The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey

R. Edelson, J. Gelbord, E. Cackett, B. M. Peterson, K. Horne, A. J. Barth, D. A. Starkey, M. Bentz, William Nielsen Brandt, M. Goad, M. Joner, K. Korista, H. Netzer, K. Page, P. Uttley, S. Vaughan, A. Breeveld, S. B. Cenko, C. Done, P. Evans & 15 others M. Fausnaugh, G. Ferland, D. Gonzalez-Buitrago, J. Gropp, D. Grupe, J. Kaastra, Jamie A. Kennea, G. Kriss, S. Mathur, M. Mehdipour, D. Mudd, John Andrew Nousek, T. Schmidt, M. Vestergaard, C. Villforth

Research output: Contribution to journalArticle

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Abstract

Swift intensive accretion disk reverberation mapping of four AGN yielded light curves sampled ∼200-350 times in 0.3-10 keV X-ray and six UV/optical bands. Uniform reduction and cross-correlation analysis of these data sets yields three main results: (1) The X-ray/UV correlations are much weaker than those within the UV/optical, posing severe problems for the lamp-post reprocessing model in which variations in a central X-ray corona drive and power those in the surrounding accretion disk. (2) The UV/optical interband lags are generally consistent with as predicted by the centrally illuminated thin accretion disk model. While the average interband lags are somewhat larger than predicted, these results alone are not inconsistent with the thin disk model given the large systematic uncertainties involved. (3) The one exception is the U band lags, which are on average a factor of ∼2.2 larger than predicted from the surrounding band data and fits. This excess appears to be due to diffuse continuum emission from the broad-line region (BLR). The precise mixing of disk and BLR components cannot be determined from these data alone. The lags in different AGN appear to scale with mass or luminosity. We also find that there are systematic differences between the uncertainties derived by JAVELIN versus more standard lag measurement techniques, with JAVELIN reporting smaller uncertainties by a factor of 2.5 on average. In order to be conservative only standard techniques were used in the analyses reported herein.

Original languageEnglish (US)
Article number123
JournalAstrophysical Journal
Volume870
Issue number2
DOIs
StatePublished - Jan 10 2019

Fingerprint

reverberation
accretion disks
time lag
accretion
corona
x rays
cross correlation
coronas
light curve
luminaires
luminosity
continuums

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Edelson, R., Gelbord, J., Cackett, E., Peterson, B. M., Horne, K., Barth, A. J., ... Villforth, C. (2019). The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey. Astrophysical Journal, 870(2), [123]. https://doi.org/10.3847/1538-4357/aaf3b4
Edelson, R. ; Gelbord, J. ; Cackett, E. ; Peterson, B. M. ; Horne, K. ; Barth, A. J. ; Starkey, D. A. ; Bentz, M. ; Brandt, William Nielsen ; Goad, M. ; Joner, M. ; Korista, K. ; Netzer, H. ; Page, K. ; Uttley, P. ; Vaughan, S. ; Breeveld, A. ; Cenko, S. B. ; Done, C. ; Evans, P. ; Fausnaugh, M. ; Ferland, G. ; Gonzalez-Buitrago, D. ; Gropp, J. ; Grupe, D. ; Kaastra, J. ; Kennea, Jamie A. ; Kriss, G. ; Mathur, S. ; Mehdipour, M. ; Mudd, D. ; Nousek, John Andrew ; Schmidt, T. ; Vestergaard, M. ; Villforth, C. / The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey. In: Astrophysical Journal. 2019 ; Vol. 870, No. 2.
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abstract = "Swift intensive accretion disk reverberation mapping of four AGN yielded light curves sampled ∼200-350 times in 0.3-10 keV X-ray and six UV/optical bands. Uniform reduction and cross-correlation analysis of these data sets yields three main results: (1) The X-ray/UV correlations are much weaker than those within the UV/optical, posing severe problems for the lamp-post reprocessing model in which variations in a central X-ray corona drive and power those in the surrounding accretion disk. (2) The UV/optical interband lags are generally consistent with as predicted by the centrally illuminated thin accretion disk model. While the average interband lags are somewhat larger than predicted, these results alone are not inconsistent with the thin disk model given the large systematic uncertainties involved. (3) The one exception is the U band lags, which are on average a factor of ∼2.2 larger than predicted from the surrounding band data and fits. This excess appears to be due to diffuse continuum emission from the broad-line region (BLR). The precise mixing of disk and BLR components cannot be determined from these data alone. The lags in different AGN appear to scale with mass or luminosity. We also find that there are systematic differences between the uncertainties derived by JAVELIN versus more standard lag measurement techniques, with JAVELIN reporting smaller uncertainties by a factor of 2.5 on average. In order to be conservative only standard techniques were used in the analyses reported herein.",
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Edelson, R, Gelbord, J, Cackett, E, Peterson, BM, Horne, K, Barth, AJ, Starkey, DA, Bentz, M, Brandt, WN, Goad, M, Joner, M, Korista, K, Netzer, H, Page, K, Uttley, P, Vaughan, S, Breeveld, A, Cenko, SB, Done, C, Evans, P, Fausnaugh, M, Ferland, G, Gonzalez-Buitrago, D, Gropp, J, Grupe, D, Kaastra, J, Kennea, JA, Kriss, G, Mathur, S, Mehdipour, M, Mudd, D, Nousek, JA, Schmidt, T, Vestergaard, M & Villforth, C 2019, 'The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey', Astrophysical Journal, vol. 870, no. 2, 123. https://doi.org/10.3847/1538-4357/aaf3b4

The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey. / Edelson, R.; Gelbord, J.; Cackett, E.; Peterson, B. M.; Horne, K.; Barth, A. J.; Starkey, D. A.; Bentz, M.; Brandt, William Nielsen; Goad, M.; Joner, M.; Korista, K.; Netzer, H.; Page, K.; Uttley, P.; Vaughan, S.; Breeveld, A.; Cenko, S. B.; Done, C.; Evans, P.; Fausnaugh, M.; Ferland, G.; Gonzalez-Buitrago, D.; Gropp, J.; Grupe, D.; Kaastra, J.; Kennea, Jamie A.; Kriss, G.; Mathur, S.; Mehdipour, M.; Mudd, D.; Nousek, John Andrew; Schmidt, T.; Vestergaard, M.; Villforth, C.

In: Astrophysical Journal, Vol. 870, No. 2, 123, 10.01.2019.

Research output: Contribution to journalArticle

TY - JOUR

T1 - The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey

AU - Edelson, R.

AU - Gelbord, J.

AU - Cackett, E.

AU - Peterson, B. M.

AU - Horne, K.

AU - Barth, A. J.

AU - Starkey, D. A.

AU - Bentz, M.

AU - Brandt, William Nielsen

AU - Goad, M.

AU - Joner, M.

AU - Korista, K.

AU - Netzer, H.

AU - Page, K.

AU - Uttley, P.

AU - Vaughan, S.

AU - Breeveld, A.

AU - Cenko, S. B.

AU - Done, C.

AU - Evans, P.

AU - Fausnaugh, M.

AU - Ferland, G.

AU - Gonzalez-Buitrago, D.

AU - Gropp, J.

AU - Grupe, D.

AU - Kaastra, J.

AU - Kennea, Jamie A.

AU - Kriss, G.

AU - Mathur, S.

AU - Mehdipour, M.

AU - Mudd, D.

AU - Nousek, John Andrew

AU - Schmidt, T.

AU - Vestergaard, M.

AU - Villforth, C.

PY - 2019/1/10

Y1 - 2019/1/10

N2 - Swift intensive accretion disk reverberation mapping of four AGN yielded light curves sampled ∼200-350 times in 0.3-10 keV X-ray and six UV/optical bands. Uniform reduction and cross-correlation analysis of these data sets yields three main results: (1) The X-ray/UV correlations are much weaker than those within the UV/optical, posing severe problems for the lamp-post reprocessing model in which variations in a central X-ray corona drive and power those in the surrounding accretion disk. (2) The UV/optical interband lags are generally consistent with as predicted by the centrally illuminated thin accretion disk model. While the average interband lags are somewhat larger than predicted, these results alone are not inconsistent with the thin disk model given the large systematic uncertainties involved. (3) The one exception is the U band lags, which are on average a factor of ∼2.2 larger than predicted from the surrounding band data and fits. This excess appears to be due to diffuse continuum emission from the broad-line region (BLR). The precise mixing of disk and BLR components cannot be determined from these data alone. The lags in different AGN appear to scale with mass or luminosity. We also find that there are systematic differences between the uncertainties derived by JAVELIN versus more standard lag measurement techniques, with JAVELIN reporting smaller uncertainties by a factor of 2.5 on average. In order to be conservative only standard techniques were used in the analyses reported herein.

AB - Swift intensive accretion disk reverberation mapping of four AGN yielded light curves sampled ∼200-350 times in 0.3-10 keV X-ray and six UV/optical bands. Uniform reduction and cross-correlation analysis of these data sets yields three main results: (1) The X-ray/UV correlations are much weaker than those within the UV/optical, posing severe problems for the lamp-post reprocessing model in which variations in a central X-ray corona drive and power those in the surrounding accretion disk. (2) The UV/optical interband lags are generally consistent with as predicted by the centrally illuminated thin accretion disk model. While the average interband lags are somewhat larger than predicted, these results alone are not inconsistent with the thin disk model given the large systematic uncertainties involved. (3) The one exception is the U band lags, which are on average a factor of ∼2.2 larger than predicted from the surrounding band data and fits. This excess appears to be due to diffuse continuum emission from the broad-line region (BLR). The precise mixing of disk and BLR components cannot be determined from these data alone. The lags in different AGN appear to scale with mass or luminosity. We also find that there are systematic differences between the uncertainties derived by JAVELIN versus more standard lag measurement techniques, with JAVELIN reporting smaller uncertainties by a factor of 2.5 on average. In order to be conservative only standard techniques were used in the analyses reported herein.

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Edelson R, Gelbord J, Cackett E, Peterson BM, Horne K, Barth AJ et al. The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey. Astrophysical Journal. 2019 Jan 10;870(2). 123. https://doi.org/10.3847/1538-4357/aaf3b4