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The evolution of the OII, H\beta and OIII emission-line luminosity functions

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(2016)cite arxiv:1605.02875Comment: 11 pages. Submitted to MNRAS. Data available at http://projects.ift.uam-csic.es/skies-universes/ via the page emission line luminosity functions.

Abstract

Emission-line galaxies (ELGs) are one of the main tracers of the large-scale structure to be targeted by the next-generation dark energy surveys. To provide a better understanding of the properties and statistics of these galaxies, we have collected spectroscopic data from the VVDS and DEEP2 deep surveys and estimated the galaxy luminosity functions (LFs) of three distinct emission lines, OII, H$\beta$ and OIII at redshifts ($0.2 < z < 1.3$). Our measurements are based on the largest sample so far. We present the first measurement of the \Hb LF at these redshifts. We have also compiled LFs from the literature that were based on independent data or covered different redshift ranges, and we fit the entire set over the whole redshift range with analytic Schechter and Saunders models, assuming a natural redshift dependence of the parameters. We find that the characteristic luminosity ($L_*$) and density ($\phi_*$) of all LFs increase with redshift. Using the Schechter model, we find that $L^*$ of OII emitters increase by a factor 12 between redshift 0.2 and 1.3, that $L^*$ of OIII emitters increase by a factor 16 between redshift 0.3 and 1 and that $L^*$ of H$\beta$ emitters increase by a factor 13 between redshift 0.3 and 0.8.

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