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We report on a study of the 2300-2600\AA FeII/FeII* multiplets in the rest-UVspectra of star-forming galaxies at 1.0<z<2.6 as probes of galactic-scaleoutflows. We extracted a mass-limited sample of 97 galaxies at z~1.0-2.6 fromultra-deep spectra obtained during the GMASS spetroscopic survey in the GOODSSouth field with the VLT and FORS2. We obtain robust measures of the restequivalent width of the FeII absorption lines down to a limit of W_r>1.5 \AAand of the FeII* emission lines to W_r>0.5 \AA. Whenever we can measure thesystemic redshift of the galaxies from the [OII] emission line, we find thatboth the FeII and MgII absorption lines are blueshifted, indicative that bothspecies trace gaseous outflows. We also find, however, that the FeII gas hasgenerally lower outflow velocity relative to that of MgII. We investigate thevariation of FeII line profiles as a function of the radiative transferproperties of the lines, and find that transitions with higher oscillatorstrengths are more blueshifted in terms of both line centroids and line wings.We discuss the possibility that FeII lines are suppressed by stellarabsorptions. The lower velocities of the FeII lines relative to the MgIIdoublet, as well as the absence of spatially extended FeII* emission in 2Dstacked spectra, suggest that most clouds responsible for the FeII absorptionlie close (3~4 kpc) to the disks of galaxies. We show that the FeII/FeII*multiplets offer unique probes of the kinematic structure of galactic outflows.

Probing Outflows in z= 1~2 Galaxies through FeII/FeII* Multiplets