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

TL;DR

This paper predicts the number of high-redshift emission line galaxies for cosmological surveys by combining photometry and spectroscopy, calibrating with existing data, and analyzing their physical properties and evolution.

Contribution

It introduces a new method for estimating emission line galaxy counts using combined photometric and spectroscopic data, calibrated with FMOS-COSMOS survey observations.

Findings

Predicted galaxy counts for various flux thresholds and redshift ranges.

Characterized physical properties of Hα emitters, including stellar mass and size.

Demonstrated the impact of aperture size on flux recovery and detection efficiency.

Abstract

We estimate the number counts of line emitters at high redshift and their evolution with cosmic time based on a combination of photometry and spectroscopy. We predict the H$\alpha$, H$\beta$, [OII], and [OIII] line fluxes for more than $35,000$ galaxies down to stellar masses of $\sim10^9$ $M_{\odot}$ in the COSMOS and GOODS-S fields, applying standard conversions and exploiting 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. We model 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 $0.9<z<1.8$. We show that the observed evolution of the Main Sequence of galaxies with redshift is enough to reproduce the observed counts variation at $0.2<z<2.5$. We characterize 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 aperture of $R\sim R_{\rm e}\sim0.5$" maximizes the signal-to-noise ratio for a detection, while causing a factor of $\sim2\times$ flux losses, influencing the recoverable number counts, if neglected. Our approach, based on deep and large photometric datasets, reduces the uncertainties on the number counts due to the selection and spectroscopic samplings, while exploring low fluxes. We publicly release the line flux predictions for the explored photometric samples.