arXiv 2104.035392021-04-08astro-ph.GA

用ALMA观测Seyfert 1星系NGC7469中的[ CI ]和CO辐射测量黑洞质量

Black hole mass measurement using ALMA observations of [CI] and CO emissions in the Seyfert 1 galaxy NGC7469

Dieu D. Nguyen, Takuma Izumi, Sabine Thater, Masatoshi Imanishi, Taiki Kawamuro, Shunsuke Baba, Suzuka Nakano, Jean L. Turner, Kotaro Kohno, Satoki Matsushita, … 展开作者

Dieu D. Nguyen, Takuma Izumi, Sabine Thater, Masatoshi Imanishi, Taiki Kawamuro, Shunsuke Baba, Suzuka Nakano, Jean L. Turner, Kotaro Kohno, Satoki Matsushita, Sergio Martin, David S. Meier, Phuong M. Nguyen, Lam T. Nguyen

备注：: 22 pages, 16 figures, 7 tables. Accepted for publication on MNRAS
DOI：: 10.1093/mnras/stab1002

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摘要：

利用阿塔卡玛大型毫米/亚毫米阵列（ALMA）在$\approx0.3$“（或$\approx$ 100 pc）的空间分辨率下观测到的原子- ${\rm [CI]}$（1-0）和分子- $^{12}$ CO（1-0）发射线，测量了Seyfert 1星系NGC 7469中的超大质量黑洞（SMBH）质量.这些排放表明，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，周围环绕着星爆环。CND的$σ/V\approx0.35$（$r\sim0.5$“）和$\sim0.19$（$r>0.5"$）相对较低，表明气体是动态沉降的，适合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${\rm [CI]}$（1-0）运动学产生一个$M_{\rm BH}=1.78^{+2.69}_{-1.10}\times10^7$ M $_\odot$和$M/L_{\rm F547M}=2.25^{+0.40}_{-0.43}$（M $_\odot$ /L $_\odot$）。使用CO（1-0）运动学的模型也给出了具有更大不确定性的一致$M_{\rm BH}$，高达一个数量级，即$M_{\rm BH}=1.60^{+11.52}_{-1.45}\times10^7$ M $_\odot$ .这种新的动态$M_{\rm BH}$是$\approx$ 2倍以上的混响映射（RM）方法使用产生的未解决的宽线区域（BLR）的排放量确定的质量。有了这个新的$M_{\rm BH}$，我们就能够约束NGC 7469中AGN BLR的特定RM无量纲标度因子$f=7.2^{+4.2}_{-3.4}$。因此，在未解决的BLR的气体有一个开普勒维里速度分量和$i\approx11.0^\circ$ $_{-2.5}^{+2.2}$的倾角，确认其面临的塞弗特1 AGN的取向，通过假设一个几何薄的BLR模型。

英文摘要：

We present a supermassive black hole (SMBH) mass measurement in the Seyfert 1 galaxy NGC7469 using Atacama Large Millimeter/submillimeter Array (ALMA) observations of the atomic-${\rm [CI]}$(1-0) and molecular-$^{12}$CO(1-0) emission lines at the spatial resolution of $\approx0.3$" (or $\approx$ 100 pc). These emissions reveal that NGC7469 hosts a circumnuclear gas disc (CND) with a ring-like structure and a two-arm/bi-symmetric spiral pattern within it, surrounded by a starbursting ring. The CND has a relatively low $σ/V\approx0.35$ ($r\sim0.5$") and $\sim0.19$ ($r>0.5"$), 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 ${\rm [CI]}$(1-0) kinematics yields a $M_{\rm BH}=1.78^{+2.69}_{-1.10}\times10^7$M$_\odot$ and $M/L_{\rm F547M}=2.25^{+0.40}_{-0.43}$ (M$_\odot$/L$_\odot$). The model using the CO(1-0) kinematics also gives a consistent $M_{\rm BH}$ with a larger uncertainty, up to an order of magnitude, i.e.\ $M_{\rm BH}=1.60^{+11.52}_{-1.45}\times10^7$M$_\odot$. This newly dynamical $M_{\rm BH}$ is $\approx$ 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 $M_{\rm BH}$, we are able to constrain the specific RM dimensionless scaling factor of $f=7.2^{+4.2}_{-3.4}$ for the AGN BLR in NGC7469. The gas within the unresolved BLR thus has a Keplerian virial velocity component and the inclination of $i\approx11.0^\circ$$_{-2.5}^{+2.2}$, confirming its face-on orientation in a Seyfert 1 AGN by assuming a geometrically thin BLR model.

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