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Outflows from active galactic nuclei (AGN) are often invoked to explain theco-evolution of AGN and their host galaxies, and the scaling relations betweenthe central black hole mass and the bulge velocity dispersion. Nuclear windsare often seen in the X-ray spectra through Fe K shell transitions and some ofthem are called ultra fast outflows (UFOs) due to their high velocities, up tosome fractions of the speed of light. If they were able to transfer somepercentage of the AGN luminosity to the host galaxy, this might be enough totrigger an efficient feedback mechanism. We aim to establish new constraints onthe covering fraction and on the kinematic properties of the UFO in thepowerful (L(bol) ~ 10^(47) erg/s) quasar PDS 456, an established Rosetta stonefor studying AGN feedback from disk winds. This will allow us to estimate themass outflow rate and the energy transfer rate of the wind, which are keyquantities to understand the potential impact on the host galaxy. We analyzetwo sets of simultaneous XMM-Newton and NuSTAR observations taken in September2013 and reported in Nardini et al. (2015) as having similar broadband spectralproperties. We fit the Fe K features with a P-Cygni profile between 5 and 14keV, using a novel Monte Carlo model for the WINd Emission (WINE). We find anoutflow velocity ranging from 0.17 to 0.28 c, with a mean value of 0.23 c. Weobtain an opening angle of the wind of 71(+13,-8) deg and a covering fractionof 0.7(+0.2,-0.3), suggesting a wide-angle outflow. We check the reliability ofthe WINE model by performing extensive simulations of joint XMM-Newton andNuSTAR observations. Furthermore, we test the accuracy of the WINE model inrecovering the geometrical properties of UFOs by simulating observations withthe forthcoming X-ray observatory ATHENA.

Constraining the geometry of the nuclear wind in PDS 456 using a novel emission model