The Black Hole Mass of NGC 4151 from Stellar Dynamical Modeling
The Black Hole Mass of NGC 4151 from Stellar Dynamical Modeling
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DOI：
10.3847/1538-4357/ac05b6
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发表时间：
2021-06
期刊：
影响因子：
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通讯作者：
C. Roberts;M. Bentz;E. Vasiliev;M. Valluri;C. Onken
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作者：
C. Roberts;M. Bentz;E. Vasiliev;M. Valluri;C. Onken
超大质量黑洞的质量是一个可以通过观测方法获得的基本性质。对于单个星系，通过多种方法约束M-BH对于验证不同技术的精确度和研究每种方法所固有的假设都很重要。然而，只有少数几个星系可以应用多种M-BH测量技术。NGC4151是这样一个罕见的星系，它可以使用多种方法：由于它的邻近(来自造父变星的D=15.8±0.4MPC)而进行的恒星和气体动力学模拟，以及由于它的主动吸积而产生的混响映射。在这项工作中，我们重新分析了来自Gemini NIF的NGC 4151原子核的H带积分场光谱，在几个关键步骤上改进了分析。然后，我们用新的轨道叠加程序Forstand建立了广泛的轴对称动力学模型。我们的主要目标之一是量化由出射密度分布、倾角、固有扁平化和质量光比的不同组合引起的M BH的系统不确定性。由于活动星系核的存在对恒星光度分布产生了不确定性，我们对M-BH的约束相当弱。具有陡峭中心尖点的模型与没有黑洞的模型是一致的；但是，在具有较中等尖点的模型中，黑洞质量位于0.25×107M⊙≲M BH≲3×107M⊙的范围内。这一衡量标准比Onken等人早先提出的分析略小。但与以前的气体动力学模型和混响映射得到的MBH值一致。未来对混响数据的动力学建模，以及JWST的IFU观测，将有助于进一步限制NGC4151中中心超大质量黑洞的质量。
The mass of a supermassive black hole (M BH) is a fundamental property that can be obtained through observational methods. Constraining M BH through multiple methods for an individual galaxy is important for verifying the accuracy of different techniques and for investigating the assumptions inherent in each method. However, there exist only a few galaxies where multiple M BH measurement techniques can be applied. NGC 4151 is one of these rare galaxies for which multiple methods can be used: stellar and gas dynamical modeling because of its proximity (D = 15.8 ± 0.4 Mpc from Cepheids), and reverberation mapping because of its active accretion. In this work, we reanalyzed H-band integral field spectroscopy of the nucleus of NGC 4151 from Gemini NIFS, improving the analysis at several key steps. We then constructed a wide range of axisymmetric dynamical models with the new orbit-superposition code Forstand. One of our primary goals is to quantify the systematic uncertainties in M BH arising from different combinations of the deprojected density profile, inclination, intrinsic flattening, and mass-to-light ratio. As a consequence of uncertainties on the stellar luminosity profile arising from the presence of the active galactic nucleus, our constraints on M BH are rather weak. Models with a steep central cusp are consistent with no black hole; however, in models with more moderate cusps, the black hole mass lies within the range of 0.25 × 107 M ⊙ ≲ M BH ≲ 3 × 107 M ⊙. This measurement is somewhat smaller than the earlier analysis presented by Onken et al. but agrees with previous M BH values from gas dynamical modeling and reverberation mapping. Future dynamical modeling of reverberation data, as well as IFU observations with JWST, will aid in further constraining the mass of the central supermassive black hole in NGC 4151.