ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
ALMA Gas-dynamical Mass Measurement of the Supermassive Black Hole in the Red Nugget Relic Galaxy PGC 11179
复制标题
DOI：
10.3847/1538-4357/ad029d
复制
发表时间：
2023-10
期刊：
影响因子：
--
通讯作者：
J. Cohn;Maeve Curliss;J. Walsh;Kyle M. Kabasares;Benjamin D. Boizelle;A. Barth;Karl Gebhardt;K. Gültekin;A. Yıldırım;D. Buote;J. Darling;Andrew J. Baker;L. C. Ho
中科院分区：
文献类型：
--
作者：
J. Cohn;Maeve Curliss;J. Walsh;Kyle M. Kabasares;Benjamin D. Boizelle;A. Barth;Karl Gebhardt;K. Gültekin;A. Yıldırım;D. Buote;J. Darling;Andrew J. Baker;L. C. Ho
我们介绍了0.“22分辨率的阿塔卡马大型毫米/亚毫米阵列（阿尔马）对红块遗迹星系PGC 11179中环核气体盘CO（2−1）发射的观测结果。该盘显示出规则的旋转，在中心附近的投影速度为400 km s−1。我们假设CO排放源自一个动态冷，薄盘和适合气体动力学模型直接的阿尔马数据。此外，我们通过测试各种模型假设对我们结果的影响来探索系统性不确定性。超大质量黑洞（BH）的质量（M BH）被测量为M BH =（1.91 ± 0.04 [1σ统计] −0.51+0.11 [系统]）× 109 M <$，H波段恒星的质光比M/L H = 1.620 ± 0.004 [1σ统计] −0.107+0.211 [系统] M <$/L <$。这个M BH符合BH质量-恒星速度色散关系，但比BH质量-球核光度关系大3.7倍。PGC 11179是局部致密早期型星系样本的一部分，这些星系可能是z 2红块的遗迹，它的行为与之前用恒星动力学测量的三个遗迹星系BH的标度关系相呼应。这些超大质量的黑洞可能表明黑洞在其宿主星系之前获得了大部分质量。然而，我们的结果也可以通过标度关系的高质量端更大的固有散射，或者通过气体和恒星动力学方法的系统差异来解释。额外的M BH测量样品中，包括分子气体和恒星动力学方法之间的独立交叉检查，将促进我们对BH及其宿主星系的共同演化的理解。
We present 0.″22-resolution Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO(2−1) emission from the circumnuclear gas disk in the red nugget relic galaxy PGC 11179. The disk shows regular rotation, with projected velocities near the center of 400 km s−1. We assume the CO emission originates from a dynamically cold, thin disk and fit gas-dynamical models directly to the ALMA data. In addition, we explore systematic uncertainties by testing the impacts of various model assumptions on our results. The supermassive black hole (BH) mass (M BH) is measured to be M BH = (1.91 ± 0.04 [1σ statistical] −0.51+0.11 [systematic]) × 109 M ⊙, and the H-band stellar mass-to-light ratio M/L H = 1.620 ± 0.004 [1σ statistical] −0.107+0.211 [systematic] M ⊙/L ⊙. This M BH is consistent with the BH mass−stellar velocity dispersion relation but over-massive compared to the BH mass−bulge luminosity relation by a factor of 3.7. PGC 11179 is part of a sample of local compact early-type galaxies that are plausible relics of z ∼ 2 red nuggets, and its behavior relative to the scaling relations echoes that of three relic galaxy BHs previously measured with stellar dynamics. These over-massive BHs could suggest that BHs gain most of their mass before their host galaxies do. However, our results could also be explained by greater intrinsic scatter at the high-mass end of the scaling relations, or by systematic differences in gas- and stellar-dynamical methods. Additional M BH measurements in the sample, including independent cross-checks between molecular gas- and stellar-dynamical methods, will advance our understanding of the co-evolution of BHs and their host galaxies.