0 Assigned ID: 1757 ----- Attempting Submission 1 (Fri Mar 01 20:54:45 GMT 2013) ----- Galaxy-scale outflows of gas driven by intense star formation are one of the primary drivers of galactic evolution. These outflows undoubtedly depend on the properties of the galaxies involved; both observations of local systems and theoretical models indicate scalings with mass, star formation rate, and the surface density of star formation, though the details of these relationships are not yet clear. The geometry of galactic outflows also depends on galaxy structure: in the local universe, outflows are observed to be collimated perpendicular to galactic disks, and evidence for such collimation is observed at redshifts up to z~1. In contrast, the ubiquitous outflows seen in galaxies at z~2 appear to be roughly spherical, with no significant dependence on inclination. The apparent increase in the collimation of outflows over the redshift range 1<z<2 coincides with the growth of disks and the development of the Hubble sequence. We propose a combined morphological and spectroscopic analysis of galaxies at 1<z<2, the epoch of disk growth and increased collimation of outflows. Using archival HST ACS imaging and Keck/DEIMOS spectra of absorption and emission lines tracing outflowing gas, we will measure galaxy sizes, star formation rate surface densities, axis ratios and other morphological parameters, and assess correlations between these quantities and spectroscopic diagnostics of outflows. The combined power of HST-based morphological measurements and deep spectra will shed light on the relationship between galactic outflows and galaxy structure, during a key period in the history of galaxy growth. COSMOLOGY Default Medium false false false false false SUPPORTED