The evolution of the [OII], H{\beta} and [OIII] 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, [OII] ($0.5 < z < 1.3$), H{\beta} ($0.3 < z < 0.8$) and [OIII] ($0.3 < z
< 0.8$). Our measurements are based on 35,639 emission line galaxies and cover
a volume of $\sim10^7$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 [OII] emitters, the characteristic luminosity
$L_*(z=0.5)=3.2\times10^{41}$ erg/s increases by a factor of $2.7 \pm 0.2$ from
z=0.5 to 1.3; for H{\beta} emitters $L_*(z=0.3)=1.3\times10^{41}$ erg/s
increases by a factor of $2.0 \pm 0.2$ from z=0.3 to 0.8; and for [OIII]
emitters $L_*(z=0.3)=7.3\times10^{41}$ erg/s increases by a factor of $3.5 \pm
0.4$ from z=0.3 to 0.8.
