We investigate galactic-scale outflowing winds in 72 star-forming galaxies at z \sim 1 in the Extended Groth Strip .
Galaxies were selected from the DEEP2 survey and follow-up LRIS spectroscopy was obtained covering Si II , C IV , Fe II , Mg II , and Mg I lines in the rest-frame ultraviolet .
Using GALEX , HST , and Spitzer imaging available for the Extended Groth Strip , we examine galaxies on a per-object basis in order to better understand both the prevalence of galactic outflows at z \sim 1 and the star-forming and structural properties of objects experiencing outflows .
Gas velocities , measured from the centroids of Fe II interstellar absorption lines , are found to span the interval [ –217 , +155 ] km s ^ { -1 } .
We find that \sim 40 % ( 10 % ) of the sample exhibits blueshifted Fe II lines at the 1 \sigma ( 3 \sigma ) level .
We also measure maximal outflow velocities using the profiles of the Fe II and Mg II lines ; we find that Mg II frequently traces higher velocity gas than Fe II .
Using quantitative morphological parameters derived from the HST imaging , we find that mergers are not a prerequisite for driving outflows .
More face-on galaxies also show stronger winds than highly inclined systems , consistent with the canonical picture of winds emanating perpendicular to galactic disks .
In light of clumpy galaxy morphologies , we develop a new physically-motivated technique for estimating areas corresponding to star formation .
We use these area measurements in tandem with GALEX -derived star-formation rates to calculate star-formation rate surface densities .
At least 70 % of the sample exceeds a star-formation rate surface density of 0.1 M _ { \odot } yr ^ { -1 } kpc ^ { -2 } , the threshold necessary for driving an outflow in local starbursts .
At the same time , the outflow detection fraction of only 40 % in Fe II absorption provides further evidence for an outflow geometry that is not spherically symmetric .
We see a \sim 3 \sigma trend between outflow velocity and star-formation rate surface density , but no significant trend between outflow velocity and star-formation rate .
Higher resolution data are needed in order to test the scaling relations between outflow velocity and both star-formation rate and star-formation rate surface density predicted by theory .