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Upcoming space-based surveys such as Euclid and WFIRST-AFTA plan to measureBaryonic Acoustic Oscillations (BAOs) in order to study dark energy. Thesesurveys will use IR slitless grism spectroscopy to measure redshifts of a largenumber of galaxies over a significant redshift range. In this paper, we use theWFC3 Infrared Spectroscopic Parallel Survey (WISP) to estimate the expectednumber of Halpha (Ha) emitters observable by these future surveys. WISP is anongoing HST slitless spectroscopic survey, covering the 0.8-1.65micronwavelength range and allowing the detection of Ha emitters up to z~1.5 and[OIII] emitters to z~2.3. We derive the Ha-[OIII] bivariate line luminosityfunction for WISP galaxies at z~1 using a maximum likelihood estimator thatproperly accounts for uncertainties in line luminosity measurement, anddemonstrate how it can be used to derive the Ha luminosity function fromexclusively fitting [OIII] data. Using the z~2 [OIII] line luminosity function,and assuming that the relation between Ha and [OIII] luminosity does not changesignificantly over the redshift range, we predict the Ha number counts at z~2 -the upper end of the redshift range of interest for the future surveys. For theredshift range 0.7<z<2, we expect ~3000 galaxies/deg^2 for a flux limit of3x10^{-16} ergs/s/cm^2 (the proposed depth of Euclid galaxy redshift survey)and ~20,000 galaxies/deg^2 for a flux limit of ~10^{-16} ergs/s/cm^2 (thebaseline depth of WFIRST galaxy redshift survey).

Predicting the redshift 2 Halpha luminosity function using [OIII] emission line galaxies