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Upcoming missions such as Euclid and the Nancy Grace Roman Space Telescope(Roman) will use emission-line selected galaxies to address a variety ofquestions in cosmology and galaxy evolution in the $z>1$ universe. The optimalobserving strategy for these programs relies upon knowing the number ofgalaxies that will be found and the bias of the galaxy population. Here wemeasure the $\rm{[O\ III]}\ \lambda 5007$ luminosity function for a vettedsample of 1951 $m_{\rm J+JH+H} < 26$ galaxies with unambiguous redshiftsbetween $1.90 < z < 2.35$, which were selected using HST/WFC3 G141 grism framesmade available by the 3D-HST program. These systems are directly analogous tothe galaxies that will be identified by the Euclid and Roman missions, whichwill utilize grism spectroscopy to find $\rm{[O\ III]}\ \lambda 5007$-emittinggalaxies at $0.8 \lesssim z \lesssim 2.7$ and $1.7 \lesssim z \lesssim 2.8$,respectively. We interpret our results in the context of the expected numbercounts for these upcoming missions. Finally, we combine our dust-corrected$\rm{[O\ III]}$ luminosities with rest-frame ultraviolet star formation ratesto present a new calibration of the SFR density associated with $1.90 < z <2.35$ $\rm{[O\ III]}$-emitting galaxies. We find that these grism-selectedgalaxies contain roughly half of the total star formation activity at $z\sim2$.

The $z \sim 2$ $\rm{[O\ III]}$ Luminosity Function of Grism-selected Emission-line Galaxies