Resolving the X-Ray Obscuration in a Low-flux Observation of the Quasar PDS 456

Abstract

Simultaneous XMM-Newton , NuSTAR , and HST observations, performed in 2017 March, of the nearby ( z = 0.184) luminous quasar PDS 456 are presented. PDS 456 had a low X-ray flux compared to past observations, where the first of the two new XMM-Newton observations occurred during a pronounced dip in the X-ray light curve. The broadband X-ray spectrum is highly absorbed, attenuated by a soft X-ray absorber of column density N H = 6 × 10 22 cm -2 . An increase in obscuration occurs during the dip, which may be due to an X-ray eclipse. In addition, the persistent, fast Fe K outflow is present, with velocity components of -0.25 c and -0.4 c . The soft absorber is less ionized ( ##IMG## [http://ej.iop.org/images/0004-637X/867/1/38/apjaae30cieqn1.gif] $\mathrmlog? =3$ ) compared to the iron K outflow ( ##IMG## [http://ej.iop.org/images/0004-637X/867/1/38/apjaae30cieqn2.gif] $\mathrmlog? =5$ ) and is outflowing with a velocity of approximately -0.2 c . A soft X-ray excess is present below 1 keV against the highly absorbed continuum and can be attributed to the re-emission from a wide-angle wind. The complex X-ray absorption present in PDS 456 suggests that the wind is inhomogeneous, whereby the soft X-ray absorber originates from denser clumps or filaments that may form farther out along the outflow. In contrast to the X-ray observations, the simultaneous UV spectrum of PDS 456 is largely unabsorbed, where only a very weak broad absorption trough is present blueward of Ly a , compared to a past observation in 2000 when the trough was significantly stronger. The relative weakness of the UV absorption may be due to the soft X-ray absorber being too highly ionized and almost transparent in the UV band.