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X-ray/UV/optical variability of NGC 4593 with Swift: reprocessing of X-rays by an extended reprocessor

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posted on 01.05.2019, 08:54 by IM McHardy, SD Connolly, K Horne, EM Cackett, J Gelbord, BM Peterson, M Pahari, N Gehrels, M Goad, P Lira, P Arevalo, RD Baldi, N Brandt, E Breedt, H Chand, G Dewangan, C Done, M Elvis, D Emmanoulopoulos, MM Fausnaugh, S Kaspi, CS Kochanek, K Korista, IE Papadakis, AR Rao, P Uttley, M Vestergaard, MJ Ward
We report the results of intensive X-ray, UV, and optical monitoring of the Seyfert 1 galaxy NGC 4593 with Swift. There is no intrinsic flux-related spectral change in any variable component with small apparent variations being due to contamination by a constant hard (reflection) component in the X-rays and the red host galaxy in the UV/optical. Relative to the shortest wavelength band, UVW2, the lags of the other UV/optical bands mostly agree with the predictions of reprocessing of high energy emission by an accretion disc. The U-band lag is, however, larger than expected, probably because of reprocessed Balmer continuum emission from the distant broad line region (BLR). The UVW2 band is well correlated with the X-rays but lags by ∼6× more than expected if the UVW2 results only from reprocessing of X-rays by the disc. However, if the light curves are filtered to remove variations on time-scales >5 d, the lag approaches the expectation from disc reprocessing. MEMECHO analysis shows that direct X-rays can be the driver of most of the UV/optical variations if the response functions have tails up to 10 d, from BLR reprocessing, together with strong peaks at short lag (<1 d) from disc reprocessing. For the 5 AGN monitored so far, the observed UVW2 to V-band lags are < ∼2 of disc reprocessing expectations and vary little between AGN. However, the X-ray to UVW2 lags greatly exceed disc reprocessing expectations and differ between AGN. The two most absorbed AGN have the largest excesses, so absorption and scattering may affect these lags, but there is no simple relationship between excess and absorption.

Funding

IMM acknowledges support from a Royal Society Leverhulme Trust Research Fellowship LT160006 and from Science and Technology Facilities Council (STFC) grant ST/M001326/1. KH acknowledges support from STFC grant ST/M001296/1 and JG acknowledges support from the US National Aeronautics and Space Administration (NASA) under awards NNX15AH49G and 80NSSC17K0126. MV acknowledges financial support from the Danish Council for Independent Research via grant DFF 4002-00275. MP acknowledges support from a Royal Society Science and Engineering Research Board Newton International Fellowship. This work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester.

History

Citation

Monthly Notices of the Royal Astronomical Society, 2018, 480 (3), pp. 2881-2897 (17)

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society

Publisher

Oxford University Press (OUP), Royal Astronomical Society

issn

0035-8711

eissn

1365-2966

Acceptance date

23/07/2018

Copyright date

2018

Available date

01/05/2019

Publisher version

https://academic.oup.com/mnras/article/480/3/2881/5064246

Language

en