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We estimate the number counts of line emitters at high redshift and theirevolution with cosmic time based on a combination of photometry andspectroscopy. We predict the H$\alpha$, H$\beta$, [OII], and [OIII] line fluxesfor more than $35,000$ galaxies down to stellar masses of $\sim10^9$$M_{\odot}$ in the COSMOS and GOODS-S fields, applying standard conversions andexploiting the spectroscopic coverage of the FMOS-COSMOS survey at $z\sim1.55$to calibrate the predictions. We calculate the number counts of H$\alpha$,[OII], and [OIII] emitters down to fluxes of $1\times10^{-17}$ erg cm$^{-2}$s$^{-1}$ in the range $1.4 < z < 1.8$ covered by the FMOS-COSMOS survey. Wemodel the time evolution of the differential and cumulative H$\alpha$ counts,steeply declining at the brightest fluxes. We expect $\sim9,300-9,700$ and$\sim2,300-2,900$ galaxies deg$^{-2}$ for fluxes $\geq1\times10^{-16}$ and$\geq2\times10^{-16}$ erg cm$^{-2}$ s$^{-1}$ over the range $0.9<z<1.8$. Weshow that the observed evolution of the Main Sequence of galaxies with redshiftis enough to reproduce the observed counts variation at $0.2<z<2.5$. Wecharacterize the physical properties of the H$\alpha$ emitters with fluxes$\geq2\times10^{-16}$ erg cm$^{-2}$ s$^{-1}$, including their stellar masses,UV sizes, [NII]/H$\alpha$ ratios, and H$\alpha$ equivalent widths. An apertureof $R\sim R_{\rm e}\sim0.5$" maximizes the signal-to-noise ratio for adetection, while causing a factor of $\sim2\times$ flux losses, influencing therecoverable number counts, if neglected. Our approach, based on deep and largephotometric datasets, reduces the uncertainties on the number counts due to theselection and spectroscopic samplings, while exploring low fluxes. We publiclyrelease the line flux predictions for the explored photometric samples.

Predicting emission line fluxes and number counts of distant galaxies for cosmological surveys