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 , \left [ \mathrm { O \textrm { { ii } } } \right ] ( \lambda \lambda 3726 , 3729 ) ( 0.5 < z < 1.3 ) , H { \beta } ( \lambda 4861 ) ( 0.3 < z < 0.8 ) and \left [ \mathrm { O \textrm { { iii } } } \right ] ( \lambda 5007 ) ( 0.3 < z < 0.8 ) .
Our measurements are based on 35,639 emission line galaxies and cover a volume of \sim 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 \left [ \mathrm { O \textrm { { ii } } } \right ] emitters , the characteristic luminosity L _ { * } ( z = 0.5 ) = 3.2 \times 10 ^ { 41 } { erg \cdot s ^ { -1 } } 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 \times 10 ^ { 41 } { erg \cdot s ^ { -1 } } increases by a factor of 2.0 \pm 0.2 from z=0.3 to 0.8 ; and for \left [ \mathrm { O \textrm { { iii } } } \right ] emitters L _ { * } ( z = 0.3 ) = 7.3 \times 10 ^ { 41 } { erg \cdot s ^ { -1 } } increases by a factor of 3.5 \pm 0.4 from z=0.3 to 0.8 .