Recurring obscuration in NGC 3783

J. S. Kaastra, M. Mehdipour, E. Behar, S. Bianchi, G. Branduardi-Raymont, L. Brenneman, M. Cappi, E. Costantini, B. De Marco, L. Di Gesu, J. Ebrero, G. A. Kriss, J. Mao, U. Peretz, P. O. Petrucci, G. Ponti, D. Walton

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Context. Obscuration of the continuum emission from active galactic nuclei by streams of gas with relatively high velocity (>1000 km s-1) and column density (>3 × 1025 m-2) has been seen in a few Seyfert galaxies. This obscuration has a transient nature. In December 2016 we witnessed such an event in NGC 3783. Aims. The frequency and duration of these obscuration events is poorly known. Here we study archival data of NGC 3783 in order to constrain this duty cycle. Methods. We use archival Chandra/NuSTAR spectra taken in August 2016. We also study the hardness ratio of all Swift XRT spectra taken between 2008 and 2017. Results. In August 2016, NGC 3783 also showed evidence of obscuration. While the column density of the obscuring material is ten times lower than in December 2016, the opacity is still sufficient to block a significant fraction of the ionising X-ray and extreme ultraviolet photons. From the Swift hardness ratio behaviour we find several other epochs with obscuration. Obscuration with columns >1026 m-2 may take place about half of the time. Also, in archival X-ray data taken by the Advanced Satellite for Cosmology and Astrophysics (ASCA) in 1993 and 1996 we find evidence of obscuration. Conclusions. Obscuration of the ionising photons in NGC 3783 occurs more frequently than previously thought. This may not always have been recognised due to low-spectral-resolution observations, overly limited spectral bandwidth or confusion with underlying continuum variations.

Original languageEnglish
Article numberA112
Number of pages9
JournalAstronomy and Astrophysics
Early online date13 Nov 2018
Publication statusPublished - 30 Nov 2018


  • Galaxies: Active
  • Galaxies: Individual: NGC 3783
  • Galaxies: Seyfert
  • Techniques: Spectroscopic
  • X-Rays: Galaxies

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