A multi-wavelength study of a massive, active galaxy at $z\sim 2$:
  coupling the kinematics of the ionized and molecular gas
  We report a multi-wavelength study of the massive ($M_{\star} \gtrsim 10^{11}
\rm{M}_{\odot}$), $z\sim 2$ star-forming galaxy GMASS 0953, which hosts an
obscured AGN. We combined near-infrared observations of the GNIRS, SINFONI and
KMOS spectrographs to study the kinematics of the [O III]$\lambda 5007$ and
H$\alpha$ emission lines. Our analysis shows that GMASS 0953 may host an
ionized disc extending up to 13 kpc, which rotates at a velocity of
$V_{\rm{ion}} = 203^{+17}_{-20} {\ \rm kms}^{-1}$ at the outermost radius.
Evidence of rotation on a smaller scale ($R \sim 1$ kpc) arises from the
CO(J=6-5) line. The central velocity $V_{\rm{CO}} = 320^{+ 92}_{-53} {\ \rm
kms}^{-1}$ traced by the molecular gas is higher than $V_{\rm{ion}}$,
suggesting that the galaxy harbors a multi-phase disc with a rotation curve
that peaks in the very central regions. The galaxy appears well located on the
$z = 0$ baryonic Tully-Fisher relation. We also discuss the possibility that
the [O III]$\lambda 5007$ and H$\alpha$ velocity gradients are due to a
galactic-scale wind. Besides, we found evidence of an AGN-driven outflow traced
by a broad blueshifted wing affecting the [O III]$\lambda 5007$ line, which
presents a velocity offset $\Delta v = -535 \pm 152 {\ \rm kms}^{-1}$ from the
systemic velocity. Because of the short depletion timescale
($\tau_{\rm{dep}}\sim 10^8$ yr) due to gas ejection and gas consumption by star
formation activity, GMASS 0953 may likely evolve into a passive galaxy.
However, the role of the AGN in depleting the gas reservoir of the galaxy is
quite unclear because of the uncertainties affecting the outflow rate.
