The black hole in NGC 3379: a comparison of gas and stellar dynamical mass measurements with HST and integral‐field data★
The black hole in NGC 3379: a comparison of gas and stellar dynamical mass measurements with HST and integral‐field data★
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NGC 3379 中的黑洞：气体和恒星动力学质量测量与 HST 和积分场数据的比较★
DOI：
10.1111/j.1365-2966.2006.10537.x
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发表时间：
2006
影响因子：
4.8
通讯作者：
T. Statler
中科院分区：
文献类型：
--
作者：
K. Shapiro;M. Cappellari;T. Zeeuw;R. McDermid;K. Gebhardt;R. V. D. Bosch;T. Statler
我们结合了哈勃太空望远镜的光谱和来自SAURON和OASIS仪器的地面积分场数据，研究了附近椭圆星系NGC 3379的中心黑洞。从这些数据中，我们得到了恒星和核气体组分的运动学。恒星运动学的轴对称三积分模型发现一个质量为1.4 +2.6 -1.0 x 10 8 M⊙（3σ误差）的黑洞。这些模型还探测了黑洞附近的速度分布，并揭示了几乎各向同性的速度分布，贯穿整个星系，一直到黑洞的影响球R BH。核气体盘的形态表明它不在赤道平面上；然而NGC 3379的核心几乎是球形的。倾斜的气体薄盘模型发现了一个质量为（2.0±0.1）x 10 8 M⊙（3a误差）的标称黑洞，但该模型与运动学拟合较差。通过在气体运动学中引入扭曲（假设黑洞质量为2.0 x 10 8 M⊙），数据得到了更好的拟合，尽管对这种扰动的性质和形状的限制不足以进行更详细的建模。考虑到气体盘外观的明显规律性，这种强烈的非圆周运动的存在表明，仅用气体动力学方法测量黑洞质量时必须谨慎。
We combine Hubble Space Telescope spectroscopy and ground-based integral-field data from the SAURON and OASIS instruments to study the central black hole in the nearby elliptical galaxy NGC 3379. From these data, we obtain kinematics of both the stars and the nuclear gaseous component. Axisymmetric three-integral models of the stellar kinematics find a black hole of mass 1.4 +2.6 -1.0 x 10 8 M ⊙ (3σ errors). These models also probe the velocity distribution in the immediate vicinity of the black hole and reveal a nearly isotropic velocity distribution throughout the galaxy and down to the black hole sphere of influence R BH . The morphology of the nuclear gas disc suggests that it is not in the equatorial plane; however the core of NGC 3379 is nearly spherical. Inclined thin-disc models of the gas find a nominal black hole of mass (2.0 ± 0.1) x 10 8 M ⊙ (3a errors), but the model is a poor fit to the kinematics. The data are better fit by introducing a twist in the gas kinematics (with the black hole mass assumed to be 2.0 x 10 8 M ⊙ ), although the constraints on the nature and shape of this perturbation are insufficient for more detailed modelling. Given the apparent regularity of the gas disc appearance, the presence of such strong non-circular motion indicates that caution must be used when measuring black hole masses with gas dynamical methods alone.