  The SINFONI survey for Unveiling the Physics and Effect of Radiative feedback
(SUPER) was designed to conduct a blind search for AGN-driven outflows on X-ray
selected AGN at redshift z$\sim$2 with high ($\sim$2 kpc) spatial resolution,
and correlate them to the properties of the host galaxy and central black hole.
The main aims of this paper are: a) to derive reliable estimates for the BH
mass and accretion rates for the Type-1 AGN in this survey; b) to characterize
the properties of the AGN driven winds in the BLR. We analyzed rest-frame
optical and UV spectra of 21 Type-1 AGN. We found that the BH masses estimated
from H$\alpha$ and H$\beta$ lines are in agreement. We estimate BH masses in
the range Log(M$\rm_{BH}/M_{\odot}$)=8.4-10.8 and Eddington ratios
$\rm\lambda_{Edd}$ =0.04-1.3. We confirm that the CIV line width does not
correlate with the Balmer lines and the peak of the line profile is
blue-shifted with respect to the [OIII]-based systemic redshift. These findings
support the idea that the CIV line is tracing outflowing gas in the BLR, with
velocities up to $\sim$4700 km/s. We confirm the strong dependence of the BLR
wind velocity with the UV-to-Xray continuum slope, L$\rm_{Bol}$ and
$\rm\lambda_{Edd}$. We inferred BLR mass outflow rates in the range 0.005-3
M$_{\odot}$/yr, showing a correlation with the bolometric luminosity consistent
with that observed for ionized winds in the NLR and X-ray winds detected in
local AGN, and kinetic power $\sim$10$^{[-7:-4]}\times$ L$\rm_{Bol}$. Finally,
we found an anti-correlation between the equivalent width of the [OIII] line
with respect to the CIV shift, and a positive correlation with [OIII] outflow
velocity. These findings, for the first time in an unbiased sample of AGN at
z$\sim$2, support a scenario where BLR winds are connected to galaxy scale
detected outflows, and are capable of affecting the gas in the NLR located at
kpc scale.
