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Swift monitoring of NGC 4151 : evidence for a second X-ray/UV reprocessing

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Date
03/05/2017
Author
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. Dalla
Emmanoulopoulos, D.
Evans, P.
Jaimes, R. Figuera
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.
Funder
Science & Technology Facilities Council
Grant ID
ST/M001296/1
Keywords
Galaxies: active
Galaxies: individual (NGC 4151)
Galaxies: nuclei
Galaxies: Seyfert
QB Astronomy
QC Physics
3rd-DAS
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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.
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
Publication
Astrophysical Journal
Status
Peer reviewed
DOI
https://doi.org/10.3847/1538-4357/aa6890
ISSN
0004-637X
Type
Journal article
Rights
© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at iopscience.iop.org / https://doi.org/10.3847/1538-4357/aa6890
Collections
  • University of St Andrews Research
URI
http://hdl.handle.net/10023/10748

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