  We investigate the connection between galactic outflows and star formation
using two independent data sets covering a sample of 22 galaxies between $1
\lesssim z \lesssim 1.5$. The HST WFC3/G141 grism provides low spectral
resolution, high spatial resolution spectroscopy yielding H$\alpha$ emission
line maps from which we measure the spatial extent and strength of star
formation. In the rest-frame near-UV, Keck/DEIMOS observes Fe II and Mg II
interstellar absorption lines, which provide constraints on the intensity and
velocity of the outflows. We compare outflow properties from individual and
composite spectra with the star formation rate (SFR) and SFR surface density
(SigmaSFR), as well as the stellar mass and specific star formation rate
(sSFR). The Fe II and Mg II equivalent widths (EWs) increase with both SFR and
SigmaSFR at $\gtrsim 3\sigma$ significance, while the composite spectra show
larger Fe II EWs and outflow velocities in galaxies with higher SFR, SigmaSFR,
and sSFR. Absorption line profiles of the composite spectra further indicate
that the differences between subsamples are driven by outflows rather than the
ISM. While these results are consistent with those of previous studies, the use
of H$\alpha$ images makes them the most direct test of the relationship between
star formation and outflows at $z>1$ to date. Future facilities such as the
James Webb Space Telescope and the upcoming Extremely Large Telescopes will
extend these direct, H$\alpha$-based studies to lower masses and star formation
rates, probing galactic feedback across orders of magnitude in galaxy
properties and augmenting the correlations we find here.
