The redshift, as determined in the AEGIS catalogues from the [OII] line using DEEP2 spectra;

the angular distance D_A and the luminosity distance D_L;

the SFR from the [OII] line luminosity in the galaxy-integrated “1D” spectrum, obtained according to Kewley et al. (2004) calibration;

the extinction-corrected SFR obtained from 24 μm and UV continuum by Tacconi et al. (2013);

the SFR extrapolated from the empirical calibration of Moustakas et al. (2006);

the gas mass derived from the IRAM Plateau de Bure observations;

the total star mass obtained by SED fittings from CFHT B, R, and I bands photometric data using kcorrect (Blanton & Roweis 2007), corrected for a Universe with H₀ = 70  km   s^-1   Mpc^-1;

the gas fraction f_gas = M_gas/(M_gas + M_star);

the optical half light radius R_1/2 as indicated in Tacconi et al. (2013);

the surface densities associated to the gas mass, the star formation rate, and the star mass, calculated within R_1/2, for example as ;

Hα, visible, and [OII] extinctions as derived from the kcorrect SED reconstruction; and

the extinction ratio A_Hα/A_[OII]. A_V, A_[OII], A_Hα/A_[OII], SFR_24μm+UV and SFR_[OII],B are given for information only. O’Donnell (1994) predicts that A_Hα/A_[OII] is around 1.86 for a diffuse interstellar medium, and the variations here observed from one galaxy to the other are representative of the quality of the kcorrect fit. The comparison between SFR_[OII], SFR_24μm+UV, and SFR_[OII],B gives an idea of the uncertainties in the SFR.