We present results from an observation of the gravitationally lensed z = 1.51 narrow absorption line AGN HSÂ 0810+2554Â performed with the Chandra X-ray Observatory .
The factor of \sim 100 lensing magnification of HSÂ 0810+2554 makes this source exceptionally bright .
Absorption lines are detected at rest-frame energies of \sim 7.7Â keV and \sim 11.0Â keV at \buildrel \scriptstyle > \over { \scriptstyle \sim } 97 % significance .
By interpreting these lines to arise from highly ionized iron the implied outflow velocities of the X-ray absorbing gas corresponding to these lines are 0.13 c and 0.41 c , respectively .
The presence of these relativistic outflows and the absence of any significant low-energy X-ray absorption suggest that a shielding gas is not required for the generation of the relativistic X-ray absorbing winds in HSÂ 0810+2554 .
UV spectroscopic observations with VLT/UVES indicate that the UV absorbing material is outflowing at v _ { UV } \sim 0.065 c .
Our analysis indicates that the fraction of the total bolometric energy released by HSÂ 0810+2554Â into the IGM in the form of kinetic energy is \epsilon _ { k } = 1.0 _ { -0.6 } ^ { +0.8 } .
An efficiency of greater than unity implies that magnetic driving is likely a significant contributor to the acceleration of this X-ray absorbing wind .
We also estimate the mass-outflow rate of the strongest absorption component to be \dot { M } _ { abs } = 1.1 _ { -0.7 } ^ { +0.9 } M _ { \odot } Â yr ^ { -1 } .
Assuming that the energetic outflow detected in the NAL AGN HSÂ 0810+2554Â is a common property of most AGN it would suggest that the X-ray absorbing wind may have a larger opening angle than previously thought .
This has important consequences for estimating the feedback contribution of X-ray absorbing winds to the surrounding IGM .