XMM-Newton reveals the quasar outflow in PG 1115+080

We report on an observation of the broad absorption line (BAL) quasar PG 1115+ 080 performed with the XMM-Newton observatory. Spectral analysis reveals the second case of a relativistic X- ray-absorbing outflow in a BAL quasar. The first case was revealed in a recent observation of APM 08279+ 5255 with the Chandra X- Ray Observatory. As in the case of APM 08279+ 5255, the observed flux of PG 1115+ 080 is greatly magnified by gravitational lensing. The relatively high redshift (z = 1.72) of the quasar places the redshifted energies of resonant absorption features in a sensitive portion of the XMM-Newton spectral response. The spectrum indicates the presence of complex low-energy absorption in the 0.2 - 0.6 keV observed energy band and high-energy absorption in the 2 - 5 keV observed energy band. The high-energy absorption is best modeled by two Gaussian absorption lines with rest-frame energies of 7.4 and 9.5 keV. Assuming that these two lines are produced by resonant absorption due to Fe xxv Kalpha, we infer that the X- ray absorbers are out. owing with velocities of similar to 0.10c and similar to 0.34c, respectively. We have detected significant variability of the energies and widths of the X- ray BALs in PG 1115+ 080 and APM 08279+ 5255 over timescales of 19 and 1.8 weeks ( proper time), respectively. The BAL variability observed from APM 08279+ 5255 supports our earlier conclusion that these absorbers are most likely launched at relatively small radii of less than or similar to 10(16) (M-bh/M-8)(1/2) cm. A comparison of the ionization properties and column densities of the low-energy and high-energy absorbers indicates that these absorbers are likely distinct; however, higher spectral resolution is needed to confirm this result. Finally, we comment on prospects for constraining the kinematic and ionization properties of these X- ray BALs with the next generation of X- ray observatories.