Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations
Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations
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DOI：
10.1051/0004-6361/201834808
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发表时间：
2019-02
影响因子：
6.5
通讯作者：
S. Thater;D. Krajnović;M. Cappellari;T. Davis;P. T. de Zeeuw;R. McDermid;M. Sarzi
中科院分区：
文献类型：
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作者：
S. Thater;D. Krajnović;M. Cappellari;T. Davis;P. T. de Zeeuw;R. McDermid;M. Sarzi
不同的大质量黑洞质量-宿主星系标度关系表明，大质量黑洞的生长与其宿主星系的演化纠缠在一起。测量到的黑洞质量的数量仍然有限，需要额外的测量来理解这种明显的共同进化的基本物理学。我们在已知的黑洞质量样本中增加了6个新的快速旋转早型星系的黑洞质量（MBH）测量值，即NGC 584，NGC 2784，NGC 3640，NGC 4570，NGC 4281和NGC 7049。我们的目标星系的有效速度色散（σe）在170和245 km s−1之间，因此这项工作为中等质量早型星系的黑洞性质提供了额外的见解。我们结合高分辨率自适应光学SINFONI数据与大规模的MUSE，VIMOS和SAURON数据从ATLAS 3D推导出二维恒星运动学地图。然后，我们建立了Jeans各向异性模型和轴对称史瓦西模型来测量中心黑洞质量。我们的史瓦西模型提供了黑洞质量NGC 584为（1.3 ± 0.5）× 108 M Ω，NGC 2784为（1.0 ± 0.6）× 108 M Ω，NGC 3640为（7.7 ± 5）× 107 M Ω，NGC 4281为（5.4 ± 0.8）× 108 M ~（-1），在3σ置信水平下，NGC 4570和NGC 7049分别为（6.8 ± 2.0）× 107和（3.2 ± 0.8）× 108 M质量，与最近的MBH−σe标度关系一致。NGC 3640有一个速度色散倾角，NGC 7049在中心有一个恒定的速度色散，但我们可以清楚地限制它们的黑洞质量下限。最后，我们对NGC 4570进行了测试，在构建动力学模型时考虑了可变的质光比（M/L）。当考虑M/L变化主要与恒星金属丰度的径向变化有关时，我们发现NGC 4570动态确定的黑洞质量减少了30%。未来需要进一步的研究来解释径向M/L梯度对动力学建模的影响。
Different massive black hole mass – host galaxy scaling relations suggest that the growth of massive black holes is entangled with the evolution of their host galaxies. The number of measured black hole masses is still limited and additional measurements are necessary to understand the underlying physics of this apparent coevolution. We add six new black hole mass (MBH) measurements of nearby fast rotating early-type galaxies to the known black hole mass sample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281, and NGC 7049. Our target galaxies have effective velocity dispersions (σe) between 170 and 245 km s−1, and thus this work provides additional insight into the black hole properties of intermediate-mass early-type galaxies. We combined high-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS and SAURON data from ATLAS3D to derive two-dimensional stellar kinematics maps. We then built both Jeans Anisotropic Models and axisymmetric Schwarzschild models to measure the central black hole masses. Our Schwarzschild models provide black hole masses of (1.3 ± 0.5) × 108 M⊙ for NGC 584, (1.0 ± 0.6) × 108 M⊙ for NGC 2784, (7.7 ± 5) × 107 M⊙ for NGC 3640, (5.4 ± 0.8) × 108 M⊙ for NGC 4281, (6.8 ± 2.0) × 107 M⊙ for NGC 4570, and (3.2 ± 0.8) × 108 M⊙ for NGC 7049 at 3σ confidence level, which are consistent with recent MBH−σe scaling relations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constant velocity dispersion in the center, but we can clearly constrain their lower black hole mass limit. We conclude our analysis with a test on NGC 4570 taking into account a variable mass-to-light ratio (M/L) when constructing dynamical models. When considering M/L variations linked mostly to radial changes in the stellar metallicity, we find that the dynamically determined black hole mass from NGC 4570 decreases by 30%. Further investigations are needed in the future to account for the impact of radial M/L gradients on dynamical modeling.