  We present infrared spectroscopy of the low-mass X-ray binary GX 1+4/V2116
Oph. This symbiotic binary consists of a 2-min accretion-powered pulsar and an
M5 III red giant. A strong He I 1.083 micron emission line with a pronounced P
Cygni profile was observed. From the blue edge of this feature, we infer an
outflow velocity of 250(50) km/s. This is an order of magnitude faster than a
typical red giant wind, and we suggest that radiation from the accretion disk
or the neutron star may contribute to the acceleration of the outflow. We infer
a wind mass loss rate of around 10^-6 Msun/yr. Accretion from such a strong
stellar wind provides a plausible alternative to Roche lobe overflow for
supplying the accretion disk which powers the X-ray source. The H I Paschen
beta and He I 1.083 micron lines showed no evidence for the dramatic changes
previously reported in some optical lines, and no evidence for pulsations at
the 2-min pulsar period.
