Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing
Swift monitoring of NGC 4151 with an similar to 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 angstrom). The three hardest X-ray bands (> 2.5 keV) are all stro...
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ndltd-arizona.edu-oai-arizona.openrepository.com-10150-6243412017-06-25T03:00:33Z Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing 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. Univ Arizona, Steward Observ galaxies: active galaxies: individual (NGC 4151) galaxies: nuclei galaxies: Seyfert Swift monitoring of NGC 4151 with an similar to 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 angstrom). 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 similar to 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 similar to 0.5-1 days. This combination of greater than or similar to 3 day lags between the X-rays and UV and less than or similar to 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. 2017-05-03 Article Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing 2017, 840 (1):41 The Astrophysical Journal 1538-4357 10.3847/1538-4357/aa6890 http://hdl.handle.net/10150/624341 http://arizona.openrepository.com/arizona/handle/10150/624341 The Astrophysical Journal en http://stacks.iop.org/0004-637X/840/i=1/a=41?key=crossref.4593b5fd47ed97abb254e75023ef72f1 © 2017. The American Astronomical Society. All rights reserved. IOP PUBLISHING LTD |
collection |
NDLTD |
language |
en |
sources |
NDLTD |
topic |
galaxies: active galaxies: individual (NGC 4151) galaxies: nuclei galaxies: Seyfert |
spellingShingle |
galaxies: active galaxies: individual (NGC 4151) galaxies: nuclei galaxies: Seyfert 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. Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing |
description |
Swift monitoring of NGC 4151 with an similar to 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 angstrom). 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 similar to 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 similar to 0.5-1 days. This combination of greater than or similar to 3 day lags between the X-rays and UV and less than or similar to 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. |
author2 |
Univ Arizona, Steward Observ |
author_facet |
Univ Arizona, Steward Observ 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. |
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. |
author_sort |
Edelson, R. |
title |
Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing |
title_short |
Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing |
title_full |
Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing |
title_fullStr |
Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing |
title_full_unstemmed |
Swift Monitoring of NGC 4151: Evidence for a Second X-Ray/UV Reprocessing |
title_sort |
swift monitoring of ngc 4151: evidence for a second x-ray/uv reprocessing |
publisher |
IOP PUBLISHING LTD |
publishDate |
2017 |
url |
http://hdl.handle.net/10150/624341 http://arizona.openrepository.com/arizona/handle/10150/624341 |
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