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We present near-infrared emission line counts and luminosity functions fromthe HST WFC3 Infrared Spectroscopic Parallels (WISP) program for 29 fields(0.037 deg^2) observed using both the G102 and G141 grisms. Altogether weidentify 1048 emission line galaxies with observed equivalent widths greaterthan 40 Angstroms, 467 of which have multiple detected emission lines. The WISPsurvey is sensitive to fainter flux levels (3-5x10^-17 ergs/s/cm^2) than thefuture space near-infrared grism missions aimed at baryonic acousticoscillation cosmology (1-4x10^-16 ergs/s/cm^2), allowing us to probe thefainter emission line galaxies that the shallower future surveys may miss.Cumulative number counts of 0.7<z<1.5 galaxies reach 10,000 deg^-2 above anH-alpha flux of 2x10^-16 ergs/s/cm^2. H-alpha-emitting galaxies with comparable[OIII] flux are roughly 5 times less common than galaxies with just H-alphaemission at those flux levels. Galaxies with low H-alpha/[OIII] ratios are veryrare at the brighter fluxes that future near-infrared grism surveys will probe;our survey finds no galaxies with H-alpha/[OIII] < 0.95 that have H-alpha fluxgreater than 3x10^-16 ergs/s/cm^2. Our H-alpha luminosity function contains acomparable number density of faint line emitters to that found by the NICMOSnear-infrared grism surveys, but significantly fewer (factors of 3-4 less) highluminosity emitters. We also find that our high redshift (z=0.9-1.5) counts arein agreement with the high redshift (z=1.47) narrow band H-alpha survey ofHiZELS (Sobral et al. 2013), while our lower redshift luminosity function(z=0.3-0.9) falls slightly below their z=0.84 result. The evolution in both theH-alpha luminosity function from z=0.3--1.5 and the [OIII] luminosity functionfrom z=0.7-2.3 is almost entirely in the L* parameter, which steadily increaseswith redshift over those ranges.

Predicting Future Space Near-IR Grism Surveys using the WFC3 Infrared Spectroscopic Parallels Survey