  We investigate the multi-phase structure of gas flows in galaxies. We study
80 galaxies during the epoch of peak star formation ($1.4\leq z\leq2.7$) using
data from Keck/LRIS and VLT/KMOS. Our analysis provides a simultaneous probe of
outflows using UV emission and absorption features and H$\alpha$ emission. With
this unprecedented data set, we examine the properties of gas flows estimated
from LRIS and KMOS in relation to other galaxy properties, such as star
formation rate (SFR), star formation rate surface density ($\Sigma_{\rm SFR}$),
stellar mass (M$_*$), and main sequence offset ($\Delta$MS). We find no strong
correlations between outflow velocity measured from rest-UV lines and galaxy
properties. However, we find that galaxies with detected outflows show higher
averages in SFR, $\Sigma_{\rm SFR}$, and $\Delta$MS than those lacking outflow
detections, indicating a connection between outflow and galaxy properties.
Furthermore, we find a lower average outflow velocity than previously reported,
suggesting greater absorption at the systemic redshift of the galaxy. Finally,
we detect outflows in 49% of our LRIS sample and 30% in the KMOS sample, and
find no significant correlation between outflow detection and inclination.
These results may indicate that outflows are not collimated and that H$\alpha$
outflows have a lower covering fraction than low-ionization interstellar
absorption lines. Additionally, these tracers may be sensitive to different
physical scales of outflow activity. A larger sample size with a wider dynamic
range in galaxy properties is needed to further test this picture.
