Robotic Reverberation Mapping of the Southern Seyfert NGC 3783
Robotic Reverberation Mapping of the Southern Seyfert NGC 3783
复制标题
DOI：
10.3847/1538-4357/abccd4
复制
发表时间：
2021-01-01
影响因子：
4.9
通讯作者：
Valluri, Monica
中科院分区：
文献类型：
--
作者：
Bentz, Misty C.;Street, Rachel;Valluri, Monica
我们介绍了2020年上半年对NGC 3783进行的光谱和光度监测。连续变化和宽的光发射线的响应之间的时间延迟被清楚地检测到，我们报告混响测量H β，他二λ 4686，H γ，和H δ。根据H β宽发射线的时间延迟和光谱可变部分的线宽，我们导出黑洞质量为M。这比以前的测定结果略小，但与以前的测定结果一致。然而，我们显着改进的时间采样（T-med = 1.7天相比，T-med = 4.0天）减少了时间延迟和推导质量的不确定性，约50%。我们还检测到明确的速度分辨的时间延迟在广泛的H β分布，较短的滞后线翼和较长的滞后线的核心。未来对全速度分辨时间延迟响应的建模将进一步改善NGC 3783的基于混响的质量，将其添加到小但不断增长的活动星系核样本中，我们已经限制了黑洞质量以及宽线区域的几何和运动学。即将在甚大望远镜上进行的MUSE观测也将允许NGC 3783加入较小的黑洞样本，在那里可以直接比较混响质量和恒星动力学模型的质量。
We present spectroscopic and photometric monitoring of NGC 3783 conducted throughout the first half of 2020. Time delays between the continuum variations and the response of the broad optical emission lines were clearly detected, and we report reverberation measurements for H beta, He ii lambda 4686, H gamma, and H delta. From the time delay in the broad H beta emission line and the line width in the variable portion of the spectrum, we derive a black hole mass of M. This is slightly smaller than, but consistent with, previous determinations. However, our significantly improved time sampling (T-med = 1.7 days compared to T-med = 4.0 days) has reduced the uncertainties on both the time delay and the derived mass by similar to 50%. We also detect clear velocity-resolved time delays across the broad H beta profile, with shorter lags in the line wings and a longer lag in the line core. Future modeling of the full velocity-resolved time-delay response will further improve the reverberation-based mass for NGC 3783, adding it to the small but growing sample of active galactic nuclei for which we have constrained the black hole mass as well as the geometry and kinematics of the broad-ine region. Upcoming MUSE observations at the Very Large Telescope will also allow NGC 3783 to join the smaller sample of black holes where reverberation masses and masses from stellar dynamical modeling may be directly compared.