Cappi, M; Marco, BD; Ponti, G; Ursini, F; Petrucci, P-O; Bianchi, S; Kaastra, JS; ... Walton, DJ; + view all Cappi, M; Marco, BD; Ponti, G; Ursini, F; Petrucci, P-O; Bianchi, S; Kaastra, JS; Kriss, GA; Mehdipour, M; Whewell, M; Arav, N; Behar, E; Boissay, R; Branduardi-Raymont, G; Costantini, E; Ebrero, J; Gesu, LD; Harrison, FA; Kaspi, S; Matt, G; Paltani, S; Peterson, BM; Steenbrugge, KC; Walton, DJ; - view fewer (2016) Anatomy of the AGN in NGC 5548 VIII. XMM-Newton's EPIC detailed view of an unexpected variable multilayer absorber. Astronomy and Astrophysics , 592 , Article A27. 10.1051/0004-6361/201628464.

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Abstract

In 2013 we conducted a large multi-wavelength campaign on the archetypical Seyfert 1 galaxy NGC 5548. Unexpectedly, this usually unobscured source appeared strongly absorbed in the soft X-rays during the entire campaign, and signatures of new and strong outflows were present in the almost simultaneous UV HST/COS data. Here we carry out a comprehensive spectral analysis of all available XMM-Newton observations of NGC 5548 (for a total of ~763 ks) in combination with 3 simultaneous NuSTAR obs. We obtain a best-fit composed by i) a weakly varying flat (Gamma~1.5-1.7) power-law component; ii) a constant, cold reflection (FeK + continuum) component; iii) a soft excess, possibly due to thermal Comptonization; and iv) a constant, ionized scattered emission-line dominated component. Our main findings are that, during the 2013 campaign, the first 3 of these components appear to be partially covered by a heavy and variable obscurer located along the l.o.s. that is consistent with a multilayer of cold and mildly ionized gas. We characterize in detail the short timescale (~ks-to-days) spectral variability of this new obscurer, and find it is mostly due to a combination of Nh and Cf variations, on top of intrinsic power-law variations. In addition, our best-fit spectrum is left with several (but marginal) absorption features at rest-frame energies ~6.7-6.9 keV and ~8 keV, as well as a weak broad emission line feature redwards of the 6.4 keV emission line. These could indicate a more complex underlying model, e.g. a P-Cygni-type profile if allowing for a large velocity and wide-angle outflow. These findings are consistent with a picture where the obscurer represents the manifestation along the l.o.s. of a multilayer of gas that is likely outflowing at high speed, and simultaneously producing heavy obscuration and scattering in the X-rays and broad absorption features in the UV.

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