%0 Generic %1 valentino2017predicting %A Valentino, F. %A Daddi, E. %A Silverman, J. D. %A Puglisi, A. %A Kashino, D. %A Renzini, A. %A Cimatti, A. %A Pozzetti, L. %A Rodighiero, G. %A Pannella, M. %A Gobat, R. %A Zamorani, G. %D 2017 %K counts fluxes galaxies line number %T Predicting emission line fluxes and number counts of distant galaxies for cosmological surveys %U http://arxiv.org/abs/1709.01936 %X 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 $\sim10^9$ $M_ødot$ 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 $RR_e\sim0.5$" 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.

@misc{valentino2017predicting, 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.}, added-at = {2017-09-08T10:15:54.000+0200}, author = {Valentino, F. and Daddi, E. and Silverman, J. D. and Puglisi, A. and Kashino, D. and Renzini, A. and Cimatti, A. and Pozzetti, L. and Rodighiero, G. and Pannella, M. and Gobat, R. and Zamorani, G.}, biburl = {https://www.bibsonomy.org/bibtex/2a684c92f4d7d2ee4b1be99a951b715b1/miki}, description = {[1709.01936] Predicting emission line fluxes and number counts of distant galaxies for cosmological surveys}, interhash = {585e1822866ff8b71577798c2ce4ab1e}, intrahash = {a684c92f4d7d2ee4b1be99a951b715b1}, keywords = {counts fluxes galaxies line number}, note = {cite arxiv:1709.01936Comment: Accepted for publication in MNRAS. 21 pages (+9 pages of appendix), 18 Figures. Machine readable tables will be available online}, timestamp = {2017-09-08T10:15:54.000+0200}, title = {Predicting emission line fluxes and number counts of distant galaxies for cosmological surveys}, url = {http://arxiv.org/abs/1709.01936}, year = 2017 }