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Swift monitoring of NGC 4151 : evidence for a second X-ray/UV reprocessing
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dc.contributor.author | Edelson, R. | |
dc.contributor.author | Gelbord, J. | |
dc.contributor.author | Cackett, E. | |
dc.contributor.author | Connolly, S. | |
dc.contributor.author | Done, C. | |
dc.contributor.author | Fausnaugh, M. | |
dc.contributor.author | Gardner, E. | |
dc.contributor.author | Gehrels, N. | |
dc.contributor.author | Goad, M. | |
dc.contributor.author | Horne, K. | |
dc.contributor.author | McHardy, I. | |
dc.contributor.author | Peterson, B. M. | |
dc.contributor.author | Vaughan, S. | |
dc.contributor.author | Vestergaard, M. | |
dc.contributor.author | Breeveld, A. | |
dc.contributor.author | Barth, A. J. | |
dc.contributor.author | Bentz, M. | |
dc.contributor.author | Bottorff, M. | |
dc.contributor.author | Brandt, W. N. | |
dc.contributor.author | Crawford, S. M. | |
dc.contributor.author | Bonta, E. Dalla | |
dc.contributor.author | Emmanoulopoulos, D. | |
dc.contributor.author | Evans, P. | |
dc.contributor.author | Jaimes, R. Figuera | |
dc.contributor.author | Filippenko, A. V. | |
dc.contributor.author | Ferland, G. | |
dc.contributor.author | Grupe, D. | |
dc.contributor.author | Joner, M. | |
dc.contributor.author | Kennea, J. | |
dc.contributor.author | Korista, K. T. | |
dc.contributor.author | Krimm, H. A. | |
dc.contributor.author | Kriss, G. | |
dc.contributor.author | Leonard, D. C. | |
dc.contributor.author | Mathur, S. | |
dc.contributor.author | Netzer, H. | |
dc.contributor.author | Nousek, J. | |
dc.contributor.author | Page, K. | |
dc.contributor.author | Romero-Colmenero, E. | |
dc.contributor.author | Siegel, M. | |
dc.contributor.author | Starkey, D. A. | |
dc.contributor.author | Treu, T. | |
dc.contributor.author | Vogler, H. A. | |
dc.contributor.author | Winkler, H. | |
dc.contributor.author | Zheng, W. | |
dc.date.accessioned | 2017-05-11T12:30:11Z | |
dc.date.available | 2017-05-11T12:30:11Z | |
dc.date.issued | 2017-05-03 | |
dc.identifier | 249953876 | |
dc.identifier | eabf6bc9-6412-420d-b4ad-efe4d4006e48 | |
dc.identifier | 85019146385 | |
dc.identifier | 000400915200005 | |
dc.identifier.citation | Edelson , R , Gelbord , J , Cackett , E , Connolly , S , Done , C , Fausnaugh , M , Gardner , E , Gehrels , N , Goad , M , Horne , K , McHardy , I , Peterson , B M , Vaughan , S , Vestergaard , M , Breeveld , A , Barth , A J , Bentz , M , Bottorff , M , Brandt , W N , Crawford , S M , Bonta , E D , Emmanoulopoulos , D , Evans , P , Jaimes , R F , Filippenko , A V , Ferland , G , Grupe , D , Joner , M , Kennea , J , Korista , K T , Krimm , H A , Kriss , G , Leonard , D C , Mathur , S , Netzer , H , Nousek , J , Page , K , Romero-Colmenero , E , Siegel , M , Starkey , D A , Treu , T , Vogler , H A , Winkler , H & Zheng , W 2017 , ' Swift monitoring of NGC 4151 : evidence for a second X-ray/UV reprocessing ' , Astrophysical Journal , vol. 840 , no. 1 , 41 . https://doi.org/10.3847/1538-4357/aa6890 | en |
dc.identifier.issn | 0004-637X | |
dc.identifier.other | ArXiv: http://arxiv.org/abs/1703.06901v2 | |
dc.identifier.uri | https://hdl.handle.net/10023/10748 | |
dc.description.abstract | Swift monitoring of NGC 4151 with an ~6 hr sampling over a total of 69 days in early 2016 is used to construct light curves covering five bands in the X-rays (0.3–50 keV) and six in the ultraviolet (UV)/optical (1900–5500 Å). The three hardest X-ray bands (>2.5 keV) are all strongly correlated with no measurable interband lag, while the two softer bands show lower variability and weaker correlations. The UV/optical bands are significantly correlated with the X-rays, lagging ~3–4 days behind the hard X-rays. The variability within the UV/optical bands is also strongly correlated, with the UV appearing to lead the optical by ~0.5–1 days. This combination of ≳ 3 day lags between the X-rays and UV and ≲ 1 day lags within the UV/optical appears to rule out the "lamp-post" reprocessing model in which a hot, X-ray emitting corona directly illuminates the accretion disk, which then reprocesses the energy in the UV/optical. Instead, these results appear consistent with the Gardner & Done picture in which two separate reprocessings occur: first, emission from the corona illuminates an extreme-UV-emitting toroidal component that shields the disk from the corona; this then heats the extreme-UV component, which illuminates the disk and drives its variability. | |
dc.format.extent | 13 | |
dc.format.extent | 796067 | |
dc.language.iso | eng | |
dc.relation.ispartof | Astrophysical Journal | en |
dc.subject | Galaxies: active | en |
dc.subject | Galaxies: individual (NGC 4151) | en |
dc.subject | Galaxies: nuclei | en |
dc.subject | Galaxies: Seyfert | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | 3rd-DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | Swift monitoring of NGC 4151 : evidence for a second X-ray/UV reprocessing | en |
dc.type | Journal article | en |
dc.contributor.sponsor | Science & Technology Facilities Council | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.identifier.doi | 10.3847/1538-4357/aa6890 | |
dc.description.status | Peer reviewed | en |
dc.identifier.grantnumber | ST/M001296/1 | en |
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