Galactic Outflows and the Morphology of Star Formation at 1 < z < 1.5

Intense star formation in galaxies results in powerful, galactic-scale outflows of gas. These outflows regulate star formation by heating or expelling gas from the galaxy, but the primary driving mechanisms are still uncertain. We investigate the connection between galactic outflows and the morphology of star formation using two independent data sets covering a sample of galaxies between 1 < z < 1.5. The Wide Field Camera 3 grism on the Hubble Space Telescope (HST) provides low spectral resolution, high spatial resolution spectroscopy yielding Hα emission line maps from which we measure the spatial extent and strength of star formation. In the rest-frame near-UV, the DEep Imaging Multi-Object Spectrograph (DEIMOS) on the Keck II telescope observes Fe II and Mg II absorption lines, which provide constraints on the intensity and velocity of the outflows. We compare the outflow properties with the star formation rate and star formation rate surface density inferred from the Hα emission line maps. The combination of rest-frame UV spectroscopy and Hα mapping at high spatial resolution enables direct comparisons between star forming regions and the outflows they drive, and future facilities such as the James Webb Space Telescope (JWST) and the upcoming Extremely Large Telescopes (ELTs) will extend these studies to lower masses and star formation rates, probing galactic feedback across orders of magnitude in galaxy properties.