Supermassive black hole mass in the massive elliptical galaxy M87 from integral-field stellar dynamics using OASIS and MUSE with adaptive optics: assessing systematic uncertainties
Supermassive black hole mass in the massive elliptical galaxy M87 from integral-field stellar dynamics using OASIS and MUSE with adaptive optics: assessing systematic uncertainties
复制标题
使用 OASIS 和 MUSE 以及自适应光学器件，根据积分场恒星动力学计算大质量椭圆星系 M87 中的超大质量黑洞质量：评估系统不确定性
DOI：
10.1093/mnras/stad3309
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发表时间：
2023
影响因子：
4.8
通讯作者：
J. Hartke
中科院分区：
文献类型：
--
作者：
David A. Simon;M. Cappellari;J. Hartke
大质量椭圆星系 M87 一直是恒星动力学、气体动力学以及最近事件视界望远镜 (EHT) 黑洞阴影等多项超大质量黑洞质量测量的对象。这使得 M87 成为替代黑洞质量测定方法的基准。在这里，我们使用 MUSE 和 OASIS 通过自适应光学 (AO) 从积分场光谱观测中提取的恒星运动学。我们利用高分辨率积分场光谱对恒星的中心活动星系核进行光谱分解。我们得出了准确的内部恒星密度剖面，发现它比之前假设的更平坦。我们还使用光谱提取的 AGN 作为参考来准确确定观测到的 MUSE 和 OASIS AO PSF。然后，我们使用新的灵活的空间可变各向异性进行牛仔裤各向异性建模 (JAM)，并测量各向异性轮廓、恒星质量与光的变化、内部暗物质分数和黑洞质量。我们首选的黑洞质量是 MBH = (8.7 ± 1.2[随机] ± 1.3[系统]) × 109 M⊙。然而，利用之前研究的内部恒星密度，我们发现首选黑洞质量为 $M_{\rm BH} = (5.5^{+0.5}_{-0.3}) \times 10^9 \ M_\odot$，与之前的工作一致。我们发现这是我们的结果与之前的工作之间存在差异的主要原因，此外还有由于运动学和建模方法造成的较小贡献。我们对运动学和模型假设进行了大量的系统测试，得出的结论是，之前确定的 M87 黑洞质量的不确定性可能被低估了，需要进一步分析。
The massive elliptical galaxy M87 has been the subject of several supermassive black hole mass measurements from stellar dynamics, gas dynamics, and recently the black hole shadow by the Event Horizon Telescope (EHT). This uniquely positions M87 as a benchmark for alternative black hole mass determination methods. Here we use stellar kinematics extracted from integral-field spectroscopy observations with Adaptive Optics (AO) using MUSE and OASIS. We exploit our high-resolution integral field spectroscopy to spectrally decompose the central AGN from the stars. We derive an accurate inner stellar-density profile and find it is flatter than previously assumed. We also use the spectrally-extracted AGN as a reference to accurately determine the observed MUSE and OASIS AO PSF. We then perform Jeans Anisotropic Modelling (JAM), with a new flexible spatially-variable anisotropy, and measure the anisotropy profile, stellar mass-to-light variations, inner dark matter fraction, and black hole mass. Our preferred black hole mass is MBH = (8.7 ± 1.2[random] ± 1.3[systematic]) × 109 M⊙. However, using the inner stellar density from previous studies, we find a preferred black hole mass of $M_{\rm BH} = (5.5^{+0.5}_{-0.3}) \times 10^9 \ M_\odot$, consistent with previous work. We find that this is the primary cause of the difference between our results and previous work, in addition to smaller contributions due to kinematics and modelling method. We conduct numerous systematic tests of the kinematics and model assumptions and conclude that uncertainties in the black hole mass of M87 from previous determinations may have been underestimated and further analyses are needed.