive black hole and we thus use it as a tracer to model the mass in the central +/-1.5". These are the first AO integral-field observations on the nucleus of Cen A, enabling us to study the regularity of the rotation around the black hole, well inside the radius of influence, and to determine the inclination angle of the gas disk in a robust way. The gas kinematics are best modeled through a tilted-ring model that describes the warped gas disk; its mean inclination angle is ~34deg and the mean position angle of the major axis is ~155deg. The best-fit black hole mass is M_BH~4.5x10^7 Msolar, based on a "kinematically hot" disk model where the velocity dispersion is included through the Jeans equation. This black hole mass estimate is somewhat lower than, but consistent with the mass values previously derived from ionized gas kinematics. It is also consistent with the stellar dynamical measurement from the same AO observations, which we present in a separate paper. It brings Cen A in agreement with the M_BH-sigma relation.
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