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dc.contributor.authorEdelson, R.
dc.contributor.authorGelbord, J. M.
dc.contributor.authorHorne, K.
dc.contributor.authorMcHardy, I. M.
dc.contributor.authorPeterson, B. M.
dc.contributor.authorArevalo, P.
dc.contributor.authorBreeveld, A. A.
dc.contributor.authorDe Rosa, G.
dc.contributor.authorEvans, P. A.
dc.contributor.authorGoad, M. R.
dc.contributor.authorKriss, G. A.
dc.contributor.authorBrandt, W. N.
dc.contributor.authorGehrels, N.
dc.contributor.authorGrupe, D.
dc.contributor.authorKennea, J. A.
dc.contributor.authorKochanek, C. S.
dc.contributor.authorNousek, J. A.
dc.contributor.authorPapadakis, I.
dc.contributor.authorSiegel, M.
dc.contributor.authorStarkey, D.
dc.contributor.authorUttley, P.
dc.contributor.authorVaughan, S.
dc.contributor.authorYoung, S.
dc.contributor.authorBarth, A. J.
dc.contributor.authorBentz, M. C.
dc.contributor.authorBrewer, B. J.
dc.contributor.authorCrenshaw, D. M.
dc.contributor.authorDalla Bontà, E.
dc.contributor.authorDe Lorenzo-Caceres, A.
dc.contributor.authorDenney, K. D.
dc.contributor.authorDietrich, M.
dc.contributor.authorEly, J.
dc.contributor.authorFausnaugh, M. M.
dc.contributor.authorGrier, C. J.
dc.contributor.authorHall, P. B.
dc.contributor.authorKaastra, J.
dc.contributor.authorKelly, B. C.
dc.contributor.authorKorista, K. T.
dc.contributor.authorLira, P.
dc.contributor.authorMathur, S.
dc.contributor.authorNetzer, H.
dc.contributor.authorPancoast, A.
dc.contributor.authorPei, L.
dc.contributor.authorPogge, R. W.
dc.contributor.authorSchimoia, J. S.
dc.contributor.authorTreu, T.
dc.contributor.authorVestergaard, M.
dc.contributor.authorVillforth, C.
dc.contributor.authorYan, H.
dc.contributor.authorZu, Y.
dc.date.accessioned2016-06-07T15:30:04Z
dc.date.available2016-06-07T15:30:04Z
dc.date.issued2015-06-12
dc.identifier.citationEdelson , R , Gelbord , J M , Horne , K , McHardy , I M , Peterson , B M , Arevalo , P , Breeveld , A A , De Rosa , G , Evans , P A , Goad , M R , Kriss , G A , Brandt , W N , Gehrels , N , Grupe , D , Kennea , J A , Kochanek , C S , Nousek , J A , Papadakis , I , Siegel , M , Starkey , D , Uttley , P , Vaughan , S , Young , S , Barth , A J , Bentz , M C , Brewer , B J , Crenshaw , D M , Dalla Bontà , E , De Lorenzo-Caceres , A , Denney , K D , Dietrich , M , Ely , J , Fausnaugh , M M , Grier , C J , Hall , P B , Kaastra , J , Kelly , B C , Korista , K T , Lira , P , Mathur , S , Netzer , H , Pancoast , A , Pei , L , Pogge , R W , Schimoia , J S , Treu , T , Vestergaard , M , Villforth , C , Yan , H & Zu , Y 2015 , ' Space Telescope and Optical Reverberation Mapping Project. II. Swift and HST reverberation mapping of the accretion disk of NGC 5548 ' , Astrophysical Journal , vol. 806 , no. 1 , 129 . https://doi.org/10.1088/0004-637X/806/1/129en
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 243133351
dc.identifier.otherPURE UUID: c4a2ae05-164c-4510-bb13-5d3f5dccd7a1
dc.identifier.otherWOS: 000356810300129
dc.identifier.otherScopus: 84935000208
dc.identifier.otherWOS: 000356810300129
dc.identifier.urihttp://hdl.handle.net/10023/8946
dc.description.abstractRecent intensive Swift monitoring of the Seyfert 1 galaxy NGC 5548 yielded 282 usable epochs over 125 days across six UV/optical bands and the X-rays. This is the densest extended active galactic nucleus (AGN) UV/optical continuum sampling ever obtained, with a mean sampling rate <0.5 day. Approximately daily Hubble Space Telescope UV sampling was also obtained. The UV/optical light curves show strong correlations (rmax = 0.57 - 0.90) and the clearest measurement to date of interband lags. These lags are well-fit by τ ∝ λ4/3 a wavelength dependence, with a normalization that indicates an unexpectedly large disk radius of ~0.35 ± 0.05 lt-day at 1367 Å, assuming a simple face-on model. The U band shows a marginally larger lag than expected from the fit and surrounding bands, which could be due to Balmer continuum emission from the broad-line region as suggested by Korista and Goad. The UV/X-ray correlation is weaker (rmax < 0.45) and less consistent over time. This indicates that while Swift is beginning to measure UV/optical lags in general agreement with accretion disk theory (although the derived size is larger than predicted), the relationship with X-ray variability is less well understood. Combining this accretion disk size estimate with those from quasar microlensing studies suggests that AGN disk sizes scale approximately linearly with central black hole mass over a wide range of masses.
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2015. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at: https://dx.doi.org/10.1088/0004-637X/806/1/129en
dc.subjectGalaxies: activeen
dc.subjectGalaxies: individual (NGC 5548)en
dc.subjectGalaxies: nucleien
dc.subjectGalaxies: Seyferten
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subjectBDCen
dc.subjectR2Cen
dc.subject~DC~en
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleSpace Telescope and Optical Reverberation Mapping Project. II. Swift and HST reverberation mapping of the accretion disk of NGC 5548en
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1088/0004-637X/806/1/129
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/M001296/1en


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