We present results from three Suzaku observations of the z = 3.91 gravitationally lensed broad absorption line quasar APM 08279+5255 .
We detect strong and broad absorption at rest-frame energies of \lesssim 2 keV ( low-energy ) and 7–12 keV ( high-energy ) .
The detection of these features confirms the results of previous long-exposure ( 80–90 ks ) Chandra and XMM-Newton observations .
The low and high-energy absorption is detected in both the back-illuminated ( BI ) and front-illuminated ( FI ) Suzaku XIS spectra ( with an F -test significance of \gtrsim 99 % ) .
We interpret the low-energy absorption as arising from a low-ionization absorber with log N _ { H } \sim 23 and the high-energy absorption as due to lines arising from highly ionized ( 2.75 \lesssim \hbox { log~ { } $ \xi$ } \lesssim 4.0 ; where \xi is the ionization parameter ) iron in a near-relativistic outflowing wind .
Assuming this interpretation we find that the velocities in the outflow range between 0.1 c and 0.6 c .
We constrain the angle between the outflow direction of the X-ray absorber and our line of sight to be \lesssim 36 ^ { o } .
We also detect likely variability of the absorption lines ( at the \gtrsim 99.9 % and \gtrsim 98 % significance levels in the FI and BI spectra , respectively ) with a rest-frame time scale of \sim 1 month .
Assuming that the detected high-energy absorption features arise from Fe xxv , we estimate that the fraction of the total bolometric energy injected over the quasar ’ s lifetime into the intergalactic medium in the form of kinetic energy to be \gtrsim 10 \% .