We present results from X-ray observations of the gravitationally lensed z - 1.51 active galactic nucleus (AGN) HS 0810+2554 performed with the Chandra X-ray Observatory and XMM-Newton. Blueshifted absorption lines are detected in both observations at rest-frame energies ranging between similar to 1 and 12 keV at greater than or similar to 99% confidence. The inferred velocities of the outflowing components range between similar to 0.1c and similar to 0.4c. A strong emission line at similar to 6.8 keV that is accompanied by a significant absorption line at similar to 7.8 keV is also detected in the Chandra observation. The presence of these lines is a characteristic feature of a P-Cygni profile supporting the presence of an expanding, outflowing, highly ionized iron absorber in this quasar. Modeling of the P-Cygni profile constrains the covering factor of the wind to be greater than or similar to 0.6, assuming disk shielding. A disk-reflection component is detected in the XMM-Newton observation accompanied by blueshifted absorption lines. The XMM-Newton observation constrains the inclination angle to be <45 degrees at 90% confidence, assuming that the hard excess is due to blurred reflection from the accretion disk. The detection of an ultrafast and wide-angle wind in an AGN with intrinsic narrow absorption lines (NALs) would suggest that quasar winds may couple efficiently with the intergalactic medium and provide significant feedback if ubiquitous in all NAL and broad absorption line (BAL) quasars. We estimate the mass-outflow rate of the absorbers to lie in the range of 1.5-3.4M(circle dot) yr(-1) for the two observations. We find that the fraction of kinetic to electromagnetic luminosity released by HS 0810+2554 is large (epsilon(k) = 9(-6)(+8)), which suggests that magnetic driving is likely a significant contributor to the acceleration of this outflow.
THE WIDE-ANGLE OUTFLOW OF THE LENSED z=1.51 AGN HS 0810+2554
