  We present near-infrared integral field spectroscopy data obtained with
VLT/SINFONI of "the Teacup galaxy". The nuclear K-band (1.95-2.45 micron)
spectrum of this radio-quiet type-2 quasar reveals a blueshifted broad
component of FWHM~1600-1800 km/s in the hydrogen recombination lines
(Pa$\alpha$, Br$\delta$, and Br$\gamma$) and also in the coronal line [Si
VI]$\lambda$1.963 micron. Thus the data confirm the presence of the nuclear
ionized outflow previously detected in the optical and reveal its coronal
counterpart. Both the ionized and coronal nuclear outflows are resolved, with
seeing-deconvolved full widths at half maximum of 1.1$\pm$0.1 and 0.9$\pm$0.1
kpc along PA$\sim$72-74 deg. This orientation is almost coincident with the
radio axis (PA=77 deg), suggesting that the radio jet could have triggered the
nuclear outflow. In the case of the H$_2$ lines we do not require a broad
component to reproduce the profiles, but the narrow lines are blueshifted by
~50 km/s on average from the galaxy systemic velocity. This could be an
indication of the presence of a nuclear molecular outflow, although the bulk of
the H$_2$ emission in the inner ~2 arcsec (~3 kpc) of the galaxy follows a
rotation pattern. We find evidence for kinematically disrupted gas (FWHM>250
km/s) at up to 5.6 kpc from the AGN, which can be naturally explained by the
action of the outflow. The narrow component of [Si VI] is redshifted with
respect to the systemic velocity, unlike any other emission line in the K-band
spectrum. This indicates that the region where the coronal lines are produced
is not co-spatial with the narrow line region.
