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We study large-scale outflows in a sample of 96 star-forming galaxies at1<z<2, using near-UV spectroscopy of FeII and MgII absorption and emission. Theaverage blueshift of the FeII interstellar absorption lines with respect to thesystemic velocity is -85+/-10 km/s at z~1.5, with standard deviation 87 km/s;this is a decrease of a factor of two from the average blueshift measured forfar-UV interstellar absorption lines in similarly selected galaxies at z~2. Theprofiles of the MgII 2796, 2803 lines show much more variety than the FeIIprofiles, which are always seen in absorption; MgII ranges from strong emissionto pure absorption, with emission more common in galaxies with blue UV slopesand at lower stellar masses. Outflow velocities, as traced by the centroids andmaximum extent of the absorption lines, increase with increasing stellar masswith 2-3sigma significance, in agreement with previous results. We study finestructure emission from FeII*, finding several lines of evidence in support ofthe model in which this emission is generated by the re-emission of continuumphotons absorbed in the FeII resonance transitions in outflowing gas. Incontrast, photoionization models indicate that MgII emission arises from theresonant scattering of photons produced in HII regions, accounting for thediffering profiles of the MgII and FeII lines. A comparison of the strengths ofthe FeII absorption and FeII* emission lines indicates that massive galaxieshave more extended outflows and/or greater extinction, while two-dimensionalcomposite spectra indicate that emission from the outflow is stronger at aradius of ~10 kpc in high mass galaxies than in low mass galaxies.

Galactic Outflows in Absorption and Emission: Near-UV Spectroscopy of Galaxies at 1