Black hole mass measurement using ALMA observations of [CI] and CO emissions in the Seyfert 1 galaxy NGC 7469
Black hole mass measurement using ALMA observations of [CI] and CO emissions in the Seyfert 1 galaxy NGC 7469
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DOI：
10.1093/mnras/stab1002
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发表时间：
2021-04
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通讯作者：
Dieu D. Nguyen;T. Izumi;S. Thater;M. Imanishi;T. Kawamuro;S. Baba;Suzuka Nakano;J. Turner;K. Kohno;S. Matsushita;S. Martín;D. Meier;P. M. Nguyen;L. Nguyen
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作者：
Dieu D. Nguyen;T. Izumi;S. Thater;M. Imanishi;T. Kawamuro;S. Baba;Suzuka Nakano;J. Turner;K. Kohno;S. Matsushita;S. Martín;D. Meier;P. M. Nguyen;L. Nguyen
利用阿塔卡马大型毫米/亚毫米波阵列（阿尔马）在空间分辨率为1000的条件下观测了Seyfert 1星系NGC 7469中的原子-[CI]（1-0）和分子-12 CO（1-0）发射谱线，测量了该星系中的超大质量黑洞（SMBH）的质量. '' 3（或≈ 100个）。这些辐射揭示了NGC 7469拥有一个环核气盘（CND），具有环状结构和双臂/双对称螺旋图案，被星爆环包围。CND具有较低的σgas/V = 0.35（r . 0.′′5）和r = 0.19（r > 0.”5），这表明气体是动态沉降的，适合于动态推导其中心源的质量。正如预期的X射线主导区（XDR）效应，显着增加原子碳丰度的解离CO分子，我们建议原子[CI]（1-0）发射是一个更好的探针SMBH质量比CO发射活动星系核。我们的动力学模型使用[CI]（1-0）运动学得出MBH = 1.78+2.69 −1.10 × 10 7 M和M/LF 547 M = 2.25+0.40 −0.43（M /L）。使用12 CO（1-0）运动学的模型也给出了一个一致的MBH，其不确定性更大，达到一个数量级，即MBH = 1.60+11.52 −1.45 × 10 7 M。这个新的动态MBH是从混响映射（RM）方法使用在未解析的宽线区域（BLR）中产生的发射确定的质量的1.22倍。有了这个新的MBH，我们就能够将NGC 7469中AGN BLR的RM无量纲标度因子f = 7.2+4.2 −3.4限制在一定范围内。因此，未解析的BLR中的气体具有开普勒维里速度分量和i <$11.0 <$+2.2 −2.5的倾角，通过假设几何薄的BLR模型，证实了它在Seyfert 1 AGN中的面对面取向。
We present a supermassive black hole (SMBH) mass measurement in the Seyfert 1 galaxy NGC 7469 using Atacama LargeMillimeter/submillimeter Array (ALMA) observations of the atomic-[CI](1-0) and molecular-12CO(1-0) emission lines at the spatial resolution of ≈ 0. ′′3 (or ≈ 100 pc). These emissions reveal that NGC 7469 hosts a circumnuclear gas disc (CND) with a ring-like structure and a two-arm/bisymmetric spiral pattern within it, surrounded by a starbursting ring. The CND has a relatively low σgas/V ≈ 0.35 (r . 0. ′′5) and≈ 0.19 (r > 0. ′′5), suggesting that the gas is dynamically settled and suitable for dynamically deriving the mass of its central source. As is expected from X-ray dominated region (XDR) effects that dramatically increase an atomic carbon abundance by dissociating CO molecules, we suggest that the atomic [CI](1-0) emission is a better probe of SMBH masses than CO emission in AGNs. Our dynamical model using the [CI](1-0) kinematics yields a MBH = 1.78+2.69 −1.10 × 10 7 M and M/LF547M = 2.25+0.40 −0.43 (M /L ). The model using the 12CO(1-0) kinematics also gives a consistent MBH with a larger uncertainty, up to an order of magnitude, i.e. MBH = 1.60+11.52 −1.45 × 10 7 M . This newly dynamical MBH is ≈ 2 times higher than the mass determined from the reverberation mapped (RM) method using emissions arising in the unresolved broad-line region (BLR). Given this new MBH, we are able to constrain the specific RM dimensionless scaling factor of f = 7.2+4.2 −3.4 for the AGN BLR in NGC 7469. The gas within the unresolved BLR thus has a Keplerian virial velocity component and the inclination of i ≈ 11.0◦+2.2 −2.5, confirming its face-on orientation in a Seyfert 1 AGN by assuming a geometrically thin BLR model.