Supermassive black holes with high accretion rates in active galactic nuclei. XI. Accretion disk reverberation mapping of Mrk 142

• Published in: arXiv.org 2020-05
• Main Authors: Cackett, Edward M, Gelbord, Jonathan, Yan-Rong, Li, Horne, Keith, Wang, Jian-Min, Barth, Aaron J, Jin-Ming, Bai, Wei-Hao Bian, Carroll, Russell W, Du, Pu, Edelson, Rick, Goad, Michael R, Ho, Luis C, Hu, Chen, Khatu, Viraja C, Luo, Bin, Miller, Jake, Ye-Fei, Yuan
• Format: Article
• Language: English
• Subjects: Accretion disks; Active galactic nuclei; Celestial bodies; Continuum radiation; Emission analysis; Flux; Light curve; Mapping; Observatories; Optical filters; Reverberation; Spectral energy distribution; Supermassive black holes; X-rays
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2005.03685

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, \(\tau(\lambda)\), generally follow the relation \(\tau(\lambda) \propto \lambda^{4/3}\), 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 \(\tau(\lambda) \propto \lambda^{2}\), 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 \(f_\nu\propto\nu^{1/3}\) 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.