A fast ionised wind in a Star Forming-Quasar system at z~1.5 resolved
  through Adaptive Optics assisted near-infrared data
  Outflows are invoked in co-evolutionary models to link the growth of SMBH and
galaxies through feedback phenomena, and from the analysis of both galaxies and
Active Galactic Nuclei (AGN) samples at z$\sim1-3$, it is becoming clear that
powerful winds are quite common in AGN hosts. High-resolution and high S/N
observations are needed in order to uncover the physical properties of the wind
through kinematics analysis. We exploited VIMOS, SINFONI and Subaru/IRCS
Adaptive Optics data to study the kinematics properties on the scale the host
galaxy of XID5395, a luminous, X-ray obscured Starburst/Quasar merging system
at z$\sim1.5$ detected in the XMM-COSMOS field, and associated with an extreme
[O II] emitter (EW$\sim200$ \AA). We mapped, for the first time, at high
resolution the kinematics of the [O III] and H$\alpha$ line complexes and
linked them with the [O II] emission. The high spatial resolution achieved
allowed us to resolve all the components of the SB-QSO system. Our analysis
with a resolution of few kpc reveals complexities and asymmetries in and around
the nucleus of XID5395. The velocity field measured via non parametric analysis
reveals different kinematic components, with maximum blueshifted and redshifted
velocities up to $\simeq1300$ km s$^{-1}$, not spatially coincident with the
nuclear core. These extreme values of the observed velocities and the spatial
location can be explained by the presence of fast moving material. We also
spectroscopically confirm the presence of a merging system at the same redshift
of the AGN host. We propose that EW as large as $>150$ \AA\ in X-ray selected
AGN may be an efficient criterion to isolate objects associated to the short,
transition phase of "feedback" in the AGN-galaxy co-evolutionary path, which
will subsequently evolve in an unobscured QSO, as suggested from the different
observational evidences we accumulated for XID5395.
