  Many theoretical models predict that quasar driven outflows account for the
observed quenching of star formation in massive galaxies. There is growing
observational evidence for quasar-launched massive outflows at z>6, while the
details of outflow-host galaxy interaction remain obscure. In this paper, we
study the feedback around the highest redshift quasar in the BlueTides
simulation, the largest volume cosmological hydrodynamic simulation so far
carried out. We present predictions for gas outflows around the brightest $z =
7.54$ quasar which hosts the most massive black hole in the simulation volume,
which has grown to black hole mass $6.7\times 10^{8}{\rm M}_\odot$ consistent
with the current record holder for high-z quasars. We introduce a method to
identify and trace the gas outflowing from the halo. We find that the total
mass of the outflow gas is about $3.6\times 10^{9}{\rm M}_\odot$, constituting
6\% of the total gas in the halo. The outflow gas contains a cold, dense
molecular component with mass about $2.6\times 10^{8}{\rm M}_\odot$, that
originates from the inner region of the halo, within a few kpc of the central
black hole. The velocities of the outflow gas reach thousands of km/s, within
which the molecular component has mass averaged outward radial velocity of
$1300$ km/s, consistent with observations. The averaged outflow rate is about
$200-300 {\rm M}_\odot/yr$, with the outflowing gas mainly in a hotter ($T \sim
10^7$ K) and lower density state than the average of the host halo gas.
