Linking the small scale relativistic winds and the large scale molecular
  outflows in the z = 1.51 lensed quasar HS 0810+2554
  We present Atacama Large Millimeter/submillimeter Array (ALMA) observations
of the quadruply lensed z=1.51 quasar HS 0810+2554 which provide useful insight
on the kinematics and morphology of the CO molecular gas and the ~2 mm
continuum emission in the quasar host galaxy. Lens modeling of the mm-continuum
and the spectrally integrated CO(3-2) images indicates that the source of the
mm-continuum has an eccentricity of e~0.9 with a size of ~1.6 kpc and the
source of line emission has an eccentricity of e~0.7 with a size of ~1 kpc. The
spatially integrated emission of the CO(2-1) and CO(3-2) lines shows a triple
peak structure with the outer peaks separated by Dv_21 = 220 +\- 19 km s^-1 and
Dv_32 = 245 +/- 28 km s^-1, respectively, suggesting the presence of rotating
molecular CO line emitting gas. Lensing inversion of the high spatial
resolution images confirms the presence of rotation of the line emitting gas.
Assuming a conversion factor of alpha_CO = 0.8 M_solar (K km s^-1 pc^2)^-1 we
find the molecular gas mass of HS 0810+2554 to be M _ Mol = [(5.2 +/-
1.5)/mu_32] x10^10 M_solar, where mu_32 is the magnification of the CO(3-2)
emission. We report the possible detection, at the 3.0 - 4.7 sigma confidence
level, of shifted CO(3-2) emission lines of high-velocity clumps of CO emission
with velocities up to 1702 km s^-1. We find that the momentum boost of the
large scale molecular wind is below the value predicted for an
energy-conserving outflow given the momentum flux observed in the small scale
ultrafast outflow.
