WISDOM Project - III. Molecular gas measurement of the supermassive black hole mass in the barred lenticular galaxy NGC4429
WISDOM Project - III. Molecular gas measurement of the supermassive black hole mass in the barred lenticular galaxy NGC4429
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DOI：
10.1093/mnras/stx2600
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发表时间：
2017-10
影响因子：
4.8
通讯作者：
T. Davis;M. Bureau;K. Onishi;F. Voort;M. Cappellari;S. Iguchi;Lijie Liu;Eve V. North;M. Sarzi;Mark D. Smith
中科院分区：
文献类型：
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作者：
T. Davis;M. Bureau;K. Onishi;F. Voort;M. Cappellari;S. Iguchi;Lijie Liu;Eve V. North;M. Sarzi;Mark D. Smith
作为暗天体质量毫米波干涉测量项目的一部分，我们对附近快速旋转的早型星系NGC 4429中的超大质量黑洞（SMBH）的质量进行了估计，该星系被禁止并具有方形/花生形凸起。这一估计是基于阿塔卡马大型毫米/亚毫米阵列（阿尔马）第2周期对12 CO（3-2）发射线的观测，线性分辨率为1.13 pc（0.18 arcsec × 0.14 arcsec）。NGC 4429有一个松散的，絮状的分子气体核盘，在小半径处被截断，可能是由于气体稳定性和潮汐剪切的综合影响。温暖/致密的12 CO（3-2）气体被限制在这个圆盘的内部，可能是因为气体在更大的半径下变得更稳定，阻止了星星的形成。气盘的低速色散为2.2+0.68−0.65 km s−1。尽管气盘内部被截断，我们还是能够模拟气体的运动学，并估计出NGC 4429中SMBH的质量为（1.5 ± 0.1+0.15−0.35）× 108 M（其中引用的不确定性分别反映了随机和系统的不确定性），与之前使用电离气体运动学设定的上限一致。我们证实，V-波段的质光比的变化范围内的400 pc的NGC 4429，如其他作者建议的百分之30。这SMBH质量测量的基础上分子气体运动学，在文献中提出的第六，再次证明了权力的阿尔马，以约束SMBH质量。
As part of the mm-Wave Interferometric Survey of Dark Object Masses project we present an estimate of the mass of the supermassive black hole (SMBH) in the nearby fast-rotating early-type galaxy NGC4429, that is barred and has a boxy/peanut-shaped bulge. This estimate is based on Atacama Large Millimeter/submillimeter Array (ALMA) cycle-2 observations of the 12CO(3-2) emission line with a linear resolution of ≈13 pc (0.18 arcsec × 0.14 arcsec). NGC4429 has a relaxed, flocculent nuclear disc of molecular gas that is truncated at small radii, likely due to the combined effects of gas stability and tidal shear. The warm/dense 12CO(3-2) emitting gas is confined to the inner parts of this disc, likely again because the gas becomes more stable at larger radii, preventing star formation. The gas disc has a low velocity dispersion of 2.2+0.68−0.65 km s−1. Despite the inner truncation of the gas disc, we are able to model the kinematics of the gas and estimate a mass of (1.5 ± 0.1+0.15−0.35) × 108 M⊙ for the SMBH in NGC4429 (where the quoted uncertainties reflect the random and systematic uncertainties, respectively), consistent with a previous upper limit set using ionized gas kinematics. We confirm that the V-band mass-to-light ratio changes by ≈30 per cent within the inner 400 pc of NGC4429, as suggested by other authors. This SMBH mass measurement based on molecular gas kinematics, the sixth presented in the literature, once again demonstrates the power of ALMA to constrain SMBH masses.