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 \ion He1 1.083 \mu m emission line with a pronounced P Cygni profile was observed .
From the blue edge of this feature , we infer an outflow velocity of 250 \pm 50 km s ^ { -1 } .
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 \sim 10 ^ { -6 } M _ { \odot } yr ^ { -1 } .
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 \ion H1 Pa \beta and \ion He1 1.083 \mu m emission lines showed no evidence for the dramatic variability previously reported in some optical lines , and no evidence for pulsations at the 2-min pulsar period .