Lifting the curtain: The Seyfert galaxy Mrk 335 emerges from deep low-state in a sequence of rapid flare events
Name
aa39098-20.pdf
Description
Published version
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404.37 KB
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Author(s)
Komossa, S
Grupe, D
Gallo, LC
Poulos, P
Blue, D
Kara, E
Kriss, G
Longinotti, AL
Parker, ML
Wilkins, D
Date Issued
2020
Journal
Astronomy and Astrophysics
Publisher
EDP Sciences
Citation
Komossa, S, Grupe, D, Gallo, LC, Poulos, P, Blue, D et al. 2020. "Lifting the curtain: The Seyfert galaxy Mrk 335 emerges from deep low-state in a sequence of rapid flare events." Astronomy and Astrophysics, 643.
Version
Final published version
Abstract
© 2020 S. Komossa et al. Context. The narrow-line Seyfert 1 galaxy Mrk 335 was one of the X-ray brightest active galactic nuclei, but it has systematically faded since 2007. Aims. We report the discovery with Swift of a sequence of bright and rapid X-ray flare events that reveal the emergence of Mrk 335 from its ultra-deep multiyear low state. Methods. Results are based on our dedicated multiyear monitoring of Mrk 335 with Swift. Results. Unlike other bright active galactic nuclei, the optical-UV is generally not correlated with the X-rays in Mrk 335 on a timescale of days to months. This fact either implies the absence of a direct link between the two emission components; or else implies that the observed X-rays are significantly affected by (dust-free) absorption along our line of sight. The UV and optical, however, are closely correlated at the 99.99% confidence level. The UV is leading the optical by Δt = 1.5 ± 1.5 d. The Swift X-ray spectrum shows strong deviations from a single power law in all brightness states of the outbursts, indicating that significant absorption or reprocessing is taking place. Mrk 335 displays a softer-when-brighter variability pattern at intermediate X-ray count rates, which has been seen in our Swift data since 2007 (based on a total of 590 observations). This pattern breaks down at the highest and lowest count rates. Conclusions. We interpret the 2020 brightening of Mrk 335 as a decrease in column density and covering factor of a partial-covering absorber along our line of sight in the form of a clumpy accretion-disk wind that reveals an increasing portion of the intrinsic emission of Mrk 335 from the disk and/or corona region, while the optical emission-line regions receive a less variable spectral energy distribution. This then also explains why Mrk 335 was never seen to change its optical Seyfert type (not "changing look") despite its factor ∼50 X-ray variability with Swift.
MIT Department
MIT Kavli Institute for Astrophysics and Space Research
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Creative Commons Attribution 4.0 International license
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DOI of Published Version
https://doi.org/10.1051/0004-6361/202039098
