The Mass of the Black Hole in NGC 5273 from Stellar Dynamical Modeling
The Mass of the Black Hole in NGC 5273 from Stellar Dynamical Modeling
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DOI：
10.3847/1538-4357/acc4bc
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发表时间：
2022-12
期刊：
影响因子：
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通讯作者：
Katie A. Merrell;E. Vasiliev;M. Bentz;M. Valluri;C. Onken
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作者：
Katie A. Merrell;E. Vasiliev;M. Bentz;M. Valluri;C. Onken
我们对活跃S 0星系NGC 5273中黑洞的质量提出了新的约束。由于星系的距离为16.6 ± 2.1 Mpc，我们能够使用双子座近红外积分场光谱仪的自适应光学辅助观测来解析和提取中央黑洞附近恒星的整体运动，以及使用存档的光谱面积单位研究和光学星云光谱学来限制大尺度运动学。高分辨率的哈勃太空望远镜成像使我们能够生成表面亮度分解，确定凸起和圆盘的近似质光比，并获得圆盘倾角的估计。我们使用史瓦西轨道叠加代码FORSTAND构建了一个广泛的动力学模型库，探索了一系列的盘和凸起形状，晕质量等。我们确定了一个黑洞质量M · = [0.5-2] × 107 M <$，其中范围的低端与混响映射测量M · = [4.7 ± 1.6] × 106 M <$一致。NGC 5273是为数不多的拥有宽线活动星系核的邻近星系之一，允许通过独立的质量测量技术对黑洞质量进行重要的比较。
We present a new constraint on the mass of the black hole in the active S0 galaxy NGC 5273. Due to the proximity of the galaxy at 16.6 ± 2.1 Mpc, we were able to resolve and extract the bulk motions of stars near the central black hole using adaptive-optics-assisted observations with the Gemini Near-infrared Integral Field Spectrograph, as well as constrain the large-scale kinematics using archival Spectroscopic Areal Unit for Research and Optical Nebulae spectroscopy. High-resolution Hubble Space Telescope imaging allowed us to generate a surface-brightness decomposition, determine approximate mass-to-light ratios for the bulge and disk, and obtain an estimate for the disk inclination. We constructed an extensive library of dynamical models using the Schwarzschild orbit-superposition code FORSTAND, exploring a range of disk and bulge shapes, halo masses, etc. We determined a black hole mass of M • = [0.5–2] × 107 M ⊙, where the low side of the range is in agreement with the reverberation mapping measurement of M • = [4.7 ± 1.6] × 106 M ⊙. NGC 5273 is one of the few nearby galaxies that hosts a broad-lined active galactic nucleus, allowing a crucial comparison of black hole masses derived from independent mass-measurement techniques.