The evolution of the [O II], H beta and [O III] emission line luminosity functions over the last nine billions years

Emission line galaxies 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, [O II] (lambda lambda 3726, 3729) (0.5 < z < 1.3), H beta (lambda 4861) (0.3 < z < 0.8) and [O III] (lambda 5007) (0.3 < z < 0.8). Our measurements are based on 35 639 emission line galaxies and cover a volume of similar to 10(7) Mpc(3). We present the first measurement of the H beta 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 over the redshift ranges considered, we find that, for [O II] emitters, the characteristic luminosity L-*(z = 0.5) = 3.2 x 10(41) erg s(-1) increases by a factor of 2.7 +/- 0.2 from z = 0.5 to 1.3; for H beta emitters L-*(z = 0.3) = 1.3 x 10(41) erg s(-1) increases by a factor of 2.0 +/- 0.2 from z = 0.3 to 0.8; and for [O III] emitters L-*(z = 0.3) = 7.3 x 10(41) erg s(-1) increases by a factor of 3.5 +/- 0.4 from z = 0.3 to 0.8.

Published in:
Monthly Notices Of The Royal Astronomical Society, 461, 1, 1076-1087
Oxford, Oxford Univ Press

 Record created 2016-10-18, last modified 2018-03-17

Rate this document:

Rate this document:
(Not yet reviewed)