The Properties and Prevalence of Galactic Outflows at z = 1 in the
  Extended Groth Strip
  We investigate galactic-scale outflowing winds in 72 star-forming galaxies at
z~1 in the Extended Groth Strip. Galaxies were selected from the DEEP2 survey
and follow-up LRIS spectroscopy was obtained covering SiII, CIV, FeII, MgII,
and MgI lines in the rest-frame ultraviolet. Using GALEX, HST, and Spitzer
imaging, we examine galaxies on a per-object basis in order to understand both
the prevalence of galactic winds at z~1 and the star-forming and structural
properties of objects experiencing outflows. Gas velocities, measured from the
centroids of FeII interstellar absorption lines, span the interval [-217, +155]
km/s. We find that ~40% (10%) of the sample exhibits blueshifted FeII lines at
the 1-sigma (3-sigma) level. We also measure maximal outflow velocities using
the profiles of the FeII and MgII lines, and show that MgII frequently traces
higher velocity gas than FeII. Quantitative morphological parameters derived
from the HST imaging suggest 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. Using star-formation rates calculated from GALEX data, and
areas estimated from HST imaging, we detect a ~3-sigma correlation between
outflow velocity and star-formation rate surface density, but only a weak
(~1-sigma) 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.
