  The environment of high-redshift galaxies is characterized by both
wind-driven outflowing gas and gravitationally infalling streams. To
investigate such galaxy-IGM interplay we have generated synthetic optical
absorption line spectra piercing the volume surrounding a starbursting analog
of a Lyman Break Galaxy selected in a $z \approx 3$ output from a SPH
simulation, including a detailed treatment of mechanical feedback from winds.
Distributions for several observable species (HI, CIII, CIV, SiII, SiIII, SiIV,
OVI, OVII, and OVIII) have been derived by post-processing the simulation
outputs. The hot wind material is characterized by the presence of
high-ionization species such as OVI, OVII, and OVIII (the latter two observable
only in X-ray bands); the colder ($T<10^{5.5}$ K) infalling streams can be
instead identified by the combined presence of SiII, SiIII, and CIII optical
absorption together with OVI that surrounds the cooler gas clumps. However,
both line profile and Pixel Optical Depth analysis of the synthetic spectra
show that the intergalactic filament in which the wind-blowing galaxy is
embedded produces absorption signatures that closely mimic those of the wind
environment. We conclude that may be difficult to clearly identify wind-blowing
galaxies and their complex gaseous environment at high redshift in optical QSO
absorption-line spectra based solely on the observed ion absorption patterns.
