  We report the detection of a massive neutral gas outflow in the z=2.09
gravitationally lensed Dusty Star-Forming Galaxy HATLASJ085358.9+015537
(G09v1.40), seen in absorption with the OH+(1_1-1_0) transition using spatially
resolved (0.5"x0.4") Atacama Large Millimeter/submillimeter Array (ALMA)
observations. The blueshifted OH+ line is observed simultaneously with the
CO(9-8) emission line and underlying dust continuum. These data are
complemented by high angular resolution (0.17"x0.13") ALMA observations of
CH+(1-0) and underlying dust continuum, and Keck 2.2 micron imaging tracing the
stellar emission. The neutral outflow, dust, dense molecular gas and stars all
show spatial offsets from each other. The total atomic gas mass of the observed
outflow is 6.7x10^9 M_sun, >25% as massive as the gas mass of the galaxy. We
find that a conical outflow geometry best describes the OH+ kinematics and
morphology and derive deprojected outflow properties as functions of possible
inclination (0.38 deg-64 deg). The neutral gas mass outflow rate is between
83-25400 M_sun/yr, exceeding the star formation rate (788+/-300 M_sun/yr) if
the inclination is >3.6 deg (mass-loading factor = 0.3-4.7). Kinetic energy and
momentum fluxes span 4.4-290x10^9 L_sun and 0.1-3.7x10^37 dyne, respectively
(energy-loading factor = 0.013-16), indicating that the feedback mechanisms
required to drive the outflow depend on the inclination assumed. We derive a
gas depletion time between 29 and 1 Myr, but find that the neutral outflow is
likely to remain bound to the galaxy, unless the inclination is small, and may
be re-accreted if additional feedback processes do not occur.
