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.
Users
Please
log in to take part in the discussion (add own reviews or comments).