AGN STORM 2. V. Anomalous Behavior of the C iv Light Curve of Mrk 817*
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Published:2024-03-01
Issue:2
Volume:963
Page:123
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ISSN:0004-637X
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Container-title:The Astrophysical Journal
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language:
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Short-container-title:ApJ
Author:
Homayouni Y.ORCID, Kriss Gerard A.ORCID, De Rosa GisellaORCID, Plesha RachelORCID, Cackett Edward M.ORCID, Goad Michael R.ORCID, Korista Kirk T.ORCID, Horne KeithORCID, Fischer TravisORCID, Waters TimORCID, Barth Aaron J.ORCID, Kara Erin A.ORCID, Landt HermineORCID, Arav NahumORCID, Boizelle Benjamin D.ORCID, Bentz Misty C.ORCID, Brotherton Michael S.ORCID, Chelouche DoronORCID, Dalla Bontà ElenaORCID, Dehghanian MaryamORCID, Du PuORCID, Ferland Gary J.ORCID, Fian CarinaORCID, Gelbord JonathanORCID, Grier Catherine J.ORCID, Hall Patrick B.ORCID, Hu Chen, Ilić DraganaORCID, Joner Michael D.ORCID, Kaastra JelleORCID, Kaspi ShaiORCID, Kovačević Andjelka B.ORCID, Kynoch DanielORCID, Li Yan-RongORCID, Mehdipour MissaghORCID, Miller Jake A.ORCID, Mitchell Jake, Montano JohnORCID, Netzer HagaiORCID, Neustadt J. M. M.ORCID, Partington EthanORCID, Popović Luka Č.ORCID, Proga DanielORCID, Storchi-Bergmann ThaisaORCID, Sanmartim DavidORCID, Siebert Matthew R.ORCID, Treu TommasoORCID, Vestergaard MarianneORCID, Wang Jian-MinORCID, Ward Martin J.ORCID, Zaidouni FatimaORCID, Zu YingORCID
Abstract
Abstract
An intensive reverberation mapping campaign of the Seyfert 1 galaxy Mrk 817 using the Cosmic Origins Spectrograph on the Hubble Space Telescope revealed significant variations in the response of broad UV emission lines to fluctuations in the continuum emission. The response of the prominent UV emission lines changes over an ∼60 day duration, resulting in distinctly different time lags in the various segments of the light curve over the 14 month observing campaign. One-dimensional echo-mapping models fit these variations if a slowly varying background is included for each emission line. These variations are more evident in the C iv light curve, which is the line least affected by intrinsic absorption in Mrk 817 and least blended with neighboring emission lines. We identify five temporal windows with a distinct emission-line response, and measure their corresponding time delays, which range from 2 to 13 days. These temporal windows are plausibly linked to changes in the UV and X-ray obscuration occurring during these same intervals. The shortest time lags occur during periods with diminishing obscuration, whereas the longest lags occur during periods with rising obscuration. We propose that the obscuring outflow shields the broad UV lines from the ionizing continuum. The resulting change in the spectral energy distribution of the ionizing continuum, as seen by clouds at a range of distances from the nucleus, is responsible for the changes in the line response.
Publisher
American Astronomical Society
Cited by
3 articles.
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