2016MNRAS.458.1311M

We present a detailed analysis of a recent, 2013 Suzaku campaign on the nearby (z=0.184) luminous (L_bol ∼ 10⁴⁷ erg/s) quasar PDS 456. This consisted of three observations, covering a total duration of ∼1 Ms and a net exposure of 455 ks. During these observations, the X-ray flux was unusually low, suppressed by a factor of >10 in the soft X-ray band when compared to previous observations. We investigated the broad-band continuum by constructing a spectral energy distribution (SED), making use of the optical/UV photometry and hard X-ray spectra from the later simultaneous XMM-Newton and NuSTAR campaign in 2014. The high-energy part of this low-flux SED cannot be accounted for by physically self-consistent accretion disc and corona models without attenuation by absorbing gas, which partially covers a substantial fraction of the line of sight towards the X-ray continuum. At least two layers of absorbing gas are required, of column density log (N_H,low//cm2)=22.3±0.1 and log (N_H,high//cm2)=23.2±0.1, with average line-of-sight covering factors of ∼80 per cent (with typical ∼5 per cent variations) and 60 per cent (±10-15 per cent), respectively. During these observations PDS 456 displays significant short-term X-ray spectral variability, on time-scales of ∼100 ks, which can be accounted for by variable covering of the absorbing gas along the line of sight. The partial covering absorber prefers an outflow velocity of at the >99.9 per cent confidence level over the case where v_pc=0. This is consistent with the velocity of the highly ionized outflow responsible for the blueshifted iron K absorption profile. We therefore suggest that the partial covering clouds could be the denser, or clumpy part of an inhomogeneous accretion disc wind. Finally estimates are placed upon the size-scale of the X-ray emission region from the source variability. The radial extent of the X-ray emitter is found to be of the order ∼15-20R_g, although the hard X-ray (>2 keV) emission may originate from a more compact or patchy corona of hot electrons, which is typically ∼6-8R_g in size.