论文标题
活性银核中具有高积聚速率的超质黑洞。 xi。 MRK 142的积聚磁盘混响映射
Supermassive black holes with high accretion rates in active galactic nuclei. XI. Accretion disk reverberation mapping of Mrk 142
论文作者
论文摘要
我们在2019年初进行了高积聚率Active Galactic Nucleus MRK 142的高积聚磁盘混响映射运动。MRK142在X射线和6个UV/Optical Filters中使用Neil Gehrels Swift Swift天文台进行了4个月的监测。从Las Cumbres天文台，利物浦望远镜和Ugriz过滤器中的Dan Zowada纪念天文台获得地面光度监测，V。MRK142中的Yunnan天文学观测值始终均高度可变，在所有波长中显示出相关的可变性。 We measure significant time lags between the different wavelength light curves, finding that through the UV and optical the wavelength-dependent lags, $τ(λ)$, generally follow the relation $τ(λ) \propto λ^{4/3}$, as expected for the $T\propto R^{-3/4}$ profile of a steady-state optically-thick, geometrically-thin accretion磁盘，虽然也可以通过$τ（λ）\ proptoλ^{2} $拟合，但对于纤毛磁盘的预期。异常是U和U带，在其他AGN中观察到的滞后滞后，并归因于在宽线区域产生的连续发射。此外，我们执行通量升分分析，以分离光谱能分布的常数和可变成分，发现变量成分的通量依赖性与$f_ν\ proptov^{1/3} $ spectrum一致。此外，X射线至紫外线滞后与紫外/光学趋势的外推明显抵消，X射线显示与紫外线的相关性较差，而不是与光学紫外线相比。紫外线/光学滞后的大小与高度超级 - 埃德丁顿积聚率一致。
We performed an intensive accretion disk reverberation mapping campaign on the high accretion rate active galactic nucleus Mrk 142 in early 2019. Mrk 142 was monitored with the Neil Gehrels Swift Observatory for 4 months in X-rays and 6 UV/optical filters. Ground-based photometric monitoring was obtained from the Las Cumbres Observatory, Liverpool Telescope and Dan Zowada Memorial Observatory in ugriz filters and the Yunnan Astronomical Observatory in V. Mrk 142 was highly variable throughout, displaying correlated variability across all wavelengths. We measure significant time lags between the different wavelength light curves, finding that through the UV and optical the wavelength-dependent lags, $τ(λ)$, generally follow the relation $τ(λ) \propto λ^{4/3}$, as expected for the $T\propto R^{-3/4}$ profile of a steady-state optically-thick, geometrically-thin accretion disk, though can also be fit by $τ(λ) \propto λ^{2}$, as expected for a slim disk. The exceptions are the u and U band, where an excess lag is observed, as has been observed in other AGN and attributed to continuum emission arising in the broad-line region. Furthermore, we perform a flux-flux analysis to separate the constant and variable components of the spectral energy distribution, finding that the flux-dependence of the variable component is consistent with the $f_ν\proptoν^{1/3}$ spectrum expected for a geometrically-thin accretion disk. Moreover, the X-ray to UV lag is significantly offset from an extrapolation of the UV/optical trend, with the X-rays showing a poorer correlation with the UV than the UV does with the optical. The magnitude of the UV/optical lags is consistent with a highly super-Eddington accretion rate.
