J/ApJ/896/1ivo://CDS.VizieR/J/ApJ/896/1doi:10.26093/cds/vizier.18960001CDSCackett E.M.Gelbord J.Li Y.-R.Horne K.Wang J.-M.Barth A.J.,Bai J.-M.Bian W.-H.Carroll R.W.Du P.Edelson R.Goad M.R.Ho L.C.,Hu C.Khatu V.C.Luo B.Miller J.Yuan Y.-F.2026-05-12T20:05:18Z2021-05-26T09:27:55ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.fractive-galactic-nucleix-ray-sourcesinfrared-photometryvisible-astronomybroad-band-photometryultraviolet-photometryWe performed an intensive accretion disk reverberation mapping campaign on the high accretion rate active galactic nucleus Mrk142 in early 2019. Mrk 142 was monitored with the Neil Gehrels Swift Observatory for four months in X-rays and six different UV/optical filters. Ground-based photometric monitoring was obtained from the Las Cumbres Observatory, the Liverpool Telescope, and the Dan Zowada Memorial Observatory in ugriz filters, as well as from 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 lightcurves. In the UV and optical, we find that 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 they can also be fit by {tau}({lambda}){propto}{lambda}^2^, as expected for a slim disk. The exceptions are the u and U bands, where an excess lag is observed, as has been observed in other active galactic nuclei 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.2020ApJ...896....1Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/896/1CatalogResearchIsServedByTAP VizieR generic servicerelated-toI/345 : Gaia DR2 (Gaia Collaboration, 2018)J/ApJ/613/682 : AGN central masses & broad-line region sizes (Peterson+, 2004)J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)J/ApJ/782/45 : SEAMBHs. I. Mrk 142, Mrk 335, and IRAS F12397+3333 (Du+, 2014)J/ApJ/806/22 : SEAMBHs IV. H{beta} time lags (Du+, 2015)J/ApJ/806/129 : Space telescope RM project. II. Swift data (Edelson+, 2015)J/ApJ/825/126 : SEAMBHs. V. The third year (Du+, 2016)J/ApJ/821/56 : HST RM project. III. NGC 5548 LCs (Fausnaugh+, 2016)J/ApJ/840/41 : X-ray/UV Swift monitoring of NGC 4151 (Edelson+, 2017)J/ApJ/856/6 : SEAMBHs IX. 10 new H{beta} light curves (Du+, 2018)J/ApJ/870/123 : Swift optical & UV flux of four AGNs (Edelson+, 2019)J/ApJ/877/23 : SEAMBHs. X. RM campaign compilation (Lu+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/896/1https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/896/1http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/896/1https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/896/1https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/896/1http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/896/1GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapX-rayUVOpticalInfrareddefaultJ/ApJ/896/1/table2Mrk 142 lightcurvesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJD[58413.934/58655.583] Modified Julian Datedtime.epochdoubleFiltFilter namemeta.id;instr.filtercharFlux[0.025/9.1] Fluxphot.flux.densityfloate_Flux[0.002/0.5] Uncertainty in Fluxstat.error;phot.fluxfloatTelTelescope identifier (1)meta.id;instr.telcharx_FluxFlux units (2)meta.unit;phot.fluxchar